J/MNRAS/403/2063 SXDF X-ray groups and galaxy clusters (Finoguenov+, 2010)
X-ray groups and clusters of galaxies in the Subaru-XMM deep field.
Finoguenov A., Watson M.G., Tanaka M., Simpson C., Cirasuolo M.,
Dunlop J.S., Peacock J.A., Farrah D., Akiyama M., Ueda Y., Smolcic V.,
Stewart G., Rawlings S., Van Breukelen C., Almaini O., Clewley L.,
Bonfield D.G., Jarvis M.J., Barr J.M., Foucaud S., McLure R.J.,
Sekiguchi K., Egami E.
<Mon. Not. R. Astron. Soc., 403, 2063-2076 (2010)>
=2010MNRAS.403.2063F 2010MNRAS.403.2063F
ADC_Keywords: Surveys ; X-ray sources ; Clusters, galaxy
Keywords: surveys - cosmology: observations - dark matter -
large-scale structure of Universe
Abstract:
We present the results of a search for galaxy clusters in the
Subaru-XMM Deep Field (SXDF). We reach a depth for a total cluster
flux in the 0.5-2keV band of 2x10-15erg/cm2/s over one of the
widest XMM-Newton contiguous raster surveys, covering an area of
1.3deg2. Cluster candidates are identified through a wavelet
detection of extended X-ray emission. The red-sequence technique
allows us to identify 57 cluster candidates. We report on the progress
with the cluster spectroscopic follow-up and derive their properties
based on the X-ray luminosity and cluster scaling relations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 117 57 Catalogue of the SXDF X-ray selected galaxy groups
table2.dat 32 132 *Spectroscopic redshifts of cluster member galaxies
table3.dat 79 6 Properties of extended X-ray emission associated
with radio jets
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Note on table2.dat: Sources identified as
<[FWT2010] DDD.dddddd+DD.dddddd> in Simbad.
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See also:
J/MNRAS/372/741 : SXDF 100µJy catalogue (Simpson+, 2006)
J/ApJS/179/124 : Subaru/XMM-Newton deep survey (SXDS) III. (Ueda+, 2008)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SXDF]
5- 6 I02 --- SXDF [01/89] Cluster number SXDFNNXGG
(<[FWT2010] SXDFNNXGG> in Simbad)
7- 9 A3 --- --- [XGG]
11- 18 F8.5 deg RAdeg Right ascension in decimal degrees (J2000)
20- 27 F8.5 deg DEdeg Declination in decimal degrees (J2000)
29- 33 F5.3 --- zph Photometric redshift (1)
35- 38 F4.2 10-17W/m2 FX Cluster flux in the 0.5-2keV band
40- 43 F4.2 10-17W/m2 e_FX rms uncertainty on FX
45- 50 F6.2 10+35W LX Rest-frame X-ray luminosity in the
0.1-2.4keV band
52- 56 F5.2 10+35W e_LX rms uncertainty on LX
58- 62 F5.2 10+13Msun M200 Estimated total mass (2)
64- 67 F4.2 10+13Msun e_M200 rms uncertainty on M200
69- 71 F3.1 arcmin R200 Radius corresponding to M200
73 I1 --- f.X [1/5] X-ray flag (3)
75- 76 I2 --- N(z) Number of member galaxies inside R200
78- 81 F4.1 --- s.X Significance of the X-ray flux estimate
83- 86 F4.1 --- s.rs Significance of the red sequence
88- 91 F4.2 --- zrs ? Red sequence redshift
93- 96 F4.2 --- E_zrs ? Error on zrs (upper value)
98-101 F4.2 --- e_zrs ? Error on zrs (lower value)
103-106 F4.2 --- zm ? Median photometric redshift of galaxies on
the red sequence
107 A1 --- n_zph [a] a for Stellar halo
109-112 I4 --- Ueda ? Reference to the extended source catalogue
in Ueda et al. (2008,
Cat. J/ApJS/179/124), [UWS2008] NNN
114-117 I4 --- Ueda2 ? Reference to the extended source catalogue
in Ueda et al. (2008,
Cat. J/ApJS/179/124), [UWS2008] NNN
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Note (1): In case there are spectroscopic redshift determinations for the
cluster member galaxies, the median spectroscopic redshift is listed
instead of photometric redshift.
Note (2): computed following Rykoff et al. (2008MNRAS.387L..28R 2008MNRAS.387L..28R) and assuming a
standard evolution of scaling relations: M200*Ez=f(LX*E-1*z)
Note (3): X-ray flags as follows:
1 = objects with high (in general >6) significance of the X-ray flux
estimate, and having a single optical counterpart
2 = low significance detections, for which X-ray centring has a large
uncertainty (up to 30 arcsec), hence a larger weight is given to the
location of the optical counterpart
3 = the clusters for which the photometric redshift of the optical or
near-infrared counterpart is uncertain which is mostly a concern at z>1.2
4 = presence of multiple optical counterparts, whose contribution to
the observed X-ray emission is not possible to separate or rule out
5 = systems with potentially wrong assignment of an optical counterpart
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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2- 10 F9.6 deg RAdeg Right ascension in decimal degrees (J2000)
13- 21 F9.6 deg DEdeg Declination in decimal degrees (J2000)
24- 28 F5.3 --- z Spectroscopic redshift
31- 32 I2 --- SXDF [1/89] Cluster ID
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 4 A4 --- --- [SXDF]
5- 6 I02 --- SXDF [01/89] Host cluster number SXDFNNXGG
(<[FWT2010] SXDFNNXGG> in Simbad)
7- 9 A3 --- --- [XGG]
11- 18 F8.5 deg RAdeg Right ascension in decimal degrees (J2000)
20- 27 F8.5 deg DEdeg Declination in decimal degrees (J2000)
29- 33 F5.3 --- z Photometric redshift (1)
35- 38 F4.2 10-17W/m2 FX Cluster flux in the 0.5-2keV band
40- 43 F4.2 10-17W/m2 e_FX rms uncertainty on FX
45- 49 F5.2 10+35W LX Rest-frame X-ray luminosity in the
0.1-2.4keV band
51- 54 F4.2 10+35W e_LX rms uncertainty on LX
56- 57 I2 --- Simp Simpson et al., 2006, Cat. J/MNRAS/372/741
identification number ([SMR2006] NNNN)
59- 62 F4.2 mJy Fr Flux at 1.4GHz
64- 68 F5.1 10+23W/Hz Lr Radio luminosity at 1.4GHz
70- 73 F4.2 10+23W/Hz e_Lr rms uncertainty on Lr
75- 78 F4.1 --- LX/Lr X-ray to radio luminosity ratio (1)
79 A1 --- n_LX/Lr [a] a when only one radio lobe is used in
the X-ray estimate
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Note (1): (LXνX/Lr/νr)*(1+z)-3.7
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 07-Feb-2012