TY - JOUR

T1 - The Growth of Intracluster Light in XCS-HSC Galaxy Clusters from $0.1 < z < 0.5$

AU - Furnell, Kate E.

AU - Collins, Chris A.

AU - Kelvin, Lee S.

AU - Baldry, Ivan K.

AU - James, Phil A.

AU - Manolopoulou, Maria

AU - Mann, Robert G.

AU - Giles, Paul A.

AU - Bermeo, Alberto

AU - Hilton, Matthew

AU - Wilkinson, Reese

AU - Romer, A. Kathy

AU - Vergara, Carlos

AU - Bhargava, Sunayana

AU - Stott, John P.

AU - Mayers, Julian

AU - Viana, Pedro

N1 - This is a pre-copy-editing, author-produced PDF of an article accepted for publication in Monthly Notices of the Royal Astronomical Society following peer review. Kate E Furnell, Chris A Collins, Lee S Kelvin, Ivan K Baldry, Phil A James, Maria Manolopoulou, Robert G Mann, Paul A Giles, Alberto Bermeo, Matthew Hilton, Reese Wilkinson, A Kathy Romer, Carlos Vergara, Sunayana Bhargava, John P Stott, Julian Mayers, Pedro Viana, The growth of intracluster light in XCS-HSC galaxy clusters from 0.1 < z < 0.5, Monthly Notices of the Royal Astronomical Society, Volume 502, Issue 2, April 2021, Pages 2419–2437, https://doi.org/10.1093/mnras/stab065 is available online at: https://academic.oup.com/mnras/article/502/2/2419/6081050

PY - 2021/4/30

Y1 - 2021/4/30

N2 - We estimate the Intracluster Light (ICL) component within a sample of 18clusters detected in XMM Cluster Survey (XCS) data using deep ($\sim$26.8 mag) Hyper Suprime Cam Subaru Strategic Program DR1 (HSC-SSP DR1)$i$-band data. We apply a rest-frame ${\mu}_{B} = 25 \\mathrm{mag/arcsec^{2}}$ isophotal threshold to our clusters, belowwhich we define light as the ICL within an aperture of $R_{X,500}$(X-ray estimate of $R_{500}$) centered on the Brightest Cluster Galaxy(BCG). After applying careful masking and corrections for flux lossesfrom background subtraction, we recover $\sim$20% of the ICL flux,approximately four times our estimate of the typical background at thesame isophotal level ($\sim$ 5%). We find that the ICL makes up about$\sim$ 24% of the total cluster stellar mass on average ($\sim$ 41%including the flux contained in the BCG within 50 kpc); this value iswell-matched with other observational studies andsemi-analytic/numerical simulations, but is significantly smaller thanresults from recent hydrodynamical simulations (even when measured in anobservationally consistent way). We find no evidence for any linksbetween the amount of ICL flux with cluster mass, but find a growth rateof $2-4$ for the ICL between $0.1 <z <0.5$. We conclude that theICL is the dominant evolutionary component of stellar mass in clustersfrom $z \sim 1$. Our work highlights the need for a consistent approachwhen measuring ICL alongside the need for deeper imaging, in order tounambiguously measure the ICL across as broad a redshift range aspossible (e.g. 10-year stacked imaging from the Vera C. RubinObservatory).

AB - We estimate the Intracluster Light (ICL) component within a sample of 18clusters detected in XMM Cluster Survey (XCS) data using deep ($\sim$26.8 mag) Hyper Suprime Cam Subaru Strategic Program DR1 (HSC-SSP DR1)$i$-band data. We apply a rest-frame ${\mu}_{B} = 25 \\mathrm{mag/arcsec^{2}}$ isophotal threshold to our clusters, belowwhich we define light as the ICL within an aperture of $R_{X,500}$(X-ray estimate of $R_{500}$) centered on the Brightest Cluster Galaxy(BCG). After applying careful masking and corrections for flux lossesfrom background subtraction, we recover $\sim$20% of the ICL flux,approximately four times our estimate of the typical background at thesame isophotal level ($\sim$ 5%). We find that the ICL makes up about$\sim$ 24% of the total cluster stellar mass on average ($\sim$ 41%including the flux contained in the BCG within 50 kpc); this value iswell-matched with other observational studies andsemi-analytic/numerical simulations, but is significantly smaller thanresults from recent hydrodynamical simulations (even when measured in anobservationally consistent way). We find no evidence for any linksbetween the amount of ICL flux with cluster mass, but find a growth rateof $2-4$ for the ICL between $0.1 <z <0.5$. We conclude that theICL is the dominant evolutionary component of stellar mass in clustersfrom $z \sim 1$. Our work highlights the need for a consistent approachwhen measuring ICL alongside the need for deeper imaging, in order tounambiguously measure the ICL across as broad a redshift range aspossible (e.g. 10-year stacked imaging from the Vera C. RubinObservatory).

KW - Astrophysics - Astrophysics of Galaxies

U2 - 10.1093/mnras/stab065

DO - 10.1093/mnras/stab065

M3 - Journal article

VL - 502

SP - 2419

EP - 2437

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 2

ER -