Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution?
| Autor: | R. L. C. Ogando, Brian Yanny, Enrique Gaztanaga, Antonella Palmese, E. Suchyta, S. Everett, August E. Evrard, M. A. G. Maia, Matt Hilton, Tesla E. Jeltema, A. Choi, J. Carretero, Douglas L. Tucker, Kyler Kuehn, G. Tarle, K. Honscheid, M. Costanzi, Michel Aguena, J. Gschwend, David J. James, M. Carrasco Kind, Ofer Lahav, D. L. Burke, Pablo Fosalba, Scarpine, Markus Rau, Chang Chihway, B. Flaugher, S. Allam, Robert A. Gruendl, T. M. C. Abbott, D. L. Hollowood, David J. Brooks, A. A. Plazas, M. March, Basilio X. Santiago, Ben Hoyle, Josh Frieman, Jesse B. Golden-Marx, J. Annis, J. De Vicente, E. J. Sanchez, Mohr Joe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Santiago Avila, Chihway Chang, Jennifer L. Marshall, F. Paz-Chinchón, Michael Schubnell, H. Sampaio-Santos, Pagul Amanda, Joe Zuntz, M. Smith, Daniel Gruen, T. Shin, D. W. Gerdes, M. Gatti, Samuel Hinton, G. Gutierrez, Risa H. Wechsler, Matt J. Jarvis, Yanxi Zhang, Ramon Miquel, E. Bertin, Peter Doel, K. Herner, H. T. Diehl, Juan Garcia-Bellido |
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| Přispěvatelé: | Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, Jesse B., Yanny, B., Herner, K., Hilton, M., Choi, A., Gatti, M., Gruen, D., Hoyle, B., Rau, M. M., De Vicente, J., Zuntz, J., Abbott, T. M. C., Aguena, M., Allam, S., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carrasco Kind, M., Carretero, J., Chang, C., Costanzi, M., da Costa, L. N., Diehl, H. T., Doel, P., Everett, S., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jarvis, M., Jeltema, T., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., March, M., Marshall, J. L., Miquel, R., Palmese, A., Paz-Chinchón, F., Plazas, A. A., Sanchez, E., Santiago, B., Scarpine, V., Schubnell, M., Smith, M., Suchyta, E., Tarle, G., Tucker, D. L., Varga, T. N., Wechsler, R. H., UAM. Departamento de Física Teórica, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES |
| Rok vydání: | 2020 |
| Předmět: |
galaxies: clusters
Cosmology and Nongalactic Astrophysics (astro-ph.CO) Stellar mass Evolution galaxies: photometry dark matter Astrophysics - Astrophysics of Galaxies Astrophysics - Cosmology and Nongalactic Astrophysics Dark matter FOS: Physical sciences Astrophysics Astrophysics::Cosmology and Extragalactic Astrophysics 01 natural sciences Optical Light Luminosity Clusters Photometry Astrophysics - Astrophysics of Galaxie Clusters: General [Galaxies] Stellar Haloes 0103 physical sciences Cluster (physics) Galaxy formation and evolution Satellite galaxy Galaxies: Photometry Dark Matter Surface brightness General 010303 astronomy & astrophysics Weak gravitational lensing Astrophysics::Galaxy Astrophysics Physics 010308 nuclear & particles physics Dark Energy Survey Física Astronomy and Astrophysics Illustristng Simulations Mass Galaxies Galaxy Space and Planetary Science cluster [galaxies] Astrophysics of Galaxies (astro-ph.GA) Calibration photometry [galaxies] [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] Galaxies: Clusters: General |
| Zdroj: | Mon.Not.Roy.Astron.Soc. Mon.Not.Roy.Astron.Soc., 2021, 501 (1), pp.1300-1315. ⟨10.1093/mnras/staa3680⟩ Biblos-e Archivo. Repositorio Institucional de la UAM instname |
| DOI: | 10.48550/arxiv.2005.12275 |
| Popis: | We explore the relation between diffuse intracluster light (central galaxy included) and the galaxy cluster (baryonic and dark) matter distribution using a sample of 528 clusters at $0.2\leq z \leq 0.35$ found in the Dark Energy Survey (DES) Year 1 data. The surface brightness of the diffuse light shows an increasing dependence on cluster total mass at larger radius, and appears to be self-similar with a universal radial dependence after scaling by cluster radius. We also compare the diffuse light radial profiles to the cluster (baryonic and dark) matter distribution measured through weak lensing and find them to be comparable. The IllustrisTNG galaxy formation simulation, TNG300, offers further insight into the connection between diffuse stellar mass and cluster matter distributions -- the simulation radial profile of the diffuse stellar component does not have a similar slope with the total cluster matter content, although that of the cluster satellite galaxies does. Regardless of the radial trends, the amount of diffuse stellar mass has a low-scatter scaling relation with cluster's total mass in the simulation, out-performing the total stellar mass of cluster satellite galaxies. We conclude that there is no consistent evidence yet on whether or not diffuse light is a faithful radial tracer of the cluster matter distribution. Nevertheless, both observational and simulation results reveal that diffuse light is an excellent indicator of the cluster's total mass. Comment: Accepted on MNRAS |
| Databáze: | OpenAIRE |
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