J/ApJS/182/378 HI and OVI absorbers in nearby Universe (Wakker+, 2009)
The relationship between intergalactic H I/O VI and nearby (z<0.017) galaxies. Wakker B.P., Savage B.D. <Astrophys. J. Suppl. Ser., 182, 378-467 (2009)> =2009ApJS..182..378W
ADC_Keywords: Active gal. nuclei ; Galaxies, nearby ; Spectra, ultraviolet ; Equivalent widths Keywords: galaxies: evolution - galaxies: halos - intergalactic medium ultraviolet: galaxies Abstract: We analyze intergalactic HI and OVI absorbers with ν<5000km/s in Hubble Space Telescope and Far Ultraviolet Spectroscopic Explorer spectra of 76 active galactic nuclei. The baryons traced by HI/OVI absorption are clearly associated with the extended surroundings of galaxies; for impact parameters <400kpc they are 2-4 times more numerous as those inside the galaxies. This large reservoir of matter likely plays a major role in galaxy evolution. We tabulate the fraction of absorbers having a galaxy of a given luminosity within a given impact parameter (ρ) and velocity difference (Δv), as well as the fraction of galaxies with an absorber closer than a given ρ and Δv. We identify possible "void absorbers" (ρ>3Mpc to the nearest L* galaxy), although at v<2500km/s all absorbers are within 1.5Mpc of an L>0.1L* galaxy. The absorber properties depend on ρ, but the relations are not simple correlations. Description: Sample size of 76 from extragalactic targets that were observed by the Far-Ultraviolet Spectroscopic Explorer (FUSE) and the Hubble Space Telescope (HST) with the Goddard High Resolution Spectrograph (GHRS) or the Space Telescope Imaging Spectrograph (STIS). For each target, we searched for nearby galaxies with low impact parameter (ρ). We started with the "Third Reference Catalogue of Galaxies" (de Vaucouleurs et al., 1991, cat. VII/155). Distances for Local Group galaxies were taken from Mateo (1998ARA&A..36..435M). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 154 134 Target exposure list (76 different targets) table3.dat 239 406 HI and OVI results table13.dat 108 6382 All known galaxies with velocity less than 7000km/s and impact parameter less than 2Mpc to the 76 extragalactic sightlines in the sample
See also: VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991) VI/129 : The FUSE Observation Log (FUSE, 1999-2007) J/ApJS/146/1 : O VI absorption in FUSE survey (Wakker+, 2003) J/ApJS/177/39 : Survey of low-redshift OVI absorbers (Tripp+, 2008) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Target Name of the target 18- 23 F6.2 deg GLON Galactic longitude 25- 30 F6.2 deg GLAT Galactic latitude 32- 37 F6.4 --- z Redshift 39- 44 A6 --- Type Object type 46- 50 F5.1 ks Exp Exposure time (2) 52- 55 F4.1 10-16W/m2/nm Flux Flux at 1031Å or 1238Å (3) 57- 58 I2 --- SN1 ? Signal to noise ratio at 1031Å (4) 60- 61 I2 --- SN2 ? Signal to noise ratio at 977Å (4) 63- 64 I2 -- SN3 ? Signal to noise ratio at 1238Å (4) 66-154 A89 --- Set FUSE and HST datasets (1)
Note (1): FUSE datasets consist of an eight-character code giving the observing program, object id, and exposure number; HST datasets list a four-character program id, followed by a two-digit object id and a three-digit observation id, which we omit; for HST STIS observations an extra identifier between parentheses shows whether the data were taken using the G140M grating centered at 1222Å(Ga) or 1272Å(Gb) or with the E140M echelle (E); datasets starting with "Z" were obtained with the GHRS. Note (2): Exposure time given separately for each FUSE exposure (which corresponds to several orbits); only a single value is given for each multiorbit HST exposure. Note (3): For FUSE datasets this is the flux at 1031Å, while for targets with only HST datasets it is the flux at 1238Å. Unit of flux is 10-14erg/cm2/s/Å. Note (4): For FUSE data the resolution element is 20km/s, while for HST data it depends on the instrument and grating: 20km/s for GHRS spectra, 30km/s for STIS grating (G140M) exposures, and 6.5km/s for STIS echelle (E140M) data.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Target Name of extragalactic UV-bright target, using the conventions of Wakker et al. (2003, Cat. J/ApJS/146/1) 17- 42 A26 --- Galaxy Name of galaxy near the sightline (1) 44- 50 A7 --- Group Group galaxy belongs to; X if none 52- 55 I4 km/s HV Heliocentric velocity of galaxy 57- 60 F4.1 kpc Diam ?=-1.0 Diameter of galaxy (usually D25) (2) 62- 67 F6.1 kpc rho ? Impact parameter to UV-bright target (3) 69 A1 --- Qual Reliability flag (4) 71- 73 A3 --- HI HI quality flag (5) 75- 77 A3 --- OVI OVI quality flag (5) 79- 81 A3 --- CIII CIII quality flag (5) 83 A1 --- Sp [GSEx] HST spectrograph (6) 85- 88 I4 10-13m EWLya ? Equivalent width for Lyα 89- 90 I2 --- n_EWLya [-3/-1]? flag for non-detection (7) 92- 94 I3 10-13m e_EWLya ?=-1 Statistical error for EWLya 96- 98 I3 10-13m esEWLya ?=-1 Systematic error for EWLya 100-103 I4 km/s LyaVel ?=-1 Velocity of detected Lya line 105-109 A5 --- Lya Lineid flag for Lya (8) 111-114 I4 10-13m EWLyb ? Equivalent width for Lyβ 115-116 I2 --- n_EWLyb [-3/-1]? flag for non-detection (7) 118-120 I3 10-13m e_EWLyb ?=-1 Statistical error for EWLyb 122-124 I3 10-13m esEWLyb ?=-1 Systematic error for EWLyb 126-129 I4 km/s LybVel ?=-1 Velocity of detected Lyb line 131-135 A5 --- Lyb Lineid flag for Lyb (8) 137-140 I4 10-13m EWLyg ? Equivalent width for Lyγ 141-142 I2 --- n_EWLyg [-3/-1]? flag for non-detection (7) 144-146 I3 10-13m e_EWLyg ?=-1 Statistical error for EWLyg 148-150 I3 10-13m esEWLyg ?=-1 Systematic error for EWLyg 152-155 I4 km/s LygVel ?=-1 Velocity of detected Lyγ line 157-161 A5 --- Lyg Lineid flag for Lyγ (8) 163-166 I4 10-13m EWOVIa ? Equivalent width for OVIa; OVI-1031 167-168 I2 --- n_EWOVIa [-3/-1]? flag for non-detection (7) 170-172 I3 10-13m e_EWOVIa ?=-1 Statistical error for EWOVIa 174-176 I3 10-13m esEWOVIa ?=-1 Systematic error for EWOVIa 178-181 I4 km/s OVIaVel ?=-1 Velocity of detected OVIa line 183-189 A7 --- OVIa Lineid flag for OVIa (8) 191-192 I2 10-13m EWOVIb ? Equivalent width for OVIb; OVI-1037 193-194 I2 --- n_EWOVIb [-3/-1]? flag for non-detection (7) 196-198 I3 10-13m e_EWOVIb ?=-1 Statistical error for EWOVIb 200-202 I3 10-13m esEWOVIb ?=-1 Systematic error for EWOVIb 204-207 I4 km/s OVIbVel ?=-1 Velocity of detected OVIb line 209-213 A5 --- OVIb Lineid flag for OVIb (8) 215-218 I4 10-13m EWCIII ? Equivalent width for CIII 219-220 I2 --- n_EWCIII [-3/-1]? flag for non-detection (7) 222-224 I3 10-13m e_EWCIII ?=-1 Statistical error for EWCIII 226-228 I3 10-13m esEWCIII ?=-1 Systematic error for EWCIII 230-233 I4 km/s CIIIVel ?=-1 Velocity of detected CIII line 235-239 A5 --- fCIII Lineid flag for CIII (8)
Note (1): With few exceptions, these names are the preferred names in the RC3 (first NGC, then UGC, ESO or other), or, if not present in the RC3, the preferred name in NED. Note (2): Calculated from the angular diameter given in the RC3 or NED and the galaxy's distance (see Section 2.2). Note (3): Impact parameter between background UV target and foreground galaxy, calculated from the latter's distance and the angular separation between the galaxy's center and the background target. Note (4): The reliability of associating the detected absorption lines with the listed galaxy. Flag as follows: ! = unambiguous detections or non-detections. + = there is more than one absorber associated with one galaxy. 2 = there are two absorbers associated with two galaxies, but it is possible that the choice could be reversed. 1 = when a choice was made between two galaxies for assigning the absorber, giving a non-detection to one of them. g = absorber associated with a group, rather than a particular galaxy. ? = ambigous associations. > = non-detections with upper limit worse than 50mÅ. x = none of the lines are measureable. i = absorbers without associated galaxy within 1Mpc. Note (5): Flags show the quality of the (non)detections: + = the detected HI, OVI or CIII line can clearly be associated with the galaxy. (+) = is given for uncertain detections. - = non-detection with 3sigma equivalent width limit better than 50mÅ. (-) = non-detections with 3sigma equivalent width limit worse than 50mÅ. Note (6): Spectrograph is abbreviated as: G = GHRS S = STIS-G140M E = STIS-E140M x = none Note (7): Equivalent width limits are indicated as follows: -1 = no measurement could be made -2 = upper limits (in which case the e_EW column gives the 3-sigma equivalent width upper limit -3 = when the possible absorption is contaminated. Note (8): "Lineid flag": X = there is no data. UL = only an upper limit could be set If the line id corresponds to the right column (for Lyα, Lyβ, Lyγ, OVIa, OVIb, CIII), that line is detected with the given equivalent width. Other line ids (flag=-3) give the contaminating absorption line.
Byte-by-byte Description of file: table13.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Target Name of the AGN target 18- 46 A29 --- Galaxy Name of galaxy near the AGN sightline 48- 54 A7 --- Type Galaxy type (for RC3 galaxies) 56- 61 F6.2 deg GLON Galactic longitude 63- 68 F6.2 deg GLAT Galactic latitude 70- 74 I5 km/s HV Heliocentric velocity of galaxy 76- 80 F5.1 Mpc Dist Estimated distance of galaxy 82- 85 F4.1 kpc Diam ?=0.0 Estimated diameter of galaxy 87- 91 F5.2 deg Sep Angular separation to background UV target 93- 96 I4 kpc rho Impact parameter of background UV target 98-108 A11 --- Note Extra information (1)
Note (1): Column gives extra information: * LGGNNN-NN.N : group membership (LGGNN)-followed by the distance that would have been derived if the galaxy's velocity was used directly, * ASSUMEV : whether the galaxy's velocity is unknown, * ASSUMEV-CHK : velocity unknown and checked in NED, * MINDIST : the minimum distance (2.9Mpc) was assumed. A plain number gives the velocity distance for galaxies for which a better distance estimate was instead taken from the literature. Note that this table is inhomogeneous. Near some sightlines deep searches for dwarf galaxies exist, near others they don't. The table should not be used for statistical analyses for faint galaxies. Only for galaxies with diameter >7.5kpc is it more-or-less complete.
History: * 30-Nov-2009: From electronic version of the journal * 12-Mar-2010: Merged in table1 the records with FUSE obervations; rewritten the 'Target' columns without blanks or underscore and appropriate upper/lowercase in order to have identical targets represented by identical names.
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 30-Nov-2009
|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|