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2023

1. Duarte, J., Gonzalez-Gaitan, S., Mourao, A., Paulino-Afonso, A., Guilherme-Garcia, P., Aguas, J., Galbany, L., Kelsey, L., Scolnic, D., Sullivan, M., Brout, D., Palmese, A., Wiseman, P., Aguena, M., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., Pereira, M., Davis, T., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Gatti, M., Gerdes, D., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Melchior, P., Miquel, R., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., 2023, A&A, 680, A56, A sample of dust attenuation laws for Dark Energy Survey supernova host galaxies
   Abstract

   Context. Type Ia supernovae (SNe Ia) are useful distance indicators in cosmology, provided their luminosity is standardized by applying empirical corrections based on light-curve properties. One factor behind these corrections is dust extinction, which is accounted for in the color-luminosity relation of the standardization. This relation is usually assumed to be universal, which can potentially introduce systematics into the standardization. The "mass step" observed for SN Ia Hubble residuals has been suggested as one such systematic.
   Aims: We seek to obtain a more complete view of dust attenuation properties for a sample of 162 SN Ia host galaxies and to probe their link to the mass step.
   Methods: We inferred attenuation laws toward hosts from both global and local (4 kpc) Dark Energy Survey photometry and composite stellar population model fits.
   Results: We recovered a relation between the optical depth and the attenuation slope, best explained by differing star-to-dust geometry for different galaxy orientations, which is significantly different from the optical depth and extinction slope relation observed directly for SNe. We obtain a large variation of attenuation slopes and confirm these change with host properties, such as the stellar mass and age, meaning a universal SN Ia correction should ideally not be assumed. Analyzing the cosmological standardization, we find evidence for a mass step and a two-dimensional "dust step", both more pronounced for red SNe. Although comparable, the two steps are not found to be completely analogous.
   Conclusions: We conclude that host galaxy dust data cannot fully account for the mass step, using either an alternative SN standardization with extinction proxied by host attenuation or a dust-step approach.

   DES-2022-069. FERMILAB-PUB-22-760-PPD.

   The DES-SN host galaxy photometric data and corresponding SN light-curve parameters are available as part of the DES3YR data release, accessible at https://www.darkenergysurvey.org/des-year-3-supernova-cosmology-results/. Cornerplots and SED fit plots for the host galaxies can be found at https://github.com/SN-CRISP/DES-SN_Host-Galaxies

2. Webber, K., Hansen, T., Marshall, J., Simon, J., Pace, A., Mutlu-Pakdil, B., Drlica-Wagner, A., Martinez-Vazquez, C., Aguena, M., Allam, S., Alves, O., Bertin, E., Brooks, D., Carnero Rosell, A., Carretero, J., da Costa, L., De Vicente, J., Doel, P., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Giannini, G., Gruen, D., Gruendl, R., Hinton, S., Hollowood, D., Honscheid, K., Kuehn, K., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Pereira, M., Pieres, A., Plazas Malagon, A., Sanchez, E., Santiago, B., Smith, J., Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., Yanny, B., 2023, ApJ, 959, 141, Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate
   Abstract

   We present a detailed chemical abundance analysis of the brightest star in the ultrafaint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from carbon to europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the -elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, and Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova originating from a star with a mass of ~11.2 M . In addition, the star has a potassium abundance of [K/Fe] = 0.81, which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature that is also present in a number of UFD galaxies. A comparison including globular clusters and stellar stream stars suggests that high K is a specific characteristic of some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies. ^* This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

3. Kareta, T., Thomas, C., Li, J., Knight, M., Moskovitz, N., Rozek, A., Bannister, M., Ieva, S., Snodgrass, C., Pravec, P., Ryan, E., Ryan, W., Fahnestock, E., Rivkin, A., Chabot, N., Fitzsimmons, A., Osip, D., Lister, T., Sarid, G., Hirabayashi, M., Farnham, T., Tancredi, G., Michel, P., Wainscoat, R., Weryk, R., Burrati, B., Pittichova, J., Ridden-Harper, R., Tan, N., Tristram, P., Brown, T., Bonavita, M., Burgdorf, M., Khalouei, E., Longa, P., Rabus, M., Sajadian, S., Jorgensen, U., Dominik, M., Kikwaya, J., Mazzotta Epifani, E., Dotto, E., Deshapriya, P., Hasselmann, P., Dall'Ora, M., Abe, L., Guillot, T., Mekarnia, D., Agabi, A., Bendjoya, P., Suarez, O., Triaud, A., Gasparetto, T., Gunther, M., Kueppers, M., Merin, B., Chatelain, J., Gomez, E., Usher, H., Stoddard-Jones, C., Bartnik, M., Bellaver, M., Chetan, B., Dugan, E., Fallon, T., Fedewa, J., Gerhard, C., Jacobson, S., Painter, S., Peterson, D., Rodriguez, J., Smith, C., Sokolovsky, K., Sullivan, H., Townley, K., Watson, S., Webb, L., Trigo-Rodriguez, J., Llenas, J., Perez-Garcia, I., Castro-Tirado, A., Vincent, J., Migliorini, A., Lazzarin, M., La Forgia, F., Ferrari, F., Polakis, T., Skiff, B., 2023, ApJL, 959, L12, Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
   Abstract

   The impact of the Double Asteroid Redirection Test spacecraft into Dimorphos, moon of the asteroid Didymos, changed Dimorphos's orbit substantially, largely from the ejection of material. We present results from 12 Earth-based facilities involved in a world-wide campaign to monitor the brightness and morphology of the ejecta in the first 35 days after impact. After an initial brightening of ~1.4 mag, we find consistent dimming rates of 0.11-0.12 mag day^-1 in the first week, and 0.08-0.09 mag day^-1 over the entire study period. The system returned to its pre-impact brightness 24.3-25.3 days after impact though the primary ejecta tail remained. The dimming paused briefly eight days after impact, near in time to the appearance of the second tail. This was likely due to a secondary release of material after re-impact of a boulder released in the initial impact, though movement of the primary ejecta through the aperture likely played a role.

4. Chandler, C., Oldroyd, W., Trujillo, C., Hsieh, H., Sedaghat, N., Kueny, J., Burris, W., DeSpain, J., Farrell, K., Magbanua, M., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., Lamperti, A., da Silva Campos, J., Goodwin, B., Terentev, I., Dukes, C., 2023, RNAAS, 7, 271, New Active Jupiter Family Comet 2008 QZ44: a Discovery with Citizen Science
   Abstract

   We report our discovery of cometary activity in the form of a diffuse tail associated with minor planet 2008 QZ₄₄ during two previous orbits: 2008 and 2017. This finding was prompted in part by Active Asteroids, our Zooniverse-hosted NASA Partner Citizen Science program. Participants flagged two UT 2017 July 12 Dark Energy Camera images of 2008 QZ₄₄ as active. Independently, our team identified activity in nine Canada-France-Hawaii Telescope MegaPrime images from UT 2008 November 20. During both apparitions 2008 QZ₄₄ was near its perihelion passage. 2008 QZ₄₄ has a Tisserand parameter with respect to Jupiter of 2.821, placing it in the Jupiter-family comet (JFC) class, and our dynamical integrations confirm this classification. JFCs contain primordial material that informs us about solar system evolution, and help us map the present-day volatile distribution. We note that 2008 QZ₄₄ has previously been classified as a quasi-Hilda comet candidate.

5. Chandler, C., Oldroyd, W., Trujillo, C., Hsieh, H., Burris, W., Kueny, J., DeSpain, J., Sedaghat, N., Farrell, K., Magbanua, M., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., Lamperti, A., da Silva Campos, J., Goodwin, B., Terentev, I., Dukes, C., 2023, RNAAS, 7, 279, Mars-Crossing Minor Planet 2018 VL10: a Jupiter-family Comet Discovery via Citizen Science
   Abstract

   We announce the discovery of cometary activity emitting from minor planet 2018 VL₁₀ in Dark Energy Camera images spanning from UT 2018 December 31 to UT 2019 March 3. The activity was identified by volunteers of our NASA Partner program Active Asteroids, a Zooniverse-hosted Citizen Science project designed to find previously unknown activity in known minor planets. Notably, 2018 VL₁₀ crosses the orbits of Mars and Jupiter, and experiences close approaches of less than 0.5 au with both Earth and Jupiter. We classify 2018 VL₁₀ as a member of the Jupiter-family comets, a group of objects especially important to understand because they hold important clues about the solar system volatile distribution, past and present.

6. Polishook, D., DeMeo, F., Burt, B., Thomas, C., Rivkin, A., Sanchez, J., Reddy, V., 2023, PSJ, 4, 229, Near-IR Spectral Observations of the Didymos System: Daily Evolution Before and After the DART Impact Indicates that Dimorphos Originated from Didymos
   Abstract

   Ejecta from Dimorphos following the DART mission impact significantly increased the brightness of the Didymos-Dimorphos system, allowing us to examine subsurface material. We report daily near-IR spectroscopic observations of the Didymos system using NASA's IRTF that follow the evolution of the spectral signature of the ejecta cloud over 1 week, from 1 day before the impact. Overall, the spectral features remained fixed (S-type classification) while the ejecta dissipated, confirming that both Didymos and Dimorphos are constructed from the same silicate material. This novel result strongly supports binary asteroid formation models that include the breaking up of a single body due to rotational breakup of kilometer-wide bodies. At impact time +14 and +38 hr, the spectral slope decreased, but the following nights presented an increasing spectral slope that almost returned to the preimpact slope. However, the parameters of the 1 m band remained fixed, and no "fresh"/Q-type-like spectrum was measured. We interpret this as follows. (1) The ejecta cloud is the main contributor (60%-70%) to the overall light during the ~40 hr after impact. (2) Coarser debris (100 m) dominated the ejecta cloud, decreasing the spectral slope (after radiation pressure removed the fine grains 10 hr after impact). (3) After approximately 1 week, the ejecta cloud dispersed enough to make the fine grains on Didymos's surface the dominant part of the light, increasing the spectral slope to the preimpact level. (4) A negligible amount of nonweathered material was ejected from Dimorphos's subsurface, suggesting that Dimorphos was accumulated from weathered material ejected from Didymos's surface.

7. DeSpain, J., Chandler, C., Oldroyd, W., Hsieh, H., Trujillo, C., Burris, W., Kueny, J., Farrell, K., Mendoza Magbanua, M., Sedaghat, N., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., Lamperti, A., da Silva Campos, J., Goodwin, B., Terentev, I., Dukes, C., 2023, RNAAS, 7, 257, Citizen Science Discovery of a Recurrently Active Jupiter-Family Comet: (551023) 2012 UQ192
   Abstract

   We have discovered evidence of cometary activity originating from (551023) 2012 UQ₁₉₂ (alternately designated 2019 SN₄₀), which we dynamically classify as a Jupiter Family Comet (JFC). JFCs have eccentric Jupiter-crossing orbits and originate in the Kuiper Belt. Analysis of these objects can provide vital information about minor planets in the outer solar system, such as the distribution of volatiles within the solar system. Activity on 2012 UQ₁₉₂ was first recognized by volunteers on our NASA Partner Citizen Science project Active Asteroids. Through our own examination of archival image data, we found a total of ~30 images presenting strong evidence of activity near perihelion during two separate orbits. 2012 UQ₁₉₂ is notable as we found it to be recurrently active. When 2012 UQ₁₉₂ approaches its perihelion passage in 2027 September, we predict it will reactivate and will be a prime subject for follow-up observations.

8. Baines, E., Clark, J., Schmitt, H., Stone, J., von Braun, K., 2023, AJ, 166, 268, 33 New Stellar Angular Diameters from the NPOI, and Nearly 180 NPOI Diameters as an Ensemble
   Abstract

   We present new angular diameter measurements for 33 stars from the Navy Precision Optical Interferometer, reaching uncertainties on the limb-darkened diameter of 2% or less for 21 targets. We also determined the physical radius, bolometric flux, luminosity, and effective temperature for each star. Our sample is a mix of giant, subgiant, and dwarf stars, and span spectral classes from mid-A to to mid-K. We combined these 33 stars with samples from previous publications to analyze how the NPOI diameters compare to those obtained using other means, namely (V - K) color, the JMMC Stellar Diameters Catalog, and Gaia predictions.

9. Toy, M., Wiseman, P., Sullivan, M., Frohmaier, C., Graur, O., Palmese, A., Popovic, B., Davis, T., Galbany, L., Kelsey, L., Lidman, C., Scolnic, D., Allam, S., Desai, S., Abbott, T., Aguena, M., Alves, O., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Conselice, C., da Costa, L., Pereira, M., De Vicente, J., Diehl, H., Doel, P., Everett, S., Ferrero, I., Frieman, J., Gerdes, D., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Marshall, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Pieres, A., Plazas Malagon, A., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., DES Collaboration, 2023, MNRAS, 526, 5292, Rates and properties of Type Ia supernovae in galaxy clusters within the dark energy survey
   Abstract

   We identify 66 photometrically classified Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline faster than those in the field (97.7 per cent confidence). However, when limiting these samples to host galaxies of similar colour and mass, there is no significant difference in the SN light-curve properties. Motivated by previous detections of a higher-normalized SN Ia delay-time distribution in galaxy clusters, we measure the intrinsic rate of SNe Ia in cluster and field environments. We find the average ratio of the SN Ia rate per galaxy between high-mass ($10\le \log \mathrm{(\mathit{ M}_{*}/{\rm \mathit{ M}}_{\odot })} \le 11.25$) cluster and field galaxies to be 0.594 0.068. This difference is mass-dependent, with the ratio declining with increasing mass, which suggests that the stellar populations in cluster hosts are older than those in field hosts. We show that the mass-normalized rate (or SNe per unit mass) in massive-passive galaxies is consistent between cluster and field environments. Additionally, both of these rates are consistent with rates previously measured in clusters at similar redshifts. We conclude that in massive-passive galaxies, which are the dominant hosts of cluster SNe, the cluster delay-time distribution is comparable to the field.

10. Anbajagane, D., Chang, C., Banerjee, A., Abel, T., Gatti, M., Ajani, V., Alarcon, A., Amon, A., Baxter, E., Bechtol, K., Becker, M., Bernstein, G., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Chen, R., Choi, A., Davis, C., DeRose, J., Diehl, H., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Gruen, D., Gruendl, R., Harrison, I., Hartley, W., Huff, E., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Kokron, N., Kuropatkin, N., Leget, P., MacCrann, N., McCullough, J., Myles, J., Navarro-Alsina, A., Pandey, S., Prat, J., Raveri, M., Rollins, R., Roodman, A., Rykoff, E., Sanchez, C., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Whiteway, L., Yanny, B., Yin, B., Zhang, Y., Abbott, T., Allam, S., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Blazek, J., Brooks, D., Cawthon, R., da Costa, L., Pereira, M., Davis, T., Desai, S., Doel, P., Ferrero, I., Frieman, J., Giannini, G., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Lahav, O., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Palmese, A., Pieres, A., Plazas Malagon, A., Reil, K., Sanchez, E., Smith, M., Swanson, M., Tarle, G., Wiseman, P., DES Collaboration, 2023, MNRAS, 526, 5530, Beyond the 3rd moment: a practical study of using lensing convergence CDFs for cosmology with DES Y3
    Abstract

    Widefield surveys probe clustered scalar fields - such as galaxy counts, lensing potential, etc. - which are sensitive to different cosmological and astrophysical processes. Constraining such processes depends on the statistics that summarize the field. We explore the cumulative distribution function (CDF) as a summary of the galaxy lensing convergence field. Using a suite of N-body light-cone simulations, we show the CDFs' constraining power is modestly better than the second and third moments, as CDFs approximately capture information from all moments. We study the practical aspects of applying CDFs to data, using the Dark Energy Survey (DES Y3) data as an example, and compute the impact of different systematics on the CDFs. The contributions from the point spread function and reduced shear approximation are $\lesssim 1~{{\ \rm per\ cent}}$ of the total signal. Source clustering effects and baryon imprints contribute 1-10 per cent. Enforcing scale cuts to limit systematics-driven biases in parameter constraints degrade these constraints a noticeable amount, and this degradation is similar for the CDFs and the moments. We detect correlations between the observed convergence field and the shape noise field at 13. The non-Gaussian correlations in the noise field must be modelled accurately to use the CDFs, or other statistics sensitive to all moments, as a rigorous cosmology tool.

11. Reuter, D., Simon, A., Lunsford, A., Kaplan, H., Garrison, M., Simpson, J., Casto, G., Dolch, Z., Finneran, P., Grundy, W., Howett, C., Kim, P., Loose, M., Null, T., Parong, F., Rodriguez-ruiz, J., Roming, P., Smith, K., Thompson, P., Tokarcik, B., Veach, T., Wall, S., Ward, J., Weigle, E., Levison, H., 2023, SSRv, 219, 69, L'Ralph: A Visible/Infrared Spectral Imager for the Lucy Mission to the Trojans
    Abstract

    The Lucy Mission to the Trojan asteroids in Jupiter's orbit carries an instrument named L'Ralph, a visible/near infrared multi-spectral imager and a short wavelength infrared hyperspectral imager. It is one of the core instruments on Lucy, NASA's first mission to the Trojans. L'Ralph's primary purpose is to map the surface geology and composition of these objects, but it will also be used to search for possible tenuous exospheres. It is compact, low mass (32.3 kg), power efficient (24.5 W), and robust with high sensitivity and excellent imaging. These characteristics, and its high degree of redundancy, make L'Ralph ideally suited to this long-duration multi-flyby reconnaissance mission.

12. Sickafoose, A., Levine, S., Bosh, A., Person, M., Zuluaga, C., Knieling, B., Lewis, M., Schindler, K., 2023, PSJ, 4, 221, Material around the Centaur (2060) Chiron from the 2018 November 28 UT Stellar Occultation
    Abstract

    A stellar occultation of Gaia DR3 2646598228351156352 by the Centaur (2060) Chiron was observed from the South African Astronomical Observatory on 2018 November 28 UT. Here we present a positive detection of material surrounding Chiron from the 74-inch telescope for this event. Additionally, a global atmosphere is ruled out at the tens of microbars level for several possible atmospheric compositions. There are multiple 3 drops in the 74-inch light curve: three during immersion and two during emersion. Occulting material is located between 242 and 270 km from the center of the nucleus in the sky plane. Assuming the ring-plane orientation proposed for Chiron from the 2011 occultation, the flux drops are located at 352, 344, and 316 km (immersion) and 357 and 364 km (emersion) from the center, with normal optical depths of 0.26, 0.36, and 0.22 (immersion) and 0.26 and 0.18 (emersion) and equivalent widths between 0.7 and 1.3 km. This detection is similar to the previously proposed two-ring system and is located within the error bars of that ring-pole plane; however, the normal optical depths are less than half of the previous values, and three features are detected on immersion. These results suggest that the properties of the surrounding material have evolved between the 2011, 2018, and 2022 observations.

13. do Nascimento, J., Barnes, S., Saar, S., de Mello, G., Hall, J., Anthony, F., de Almeida, L., Velloso, E., da Costa, J., Petit, P., Strugarek, A., Wargelin, B., Castro, M., Strassmeier, K., Brun, A., 2023, ApJ, 958, 57, A Hale-like Cycle in the Solar Twin 18 Scorpii
    Abstract

    Characterizing the cyclic magnetic activity of stars that are close approximations of our Sun offers our best hope for understanding our Sun's current and past magnetism, the space weather around solar-type stars, and more generally, the dynamos of other cool stars. The nearest current approximation to the Sun is the solar twin 18 Scorpii, a naked-eye Sun-like star of spectral type G2 Va. However, while 18 Scorpii's physical parameters closely match those of the Sun, its activity cycle is about 7 yr, and shorter than the solar cycle. We report the measurement of a periodicity of 15 yr that corresponds to a longer activity cycle for 18 Scorpii based on observations extending to the last three decades. The global magnetic geometry of 18 Scorpii changes with this 15 yr cycle and appears to be equivalent to the solar 22 yr magnetic polarity cycle. These results suggest that 18 Scorpii is also a magnetic proxy for a younger Sun, adding an important new datum for testing dynamo theory and magnetic evolution of low-mass stars. The results perturb our understanding of the relationship between cycle and rotation, constrain the Sun's magnetism and the Sun-Earth connection over the past billion years, and suggest that solar Schwabe and Hale cycle periods have increased over that time span.

14. Asaki, Y., Maud, L., Francke, H., Nagai, H., Petry, D., Fomalont, E., Humphreys, E., Richards, A., Wong, K., Dent, W., Hirota, A., Fernandez, J., Takahashi, S., Hales, A., 2023, ApJ, 958, 86, ALMA High-frequency Long Baseline Campaign in 2021: Highest Angular Resolution Submillimeter Wave Images for the Carbon-rich Star R Lep
    Abstract

    The Atacama Large Millimeter/submillimeter Array (ALMA) was used in 2021 to image the carbon-rich evolved star R Lep in Bands 8-10 (397-908 GHz) with baselines up to 16 km. The goal was to validate the calibration, using band-to-band (B2B) phase referencing with a close phase calibrator J0504-1512, 1.2 from R Lep in this case, and the imaging procedures required to obtain the maximum angular resolution achievable with ALMA. Images of the continuum emission and the hydrogen cyanide (HCN) maser line at 890.8 GHz, from the J = 10-9 transition between the (11¹0) and (04⁰0) vibrationally excited states, achieved angular resolutions of 13, 6, and 5 mas in Bands 8-10, respectively. Self-calibration (self-cal) was used to produce ideal images to compare with the B2B phase referencing technique. The continuum emission was resolved in Bands 9 and 10, leaving too little flux for the self-cal of the longest baselines, so these comparisons are made at coarser resolution. Comparisons showed that B2B phase referencing provided phase corrections sufficient to recover 92%, 83%, and 77% of the ideal image continuum flux densities. The HCN maser was sufficiently compact to obtain self-cal solutions in Band 10 for all baselines (up to 16 km). In Band 10, B2B phase referencing as compared to the ideal images recovered 61% and 70% of the flux density for the HCN maser and continuum, respectively.

15. Marciniak, A., Durech, J., Choukroun, A., Hanus, J., Ogoza, W., Szakats, R., Molnar, L., Pal, A., Monteiro, F., Frappa, E., Beisker, W., Pavlov, H., Moore, J., Adomaviciene, R., Aikawa, R., Andersson, S., Antonini, P., Argentin, Y., Asai, A., Assoignon, P., Barton, J., Baruffetti, P., Bath, K., Behrend, R., Benedyktowicz, L., Bernasconi, L., Biguet, G., Billiani, M., Bazewicz, D., Boninsegna, R., Borkowski, M., Bosch, J., Brazill, S., Bronikowska, M., Bruno, A., Butkiewicz-Bak, M., Caron, J., Casalnuovo, G., Castellani, J., Ceravolo, P., Conjat, M., Delincak, P., Delpau, J., Demeautis, C., Demirkol, A., Drozdz, M., Duffard, R., Durandet, C., Eisfeldt, D., Evangelista, M., Fauvaud, S., Fauvaud, M., Ferrais, M., Filipek, M., Fini, P., Fukui, K., Gahrken, B., Geier, S., George, T., Goffin, B., Golonka, J., Goto, T., Grice, J., Guhl, K., Halir, K., Hanna, W., Harman, M., Hashimoto, A., Hasubick, W., Higgins, D., Higuchi, M., Hirose, T., Hirsch, R., Hofschulz, O., Horaguchi, T., Horbowicz, J., Ida, M., Ignacz, B., Ishida, M., Isobe, K., Jehin, E., Joachimczyk, B., Jones, A., Juan, J., Kaminski, K., Kaminska, M., Kankiewicz, P., Kasebe, H., Kattentidt, B., Kim, D., Kim, M., Kitazaki, K., Klotz, A., Komraus, M., Konstanciak, I., Konyves-Toth, R., Kouno, K., Kowald, E., Krajewski, J., Krannich, G., Kreutzer, A., Kryszczynska, A., Kubanek, J., Kudak, V., Kugel, F., Kukita, R., Kulczak, P., Lazzaro, D., Licandro, J., Livet, F., Maley, P., Manago, N., Manek, J., Manna, A., Matsushita, H., Meister, S., Mesquita, W., Messner, S., Michelet, J., Michimani, J., Mieczkowska, I., Morales, N., Motylinski, M., Murawiecka, M., Newman, J., Nikitin, V., Nishimura, M., Oey, J., Oszkiewicz, D., Owada, M., Pakstiene, E., Pawowski, M., Pereira, W., Perig, V., Pera, J., Pilcher, F., Podlewska-Gaca, E., Polak, J., Polakis, T., Polinska, M., Popowicz, A., Richard, F., Rives, J., Rodrigues, T., Roginski, .., Rondon, E., Rottenborn, M., Schafer, R., Schnabel, C., Schreurs, O., Selva, A., Simon, M., Skiff, B., Skrutskie, M., Skrzypek, J., Sobkowiak, K., Sonbas, E., Sposetti, S., Stuart, P., Szyszka, K., Terakubo, K., Thomas, W., Trela, P., Uchiyama, S., Urbanik, M., Vaudescal, G., Venable, R., Watanabe, H., Watanabe, H., Winiarski, M., Wroblewski, R., Yamamura, H., Yamashita, M., Yoshihara, H., Zawilski, M., Zeleny, P., Zejmo, M., Zukowski, K., Zywica, S., 2023, A&A, 679, A60, Scaling slowly rotating asteroids with stellar occultations
    Abstract

    Context. As evidenced by recent survey results, the majority of asteroids are slow rotators (spin periods longer than 12 h), but lack spin and shape models because of selection bias. This bias is skewing our overall understanding of the spins, shapes, and sizes of asteroids, as well as of their other properties. Also, diameter determinations for large (>60 km) and medium-sized asteroids (between 30 and 60 km) often vary by over 30% for multiple reasons.
    Aims: Our long-term project is focused on a few tens of slow rotators with periods of up to 60 h. We aim to obtain their full light curves and reconstruct their spins and shapes. We also precisely scale the models, typically with an accuracy of a few percent.
    Methods: We used wide sets of dense light curves for spin and shape reconstructions via light-curve inversion. Precisely scaling them with thermal data was not possible here because of poor infrared datasets: large bodies tend to saturate in WISE mission detectors. Therefore, we recently also launched a special campaign among stellar occultation observers, both in order to scale these models and to verify the shape solutions, often allowing us to break the mirror pole ambiguity.
    Results: The presented scheme resulted in shape models for 16 slow rotators, most of them for the first time. Fitting them to chords from stellar occultation timings resolved previous inconsistencies in size determinations. For around half of the targets, this fitting also allowed us to identify a clearly preferred pole solution from the pair of two mirror pole solutions, thus removing the ambiguity inherent to light-curve inversion. We also address the influence of the uncertainty of the shape models on the derived diameters.
    Conclusions: Overall, our project has already provided reliable models for around 50 slow rotators. Such well-determined and scaled asteroid shapes will, for example, constitute a solid basis for precise density determinations when coupled with mass information. Spin and shape models in general continue to fill the gaps caused by various biases.

    Lighcurves are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/679/A60

16. Chandler, C., Oldroyd, W., Trujillo, C., Burris, W., Hsieh, H., Kueny, J., Farrell, K., DeSpain, J., Sedaghat, N., Mendoza Magbanua, M., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., Lamperti, A., Dukes, C., Terentev, I., da Silva Campos, J., Goodwin, B., 2023, RNAAS, 7, 237, New Active Quasi-Hilda Asteroid 2004 CV50: A Citizen Science Discovery
    Abstract

    We report that minor planet 2004 CV₅₀ displayed cometary activity in the form of a short, diffuse tail, first identified by volunteers of the Citizen Science program Active Asteroids, a NASA Partner program hosted on the Zooniverse online platform. The activity is present in three images, from UT 2020 February 15 and UT 2020 March 14, that were acquired with the Dark Energy Camera on the Blanco 4 m telescope at the Cerro-Tololo Inter-American Observatory in Chile. We find that 2004 CV₅₀ is most likely an active quasi-Hilda object rather than an active asteroid, despite 2004 CV₅₀ having a Tisserand parameter with respect to Jupiter of 3.06.

17. Bernardinelli, P., Bernstein, G., Jindal, N., Abbott, T., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., da Costa, L., Pereira, M., Davis, T., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Giannini, G., Gruen, D., Herner, K., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Palmese, A., Pieres, A., Plazas Malagon, A., Raveri, M., Sanchez, E., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., To, C., Walker, A., Wiseman, P., Zhang, Y., DES Collaboration, 2023, ApJS, 269, 18, Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries
    Abstract

    We report the methods of and initial scientific inferences from the extraction of precision photometric information for the >800 trans-Neptunian objects (TNOs) discovered in the images of the Dark Energy Survey (DES). Scene-modeling photometry is used to obtain shot-noise-limited flux measures for each exposure of each TNO, with background sources subtracted. Comparison of double-source fits to the pixel data with single-source fits are used to identify and characterize two binary TNO systems. A Markov Chain Monte Carlo method samples the joint likelihood of the intrinsic colors of each source as well as the amplitude of its flux variation, given the time series of multiband flux measurements and their uncertainties. A catalog of these colors and light-curve amplitudes A is included with this publication. We show how to assign a likelihood to the distribution q(A) of light-curve amplitudes in any subpopulation. Using this method, we find decisive evidence (i.e., evidence ratio <0.01) that cold classical (CC) TNOs with absolute magnitude 6 < H _r < 8.2 are more variable than the hot classical (HC) population of the same H _r , reinforcing theories that the former form in situ and the latter arise from a different physical population. Resonant and scattering TNOs in this H _r range have variability consistent with either the HCs or CCs. DES TNOs with H _r < 6 are seen to be decisively less variable than higher-H _r members of any dynamical group, as expected. More surprising is that detached TNOs are decisively less variable than scattering TNOs, which requires them to have distinct source regions or some subsequent differential processing.

18. Oldroyd, W., Chandler, C., Trujillo, C., Sheppard, S., Hsieh, H., Kueny, J., Burris, W., DeSpain, J., Farrell, K., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, ApJL, 957, L1, Recurring Activity Discovered on Quasi-Hilda 2009 DQ118
    Abstract

    We have discovered two epochs of activity on quasi-Hilda 2009 DQ₁₁₈. Small bodies that display comet-like activity, such as active asteroids and active quasi-Hildas, are important for understanding the distribution of water and other volatiles throughout the solar system. Through our NASA Partner Citizen Science project, Active Asteroids, volunteers classified archival images of 2009 DQ₁₁₈ as displaying comet-like activity. By performing an in-depth archival image search, we found over 20 images from UT 2016 March 8-9 with clear signs of a comet-like tail. We then carried out follow-up observations of 2009 DQ₁₁₈ using the 3.5 m Astrophysical Research Consortium Telescope at Apache Point Observatory, Sunspot, New Mexico, USA and the 6.5 m Magellan Baade Telescope at Las Campanas Observatory, Chile. These images revealed a second epoch of activity associated with the UT 2023 April 22 perihelion passage of 2009 DQ₁₁₈. We performed photometric analysis of the tail and find that it had a similar apparent length and surface brightness during both epochs. We also explored the orbital history and future of 2009 DQ₁₁₈ through dynamical simulations. These simulations show that 2009 DQ₁₁₈ is currently a quasi-Hilda and that it frequently experiences close encounters with Jupiter. We find that 2009 DQ₁₁₈ is currently on the boundary between asteroidal and cometary orbits. Additionally, it has likely been a Jupiter family comet or Centaur for much of the past 10 kyr and will be in these same regions for the majority of the next 10 kyr. Since both detected epochs of activity occurred near perihelion, the observed activity is consistent with sublimation of volatile ices. 2009 DQ₁₁₈ is currently observable until ~mid-October 2023. Further observations would help to characterize the observed activity.

19. Zhou, C., Tong, A., Troxel, M., Blazek, J., Lin, C., Bacon, D., Bleem, L., Chang, C., Costanzi, M., DeRose, J., Dietrich, J., Drlica-Wagner, A., Gruen, D., Gruendl, R., Hoyle, B., Jarvis, M., MacCrann, N., Mawdsley, B., McClintock, T., Melchior, P., Prat, J., Pujol, A., Rozo, E., Rykoff, E., Samuroff, S., Sheldon, E., Shin, T., Rosell, A., Yanny, B., Sanchez, C., Tucker, D., Sevilla-Noarbe, I., Zuntz, J., Varga, T., Zhang, Y., Alves, O., Amon, A., Bertin, E., Brooks, D., Burke, D., Kind, M., da Costa, L., Davis, T., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Gerdes, D., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A., Porredon, A., Raveri, M., Romer, A., Sanchez, E., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., To, C., Weaverdyck, N., Weller, J., Wiseman, P., 2023, MNRAS, 526, 323, The intrinsic alignment of red galaxies in DES Y1 redMaPPer galaxy clusters
    Abstract

    Clusters of galaxies trace the most non-linear peaks in the cosmic density field. The weak gravitational lensing of background galaxies by clusters can allow us to infer their masses. However, galaxies associated with the local environment of the cluster can also be intrinsically aligned due to the local tidal gradient, contaminating any cosmology derived from the lensing signal. We measure this intrinsic alignment in Dark Energy Survey (DES) Year 1 REDMAPPER clusters. We find evidence of a non-zero mean radial alignment of galaxies within clusters between redshifts 0.1-0.7. We find a significant systematic in the measured ellipticities of cluster satellite galaxies that we attribute to the central galaxy flux and other intracluster light. We attempt to correct this signal, and fit a simple model for intrinsic alignment amplitude (A_IA) to the measurement, finding A_IA = 0.15 0.04, when excluding data near the edge of the cluster. We find a significantly stronger alignment of the central galaxy with the cluster dark matter halo at low redshift and with higher richness and central galaxy absolute magnitude (proxies for cluster mass). This is an important demonstration of the ability of large photometric data sets like DES to provide direct constraints on the intrinsic alignment of galaxies within clusters. These measurements can inform improvements to small-scale modelling and simulation of the intrinsic alignment of galaxies to help improve the separation of the intrinsic alignment signal in weak lensing studies.

20. Pace, A., Koposov, S., Walker, M., Caldwell, N., Mateo, M., Olszewski, E., Roederer, I., Bailey, J., Belokurov, V., Kuehn, K., Li, T., Zucker, D., 2023, MNRAS, 526, 1075, The kinematics, metallicities, and orbits of six recently discovered Galactic star clusters with Magellan/M2FS spectroscopy
    Abstract

    We present Magellan/M2FS spectroscopy of four recently discovered Milky Way star clusters (Gran 3/Patchick 125, Gran 4, Garro 01, and LP 866) and two newly discovered open clusters (Gaia 9 and Gaia 10) at low Galactic latitudes. We measure line-of-sight velocities and stellar parameters ([Fe/H], log g, T_eff, and [Mg/Fe]) from high-resolution spectroscopy centred on the Mg triplet and identify 20-80 members per star cluster. We determine the kinematics and chemical properties of each cluster and measure the systemic proper motion and orbital properties by utilizing Gaia astrometry. We find Gran 3 to be an old, metal-poor (mean metallicity of [Fe/H] = -1.83) globular cluster located in the Galactic bulge on a retrograde orbit. Gran 4 is an old, metal-poor ([Fe/H] = -1.84) globular cluster with a halo-like orbit that happens to be passing through the Galactic plane. The orbital properties of Gran 4 are consistent with the proposed LMS-1/Wukong and/or Helmi streams merger events. Garro 01 is metal-rich ([Fe/H] = -0.30) and on a near-circular orbit in the outer disc but its classification as an open cluster or globular cluster is ambiguous. Gaia 9 and Gaia 10 are among the most distant known open clusters at $R_{\mathrm{GC}}\sim 18,~21.2~\mathrm{\, kpc}$ and most metal-poor with [Fe/H] ~-0.50, -0.34 for Gaia 9 and Gaia 10, respectively. LP 866 is a nearby, metal-rich open cluster ([Fe/H] = +0.10). The discovery and confirmation of multiple star clusters in the Galactic plane shows the power of Gaia astrometry and the star cluster census remains incomplete.

21. Sanchez, C., Alarcon, A., Bernstein, G., Sanchez, J., Pandey, S., Raveri, M., Prat, J., Weaverdyck, N., Sevilla-Noarbe, I., Chang, C., Baxter, E., Omori, Y., Jain, B., Alves, O., Amon, A., Bechtol, K., Becker, M., Blazek, J., Choi, A., Campos, A., Rosell, A., Kind, M., Crocce, M., Cross, D., DeRose, J., Diehl, H., Dodelson, S., Drlica-Wagner, A., Eckert, K., Eifler, T., Elvin-Poole, J., Everett, S., Fang, X., Fosalba, P., Gruen, D., Gruendl, R., Harrison, I., Hartley, W., Huang, H., Huff, E., Kuropatkin, N., MacCrann, N., McCullough, J., Myles, J., Krause, E., Porredon, A., Rodriguez-Monroy, M., Rykoff, E., Secco, L., Sheldon, E., Troxel, M., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T., Aguena, M., Allam, S., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carretero, J., Castander, F., Cawthon, R., Conselice, C., Costanzi, M., Pereira, M., Desai, S., Doel, P., Doux, C., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gutierrez, G., Herner, K., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Thomas, D., To, C., (DES Collaboration), 2023, MNRAS, 525, 3896, The Dark Energy Survey Year 3 high-redshift sample: selection, characterization, and analysis of galaxy clustering
    Abstract

    The fiducial cosmological analyses of imaging surveys like DES typically probe the Universe at redshifts z < 1. We present the selection and characterization of high-redshift galaxy samples using DES Year 3 data, and the analysis of their galaxy clustering measurements. In particular, we use galaxies that are fainter than those used in the previous DES Year 3 analyses and a Bayesian redshift scheme to define three tomographic bins with mean redshifts around z ~ 0.9, 1.2, and 1.5, which extend the redshift coverage of the fiducial DES Year 3 analysis. These samples contain a total of about 9 million galaxies, and their galaxy density is more than 2 times higher than those in the DES Year 3 fiducial case. We characterize the redshift uncertainties of the samples, including the usage of various spectroscopic and high-quality redshift samples, and we develop a machine-learning method to correct for correlations between galaxy density and survey observing conditions. The analysis of galaxy clustering measurements, with a total signal to noise S/N ~ 70 after scale cuts, yields robust cosmological constraints on a combination of the fraction of matter in the Universe _m and the Hubble parameter h, $\Omega _m h = 0.195^{+0.023}_{-0.018}$, and 2-3 per cent measurements of the amplitude of the galaxy clustering signals, probing galaxy bias and the amplitude of matter fluctuations, b₈. A companion paper (in preparation) will present the cross-correlations of these high-z samples with cosmic microwave background lensing from Planck and South Pole Telescope, and the cosmological analysis of those measurements in combination with the galaxy clustering presented in this work.

22. Rommel, F., Braga-Ribas, F., Ortiz, J., Sicardy, B., Santos-Sanz, P., Desmars, J., Camargo, J., Vieira-Martins, R., Assafin, M., Morgado, B., Boufleur, R., Benedetti-Rossi, G., Gomes-Junior, A., Fernandez-Valenzuela, E., Holler, B., Souami, D., Duffard, R., Margoti, G., Vara-Lubiano, M., Lecacheux, J., Plouvier, J., Morales, N., Maury, A., Fabrega, J., Ceravolo, P., Jehin, E., Albanese, D., Mariey, H., Cikota, S., Ruzdjak, D., Cikota, A., Szakats, R., Baba Aissa, D., Gringahcene, Z., Kashuba, V., Koshkin, N., Zhukov, V., Fisek, S., Cakir, O., Ozer, S., Schnabel, C., Schnabel, M., Signoret, F., Morrone, L., Santana-Ros, T., Pereira, C., Emilio, M., Burdanov, A., de Wit, J., Barkaoui, K., Gillon, M., Leto, G., Frasca, A., Catanzaro, G., Sanchez, R., Tagliaferri, U., Di Sora, M., Isopi, G., Krugly, Y., Slyusarev, I., Chiorny, V., Mikuz, H., Bacci, P., Maestripieri, M., Grazia, M., de la Cueva, I., Yuste-Moreno, M., Ciabattari, F., Kozhukhov, O., Serra-Ricart, M., Alarcon, M., Licandro, J., Masi, G., Bacci, R., Bosch, J., Behem, R., Prost, J., Renner, S., Conjat, M., Bachini, M., Succi, G., Stoian, L., Juravle, A., Carosati, D., Gowe, B., Carrillo, J., Zheleznyak, A., Montigiani, N., Foster, C., Mannucci, M., Ruocco, N., Cuevas, F., Di Marcantonio, P., Coretti, I., Iafrate, G., Baldini, V., Collins, M., Pal, A., Csak, B., Fernandez-Garcia, E., Castro-Tirado, A., Hudin, L., Madiedo, J., Anghel, R., Calvo-Fernandez, J., Valvasori, A., Guido, E., Gherase, R., Kamoun, S., Fafet, R., Sanchez-Gonzalez, M., Curelaru, L., Vintdevara, C., Danescu, C., Gout, J., Schmitz, C., Sota, A., Belskaya, I., Rodriguez-Marco, M., Kilic, Y., Frappa, E., Klotz, A., Lavayssiere, M., Oliveira, J., Popescu, M., Mammana, L., Fernandez-Lajus, E., Schmidt, M., Hopp, U., Komzik, R., Pribulla, T., Tomko, D., Husarik, M., Erece, O., Eryilmaz, S., Buzzi, L., Gahrken, B., Nardiello, D., Hornoch, K., Sonbas, E., Er, H., Burwitz, V., Sybilski, P., Bykowski, W., Muller, T., Ogloza, W., Goncalves, R., Ferreira, J., Ferreira, M., Bento, M., Meister, S., Bagiran, M., Tekes, M., Marciniak, A., Moravec, Z., Delincak, P., Gianni, G., Casalnuovo, G., Boutet, M., Sanchez, J., Klemt, B., Wuensche, N., Burzynski, W., Borkowski, M., Serrau, M., Dangl, G., Klos, O., Weber, C., Urbanik, M., Rousselot, L., Kubanek, J., Andre, P., Colazo, C., Spagnotto, J., Sickafoose, A., Hueso, R., Sanchez-Lavega, A., Fisher, R., Rengstorf, A., Perello, C., Dascalu, M., Altan, M., Gazeas, K., de Santana, T., Sfair, R., Winter, O., Kalkan, S., Canales-Moreno, O., Trigo-Rodriguez, J., Tsamis, V., Tigani, K., Sioulas, N., Lekkas, G., Bertesteanu, D., Dumitrescu, V., Wilberger, A., Barnes, J., Fieber-Beyer, S., Swaney, R., Fuentes, C., Mendez, R., Dumitru, B., Flynn, R., Wake, D., 2023, A&A, 678, A167, A large topographic feature on the surface of the trans-Neptunian object (307261) 2002 MS₄ measured from stellar occultations
    Abstract

    Context. The physical characterization of trans-Neptunian objects is essential for improving our understanding of the formation and evolution of our Solar System. Stellar occultation is a ground-based technique that can be successfully used to determine some of the TNOs' fundamental physical properties with high precision, such as size and shape.
    Aims: This work is aimed at constraining the size, shape, and geometric albedo of the dwarf planet candidate (307261) 2002 MS₄ through the analysis of nine stellar occultation events. Using multichord detection, we also study the object's topography by analyzing the obtained limb and residuals between the observed chords and the best-fit ellipse. Metods. We predicted and organized the observational campaigns of nine stellar occultations by 2002 MS₄ between 2019 and 2022, resulting in two single-chord events, four double-chord detections, and three events with between 3 and 61 positive chords. We derived the occultation light curves using differential aperture photometry, from which the star ingress and egress instants were calculated. Using 13 selected chords from the 8 August 2020 event, we determined the global elliptical limb of 2002 MS₄. The best-fit ellipse, combined with the object's rotational information from the literature, sets constraints on the object's size, shape, and albedo. Additionally, we developed a new method to characterize the topography features on the object's limb.
    Results: The global limb has a semi-major axis of a = 412 10 km, a semi-minor axis of b= 385 17 km, and the position angle of the minor axis is 121 16. From this instantaneous limb, we obtained 2002 MS₄'s geometric albedo of p_V = 0.1 0.025, using H_V = 3.63 0.05 mag and a projected area-equivalent diameter of 796 24 km. Significant deviations from the fitted ellipse in the northernmost limb were detected from multiple sites, highlighting three distinct topographic features: one 11 km depth depression, followed by a 25₅⁺⁴ km height elevation next to a crater-like depression, with an extension of 322 39 km and 45.1 1.5 km deep.
    Conclusions: Our results indicate the presence of an object that is 138 km smaller in diameter than that derived from thermal data, possibly indicating the presence of a thus-far unknown satellite. However, within the error bars, the geometric albedo in the V-band is in agreement with the results published in the literature, even with the radiometric-derived albedo. This stellar occultation has allowed for the first multichord measurement of a large topography in a TNO.

    Tables B.1-B.5 are available at the CDS via anonymous ftp to cdsarc.cds.unistra.fr (ftp://130.79.128.5) or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/678/A167

23. Noll, K., Brown, M., Buie, M., Grundy, W., Levison, H., Marchi, S., Olkin, C., Stern, S., Weaver, H., 2023, SSRv, 219, 59, Trojan Asteroid Satellites, Rings, and Activity
    Abstract

    The Lucy mission will encounter five Jupiter Trojans during its mission with three of the five already known to be multiple systems. These include a near-equal-mass binary, a small and widely separated satellite, and one intermediate-size satellite system. This chapter reviews the current state of knowledge of Trojan asteroid satellites in the context of similar satellite systems in other small body populations. The prospects for the detection of additional satellites as well as other near-body phenomena are considered. The scientific utility of satellites makes their observation with Lucy an important scientific priority for the mission.

24. Zhao, L., Dumusque, X., Ford, E., Llama, J., Mortier, A., Bedell, M., Al Moulla, K., Bender, C., Blake, C., Brewer, J., Collier Cameron, A., Cosentino, R., Figueira, P., Fischer, D., Ghedina, A., Gonzalez, M., Halverson, S., Kanodia, S., Latham, D., Lin, A., Lo Curto, G., Lodi, M., Logsdon, S., Lovis, C., Mahadevan, S., Monson, A., Ninan, J., Pepe, F., Roettenbacher, R., Roy, A., Santos, N., Schwab, C., Stefansson, G., Szymkowiak, A., Terrien, R., Udry, S., Weiss, S., Wildi, F., Wildi, T., Wright, J., 2023, AJ, 166, 173, The Extreme Stellar-signals Project. III. Combining Solar Data from HARPS, HARPS-N, EXPRES, and NEID
    Abstract

    We present an analysis of Sun-as-a-star observations from four different high-resolution, stabilized spectrographs-HARPS, HARPS-N, EXPRES, and NEID. With simultaneous observations of the Sun from four different instruments, we are able to gain insight into the radial velocity precision and accuracy delivered by each of these instruments and isolate instrumental systematics that differ from true astrophysical signals. With solar observations, we can completely characterize the expected Doppler shift contributed by orbiting Solar System bodies and remove them. This results in a data set with measured velocity variations that purely trace flows on the solar surface. Direct comparisons of the radial velocities measured by each instrument show remarkable agreement with residual intraday scatter of only 15-30 cm s^-1. This shows that current ultra-stabilized instruments have broken through to a new level of measurement precision that reveals stellar variability with high fidelity and detail. We end by discussing how radial velocities from different instruments can be combined to provide powerful leverage for testing techniques to mitigate stellar signals.

25. Hernandez-Lang, D., Klein, M., Mohr, J., Grandis, S., Melin, J., Tarrio, P., Arnaud, M., Pratt, G., Abbott, T., Aguena, M., Alves, O., Andrade-Oliveira, F., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Costanzi, M., da Costa, L., Pereira, M., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Lidman, C., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Romer, A., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., Thomas, D., Weaverdyck, N., (DES Collaboration), 2023, MNRAS, 525, 24, The PSZ-MCMF catalogue of Planck clusters over the DES region
    Abstract

    We present the first systematic follow-up of Planck Sunyaev-Zeldovich effect (SZE) selected candidates down to signal-to-noise (S/N) of 3 over the 5000 deg² covered by the Dark Energy Survey. Using the MCMF cluster confirmation algorithm, we identify optical counterparts, determine photometric redshifts, and richnesses and assign a parameter, f_cont, that reflects the probability that each SZE-optical pairing represents a random superposition of physically unassociated systems rather than a real cluster. The new PSZ-MCMF cluster catalogue consists of 853 MCMF confirmed clusters and has a purity of 90 per cent. We present the properties of subsamples of the PSZ-MCMF catalogue that have purities ranging from 90 per cent to 97.5 per cent, depending on the adopted f_cont threshold. Halo mass estimates M₅₀₀, redshifts, richnesses, and optical centres are presented for all PSZ-MCMF clusters. The PSZ-MCMF catalogue adds 589 previously unknown Planck identified clusters over the DES footprint and provides redshifts for an additional 50 previously published Planck-selected clusters with S/N>4.5. Using the subsample with spectroscopic redshifts, we demonstrate excellent cluster photo-z performance with an RMS scatter in z/(1 + z) of 0.47 per cent. Our MCMF based analysis allows us to infer the contamination fraction of the initial S/N>3 Planck-selected candidate list, which is ~50 per cent. We present a method of estimating the completeness of the PSZ-MCMF cluster sample. In comparison to the previously published Planck cluster catalogues, this new S/N>3 MCMF confirmed cluster catalogue populates the lower mass regime at all redshifts and includes clusters up to z~1.3.

26. McNeill, A., Gowanlock, M., Mommert, M., Trilling, D., Llama, J., Paddock, N., 2023, AJ, 166, 152, An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
    Abstract

    We present photometric data for minor planets observed by the Transiting Exoplanet Survey Satellite during its Cycle 1 operations. In total, we extracted usable detections for 37,965 objects. We present an examination of the reliability of the rotation period and light-curve amplitudes derived from each object based upon the number of detections and the normalized Lomb-Scargle power of our period fitting and compare and contrast our results with previous similar works. We show that for objects with 200 or more photometric detections and a derived normalized, generalized Lomb-Scargle power greater than 0.2, we have an 85% confidence in that period; this encompasses 3492 rotation periods we consider to be highly reliable. We independently examine a series of periods first reported by Pal et al.; periods derived in both works found to have similar results should be considered reliable. Additionally, we demonstrate the need to properly account for the true proportion of slow rotators (P > 100 hr) when inferring shape distributions from sparse photometry.

27. Mosenkov, A., Rich, R., Fusco, M., Kennefick, J., Thilker, D., Marchuk, A., Brosch, N., West, M., Gregg, M., Longstaff, F., Koch-Hansen, A., Abdeen, S., Roque, W., 2023, MNRAS, 525, 3016, The haloes and environments of nearby galaxies (HERON) - III. A 45-kpc spiral structure in the GLSB galaxy UGC 4599
    Abstract

    We use a 0.7-m telescope in the framework of the Halos and Environments of Nearby Galaxies (HERON) survey to probe low surface brightness (LSB) structures in nearby galaxies. One of our targets, UGC 4599, is usually classified as an early-type galaxy surrounded by a blue ring making it a potential Hoag's Object analogue. Prior photometric studies of UGC 4599 were focused on its bright core and the blue ring. However, the HERON survey allows us to study its faint extended regions. With an 8-h integration, we detect an extremely faint outer disc with an extrapolated central surface brightness of _{0, d}(r) = 25.5 mag arcsec^-2 down to 31 mag arcsec^-2 and a scale length of 15 kpc. We identify two distinct spiral arms of pitch angle ~6 surrounding the ring. The spiral arms are detected out to ~45 kpc in radius and the faint disc continues to ~70 kpc. These features are also seen in the GALEX far- and near-ultraviolet bands, in a deep u-band image from the 4.3-m Lowell Discovery Telescope (which reveals inner spiral structure emerging from the core), and in H I. We compare this galaxy to ordinary spiral and elliptical galaxies, giant low surface brightness (GLSB) galaxies, and Hoag's Object itself using several standard galaxy scaling relations. We conclude that the pseudo-bulge and disc properties of UGC 4599 significantly differ from those of Hoag's Object and of normal galaxies, pointing toward a GLSB galaxy nature and filamentary accretion of gas to generate its outer disc.

28. Barnes, J., Standing, M., Haswell, C., Staab, D., Doherty, J., Waller-Bridge, M., Fossati, L., Soto, M., Anglada-Escude, G., Llama, J., McCune, C., Lewis, F., 2023, MNRAS, 524, 5196, DMPP-4: candidate sub-Neptune mass planets orbiting a naked-eye star
    Abstract

    We present radial velocity measurements of the very bright (V ~ 5.7) nearby F star, DMPP-4 (HD 184960). The anomalously low Ca II H&K emission suggests mass-loss from planets orbiting a low activity host star. Periodic radial velocity variability with ~10 m s^-1 amplitude is found to persist over a >4 yr time-scale. Although the non-simultaneous photometric variability in four TESS sectors supports the view of an inactive star, we identify periodic photometric signals and also find spectroscopic evidence for stellar activity. We used a posterior sampling algorithm that includes the number of Keplerian signals, N_p, as a free parameter to test and compare (1) purely Keplerian models (2) a Keplerian model with linear activity correlation and (3) Keplerian models with Gaussian processes. A preferred model, with one Keplerian and quasi-periodic Gaussian process indicates a planet with a period of $P_\textrm {b} = 3.4982^{+0.0015}_{-0.0027}$ d and corresponding minimum mass of $m_\textrm {b}\, \textrm {sin}\, i = 12.2^{+1.8}_{-1.9}$ M. Without further high-time resolution observations over a longer time-scale, we cannot definitively rule out the purely Keplerian model with two candidates planets with $P_\textrm {b} = 2.4570^{+0.0026}_{-0.0462}$ d, minimum mass $m_\textrm {b}\, \textrm {sin}\, i = 8.0^{+1.1}_{-1.5}$ M and $P_\textrm {c} = 5.4196^{+0.6766}_{-0.0030}$ d and corresponding minimum mass of $m_\textrm {b}\, \textrm {sin}\, i = 12.2^{+1.4}_{-1.6}$ M. The candidate planets lie in the region below the lower-envelope of the Neptune Desert. Continued mass-loss may originate from the highly irradiated planets or from an as yet undetected body in the system.

29. Kareta, T., Reddy, V., 2023, PSJ, 4, 174, Nuclear and Orbital Characterization of the Transition Object (4015) 107P/Wilson-Harrington
    Abstract

    Comet 107P/Wilson-Harrington, cross-listed as asteroid 4015, is one of the original transition objects whose properties do not neatly fit into a cometary or asteroidal origin. Discovered in a period of apparently gas-dominated activity in 1949, it was subsequently lost and recovered as the inactive asteroid 1979 VA. We obtained new and reanalyzed archival observations of the object, compared to meteorites, and conducted new orbital integrations in order to understand the nature of this object and to understand where it falls on the asteroid-comet continuum. Wilson-Harrington's reflectance spectrum is approximately neutral from visible to near-infrared wavelengths, but has a reflectance maximum near 0.8-0.9 m. The object's spectrum is well matched by laboratory spectra of carbonaceous chondrite meteorites like the CM Murchison or the C I Ivuna. The object's phase curve slope is compatible with either an asteroidal or cometary origin, and its recent orbital history has no periods with high enough temperatures to have altered its surface. While it is possible that some unknown process has acted to change the surface from an originally cometary one, we instead prefer a fundamentally asteroidal origin for Wilson-Harrington, which can explain its surface and orbital properties. However, this would require a way to maintain significant (hyper)volatile supplies on the near-Earth objects beyond what is currently expected. Wilson-Harrington's similar meteorite affinity and possible orbital link to sample return targets (162173) Ryugu and (101955) Bennu suggest that the returned samples from the Hayabusa-2 and OSIRIS-REx missions might hold the key to understanding this object.

30. Stern, S., White, O., Grundy, W., Keeney, B., Hofgartner, J., Nesvorny, D., McKinnon, W., Richardson, D., Marohnic, J., Verbiscer, A., Benecchi, S., Schenk, P., Moore, J., New Horizons Geology, Geophysics Investigation Team, 2023, PSJ, 4, 176, The Properties and Origin of Kuiper Belt Object Arrokoth's Large Mounds
    Abstract

    We report on a study of the mounds that dominate the appearance of Kuiper Belt Object (486958) Arrokoth's larger lobe, named Wenu. We compare the geological context of these mounds and measure and intercompare their shapes, sizes/orientations, reflectance, and colors. We find the mounds are broadly self-similar in many respects and interpret them as the original building blocks of Arrokoth. It remains unclear why these building blocks are so similar in size-and this represents a new constraint and challenge for solar system formation models. We then discuss the implications of this interpretation.

31. van Holstein, R., Keller, C., Snik, F., Bos, S., 2023, A&A, 677, A150, Polarization-dependent beam shifts upon metallic reflection in high-contrast imagers and telescopes
    Abstract

    Context. To directly image rocky exoplanets in reflected (polarized) light, future space- and ground-based high-contrast imagers and telescopes aim to reach extreme contrasts at close separations from the star. However, the achievable contrast will be limited by reflection-induced polarization aberrations. While polarization aberrations can be modeled with numerical codes, these computations provide little insight into the full range of effects, their origin and characteristics, and possible ways to mitigate them.
    Aims: We aim to understand polarization aberrations produced by reflection off flat metallic mirrors at the fundamental level.
    Methods: We used polarization ray tracing to numerically compute polarization aberrations and interpret the results in terms of the polarization-dependent spatial and angular Goos-Hanchen and Imbert-Federov shifts of the beam of light as described with closed-form mathematical expressions in the physics literature.
    Results: We find that all four beam shifts are fully reproduced by polarization ray tracing. We study the origin and characteristics of the shifts as well as the dependence of their size and direction on the beam intensity profile, incident polarization state, angle of incidence, mirror material, and wavelength. Of the four beam shifts, only the spatial Goos-Hanchen and Imbert-Federov shifts are relevant for high-contrast imagers and telescopes because these shifts are visible in the focal plane and create a polarization structure in the point-spread function that reduces the performance of coronagraphs and the polarimetric speckle suppression close to the star.
    Conclusions: Our study provides a fundamental understanding of the polarization aberrations resulting from reflection off flat metallic mirrors in terms of beam shifts and lays out the analytical and numerical tools to describe these shifts. The beam shifts in an optical system can be mitigated by keeping the f-numbers large and angles of incidence small. Most importantly, mirror coatings should not be optimized for maximum reflectivity, but should be designed to have a retardance close to 180. The insights from our study can be applied to improve the performance of SPHERE-ZIMPOL at the VLT and future telescopes and instruments such as the Roman Space Telescope, the Habitable Worlds Observatory, GMagAO-X at the GMT, PSI at the TMT, and PCS (or EPICS) at the ELT.

32. Jung, D., Calzetti, D., Messa, M., Heyer, M., Sirressi, M., Linden, S., Adamo, A., Chandar, R., Cignoni, M., Cook, D., Dobbs, C., Elmegreen, B., Evans, A., Fumagalli, M., Gallagher, J., Hunter, D., Johnson, K., Kennicutt, R., Krumholz, M., Schaerer, D., Sabbi, E., Smith, L., Tosi, M., Wofford, A., 2023, ApJ, 954, 136, Universal Upper End of the Stellar Initial Mass Function in the Young and Compact LEGUS Clusters
    Abstract

    We investigate the variation in the upper end of the stellar initial mass function (uIMF) in 375 young and compact star clusters in five nearby galaxies within ~5 Mpc. All the young stellar clusters (YSCs) in the sample have ages 4 Myr and masses above 500 M , according to standard stellar models. The YSC catalogs were produced from Hubble Space Telescope images obtained as part of the Legacy ExtraGalactic UV Survey (LEGUS) Hubble treasury program. They are used here to test whether the uIMF is universal or changes as a function of the cluster's stellar mass. We perform this test by measuring the H luminosity of the star clusters as a proxy for their ionizing photon rate, and charting its trend as a function of cluster mass. Large cluster numbers allow us to mitigate the stochastic sampling of the uIMF. The advantage of our approach relative to previous similar attempts is the use of cluster catalogs that have been selected independently of the presence of H emission, thus removing a potential sample bias. We find that the uIMF, as traced by the H emission, shows no dependence on cluster mass, suggesting that the maximum stellar mass that can be produced in star clusters is universal, in agreement with previous findings.

33. Korolik, M., Roettenbacher, R., Fischer, D., Kane, S., Perkins, J., Monnier, J., Davies, C., Kraus, S., Le Bouquin, J., Anugu, N., Gardner, T., Lanthermann, C., Schaefer, G., Setterholm, B., Brewer, J., Llama, J., Zhao, L., Szymkowiak, A., Henry, G., 2023, AJ, 166, 123, Refining the Stellar Parameters of Ceti: a Pole-on Solar Analog
    Abstract

    To accurately characterize the planets a star may be hosting, stellar parameters must first be well determined. Ceti is a nearby solar analog and often a target for exoplanet searches. Uncertainties in the observed rotational velocities have made constraining Ceti's inclination difficult. For planet candidates from radial velocity (RV) observations, this leads to substantial uncertainties in the planetary masses, as only the minimum mass ( $m\sin i$ ) can be constrained with RV. In this paper, we used new long-baseline optical interferometric data from the CHARA Array with the MIRC-X beam combiner and extreme precision spectroscopic data from the Lowell Discovery Telescope with EXPRES to improve constraints on the stellar parameters of Ceti. Additional archival data were obtained from a Tennessee State University Automatic Photometric Telescope and the Mount Wilson Observatory HK project. These new and archival data sets led to improved stellar parameter determinations, including a limb-darkened angular diameter of 2.019 0.012 mas and rotation period of 46 4 days. By combining parameters from our data sets, we obtained an estimate for the stellar inclination of 7 7. This nearly pole-on orientation has implications for the previously reported exoplanets. An analysis of the system dynamics suggests that the planetary architecture described by Feng et al. may not retain long-term stability for low orbital inclinations. Additionally, the inclination of Ceti reveals a misalignment between the inclinations of the stellar rotation axis and the previously measured debris disk rotation axis (i _disk = 35 10).

34. Zaborowski, E., Drlica-Wagner, A., Ashmead, F., Wu, J., Morgan, R., Bom, C., Shajib, A., Birrer, S., Cerny, W., Buckley-Geer, E., Mutlu-Pakdil, B., Ferguson, P., Glazebrook, K., Lozano, S., Gordon, Y., Martinez, M., Manwadkar, V., O'Donnell, J., Poh, J., Riley, A., Sakowska, J., Santana-Silva, L., Santiago, B., Sluse, D., Tan, C., Tollerud, E., Verma, A., Carballo-Bello, J., Choi, Y., James, D., Kuropatkin, N., Martinez-Vazquez, C., Nidever, D., Castellon, J., Noel, N., Olsen, K., Pace, A., Mau, S., Yanny, B., Zenteno, A., Abbott, T., Aguena, M., Alves, O., Andrade-Oliveira, F., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Conselice, C., Costanzi, M., Pereira, M., de Vicente, J., Desai, S., Dietrich, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., Garcia-Bellido, J., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Kuehn, K., Lin, H., Marshall, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A., Prat, J., Rodriguez-Monroy, M., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., To, C., Weaverdyck, N., Delve Collaboration, Des Collaboration, 2023, ApJ, 954, 68, Identification of Galaxy-Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
    Abstract

    We perform a search for galaxy-galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey, which contains ~520 million astronomical sources covering ~4000 deg² of the southern sky to a 5 point-source depth of g = 24.3, r = 23.9, i = 23.3, and z = 22.8 mag. Following the methodology of similar searches using Dark Energy Camera data, we apply color and magnitude cuts to select a catalog of ~11 million extended astronomical sources. After scoring with our CNN, the highest-scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (not a lens) to 3 (very probable lens). We present a list of 581 strong lens candidates, 562 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 55 Grade A candidates, 149 Grade B candidates, and 377 Grade C candidates. We additionally highlight eight potential quadruply lensed quasars from this sample. Due to the location of our search footprint in the northern Galactic cap (b > 10 deg) and southern celestial hemisphere (decl. < 0 deg), our candidate list has little overlap with other existing ground-based searches. Where our search footprint does overlap with other searches, we find a significant number of high-quality candidates that were previously unidentified, indicating a degree of orthogonality in our methodology. We report properties of our candidates including apparent magnitude and Einstein radius estimated from the image separation.

35. Pang, X., Wang, Y., Tang, S., Rui, Y., Bai, J., Li, C., Feng, F., Kouwenhoven, M., Chen, W., Chuang, R., 2023, AJ, 166, 110, Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
    Abstract

    Using membership of 85 open clusters from previous studies based on Gaia Data Release 3 data, we identify binary candidates in the color-magnitude diagram for systems with mass ratio q > 0.4. The binary fraction is corrected for incompleteness at different distances due to the Gaia angular resolution limit. We find a decreasing binary fraction with increasing cluster age, with substantial scatter. For clusters with a total mass >200 M , the binary fraction is independent of cluster mass. The binary fraction depends strongly on stellar density. Among the four types of cluster environments, the lowest-density filamentary and fractal stellar groups have the highest mean binary fraction: 23.6% and 23.2%, respectively. The mean binary fraction in tidal tail clusters is 20.8% and is lowest in the densest halo-type clusters: 14.8%. We find clear evidence of early disruptions of binary stars in the cluster sample. The radial binary fraction depends strongly on the clustercentric distance across all four types of environments, with the smallest binary fraction within the half-mass radius r _h and increasing toward a few r _h. Only hints of mass segregation are found in the target clusters. The observed amounts of mass segregation are not significant enough to generate a global effect inside the target clusters. We evaluate the bias of unresolved binary systems (assuming a primary mass of 1 M ) in 1D tangential velocity, which is 0.1-1 km s^-1. Further studies are required to characterize the internal star cluster kinematics using Gaia proper motions.

36. Samuroff, S., Mandelbaum, R., Blazek, J., Campos, A., MacCrann, N., Zacharegkas, G., Amon, A., Prat, J., Singh, S., Elvin-Poole, J., Ross, A., Alarcon, A., Baxter, E., Bechtol, K., Becker, M., Bernstein, G., Rosell, A., Kind, M., Cawthon, R., Chang, C., Chen, R., Choi, A., Crocce, M., Davis, C., DeRose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Everett, S., Ferte, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R., Harrison, I., Herner, K., Huff, E., Jarvis, M., Kuropatkin, N., Leget, P., Lemos, P., McCullough, J., Myles, J., Navarro-Alsina, A., Pandey, S., Porredon, A., Raveri, M., Rodriguez-Monroy, M., Rollins, R., Roodman, A., Rossi, G., Rykoff, E., Sanchez, C., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Weaverdyck, N., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Alves, O., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Dietrich, J., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Lahav, O., Marshall, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Newman, J., Palmese, A., Pieres, A., Malagon, A., Sanchez, E., Scarpine, V., Smith, M., Suchyta, E., Swanson, M., Tarle, G., To, C., DES Collaboration, 2023, MNRAS, 524, 2195, The Dark Energy Survey Year 3 and eBOSS: constraining galaxy intrinsic alignments across luminosity and colour space
    Abstract

    We present direct constraints on galaxy intrinsic alignments (IAs) using the Dark Energy Survey Year 3 (DES Y3), the Extended Baryon Oscillation Spectroscopic Survey (eBOSS), and its precursor, the Baryon Oscillation Spectroscopic Survey (BOSS). Our measurements incorporate photometric red sequence (redMaGiC) galaxies from DES with median redshift z ~ 0.2-1.0, luminous red galaxies from eBOSS at z ~ 0.8, and also an SDSS-III BOSS CMASS sample at z ~ 0.5. We measure two-point IA correlations, which we fit using a model that includes lensing, magnification, and photometric redshift error. Fitting on scales 6 Mpc h^-1 < r_p < 70 Mpc h^-1, we make a detection of IAs in each sample, at 5-22 (assuming a simple one-parameter model for IAs). Using these red samples, we measure the IA-luminosity relation. Our results are statistically consistent with previous results, but offer a significant improvement in constraining power, particularly at low luminosity. With this improved precision, we see detectable dependence on colour between broadly defined red samples. It is likely that a more sophisticated approach than a binary red/blue split, which jointly considers colour and luminosity dependence in the IA signal, will be needed in future. We also compare the various signal components at the best-fitting point in parameter space for each sample, and find that magnification and lensing contribute $\sim 2\!-\!18~{{\ \rm per\ cent}}$ of the total signal. As precision continues to improve, it will certainly be necessary to account for these effects in future direct IA measurements. Finally, we make equivalent measurements on a sample of emission-line galaxies from eBOSS at z ~ 0.8. We constrain the non-linear alignment amplitude to be $A_1=0.07^{+0.32}_{-0.42}$ (|A₁| < 0.78 at 95 per cent CL).

37. Meyer, A., Agrusa, H., Richardson, D., Daly, R., Fuentes-Munoz, O., Hirabayashi, M., Michel, P., Merrill, C., Nakano, R., Cheng, A., Barbee, B., Barnouin, O., Chesley, S., Ernst, C., Gkolias, I., Moskovitz, N., Naidu, S., Pravec, P., Scheirich, P., Thomas, C., Tsiganis, K., Scheeres, D., 2023, PSJ, 4, 141, The Perturbed Full Two-body Problem: Application to Post-DART Didymos
    Abstract

    With the successful impact of the NASA Double Asteroid Redirection Test (DART) spacecraft in the Didymos-Dimorphos binary asteroid system, we provide an initial analysis of the post-impact perturbed binary asteroid dynamics. To compare our simulation results with observations, we introduce a set of "observable elements" calculated using only the physical separation of the binary asteroid, rather than traditional Keplerian elements. Using numerical methods that treat the fully spin-orbit-coupled dynamics, we estimate the system's mass and the impact-induced changes in orbital velocity, semimajor axis, and eccentricity. We find that the changes to the mutual orbit depend strongly on the separation distance between Didymos and Dimorphos at the time of impact. If Dimorphos enters a tumbling state after the impact, this may be observable through changes in the system's eccentricity and orbit period. We also find that any DART-induced reshaping of Dimorphos would generally reduce the required change in orbital velocity to achieve the measured post-impact orbit period, and will be assessed by the ESA Hera mission in 2027.

38. Chandler, C., Oldroyd, W., Trujillo, C., Hsieh, H., Burris, W., Kueny, J., DeSpain, J., Farrell, K., Magbanua, M., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 170, Erratum: "A Jupiter-family Comet Discovery via Citizen Science: 2005 XR132" (2023, RNAAS, 7, 146)
    Abstract

    No abstract found.

39. Neugent, K., Massey, P., 2023, AJ, 166, 68, Newly Discovered Wolf-Rayet Stars in M31
    Abstract

    The evolved massive star populations of the Local Group galaxies are generally thought to be well understood. However, recent work has suggested that the Wolf-Rayet (WR) content of M31 may have been underestimated. We therefore began a pilot project to search for new WRs in M31 and to reexamine the completeness of our previous WR survey, finished almost a decade prior. Our improved imaging data and spectroscopic follow-up confirmed 19 new WRs across three small fields in M31. These newly discovered WRs are generally fainter than the previously known sample due to slightly increased reddening as opposed to intrinsic faintness. From these findings, we estimate that there are another ~60 WRs left to be discovered in M31; however, the overall ratio of WN-type (nitrogen-rich) to WC-type (carbon-rich) WRs remains unchanged with our latest additions to the M31 WR census. We are in the process of extending this pilot WR survey to include the rest of M31, and a more complete population will be detailed in our future work.

40. Brewer, J., Zhao, L., Fischer, D., Roettenbacher, R., Henry, G., Llama, J., Szymkowiak, A., Cabot, S., Weiss, S., McCarthy, C., 2023, AJ, 166, 46, EXPRES. IV. Two Additional Planets Orbiting Coronae Borealis Reveal Uncommon System Architecture
    Abstract

    Thousands of exoplanet detections have been made over the last 25 years using Doppler observations, transit photometry, direct imaging, and astrometry. Each of these methods is sensitive to different ranges of orbital separations and planetary radii (or masses). This makes it difficult to fully characterize exoplanet architectures and to place our solar system in context with the wealth of discoveries that have been made. Here, we use the EXtreme PREcision Spectrograph to reveal planets in previously undetectable regions of the mass-period parameter space for the star Coronae Borealis. We add two new planets to the previously known system with one hot Jupiter in a 39 day orbit and a warm super-Neptune in a 102 day orbit. The new detections include a temperate Neptune planet ( $M\sin i\sim 20$ M ) in a 281.4 day orbit and a hot super-Earth ( $M\sin i=3.7$ M ) in a 12.95 day orbit. This result shows that details of planetary system architectures have been hiding just below our previous detection limits; this signals an exciting era for the next generation of extreme precision spectrographs.

41. Hofgartner, J., Buratti, B., Beyer, R., Ennico, K., Grundy, W., Howett, C., Johnson, P., Lauer, T., Olkin, C., Spencer, J., Alan Stern, S., Weaver, H., Young, L., 2023, PSJ, 4, 132, Bolometric Hemispherical Albedo Map of Pluto from New Horizons Observations
    Abstract

    The New Horizons encounter with the Pluto system revealed Pluto to have an extremely spatially variable surface with expansive dark, bright, and intermediate terrains, refractory and volatile ices, and ongoing/recent endogenous and exogenous processes. Albedo is useful for understanding volatile transport because it quantifies absorbed solar energy; albedo may also provide insights into surface processes. Four filters of the New Horizons LORRI and MVIC imagers are used to approximate the bolometric (flux-weighted, wavelength-integrated) albedo. The bolometric hemispherical albedo (local energy balance albedo) as a function of the incidence angle of the solar illumination is measured for both Cthulhu and Sputnik Planitia, which are extensive, extreme dark and extreme bright terrains on Pluto. For both terrains, the bolometric hemispherical albedo increases by >30% from 0 to 90 incidence. The incidence-angle-average bolometric hemispherical albedo of Cthulhu is 0.12 0.01, and that of Sputnik Planitia is 0.80 0.06, where uncertainties are estimates based on scatter from different photometric functional approximations. The bolometric Bond albedo (global energy balance albedo) of Cthulhu is 0.12 0.01, and that of Sputnik Planitia is 0.80 0.07. A map of Pluto's incidence-angle-average bolometric hemispherical albedo is produced. The incidence-angle-average bolometric hemispherical albedo, spatially averaged over areas north of 30 S, is 0.54. Pluto has three general albedo categories: (1) very low albedo southern equatorial terrains, including Cthulhu; (2) high-albedo terrains, which constitute most of Pluto's surface; and (3) very high albedo terrains, including Sputnik Planitia. Pluto's extraordinary albedo variability with location is also spatially sharp at some places.

42. Mallaby-Kay, M., Amodeo, S., Hill, J., Aguena, M., Allam, S., Alves, O., Annis, J., Battaglia, N., Battistelli, E., Baxter, E., Bechtol, K., Becker, M., Bertin, E., Bond, J., Brooks, D., Calabrese, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Choi, A., Crocce, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Dietrich, J., Doel, P., Doux, C., Drlica-Wagner, A., Dunkley, J., Elvin-Poole, J., Everett, S., Ferraro, S., Ferrero, I., Frieman, J., Gallardo, P., Garcia-Bellido, J., Giannini, G., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., James, D., Kosowsky, A., Kuehn, K., Lokken, M., Louis, T., Marshall, J., McMahon, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Moodley, K., Mroczkowski, T., Naess, S., Niemack, M., Ogando, R., Page, L., Pandey, S., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Rykoff, E., Samuroff, S., Sanchez, E., Schaan, E., Sevilla-Noarbe, I., Sheldon, E., Sifon, C., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Tarle, G., To, C., Vargas, C., Vavagiakis, E., Weaverdyck, N., Weller, J., Wiseman, P., Yanny, B., 2023, PhRvD, 108, 023516, Kinematic Sunyaev-Zel'dovich effect with ACT, DES, and BOSS: A novel hybrid estimator
    Abstract

    The kinematic and thermal Sunyaev-Zel'dovich (kSZ and tSZ) effects probe the abundance and thermodynamics of ionized gas in galaxies and clusters. We present a new hybrid estimator to measure the kSZ effect by combining cosmic microwave background temperature anisotropy maps with photometric and spectroscopic optical survey data. The method interpolates a velocity reconstruction from a spectroscopic catalog at the positions of objects in a photometric catalog, which makes it possible to leverage the high number density of the photometric catalog and the precision of the spectroscopic survey. Combining this hybrid kSZ estimator with a measurement of the tSZ effect simultaneously constrains the density and temperature of free electrons in the photometrically selected galaxies. Using the 1000 deg² of overlap between the Atacama Cosmology Telescope (ACT) Data Release 5, the first three years of data from the Dark Energy Survey (DES), and the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 12, we detect the kSZ signal at 4.8 and reject the null (no-kSZ) hypothesis at 5.1 . This corresponds to 2.0 per 100,000 photometric objects with a velocity field based on a spectroscopic survey with 1 /5^th the density of the photometric catalog. For comparison, a recent ACT analysis using exclusively spectroscopic data from BOSS measured the kSZ signal at 2.1 per 100,000 objects. Our derived constraints on the thermodynamic properties of the galaxy halos are consistent with previous measurements. With future surveys, such as the Dark Energy Spectroscopic Instrument and the Rubin Observatory Legacy Survey of Space and Time, we expect that this hybrid estimator could result in measurements with significantly better signal-to-noise than those that rely on spectroscopic data alone.

43. Prato, L., Simon, M., 2023, RNAAS, 7, 150, Evolution of Circumstellar Disks around T Tauri Stars as a Function of Stellar Age
    Abstract

    We analyzed the distribution of surface gravities, $\mathrm{log}\,g$ , of a sample of classical T Tauri stars in Taurus to examine the relationship between stellar ages and circumstellar disk evolution. This is critical to understanding the timescales for planet formation. Given the uncertainties in $\mathrm{log}\,g$ , we find no distinction between the ages of stars with and without disks beyond that identified previously. This approach, while avoiding the contamination that plagues young star luminosity measurements, will require precisions in $\mathrm{log}\,g$ of 0.05 dex or better to be effective.

44. Landman, R., Snellen, I., Keller, C., N'Diaye, M., Fagginger-Auer, F., Desgrange, C., 2023, A&A, 675, A157, Trade-offs in high-contrast integral field spectroscopy for exoplanet detection and characterisation. Young gas giants in emission
    Abstract

    Context. Combining high-contrast imaging with medium- or high-resolution integral field spectroscopy has the potential to boost the detection rate of exoplanets, especially at small angular separations. Furthermore, it immediately provides a spectrum of the planet that can be used to characterise its atmosphere. The achievable spectral resolution, wavelength coverage, and FOV of such an instrument are limited by the number of available detector pixels.
    Aims: We aim to study the effect of the spectral resolution, wavelength coverage, and FOV on the detection and characterisation potential of medium- to high-resolution integral field spectrographs with molecule mapping.
    Methods: The trade-offs are studied through end-to-end simulations of a typical high-contrast imaging instrument, analytical considerations, and atmospheric retrievals. The results are then validated with archival VLT/SINFONI data of the planet Pictoris b.
    Results: We show that molecular absorption spectra generally have decreasing power towards higher spectral resolution and that molecule mapping is already powerful for moderate resolutions (R 300). When choosing between wavelength coverage and spectral resolution for a given number of spectral bins, it is best to first increase the spectral resolution until R ~ 2000 and then maximise the bandwidth within an observing band. We find that T-type companions are most easily detected in the J/H band through methane and water features, while L-type companions are best observed in the H/K band through water and CO features. Such an instrument does not need to have a large FOV, as most of the gain in contrast is obtained in the speckle-limited regime close to the star. We show that the same conclusions are valid for the constraints on atmospheric parameters such as the C/O ratio, metallicity, surface gravity, and temperature, while higher spectral resolution (R 10 000) is required to constrain the radial velocity and spin of the planet.

45. Chandler, C., Oldroyd, W., Trujillo, C., Hsieh, H., Burris, W., Kueny, J., DeSpain, J., Farrell, K., Magbanua, M., Sheppard, S., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 146, A Jupiter-family Comet Discovery via Citizen Science: 2005 XR132
    Abstract

    We report the discovery of cometary activity associated with minor planet 2005 XR₁₃₂, a finding facilitated by our NASA Partner program Active Asteroids, hosted on the Zooniverse online Citizen Science platform. Volunteers identified activity in a Dark Energy Camera image of 2005 XR₁₃₂ from UT 2021 March 26, and our own investigation uncovered additional images of activity in Zwicky Transient Facility data spanning UT 2021 January 3 through March 31. 2005 XR₁₃₂ has a semimajor axis a = 3.760 au, eccentricity e = 0.432, inclination i = 14.474, and a Tisserand parameter with respect to Jupiter of T _J = 2.869, and thus is dynamically classified as a Jupiter-family comet.

46. Dijkema, T., Vida, D., Bassa, C., Moskovitz, N., Eschman, P., 2023, eMetN, 8, 252, GMN observations of the Crew-5 trunk reentry
    Abstract

    Using the cameras of the Global Meteor Network in Arizona, Colorado and New Mexico we reconstruct the reentry trajectory of the Dragon capsule trunk (Crew-5 flight) which occurred on 2023 April 27 around 08h52m UTC. We compare the preliminary trajectory to known orbital information of the object and deduce the moment of rapid reentry.

47. Richey-Yowell, T., Shkolnik, E., Schneider, A., Peacock, S., Huseby, L., Jackman, J., Barman, T., Osby, E., Meadows, V., 2023, ApJ, 951, 44, HAZMAT. IX. An Analysis of the UV and X-Ray Evolution of Low-mass Stars in the Era of Gaia
    Abstract

    Low-mass stars (1 M ) are some of the best candidates for hosting planets with detectable life because of these stars' long lifetimes and relative ratios of planet to star mass and radius. An important aspect of these stars to consider is the amount of ultraviolet (UV) and X-ray radiation incident on planets in the habitable zones due to the ability of UV and X-ray radiation to alter the chemistry and evolution of planetary atmospheres. In this work, we build on the results of the HAZMAT I and HAZMAT III M-star studies to determine the intrinsic UV and X-ray flux evolution with age for M stars using Gaia parallactic distances. We then compare these results to the intrinsic fluxes of K stars adapted from HAZMAT V. We find that although the intrinsic M-star UV flux is 10-100 times lower than that of K stars, the UV fluxes in their respective habitable zone are similar. However, the habitable zone X-ray flux evolutions are slightly more distinguishable with a factor of 3-15 times larger X-ray flux for late M stars than for K stars. These results suggest that there may not be a K-dwarf advantage compared to M stars in the UV, but one may still exist in the X-ray.

48. Upsdell, E., Giles, P., Romer, A., Wilkinson, R., Turner, D., Hilton, M., Rykoff, E., Farahi, A., Bhargava, S., Jeltema, T., Klein, M., Bermeo, A., Collins, C., Ebrahimpour, L., Hollowood, D., Mann, R., Manolopoulou, M., Miller, C., Rooney, P., Sahlen, M., Stott, J., Viana, P., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Dietrich, J., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gutierrez, G., Hinton, S., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lima, M., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J., Ogando, R., Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., To, C., Weaverdyck, N., Weller, J., Wiseman, P., 2023, MNRAS, 522, 5267, The XMM cluster survey: exploring scaling relations and completeness of the dark energy survey year 3 redMaPPer cluster catalogue
    Abstract

    We cross-match and compare characteristics of galaxy clusters identified in observations from two sky surveys using two completely different techniques. One sample is optically selected from the analysis of 3 years of Dark Energy Survey observations using the redMaPPer cluster detection algorithm. The second is X-ray selected from XMM observations analysed by the XMM Cluster Survey. The samples comprise a total area of 57.4 deg², bounded by the area of four contiguous XMM survey regions that overlap the DES footprint. We find that the X-ray-selected sample is fully matched with entries in the redMaPPer catalogue, above > 20 and within 0.1 <$z$ <0.9. Conversely, only 38 per cent of the redMaPPer catalogue is matched to an X-ray extended source. Next, using 120 optically clusters and 184 X-ray-selected clusters, we investigate the form of the X-ray luminosity-temperature (L_X -T_X ), luminosity-richness (L_X -), and temperature-richness (T_X -) scaling relations. We find that the fitted forms of the L_X -T_X relations are consistent between the two selection methods and also with other studies in the literature. However, we find tentative evidence for a steepening of the slope of the relation for low richness systems in the X-ray-selected sample. When considering the scaling of richness with X-ray properties, we again find consistency in the relations (i.e. L_X - and T_X -) between the optical and X-ray-selected samples. This is contrary to previous similar works that find a significant increase in the scatter of the luminosity scaling relation for X-ray-selected samples compared to optically selected samples.

49. Yu, Z., Martini, P., Penton, A., Davis, T., Kochanek, C., Lewis, G., Lidman, C., Malik, U., Sharp, R., Tucker, B., Aguena, M., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Diehl, H., Doel, P., Everett, S., Ferrero, I., Garcia-Bellido, J., Gatti, M., Gerdes, D., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Mena-Fernandez, J., Menanteau, F., Miquel, R., Nichol, B., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Raveri, M., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Vincenzi, M., Walker, A., Weaverdyck, N., 2023, MNRAS, 522, 4132, OzDES Reverberation Mapping Programme: Mg II lags and R-L relation
    Abstract

    The correlation between the broad line region radius and continuum luminosity (R-L relation) of active galactic nuclei (AGNs) is critical for single-epoch mass estimates of supermassive black holes (SMBHs). At z ~ 1-2, where AGN activity peaks, the R-L relation is constrained by the reverberation mapping (RM) lags of the Mg II line. We present 25 Mg II lags from the Australian Dark Energy Survey RM project based on 6 yr of monitoring. We define quantitative criteria to select good lag measurements and verify their reliability with simulations based on both the damped random walk stochastic model and the rescaled, resampled versions of the observed light curves of local, well-measured AGN. Our sample significantly increases the number of Mg II lags and extends the R-L relation to higher redshifts and luminosities. The relative iron line strength $\mathcal {R}_{\rm Fe}$ has little impact on the R-L relation. The best-fitting Mg IIR-L relation has a slope = 0.39 0.08 with an intrinsic scatter $\sigma _{\rm rl} = 0.15^{+0.03}_{-0.02}$ . The slope is consistent with previous measurements and shallower than the H R-L relation. The intrinsic scatter of the new R-L relation is substantially smaller than previous studies and comparable to the intrinsic scatter of the H R-L relation. Our new R-L relation will enable more precise single-epoch mass estimates and SMBH demographic studies at cosmic noon.

50. Sidhu, S., Cloutis, E., Mann, P., Applin, D., Hiroi, T., Mengel, K., Kareta, T., Reddy, V., Beck, P., Mertzman, S., 2023, Icar, 398, 115522, Spectral and mineralogical effects of heating on CM chondrite and related asteroids
    Abstract

    Several carbonaceous chondrites (CCs) display evidence of aqueous and thermal alteration. However, the process of thermal alteration is not fully understood. To investigate the spectral variations caused by thermal alteration, we heated powders of CM2 CCs Murchison and Jbilet Winselwan, as well as a simulant Murchison mixture (WMM) and its end members. Heating was conducted up to 1200 C, in 100 C increments under a purified nitrogen environment. We also compared the findings of our study with results of previous heating experiments conducted on CCs to better understand the effect differing conditions have on the spectral properties observed. Formation of Fe³⁺ oxyhydroxides and the decomposition of serpentine due to heating are confirmed by both reflectance and X-ray diffraction (XRD) data. Fe³⁺ oxyhydroxides features such as a steep slope in between 350 to 700 nm, and an 850 nm feature can be seen starting at 300 and 400 C, respectively. The serpentine-associated features start to decompose at 700 C and disappear by 900 C. Spectra >1000 C are generally dark and featureless and above this temperature, mafic silicate absorption bands begin to appear. Our results show that heating-induced spectral variations are evident, and the nature of these changes depends on various parameters including temperature, experimental conditions, duration of heating, sample grain size, as well as mineralogical changes accompanying heating, and heterogeneity between CCs.

51. Bernstein, G., Holler, B., Navarro-Escamilla, R., Bernardinelli, P., Abbott, T., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Brooks, D., Burke, D., Carnero Rosell, A., Carretero, J., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Doel, P., Drlica-Wagner, A., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruen, D., Gutierrez, G., Herner, K., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Marshall, J., Mena-Fernandez, J., Miquel, R., Ogando, R., Pieres, A., Plazas Malagon, A., Raveri, M., Reil, K., Sanchez, E., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Wiseman, P., DES Collaboration, 2023, PSJ, 4, 115, Synchronous Rotation in the (136199) Eris-Dysnomia System
    Abstract

    We combine photometry of Eris from a 6 month campaign on the Palomar 60 inch telescope in 2015, a 1 month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013-2018 to determine a light curve of definitive period 15.771 0.008 days (1 formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3%. This is consistent at part-per-thousand precision with the P = 15.785 90 0.00005 day sidereal period of Dysnomia's orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakats et al. with independent data. Photometry from Gaia are consistent with the same light curve. We detect a slope of 0.05 0.01 mag per degree of Eris's brightness with respect to illumination phase averaged across g, V, and r bands, intermediate between Pluto's and Charon's values. Variations of 0.3 mag are detected in Dysnomia's brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. The high albedo contrast between Eris and Dysnomia remains unexplained in the giant-impact scenario.

52. Standing, M., Sairam, L., Martin, D., Triaud, A., Correia, A., Coleman, G., Baycroft, T., Kunovac, V., Boisse, I., Cameron, A., Dransfield, G., Faria, J., Gillon, M., Hara, N., Hellier, C., Howard, J., Lane, E., Mardling, R., Maxted, P., Miller, N., Nelson, R., Orosz, J., Pepe, F., Santerne, A., Sebastian, D., Udry, S., Welsh, W., 2023, NatAs, 7, 702, Radial-velocity discovery of a second planet in the TOI-1338/BEBOP-1 circumbinary system
    Abstract

    Circumbinary planets, those that orbit around both stars of a central binary star system, challenge our understanding of planet formation. With only 12 binary systems known to host circumbinary planets, identifying more of these planets, along with their physical properties, could help to discern some of the physical processes that govern planet formation. Here we analyse radial-velocity data obtained by the HARPS and ESPRESSO spectrographs and report the detection of BEBOP-1 c, a gas giant planet with a mass of 65.2 11.8 Earth masses (M) orbiting around both stars of an eclipsing binary star system with a period of 215.5 3.3 days. The system TOI-1338, hereafter referred to as BEBOP-1, which also hosts the smaller and inner transiting planet TOI-1338 b, is only the second confirmed multiplanetary circumbinary system. We do not detect TOI-1338 b with radial-velocity data alone, and we can place an upper limit on its mass of 21.8 M with 99% confidence. TOI-1338 b is amenable to atmospheric characterization using JWST, so the BEBOP-1 system has the potential to act as a benchmark for circumbinary exo-atmospheric studies.

53. Tang, S., Stahl, A., Prato, L., Schaefer, G., Johns-Krull, C., Skiff, B., Beichman, C., Uyama, T., 2023, ApJ, 950, 92, Star-crossed Lovers DI Tau A and B: Orbit Characterization and Physical Properties Determination
    Abstract

    The stellar companion to the weak-line T Tauri star DI Tau A was first discovered by the lunar occultation technique in 1989 and was subsequently confirmed by a speckle imaging observation in 1991. It has not been detected since, despite being targeted by five different studies that used a variety of methods and spanned more than 20 yr. Here, we report the serendipitous rediscovery of DI Tau B during our Young Exoplanets Spectroscopic Survey (YESS). Using radial velocity data from YESS spanning 17 yr, new adaptive optics observations from Keck II, and a variety of other data from the literature, we derive a preliminary orbital solution for the system that effectively explains the detection and (almost all of the) non-detection history of DI Tau B. We estimate the dynamical masses of both components, finding that the large mass difference (q ~ 0.17) and long orbital period (35 yr) make the DI Tau system a noteworthy and valuable addition to studies of stellar evolution and pre-main-sequence models. With a long orbital period and a small flux ratio (f2/f1) between DI Tau A and B, additional measurements are needed for a better comparison between these observational results and pre-main-sequence models. Finally, we report an average surface magnetic field strength ( $\bar{B}$ ) for DI Tau A, of ~0.55 kG, which is unusually low in the context of young active stars.

54. Shipp, N., Panithanpaisal, N., Necib, L., Sanderson, R., Erkal, D., Li, T., Santistevan, I., Wetzel, A., Cullinane, L., Ji, A., Koposov, S., Kuehn, K., Lewis, G., Pace, A., Zucker, D., Bland-Hawthorn, J., Cunningham, E., Kim, S., Lilleengen, S., Moreno, J., Sharma, S., S Collaboration, FIRE Collaboration, 2023, ApJ, 949, 44, Streams on FIRE: Populations of Detectable Stellar Streams in the Milky Way and FIRE
    Abstract

    We present the first detailed comparison of populations of dwarf galaxy stellar streams in cosmological simulations and the Milky Way. In particular, we compare streams identified around 13 Milky Way analogs in the FIRE-2 simulations to streams observed by the Southern Stellar Stream Spectroscopic Survey (S ⁵). For an accurate comparison, we produce mock Dark Energy Survey (DES) observations of the FIRE streams and estimate the detectability of their tidal tails and progenitors. The number and stellar mass distributions of detectable stellar streams is consistent between observations and simulations. However, there are discrepancies in the distributions of pericenters and apocenters, with the detectable FIRE streams, on average, forming at larger pericenters (out to >110 kpc) and surviving only at larger apocenters (40 kpc) than those observed in the Milky Way. We find that the population of high-stellar-mass dwarf galaxy streams in the Milky Way is incomplete. Interestingly, a large fraction of the FIRE streams would only be detected as intact satellites in DES-like observations, since their tidal tails have too low surface brightness to be detectable. We thus predict a population of yet-undetected tidal tails around Milky Way satellites, as well as a population of fully undetected low-surface-brightness stellar streams, and estimate their detectability with the Rubin Observatory. Finally, we discuss the causes and implications of the discrepancies between the stream populations in FIRE and the Milky Way, and explore future avenues for tests of satellite disruption in cosmological simulations.

55. Schwamb, M., Jones, R., Yoachim, P., Volk, K., Dorsey, R., Opitom, C., Greenstreet, S., Lister, T., Snodgrass, C., Bolin, B., Inno, L., Bannister, M., Eggl, S., Solontoi, M., Kelley, M., Juric, M., Lin, H., Ragozzine, D., Bernardinelli, P., Chesley, S., Daylan, T., Durech, J., Fraser, W., Granvik, M., Knight, M., Lisse, C., Malhotra, R., Oldroyd, W., Thirouin, A., Ye, Q., 2023, ApJS, 266, 22, Tuning the Legacy Survey of Space and Time (LSST) Observing Strategy for Solar System Science
    Abstract

    The Vera C. Rubin Observatory is expected to start the Legacy Survey of Space and Time (LSST) in early to mid-2025. This multiband wide-field synoptic survey will transform our view of the solar system, with the discovery and monitoring of over five million small bodies. The final survey strategy chosen for LSST has direct implications on the discoverability and characterization of solar system minor planets and passing interstellar objects. Creating an inventory of the solar system is one of the four main LSST science drivers. The LSST observing cadence is a complex optimization problem that must balance the priorities and needs of all the key LSST science areas. To design the best LSST survey strategy, a series of operation simulations using the Rubin Observatory scheduler have been generated to explore the various options for tuning observing parameters and prioritizations. We explore the impact of the various simulated LSST observing strategies on studying the solar system's small body reservoirs. We examine what are the best observing scenarios and review what are the important considerations for maximizing LSST solar system science. In general, most of the LSST cadence simulations produce 5% or less variations in our chosen key metrics, but a subset of the simulations significantly hinder science returns with much larger losses in the discovery and light-curve metrics.

56. Lee, J., Acevedo, M., Sako, M., Vincenzi, M., Brout, D., Sanchez, B., Chen, R., Davis, T., Jarvis, M., Scolnic, D., Qu, H., Galbany, L., Kessler, R., Lasker, J., Sullivan, M., Wiseman, P., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kent, S., Kuehn, K., Kuropatkin, N., Mena-Fernandez, J., Miquel, R., Ogando, R., Palmese, A., Pieres, A., Malagon, A., Raveri, M., Reil, K., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., DES Collaboration, 2023, AJ, 165, 222, The Dark Energy Survey Supernova Program: Corrections on Photometry Due to Wavelength-dependent Atmospheric Effects
    Abstract

    Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program's 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters w and _m . We use g - i colors of Type Ia supernovae to quantify astrometric offsets caused by DCR and simulate point-spread functions (PSFs) using the GalSIM package to predict the shapes of the PSFs with DCR and wavelength-dependent seeing. We calculate the magnitude corrections and apply them to the magnitudes computed by the DES-SN5YR photometric pipeline. We find that for the DES-SN5YR analysis, not accounting for the astrometric offsets and changes in the PSF shape cause an average bias of +0.2 mmag and -0.3 mmag, respectively, with standard deviations of 0.7 mmag and 2.7 mmag across all DES observing bands (griz) throughout all redshifts. When the DCR and seeing effects are not accounted for, we find that w and _m are lower by less than 0.004 0.02 and 0.001 0.01, respectively, with 0.02 and 0.01 being the 1 statistical uncertainties. Although we find that these biases do not limit the constraints of the DES-SN5YR sample, future surveys with much higher statistics, lower systematics, and especially those that observe in the u band will require these corrections as wavelength-dependent atmospheric effects are larger at shorter wavelengths. We also discuss limitations of our method and how they can be better accounted for in future surveys.

57. Sanchez, J., Omori, Y., Chang, C., Bleem, L., Crawford, T., Drlica-Wagner, A., Raghunathan, S., Zacharegkas, G., Abbott, T., Aguena, M., Alarcon, A., Allam, S., Alves, O., Amon, A., Avila, S., Baxter, E., Bechtol, K., Benson, B., Bernstein, G., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Campos, A., Carlstrom, J., Rosell, A., Kind, M., Carretero, J., Castander, F., Cawthon, R., Chang, C., Chen, A., Choi, A., Chown, R., Costanzi, M., Crites, A., Crocce, M., da Costa, L., Pereira, M., de Haan, T., De Vicente, J., DeRose, J., Desai, S., Diehl, H., Dobbs, M., Dodelson, S., Doel, P., Elvin-Poole, J., Everett, W., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gatti, M., George, E., Gerdes, D., Giannini, G., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Halverson, N., Hinton, S., Holder, G., Hollowood, D., Holzapfel, W., Honscheid, K., Hrubes, J., James, D., Knox, L., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A., Luong-Van, D., MacCrann, N., Marshall, J., McCullough, J., McMahon, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mocanu, L., Mohr, J., Muir, J., Myles, J., Natoli, T., Padin, S., Palmese, A., Pandey, S., Paz-Chinchon, F., Pieres, A., Malagon, A., Porredon, A., Pryke, C., Raveri, M., Reichardt, C., Rodriguez-Monroy, M., Ross, A., Ruhl, J., Rykoff, E., Sanchez, C., Sanchez, E., Scarpine, V., Schaffer, K., Sevilla-Noarbe, I., Sheldon, E., Shirokoff, E., Smith, M., Soares-Santos, M., Staniszewski, Z., Stark, A., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., Troxel, M., Tucker, D., Vieira, J., Vincenzi, M., Weaverdyck, N., Williamson, R., Yanny, B., Yin, B., DES Collaboration, SPT Collaboration, 2023, MNRAS, 522, 3163, Mapping gas around massive galaxies: cross-correlation of DES Y3 galaxies and Compton-y maps from SPT and Planck
    Abstract

    We cross-correlate positions of galaxies measured in data from the first three years of the Dark Energy Survey with Compton-y maps generated using data from the South Pole Telescope (SPT) and the Planck mission. We model this cross-correlation measurement together with the galaxy autocorrelation to constrain the distribution of gas in the Universe. We measure the hydrostatic mass bias or, equivalently, the mean halo bias-weighted electron pressure <b_hP_e >, using large-scale information. We find <b_hP_e > to be $[0.16^{+0.03}_{-0.04},0.28^{+0.04}_{-0.05},0.45^{+0.06}_{-0.10},0.54^{+0.08}_{-0.07},0.61^{+0.08}_{-0.06},0.63^{+0.07}_{-0.08}]$ meV cm^-3 at redshifts z ~ [0.30, 0.46, 0.62, 0.77, 0.89, 0.97]. These values are consistent with previous work where measurements exist in the redshift range. We also constrain the mean gas profile using small-scale information, enabled by the high-resolution of the SPT data. We compare our measurements to different parametrized profiles based on the cosmo-OWLS hydrodynamical simulations. We find that our data are consistent with the simulation that assumes an AGN heating temperature of 10^8.5 K but are incompatible with the model that assumes an AGN heating temperature of 10^8.0 K. These comparisons indicate that the data prefer a higher value of electron pressure than the simulations within r_500c of the galaxies' haloes.

58. dal Ponte, M., Santiago, B., Carnero Rosell, A., De Paris, L., Pace, A., Bechtol, K., Abbott, T., Aguena, M., Allam, S., Alves, O., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., Desai, S., De Vicente, J., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruendl, R., Gruen, D., Gutierrez, G., Hinton, S., Hollowood, D., James, D., Kuehn, K., Kuropatkin, N., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Pereira, M., Plazas Malagon, A., Pieres, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Weaverdyck, N., DES Collaboration, 2023, MNRAS, 522, 1951, Ultracool dwarfs candidates based on 6 yr of the Dark Energy Survey data
    Abstract

    We present a sample of 19 583 ultracool dwarf candidates brighter than z 23 selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5, and AllWISE covering ~ 480 deg². The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared, and mid-infrared colours against templates of M, L, and T dwarfs. 14 099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of 12 new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method.

59. Oszkiewicz, D., Troianskyi, V., Galad, A., Hanus, J., Durech, J., Wilawer, E., Marciniak, A., Kwiatkowski, T., Kolenczuk, P., Skiff, B., Polakis, T., Moskovitz, N., Geier, S., Fohring, D., Hung, D., Gajdos, S., Vilagi, J., Polcic, L., Kashuba, V., Udovichenko, S., Keir, L., Benishek, V., Pray, D., Shevchenko, V., Krugly, Y., Kankiewicz, P., Hasegawa, S., Behrend, R., Bernasconi, L., Leroy, A., Roy, R., Ivanova, O., Husarik, M., Simon, A., 2023, Icar, 397, 115520, Spins and shapes of basaltic asteroids and the missing mantle problem
    Abstract

    Basaltic V-type asteroids are common in the inner part of the Main Asteroid Belt and much less abundant in the mid and outer parts. They are of scientific interest because they sample crusts and mantles of theoretically plentiful differentiated planetesimals that existed in the Solar System four billion years ago. Some Solar System theories suggest that those objects formed in the terrestrial planet region and were then implanted in the main asteroid belt. In consequence, we should observe a large number of fragments of multiple differentiated planetesimals in the inner Main Belt. That region of the Asteroid Belt is filled with V-type fragments; however, they are difficult to tell apart from typical Vestoids and Vesta fugitives. In this work, we focus on physical and dynamical characterization of V-types in the inner Main-Belt and aim to reconcile those properties with the planetesimal formation and evolution theories.

    We conducted an observing campaign over the years 2013-2022 and obtained photometric observations of V-type asteroids located mostly outside the Vesta family at specific locations of the inner Main Belt (the so-called Cells I and II). The total number of partial dense photometric lightcurves obtained in this study was 2910. We were able to model 100 V-types. We further supplement those data with 133 spins of V-types from the DAMIT database and 237 objects derived from Gaia DR3 (Durech & Hanus 2023). We found 78% 11% and 38% 13% retrograde rotators in Cell I and II, respectively. This statistic is remarkably consistent with the numerical simulations of the escape paths of Vesta fugitives that predict 81% retrograde rotators in Cell I and 40% in Cell II after the dynamical integration of 2 Gys. Based on our statistics we conclude that if there are non-Vestoids in the inner main belt, they are likely to be very few. This is consistent with the small fraction of anomalous HED meteorites in meteorite collections, small number of non-Vestoids in the middle and outer Main Belt and points to planetesimal formation location close to the Sun.

60. Duck, A., Martin, D., Gill, S., Armitage, T., Rodriguez Martinez, R., Maxted, P., Sebastian, D., Sethi, R., Swayne, M., Cameron, A., Dransfield, G., Gaudi, B., Gillon, M., Hellier, C., Kunovac, V., Lovis, C., McCormac, J., Pepe, F., Pollacco, D., Sairam, L., Santerne, A., Segransan, D., Standing, M., Southworth, J., Triaud, A., Udry, S., 2023, MNRAS, 521, 6305, The EBLM project X. Benchmark masses, radii, and temperatures for two fully convective M-dwarfs using K2
    Abstract

    M-dwarfs are the most abundant stars in the galaxy and popular targets for exoplanet searches. However, their intrinsic faintness and complex spectra inhibit precise characterization. We only know of dozens of M-dwarfs with fundamental parameters of mass, radius, and effective temperature characterized to better than a few per cent. Eclipsing binaries remain the most robust means of stellar characterization. Here we present two targets from the Eclipsing Binary Low Mass (EBLM) survey that were observed with K2: EBLM J0055-00 and EBLM J2217-04. Combined with HARPS and CORALIE spectroscopy, we measure M-dwarf masses with precisions better than 5 per cent, radii better than 3 per cent, and effective temperatures on order 1 per cent. However, our fits require invoking a model to derive parameters for the primary star and fitting the M-dwarf using the transit and radial velocity observations. By investigating three popular stellar models, we determine that the model uncertainty in the primary star is of similar magnitude to the statistical uncertainty in the model fits of the secondary M-dwarf. Therefore, whilst these can be considered benchmark M-dwarfs, we caution the community to consider model uncertainty when pushing the limits of precise stellar characterization.

61. Koposov, S., Erkal, D., Li, T., Da Costa, G., Cullinane, L., Ji, A., Kuehn, K., Lewis, G., Pace, A., Shipp, N., Zucker, D., Bland-Hawthorn, J., Lilleengen, S., Martell, S., S5 Collaboration, 2023, MNRAS, 521, 4936, S ⁵: Probing the Milky Way and Magellanic Clouds potentials with the 6D map of the Orphan-Chenab stream
    Abstract

    We present a 6D map of the Orphan-Chenab (OC) stream by combining the data from Southern Stellar Stream Spectroscopic Survey (S⁵) and Gaia. We reconstruct the proper motion, radial velocity, distance, on-sky track, and stellar density along the stream with spline models. The stream has a total luminosity of M_V = -8.2 and metallicity of [Fe/H] = -1.9, similar to classical Milky Way (MW) satellites like Draco. The stream shows drastic changes in its physical width varying from 200 pc to 1 kpc, but a constant line-of-sight velocity dispersion of 5 $\mathrm{km\, s^{-1}}$. Despite the large apparent variation in the stellar number density along the stream, the flow rate of stars along the stream is remarkably constant. We model the 6D stream track by a Lagrange-point stripping method with a flexible MW potential in the presence of a moving extended Large Magellanic Cloud (LMC). This allows us to constrain the mass profile of the MW within the distance range 15.6 < r < 55.5 kpc, with the best measured enclosed mass of $(2.85\pm 0.1)\times 10^{11}\, \mathrm{\, M_\odot }$ within 32.4 kpc. Our stream measurements are highly sensitive to the LMC mass profile with the most precise measurement of its enclosed mass made at 32.8 kpc, $(7.02\pm 0.9)\times 10^{10}\, {\rm M}_\odot$. We also detect that the LMC dark matter halo extends to at least 53 kpc. The fitting of the OC stream allows us to constrain the past LMC trajectory and the degree of dynamical friction it experienced. We demonstrate that the stars in the OC stream show large energy and angular momentum spreads caused by LMC perturbation.

62. French, R., McGhee-French, C., Gordon, M., Baron, R., Bosh, A., Buie, M., Chanover, N., Clark, M., Dunham, E., French, L., Glass, I., Goguen, J., Gregory, B., Hock, R., Kangas, J., Levine, S., Matthews, K., McMason, E., Meech, K., Mink, J., Nicholson, P., Person, M., Roques, F., Sicardy, B., Stecklum, B., Tholen, D., Young, E., Young, L., 2023, Icar, 395, 115474, Uranus ring occultation observations: 1977-2006
    Abstract

    The Uranian rings were discovered serendipitously on 10 March 1977 during a stellar occultation (Elliot et al., 1977a; Millis et al., 1977), and a rich set of subsequent Earth-based occultations revealed that these narrow and sharp-edged rings were eccentric and inclined, precessing under the gravitational influence of the oblate central planet. Considerable progress has been made in understanding the observed characteristics of narrow rings and sharp edges (Nicholson et al., 2018) and their associated dynamics (Longaretti, 2018), but ever since their discovery, the Uranian rings have posed dynamical puzzles that resist simple explanations. The observational basis to address these questions for the Uranus system rests largely on occultation measurements of the narrow rings spanning nearly 30 years, beginning in 1977 and concluding most recently in 2006. Nearly all of these occultation data sets are available in digital form on NASA's Planetary Data System (PDS) Ring-Moon Systems node, but many of them have not been previously published or described in detail. This paper serves as a guide to the PDS archive and provides essential information about the observations and the methods used to determine the ring widths, mean optical depths, and occultation event times from individual occultation profiles. Additional detail is provided in the Supplementary Online Material accompanying this publication. In a companion paper (French et al., 2023b), we make use of these observations to determine the Uranus ring orbits, pole direction, and gravity field, and the orbital characteristics and masses of three small Uranian moons - Cressida, Ophelia, and Cordelia - from their forced normal modes on the rings.

63. Trujillo, C., Chandler, C., Oldroyd, W., Burris, W., Hsieh, H., Kueny, J., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 106, Cometary Activity on Quasi-Hilda Object 2018 CZ16
    Abstract

    We present the discovery of activity originating from quasi-Hilda Object 2018 CZ₁₆, a finding stemming from the Citizen Science project Active Asteroids. For 2018 CZ₁₆ we identified a broad (~60) but short (~5) tail in archival Blanco 4 m data from Cerro Tololo Inter-American Observatory, Chile, (CTIO) Dark Energy Camera images from UT 2018 May 15, 17 and 18. Activity occurred 2 months prior to perihelion, consistent with sublimation-driven activity.

64. Windsor, J., Robinson, T., Kopparapu, R., Young, A., Trilling, D., LLama, J., 2023, PSJ, 4, 94, A Radiative-convective Model for Terrestrial Planets with Self-consistent Patchy Clouds
    Abstract

    Clouds are ubiquitous: they arise for every solar system planet that possesses an atmosphere and have also been suggested as a leading mechanism for obscuring spectral features in exoplanet observations. As exoplanet observations continue to improve, there is a need for efficient and general planetary climate models that appropriately handle the possible cloudy atmospheric environments that arise on these worlds. We generate a new 1D radiative-convective terrestrial planet climate model that self-consistently handles patchy clouds through a parameterized microphysical treatment of condensation and sedimentation processes. Our model is general enough to recreate Earth's atmospheric radiative environment without overparameterization, while also maintaining a simple implementation that is applicable to a wide range of atmospheric compositions and physical planetary properties. We first validate this new 1D patchy-cloud radiative-convective climate model by comparing it to Earth thermal structure data and to existing climate and radiative-transfer tools. We produce partially clouded Earth-like climates with cloud structures that are representative of deep tropospheric convection and are adequate 1D representations of clouds within rocky planet atmospheres. After validation against Earth, we then use our partially clouded climate model and explore the potential climates of super-Earth exoplanets with secondary nitrogen-dominated atmospheres which we assume are abiotic. We also couple the partially clouded climate model to a full-physics, line-by-line radiative-transfer model and generate high-resolution spectra of simulated climates. These self-consistent climate-to-spectral models bridge the gap between climate modeling efforts and observational studies of rocky worlds.

65. Chandler, C., Oldroyd, W., Hsieh, H., Trujillo, C., Burris, W., Kueny, J., DeSpain, J., Farrell, K., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 102, New Active Asteroid (588045) 2007 FZ18
    Abstract

    We present evidence that, on UT 2018 February 15, main-belt asteroid (588045) 2007 FZ₁₈ displayed cometary activity in the form of two tails, one each in the anti-solar and anti-motion directions. Activity was first identified by volunteers of the NASA Partner program Active Asteroids, a Citizen Science program hosted on the Zooniverse platform, in an image acquired with the Dark Energy Camera on the Blanco 4 m telescope at the Cerro Tololo Inter-American Observatory in Chile. Notably, (588045) 2007 FZ₁₈ is inbound toward perihelion, so telescope observations are timely to detect a possible second activity outburst.

66. Long, J., Males, J., Haffert, S., Pearce, L., Marley, M., Morzinski, K., Close, L., Otten, G., Snik, F., Kenworthy, M., Keller, C., Hinz, P., Monnier, J., Weinberger, A., Tolls, V., 2023, AJ, 165, 216, Improved Companion Mass Limits for Sirius A with Thermal Infrared Coronagraphy Using a Vector-apodizing Phase Plate and Time-domain Starlight-subtraction Techniques
    Abstract

    We use observations with the infrared-optimized Magellan Adaptive Optics (MagAO) system and Clio camera in 3.9 m light to place stringent mass constraints on possible undetected companions to Sirius A. We suppress the light from Sirius A by imaging it through a grating vector-apodizing phase plate coronagraph with a 180 dark region (gvAPP-180). To remove residual starlight in postprocessing, we apply a time-domain principal-components-analysis-based algorithm we call PCA-Temporal, which uses eigen time series rather than eigenimages to subtract starlight. By casting the problem in terms of eigen time series, we reduce the computational cost of postprocessing the data, enabling the use of the fully sampled data set for improved contrast at small separations. We also discuss the impact of retaining fine temporal sampling of the data on final contrast limits. We achieve postprocessed contrast limits of 1.5 10^-6-9.8 10^-6 outside of 0.75, which correspond to planet masses of 2.6-8.0 M _J. These are combined with values from the recent literature of high-contrast imaging observations of Sirius to synthesize an overall completeness fraction as a function of mass and separation. After synthesizing these recent studies and our results, the final completeness analysis rules out 99% of 9 M _J planets from 2.5 to 7 au.

67. Kareta, T., Noonan, J., Harris, W., Springmann, A., 2023, PSJ, 4, 85, Ice, Ice, Maybe? Investigating 46P/Wirtanen's Inner Coma for Icy Grains
    Abstract

    The release of volatiles from comets is usually from direct sublimation of ices on the nucleus, but for very or hyperactive comets other sources have to be considered to account for the total production rates. In this work, we present new near-IR (NIR) imaging and spectroscopic observations of 46P/Wirtanen taken during its close approach to Earth on 2018 December 19 with the MMIRS instrument at the MMT Observatory to search for signatures of icy or ice-rich grains in its inner coma that might explain its previously reported excess water production. The morphology of the images does not suggest any change in grain properties within the field of view, and the NIR spectra do not show the characteristic absorption features of water ice. Using a new Markov Chain Monte Carlo-based implementation of the spectral modeling approach of Protopapa et al., we estimate the areal water ice fraction of the coma to be <0.6%. When combined with slit-corrected Af values for the J, H, and K bands and previously measured dust velocities for this comet, we estimate an icy grain production rate of less than 4.6 kg s^-1. This places a strict constraint on the water production rate from pure icy grains in the coma, and in turn we find that for the 2018-2019 apparition approximately 64% of 46P's surface was actively sublimating water near perihelion. We then discuss 46P's modern properties within the context of other (formerly) hyperactive comets to understand how these complex objects evolve.

68. Graham, K., O'Donnell, J., Silverstein, M., Eiger, O., Jeltema, T., Hollowood, D., Cross, D., Everett, S., Giles, P., Jobel, J., Laubner, D., McDaniel, A., Romer, A., Swart, A., Aguena, M., Allam, S., Alves, O., Brooks, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Dietrich, J., Doel, P., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gruen, D., Gruendl, R., Hinton, S., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Marshall, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Palmese, A., Pieres, A., Malagon, A., Reil, K., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., To, C., Weaverdyck, N., DES Collaboration, 2023, RNAAS, 7, 86, Cool Cores in Clusters of Galaxies in the Dark Energy Survey
    Abstract

    We search for the presence of cool cores in optically selected galaxy clusters from the Dark Energy Survey (DES) and investigate their prevalence as a function of redshift and cluster richness. Clusters were selected from the redMaPPer analysis of three years of DES observations that have archival Chandra X-ray observations, giving a sample of 99 clusters with a redshift range of 0.11 < z < 0.87 and a richness range of 25 < < 207. Using the X-ray data, the core temperature was compared to the outer temperature to identify clusters where the core temperature is a factor of 0.7 or less than the outer temperature. We found a cool core fraction of approximately 20% with no significant trend in the cool core fraction with either redshift or richness.

69. Lemos, P., Weaverdyck, N., Rollins, R., Muir, J., Ferte, A., Liddle, A., Campos, A., Huterer, D., Raveri, M., Zuntz, J., Di Valentino, E., Fang, X., Hartley, W., Aguena, M., Allam, S., Annis, J., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Choi, A., Costanzi, M., Crocce, M., da Costa, L., Pereira, M., Dietrich, J., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lima, M., March, M., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A., Porredon, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Varga, T., Weller, J., DES Collaboration, 2023, MNRAS, 521, 1184, Robust sampling for weak lensing and clustering analyses with the Dark Energy Survey
    Abstract

    Recent cosmological analyses rely on the ability to accurately sample from high-dimensional posterior distributions. A variety of algorithms have been applied in the field, but justification of the particular sampler choice and settings is often lacking. Here, we investigate three such samplers to motivate and validate the algorithm and settings used for the Dark Energy Survey (DES) analyses of the first 3 yr (Y3) of data from combined measurements of weak lensing and galaxy clustering. We employ the full DES Year 1 likelihood alongside a much faster approximate likelihood, which enables us to assess the outcomes from each sampler choice and demonstrate the robustness of our full results. We find that the ellipsoidal nested sampling algorithm MULTINEST reports inconsistent estimates of the Bayesian evidence and somewhat narrower parameter credible intervals than the sliced nested sampling implemented in POLYCHORD. We compare the findings from MULTINEST and POLYCHORD with parameter inference from the Metropolis-Hastings algorithm, finding good agreement. We determine that POLYCHORD provides a good balance of speed and robustness for posterior and evidence estimation, and recommend different settings for testing purposes and final chains for analyses with DES Y3 data. Our methodology can readily be reproduced to obtain suitable sampler settings for future surveys.

70. Golden-Marx, J., Zhang, Y., Ogando, R., Allam, S., Tucker, D., Miller, C., Hilton, M., Mutlu-Pakdil, B., Abbott, T., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Castander, F., Conselice, C., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruen, D., Gruendl, R., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Marshall, J., Melchior, P., Mena-Fernandez, J., Miquel, R., Mohr, J., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Sifon, C., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Vincenzi, M., Weaverdyck, N., Yanny, B., DES Collaboration, 2023, MNRAS, 521, 478, Characterizing the intracluster light over the redshift range 0.2 < z < 0.8 in the DES-ACT overlap
    Abstract

    We characterize the properties and evolution of bright central galaxies (BCGs) and the surrounding intracluster light (ICL) in galaxy clusters identified in the Dark Energy Survey and Atacama Cosmology Telescope Survey (DES-ACT) overlapping regions, covering the redshift range 0.20 < z < 0.80. Over this redshift range, we measure no change in the ICL's stellar content (between 50 and 300 kpc) in clusters with log₁₀(M_200m,SZ/M) >14.4. We also measure the stellar mass-halo mass (SMHM) relation for the BCG+ICL system and find that the slope, , which characterizes the dependence of M_200m,SZ on the BCG+ICL stellar mass, increases with radius. The outskirts are more strongly correlated with the halo than the core, which supports that the BCG+ICL system follows a two-phase growth, where recent growth (z < 2) occurs beyond the BCG's core. Additionally, we compare our observed SMHM relation results to the IllustrisTNG300-1 cosmological hydrodynamic simulations and find moderate qualitative agreement in the amount of diffuse light. However, the SMHM relation's slope is steeper in TNG300-1 and the intrinsic scatter is lower, likely from the absence of projection effects in TNG300-1. Additionally, we find that the ICL exhibits a colour gradient such that the outskirts are bluer than the core. Moreover, for the lower halo mass clusters (log₁₀(M_200m,SZ/M) < 14.59), we detect a modest change in the colour gradient's slope with lookback time, which combined with the absence of stellar mass growth may suggest that lower mass clusters have been involved in growth via tidal stripping more recently than their higher mass counterparts.

71. Stone, Z., Shen, Y., Burke, C., Chen, Y., Yang, Q., Liu, X., Gruendl, R., Adamow, M., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Doel, P., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lidman, C., Maia, M., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Serrano, S., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., To, C., DES Collaboration, 2023, MNRAS, 521, 836, Correction to: Optical variability of quasars with 20-year photometric light curves
    Abstract

    No abstract found.

72. Quirico, E., Bacmann, A., Wolters, C., Auge, B., Flandinet, L., Launois, T., Cooper, J., Vuitton, V., Gautier, T., Jovanovic, L., Boduch, P., Rothard, H., Desage, L., Faure, A., Schmitt, B., Poch, O., Grundy, W., Protopapa, S., Fornasier, S., Cruikshank, D., Stern, S., New Horizons Team, 2023, Icar, 394, 115396, On a radiolytic origin of red organics at the surface of the Arrokoth Trans-Neptunian Object
    Abstract

    The classical Kuiper Belt Object (KBO) Arrokoth was surveyed by the New Horizons spacecraft on 1st January 2019, revealing a small bilobed object with a red surface, whose spectral slope lies in the average of the whole KBOs population. This red color has been assigned to reddish organic materials, either inherited from the protosolar disk during accretion, or formed through radiolytic processes in the surface due to exposure to solar or interstellar photons, Solar Wind, Solar Energetic Particles or Galactic Cosmic Rays. We report here a study investigating the radiolytic scenario, based on numerical calculations and experimental simulations run with swift heavy ions (74.8 MeV ¹³⁶Xe19⁺ and 33.06 MeV ⁵⁸Ni9⁺), and low-energy 105 keV ¹⁸O6⁺ ions on CH₃OH ice, the only molecule identified at Arrokoth's surface. Calculations show that sputtering is essentially controlled by Solar Wind (H and He), and that the sputtering rate depends on the nature of the material: erosion thickness over 4.55 Gyr are a few micrometers for amorphous carbon (as an analog of red organics) and a 240 m to around 10 mm for H₂O and CO ice, respectively. Chemistry within the subsurface is essentially controlled by Galactic Cosmic rays (H and He), which penetrate deep down to several tens of meters and deliver an electronic dose higher than 1 eV.atom^-1 in the first meter. The electronic and elastic doses delivered by Solar Wind ions are limited to the first 10s nm of the top surface, but Solar Energetic Particles deliver high electronic doses in the first 100 m of the surface (up to 200 eV.atom^-1). Experimental simulations show that irradiating methanol ice with a dose consistent with that in planetary conditions, results in the formation of reddish organic materials made of aliphatic, conjugated and unconjugated olefinic, acetylinic, carbonyl and hydroxyl groups. A similarity with irradiated simple polymers (e.g. polyethyleneglycol) and materials formed through cold plasma experiments (tholins) is observed. There is little dependence with the nature and energy of the ion. The residue recovered at room temperature was analyzed with High Resolution Mass Spectrometry (Orbitrap), revealing a complex composition with around 6596 chemical formulas and likely several tens of thousands of molecules. Altogether, these analyses support active polymerization mechanisms similar to those observed in irradiated polymers, as bond-breaking, cross-linking or formation of olefinic bonds through recombination of radicals in adjacent carbon atoms. Considering both sputtering and radiolysis, as well as material ablation due to dust bombardment reported in literature, a scenario is taking shape as the production of reddish organics deep in the subsurface, and the settling of an organic crust at the top surface through volatiles removal. The presence of methanol and absence of water, inconsistent with sputtering fractionation, remains unexplained.

73. Malik, U., Sharp, R., Penton, A., Yu, Z., Martini, P., Lidman, C., Tucker, B., Davis, T., Lewis, G., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Asorey, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruen, D., Gruendl, R., Gschwend, J., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M., Tarle, G., Taylor, G., Tucker, D., Weaverdyck, N., Wilkinson, R., 2023, MNRAS, 520, 2009, OzDES Reverberation Mapping Program: H lags from the 6-yr survey
    Abstract

    Reverberation mapping measurements have been used to constrain the relationship between the size of the broad-line region and luminosity of active galactic nuclei (AGN). This R-L relation is used to estimate single-epoch virial black hole masses, and has been proposed to use to standardize AGN to determine cosmological distances. We present reverberation measurements made with H from the 6-yr Australian Dark Energy Survey (OzDES) Reverberation Mapping Program. We successfully recover reverberation lags for eight AGN at 0.12 < z < 0.71, probing higher redshifts than the bulk of H measurements made to date. Our fit to the R-L relation has a slope of = 0.41 0.03 and an intrinsic scatter of = 0.23 0.02 dex. The results from our multi-object spectroscopic survey are consistent with previous measurements made by dedicated source-by-source campaigns, and with the observed dependence on accretion rate. Future surveys, including LSST, TiDES, and SDSS-V, which will be revisiting some of our observed fields, will be able to build on the results of our first-generation multi-object reverberation mapping survey.

74. Daly, R., Ernst, C., Barnouin, O., Chabot, N., Rivkin, A., Cheng, A., Adams, E., Agrusa, H., Abel, E., Alford, A., Asphaug, E., Atchison, J., Badger, A., Baki, P., Ballouz, R., Bekker, D., Bellerose, J., Bhaskaran, S., Buratti, B., Cambioni, S., Chen, M., Chesley, S., Chiu, G., Collins, G., Cox, M., DeCoster, M., Ericksen, P., Espiritu, R., Faber, A., Farnham, T., Ferrari, F., Fletcher, Z., Gaskell, R., Graninger, D., Haque, M., Harrington-Duff, P., Hefter, S., Herreros, I., Hirabayashi, M., Huang, P., Hsieh, S., Jacobson, S., Jenkins, S., Jensenius, M., John, J., Jutzi, M., Kohout, T., Krueger, T., Laipert, F., Lopez, N., Luther, R., Lucchetti, A., Mages, D., Marchi, S., Martin, A., McQuaide, M., Michel, P., Moskovitz, N., Murphy, I., Murdoch, N., Naidu, S., Nair, H., Nolan, M., Ormo, J., Pajola, M., Palmer, E., Peachey, J., Pravec, P., Raducan, S., Ramesh, K., Ramirez, J., Reynolds, E., Richman, J., Robin, C., Rodriguez, L., Roufberg, L., Rush, B., Sawyer, C., Scheeres, D., Scheirich, P., Schwartz, S., Shannon, M., Shapiro, B., Shearer, C., Smith, E., Steele, R., Steckloff, J., Stickle, A., Sunshine, J., Superfin, E., Tarzi, Z., Thomas, C., Thomas, J., Trigo-Rodriguez, J., Tropf, B., Vaughan, A., Velez, D., Waller, C., Wilson, D., Wortman, K., Zhang, Y., 2023, Natur, 616, 443, Successful kinetic impact into an asteroid for planetary defence
    Abstract

    Although no known asteroid poses a threat to Earth for at least the next century, the catalogue of near-Earth asteroids is incomplete for objects whose impacts would produce regional devastation^1,2. Several approaches have been proposed to potentially prevent an asteroid impact with Earth by deflecting or disrupting an asteroid^1-3. A test of kinetic impact technology was identified as the highest-priority space mission related to asteroid mitigation¹. NASA's Double Asteroid Redirection Test (DART) mission is a full-scale test of kinetic impact technology. The mission's target asteroid was Dimorphos, the secondary member of the S-type binary near-Earth asteroid (65803) Didymos. This binary asteroid system was chosen to enable ground-based telescopes to quantify the asteroid deflection caused by the impact of the DART spacecraft⁴. Although past missions have utilized impactors to investigate the properties of small bodies^5,6, those earlier missions were not intended to deflect their targets and did not achieve measurable deflections. Here we report the DART spacecraft's autonomous kinetic impact into Dimorphos and reconstruct the impact event, including the timeline leading to impact, the location and nature of the DART impact site, and the size and shape of Dimorphos. The successful impact of the DART spacecraft with Dimorphos and the resulting change in the orbit of Dimorphos⁷ demonstrates that kinetic impactor technology is a viable technique to potentially defend Earth if necessary.

75. Thomas, C., Naidu, S., Scheirich, P., Moskovitz, N., Pravec, P., Chesley, S., Rivkin, A., Osip, D., Lister, T., Benner, L., Brozovic, M., Contreras, C., Morrell, N., RoZek, A., Kusnirak, P., Hornoch, K., Mages, D., Taylor, P., Seymour, A., Snodgrass, C., Jrgensen, U., Dominik, M., Skiff, B., Polakis, T., Knight, M., Farnham, T., Giorgini, J., Rush, B., Bellerose, J., Salas, P., Armentrout, W., Watts, G., Busch, M., Chatelain, J., Gomez, E., Greenstreet, S., Phillips, L., Bonavita, M., Burgdorf, M., Khalouei, E., Longa-Pena, P., Rabus, M., Sajadian, S., Chabot, N., Cheng, A., Ryan, W., Ryan, E., Holt, C., Agrusa, H., 2023, Natur, 616, 448, Orbital period change of Dimorphos due to the DART kinetic impact
    Abstract

    The Double Asteroid Redirection Test (DART) spacecraft successfully performed the first test of a kinetic impactor for asteroid deflection by impacting Dimorphos, the secondary of near-Earth binary asteroid (65803) Didymos, and changing the orbital period of Dimorphos. A change in orbital period of approximately 7 min was expected if the incident momentum from the DART spacecraft was directly transferred to the asteroid target in a perfectly inelastic collision¹, but studies of the probable impact conditions and asteroid properties indicated that a considerable momentum enhancement () was possible^2,3. In the years before impact, we used lightcurve observations to accurately determine the pre-impact orbit parameters of Dimorphos with respect to Didymos^4-6. Here we report the change in the orbital period of Dimorphos as a result of the DART kinetic impact to be 33.0 1.0 (3) min. Using new Earth-based lightcurve and radar observations, two independent approaches determined identical values for the change in the orbital period. This large orbit period change suggests that ejecta contributed a substantial amount of momentum to the asteroid beyond what the DART spacecraft carried.

76. Li, J., Hirabayashi, M., Farnham, T., Sunshine, J., Knight, M., Tancredi, G., Moreno, F., Murphy, B., Opitom, C., Chesley, S., Scheeres, D., Thomas, C., Fahnestock, E., Cheng, A., Dressel, L., Ernst, C., Ferrari, F., Fitzsimmons, A., Ieva, S., Ivanovski, S., Kareta, T., Kolokolova, L., Lister, T., Raducan, S., Rivkin, A., Rossi, A., Soldini, S., Stickle, A., Vick, A., Vincent, J., Weaver, H., Bagnulo, S., Bannister, M., Cambioni, S., Campo Bagatin, A., Chabot, N., Cremonese, G., Daly, R., Dotto, E., Glenar, D., Granvik, M., Hasselmann, P., Herreros, I., Jacobson, S., Jutzi, M., Kohout, T., La Forgia, F., Lazzarin, M., Lin, Z., Lolachi, R., Lucchetti, A., Makadia, R., Mazzotta Epifani, E., Michel, P., Migliorini, A., Moskovitz, N., Ormo, J., Pajola, M., Sanchez, P., Schwartz, S., Snodgrass, C., Steckloff, J., Stubbs, T., Trigo-Rodriguez, J., 2023, Natur, 616, 452, Ejecta from the DART-produced active asteroid Dimorphos
    Abstract

    Some active asteroids have been proposed to be formed as a result of impact events¹. Because active asteroids are generally discovered by chance only after their tails have fully formed, the process of how impact ejecta evolve into a tail has, to our knowledge, not been directly observed. The Double Asteroid Redirection Test (DART) mission of NASA², in addition to having successfully changed the orbital period of Dimorphos³, demonstrated the activation process of an asteroid resulting from an impact under precisely known conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope from impact time T + 15 min to T + 18.5 days at spatial resolutions of around 2.1 km per pixel. Our observations reveal the complex evolution of the ejecta, which are first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and subsequently by solar radiation pressure. The lowest-speed ejecta dispersed through a sustained tail that had a consistent morphology with previously observed asteroid tails thought to be produced by an impact^4,5. The evolution of the ejecta after the controlled impact experiment of DART thus provides a framework for understanding the fundamental mechanisms that act on asteroids disrupted by a natural impact^1,6.

77. Massey, P., Neugent, K., Morrell, N., 2023, ApJ, 947, 77, Constraints on the Binarity of the WN3/O3 Class of Wolf-Rayet Stars
    Abstract

    The WN3/O3 Wolf-Rayet (WR) stars were discovered as part of our survey for WRs in the Magellanic Clouds. The WN3/O3s show the emission lines of a high-excitation WN star and the absorption lines of a hot O-type star, but our prior work has shown that the absorption spectrum is intrinsic to the WR star. Their place in the evolution of massive stars remains unclear. Here we investigate the possibility that they are the products of binary evolution. Although these are not WN3+O3 V binaries, they could still harbor unseen companions. To address this possibility, we have conducted a multiyear radial velocity study of six of the nine known WN3/O3s. Our study finds no evidence of statistically significant radial velocity variations, and allows us to set stringent upper limits on the mass of any hypothetical companion star: for probable orbital inclinations, any companion with a period less than 100 days must have a mass <2M . For periods less than 10 days, any companion would have to have a mass <1M . We argue that scenarios where any such companion is a compact object are unlikely. The absorption lines indicate a normal projected rotational velocity, making it unlikely that these stars evolved with the aid of a companion star that has since merged. The modest rotation also suggests that these stars are not the result of homogenous evolution. Thus it is likely that these stars are a normal but short-lived stage in the evolution of massive stars. ^* This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

78. de Leon, J., Licandro, J., Pinilla-Alonso, N., Moskovitz, N., Kareta, T., Popescu, M., 2023, A&A, 672, A174, Characterisation of the new target of the NASA Lucy mission: Asteroid 152830 Dinkinesh (1999 VD57)
    Abstract

    Context. The NASA Lucy mission is designed to collect data that will be used to study the very interesting population of Jupiter Trojans, which are considered to be time capsules from the time of birth of our Solar System. During its journey, the mission will pass near a main belt asteroid, Donaldjohanson. Recently, NASA announced that a new asteroid in the belt will also be visited by Lucy: 152830 Dinkinesh (1999 VD57).
    Aims: The main goal of this work is to characterise this newly selected target, asteroid Dinkinesh, in order to provide critical information to the mission team. This information includes the most likely surface composition, albedo, and size of the asteroid, which will be used to better plan the data acquisition strategy at the time of the fly-by.
    Methods: To this end, we obtained visible spectra, colour photometry, and time-series photometry for Dinkinesh using several telescopes located at different observatories. For the spectra, we used the 10.4 m Gran Telescopio Canarias (GTC) on the island of La Palma (Spain); for the colour photometry, we used the 4.3 m Lowell Discovery Telescope (LDT) near Happy Jack, Arizona (USA); and for the time-series photometry, we used the 82 cm IAC80 telescope located on the island of Tenerife (Spain). We used the visible reflectance spectrum to obtain the taxonomical class of the asteroid in order to constrain its albedo value. Colour and time-series photometry were used to compute the absolute magnitude of Dinkinesh, which was used in conjunction with an albedo estimation to constrain its size.
    Results: Both the visible spectrum and reflectance values computed from colour photometry show that Dinkinesh is an S-type asteroid; that is, it is composed mainly of silicates and some metal. According to observations carried out as part of the NEOWISE survey, S-type asteroids have a typical geometric albedo of p_V = 0.223 0.073. From our time-series photometry, we obtain an asteroid mean magnitude of r' = 19.99 0.05, which provides an absolute magnitude H_r' = 17.53 0.07 assuming G = 0.19 0.25 for S-types. Using our colour-photometry, we transformed H_r' to H_V = 17.48 0.05. This value of absolute magnitude combined with the geometric albedo provides a mean diameter for Dinkinesh of ~900 m, ranging between a minimum size of 542 m and a maximum size of 1309 m.

79. Abbott, T., Aguena, M., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M., Bernstein, G., Birrer, S., Blazek, J., Bocquet, S., Brandao-Souza, A., Bridle, S., Brooks, D., Burke, D., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F., Cawthon, R., Chang, C., Chen, A., Chen, R., Choi, A., Conselice, C., Cordero, J., Costanzi, M., Crocce, M., da Costa, L., Pereira, M., Davis, C., Davis, T., DeRose, J., Desai, S., Di Valentino, E., Diehl, H., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Farahi, A., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Friedel, D., Friedrich, O., Frieman, J., Garcia-Bellido, J., Gatti, M., Giani, L., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hamaus, N., Harrison, I., Hartley, W., Herner, K., Hinton, S., Hollowood, D., Honscheid, K., Huang, H., Huff, E., Huterer, D., Jain, B., James, D., Jarvis, M., Jeffrey, N., Jeltema, T., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Leget, P., Lemos, P., Leonard, C., Liddle, A., Lima, M., Lin, H., MacCrann, N., Marshall, J., McCullough, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Miranda, V., Mohr, J., Muir, J., Myles, J., Nadathur, S., Navarro-Alsina, A., Nichol, R., Ogando, R., Omori, Y., Palmese, A., Pandey, S., Park, Y., Paterno, M., Paz-Chinchon, F., Percival, W., Pieres, A., Plazas Malagon, A., Porredon, A., Prat, J., Raveri, M., Rodriguez-Monroy, M., Rogozenski, P., Rollins, R., Romer, A., Roodman, A., Rosenfeld, R., Ross, A., Rykoff, E., Samuroff, S., Sanchez, C., Sanchez, E., Sanchez, J., Sanchez Cid, D., Scarpine, V., Scolnic, D., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Smith, M., Soares-Santos, M., Suchyta, E., Tabbutt, M., Tarle, G., Thomas, D., To, C., Troja, A., Troxel, M., Tutusaus, I., Varga, T., Vincenzi, M., Walker, A., Weaverdyck, N., Wechsler, R., Weller, J., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., DES Collaboration, 2023, PhRvD, 107, 083504, Dark Energy Survey Year 3 results: Constraints on extensions to CDM with weak lensing and galaxy clustering
    Abstract

    We constrain six possible extensions to the cold dark matter (CDM) model using measurements from the Dark Energy Survey's first three years of observations, alone and in combination with external cosmological probes. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data vectors and blind analyses of real data to validate the robustness of our results to astrophysical and modeling systematic errors. In many cases, constraining power is limited by the absence of theoretical predictions beyond the linear regime that are reliable at our required precision. The CDM extensions are dark energy with a time-dependent equation of state, nonzero spatial curvature, additional relativistic degrees of freedom, sterile neutrinos with eV-scale mass, modifications of gravitational physics, and a binned ₈(z ) model which serves as a phenomenological probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find (w_p,w_a)=(-0.9 9_-0.17^+0.28,-0.9 1.2 ) at 68% confidence with z_p=0.24 from the DES measurements alone, and (w_p,w_a)=(-1.0 3_-0.03^+0.04,-0. 4_-0.3^+0.4) with z_p=0.21 for the combination of all data considered. Curvature constraints of _k=0.0009 0.0017 and effective relativistic species N_eff=3.1 0_-0.16^+0.15 are dominated by external data, though adding DES information to external low-redshift probes tightens the _k constraints that can be made without cosmic microwave background observables by 20%. For massive sterile neutrinos, DES combined with external data improves the upper bound on the mass m_eff by a factor of 3 compared to previous analyses, giving 95% limits of ( N_eff,m_eff)(0.28 ,0.20 eV ) when using priors matching a comparable Planck analysis. For modified gravity, we constrain changes to the lensing and Poisson equations controlled by functions (k ,z )=₀(z )/ _,0 and (k ,z )=₀(z )/ _,0, respectively, to ₀=0. 6_-0.5^+0.4 from DES alone and (₀,₀)=(0.04 0.05 ,0.0 8_-0.19^+0.21) for the combination of all data, both at 68% confidence. Overall, we find no significant evidence for physics beyond CDM .

80. Loyd, R., Schneider, P., Jackman, J., France, K., Shkolnik, E., Arulanantham, N., Cauley, P., Llama, J., Schneider, A., 2023, AJ, 165, 146, Flares, Rotation, Activity Cycles, and a Magnetic Star-Planet Interaction Hypothesis for the Far-ultraviolet Emission of GJ 436
    Abstract

    Variability in the far-ultraviolet (FUV) emission produced by stellar activity affects photochemistry and heating in orbiting planetary atmospheres. We present a comprehensive analysis of the FUV variability of GJ 436, a field-age M2.5V star (P _rot 44 days) that is orbited by a warm Neptune-sized planet (M 25 M , R 4.1 M , P _orb 2.6 days). Observations at three epochs from 2012 to 2018 span nearly a full activity cycle, sample two rotations of the star and two orbital periods of the planet, and reveal a multitude of brief flares. From 2012 to 2018, the star's 7.75 0.10 yr activity cycle produced the largest observed variations, 38% 3% in the summed flux of the major FUV emission lines. In 2018, the variability due to rotation was 8% 2%. An additional 11% 1% scatter at a cadence of 10 minutes, which is treated as white noise in the fits, likely has both instrumental and astrophysical origins. Flares increased time-averaged emission by 15% over the 0.88 days of cumulative exposure, peaking as high as 25 quiescence. We interpret these flare values as lower limits given that flares too weak or too infrequent to have been observed likely exist. GJ 436's flare frequency distribution at FUV wavelengths is unusual compared to other field-age M dwarfs, exhibiting a statistically significant dearth of high-energy (>4 10²⁸ erg) events, which we hypothesize to be the result of a magnetic star-planet interaction (SPI) triggering premature flares. If an SPI is present, GJ 436 b's magnetic field strength must be 100 G to explain the statistically insignificant increase in the orbit-phased FUV emission.

81. Grayling, M., Gutierrez, C., Sullivan, M., Wiseman, P., Vincenzi, M., Galbany, L., Moller, A., Brout, D., Davis, T., Frohmaier, C., Graur, O., Kelsey, L., Lidman, C., Popovic, B., Smith, M., Toy, M., Tucker, B., Zontos, Z., Abbott, T., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Asorey, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Gatti, M., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lewis, G., Malik, U., March, M., Menanteau, F., Miquel, R., Morgan, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Rodriguez-Monroy, M., Romer, A., Roodman, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Tucker, D., Varga, T., DES Collaboration, 2023, MNRAS, 520, 684, Core-collapse supernovae in the Dark Energy Survey: luminosity functions and host galaxy demographics
    Abstract

    We present the luminosity functions and host galaxy properties of the Dark Energy Survey (DES) core-collapse supernova (CCSN) sample, consisting of 69 Type II and 50 Type Ibc spectroscopically and photometrically confirmed supernovae over a redshift range 0.045 < z < 0.25. We fit the observed DES griz CCSN light curves and K-correct to produce rest-frame R-band light curves. We compare the sample with lower redshift CCSN samples from Zwicky Transient Facility (ZTF) and Lick Observatory Supernova Search (LOSS). Comparing luminosity functions, the DES and ZTF samples of SNe II are brighter than that of LOSS with significances of 3.0 and 2.5, respectively. While this difference could be caused by redshift evolution in the luminosity function, simpler explanations such as differing levels of host extinction remain a possibility. We find that the host galaxies of SNe II in DES are on average bluer than in ZTF, despite having consistent stellar mass distributions. We consider a number of possibilities to explain this - including galaxy evolution with redshift, selection biases in either the DES or ZTF samples, and systematic differences due to the different photometric bands available - but find that none can easily reconcile the differences in host colour between the two samples and thus its cause remains uncertain.

82. Cartwright, R., DeColibus, R., C. Castillo-Rogez, J., Beddingfield, C., Grundy, W., Nordheim, T., 2023, PSJ, 4, 42, Evidence for Nitrogen-bearing Species on Umbriel: Sourced from a Subsurface Ocean, Undifferentiated Crust, or Impactors?
    Abstract

    Near-infrared spectra of Umbriel and the other classical Uranian moons exhibit 2.2 m absorption bands that could result from ammonia (NH₃) bearing species, possibly exposed in the geologically recent past. However, Umbriel has an ancient surface with minimal evidence for recent endogenic activity, raising the possibility that more refractory species are present, and/or that NH₃ is retained over long timescales. We analyzed 33 spectra of Umbriel to investigate its 2.2 m band, along with three other absorption features we identified near 2.14, 2.22, and 2.24 m. We assessed the subobserver longitudinal distributions of these four bands, finding that they are present across Umbriel and may be spatially associated with geologic features such as craters and large basins. We compared the bands to 15 candidate constituents. We found that Umbriel's 2.14 m and 2.22 m bands are most consistent with the spectral signature of organics, its 2.24 m band is best matched by NH₃ ice, and its 2.2 m band is consistent with the signatures of NH₃-H₂O mixtures, aluminum-bearing phyllosilicates, and sodium-bearing carbonates. However, some of these candidate constituents do not match Umbriel's spectral properties in other wavelength regions, highlighting the gaps in our understanding of the Uranian moons' surface compositions. Umbriel's 2.14 m band may alternatively result from a 2 ₃ overtone mode of CO₂ ice. If present on Umbriel, these candidate constituents could have formed in contact with an internal ocean and were subsequently exposed during Umbriel's early history. Alternatively, these constituents might have originated in an undifferentiated crust or were delivered by impactors.

83. Shrestha, M., Sand, D., Alexander, K., Bostroem, K., Hosseinzadeh, G., Pearson, J., Aghakhanloo, M., Vinko, J., Andrews, J., Jencson, J., Lundquist, M., Wyatt, S., Howell, D., McCully, C., Gonzalez, E., Pellegrino, C., Terreran, G., Hiramatsu, D., Newsome, M., Farah, J., Jha, S., Smith, N., Wheeler, J., Martinez-Vazquez, C., Carballo-Bello, J., Drlica-Wagner, A., James, D., Mutlu-Pakdil, B., Stringfellow, G., Sakowska, J., Noel, N., Bom, C., Kuehn, K., 2023, ApJL, 946, L25, Limit on Supernova Emission in the Brightest Gamma-Ray Burst, GRB 221009A
    Abstract

    We present photometric and spectroscopic observations of the extraordinary gamma-ray burst (GRB) 221009A in search of an associated supernova. Some past GRBs have shown bumps in the optical light curve that coincide with the emergence of supernova spectral features, but we do not detect any significant light-curve features in GRB 221009A, nor do we detect any clear sign of supernova spectral features. Using two well-studied GRB-associated supernovae (SN 2013dx, ${M}_{r,\max }=-19.54;$ SN 2016jca, ${M}_{r,\max }=-19.04$ ) at a similar redshift as GRB 221009A (z = 0.151), we modeled how the emergence of a supernova would affect the light curve. If we assume the GRB afterglow to decay at the same rate as the X-ray data, the combination of afterglow and a supernova component is fainter than the observed GRB brightness. For the case where we assume the best-fit power law to the optical data as the GRB afterglow component, a supernova contribution should have created a clear bump in the light curve, assuming only extinction from the Milky Way. If we assume a higher extinction of E(B - V) = 1.74 mag (as has been suggested elsewhere), the supernova contribution would have been hard to detect, with a limit on the associated supernova of ${M}_{r,\max }\approx -$ 19.54. We do not observe any clear supernova features in our spectra, which were taken around the time of expected maximum light. The lack of a bright supernova associated with GRB 221009A may indicate that the energy from the explosion is mostly concentrated in the jet, leaving a lower energy budget available for the supernova.

84. Kueny, J., Chandler, C., Devogele, M., Moskovitz, N., Pravec, P., Kucakova, H., Hornoch, K., Kusnirak, P., Granvik, M., Konstantopoulou, C., Jannsen, N., Moran, S., Siltala, L., Fedorets, G., Ferrais, M., Jehin, E., Kareta, T., Hanus, J., 2023, PSJ, 4, 56, Implications for the Formation of (155140) 2005 UD from a New Convex Shape Model
    Abstract

    (155140) 2005 UD has a similar orbit to (3200) Phaethon, an active asteroid in a highly eccentric orbit thought to be the source of the Geminid meteor shower. Evidence points to a genetic relationship between these two objects, but we have yet to fully understand how 2005 UD and Phaethon could have separated into this associated pair. Presented herein are new observations of 2005 UD from five observatories that were carried out during the 2018, 2019, and 2021 apparitions. We implemented light curve inversion using our new data, as well as dense and sparse archival data from epochs in 2005-2021, to better constrain the rotational period and derive a convex shape model of 2005 UD. We discuss two equally well-fitting pole solutions ( = 116.6, = -53.6) and ( = 300.3, = -55.4), the former largely in agreement with previous thermophysical analyses and the latter interesting due to its proximity to Phaethon's pole orientation. We also present a refined sidereal period of P _sid = 5.234246 0.000097 hr. A search for surface color heterogeneity showed no significant rotational variation. An activity search using the deepest stacked image available of 2005 UD near aphelion did not reveal a coma or tail but allowed modeling of an upper limit of 0.04-0.37 kg s^-1 for dust production. We then leveraged our spin solutions to help limit the range of formation scenarios and the link to Phaethon in the context of nongravitational forces and timescales associated with the physical evolution of the system.

85. Zhao, L., Kunovac, V., Brewer, J., Llama, J., Millholland, S., Hedges, C., Szymkowiak, A., Roettenbacher, R., Cabot, S., Weiss, S., Fischer, D., 2023, NatAs, 7, 366, Author Correction: Measured spin-orbit alignment of ultra-short-period super-Earth 55 Cancri e
    Abstract

    No abstract found.

86. Bowen, B., Reddy, V., De Florio, M., Kareta, T., Pearson, N., Furfaro, R., Sharkey, B., McGraw, A., Cantillo, D., Sanchez, J., Battle, A., 2023, PSJ, 4, 52, Grain Size Effects on Visible and Near-infrared (0.35-2.5 m) Laboratory Spectra of Ordinary Chondrite and HED Meteorites
    Abstract

    Remote spectral characterization of near-Earth asteroids (NEAs) relies on laboratory spectral calibration to constrain their surface composition, including mineral chemistry and relative mineral abundances. Often these calibrations are based on fine meteorite powders that are representative of regolith observed on large NEAs such as (433) Eros. However, spacecraft observations of smaller NEAs such as (25143) Itokawa, (101955) Bennu, and (162173) Ryugu show surfaces devoid of a thick layer of regolith and instead find variegated landscapes with millimeter-sized particles to meter-scale boulders. Here we present the results of a laboratory study to understand the effects of grain size on the spectral properties of meteorites and how this can impact ground-based characterization of NEAs. Our study focuses on ordinary chondrites (H, L, LL) and HED meteorites, as they comprise ~90% of all meteorites that fall on Earth. Compared to ordinary chondrites, the spectral band parameters of HED meteorites are less affected by changing grain size. Among the ordinary chondrites, LL chondrites are least affected, but the spectral band parameters and mineral chemistries and abundances for H and L chondrites are most affected by changing grain size. Grain size does not seem to have any significant effect on the taxonomic classification of our meteorite spectra. We also used the Hapke model to investigate trends in single-scattering albedo as a function of grain size and present equations to recover the grain size from a spectrum.

87. Chandler, C., Oldroyd, W., Hsieh, H., Trujillo, C., Burris, W., Kueny, J., DeSpain, J., Farrell, K., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 60, New Recurrently Active Main-belt Comet 2010 LH15
    Abstract

    We announce the discovery of a main-belt comet (MBC), 2010 LH₁₅ (alternately designated 2010 TJ₁₇₅). MBCs are a rare type of main-belt asteroid that display comet-like activity, such as tails or comae, caused by sublimation. Consequently, MBCs help us map the location of solar system volatiles, providing insight into the origins of material prerequisite for life as we know it. However, MBCs have proven elusive, with fewer than 20 found among the 1.1 million known main-belt asteroids. This finding derives from Active Asteroids, a NASA Partner Citizen Science program we designed to identify more of these important objects. After volunteers classified an image of 2010 LH₁₅ as showing activity, we carried out a follow-up investigation which revealed evidence of activity from two epochs spanning nearly a decade. This discovery is timely, with 2010 LH₁₅ inbound toward its 2024 March perihelion passage, with potential activity onset as early as late 2023.

88. Hsieh, H., Micheli, M., Kelley, M., Knight, M., Moskovitz, N., Pittichova, J., Sheppard, S., Thirouin, A., Trujillo, C., Wainscoat, R., Weryk, R., Ye, Q., 2023, PSJ, 4, 43, Observational Characterization of Main-belt Comet and Candidate Main-belt Comet Nuclei
    Abstract

    We report observations of nine main-belt comets (MBCs) or candidate MBCs, most of which were obtained when the targets were apparently inactive. We find effective nucleus radii (assuming albedos of p _V = 0.05 0.02) of r _n = (0.24 0.05) km for 238P/Read, r _n = (0.9 0.2) km for 313P/Gibbs, r _n = (0.6 0.1) km for 324P/La Sagra, r _n = (1.0 0.2) km for 426P/PANSTARRS, r _n = (0.5 0.1) km for 427P/ATLAS, r _n < (0.3 0.1) km for P/2016 J1-A (PANSTARRS), r _n < (0.17 0.04) km for P/2016 J1-B (PANSTARRS), r _n (0.5 0.2) km for P/2017 S9 (PANSTARRS), recently redesignated 455P/PANSTARRS, and r _n = (0.4 0.1) km for P/2019 A3 (PANSTARRS). We identify evidence of activity in observations of 238P in 2021, and find similar inferred activity onset times and net initial mass-loss rates for 238P during perihelion approaches in 2010, 2016, and 2021. P/2016 J1-A and P/2016 J1-B are also found to be active in 2021 and 2022, making them collectively the tenth MBC confirmed to be recurrently active near perihelion and therefore likely to be exhibiting sublimation-driven activity. The nucleus of 313P is found to have colors of $g^{\prime} -r^{\prime} =0.52\pm 0.05$ and $r^{\prime} -i^{\prime} =0.22\pm 0.07$ , consistent with 313P being a Lixiaohua family member. We also report nondetections of P/2015 X6 (PANSTARRS), where we conclude that its current nucleus size is likely below our detection limits (r _n 0.3 km). Lastly, we find that of 17 MBCs or candidate MBCs for which nucleus sizes (or inferred parent body sizes) have been estimated, >80% have r _n 1.0 km, pointing to an apparent physical preference toward small MBCs, where we suggest that Yarkovsky-O'Keefe-Radzievskii-Paddack spin-up may play a significant role in triggering and/or facilitating MBC activity.

89. Velloso, E., Anthony, F., do Nascimento, J., Silveira, L., Hall, J., Saar, S., 2023, ApJL, 945, L12, Multicomponent Activity Cycles Using Hilbert-Huang Analysis
    Abstract

    The temporal analysis of stellar activity evolution is usually dominated by a complex trade-off between model complexity and interpretability, often by neglecting the nonstationary nature of the process. Recent studies appear to indicate that the presence of multiple coexisting cycles in a single star is more common than previously thought. The correct identification of physically meaningful cyclic components in spectroscopic time series is therefore a crucial task, which cannot overlook local behaviors. Here we propose a decomposition technique that adaptively recovers amplitude- and frequency-varying components. We present our results for the solar activity as measured both by the sunspot number and the K-line emission index, and we consistently recover the Schwabe and Gleissberg cycles as well as the Gnevyshev-Ohl pattern probably related to the Hale cycle. We also recover the known 8 yr cycle for 61 Cygni A, in addition to evidence of a three-cycles-long pattern reminiscent of the Gnevyshev-Ohl rule. This is particularly interesting as we cannot discard the possibility of a relationship between the measured field polarity reversals and this Hale-like periodicity.

90. Oldroyd, W., Chandler, C., Trujillo, C., Burris, W., Kueny, J., Hsieh, H., Farrell, K., DeSpain, J., Mazzucato, M., Bosch, M., Shaw-Diaz, T., Gonano, V., 2023, RNAAS, 7, 42, Comet-like Activity Discovered on Quasi-Hilda Asteroid 2009 DQ118
    Abstract

    We report evidence of comet-like activity on asteroid 2009 DQ118, a quasi-Hilda object near the 3:2 interior mean-motion resonance with Jupiter. This discovery was made by volunteers as part of the Active Asteroids Citizen Science project, a NASA Partner hosted on the Zooniverse platform. Follow-up archival searches yielded over 20 images of 2009 DQ118 exhibiting a comet-like tail on UT 2016 March 8 and 9 acquired with the Dark Energy Camera on the Blanco 4 m telescope at the Cerro Tololo Inter-American Observatory, Chile. These images were taken when 2009 DQ118 was near its 2016 perihelion passage. 2009 DQ118 will next reach perihelion on UT 2023 April 22; hence, the next several months are an excellent time to observe 2009 DQ118 to search for a second epoch of activity for this object.

91. Sebastian, D., Swayne, M., Maxted, P., Triaud, A., Sousa, S., Olofsson, G., Beck, M., Billot, N., Hoyer, S., Gill, S., Heidari, N., Martin, D., Persson, C., Standing, M., Alibert, Y., Alonso, R., Anglada, G., Asquier, J., Barczy, T., Barrado, D., Barros, S., Battley, M., Baumjohann, W., Beck, T., Benz, W., Bergomi, M., Boisse, I., Bonfils, X., Brandeker, A., Broeg, C., Cabrera, J., Charnoz, S., Collier Cameron, A., Csizmadia, S., Davies, M., Deleuil, M., Delrez, L., Demangeon, O., Demory, B., Dransfield, G., Ehrenreich, D., Erikson, A., Fortier, A., Fossati, L., Fridlund, M., Gandolfi, D., Gillon, M., Gudel, M., Hasiba, J., Hebrard, G., Heng, K., Isaak, K., Kiss, L., Kopp, E., Kunovac, V., Laskar, J., Lecavelier des Etangs, A., Lendl, M., Lovis, C., Magrin, D., McCormac, J., Miller, N., Nascimbeni, V., Ottensamer, R., Pagano, I., Palle, E., Pepe, F., Peter, G., Piotto, G., Pollacco, D., Queloz, D., Ragazzoni, R., Rando, N., Rauer, H., Ribas, I., Lalitha, S., Santerne, A., Santos, N., Scandariato, G., Segransan, D., Simon, A., Smith, A., Steller, M., Szabo, G., Thomas, N., Udry, S., Van Grootel, V., Walton, N., 2023, MNRAS, 519, 3546, The EBLM project - IX. Five fully convective M-dwarfs, precisely measured with CHEOPS and TESS light curves
    Abstract

    Eclipsing binaries are important benchmark objects to test and calibrate stellar structure and evolution models. This is especially true for binaries with a fully convective M-dwarf component for which direct measurements of these stars' masses and radii are difficult using other techniques. Within the potential of M-dwarfs to be exoplanet host stars, the accuracy of theoretical predictions of their radius and effective temperature as a function of their mass is an active topic of discussion. Not only the parameters of transiting exoplanets but also the success of future atmospheric characterization relies on accurate theoretical predictions. We present the analysis of five eclipsing binaries with low-mass stellar companions out of a subsample of 23, for which we obtained ultra-high-precision light curves using the CHEOPS satellite. The observation of their primary and secondary eclipses are combined with spectroscopic measurements to precisely model the primary parameters and derive the M-dwarfs mass, radius, surface gravity, and effective temperature estimates using the PYCHEOPS data analysis software. Combining these results to the same set of parameters derived from TESS light curves, we find very good agreement (better than 1 per cent for radius and better than 0.2 per cent for surface gravity). We also analyse the importance of precise orbits from radial velocity measurements and find them to be crucial to derive M-dwarf radii in a regime below 5 per cent accuracy. These results add five valuable data points to the mass-radius diagram of fully convective M-dwarfs.

92. Jackman, J., Shkolnik, E., Million, C., Fleming, S., Richey-Yowell, T., Loyd, R., 2023, MNRAS, 519, 3564, Extending optical flare models to the UV: results from comparing of TESS and GALEX flare observations for M Dwarfs
    Abstract

    The ultraviolet (UV) emission of stellar flares may have a pivotal role in the habitability of rocky exoplanets around low-mass stars. Previous studies have used white-light observations to calibrate empirical models which describe the optical and UV flare emission. However, the accuracy of the UV predictions of models has previously not been tested. We combined TESS optical and GALEX UV observations to test the UV predictions of empirical flare models calibrated using optical flare rates of M stars. We find that the canonical 9000-K black-body model used by flare studies underestimates the GALEX near-ultraviolet (NUV) energies of field age M stars by up to a factor of 6.5 0.7 and the GALEX far-ultraviolet energies of fully convective field age M stars by 30.6 10.0. We calculated energy correction factors that can be used to bring the UV predictions of flare models closer in line with observations. We calculated pseudo-continuum flare temperatures that describe both the white-light and GALEX NUV emission. We measured a temperature of 10 700 K for flares from fully convective M stars after accounting for the contribution from UV line emission. We also applied our correction factors to the results of previous studies of the role of flares in abiogenesis. Our results show that M stars do not need to be as active as previously thought in order to provide the NUV flux required for prebiotic chemistry, however, we note that flares will also provide more FUV flux than previously modelled.

93. Radhakrishnan, V., Keller, C., Doelman, N., Por, E., 2023, A&A, 670, A137, Estimating non-common path aberrations with an adaptive coronagraph
    Abstract

    Context. The focal-plane contrast of exoplanet imagers is affected by non-common path aberrations (NCPAs) that the adaptive optics system cannot correct for because they occur after the wavefront has been measured. NCPA estimation is commonly based on the long-exposure science image. Phase retrieval algorithms are often used, and they mostly assume that the residual phase error right after the adaptive optics system and averaged over the integration time is zero. This assumption is not always correct, for instance when controlling the adaptive optics to maximize the focal-plane contrast at the location of an exoplanet, that is to say in an adaptive coronagraph. For such cases, we present a method to calculate the NCPA using the phase information derived from the wavefront sensor (WFS) data and the science focal-plane image.
    Aims: We aim to accurately estimate the NCPA phase in the presence of (residual) atmospheric turbulence with a nonzero average wavefront. We then aim to take the NCPA into account in the adaptive coronagraph controller and achieve a higher contrast.
    Methods: The WFS measures the wavefront throughout the integration time of the science image. We combine information from the recorded WFS phases to remove the effects of the nonzero average phase from the Point Spread Function (PSF) and to remove the effects of the residual turbulence averaging over time. Then we estimate the NCPA by applying a phase-diversity-based algorithm to the resulting images. Our method is currently limited to imagers with pupil-plane coronagraphs.
    Results: We are able to recover the NCPA in an adaptive coronagraph setting with 0.01 radian RMS residuals and with a residual turbulence phase error of approximately 0.4 radian RMS. When accounted for in a contrast-control scheme, the NCPA correction leads to an order of magnitude improvement of contrast and a 50% increase in Strehl ratio, in numerical simulations.

94. Zhao, L., Kunovac, V., Brewer, J., Llama, J., Millholland, S., Hedges, C., Szymkowiak, A., Roettenbacher, R., Cabot, S., Weiss, S., Fischer, D., 2023, NatAs, 7, 198, Measured spin-orbit alignment of ultra-short-period super-Earth 55 Cancri e
    Abstract

    A planet's orbital alignment places important constraints on how a planet formed and consequently evolved. The dominant formation pathway of ultra-short-period planets (P < 1 day) is particularly mysterious as such planets most likely formed further out, and it is not well understood what drove their migration inwards to their current positions. Measuring the orbital alignment is difficult for smaller super-Earth/sub-Neptune planets, which give rise to smaller amplitude signals. Here we present radial velocities across two transits of 55 Cancri (Cnc) e, an ultra-short-period super-Earth, observed with the Extreme Precision Spectrograph. Using the classical Rossiter-McLaughlin method, we measure 55 Cnc e's sky-projected stellar spin-orbit alignment (that is, the projected angle between the planet's orbital axis and its host star's spin axis) to be =10_-20⁺¹⁷ with an unprojected angle of =23_-12⁺¹⁴. The best-fit Rossiter-McLaughlin model to the Extreme Precision Spectrograph data has a radial velocity semi-amplitude of just 0.41_-0.10^+0.09 m s¹. The spin-orbit alignment of 55 Cnc e favours dynamically gentle migration theories for ultra-short-period planets, namely tidal dissipation through low-eccentricity planet-planet interactions and/or planetary obliquity tides.

95. Schiappucci, E., Bianchini, F., Aguena, M., Archipley, M., Balkenhol, L., Bleem, L., Chaubal, P., Crawford, T., Grandis, S., Omori, Y., Reichardt, C., Rozo, E., Rykoff, E., To, C., Abbott, T., Ade, P., Alves, O., Anderson, A., Andrade-Oliveira, F., Annis, J., Avva, J., Bacon, D., Benabed, K., Bender, A., Benson, B., Bernstein, G., Bertin, E., Bocquet, S., Bouchet, F., Brooks, D., Burke, D., Carlstrom, J., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cecil, T., Chang, C., Chichura, P., Chou, T., Costanzi, M., Cukierman, A., da Costa, L., Daley, C., de Haan, T., Desai, S., Dibert, K., Diehl, H., Dobbs, M., Doel, P., Doux, C., Dutcher, D., Everett, S., Everett, W., Feng, C., Ferguson, K., Ferrero, I., Ferte, A., Flaugher, B., Foster, A., Frieman, J., Galli, S., Gambrel, A., Garcia-Bellido, J., Gardner, R., Gatti, M., Giannantonio, T., Goeckner-Wald, N., Gruen, D., Gualtieri, R., Guns, S., Gutierrez, G., Halverson, N., Hinton, S., Hivon, E., Holder, G., Hollowood, D., Holzapfel, W., Honscheid, K., Hood, J., Huang, N., James, D., Knox, L., Korman, M., Kuehn, K., Kuo, C., Lahav, O., Lee, A., Lidman, C., Lima, M., Lowitz, A., Lu, C., March, M., Mena-Fernandez, J., Menanteau, F., Millea, M., Miquel, R., Mohr, J., Montgomery, J., Muir, J., Natoli, T., Noble, G., Novosad, V., Ogando, R., Padin, S., Pan, Z., Paz-Chinchon, F., Pereira, M., Pieres, A., Plazas Malagon, A., Prabhu, K., Prat, J., Quan, W., Rahlin, A., Raveri, M., Rodriguez-Monroy, M., Romer, A., Rouble, M., Ruhl, J., Sanchez, E., Scarpine, V., Schubnell, M., Smecher, G., Smith, M., Soares-Santos, M., Sobrin, J., Suchyta, E., Suzuki, A., Tarle, G., Thomas, D., Thompson, K., Thorne, B., Tucker, C., Umilta, C., Vieira, J., Vincenzi, M., Wang, G., Weaverdyck, N., Weller, J., Whitehorn, N., Wu, W., Yefremenko, V., Young, M., SPT-3G, DES Collaborations, 2023, PhRvD, 107, 042004, Measurement of the mean central optical depth of galaxy clusters via the pairwise kinematic Sunyaev-Zel'dovich effect with SPT-3G and DES
    Abstract

    We infer the mean optical depth of a sample of optically selected galaxy clusters from the Dark Energy Survey via the pairwise kinematic Sunyaev-Zel'dovich (KSZ) effect. The pairwise KSZ signal between pairs of clusters drawn from the Dark Energy Survey Year-3 cluster catalog is detected at 4.1 in cosmic microwave background temperature maps from two years of observations with the SPT-3G camera on the South Pole Telescope. After cuts, there are 24,580 clusters in the 1 ,400 deg² of the southern sky observed by both experiments. We infer the mean optical depth of the cluster sample with two techniques. The optical depth inferred from the pairwise KSZ signal is _e=(2.97 0.73 )10^-3 , while that inferred from the thermal SZ signal is _e=(2.51 0.5 5^stat0.1 5^syst)10^-3 . The two measures agree at 0.6 . We perform a suite of systematic checks to test the robustness of the analysis.

96. Chandler, C., Oldroyd, W., Trujillo, C., Burris, W., Hsieh, H., Kueny, J., Mazzucato, M., Bosch, M., Shaw-Diaz, T., 2023, RNAAS, 7, 27, New Active Asteroid 2015 VA108: A Citizen Science Discovery
    Abstract

    We announce the discovery of activity, in the form of a distinct cometary tail, emerging from main-belt asteroid 2015 VA₁₀₈. Activity was first identified by volunteers of the Citizen Science project Active Asteroids (a NASA Partner). We uncovered one additional image from the same observing run which also unambiguously shows 2015 VA₁₀₈ with a tail oriented between the anti-solar and anti-motion vectors that are often correlated with activity orientation on sky. Both publicly available archival images were originally acquired UT 2015 October 11 with the Dark Energy Camera (DECam) on the Blanco 4 m telescope at the Cerro Tololo Inter-American Observatory (Chile) as part of the Dark Energy Camera Legacy Survey. Activity occurred near perihelion and, combined with its residence in the main asteroid belt, 2015 VA₁₀₈ is a candidate main-belt comet, an active asteroid subset known for volatile sublimation.

97. Simon, J., Brown, T., Mutlu-Pakdil, B., Ji, A., Drlica-Wagner, A., Avila, R., Martinez-Vazquez, C., Li, T., Balbinot, E., Bechtol, K., Frebel, A., Geha, M., Hansen, T., James, D., Pace, A., Aguena, M., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gatti, M., Gerdes, D., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Kuehn, K., Kuropatkin, N., Marshall, J., Mena-Fernandez, J., Miquel, R., Palmese, A., Paz-Chinchon, F., Pereira, M., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Sanchez, E., Santiago, B., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., To, C., Vincenzi, M., Weaverdyck, N., Wilkinson, R., 2023, ApJ, 944, 43, Timing the r-process Enrichment of the Ultra-faint Dwarf Galaxy Reticulum II
    Abstract

    The ultra-faint dwarf galaxy Reticulum II (Ret II) exhibits a unique chemical evolution history, with ${72}_{-12}^{+10}$ % of its stars strongly enhanced in r-process elements. We present deep Hubble Space Telescope photometry of Ret II and analyze its star formation history. As in other ultra-faint dwarfs, the color-magnitude diagram is best fit by a model consisting of two bursts of star formation. If we assume that the bursts were instantaneous, then the older burst occurred around the epoch of reionization, forming ~80% of the stars in the galaxy, while the remainder of the stars formed ~3 Gyr later. When the bursts are allowed to have nonzero durations, we obtain slightly better fits. The best-fitting model in this case consists of two bursts beginning before reionization, with approximately half the stars formed in a short (100 Myr) burst and the other half in a more extended period lasting 2.6 Gyr. Considering the full set of viable star formation history models, we find that 28% of the stars formed within 500 200 Myr of the onset of star formation. The combination of the star formation history and the prevalence of r-process-enhanced stars demonstrates that the r-process elements in Ret II must have been synthesized early in its initial star-forming phase. We therefore constrain the delay time between the formation of the first stars in Ret II and the r-process nucleosynthesis to be less than 500 Myr. This measurement rules out an r-process source with a delay time of several Gyr or more, such as GW170817.

98. Chandler, C., Trujillo, C., Oldroyd, W., Kueny, J., Burris, W., Hsieh, H., Mazzucato, M., Bosch, M., Shaw-Diaz, T., 2023, RNAAS, 7, 22, Discovery of Dust Emission Activity Emanating from Main-belt Asteroid 2015 FW412
    Abstract

    We present the discovery of activity emanating from main-belt asteroid 2015 FW₄₁₂, a finding stemming from the Citizen Science project Active Asteroids, a NASA Partner program. We identified a pronounced tail originating from 2015 FW₄₁₂ and oriented in the anti-motion direction in archival Blanco 4 m (Cerro Tololo Inter-American Observatory, Chile) Dark Energy Camera images from UT 2015 April 13, 18, 19, 21 and 22. Activity occurred near perihelion, consistent with the main-belt comets (MBCs), an active asteroid subset known for sublimation-driven activity in the main asteroid belt; thus 2015 FW₄₁₂ is a candidate MBC. We did not detect activity on UT 2021 December 12 using the Inamori-Magellan Areal Camera and Spectrograph on the 6.5 m Baade telescope, when 2015 FW₄₁₂ was near aphelion.

99. Baines, E., Blomquist, S., Clark, J., Gorney, J., Maier, E., Sanborn, J., Schmitt, H., Stone, J., van Belle, G., von Braun, K., 2023, AJ, 165, 41, Simultaneous Six-way Observations from the Navy Precision Optical Interferometer
    Abstract

    We measured the angular diameters of six stars using the six-element observing mode of the Navy Precision Optical Interferometer (NPOI) for the first time since the early 2000s. Four of the diameters ranged from 1.2 to 1.9 mas, while the two others were much smaller at approximately 0.5 mas to 0.7 mas, which are the two smallest angular diameters measured to date with the NPOI. There is a larger spread in the measurements than data obtained with three-, four-, or five-element modes, which can be attributed in part to the flux imbalance due to the combination of more than two siderostats in a single spectrograph, and also to crosstalk between multiple baselines related to nonlinearities in the fast-delay-line dither strokes. We plan to address this in the future by using the VISION beam combiner.

100. Kelsey, L., Sullivan, M., Wiseman, P., Armstrong, P., Chen, R., Brout, D., Davis, T., Dixon, M., Frohmaier, C., Galbany, L., Graur, O., Kessler, R., Lidman, C., Moller, A., Popovic, B., Rose, B., Scolnic, D., Smith, M., Vincenzi, M., Abbott, T., Aguena, M., Allam, S., Alves, O., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Costanzi, M., da Costa, L., Pereira, M., Desai, S., Diehl, H., Everett, S., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lewis, G., Mena-Fernandez, J., Miquel, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Raveri, M., Rodriguez-Monroy, M., Romer, A., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Suchyta, E., Swanson, M., Tarle, G., Tucker, D., Weaverdyck, N., DES Collaboration, 2023, MNRAS, 519, 3046, Concerning colour: The effect of environment on type Ia supernova colour in the dark energy survey
     Abstract

     Recent analyses have found intriguing correlations between the colour (c) of type Ia supernovae (SNe Ia) and the size of their 'mass-step', the relationship between SN Ia host galaxy stellar mass (M_stellar) and SN Ia Hubble residual, and suggest that the cause of this relationship is dust. Using 675 photometrically classified SNe Ia from the Dark Energy Survey 5-yr sample, we study the differences in Hubble residual for a variety of global host galaxy and local environmental properties for SN Ia subsamples split by their colour. We find a 3 difference in the mass-step when comparing blue (c < 0) and red (c > 0) SNe. We observe the lowest r.m.s. scatter (~0.14 mag) in the Hubble residual for blue SNe in low mass/blue environments, suggesting that this is the most homogeneous sample for cosmological analyses. By fitting for c-dependent relationships between Hubble residuals and M_stellar, approximating existing dust models, we remove the mass-step from the data and find tentative ~2 residual steps in rest-frame galaxy U - R colour. This indicates that dust modelling based on M_stellar may not fully explain the remaining dispersion in SN Ia luminosity. Instead, accounting for a c-dependent relationship between Hubble residuals and global U - R, results in 1 residual steps in M_stellar and local U - R, suggesting that U - R provides different information about the environment of SNe Ia compared to M_stellar, and motivating the inclusion of galaxy U - R colour in SN Ia distance bias correction.

101. Myles, J., Gruen, D., Amon, A., Alarcon, A., DeRose, J., Everett, S., Dodelson, S., Bernstein, G., Campos, A., Harrison, I., MacCrann, N., McCullough, J., Raveri, M., Sanchez, C., Troxel, M., Yin, B., Abbott, T., Allam, S., Alves, O., Andrade-Oliveira, F., Bertin, E., Brooks, D., Burke, D., Rosell, A., Kind, M., Carretero, J., Cawthon, R., Costanzi, M., da Costa, L., Pereira, M., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gatti, M., Gerdes, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hartley, W., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Lahav, O., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J., Palmese, A., Paz-Chinchon, F., Pieres, A., Malagon, A., Prat, J., Rodriguez-Monroy, M., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Tucker, D., Vincenzi, M., Weaverdyck, N., DES Collaboration, 2023, MNRAS, 519, 1792, Mapping variations of redshift distributions with probability integral transforms
     Abstract

     We present a method for mapping variations between probability distribution functions and apply this method within the context of measuring galaxy redshift distributions from imaging survey data. This method, which we name PITPZ for the probability integral transformations it relies on, uses a difference in curves between distribution functions in an ensemble as a transformation to apply to another distribution function, thus transferring the variation in the ensemble to the latter distribution function. This procedure is broadly applicable to the problem of uncertainty propagation. In the context of redshift distributions, for example, the uncertainty contribution due to certain effects can be studied effectively only in simulations, thus necessitating a transfer of variation measured in simulations to the redshift distributions measured from data. We illustrate the use of PITPZ by using the method to propagate photometric calibration uncertainty to redshift distributions of the Dark Energy Survey Year 3 weak lensing source galaxies. For this test case, we find that PITPZ yields a lensing amplitude uncertainty estimate due to photometric calibration error within 1 per cent of the truth, compared to as much as a 30 per cent underestimate when using traditional methods.

102. Chen, A., Arico, G., Huterer, D., Angulo, R., Weaverdyck, N., Friedrich, O., Secco, L., Hernandez-Monteagudo, C., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Baxter, E., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Brandao-Souza, A., Bridle, S., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chang, C., Chen, R., Chintalapati, P., Choi, A., Cordero, J., Crocce, M., Pereira, M., Davis, C., DeRose, J., Di Valentino, E., Diehl, H., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferte, A., Fosalba, P., Gatti, M., Gaztanaga, E., Giannini, G., Gruen, D., Gruendl, R., Harrison, I., Hartley, W., Herner, K., Hoffmann, K., Huang, H., Huff, E., Jain, B., Jarvis, M., Jeffrey, N., Kacprzak, T., Krause, E., Kuropatkin, N., Leget, P., Lemos, P., Liddle, A., MacCrann, N., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Omori, Y., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Refregier, A., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A., Rykoff, E., Samuroff, S., Sanchez, C., Sanchez, J., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troja, A., Troxel, M., Tutusaus, I., Varga, T., Wechsler, R., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Aguena, M., Annis, J., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carretero, J., Conselice, C., Costanzi, M., da Costa, L., De Vicente, J., Desai, S., Doel, P., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gerdes, D., Giannantonio, T., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Lahav, O., March, M., Marshall, J., Melchior, P., Menanteau, F., Miquel, R., Mohr, J., Morgan, R., Paz-Chinchon, F., Pieres, A., Sanchez, E., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., DES Collaboration, 2023, MNRAS, 518, 5340, Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurements
     Abstract

     We use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package BACCOEMU to accelerate the evaluation of the baryonic non-linear matter power spectrum. We design our analysis pipeline to focus on the constraints of the baryonic suppression effects, utilizing the implication given by a principal component analysis on the Fisher forecasts. Our constraint on the baryonic effects can then be used to better model and ameliorate the effects of baryons in producing cosmological constraints from the next-generation large-scale structure surveys. We detect the baryonic suppression on the cosmic shear measurements with a ~2 significance. The characteristic halo mass for which half of the gas is ejected by baryonic feedback is constrained to be $M_c \gt 10^{13.2} \, h^{-1} \, \mathrm{M}_{\odot }$ (95 per cent C.L.). The best-fitting baryonic suppression is $\sim 5{{\ \rm per\ cent}}$ at $k=1.0 \, {\rm Mpc}\ h^{-1}$ and $\sim 15{{\ \rm per\ cent}}$ at $k=5.0 \, {\rm Mpc} \ h^{-1}$. Our findings are robust with respect to the assumptions about the cosmological parameters, specifics of the baryonic model, and intrinsic alignments.

103. Omori, Y., Baxter, E., Chang, C., Friedrich, O., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Bechtol, K., Becker, M., Bernstein, G., Blazek, J., Bleem, L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Choi, A., Cordero, J., Crawford, T., Crocce, M., Davis, C., DeRose, J., Dodelson, S., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferte, A., Fosalba, P., Gatti, M., Giannini, G., Gruen, D., Gruendl, R., Harrison, I., Herner, K., Huang, H., Huff, E., Huterer, D., Jarvis, M., Krause, E., Kuropatkin, N., Leget, P., Lemos, P., Liddle, A., MacCrann, N., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Pandey, S., Park, Y., Porredon, A., Prat, J., Raveri, M., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A., Rykoff, E., Sanchez, C., Sanchez, J., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Varga, T., Weaverdyck, N., Wechsler, R., Wu, W., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T., Aguena, M., Allam, S., Annis, J., Bacon, D., Benson, B., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carlstrom, J., Carretero, J., Chang, C., Chown, R., Costanzi, M., da Costa, L., Crites, A., Pereira, M., de Haan, T., De Vicente, J., Desai, S., Diehl, H., Dobbs, M., Doel, P., Everett, W., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., George, E., Giannantonio, T., Halverson, N., Hinton, S., Holder, G., Hollowood, D., Holzapfel, W., Honscheid, K., Hrubes, J., James, D., Knox, L., Kuehn, K., Lahav, O., Lee, A., Lima, M., Luong-Van, D., March, M., McMahon, J., Melchior, P., Menanteau, F., Meyer, S., Miquel, R., Mocanu, L., Mohr, J., Morgan, R., Natoli, T., Padin, S., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Pryke, C., Reichardt, C., Romer, A., Ruhl, J., Sanchez, E., Schaffer, K., Schubnell, M., Serrano, S., Shirokoff, E., Smith, M., Staniszewski, Z., Stark, A., Suchyta, E., Tarle, G., Thomas, D., To, C., Vieira, J., Weller, J., Williamson, R., DES, SPT Collaborations, 2023, PhRvD, 107, 023529, Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. I. Construction of CMB lensing maps and modeling choices
     Abstract

     Joint analyses of cross-correlations between measurements of galaxy positions, galaxy lensing, and lensing of the cosmic microwave background (CMB) offer powerful constraints on the large-scale structure of the Universe. In a forthcoming analysis, we will present cosmological constraints from the analysis of such cross-correlations measured using Year 3 data from the Dark Energy Survey (DES), and CMB data from the South Pole Telescope (SPT) and Planck. Here we present two key ingredients of this analysis: (1) an improved CMB lensing map in the SPT-SZ survey footprint and (2) the analysis methodology that will be used to extract cosmological information from the cross-correlation measurements. Relative to previous lensing maps made from the same CMB observations, we have implemented techniques to remove contamination from the thermal Sunyaev Zel'dovich effect, enabling the extraction of cosmological information from smaller angular scales of the cross-correlation measurements than in previous analyses with DES Year 1 data. We describe our model for the cross-correlations between these maps and DES data, and validate our modeling choices to demonstrate the robustness of our analysis. We then forecast the expected cosmological constraints from the galaxy survey-CMB lensing auto and cross-correlations. We find that the galaxy-CMB lensing and galaxy shear-CMB lensing correlations will on their own provide a constraint on S₈=₈{_m/0.3 } at the few percent level, providing a powerful consistency check for the DES-only constraints. We explore scenarios where external priors on shear calibration are removed, finding that the joint analysis of CMB lensing cross-correlations can provide constraints on the shear calibration amplitude at the 5% to 10% level.

104. Chang, C., Omori, Y., Baxter, E., Doux, C., Choi, A., Pandey, S., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Bechtol, K., Becker, M., Bernstein, G., Bianchini, F., Blazek, J., Bleem, L., Camacho, H., Campos, A., Carnero Rosell, A., Carrasco Kind, M., Cawthon, R., Chen, R., Cordero, J., Crawford, T., Crocce, M., Davis, C., DeRose, J., Dodelson, S., Drlica-Wagner, A., Eckert, K., Eifler, T., Elsner, F., Elvin-Poole, J., Everett, S., Fang, X., Ferte, A., Fosalba, P., Friedrich, O., Gatti, M., Giannini, G., Gruen, D., Gruendl, R., Harrison, I., Herner, K., Huang, H., Huff, E., Huterer, D., Jarvis, M., Kovacs, A., Krause, E., Kuropatkin, N., Leget, P., Lemos, P., Liddle, A., MacCrann, N., McCullough, J., Muir, J., Myles, J., Navarro-Alsina, A., Park, Y., Porredon, A., Prat, J., Raveri, M., Rollins, R., Roodman, A., Rosenfeld, R., Ross, A., Rykoff, E., Sanchez, C., Sanchez, J., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troxel, M., Tutusaus, I., Varga, T., Weaverdyck, N., Wechsler, R., Wu, W., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., Abbott, T., Aguena, M., Allam, S., Annis, J., Bacon, D., Benson, B., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carlstrom, J., Carretero, J., Chang, C., Chown, R., Costanzi, M., da Costa, L., Crites, A., Pereira, M., de Haan, T., De Vicente, J., Desai, S., Diehl, H., Dobbs, M., Doel, P., Everett, W., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., George, E., Giannantonio, T., Halverson, N., Hinton, S., Holder, G., Hollowood, D., Holzapfel, W., Honscheid, K., Hrubes, J., James, D., Knox, L., Kuehn, K., Lahav, O., Lee, A., Lima, M., Luong-Van, D., March, M., McMahon, J., Melchior, P., Menanteau, F., Meyer, S., Miquel, R., Mocanu, L., Mohr, J., Morgan, R., Natoli, T., Padin, S., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Pryke, C., Reichardt, C., Rodriguez-Monroy, M., Romer, A., Ruhl, J., Sanchez, E., Schaffer, K., Schubnell, M., Serrano, S., Shirokoff, E., Smith, M., Staniszewski, Z., Stark, A., Suchyta, E., Tarle, G., Thomas, D., To, C., Vieira, J., Weller, J., Williamson, R., DES, SPT Collaborations, 2023, PhRvD, 107, 023530, Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and P l a n c k . II. Cross-correlation measurements and cosmological constraints
     Abstract

     Cross-correlations of galaxy positions and galaxy shears with maps of gravitational lensing of the cosmic microwave background (CMB) are sensitive to the distribution of large-scale structure in the Universe. Such cross-correlations are also expected to be immune to some of the systematic effects that complicate correlation measurements internal to galaxy surveys. We present measurements and modeling of the cross-correlations between galaxy positions and galaxy lensing measured in the first three years of data from the Dark Energy Survey with CMB lensing maps derived from a combination of data from the 2500 deg² SPT-SZ survey conducted with the South Pole Telescope and full-sky data from the Planck satellite. The CMB lensing maps used in this analysis have been constructed in a way that minimizes biases from the thermal Sunyaev Zel'dovich effect, making them well suited for cross-correlation studies. The total signal-to-noise of the cross-correlation measurements is 23.9 (25.7) when using a choice of angular scales optimized for a linear (nonlinear) galaxy bias model. We use the cross-correlation measurements to obtain constraints on cosmological parameters. For our fiducial galaxy sample, which consist of four bins of magnitude-selected galaxies, we find constraints of _m=0.272_-0.052^+0.032 and S₈₈{_m/0.3 }=0.736_-0.028^+0.032 (_m=0.245_-0.044^+0.026 and S₈=0.734_-0.028^+0.035 ) when assuming linear (nonlinear) galaxy bias in our modeling. Considering only the cross-correlation of galaxy shear with CMB lensing, we find _m=0.270_-0.061^+0.043 and S₈=0.740_-0.029^+0.034 . Our constraints on S₈ are consistent with recent cosmic shear measurements, but lower than the values preferred by primary CMB measurements from Planck.

105. Abbott, T., Aguena, M., Alarcon, A., Alves, O., Amon, A., Andrade-Oliveira, F., Annis, J., Ansarinejad, B., Avila, S., Bacon, D., Baxter, E., Bechtol, K., Becker, M., Benson, B., Bernstein, G., Bertin, E., Blazek, J., Bleem, L., Bocquet, S., Brooks, D., Buckley-Geer, E., Burke, D., Camacho, H., Campos, A., Carlstrom, J., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Cawthon, R., Chang, C., Chang, C., Chen, R., Choi, A., Chown, R., Conselice, C., Cordero, J., Costanzi, M., Crawford, T., Crites, A., Crocce, M., da Costa, L., Davis, C., Davis, T., de Haan, T., De Vicente, J., DeRose, J., Desai, S., Diehl, H., Dobbs, M., Dodelson, S., Doel, P., Doux, C., Drlica-Wagner, A., Eckert, K., Eifler, T., Elsner, F., Elvin-Poole, J., Everett, S., Everett, W., Fang, X., Ferrero, I., Ferte, A., Flaugher, B., Fosalba, P., Friedrich, O., Frieman, J., Garcia-Bellido, J., Gatti, M., George, E., Giannantonio, T., Giannini, G., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Halverson, N., Harrison, I., Herner, K., Hinton, S., Holder, G., Hollowood, D., Holzapfel, W., Honscheid, K., Hrubes, J., Huang, H., Huff, E., Huterer, D., Jain, B., James, D., Jarvis, M., Jeltema, T., Kent, S., Knox, L., Kovacs, A., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, A., Leget, P., Lemos, P., Liddle, A., Lidman, C., Luong-Van, D., McMahon, J., MacCrann, N., March, M., Marshall, J., Martini, P., McCullough, J., Melchior, P., Menanteau, F., Meyer, S., Miquel, R., Mocanu, L., Mohr, J., Morgan, R., Muir, J., Myles, J., Natoli, T., Navarro-Alsina, A., Nichol, R., Omori, Y., Padin, S., Pandey, S., Park, Y., Paz-Chinchon, F., Pereira, M., Pieres, A., Plazas Malagon, A., Porredon, A., Prat, J., Pryke, C., Raveri, M., Reichardt, C., Rollins, R., Romer, A., Roodman, A., Rosenfeld, R., Ross, A., Ruhl, J., Rykoff, E., Sanchez, C., Sanchez, E., Sanchez, J., Schaffer, K., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Shirokoff, E., Smith, M., Staniszewski, Z., Stark, A., Suchyta, E., Swanson, M., Tarle, G., To, C., Troxel, M., Tutusaus, I., Varga, T., Vieira, J., Weaverdyck, N., Wechsler, R., Weller, J., Williamson, R., Wu, W., Yanny, B., Yin, B., Zhang, Y., Zuntz, J., DES, SPT Collaborations, 2023, PhRvD, 107, 023531, Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. III. Combined cosmological constraints
     Abstract

     We present cosmological constraints from the analysis of two-point correlation functions between galaxy positions and galaxy lensing measured in Dark Energy Survey (DES) Year 3 data and measurements of cosmic microwave background (CMB) lensing from the South Pole Telescope (SPT) and Planck. When jointly analyzing the DES-only two-point functions and the DES cross-correlations with SPT +P l a n c k CMB lensing, we find _m=0.344 0.030 and S₈₈(_m/0.3 )^0.5=0.773 0.016 , assuming CDM . When additionally combining with measurements of the CMB lensing autospectrum, we find _m=0.306_-0.021^+0.018 and S₈=0.792 0.012 . The high signal-to-noise of the CMB lensing cross-correlations enables several powerful consistency tests of these results, including comparisons with constraints derived from cross-correlations only, and comparisons designed to test the robustness of the galaxy lensing and clustering measurements from DES. Applying these tests to our measurements, we find no evidence of significant biases in the baseline cosmological constraints from the DES-only analyses or from the joint analyses with CMB lensing cross-correlations. However, the CMB lensing cross-correlations suggest possible problems with the correlation function measurements using alternative lens galaxy samples, in particular the REDMAGIC galaxies and high-redshift MAGLIM galaxies, consistent with the findings of previous studies. We use the CMB lensing cross-correlations to identify directions for further investigating these problems.

106. O'Grady, A., Drout, M., Gaensler, B., Kochanek, C., Neugent, K., Doherty, C., Speagle, J., Shappee, B., Rauch, M., Gotberg, Y., Ludwig, B., Thompson, T., 2023, ApJ, 943, 18, Cool, Luminous, and Highly Variable Stars in the Magellanic Clouds. II. Spectroscopic and Environmental Analysis of Thorne-Zytkow Object and Super-AGB Star Candidates
     Abstract

     In previous work, we identified a population of 38 cool and luminous variable stars in the Magellanic Clouds and examined 11 in detail in order to classify them as either Thorne-Zytkow objects (TZOs; red supergiants with a neutron star cores) or super-asymptotic giant branch (sAGB) stars (the most massive stars that will not undergo core collapse). This population includes HV 2112, a peculiar star previously considered in other works to be either a TZO or high-mass asymptotic giant branch (AGB) star. Here we continue this investigation, using the kinematic and radio environments and local star formation history of these stars to place constraints on the age of the progenitor systems and the presence of past supernovae. These stars are not associated with regions of recent star formation, and we find no evidence of past supernovae at their locations. Finally, we also assess the presence of heavy elements and lithium in their spectra compared to red supergiants. We find strong absorption in Li and s-process elements compared to RSGs in most of the sample, consistent with sAGB nucleosynthesis, while HV 2112 shows additional strong lines associated with TZO nucleosynthesis. Coupled with our previous mass estimates, the results are consistent with the stars being massive (~4-6.5 M ) or sAGB (~6.5-12 M ) stars in the thermally pulsing phase, providing crucial observations of the transition between low- and high-mass stellar populations. HV 2112 is more ambiguous; it could either be a maximally massive sAGB star, or a TZO if the minimum mass for stability extends down to 13 M .

107. Morgan, R., Nord, B., Bechtol, K., Moller, A., Hartley, W., Birrer, S., Gonzalez, S., Martinez, M., Gruendl, R., Buckley-Geer, E., Shajib, A., Carnero Rosell, A., Lidman, C., Collett, T., Abbott, T., Aguena, M., Andrade-Oliveira, F., Annis, J., Bacon, D., Bocquet, S., Brooks, D., Burke, D., Carrasco Kind, M., Carretero, J., Castander, F., Conselice, C., da Costa, L., Costanzi, M., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Friedel, D., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Pereira, M., Pieres, A., Plazas Malagon, A., Prat, J., Rodriguez-Monroy, M., Romer, A., Roodman, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., Varga, T., 2023, ApJ, 943, 19, DeepZipper. II. Searching for Lensed Supernovae in Dark Energy Survey Data with Deep Learning
     Abstract

     Gravitationally lensed supernovae (LSNe) are important probes of cosmic expansion, but they remain rare and difficult to find. Current cosmic surveys likely contain 5-10 LSNe in total while next-generation experiments are expected to contain several hundred to a few thousand of these systems. We search for these systems in observed Dark Energy Survey (DES) five year SN fields-10 3 sq. deg. regions of sky imaged in the griz bands approximately every six nights over five years. To perform the search, we utilize the DeepZipper approach: a multi-branch deep learning architecture trained on image-level simulations of LSNe that simultaneously learns spatial and temporal relationships from time series of images. We find that our method obtains an LSN recall of 61.13% and a false-positive rate of 0.02% on the DES SN field data. DeepZipper selected 2245 candidates from a magnitude-limited (m _i < 22.5) catalog of 3,459,186 systems. We employ human visual inspection to review systems selected by the network and find three candidate LSNe in the DES SN fields.

108. Lopez-Valdivia, R., Mace, G., Han, E., Sawczynec, E., Hernandez, J., Prato, L., Johns-Krull, C., Oh, H., Lee, J., Kraus, A., Llama, J., Jaffe, D., 2023, ApJ, 943, 49, The IGRINS YSO Survey. III. Stellar Parameters of Pre-main-sequence Stars in Ophiuchus and Upper Scorpius
     Abstract

     We used the Immersion GRating Infrared Spectrometer (IGRINS) to determine fundamental parameters for 61 K- and M-type young stellar objects (YSOs) located in the Ophiuchus and Upper Scorpius star-forming regions. We employed synthetic spectra and a Markov chain Monte Carlo approach to fit specific K-band spectral regions and determine the photospheric temperature (T), surface gravity ( $\mathrm{log}g$ ), magnetic field strength (B), projected rotational velocity ( $v\sin i$ ), and K-band veiling (r _K ). We determined B for ~46% of our sample. Stellar parameters were compared to the results from Taurus-Auriga and the TW Hydrae association presented in Paper I of this series. We classified all the YSOs in the IGRINS survey with infrared spectral indices from Two Micron All Sky Survey and Wide-field Infrared Survey Explorer photometry between 2 and 24 m. We found that Class II YSOs typically have lower $\mathrm{log}g$ and $v\sin i$ , similar B, and higher K-band veiling than their Class III counterparts. Additionally, we determined the stellar parameters for a sample of K and M field stars also observed with IGRINS. We have identified intrinsic similarities and differences at different evolutionary stages with our homogeneous determination of stellar parameters in the IGRINS YSO survey. Considering $\mathrm{log}g$ as a proxy for age, we found that the Ophiuchus and Taurus samples have a similar age. We also find that Upper Scorpius and TWA YSOs have similar ages, and are more evolved than Ophiuchus/Taurus YSOs.

109. Massey, P., Neugent, K., Ekstrom, S., Georgy, C., Meynet, G., 2023, ApJ, 942, 69, The Time-averaged Mass-loss Rates of Red Supergiants as Revealed by Their Luminosity Functions in M31 and M33
     Abstract

     Mass loss in red supergiants (RSGs) is generally recognized to be episodic, but mass-loss prescriptions fail to reflect this. Evolutionary models show that the total amount of mass lost in this phase determines if these stars evolve to warmer temperatures before undergoing core collapse. The current Geneva evolutionary models mimic episodic mass loss by enhancing the quiescent prescription rates whenever the star's outer layers exceed the Eddington luminosity by a large factor. This results in a 20 M model undergoing 10 more mass loss than it would otherwise, but has little effect on models of lower mass. We can test the validity of this approach observationally by measuring the proportion of high-luminosity RSGs to that predicted by the models. To do this, we use our recent luminosity-limited census of RSGs in M31 and M33, making modest improvements to membership, and adopting extinctions based on the recent panchromatic M31 and M33 Hubble surveys. We then compare the proportions of the highest luminosity RSGs found to that predicted by published Geneva models, as well as to a special set of models computed without the enhanced rates. We find good agreement with the models which include the supra-Eddington enhanced mass loss. The models with lower mass-loss rates predict a larger fraction of high-luminosity RSGs than observed, and thus can be ruled out. We also use these improved data to confirm that the upper luminosity limit of RSGs is $\mathrm{log}L/{L}_{\odot }\sim 5.4$ , regardless of metallicity, using our improved data on M31 and M33 plus previous results on the Magellanic Clouds.

110. Margon, B., Morrell, N., Massey, P., Neugent, K., Williams, R., 2023, ApJ, 942, 85, A Survey for C II Emission-line Stars in the Large Magellanic Cloud. II. Final Results and the Origin of C II Emission in [WC] Spectra
     Abstract

     We present the final results of an imaging and spectroscopic search for stars in the Large Magellanic Cloud (LMC) with C II 7231, 7236 emission lines. The goal is to identify and study [WC11] stars, the coolest of the low-mass Wolf-Rayet sequence, and a subset of central stars of planetary nebulae where the C II lines are known to be especially prominent. A recent serendipitous discovery of an LMC [WC11] raised the possibility that these objects, although difficult to identify, might in fact be more common than previously believed. Several new members of this rare class have been found in this survey. It now seems clear, however, that a significant number of these stars are not hiding among the general [WC] population. We point out that the C II doublet intensity ratio observed in our spectra proves to neatly divide the objects into two distinct groups, with the C II emission likely originating from either the stellar wind or a surrounding nebula. The physics of the C II emission mechanism correctly explains this bifurcation. Spectral subtypes are suggested for most of the objects. The numerous spectroscopic clues now available for these objects should facilitate future detailed modeling.

111. Meldorf, C., Palmese, A., Brout, D., Chen, R., Scolnic, D., Kelsey, L., Galbany, L., Hartley, W., Davis, T., Drlica-Wagner, A., Vincenzi, M., Annis, J., Dixon, M., Graur, O., Lidman, C., Moller, A., Nugent, P., Rose, B., Smith, M., Allam, S., Tucker, D., Asorey, J., Calcino, J., Carollo, D., Glazebrook, K., Lewis, G., Taylor, G., Tucker, B., Kim, A., Diehl, H., Aguena, M., Andrade-Oliveira, F., Bacon, D., Bertin, E., Bocquet, S., Brooks, D., Burke, D., Carretero, J., Carrasco Kind, M., Castander, F., Costanzi, M., da Costa, L., Desai, S., Doel, P., Everett, S., Ferrero, I., Friedel, D., Frieman, J., Garcia-Bellido, J., Gatti, M., Gruen, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., March, M., Marshall, J., Menanteau, F., Miquel, R., Morgan, R., Paz-Chinchon, F., Pereira, M., Plazas Malagon, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., Varga, T., DES Collaboration, 2023, MNRAS, 518, 1985, The Dark Energy Survey Supernova Program results: type Ia supernova brightness correlates with host galaxy dust
     Abstract

     Cosmological analyses with type Ia supernovae (SNe Ia) often assume a single empirical relation between colour and luminosity () and do not account for varying host-galaxy dust properties. However, from studies of dust in large samples of galaxies, it is known that dust attenuation can vary significantly. Here, we take advantage of state-of-the-art modelling of galaxy properties to characterize dust parameters (dust attenuation A_V, and a parameter describing the dust law slope R_V) for 1100 Dark Energy Survey (DES) SN host galaxies. Utilizing optical and infrared data of the hosts alone, we find three key aspects of host dust that impact SN cosmology: (1) there exists a large range (~1-6) of host R_V; (2) high-stellar mass hosts have R_V on average ~0.7 lower than that of low-mass hosts; (3) for a subsample of 81 spectroscopically classified SNe there is a significant (>3) correlation between the Hubble diagram residuals of red SNe Ia and the host R_V that when corrected for reduces scatter by $\sim 13{{\ \rm per\ cent}}$ and the significance of the 'mass step' to ~1. These represent independent confirmations of recent predictions based on dust that attempted to explain the puzzling 'mass step' and intrinsic scatter (_int) in SN Ia analyses.

112. Cheng, T., Dominguez Sanchez, H., Vega-Ferrero, J., Conselice, C., Siudek, M., Aragon-Salamanca, A., Bernardi, M., Cooke, R., Ferreira, L., Huertas-Company, M., Krywult, J., Palmese, A., Pieres, A., Plazas Malagon, A., Carnero Rosell, A., Gruen, D., Thomas, D., Bacon, D., Brooks, D., James, D., Hollowood, D., Friedel, D., Suchyta, E., Sanchez, E., Menanteau, F., Paz-Chinchon, F., Gutierrez, G., Tarle, G., Sevilla-Noarbe, I., Ferrero, I., Annis, J., Frieman, J., Garcia-Bellido, J., Mena-Fernandez, J., Honscheid, K., Kuehn, K., da Costa, L., Gatti, M., Raveri, M., Pereira, M., Rodriguez-Monroy, M., Smith, M., Carrasco Kind, M., Aguena, M., Swanson, M., Weaverdyck, N., Doel, P., Miquel, R., Ogando, R., Gruendl, R., Allam, S., Hinton, S., Dodelson, S., Bocquet, S., Desai, S., Everett, S., Scarpine, V., 2023, MNRAS, 518, 2794, Lessons learned from the two largest Galaxy morphological classification catalogues built by convolutional neural networks
     Abstract

     We compare the two largest galaxy morphology catalogues, which separate early- and late-type galaxies at intermediate redshift. The two catalogues were built by applying supervised deep learning (convolutional neural networks, CNNs) to the Dark Energy Survey data down to a magnitude limit of ~21 mag. The methodologies used for the construction of the catalogues include differences such as the cutout sizes, the labels used for training, and the input to the CNN - monochromatic images versus gri-band normalized images. In addition, one catalogue is trained using bright galaxies observed with DES (i < 18), while the other is trained with bright galaxies (r < 17.5) and 'emulated' galaxies up to r-band magnitude 22.5. Despite the different approaches, the agreement between the two catalogues is excellent up to i < 19, demonstrating that CNN predictions are reliable for samples at least one magnitude fainter than the training sample limit. It also shows that morphological classifications based on monochromatic images are comparable to those based on gri-band images, at least in the bright regime. At fainter magnitudes, i > 19, the overall agreement is good (~95 per cent), but is mostly driven by the large spiral fraction in the two catalogues. In contrast, the agreement within the elliptical population is not as good, especially at faint magnitudes. By studying the mismatched cases, we are able to identify lenticular galaxies (at least up to i < 19), which are difficult to distinguish using standard classification approaches. The synergy of both catalogues provides an unique opportunity to select a population of unusual galaxies.

113. Vincenzi, M., Sullivan, M., Moller, A., Armstrong, P., Bassett, B., Brout, D., Carollo, D., Carr, A., Davis, T., Frohmaier, C., Galbany, L., Glazebrook, K., Graur, O., Kelsey, L., Kessler, R., Kovacs, E., Lewis, G., Lidman, C., Malik, U., Nichol, R., Popovic, B., Sako, M., Scolnic, D., Smith, M., Taylor, G., Tucker, B., Wiseman, P., Aguena, M., Allam, S., Annis, J., Asorey, J., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carretero, J., Castander, F., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Diehl, H., Doel, P., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gruen, D., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T., Lima, M., Maia, M., Marshall, J., Miquel, R., Morgan, R., Ogando, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Reil, K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Suchyta, E., Tarle, G., To, C., Varga, T., Weller, J., Wilkinson, R., DES Collaboration, 2023, MNRAS, 518, 1106, The Dark Energy Survey supernova program: cosmological biases from supernova photometric classification
     Abstract

     Cosmological analyses of samples of photometrically identified type Ia supernovae (SNe Ia) depend on understanding the effects of 'contamination' from core-collapse and peculiar SN Ia events. We employ a rigorous analysis using the photometric classifier SuperNNova on state-of-the-art simulations of SN samples to determine cosmological biases due to such 'non-Ia' contamination in the Dark Energy Survey (DES) 5-yr SN sample. Depending on the non-Ia SN models used in the SuperNNova training and testing samples, contamination ranges from 0.8 to 3.5 per cent, with a classification efficiency of 97.7-99.5 per cent. Using the Bayesian Estimation Applied to Multiple Species (BEAMS) framework and its extension BBC ('BEAMS with Bias Correction'), we produce a redshift-binned Hubble diagram marginalized over contamination and corrected for selection effects, and use it to constrain the dark energy equation-of-state, w. Assuming a flat universe with Gaussian _M prior of 0.311 0.010, we show that biases on w are <0.008 when using SuperNNova, with systematic uncertainties associated with contamination around 10 per cent of the statistical uncertainty on w for the DES-SN sample. An alternative approach of discarding contaminants using outlier rejection techniques (e.g. Chauvenet's criterion) in place of SuperNNova leads to biases on w that are larger but still modest (0.015-0.03). Finally, we measure biases due to contamination on w₀ and w_a (assuming a flat universe), and find these to be <0.009 in w₀ and <0.108 in w_a, 5 to 10 times smaller than the statistical uncertainties for the DES-SN sample.

114. Schmidt, T., Treu, T., Birrer, S., Shajib, A., Lemon, C., Millon, M., Sluse, D., Agnello, A., Anguita, T., Auger-Williams, M., McMahon, R., Motta, V., Schechter, P., Spiniello, C., Kayo, I., Courbin, F., Ertl, S., Fassnacht, C., Frieman, J., More, A., Schuldt, S., Suyu, S., Aguena, M., Andrade-Oliveira, F., Annis, J., Bacon, D., Bertin, E., Brooks, D., Burke, D., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Conselice, C., Costanzi, M., da Costa, L., Pereira, M., De Vicente, J., Desai, S., Doel, P., Everett, S., Ferrero, I., Friedel, D., Garcia-Bellido, J., Gaztanaga, E., Gruen, D., Gruendl, R., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., James, D., Kuehn, K., Lahav, O., Menanteau, F., Miquel, R., Palmese, A., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Prat, J., Rodriguez-Monroy, M., Romer, A., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Tarle, G., To, C., Varga, T., DES Collaboration, 2023, MNRAS, 518, 1260, STRIDES: automated uniform models for 30 quadruply imaged quasars
     Abstract

     Gravitational time delays provide a powerful one-step measurement of H₀, independent of all other probes. One key ingredient in time-delay cosmography are high-accuracy lens models. Those are currently expensive to obtain, both, in terms of computing and investigator time (10⁵-10⁶ CPU hours and ~0.5-1 yr, respectively). Major improvements in modelling speed are therefore necessary to exploit the large number of lenses that are forecast to be discovered over the current decade. In order to bypass this roadblock, we develop an automated modelling pipeline and apply it to a sample of 31 lens systems, observed by the Hubble Space Telescope in multiple bands. Our automated pipeline can derive models for 30/31 lenses with few hours of human time and <100 CPU hours of computing time for a typical system. For each lens, we provide measurements of key parameters and predictions of magnification as well as time delays for the multiple images. We characterize the cosmography-readiness of our models using the stability of differences in the Fermat potential (proportional to time delay) with respect to modelling choices. We find that for 10/30 lenses, our models are cosmography or nearly cosmography grade (<3 per cent and 3-5 per cent variations). For 6/30 lenses, the models are close to cosmography grade (5-10 per cent). These results utilize informative priors and will need to be confirmed by further analysis. However, they are also likely to improve by extending the pipeline modelling sequence and options. In conclusion, we show that uniform cosmography grade modelling of large strong lens samples is within reach.

115. Amon, A., Robertson, N., Miyatake, H., Heymans, C., White, M., DeRose, J., Yuan, S., Wechsler, R., Varga, T., Bocquet, S., Dvornik, A., More, S., Ross, A., Hoekstra, H., Alarcon, A., Asgari, M., Blazek, J., Campos, A., Chen, R., Choi, A., Crocce, M., Diehl, H., Doux, C., Eckert, K., Elvin-Poole, J., Everett, S., Ferte, A., Gatti, M., Giannini, G., Gruen, D., Gruendl, R., Hartley, W., Herner, K., Hildebrandt, H., Huang, S., Huff, E., Joachimi, B., Lee, S., MacCrann, N., Myles, J., Navarro-Alsina, A., Nishimichi, T., Prat, J., Secco, L., Sevilla-Noarbe, I., Sheldon, E., Shin, T., Troster, T., Troxel, M., Tutusaus, I., Wright, A., Yin, B., Aguena, M., Allam, S., Annis, J., Bacon, D., Bilicki, M., Brooks, D., Burke, D., Carnero Rosell, A., Carretero, J., Castander, F., Cawthon, R., Costanzi, M., da Costa, L., Pereira, M., de Jong, J., De Vicente, J., Desai, S., Dietrich, J., Doel, P., Ferrero, I., Frieman, J., Garcia-Bellido, J., Gerdes, D., Gschwend, J., Gutierrez, G., Hinton, S., Hollowood, D., Honscheid, K., Huterer, D., Kannawadi, A., Kuehn, K., Kuropatkin, N., Lahav, O., Lima, M., Maia, M., Marshall, J., Menanteau, F., Miquel, R., Mohr, J., Morgan, R., Muir, J., Paz-Chinchon, F., Pieres, A., Plazas Malagon, A., Porredon, A., Rodriguez-Monroy, M., Roodman, A., Sanchez, E., Serrano, S., Shan, H., Suchyta, E., Swanson, M., Tarle, G., Thomas, D., To, C., Zhang, Y., 2023, MNRAS, 518, 477, Consistent lensing and clustering in a low-S₈ Universe with BOSS, DES Year 3, HSC Year 1, and KiDS-1000
     Abstract

     We evaluate the consistency between lensing and clustering based on measurements from Baryon Oscillation Spectroscopic Survey combined with galaxy-galaxy lensing from Dark Energy Survey (DES) Year 3, Hyper Suprime-Cam Subaru Strategic Program (HSC) Year 1, and Kilo-Degree Survey (KiDS)-1000. We find good agreement between these lensing data sets. We model the observations using the DARK EMULATOR and fit the data at two fixed cosmologies: Planck (S₈ = 0.83), and a Lensing cosmology (S₈ = 0.76). For a joint analysis limited to large scales, we find that both cosmologies provide an acceptable fit to the data. Full utilization of the higher signal-to-noise small-scale measurements is hindered by uncertainty in the impact of baryon feedback and assembly bias, which we account for with a reasoned theoretical error budget. We incorporate a systematic inconsistency parameter for each redshift bin, A, that decouples the lensing and clustering. With a wide range of scales, we find different results for the consistency between the two cosmologies. Limiting the analysis to the bins for which the impact of the lens sample selection is expected to be minimal, for the Lensing cosmology, the measurements are consistent with A = 1; A = 0.91 0.04 (A = 0.97 0.06) using DES+KiDS (HSC). For the Planck case, we find a discrepancy: A = 0.79 0.03 (A = 0.84 0.05) using DES+KiDS (HSC). We demonstrate that a kinematic Sunyaev-Zeldovich-based estimate for baryonic effects alleviates some of the discrepancy in the Planck cosmology. This analysis demonstrates the statistical power of small-scale measurements; however, caution is still warranted given modelling uncertainties and foreground sample selection effects.

116. Fitzmaurice, E., Martin, D., Rodriguez Martinez, R., Vallely, P., Stephan, A., Boley, K., Pogge, R., El-Badry, K., Kunovac, V., Triaud, A., 2023, MNRAS, 518, 636, Spectroscopy of TOI-1259B - an unpolluted white dwarf companion to an inflated warm Saturn
     Abstract

     TOI-1259 consists of a transiting exoplanet orbiting a main-sequence star, with a bound outer white dwarf (WDs) companion. Less than a dozen systems with this architecture are known. We conduct follow-up spectroscopy on the WD TOI-1259B using the Large Binocular Telescope to better characterize it. We observe only strong hydrogen lines, making TOI-1259B a DA WD. We see no evidence of heavy element pollution, which would have been evidence of planetary material around the WD. Such pollution is seen in $\sim 25{-}50{{\ \rm per\ cent}}$ of WDs, but it is unknown if this rate is higher or lower in TOI-1259-like systems that contain a known planet. Our spectroscopy permits an improved WD age measurement of $4.05^{+1.00}_{-0.42}$ Gyr, which matches gyrochronology of the main-sequence star. This is the first of an expanded sample of similar binaries that will allow us to calibrate these dating methods and provide a new perspective on planets in binaries.

117. del Ser, D., Fors, O., del Alcazar, M., Dyachenko, V., Horch, E., Tokovinin, A., Ziegler, C., van Belle, G., Clark, C., Hartman, Z., 2023, MNRAS, 518, 669, TFAW survey II: six newly validated planets and 13 planet candidates from K2
     Abstract

     Searching for Earth-sized planets in data from Kepler's extended mission (K2) is a niche that still remains to be fully exploited. The TFAW survey is an ongoing project that aims to re-analyse all light curves in K2 C1-C8 and C12-C18 campaigns with a wavelet-based detrending and denoising method, and the period search algorithm TLS to search for new transit candidates not detected in previous works. We have analysed a first subset of 24 candidate planetary systems around relatively faint host stars (10.9 < K_p < 15.4) to allow for follow-up speckle imaging observations. Using vespa and TRICERATOPS, we statistically validate six candidates orbiting four unique host stars by obtaining false-positive probabilities smaller than 1 per cent with both methods. We also present 13 vetted planet candidates that might benefit from other, more precise follow-up observations. All of these planets are sub-Neptune-sized with two validated planets and three candidates with sub-Earth sizes, and have orbital periods between 0.81 and 23.98 d. Some interesting systems include two ultra-short-period planets, three multiplanetary systems, three sub-Neptunes that appear to be within the small planet Radius Gap, and two validated and one candidate sub-Earths (EPIC 210706310.01, K2-411 b, and K2-413 b) orbiting metal-poor stars.

118. Lilleengen, S., Petersen, M., Erkal, D., Penarrubia, J., Koposov, S., Li, T., Cullinane, L., Ji, A., Kuehn, K., Lewis, G., Mackey, D., Pace, A., Shipp, N., Zucker, D., Bland-Hawthorn, J., Hilmi, T., S5 Collaboration, 2023, MNRAS, 518, 774, The effect of the deforming dark matter haloes of the Milky Way and the Large Magellanic Cloud on the Orphan-Chenab stream
     Abstract

     It has recently been shown that the Large Magellanic Cloud (LMC) has a substantial effect on the Milky Way's stellar halo and stellar streams. Here, we explore how deformations of the Milky Way and LMC's dark matter haloes affect stellar streams, and whether these effects are observable. In particular, we focus on the Orphan-Chenab (OC) stream which passes particularly close to the LMC and spans a large portion of the Milky Way's halo. We represent the Milky Way-LMC system using basis function expansions that capture their evolution in an N-body simulation. We present the properties of this system, such as the evolution of the densities and force fields of each galaxy. The OC stream is evolved in this time-dependent, deforming potential, and we investigate the effects of the various moments of the Milky Way and the LMC. We find that the simulated OC stream is strongly influenced by the deformations of both the Milky Way and the LMC and that this effect is much larger than current observational errors. In particular, the Milky Way dipole has the biggest impact on the stream, followed by the evolution of the LMC's monopole, and the LMC's quadrupole. Detecting these effects would confirm a key prediction of collisionless, cold dark matter, and would be a powerful test of alternative dark matter and alternative gravity models.

119. Cook, J., Protopapa, S., Dalle Ore, C., Cruikshank, D., Grundy, W., Lisse, C., Schmitt, B., Verbiscer, A., Singer, K., Spencer, J., Stern, S., Weaver, H., 2023, Icar, 389, 115242, Analysis of Charon's spectrum at 2.21- m from New Horizons/LEISA and Earth-based observations
     Abstract

     We examine the 2.21- m band from 19 disk-integrated Charon spectra measured by New Horizons/LEISA in the week leading up to its closest encounter with the Pluto system. These observations cover one Charon rotation period. Additionally, we analyze Charon's 2.21- m band from 22 Earth-based spectra obtained over the last two decades. We measure the equivalent width of the 2.21- m band from all observations and study it as a function of sub-observer longitude. We find no significant variation in the 2.21- m band as Charon rotates. Compared to the same band seen on Nix and Hydra, Charon's 2.21- m band is several times weaker. We attribute the 2.21- m band to NH₄Cl based on the appearance of a weaker band at 2.24- m . Furthermore, we see two never-before-reported absorption features in Charon's spectrum at 1.60 and 1.63- m , which may also be due to NH₄Cl. If NH₃-H₂O-ice mixtures are present on Charon, they must be a small fraction of the disk-average composition to be consistent with the spectrum at 1.99- m .

120. DeMeo, F., Marsset, M., Polishook, D., Burt, B., Binzel, R., Hasegawa, S., Granvik, M., Moskovitz, N., Earle, A., Bus, S., Thomas, C., Rivkin, A., Slivan, S., 2023, Icar, 389, 115264, Isolating the mechanisms for asteroid surface refreshing
     Abstract

     Evidence is seen for young, fresh surfaces among Near-Earth and Main-Belt asteroids even though space-weathering timescales are shorter than the age of the surfaces. A number of mechanisms have been proposed to refresh asteroid surfaces on short timescales, such as planetary encounters, YORP spinup, thermal degradation, and collisions. Additionally, other factors such as grain size effects have been proposed to explain the existence of these "fresh-looking" spectra. To investigate the role each of these mechanisms may play, we collected a sample of visible and near-infrared spectra of 477 near-Earth and Mars Crosser asteroids with similar sizes and compositions - all with absolute magnitude H > 16 and within the S-complex and having olivine to pyroxene (ol/(ol+opx)) ratios >0.65. We taxonomically classify these objects in the Q (fresh) and S (weathered) classes. We find four trends in the Q/S ratio: (1) previous work demonstrated the Q/S ratio increases at smaller sizes down to H 16, but we find a sharp increase near H 19 after which the ratio decreases monotonically. (2) in agreement with many previous studies, the Q/S ratio increases with decreasing perihelion distance, and we find it is non-zero for larger perihelia >1.2AU, (3) as a new finding our work reveals the Q/S ratio has a sharp, significant peak near 5 orbital inclination, and (4) we confirm previous findings that the Q/S ratio is higher for objects that have the possibility of encounter with Earth and Venus versus those that do not, however this finding cannot be distinguished from the perihelion trend. No single resurfacing mechanism can explain all of these trends, so multiple mechanisms are required. YORP spin-up scales with size, thermal degradation is dependent on perihelion, planetary encounters trend with inclination, perihelion and MOID, noting that asteroid-asteroid collisions are also dependent on inclination. It is likely that a combination of all four resurfacing mechanisms are needed to account for all observational trends.

121. Elmegreen, B., Hunter, D., Martinez, Z., Archer, H., Simpson, C., Cigan, P., 2023, IAUS, 373, 93, A search for correlations between turbulence and star formation in LITTLE THINGS and THINGS galaxies
     Abstract

     Azimuthal variations in HI velocity dispersion do not correlate with variations in the star formation rate per unit area, SFR/A, suggesting that local star formation does not increase HI turbulence significantly. These variations are determined for each pixel in HI and FUV maps of THINGS and LITTLE THINGS galaxies by subtracting the average radial profiles from the measured quantities. The kinetic energy density and HI surface density increase slightly with SFR/A, suggesting that feedback goes into pushing the local dense gas around without increasing the velocity dispersion. We suggest that star formation feedback does not promote large-scale stability against gravitational forces through turbulence regulation, and that gravitational energy from recurrent instabilities drives turbulence on galactic scales.

121 publications and 1067 citations in 2023.

121 publications and 1067 citations total.