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J/MNRAS/463/1929      BOSS galaxies in X-ray clusters          (Mehrtens+, 2016)

The XMM Cluster Survey: the halo occupation number of BOSS galaxies in X-ray clusters. Mehrtens N., Romer A.K., Nichol R.C., Collins C.A., Sahlen M., Rooney P.J., Mayers J.A., Bermeo-hernandez A., Bristow M., Capozzi D., Christodoulou L., Comparat J., Hilton M., Hoyle B., Kay S.T., Liddle A.R., Mann R.G., Masters K., Miller C.J., Parejko J.K., Prada F., Ross A.J., Schneider D.P., Stott J.P., Streblyanska A., Viana P.T.P., White M., Wilcox H., Zehavi I. <Mon. Not. R. Astron. Soc., 463, 1929-1943 (2016)> =2016MNRAS.463.1929M (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources Keywords: galaxies: haloes - X-rays: galaxies: clusters Abstract: We present a direct measurement of the mean halo occupation distribution (HOD) of galaxies taken from the eleventh data release (DR11) of the Sloan Digital Sky Survey-III Baryon Oscillation Spectroscopic Survey (BOSS). The HOD of BOSS low-redshift (LOWZ: 0.2<z<0.4) and Constant-Mass (CMASS: 0.43<z<0.7) galaxies is inferred via their association with the dark-matter halos of 174 X-ray-selected galaxy clusters drawn from the XMM Cluster Survey (XCS). Halo masses are determined for each galaxy cluster based on X-ray temperature measurements, and range between log10(M180/M)=13-15. Our directly measured HODs are consistent with the HOD-model fits inferred via the galaxy-clustering analyses of Parejko et al. for the BOSS LOWZ sample and White et al. for the BOSS CMASS sample. Under the simplifying assumption that the other parameters that describe the HOD hold the values measured by these authors, we have determined a best-fit alpha-index of 0.91±0.08 and 1.27+0.03-0.04 for the CMASS and LOWZ HOD, respectively. These alpha-index values are consistent with those measured by White et al. and Parejko et al. In summary, our study provides independent support for the HOD models assumed during the development of the BOSS mock-galaxy catalogues that have subsequently been used to derive BOSS cosmological constraints. Description: The data used in this paper are taken from two main sources: the BOSS (Dawson et al., 2013AJ....145...10D) and the XCS (Romer et al., 2001ApJ...547..594R). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 74 174 The halo occupation distribution of BOSS-galaxies in XCS clusters (0.2<z<0.7)
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 18 A18 --- XCS XMMXCS ID (JHHMMSS.s+DDMMSS.s) 20- 24 F5.3 --- z Mear spectroscopic redshift 26 I1 --- n_z [1/3]? Note on z (1) 28- 32 F5.2 10+14Msun M180 Estimate of the cluster halo mass, M180 (in 1014h-1M_☉ unit) 34- 38 F5.2 10+14Msun e_M180 rms uncertainty on M180 41- 45 F5.2 10+14Msun M180B Best fitting mean halo mass 48- 51 F4.2 Mpc R180 Cluster virial radius, R180 (in h-1Mpc unit) 53- 56 F4.2 Mpc e_R180 rms uncertainty on R180 (in h-1Mpc unit) 59- 62 F4.2 Mpc R180B Best fitting mean virial radius (in h-1Mpc unit) 65- 66 I2 --- HONspec Halo occupation number of BOSS galaxies 68- 70 F3.1 --- E_HONspec Error on HONspec (upper value) 72- 74 F3.1 --- e_HONspec Error on HONspec (lower value)
Note (1): There are seven clusters in our sample where the lower 1-sigma uncertainty bound on the cluster mass and radii lie above the best-fit value. These cases reflect instances where the pdf is sufficiently non-Gaussian that the best-fit peak lies outside the 68 per cent confidence levels. Codes for references for theses clusters: 1 = Valtchanov et al. (2004A&A...423...75V) 2 = McHardy et al. (1998MNRAS.295..641M) 3 = Stocke et al. (1991ApJS...76..813S, Cat. IX/15)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 04-May-2018
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