Euclid: Early Release Observations – Overview of the Perseus cluster and analysis of its luminosity and stellar mass functions
arxiv(2024)
摘要
The Euclid ERO programme targeted the Perseus cluster of galaxies, gathering
deep data in the central region of the cluster over 0.7 square degree,
corresponding to approximately 0.25 r_200. The data set reaches a point-source
depth of IE=28.0 (YE, JE, HE = 25.3) AB magnitudes at 5 sigma with a 0.16" and
0.48" FWHM, and a surface brightness limit of 30.1 (29.2) mag per square
arcsec. The exceptional depth and spatial resolution of this wide-field
multi-band data enable the simultaneous detection and characterisation of both
bright and low surface brightness galaxies, along with their globular cluster
systems, from the optical to the NIR. This study advances beyond previous
analyses of the cluster and enables a range of scientific investigations
summarised here. We derive the luminosity and stellar mass functions (LF and
SMF) of the Perseus cluster in the Euclid IE band, thanks to supplementary
u,g,r,i,z and Halpha data from the CFHT. We adopt a catalogue of 1100 dwarf
galaxies, detailed in the corresponding ERO paper. We identify all other
sources in the Euclid images and obtain accurate photometric measurements using
AutoProf or AstroPhot for 138 bright cluster galaxies, and SourceExtractor for
half a million compact sources. Cluster membership for the bright sample is
determined by calculating photometric redshifts with Phosphoros. Our LF and SMF
are the deepest recorded for the Perseus cluster, highlighting the
groundbreaking capabilities of the Euclid telescope. Both the LF and SMF fit a
Schechter plus Gaussian model. The LF features a dip at M(IE)=-19 and a
faint-end slope of alpha_S = -1.2 to -1.3. The SMF displays a low-mass-end
slope of alpha_S = -1.2 to -1.35. These observed slopes are flatter than those
predicted for dark matter halos in cosmological simulations, offering
significant insights for models of galaxy formation and evolution.
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