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 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 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 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:
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FileName Lrecl Records Explanations
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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)
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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
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Bytes Format Units Label Explanations
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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
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Note (1): Catalog source refers to Stocke et al. 2006ApJ...641..217S 2006ApJ...641..217S
Note (2): See Figure 1 in Stocke et al. 2013ApJ...763..148S 2013ApJ...763..148S
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History:
From electronic version of the journal
References:
Savage et al., Paper I, 2014ApJS..212....8S 2014ApJS..212....8S
(End) Prepared by Tiphaine Pouvreau [CDS] 30-Mar-2017