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2023

1. 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.

2. 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.

3. 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.

3 publications and 0 citations in 2023.

3 publications and 0 citations total.