J/ApJS/191/340 Southern Cosmology Survey. II. (Menanteau+, 2010)
Southern Cosmology Survey.
II. Massive optically selected clusters from 70 square degrees of the
Sunyaev-Zel'dovich effect common survey area.
Menanteau F., Hughes J.P., Barrientos L.F., Deshpande A.J., Hilton M.,
Infante L., Jimenez R., Kosowsky A., Moodley K., Spergel D., Verde L.
<Astrophys. J. Suppl. Ser., 191, 340-351 (2010)>
=2010ApJS..191..340M 2010ApJS..191..340M
ADC_Keywords: Clusters, galaxy ; Redshifts ; X-ray sources
Keywords: cosmic background radiation - cosmology: observations -
galaxies: clusters: general - galaxies: distances and redshifts -
large-scale structure of universe
Abstract:
We present a catalog of 105 rich and massive (M>3x1014M☉)
optically selected clusters of galaxies extracted from 70deg2 of
public archival griz imaging from the Blanco 4m telescope acquired
over 45 nights between 2005 and 2007. We use the clusters' optically
derived properties to estimate photometric redshifts, optical
luminosities, richness, and masses. We complement the optical
measurements with archival XMM-Newton and ROSAT X-ray data which
provide additional luminosity and mass constraints on a modest
fraction of the cluster sample. Two of our clusters show clear
evidence for central lensing arcs; one of these has a spectacular
large diameter, nearly complete Einstein Ring surrounding the
brightest cluster galaxy.
Description:
Our cluster analysis is based on all of the public unprocessed imaging
data available for download at the time of writing from the
observations carried out for the Blanco Cosmology Survey (BCS)
proposal. This was a NOAO Large Survey project (05B-0043, PI: Joe
Mohr) that was awarded 45 nights between 2005 and 2007 to carry out
intermediate depth g, r, i, z-band observations on the Cerro Tololo
Inter-American Observatory (CTIO) Blanco 4m telescope using the
8192x8192pixel (0.36deg2) MOSAIC-II camera.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table3.dat 79 44 Optical clusters with M(N200)>3x1014M☉
or M(L200)>3x1014M☉ in the 23hr field
table4.dat 79 61 Optical clusters with M(N200)>3x1014M☉
or M(L200)>3x1014M☉ in the 5hr Field
table5.dat 80 29 Cataloged sources associated with SCS optical
clusters
table6.dat 59 10 Optical clusters with X-ray Counterparts from
the RASS (Voges et al. 1999, Cat. IX/10)
table7.dat 90 7 Optical clusters located within the field of
view of XMM-Newton observations
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See also:
VII/110 : Rich Clusters of Galaxies (Abell+ 1989)
IX/10 : ROSAT All-Sky Bright Source Catalogue (1RXS) (Voges+ 1999)
VIII/81 : Sydney University Molonglo Sky Survey (SUMSS V2.1) (Mauch+ 2008)
B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center,
2009)
J/A+AS/101/259 : Redshifts of southern rich clusters (Galli+ 1993)
J/ApJS/96/343 : Redshifts of rich clusters of galaxies (Quintana+ 1995)
J/AJ/126/119 : Optical and radio data for rich Abell clusters (Rizza+, 2003)
Byte-by-byte Description of file: table3.dat table4.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SCSO]
6- 19 A14 --- SCSO SCS identification (JHHMMSS+DDMMSS; based on
the position of the BCG)
21- 24 F4.2 --- zCl Cluster median photometric redshift (1)
26- 29 F4.2 --- zBCG BCG photometric redshift
31- 35 F5.1 --- Ng Number of galaxies within 1h-1Mpc of the
cluster center
37- 40 F4.1 --- e_Ng Ng uncertainty
42- 46 F5.1 --- Ng200 Cluster richness (2)
48- 51 F4.1 --- e_Ng200 Ng200 uncertainty
53- 58 E6.2 --- L200 Total rest-frame integrated r-band
luminosity in units of 1010h-2L☉ (3)
60- 65 E6.2 --- e_L200 L200 uncertainty
67- 72 E6.2 Msun MN200 Mass relative to Ngal200 (4)
74- 79 E6.2 Msun ML200 Mass relative to L200 (4)
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Note (1): using the members within 250kpc of the center of the cluster.
Note (2): Ngal200 is the number of E and E/S0 galaxies within a given
radius, originally defined by Hansen et al. (2005ApJ...633..122H 2005ApJ...633..122H)
as R200=0.156N0.61Mpch-1Mpc, with colors and luminosities that
satisfy specific conditions for membership.
Note (3): L200 is the total rest-frame integrated r-band luminosity,
k-corrected to z=0.25, of all member galaxies included in Ngal200.
Note (4): We computed the two fitting functions based on L200 and
Ngal200, (see Section 5.2.1 from Reyes et al. 2008MNRAS.390.1157R 2008MNRAS.390.1157R
for full details), which are described as
M(N200,LBCG)=MN0(N200/20)αN_^
(LBCG/L{bar}BCG(N))γN_^
and M(L200,LBCG)=ML0(L200/40)αL_^
(LBCG/{bar}LBCG(L))γL_^,
where M is the mass observational equivalent of M200{bar}ρ
(i.e., the halo mass enclosed within a radius of spherical volume
within which the mean density is 200 times the average density) in
units of 1014M☉, L200 is in units of 1010h-2L☉,
and the LBCG dependence is normalized by its mean value. See section
3.1 for further details.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SCSO]
6- 19 A14 --- SCSO SCS identification (JHHMMSS+DDMMSS)
21- 54 A34 --- Cat Cataloged source(s) associated (1)
56- 58 I3 arcsec Sep Distance to BCG
59 A1 --- x_Sep [ms] Original unit of Sep (for arcmin
or arcsec)
61- 62 I2 arcsec Sep2 ? Distance to BCG for the 2d source
65- 73 A9 --- OType NED object type
75- 80 F6.4 --- z ? NED redshift
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Note (1): We queried the NASA/IPCA Extragalactic Database (NED) for
cataloged clusters from ROSAT, Abell et al. (1989, Cat. VII/110), ACT
(Hincks et al. 2010ApJS..191..423H 2010ApJS..191..423H), and SPT (Staniszewski et al.
2009ApJ...701...32S 2009ApJ...701...32S; Menanteau & Hughes 2009ApJ...694L.136M 2009ApJ...694L.136M) within a
3' radius of the location of each SCS cluster. In some cases, there
was a cataloged galaxy from the Two Micron All Sky Survey (Skrutskie
et al. 2006, Cat. VII/233), which we report if it is within 10" of the
BCG. We also take note of radio sources within 1' of our cluster
positions since these could potentially bias the cluster SZ signal. We
only found radio sources from the Sydney University Molonglo Sky
Survey (SUMSS) at 843MHz (Mauch et al. 2003, Cat. VIII/81). Finally,
we find one unidentified bright X-ray source from the ROSAT All Sky
Survey (RASS; Voges et al. 1999, Cat. IX/10) that is coincident with
one of our clusters.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SCSO]
6- 19 A14 --- SCSO SCS identification (JHHMMSS+DDMMSS)
21- 26 F6.4 --- zCl Cluster redshift
27 A1 --- f_zCl [*] * means NED spectroscopic redshift
29- 32 F4.2 10+20/cm2 NH H column density
34- 38 F5.3 ct/s Rate O.5-2.0keV count rate
40- 44 F5.3 ct/s e_Rate Rate uncertainty
46- 48 F3.1 10+37W Lx 0.5-2.0keV luminosity
50- 52 F3.1 10+37W e_Lx Lx uncertainty
54- 59 E6.2 Msun M200 X-ray mass (1)
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Note (1): X-ray masses within an overdensity of 500 times the critical
density were determined using the LX versus M500 scaling relation
from Vikhlinin et al. (2009ApJ...692.1033V 2009ApJ...692.1033V). These were then converted
to an overdensity of 200 with respect to the average density of the
universe for comparison to the optically derived masses using a simple
multiplicative scaling factor of 1.77.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SCSO]
6- 19 A14 --- SCSO SCS identification (JHHMMSS+DDMMSS)
21- 26 F6.4 --- zCl Cluster redshift (from tables 3 and 4)
27 A1 --- f_zCl [*] * means NED spectroscopic redshift
29- 32 F4.2 10+20/cm2 NH H column density
34- 51 A18 --- Xid X-ray counterpart identification
53- 54 I2 arcsec off ? Offset between the X-ray source and the
optical cluster position
56- 58 A3 --- Ext? [Yes/No ] Extended X-ray source
60- 63 I4 kpc Rad Extraction radius
65- 67 F3.1 arcmin Rad2 Extraction radius in arcmin
69- 74 F6.1 ct/ks Rate 0.5-2.0keV count
76- 79 F4.1 ct/ks e_Rate Rate uncertainty
81- 85 F5.3 10+37W Lx 0.5-2.0keV luminosity in 1044erg/s (1)
87- 90 F4.1 10+14Msun MLx Cluster mass from X-ray luminosity
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Note (1): Luminosities calculated by fitting an absorbed thermal emission
model with a fixed 5keV temperature, except for SCSO J051558-543906,
SCSO J051637-543001, and SCSO J231651-545356 for which there was
enough signal to determine their temperatures (see the text).
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History:
From electronic version of the journal
References:
Menanteau et al. Paper I. 2009ApJ...698.1221M 2009ApJ...698.1221M
Jimenez et al. Paper III. 2009ApJS..181..439J 2009ApJS..181..439J
(End) Emmanuelle Perret [CDS] 17-Jan-2011