Galaxy populations study on Clusters of Galaxies detected by the South Pole Telescope Alfredo Zenteno Cerro Tololo Inter-American Observatory September 8, 2015. Soverato, Italy.
Outline! The south Pole Telescope and the SZE Photometric redshifts Galaxy populations Conclusions
SPT Collaboration! John Carlstrom, PI! William Holzapfel Adrian Lee Martin White Sherry Cho Huan Tran Martin Lueker Jared Mehl Christian Reichart Dan Schwan Erik Shirokoff Oliver Zahn Helmuth Spieler John Ruhl Tom Montroy Joe Mohr Gurvan Bazin Shantanu Desai Alex Saro Robert Suhada Sebastian Bocquet Jiayi Liu Alfredo Zenteno Jeff McMahon Jeeseon Song John Carlstrom Steve Padin Stephan Meyer Clem Pryke Wayne Hu Andrey Kravtsov Brad Benson Clarence Chang Tom Crawford Will High Tom Plagge Nils Halverson Matt Dobbs Gil Holder Jonathan Dudley Keith Vanderline Peter Ade 7 October 2011 Mohr - Dark Universe Meeting 4 Joaquin Vieira Abbie Crites Ryan Keisler Lindsey Bleem Jonathan Stricker Erik Leitch Lloyd Knox Jason Dick Antony Stark Chris Stubbs Brian Stalder Jonathan Ruell Alejandro Clocchiatti
The South Pole Telescope Williamson et al 2011! Text - 10m telescope located in the geographical south pole at 2700 m altitude 1 deg FOV 1.1 FWHM beam at 150Ghz 2 pointing accuracy Feb. 16, 2007 first light Nov. 2011 2500 survey complete
from Leon Van Speybroeck Sunyaev-Zel dovich Effect Measured SZ spectrum of A2163 SPT Bands from Ned Wright 9 Promise: clean, low scatter, redshift independent cluster selection technique! Also y is a mass proxy. e.g., Motl et al (2005), Nagai (2006)
The South Pole Telescope Example of a cluster in an SPT map
Blanco Cosmology Survey: First four Blindly selected SPT clusters BCS gri pseudo color images of the SPT detection fields BCS Optical 26 Green circles mark 1 diameter centered on SPT location Staniszewski et al (2009), Zenteno et al (2011)
Cluster Photo-z and Red Galaxy pop Red sequence redshifts High et al (2010), Song et al (2011), Bleem et al. (2015)
The South Pole Telescope: SZ Survey M500c [1014 M h-1 70 ] he Astrophysical Journal Supplement Series, 216:27 (21pp), 2015 February Bleem et al. SPT-SZ 2500 deg2 ROSAT-All sky Planck-DR1 ACT 10 1 0.0 0.5 1.0 1.5 Redshift gure 6. Comparison of the 2500 deg2 SPT-SZ cluster catalog to other X-ray and SZ-selected cluster samples. Here we plot the estimated mass vs. redshift for the 516 ptically confirmed clusters 2from the SPT catalog, 91 clusters from the ACT survey (Marriage et al. 2011; Hasselfield et al. 2013), 809 SZ-selected clusters from the anck survey (Planck Collaboration et al. 2014a), and 740 X-ray clusters selected from the ROSAT all-sky survey (Piffaretti et al. 2011) with M500c! 1 1014 h 1 70 M. We mark 68% confidence lower limits for the redshifts of the three high-redshift SPT systems for which the Spitzer redshift model is poorly constrained (right arrows). We plot clusters in common between SPT and the other data sets (see, e.g., Table 5) at the SPT mass and redshift and, for common clusters in the other data sets, at e mass and redshift of the data set in which the cluster was first reported. While the SPT data provides a nearly mass-limited sample, the cluster samples selected om ROSAT and Planck data are redshift-dependent owing to cosmological dimming of X-ray emission and the dilution of the SZ signal by the large Planck beams, spectively. 14 \odot - 2500 deg surveyed 677 (409) cluster candidates above SN of 4.5 (5): 28% observed with Blanco (Bleem+15). 76 (95)% of SN > 4.5 (5) candidates confirmed but Space- and ground-base OIR imaging 415 clusters discovered for the first time Median mass M500c ~ 3.5 x 10 M Median redshift of 0.55 with highest-z at ~1.4 1.0 angular-scale signal of high-redshift clusters by the large Planck
The South Pole Telescope: SZ Survey M500c [1014 M h-1 70 ] he Astrophysical Journal Supplement Series, 216:27 (21pp), 2015 February Bleem et al. SPT-SZ 2500 deg2 ROSAT-All sky Planck-DR1 ACT 10 Our Sample 1 0.0 0.5 1.0 1.5 Redshift gure 6. Comparison of the 2500 deg2 SPT-SZ cluster catalog to other X-ray and SZ-selected cluster samples. Here we plot the estimated mass vs. redshift for the 516 ptically confirmed clusters from the SPT catalog, 91 clusters from the ACT survey (Marriage et al. 2011; Hasselfield et al. 2013), 809 SZ-selected clusters from the anck survey (Planck Collaboration et al. 2014a), and 740 X-ray clusters selected from the ROSAT all-sky survey (Piffaretti et al. 2011) with M500c! 1 1014 h 1 70 M. We mark 68% confidence lower limits for the redshifts of the three high-redshift SPT systems for which the Spitzer redshift model is poorly constrained (right arrows). We plot clusters in common between SPT and the other data sets (see, e.g., Table 5) at the SPT mass and redshift and, for common clusters in the other data sets, at e mass and redshift of the data set in which the cluster first reported. While the SPT data provides a nearly mass-limited sample, the cluster samples selected 14 was\odot om ROSAT and Planck data are redshift-dependent owing to cosmological dimming of X-ray emission and the dilution of the SZ signal by the large Planck beams, spectively. - 26 most massive systems (Williamson et al. 2011) Mass M500c > 6.0 x 10 M Wide redshift range from 0.1 to 1.13 1.0 angular-scale signal of high-redshift clusters by the large Planck
Details: BCG position == cluster center BCG luminosity set as the bright end limit R200 via SZ mass* Local statistical background subtraction Red-sequence width of \pm 0.22 (3 sigma)** LF fitting done fixing m* to a Single Stellar Population model*** on the band redwards of the 4000A break. RP stacks done simultaneously fitting cg and N(M200) and marginalizing over the *Bocquet et al. (2015) background **Lopez-Cruz (2004) Typical depth of m*+2 at 10 sigma ***Bruzual & Charlot (2003)
GALAXY POPULATIONS: Radial Profile NFW integrated along the line-of-sight Zenteno in prep
GALAXY POPULATIONS: Lum. Function m* If we fit all three parameters of the schechter function
GALAXY POPULATIONS: Lum. Function Stacked LF of the 26 clusters consistent with literature Paolillo+01 Lin+04 Popesso+05 Rudnick+09 etc. Zenteno in prep
GALAXY POPULATIONS: Lum. Function m* evolution with the faint end slope fixed to the stack value Zenteno in prep
GALAXY POPULATIONS: Lum. Function Fixing m* to an SSP model to explore alpha and phi evolution Zenteno in prep
GALAXY POPULATIONS Halo Occupation Number HON200(M*+3) 800 400 200 100 15 10 15 2 x 10-1 h70 [M ] Zenteno in prep
(c) ( 5 5 GALAXY POPULATIONS 4 4 φ*/e2(z) 3 φ*/e2(z) 3 Halo Occupation Number Evolution 2 2 1 1 0 0 800 400 200 HON(m*+3) ratio HON200(M*+3) 2 (d) Fig. 6. Sa There is no sig cating the SSP over this redsh the data with 0.2+0.15 0.15. Pane tent with no ev 1 0.9 0.8 0.7 0.6 0.5 0.4 0.3 0.2 0.1 0.3 0.5 0.7 0.9 1.1 redshift 100 Fig. 5. LF parameter evolution with redshift. As noted before, -1 15 15 10 extracted using the band2 redward x 10 the LFs are of theh4000 70 [MA ] break. We fit a line in each case, marking the allowed 1 region. Panel (a): There is no significant evolution in mag = (m model m ), indicating the SSP model provides a good description of cluster galaxies over this redshift range. Panel (b): Evolution of is sug- Zenteno in prep at high redsh beyond this the case whe SSP model. galaxies, and fitting a line using m fix
CONCLUSIONS: - The spatial distribution of galaxies shows no evidence of evolution. - The most massive clusters in the universe tend to have lower concentrations - LF for red and total population have not change their shape from redshift 1 - larger samples are needed, specially in the high redshift end: DES, see Yuan-Yuan Zhang Talk for a sneak peek!