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J/ApJ/791/128   Basic galaxy data for spiral-rich group members  (Stocke+, 2014)

Absorption-line detections of 105-106 K gas in spiral-rich groups of galaxies. Stocke J.T., Keeney B.A., Danforth C.W., Syphers D., Yamamoto H., Shull J.M., Green J.C., Froning C., Savage B.D., Wakker B., Kim T.-S., Ryan-Weber E.V., Kacprzak G.G. <Astrophys. J., 791, 128 (2014)> =2014ApJ...791..128S (SIMBAD/NED BibCode)
ADC_Keywords: Galaxy catalogs ; Clusters, galaxy ; QSOs ; Redshifts Keywords: cosmological parameters - cosmology: observations - galaxies: halos galaxies: spiral - galaxies: structure - intergalactic medium quasars: absorption lines - ultraviolet: general Abstract: Using the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope, the COS Science Team has conducted a high signal-to-noise survey of 14 bright QSOs. In a previous paper (Savage et al., 2014ApJS..212....8S), these far-UV spectra were used to discover 14 "warm" (T ≥ 105 K) absorbers using a combination of broad Lyα and broad O VI absorptions. A reanalysis of a few of this new class of absorbers using slightly relaxed fitting criteria finds as many as 20 warm absorbers could be present in this sample. A shallow, wide spectroscopic galaxy redshift survey has been conducted around these sight lines to investigate the warm absorber environment, which is found to be spiral-rich groups or cluster outskirts with radial velocity dispersions σ=250-750 km/s. While 2σ evidence is presented favoring the hypothesis that these absorptions are associated with the galaxy groups and not with the individual, nearest galaxies, this evidence has considerable systematic uncertainties and is based on a small sample size so it is not entirely conclusive. If the associations are with galaxy groups, the observed frequency of warm absorbers (idN/dz = 3.5-5 per unit redshift) requires them to be very extended as an ensemble on the sky (∼1 Mpc in radius at high covering factor). Most likely these warm absorbers are interface gas clouds whose presence implies the existence of a hotter (T ∼ 106.5 K), diffuse, and probably very massive (>1011 M) intra-group medium which has yet to be detected directly. Description: In order to determine the galaxy environment of the warm and cool absorbers (see Tables 2-4 for a summary of observed properties of the warm and cool absorbers considered here), we have used a combination of large-area redshift surveys like the Sloan Digital Sky Survey (SDSS) and the 2dF survey done at the Anglo-Australian Telescope (AAT) and our own MOS program centered on the sight lines observed by the COS Science Team. Our new observations include all but one of the 14 sight lines in Paper I (Savage et al., 2014ApJS..212....8S) and extend ∼2-3 mag deeper than the SDSS (B.A. Keeney et al. 2014, in preparation). For these 14 sight lines, spectra and redshifts were obtained mostly at the Wisconsin-Indiana-Yale-NOAO (WIYN) 3.5 m telescope using the HYDRA MOS. Additional observations of southern targets were obtained at the Cerro Tololo Inter-American Observatory's (CTIO) 4 m Blanco Telescope using the version of HYDRA available there. A few additional southern targets were observed at the AAT using the AAOmega MOS system. Occasional long-slit spectra of galaxies nearest to absorbers were obtained at the Apache Point Observatory (APO) 3.5 m telescope using the Dual-Imaging Spectrograph. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table13.dat 80 161 Galaxy Group Members near 3C 273 (z_abs = 0.00336) table14.dat 80 24 Galaxy Group Members near Mrk 290 (z_abs = 0.01027) table15.dat 80 126 Galaxy Group Members near PHL 1811 (z_abs = 0.07773) table16.dat 80 30 Galaxy Group Members near PHL 1811 (z_abs = 0.13280) table17.dat 80 13 Galaxy Group Members near PG 0953+414 (z_abs = 0.00212) table18.dat 80 21 Galaxy Group Members near HE 0226-4110 (z_abs = 0.01750) table19.dat 80 23 Galaxy Group Members near PG 1259+593 (z_abs = 0.04625) table20.dat 80 16 Galaxy Group Members near PG 1116+215 (z_abs = 0.05897) table21.dat 80 14 Galaxy Group Members near PG 0953+414 (z_abs = 0.06808) table22.dat 80 8 Galaxy Group Members near PKS 2155-304 (z_abs = 0.05422) table23.dat 80 8 Galaxy Group Members near PKS 2155-304 (z_abs = 0.05722) table24.dat 80 13 Galaxy Group Members near 3C 273 (z_abs = 0.09010) table25.dat 80 7 Galaxy Group Members near 3C 263 (z_abs = 0.11389)
See also: J/A+A/316/123 : QSO absorber and galaxy evolution (Lindner+ 1996) J/AJ/112/62 : Quasar absorption-line systems (Tanner+ 1996) J/A+A/412/707 : Absorption-line systems in QSO spectra - CoALS (Ryabinkov+, 2003) J/AJ/125/1711 : Broad Absorption Line Quasars from SDSS (Reichard+, 2003) J/MNRAS/410/860 : Redshift dependence of BAL QSOs (Allen+, 2011) J/ApJ/814/150 : Variability of SDSS broad absorption line QSOs (Wang+, 2015) J/A+A/590/A68 : AGN data and absorption-line measurements (Richter+, 2016) Byte-by-byte Description of file: table1[3456789].dat table2[012345].dat
Bytes Format Units Label Explanations
1- 17 A17 --- Name Galaxy name 19- 20 I2 h RAh Hour of Right Ascension (J2000) 22- 23 I2 min RAm Minute of Right Ascension (J2000) 25- 29 F5.2 s RAs Second of Right Ascension (J2000) 31 A1 --- DE- Sign of the Declination (J2000) 32- 33 I2 deg DEd Degree of Declination (J2000) 35- 36 I2 arcmin DEm Arcminute of Declination (J2000) 38- 41 F4.1 arcsec DEs Arcsecond of Declination (J2000) 43- 49 A7 --- Source Source for the redshift (Catalog, SDSS, HYDRA, AAT) (1) 51- 57 F7.5 --- z Heliocentric redshift (±30 km/s) 59- 63 F5.3 Lsun Lg Galaxy g-band luminosity 65- 68 I4 kpc rho Impact parameter from the sight line to the galaxy 70- 74 F5.2 --- rho/Rvir Impact parameter from the sight line to the galaxy in units of the galaxy's virial radius (2) 76- 80 I5 km/s Deltav Velocity difference between the galaxy and the absorber
Note (1): Catalog source refers to Stocke et al. 2006ApJ...641..217S Note (2): See Figure 1 in Stocke et al. 2013ApJ...763..148S
History: From electronic version of the journal References: Savage et al., Paper I, 2014ApJS..212....8S
(End) Prepared by Tiphaine Pouvreau [CDS] 30-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

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