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2026

1. Tan, C., Drlica-Wagner, A., Pace, A., Cerny, W., Nadler, E., Doliva-Dolinsky, A., Anbajagane, D., Li, T., Simon, J., Vivas, A., Walker, A., Adamow, M., Bechtol, K., Carlin, J., Casey, Q., Chang, C., Chaturvedi, A., Cheng, T., Chiti, A., Choi, Y., Crnojevic, D., Ferguson, P., Gruendl, R., Ji, A., Limberg, G., Medina, G., Mutlu-Pakdil, B., Noel, N., Overdeck, K., Placco, V., Riley, A., Sand, D., Sharp, J., Sherman, N., Stringfellow, G., Wechsler, R., Aguena, M., Allam, S., Alves, O., Bacon, D., Brooks, D., Burke, D., Camilleri, R., Carballo-Bello, J., Carnero Rosell, A., Carretero, J., da Costa, L., da Silva Pereira, M., Davis, T., de Vicente, J., Desai, S., Everett, S., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gruen, D., Gutierrez, G., Herner, K., Hinton, S., Hollowood, D., James, D., Kuehn, K., Lahav, O., Lee, S., Marshall, J., Martinez-Vazquez, C., Massana, P., Mena-Fernandez, J., Miquel, R., Muir, J., Myles, J., Ogando, R., Plazas Malagon, A., Porredon, A., Sanchez, E., Sanchez Cid, D., Sevilla-Noarbe, I., Smith, M., Suchyta, E., Swanson, M., To, C., Tollerud, E., Tucker, D., Vikram, V., Weaverdyck, N., Yamamoto, M., Zenteno, A., Delve Collaboration, Des Collaboration, 2026, ApJ, 1000, 87, DELVE Milky Way Satellite Galaxy Census. I. Satellite Population and Survey Selection Function in DES, DELVE, and Pan-STARRS
   Abstract

   The properties of Milky Way satellite galaxies have important implications for galaxy formation, reionization, and the fundamental physics of dark matter. However, the population of Milky Way satellites includes the faintest known galaxies, and current observations are incomplete. To understand the impact of observational selection effects on the known satellite population, we perform rigorous, quantitative estimates of the Milky Way satellite galaxy detection efficiency in three wide-field survey datasets: the Dark Energy Survey Year 6, the DECam Local Volume Exploration Data Release 3, and the Pan-STARRS1 Data Release 1. Together, these surveys cover 13,600 deg² to g 24.0 and 27,700 deg² to g 22.5, spanning 91% of the high-Galactic-latitude sky (b 15). We apply multiple detection algorithms over the combined footprint and recover 49 known satellites above a strict census detection threshold. To characterize the sensitivity of our census, we run our detection algorithms on a large set of simulated galaxies injected into the survey data, which allows us to develop models that predict the detectability of satellites as a function of their properties. We then fit an empirical model to our data and infer the luminosity function, radial distribution, and sizeluminosity relation of Milky Way satellite galaxies. Our empirical model predicts a total of 26547+79 satellite galaxies with 20 M_V 0, half-light radii of 15 r_1/2, (pc) 3000, and galactocentric distances of 10 D_GC(kpc) 300. We also identify a mild anisotropy in the angular distribution of the observed galaxies, at a significance of 2, which can be attributed to the clustering of satellites associated with the LMC.

2. Zhang, Q., Knight, M., Ye, Q., Schmidt, C., Battams, K., 2026, RNAAS, 10, 57, Preliminary Nucleus Size Estimate for Kreutz Sungrazer C/2026 A1 (MAPS)
   Abstract

   JWST imagery of the approaching Kreutz sungrazer C/2026 A1 (MAPS) appears sufficient to distinguish the comet's nucleus from the surrounding dust. Coma model fitting indicates the morphology is compatible with a 0.4 km diameter nucleuslikely larger than those of the minor Kreutz fragments routinely discovered with coronagraphs, and comparable to or slightly smaller than that of C/2011 W3 (Lovejoy). However, since C/2026 A1 is the only Kreutz sungrazer whose nucleus has been directly observed, these comparisons should be treated with caution.

3. Kilic, Y., Braga-Ribas, F., Pereira, C., Ortiz, J., Sicardy, B., Santos-Sanz, P., Erece, O., Rizos, J., Gomez-Limon, J., Margoti, G., Souami, D., Morgado, B., Gomes-Junior, A., Catani, L., Desmars, J., Kretlow, M., Rommel, F., Duffard, R., Alvarez-Candal, A., Camargo, J., Kaplan, M., Morales, N., Herald, D., Assafin, M., Benedetti-Rossi, G., Sfair, R., Savalle, R., Arcas-Silva, J., Bernasconi, L., Blank, T., Bonavita, M., Carlson, N., Christophe, B., Colesanti, C., Collins, M., Columba, G., Dunford, R., Dunham, D., Dunham, J., Emilio, M., Ferrante, W., George, T., Hanna, W., Isopi, G., Jones, R., Kenyon, D., Kerr, S., Kouprianov, V., Maley, P., Mallia, F., Mattei, J., Meunier, M., Napoleao, T., Peixoto, V., Pollock, J., Snodgrass, C., Stechina, A., Thomas, W., Venable, R., Viscome, G., Zapparata, A., Bardecker, J., Castro, N., Cebral, C., Chapman, A., Gao, C., Green, K., Guimaraes, A., Jacques, C., Jehin, E., Konishi, M., Leiva, R., Liberato, L., Magliano, C., Mammana, L., Melita, M., Moura, V., Olivera-Cuello, Y., Peiro, L., Spagnotto, J., Stuart, P., Vanzi, L., Wilberger, A., Malacarne, M., 2026, A&A, 707, A70, Constraining the size, shape, and albedo of the large trans-Neptunian object (28978) Ixion with multi-chord stellar occultations
   Abstract

   Context. Trans-Neptunian objects (TNOs) are among the most primitive remnants of the early Solar System. Determining their sizes, shapes, albedos, and surface properties is essential for understanding their origin and evolution. Stellar occultations provide highly accurate size and shape information for TNOs, while photometry constrains their albedo and surface colours. (28978) Ixion is one of the largest TNOs and a prominent Plutino, making it a key target for comparative studies. Aims. The aim of this work is to constrain Ixion's projected size, shape, absolute magnitude, geometric albedo, and surface colours, and to search for evidence of an atmosphere or circum-object material. Methods. We conducted a series of campaigns targeting stellar occultations by Ixion between 2020 and 2023 as part of the Lucky Star collaboration, gathering 51 observations from eight events, including 30 positive detections. Five multi-chord events were used for a global limb fit, enabling an accurate reconstruction of Ixion's projected shape. Calibrated photometric data, including new and archival measurements, were analysed to derive its absolute magnitude, phase-curve parameters, and broadband colours. Results. The multi-chord occultations reveal a slightly elongated limb that is well represented by a single projected ellipse with semi-axes a = 363.42_3.85^+3.53 km and b = 333.98_4.96^+7.07 km, yielding R_equiv = 348.39_4.43^+5.37 km (D_equiv = 696.78_8.87^+10.75 km), and an apparent oblateness ' = 0.081_0.010^+0.004. The geometry is consistent with a moderately flattened, nearly spheroidal body that may show slight departures from axial symmetry. The typical radial residuals (~10 km) support a largely stable shape across the observed epochs, with modest epoch-dependent variations. The phase-curve fit gives H_V = 3.845 0.006, = 0.1301 0.0078 mag deg¹, and p_V = 0.106_0.003^+0.003. Multi-band photometry yields B V = 1.06 0.03, V R = 0.61 0.02, and R I = 0.54 0.03, which is consistent with moderately red TNO surfaces. No atmosphere or circum-object material was detected down to our sensitivity limits. The best-sampled event (13 October 2020) also allowed us to measure the angular diameter of the occulted star Gaia DR3 4056440205544338944, = 0.670 0.010 mas, which corresponds to R = 128 10 R at the Gaia distance.

4. Tan, C., Cerny, W., Pace, A., Sharp, J., Overdeck, K., Drlica-Wagner, A., Simon, J., Mutlu-Pakdil, B., Sand, D., Senkevich, A., Erkal, D., Ferguson, P., Sobreira, F., Atzberger, K., Carlin, J., Chiti, A., Crnojevic, D., Ji, A., Johnson, L., Li, T., Limberg, G., Martinez-Vazquez, C., Medina, G., Placco, V., Riley, A., Tollerud, E., Vivas, A., Abbott, T., Aguena, M., Alves, O., Bacon, D., Bocquet, S., Brooks, D., Burke, D., Camilleri, R., Carballo-Bello, J., Carnero Rosell, A., Carretero, J., Cheng, T., Choi, Y., da Costa, L., da Silva Pereira, M., Davis, T., de Vicente, J., Desai, S., Doel, P., Everett, S., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gruen, D., Gutierrez, G., Hinton, S., Hollowood, D., James, D., Kuehn, K., Lee, S., Marshall, J., Mena-Fernandez, J., Menanteau, F., Miquel, R., Myles, J., Navabi, M., Nidever, D., Noel, N., Ogando, R., Plazas Malagon, A., Porredon, A., Samuroff, S., Sanchez, E., Sanchez Cid, D., Sevilla-Noarbe, I., Smith, M., Stringfellow, G., Suchyta, E., Swanson, M., Vikram, V., Walker, A., Zenteno, A., Delve Collaboration, Des Collaboration, 2026, ApJ, 1000, 46, Ultra-faint Milky Way Satellites Discovered in Carina, Phoenix, and Telescopium with DELVE Data Release 3
   Abstract

   We report the discovery of three Milky Way satellite candidates: Carina IV, Phoenix III, and DELVE 7, in the third data release of the DECam Local Volume Exploration survey (DELVE). The candidate systems were identified by cross-matching results from two independent search algorithms. All three are extremely faint systems composed of old, metal-poor stellar populations ( 10 Gyr, [Fe/H] 1.4). Carina IV (M_V = 2.8; r_1/2 = 40 pc) and Phoenix III (M_V = 1.2; r_1/2 = 19 pc) have half-light radii that are consistent with the known population of dwarf galaxies, while DELVE 7 (M_V = 1.2; r_1/2 = 2 pc) is very compact and seems more likely to be a star cluster, though its nature remains ambiguous without spectroscopic follow-up. The Gaia proper motions of stars in Carina IV ( M=2250830+1180M ) indicate that it is unlikely to be associated with the LMC, while DECam CaHK photometry confirms that its member stars are metal poor. Phoenix III ( M=520290+660M ) is the faintest known satellite in the extreme outer stellar halo (D_GC > 100 kpc), while DELVE 7 ( M=6040+120M ) is the faintest known satellite with D_GC > 20 kpc.

5. Godoy-Rivera, D., Grossmann, D., Richey-Yowell, T., Santos, A., Mathur, S., Garcia, R., 2026, RNAAS, 10, 53, Mining the Kepler Field: Atmospheric Parameters, Bolometric Corrections, and Luminosities
   Abstract

   The 200,000 stars observed by the Kepler mission have provided unprecedented constraints across astrophysics. With the advent of modern spectroscopic and photometric surveys, new limits in stellar characterizations are within reach. In this work, we report a compilation of atmospheric parameters (T_eff, log(g) , and [M/H]) for the Kepler stars by crossmatching with several spectroscopic and spectro-photometric surveys. We use these to calculate bolometric corrections, which combined with colormagnitude diagram information from Gaia yield self-consistent luminosities on a survey-by-survey basis. These properties will aid in future explorations of Kepler data toward new astrophysical insights. We make our catalog publicly available online in Zenodo (doi:10.5281/zenodo.18620911).

6. Brasseur, C., Jardine, M., Daley-Yates, S., Donati, J., Morin, J., 2026, MNRAS, 546, stag042, Electron cyclotron maser emission from ejected stellar prominences on V374 Peg
   Abstract

   We investigate a possible origin for bursty radio emission observed on the active M dwarf V374 Peg, combining data-driven magnetic field modelling with archival radio light curves. We examine whether stellar prominence ejection can plausibly account for the observed radio bursts that have been attributed to electron cyclotron maser (ECM) emission. Our analysis shows that ejected prominences can produce the required energy range to drive the emission, and that modelled ECM visibility exhibits a rotational phase dependence consistent with the limited observational data (four observed bursts). The results support prominence ejection as a viable mechanism for ECM generation on V374 Peg and motivate further observational campaigns to constrain this process.

7. Hoppe, R., Bergemann, M., Eitner, P., Ellwarth, M., Nordlund, A., Leenaarts, J., Plez, B., Serenelli, A., 2026, MNRAS, 546, staf2085, Solar carbon abundance from 3D non-LTE modelling of the diagnostic lines of the CH molecule
   Abstract

   The spectral lines of the CH molecule are a key carbon (C) abundance diagnostic in FGKM-type stars. These lines are detectable in metal-rich and, in contrast to atomic C lines, also in metal-poor late-type stars. However, only 3D LTE analyses of the CH lines have been performed so far. We test the formation of CH lines in the solar spectrum, using for the first time, 3D Non-LTE (NLTE) models. We also aim to derive the solar photospheric abundance of C, using the diagnostic transitions in the optical (4218$4356 \,\rm{\mathring{\rm A}}$) and infrared (33025$37944 \,\rm{\mathring{\rm A}}$). We use the updated NLTE model molecule from S. A. Popa et al. (2023) and different solar 3D radiation-hydrodynamics model atmospheres. The models are contrasted against new spatially resolved optical solar spectra, and the centre-to-limb variation (CLV) of CH lines is studied. We find generally small ($\sim$0.01 dex) NLTE effects in the optical and IR diagnostic CH AX lines in the solar atmosphere. Both 3D NLTE and 3D LTE spectral modelling yield an excellent fit to the solar intensity observations at all viewing angles. The 1D LTE and 1D NLTE models fail to describe the line CLV, and lead to underestimated solar C abundances. The 3D NLTE modelling of diagnostic lines in the optical and IR yields a carbon abundance of A(C) = $8.52\pm 0.07$ dex. The estimate is in agreement with recent results based on neutrino fluxes measured by Borexino. 3D NLTE modelling and tests on spatially resolved solar data are essential to derive robust solar abundances. The analysis presented here focuses on CH, but we expect that similar effects will be present for other molecules of astrophysical interest.

7 publications and 12 citations in 2026.

7 publications and 12 citations total.