Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution

H. Sampaio-Santos; Y. Zhang; R. L.C. Ogando; T. Shin; Jesse B. Golden-Marx; B. Yanny; K. Herner; M. Hilton; A. Choi; M. Gatti; D. Gruen; B. Hoyle; M. M. Rau; J. De Vicente; J. Zuntz; T. M.C. Abbott; M. Aguena; S. Allam; J. Annis; S. Avila; E. Bertin; D. Brooks; D. L. Burke; M. Carrasco Kind; J. Carretero; C. Chang; M. Costanzi; L. N. Da Costa; H. T. Diehl; P. Doel; S. Everett; A. E. Evrard; B. Flaugher; P. Fosalba; J. Frieman; J. García-Bellido; E. Gaztanaga; D. W. Gerdes; R. A. Gruendl; J. Gschwend; G. Gutierrez; S. R. Hinton; D. L. Hollowood; K. Honscheid; D. J. James; M. Jarvis; T. Jeltema; K. Kuehn; N. Kuropatkin; O. Lahav; M. A.G. Maia; M. March; J. L. Marshall; R. Miquel; A. Palmese; F. Paz-Chinchón; A. A. Plazas; E. Sanchez; B. Santiago; V. Scarpine; M. Schubnell; M. Smith; E. Suchyta; G. Tarle; D. L. Tucker; T. N. Varga; R. H. Wechsler; Pagul Amanda; Mohr Joe; Chang Chihway

doi:10.1093/mnras/staa3680

Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution

H. Sampaio-Santos, Y. Zhang, R. L.C. Ogando, T. Shin, Jesse B. Golden-Marx, B. Yanny, K. Herner, M. Hilton, A. Choi, M. Gatti, D. Gruen, B. Hoyle, M. M. Rau, J. De Vicente, J. Zuntz, T. M.C. Abbott, M. Aguena, S. Allam, J. Annis, S. AvilaE. Bertin, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, C. Chang, M. Costanzi, L. N. Da Costa, H. T. Diehl, P. Doel, S. Everett, A. E. Evrard, B. Flaugher, P. Fosalba, J. Frieman, J. García-Bellido, E. Gaztanaga, D. W. Gerdes, R. A. Gruendl, J. Gschwend, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, M. Jarvis, T. Jeltema, K. Kuehn, N. Kuropatkin, O. Lahav, M. A.G. Maia, M. March, J. L. Marshall, R. Miquel, A. Palmese, F. Paz-Chinchón, A. A. Plazas, E. Sanchez, B. Santiago, V. Scarpine, M. Schubnell, M. Smith, E. Suchyta, G. Tarle, D. L. Tucker, T. N. Varga, R. H. Wechsler, Pagul Amanda, Mohr Joe, Chang Chihway

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Abstract

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 ≤ z ≤ 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.

Original language	English
Pages (from-to)	1300-1315
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	501
Issue number	1
DOIs	https://doi.org/10.1093/mnras/staa3680
State	Published - Feb 1 2021
Externally published	Yes

Funding

Funders	Funder number
National Science Foundation	1138766, 240672, 306478, 291329

Keywords

clusters
dark matter
galaxies
galaxies
general
photometry

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10.1093/mnras/staa3680

Cite this

Sampaio-Santos, H., Zhang, Y., Ogando, R. L. C., Shin, T., Golden-Marx, J. 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., ... Chihway, C. (2021). Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution. Monthly Notices of the Royal Astronomical Society, 501(1), 1300-1315. https://doi.org/10.1093/mnras/staa3680

@article{8ca40e661634416cbbd280eb1b7b837f,

title = "Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution",

abstract = "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 ≤ z ≤ 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.",

keywords = "clusters, dark matter, galaxies, galaxies, general, photometry",

author = "H. Sampaio-Santos and Y. Zhang and Ogando, {R. L.C.} and T. Shin and Golden-Marx, {Jesse B.} and B. Yanny and K. Herner and M. Hilton and A. Choi and M. Gatti and D. Gruen and B. Hoyle and Rau, {M. M.} and {De Vicente}, J. and J. Zuntz and Abbott, {T. M.C.} and M. Aguena and S. Allam and J. Annis and S. Avila and E. Bertin and D. Brooks and Burke, {D. L.} and {Carrasco Kind}, M. and J. Carretero and C. Chang and M. Costanzi and {Da Costa}, {L. N.} and Diehl, {H. T.} and P. Doel and S. Everett and Evrard, {A. E.} and B. Flaugher and P. Fosalba and J. Frieman and J. Garc{\'i}a-Bellido and E. Gaztanaga and Gerdes, {D. W.} and Gruendl, {R. A.} and J. Gschwend and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and M. Jarvis and T. Jeltema and K. Kuehn and N. Kuropatkin and O. Lahav and Maia, {M. A.G.} and M. March and Marshall, {J. L.} and R. Miquel and A. Palmese and F. Paz-Chinch{\'o}n and Plazas, {A. A.} and E. Sanchez and B. Santiago and V. Scarpine and M. Schubnell and M. Smith and E. Suchyta and G. Tarle and Tucker, {D. L.} and Varga, {T. N.} and Wechsler, {R. H.} and Pagul Amanda and Mohr Joe and Chang Chihway",

note = "Publisher Copyright: {\textcopyright} 2020 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2021",

month = feb,

day = "1",

doi = "10.1093/mnras/staa3680",

language = "English",

volume = "501",

pages = "1300--1315",

journal = "Monthly Notices of the Royal Astronomical Society",

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Sampaio-Santos, H, Zhang, Y, Ogando, RLC, Shin, T, Golden-Marx, JB, Yanny, B, Herner, K, Hilton, M, Choi, A, Gatti, M, Gruen, D, Hoyle, B, Rau, MM, De Vicente, J, Zuntz, J, Abbott, TMC, Aguena, M, Allam, S, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Carrasco Kind, M, Carretero, J, Chang, C, Costanzi, M, Da Costa, LN, Diehl, HT, Doel, P, Everett, S, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, García-Bellido, J, Gaztanaga, E, Gerdes, DW, Gruendl, RA, Gschwend, J, Gutierrez, G, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Jarvis, M, Jeltema, T, Kuehn, K, Kuropatkin, N, Lahav, O, Maia, MAG, March, M, Marshall, JL, Miquel, R, Palmese, A, Paz-Chinchón, F, Plazas, AA, Sanchez, E, Santiago, B, Scarpine, V, Schubnell, M, Smith, M, Suchyta, E, Tarle, G, Tucker, DL, Varga, TN, Wechsler, RH, Amanda, P, Joe, M & Chihway, C 2021, 'Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution', Monthly Notices of the Royal Astronomical Society, vol. 501, no. 1, pp. 1300-1315. https://doi.org/10.1093/mnras/staa3680

TY - JOUR

T1 - Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution

AU - Sampaio-Santos, H.

AU - Zhang, Y.

AU - Ogando, R. L.C.

AU - Shin, T.

AU - Golden-Marx, Jesse B.

AU - Yanny, B.

AU - Herner, K.

AU - Hilton, M.

AU - Choi, A.

AU - Gatti, M.

AU - Gruen, D.

AU - Hoyle, B.

AU - Rau, M. M.

AU - De Vicente, J.

AU - Zuntz, J.

AU - Abbott, T. M.C.

AU - Aguena, M.

AU - Allam, S.

AU - Annis, J.

AU - Avila, S.

AU - Bertin, E.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Chang, C.

AU - Costanzi, M.

AU - Da Costa, L. N.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Evrard, A. E.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gaztanaga, E.

AU - Gerdes, D. W.

AU - Gruendl, R. A.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Jarvis, M.

AU - Jeltema, T.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Lahav, O.

AU - Maia, M. A.G.

AU - March, M.

AU - Marshall, J. L.

AU - Miquel, R.

AU - Palmese, A.

AU - Paz-Chinchón, F.

AU - Plazas, A. A.

AU - Sanchez, E.

AU - Santiago, B.

AU - Scarpine, V.

AU - Schubnell, M.

AU - Smith, M.

AU - Suchyta, E.

AU - Tarle, G.

AU - Tucker, D. L.

AU - Varga, T. N.

AU - Wechsler, R. H.

AU - Amanda, Pagul

AU - Joe, Mohr

AU - Chihway, Chang

PY - 2021/2/1

Y1 - 2021/2/1

N2 - 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 ≤ z ≤ 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.

AB - 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 ≤ z ≤ 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.

KW - clusters

KW - dark matter

KW - galaxies

KW - general

KW - photometry

UR - http://www.scopus.com/inward/record.url?scp=85100332336&partnerID=8YFLogxK

U2 - 10.1093/mnras/staa3680

DO - 10.1093/mnras/staa3680

M3 - Article

AN - SCOPUS:85100332336

SN - 0035-8711

VL - 501

SP - 1300

EP - 1315

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 1

ER -

Is diffuse intracluster light a good tracer of the galaxy cluster matter distribution

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