J/ApJ/701/1219 Galaxy survey in 3 QSO fields (Chen+, 2009)
Probing the intergalactic medium-galaxy connection at z < 0.5. I. A galaxy survey in QSO fields and a galaxy-absorber cross-correlation study. Chen H.-W., Mulchaey J.S. <Astrophys. J., 701, 1219-1242 (2009)> =2009ApJ...701.1219C
ADC_Keywords: Galaxies, spectra ; Photometry, UBVRI ; Redshifts ; Surveys ; QSOs Keywords: cosmology: observations - intergalactic medium - quasars: absorption lines Abstract: We present an imaging and spectroscopic survey of galaxies in fields around QSOs HE 0226-4110, PKS 0405-123, and PG 1216+069. The fields are selected to have ultraviolet echelle spectra available, which uncover 195 Lyα absorbers and 13 OVI absorbers along the three sightlines. We obtain robust redshifts for 1104 galaxies of rest-frame absolute magnitude MR-5logh≲-16 and at projected physical distances ρ≲4h-1Mpc from the QSOs. Hubble Space Telescope (HST)/WFPC2 images of the fields around PKS 0405-123 and PG 1216+069 are available for studying the optical morphologies of absorbing galaxies. Combining the absorber and galaxy data, we perform a cross-correlation study to understand the physical origin of Lyα and OVI absorbers and to constrain the properties of extended gas around galaxies. Description: The observing program of the galaxy survey consists of three phases: (1) imaging observations of the QSO fields to identify candidate galaxies: optical images of the field around HE 0226-4110 were obtained on 2004 September 19, using the IMACS short camera and the B, R, and I filters on the Magellan Baade Telescope. Optical images of the field around PG 1216+069 were obtained on 2005 March 19, using the IMACS short camera and the B, R, and I filters; and additional optical images of PKS 0405-123 and PG1216+069 were obtained from the HST data archive for the Wide Field and Planetary Camera2 (WFPC2) with the F702W filter; (2) object selection for follow-up faint galaxy spectroscopy; and (3) multislit spectroscopic observations, using IMACS and the short camera during three different runs in 2004 November, 2006 May, and 2007 April, to measure the redshifts of the selected galaxies. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 27 66 Lyα absorbers identified along the sightline toward PG 1216+069 table4.dat 116 1793 Photometric and spectroscopic catalog of objects in the field around HE0226-4110 table5.dat 116 1379 *Photometric and spectroscopic catalog of objects in the field around PKS0405-123 table6.dat 116 1619 Photometric and spectroscopic catalog of objects in the field around PG1216+069
Notes on table5.dat: The object ID, coordinates, and R-band photometry are adopted from Prochaska et al. (2006, Cat. J/ApJ/643/680).
See also: J/ApJ/679/194 : Low-z intergalactic medium. III. (Danforth+, 2008) J/ApJ/643/680 : Imaging and spectroscopy around PKS 0405-123 (Prochaska+, 2006) J/ApJ/617/718 : Atomic data and EW for PKS 0405-123 (Prochaska+, 2004) J/ApJ/508/200 : QSO low-z Lyα absorbers (Tripp+, 1998) J/A+A/316/123 : QSO absorber and galaxy evolution (Lindner+ 1996) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 7 F7.5 --- z Lyα absorber redshift 8- 10 A3 --- f_z [ab, ] Flag on z (1) 12- 16 F5.2 [cm-2] logNHI HI column density 18- 21 F4.2 [cm-2] e_logNHI logNHI uncertainty 23- 24 I2 km/s b ? Doppler impact parameter b 26- 27 I2 km/s e_b ? b uncertainty
Note (1): Flag as follows: a = The measurement is adopted from Tripp et al. (2005ApJ...619..714T). b = These lines have also been identified by Jannuzi et al. (1998ApJS..118....1J) in low-resolution data obtained using the Faint Object Spectrograph.
Byte-by-byte Description of file: table.dat
Bytes Format Units Label Explanations
1- 5 I5 --- ID Identification number (see the "Nomenclature Notes" section below) 6 A1 --- r_z [IP] origin of z (table5 only) (1) 8- 9 I2 h RAh Hour of Right Ascension (J2000) 11- 12 I2 min RAm Minute of Right Ascension (J2000) 14- 19 F6.3 s RAs Second of Right Ascension (J2000) 21 A1 --- DE- Sign of the Declination (J2000) 22- 23 I2 deg DEd Degree of Declination (J2000) 25- 26 I2 arcmin DEm Arcminute of Declination (J2000) 28- 32 F5.2 arcsec DEs Arcsecond of Declination (J2000) 34- 39 F6.1 arcsec offRA Offset in Right Ascension from QSO 41- 46 F6.1 arcsec offDE Offset in Declination from QSO 48- 52 F5.1 arcsec Sep Angular distance to QSO 54- 60 F7.2 kpc Dist ?=-1 Projected physical distance in units of h-1kpc 62- 67 F6.3 mag Bmag ? B band magnitude (not for table 5) 69- 73 F5.3 mag e_Bmag ? Uncertainty in Bmag 75- 80 F6.3 mag Rmag R band magnitude 82- 86 F5.3 mag e_Rmag Uncertainty in Rmag 88- 93 F6.3 mag Imag ? I band magnitude (not for table 5) 95- 99 F5.3 mag e_Imag ? Uncertainty in Imag 101-107 F7.4 --- z ?=-1 Spectroscopic redshift 109 I1 --- Type [1,2]?=0 absorption or emission galaxy (2) 111-116 F6.2 mag RMag ?=0 Rest-frame R band absolute band magnitude (3)
Note (1): Code as follows: I = New Spectroscopic redshifts obtained in our survey. P = Spectroscopic redshifts published in Prochaska et al., Cat. J/ApJ/643/680 Note (2): Code as follows: 1 = absorption-line dominated; 2 = emission-line dominated. Note (3): The rest-frame R band magnitude of each spectroscopically identified object was estimated based on the observed R band magnitude and spectral type. For absorption-line dominated galaxies, we evaluate the k-correction using the early-type E/S0 and Sab galaxy templates from Coleman et al. (1980ApJS...43..393C). For emission-line dominated galaxies, we evaluate the k-correction using the Irr templates.
Nomenclature Notes: For table 3, absorbers are <[CM2009b] PG1216+069 abs N.NNNNN> in the Dictionary of Nomenclature. For table 4, galaxies are <[CM2009b] HE0226-4110 NNNNN> in Simbad. For table 5, galaxies are <[PWC2006b] NNNNN> for Simbad. For table 6, galaxies are <[CM2009b] PG1216+069 NNNNN> in Simbad. History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 15-Sep-2011
|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|