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J/A+A/606/A122      Catalogue of X-ray luminous clusters members   (Foex+, 2017)

Comparison of hydrostatic and dynamical masses of distant X-ray luminous galaxy clusters. Foex G., Bohringer H., Chon G. <Astron. Astrophys. 606, A122 (2017)> =2017A&A...606A.122F (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Positional data ; Redshifts Keywords: cosmology: observations - galaxies: clusters: general - galaxies: kinematics and dynamics - X-rays: galaxies: clusters Abstract: A robust determination of galaxy cluster mass is crucial to use them as cosmological probes, or to study the physics governing their formation and evolution. Applying various estimators on well-defined cluster samples is a mandatory step in characterising their respective systematics. Our main goal is to compare the results of three dynamical mass estimators to the X-ray hydrostatic values. Here we focus on massive galaxy clusters at intermediate redshifts z∼0.3. We estimated dynamical masses with the virial theorem, the Jeans equation, and the caustic method using wide-field VIMOS spectroscopy; the hydrostatic masses were obtained previously from XMM-Newton observations.We investigated the role of colour selection and the impact of substructures on the dynamical estimators. Description: Photometric and spectroscopic redshifts of the cluster members for RXCJ0014.3-3023, RXCJ0225.9-4154, RXCJ0516.6-5430, RXCJ0528.9-3927, RXCJ0658.5-5556, RXCJ1131.9-1955, RXCJ1206.2-0848, RXCJ1347.5-114, RXCJ2011.3-5725, and RXCJ2308.3-2011. When a spectroscopic redshift is available, the photometric value is the same. In addition, we provide a quality flag for the spectroscopic redshift (except for redshifts taken from the literature) and an uncertainty on the photometric estimate. We also provide a red-sequence membership flag. Spectroscopic redshifts have a typical uncertainty of 250-300km/s. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 85 10 Presentation of the sample and data sets redshift.dat 52 17293 Position and redshift of 17293 galaxies in ten galaxy clusters (table D1)
See also: J/ApJ/658/865 : Redshifts of galaxies in X-ray-luminous groups (Jeltema+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Cluster name 17- 18 I2 h RAh Right ascension (J2000) (1) 20- 21 I2 min RAm Right ascension (J2000) (1) 23- 26 F4.1 s RAs Right ascension (J2000) (1) 28 A1 --- DE- Declination sign (J2000) (1) 29- 30 I2 deg DEd Declination (J2000) (1) 32- 33 I2 arcmin DEm Declination (J2000) (1) 35- 38 F4.1 arcsec DEs Declination (J2000) (1) 40- 45 F6.4 --- zsp Spectroscopic redshift estimated in this work 47- 52 F6.4 --- e_zsp rms uncertainty on zsp 54- 57 A4 --- Band Available WFI pass bands 59- 61 I3 --- Nz Number of cluster members with a spectroscopic redshift 63- 76 A14 --- AName Alternative name 78- 85 A8 --- Cluster Cluster shorted name as in redshift file
Note (1): Equatorial coordinates of the surface density peak of spectroscopic members.
Byte-by-byte Description of file: redshift.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Cluster Cluster shorted name 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- 38 F6.4 --- zspec ? Spectroscopic redshift 40 I1 --- EZflag [2/4]? EZ flag 42- 45 F4.2 --- zphot ? Photometric redshift 47- 50 F4.2 --- e_zphot ? rms uncertainty on photometric redshift 52 A1 --- RSflag [0/1] Red-sequence membership flag (1)
Note (1): Red-sequence membership flag as follows: 1 = galaxy belongs to the cluster red sequence 0 = galaxy does not belong to the cluster red sequence
Acknowledgements: Gael Foex, foex.gael(at)gmail.com
(End) Gael Foex [MPE, Germany], Patricia Vannier [CDS] 03-Aug-2017
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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