Dark Energy Survey Year 1 results: Detection of Intra-cluster Light at Redshift $sim$ 0.25. (arXiv:1812.04004v1 [astro-ph.CO])

Dark Energy Survey Year 1 results: Detection of Intra-cluster Light at Redshift $sim$ 0.25. (arXiv:1812.04004v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_Y/0/1/0/all/0/1">Y. Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yanny_B/0/1/0/all/0/1">B. Yanny</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palmese_A/0/1/0/all/0/1">A. Palmese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruen_D/0/1/0/all/0/1">D. Gruen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+To_C/0/1/0/all/0/1">C. To</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rykoff_E/0/1/0/all/0/1">E. S. Rykoff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Leung_Y/0/1/0/all/0/1">Y. Leung</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Collins_C/0/1/0/all/0/1">C. Collins</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_M/0/1/0/all/0/1">M. Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abbott_T/0/1/0/all/0/1">T. M. C. Abbott</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Annis_J/0/1/0/all/0/1">J. Annis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avila_S/0/1/0/all/0/1">S. Avila</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bertin_E/0/1/0/all/0/1">E. Bertin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brooks_D/0/1/0/all/0/1">D. Brooks</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Burke_D/0/1/0/all/0/1">D. L. Burke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosell_A/0/1/0/all/0/1">A. Carnero Rosell</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kind_M/0/1/0/all/0/1">M. Carrasco Kind</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carretero_J/0/1/0/all/0/1">J. Carretero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cunha_C/0/1/0/all/0/1">C. E. Cunha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+DAndrea_C/0/1/0/all/0/1">C. B. D'Andrea</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Costa_L/0/1/0/all/0/1">L. N. Da Costa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vicente_J/0/1/0/all/0/1">J. De Vicente</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">S. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diehl_H/0/1/0/all/0/1">H. T. Diehl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_J/0/1/0/all/0/1">J. P. Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Doel_P/0/1/0/all/0/1">P. Doel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Drlica_Wagner_A/0/1/0/all/0/1">A. Drlica-Wagner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eifler_T/0/1/0/all/0/1">T. F. Eifler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Evrard_A/0/1/0/all/0/1">A. E. Evrard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Flaugher_B/0/1/0/all/0/1">B. Flaugher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fosalba_P/0/1/0/all/0/1">P. Fosalba</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frieman_J/0/1/0/all/0/1">J. Frieman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+GarcIa_Bellido_J/0/1/0/all/0/1">J. Garc'Ia-Bellido</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gaztanaga_E/0/1/0/all/0/1">E. Gaztanaga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gerdes_D/0/1/0/all/0/1">D. W. Gerdes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gruendl_R/0/1/0/all/0/1">R. A. Gruendl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gschwend_J/0/1/0/all/0/1">J. Gschwend</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gutierrez_G/0/1/0/all/0/1">G. Gutierrez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartley_W/0/1/0/all/0/1">W. G. Hartley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hollowood_D/0/1/0/all/0/1">D. L. Hollowood</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Honscheid_K/0/1/0/all/0/1">K. Honscheid</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoyle_B/0/1/0/all/0/1">B. Hoyle</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_D/0/1/0/all/0/1">D. J. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jeltema_T/0/1/0/all/0/1">T. Jeltema</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuehn_K/0/1/0/all/0/1">K. Kuehn</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kuropatkin_N/0/1/0/all/0/1">N. Kuropatkin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Li_T/0/1/0/all/0/1">T. S. Li</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lima_M/0/1/0/all/0/1">M. Lima</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Maia_M/0/1/0/all/0/1">M. A. G. Maia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+March_M/0/1/0/all/0/1">M. March</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_J/0/1/0/all/0/1">J. L. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Melchior_P/0/1/0/all/0/1">P. Melchior</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menanteau_F/0/1/0/all/0/1">F. Menanteau</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_C/0/1/0/all/0/1">C. J. Miller</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miquel_R/0/1/0/all/0/1">R. Miquel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohr_J/0/1/0/all/0/1">J. J. Mohr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ogando_R/0/1/0/all/0/1">R. L. C. Ogando</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plazas_A/0/1/0/all/0/1">A. A. Plazas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romer_A/0/1/0/all/0/1">A. K. Romer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_E/0/1/0/all/0/1">E. Sanchez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Scarpine_V/0/1/0/all/0/1">V. Scarpine</a>, et al. (11 additional authors not shown)

Using data collected by the Dark Energy Survey (DES), we report the detection
of intra-cluster light (ICL) with $sim300$ galaxy clusters in the redshift
range of 0.2 to 0.3. We design methods to mask detected galaxies and stars in
the images and stack the cluster light profiles, while accounting for several
systematic effects (sky subtraction, instrumental Point Spread Function,
cluster selection effects and residual light in the ICL raw detection from
background and cluster galaxies). The methods allow us to acquire high
signal-to-noise measurements of ICL and central galaxies (CGs), which we
separate with radial cuts. The ICL appears as faint and diffuse extending to at
least 1 Mpc from the cluster center, reaching a surface brightness level of 30
mag/arcsecond$^{2}$. Despite its low surface brightness, the diffuse light
contained in an annulus 30 kpc to 1 Mpc from the center of the CGs appears to
be $sim 3$ times as luminous as the CG light within the inner 30 kpc. ICL and
the cluster central galaxy contribute to $44pm17$% of the total cluster
stellar luminosity within 1 Mpc. The ICL color is overall consistent with that
of the cluster red sequence galaxies, but displays a trend of getting bluer
with increasing radius. The ICL demonstrates an interesting self-similarity
feature — for clusters in different richness ranges, their ICL radial profiles
are similar after scaling with cluster $R_mathrm{200m}$, and the ICL
brightness appears to be a good tracer of the cluster radial mass distribution.
These analyses are based on the DES redMaPPer cluster sample identified in the
first year’s observations. We expect to further apply the methods to larger
cluster samples from future DES data, as well as measuring faint diffuse light
around a variety of galaxies.

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