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J/ApJ/645/955    ChaMP serendipitous galaxy cluster survey    (Barkhouse+, 2006)

ChaMP serendipitous galaxy cluster survey. Barkhouse W.A., Green P.J., Vikhlinin A., Kim D.-W., Perley D., Cameron R., Silverman J., Mossman A., Burenin R., Jannuzi B.T., Kim M., Smith M.G., Smith R.C., Tananbaum H., Wilkes B.J. <Astrophys. J., 645, 955-976 (2006)> =2006ApJ...645..955B
ADC_Keywords: Surveys ; X-ray sources ; Redshifts Keywords: galaxies: clusters: general - surveys - X-rays: galaxies: clusters Abstract: We present a survey of serendipitous extended X-ray sources and optical cluster candidates from the Chandra Multiwavelength Project (ChaMP). Our main goal is to make an unbiased comparison of X-ray and optical cluster detection methods. In 130 archival Chandra pointings covering 13deg2, we use a wavelet decomposition technique to detect 55 extended sources, of which 6 are nearby single galaxies. Our X-ray cluster catalog reaches a typical flux limit of about 10-14ergs/cm2/s, with a median cluster core radius of 21". For 56 of the 130 X-ray fields, we use the ChaMP's deep NOAO 4m MOSAIC g', r', and i' imaging to independently detect cluster candidates using a Voronoi tessellation and percolation (VTP) method. Red-sequence filtering decreases the galaxy fore- and background contamination and provides photometric redshifts to z∼0.7. From the overlapping 6.1deg2 X-ray/optical imaging, we find 115 optical clusters (of which 11% are in the X-ray catalog) and 28 X-ray clusters (of which 46% are in the optical VTP catalog). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 57 55 X-Ray detected extended sources table3.dat 84 55 X-Ray properties of extended sources table4.dat 62 102 VTP clusters with X-ray upper limits table5.dat 91 55 *Published sources near X-ray positions table6.dat 102 102 *Published sources near optical-only detections
Note on table5.dat and table6.dat: Published references acquired from NED.
See also: J/ApJS/150/19 : ChaMP. I. First X-ray source catalog (Kim+, 2004) J/ApJ/618/123 : Hard X-ray-emitting AGNs (Silverman+, 2005) J/ApJ/644/829 : Chandra normal galaxies at intermediate redshift (Kim+, 2006) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 16 A16 --- CXOMP Source Name, JHHMMSS.S+DDMMSS 18- 21 I4 --- ObsID Observation ID 23- 24 I2 h RAh Right ascension (J2000.0) 26- 27 I2 min RAm Right ascension (J2000.0) 29- 32 F4.1 s RAs Right ascension (J2000.0) 34 A1 --- DE- Declination sign (J2000.0) 35- 36 I2 deg DEd Declination (J2000.0) 38- 39 I2 arcmin DEm Declination (J2000.0) 41- 44 F4.1 arcsec DEs Declination (J2000.0) 46- 51 I6 s ExpTime Vignetting-corrected exposure time 53- 57 F5.2 10+20cm-2 NH Galactic NH values (from Stark et al., 1992, See Cat. VIII/28)
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 16 A16 --- CXOMP Source Name (JHHMMSS.s+DDMMSS) 18- 24 F7.2 ct Counts Counts 26- 31 F6.3 10-17W/m2 FX X-ray flux 33- 37 F5.3 10-17W/m2 e_FX rms uncertainty on FX 39- 45 F7.3 10+35W LX ?=- X-ray luminosity, in 10^+42^erg/s (1) 47- 52 F6.3 10+35W e_LX ?=- rms uncertainty on LX 54- 58 F5.2 arcsec rc Source core radius (2) 60- 64 F5.2 arcsec PSF Chandra PSF size at the location of extended X-ray source (3) 66- 70 F5.2 arcmin OAA Off-axis angle 72- 77 F6.4 --- zsp ?=- Spectroscopic redshift (4) 78 A1 --- n_zsp [h] h: Redshift measured from our ChaMP spectroscopic program 80- 84 F5.3 --- z ?=- Red-sequence filtered VTP corrected redshifts (5)
Note (1): Luminosities are calculated from spectroscopic redshifts unless only VTP (Voronoi Tessellation and Percolation) estimates are available. Note (2): Source core radius is estimated from the circular β model fits. The uncertainty in rc is on the order of 10%-20%. Note (3): The PSF is derived from the best-fit analytic relation between the Gaussian sigma of point sources and is similar to the radius encircling 50% of total counts for a monochromatic source at 0.75keV. Note (4): Redshifts obtained from the literature have NED IDs listed in Table 5. Typical spectroscopic redshift uncertainties are 0.0006. Note (5): The dispersion of the VTP (Voronoi Tessellation and Percolation) i redshifts about the spectroscopic values is 0.03.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [BGV2006] Sequential number 5- 8 I4 --- ObsID Observation ID 10- 11 I2 h RAh Right ascension (J2000.0) 13- 14 I2 min RAm Right ascension (J2000.0) 16- 19 F4.1 s RAs Right ascension (J2000.0) 21 A1 --- DE- Declination sign (J2000.0) 22- 23 I2 deg DEd Declination (J2000.0) 25- 26 I2 arcmin DEm Declination (J2000.0) 28- 31 F4.1 arcsec DEs Declination (J2000.0) 33- 37 F5.3 --- z Corrected redshift (1) 38 A1 --- n_z [de] Redshift origin (2) 40- 41 A2 --- l_FX [≤ ] Limit flag on FX 42- 46 F5.3 --- FX X-ray flux (3) 49- 50 A2 --- l_LX [≤ ] Limit flag on LX 51- 56 F6.3 10+35W LX X-ray luminosity, in 10^+42^erg/s (3) 58- 62 F5.2 arcsec PSF Chandra PSF size at the location of optically detected source (4)
Note (1): Corrected redshifts estimated from red-sequence VTP (Voronoi Tessellation and Percolation) unless otherwise noted. Note (2): Note as follows: d = Redshift measurement from NED e = Redshift measurement from ChaMP spectroscopic program Note (3): X-ray fluxes and luminosities are 3σ upper limits for cluster candidates not detected in X-rays. Note (4): The PSF is derived from the best-fit analytic relation between the Gaussian sigma of point sources and is similar to the radius encircling 50% of total counts for a monochromatic source at 0.75keV.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 16 A16 --- CXOMP Source Name (JHHMMSS.s+DDMMSS) 18- 48 A31 --- Name Published ID (1) 50- 88 A39 --- Com Comments (2) 90- 91 I2 arcsec Dist ? Distance from extended X-ray centroid
Note (1): Blank field if published sources >2' from object position. Note (2): Available redshifts tabulated in Table 3.
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 3 I3 --- [BGV2006] Sequential number 5- 35 A31 --- Name Published ID (1) 37-102 A66 --- Com Comments
Note (1): Blank field if published sources >2' from object position.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 05-Oct-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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