GALAXY CLUSTERS DISCOVERED WITH A SUNYAEV-ZEL'DOVICH EFFECT SURVEY

“…all motivated by some guess at the underlying threedimensional pressure profile of clusters: a modified version of the Navarro-Frenk-White (NFW; Navarro et al. 1996, 1997) model as suggested in Nagai et al. (2007), numerically integrated along the line of sight to produce a model for the SZ…”

“…all motivated by some guess at the underlying threedimensional pressure profile of clusters: a modified version of the Navarro-Frenk-White (NFW; Navarro et al. 1996, 1997) model as suggested in Nagai et al. (2007), numerically integrated along the line of sight to produce a model for the SZ…”

“In SPT-CL 0517-5430, the cluster that was previously included in the Abell supplementary southern cluster catalog (Abell et al. 1989) and the REFLEX catalog (Böhringer et al. 2004), there is a strong red sequence population apparent in g − r versus r and a peak in the photo-z histogram.”

“A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”

“Observations of the SZ effect, therefore, permit the detection of clusters with a selection function that is nearly redshift-independent (Birkinshaw 1999; Carlstrom et al. 2002).”

“The astrometry of the pointing model is tied to the PMN and SUMSS catalogs (Wright et al. 1994; Mauch et al. 2003) and is accurate to 10 arcsec in the final maps.”

“…drawn from models based on the Borys et al. (2003) counts for dusty protogalaxies and a version of the Toffolatti et al. (1998) counts for radio-loud active galactic nuclei (AGN) modified to match the DASI, CBI, and VSA counts at 30 GHz (Kovac et al. 2002; Mason et al. 2003; Cleary et al. 2005).”

“…threedimensional pressure profile of clusters: a modified version of the Navarro-Frenk-White (NFW; Navarro et al. 1996, 1997) model as suggested in Nagai et al. (2007), numerically integrated along the line of sight to produce a model for the SZ surface brightness; a Gaussian profile; and a…”

“We have used ANNz (Collister & Lahav 2004) photoz’s and color-magnitude diagrams to probe for a cluster galaxy population and to provide rough redshift estimates for each of the SPT systems.”

“Neither of these sources would have been included in the Massive Cluster Survey (Ebeling et al. 2001), which only considered sources in the RASS-BSC.”

“A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”

“Significant SZ detections of previously known clusters have been reported in many tens of X-ray and optically selected galaxy clusters with observations spanning from radio to submillimeter wavelengths (e.g., Jones et al. 2005; Bonamente et al. 2006; Benson et al. 2004; Halverson et al. 2008).”

“The astrometry of the pointing model is tied to the PMN and SUMSS catalogs (Wright et al. 1994; Mauch et al. 2003) and is accurate to 10 arcsec in the final maps.”

“…is a spatially random distribution of sources drawn from models based on the Borys et al. (2003) counts for dusty protogalaxies and a version of the Toffolatti et al. (1998) counts for radio-loud active galactic nuclei (AGN) modified to match the DASI, CBI, and VSA counts at 30 GHz (Kovac et al.…”

“We enhance the signal to noise in the SPT maps for sources with morphologies similar to that expected for SZ galaxy clusters through the application of matched spatial filters (Haehnelt & Tegmark 1996; Herranz et al. 2002a,b; Melin et al. 2006).”

“Galaxy cluster catalogs selected via the SunyaevZel’dovich effect are promising in both respects (Carlstrom et al. 2002; Majumdar & Mohr 2004; Melin et al. 2005).”

“The signal covariance of the primary CMB and undetected point sources is estimated analytically from the best-fit WMAP5 CMB power spectrum (Nolta et al. 2009) and the Borys et al. (2003) model for dusty point sources.”

“The amplitude of the SZ spectral distortion is proportional to the integrated pressure along the line of sight through the cluster, and the relationship between integrated SZ flux and cluster mass is expected to have relatively low scatter (Motl et al. 2005; Nagai 2006; Shaw et al. 2008).”

“The amplitude of the SZ spectral distortion is proportional to the integrated pressure along the line of sight through the cluster, and the relationship between integrated SZ flux and cluster mass is expected to have relatively low scatter (Motl et al. 2005; Nagai 2006; Shaw et al. 2008).”

“We enhance the signal to noise in the SPT maps for sources with morphologies similar to that expected for SZ galaxy clusters through the application of matched spatial filters (Haehnelt & Tegmark 1996; Herranz et al. 2002a,b; Melin et al. 2006).”

“We enhance the signal to noise in the SPT maps for sources with morphologies similar to that expected for SZ galaxy clusters through the application of matched spatial filters (Haehnelt & Tegmark 1996; Herranz et al. 2002a,b; Melin et al. 2006).”

“Significant SZ detections of previously known clusters have been reported in many tens of X-ray and optically selected galaxy clusters with observations spanning from radio to submillimeter wavelengths (e.g., Jones et al. 2005; Bonamente et al. 2006; Benson et al. 2004; Halverson et al. 2008).”

“A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”

“6-5430 (Zhang et al. 2006).”

“(See Section 2.3.4 and Padin et al. (2008) for details.)”

“We enhance the signal to noise in the SPT maps for sources with morphologies similar to that expected for SZ galaxy clusters through the application of matched spatial filters (Haehnelt & Tegmark 1996; Herranz et al. 2002a,b; Melin et al. 2006).”

“Significant SZ detections of previously known clusters have been reported in many tens of X-ray and optically selected galaxy clusters with observations spanning from radio to submillimeter wavelengths (e.g., Jones et al. 2005; Bonamente et al. 2006; Benson et al. 2004; Halverson et al. 2008).”

“A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”

“The amplitude of the SZ spectral distortion is proportional to the integrated pressure along the line of sight through the cluster, and the relationship between integrated SZ flux and cluster mass is expected to have relatively low scatter (Motl et al. 2005; Nagai 2006; Shaw et al. 2008).”

“The power spectrum of this source count distribution is estimated with the formalism in White & Majumdar (2004).”

“…drawn from models based on the Borys et al. (2003) counts for dusty protogalaxies and a version of the Toffolatti et al. (1998) counts for radio-loud active galactic nuclei (AGN) modified to match the DASI, CBI, and VSA counts at 30 GHz (Kovac et al. 2002; Mason et al. 2003; Cleary et al. 2005).”

“Galaxy cluster catalogs selected via the SunyaevZel’dovich effect are promising in both respects (Carlstrom et al. 2002; Majumdar & Mohr 2004; Melin et al. 2005).”

“The instrumental and atmospheric noise properties of the maps are estimated using the two-dimensional power spectrum of jackknife noise maps (Sayers et al. 2009; Halverson et al. 2008).”

“A catalog of clusters with masses and redshifts can be used to constrain the matter density, the density fluctuation amplitude, and the dark energy equation of state (Wang & Steinhardt 1998; Haiman et al. 2001; Holder et al. 2001; Molnar et al. 2004; Wang et al. 2004; Lima & Hu 2007).”

“A deep survey of a relatively small field with the VLA at 8.4 GHz produced what appeared to be a significant flux decrement (Richards et al. 1997).”

“However, subsequent BIMA observations at 30 GHz were found to be inconsistent with the interpretation of the VLA decrement as being due to the SZ effect (Holzapfel et al. 2000).”

“New measurements of the SZ effect toward many individual clusters with unprecedented sensitivity are now becoming available (Staniszewski et al. 2009; Hincks et al. 2009; Plagge et al. 2010).”

“In addition, LSST will identify optical counterparts and provide deep optical imaging for clusters detected in other wavebands (e.g., Staniszewski et al. 2009).”

“…years, SZ observational capability has made spectacular progress, from the first spatially resolved (single–dish) observations of individual objects (Pointecouteau et al. 1999, 2001; Komatsu et al. 1999, 2001) to the first discovery of new clusters with a blind SZ survey (Staniszewski et al. 2009).”

“The bolometer array on the SPT completed a 87 deg2 survey of the sky looking for the detection of galaxy clusters via the Sunyaev–Zel’dovich effect (Staniszewski et al., 2009; Vieira et al., 2010), then later some larger surveys to 770 deg2 (Mocanu et al., 2013); the full survey area completed in…”