Access to Astronomical Catalogues

← Click to display the menu
J/A+A/602/A20       Abell 315 spectroscopic dataset             (Biviano+, 2017)

Abell 315: reconciling cluster mass estimates from kinematics, X-ray, and lensing. Biviano A., Popesso P., Dietrich J.P., Zhang Y.-Y., Erfanianfar G., Romaniello M., Sartoris B. <Astron. Astrophys. 602, A20 (2017)> =2017A&A...602A..20B (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, optical ; Redshifts Keywords: galaxies: clusters: individual: Abell 315 - galaxies: kinematics and dynamics Abstract: Determination of cluster masses is a fundamental tool for cosmology. Comparing mass estimates obtained by different probes allows to understand possible systematic uncertainties. Aims. The cluster Abell 315 is an interesting test case, since it has been claimed to be underluminous in X-ray for its mass (determined via kinematics and weak lensing). We have undertaken new spectroscopic observations with the aim of improving the cluster mass estimate, using the distribution of galaxies in projected phase space. We identified cluster members in our new spectroscopic sample. We estimated the cluster mass from the projected phase-space distribution of cluster members using the MAMPOSSt method. In doing this estimate we took into account the presence of substructures that we were able to identify. We identify several cluster substructures. The main two have an overlapping spatial distribution, suggesting a (past or ongoing) collision along the line-of-sight. After accounting for the presence of substructures, the mass estimate of Abell 315 from 14 kinematics is reduced by a factor 4, down to M200=0.8-0.4+0.610+14M. We also find evidence that the cluster mass concentration is unusually low, c200=r200/r-2<1. Using our new estimate of c200 we revise the weak lensing mass estimate down to M200=1.8-0.9+1.710+14M. Our new mass estimates are in agreement with that derived from the cluster X-ray luminosity via a scaling relation, M200=0.9±0.2*1014M. Abell 315 no longer belongs to the class of X-ray underluminous clusters. Its mass estimate was inflated by the presence of an undetected subcluster in collision with the main cluster. Whether the presence of undetected line-of-sight structures can be a general explanation for all X-ray underluminous clusters remains to be explored using a statistically significant sample. Description: Abell 315 was observed at the European Southern Observatory (ESO) Very Large Telescope (VLT) with the VIsible MultiObject Spectrograph (VIMOS). The VIMOS data were acquired using 8 separate pointings, plus 2 additional pointings required to provide the needed redundancy within the central region and to cover the gaps between the VIMOS quadrants. Catalog of galaxies with redshifts in the region of the cluster Abell 315, with flags indicating whether these galaxies are members of the cluster, members of substructures within the cluster, and with probabilities for the cluster members to belong to the main cluster structure. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 52 946 Redshift and membership for 946 galaxies in the Abell 315 cluster field
See also: V/139 : The SDSS Photometric Catalog, Release 9 (Adelman-McCarthy+, 2012) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 5 I5 --- Galaxy Galaxy identification number 7- 8 I2 h RAh Right Ascension (J2000) 10- 11 I2 min RAm Right Ascension (J2000) 13- 17 F5.2 s RAs Right Ascension (J2000) 19 A1 --- DE- Declination sign (J2000) 21 I1 deg DEd Declination (J2000) 23- 24 I2 arcmin DEm Declination (J2000) 26- 29 F4.1 arcsec DEs Declination (J2000) 31- 36 F6.4 --- zSDSS ?=0 Heliocentric redshift from SDSS 38- 43 F6.4 --- zVIMOS ?=0 Heliocentric redshift from VIMOS 45 I1 --- Member [0/1] Cluster membership flag 47 I1 --- Subst [0/1] Cluster substructure flag 49- 52 F4.2 --- Prob Main cluster membership probability
Acknowledgements: Andrea Biviano, biviano(at)
(End) Andrea Biviano [INAF-Trieste], Patricia Vannier [CDS] 24-Mar-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

catalogue service