J/ApJS/146/1 O VI absorption in FUSE survey (Wakker+, 2003)
The Far Ultraviolet Spectroscopic Explorer Survey of O VI absorption in and
near the galaxy.
Wakker B.P., Savage B.D., Sembach K.R., Richter P., Meade M., Jenkins E.B.,
Shull J.M., Ake T.B., Blair W.P., Dixon W.V., Friedman S.D., Green J.C.,
Green R.F., Kruk J.W., Moos H.W., Murphy E.M., Oegerle W.R., Sahnow D.J.,
Sonneborn G., Wilkinson E., York D.G.
<Astrophys. J. Suppl. Ser. 146, 1 (2003)>
=2003ApJS..146....1W 2003ApJS..146....1W
ADC_Keywords: Interstellar medium ; Ultraviolet ; Molecular clouds ;
Radial velocities
Keywords: Galaxy: halo - ISM: structure - ultraviolet: ISM
Abstract:
We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations
of the O VI λλ1031.926, 1037.617 absorption lines
associated with gas in and near the Milky Way, as detected in the
spectra of a sample of 100 extragalactic targets and two distant halo
stars. We combine data from several FUSE Science Team programs with
guest observer data that were public before 2002 May 1. The sight
lines cover most of the sky above Galactic latitude |b|>25°, at
lower latitude the ultraviolet extinction is usually too large for
extragalactic observations.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 167 289 Basic target data
table2.dat 165 242 Derived Data
notes.dat 54 28 Galaxy groups intersected by sightline flags
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See also:
J/ApJS/146/125 : O VI in the galactic halo (Savage+, 2003)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- Name Object name (1)
18- 19 I2 h RAh Hour of Right Ascension (J2000) (2)
21- 22 I2 min RAm Minute of Right Ascension (J2000) (2)
24- 27 F4.1 s RAs Second of Right Ascension (J2000) (2)
29 A1 --- DE- Sign of the Declination (J2000) (2)
30- 31 I2 deg DEd Degree of Declination (J2000) (2)
33- 34 I2 arcmin DEm Arcminute of Declination (J2000) (2)
36- 37 I2 arcsec DEs Arcsecond of Declination (J2000) (2)
39- 44 F6.2 deg GLON Galactic longitude
46- 51 F6.2 deg GLAT Galactic latitude
53- 58 F6.4 --- z ? NED Redshift
60- 63 I4 km/s RV ? NED Radial velocity
65- 82 A18 --- Type NED classification (3)
84- 88 F5.2 --- Bmag Veron-Cetty & Veron (2000, Cat. VII/224)
blue band magnitude
90- 94 F5.3 mag E(B-V) Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S)
(B-V) color excess
96 A1 --- n_Obs.Date [n] Indicates observation was not used in
the final combined spectrum
98-107 A10 "YYYY/MM/DD" Obs.Date Date of the FUSE observation
109-116 A8 --- ObsID Observation identification (4)
119-123 F5.1 s TNom Nominal exposure time (5)
125-128 F4.1 s T1A ? Useful on-object time for the
LiF1A channel
130-133 F4.1 s T2B ? Useful on-object time for the
LiF1B channel
135 A1 --- f_T2B [n] Indicates no signal in the
LiF1B channel
137-167 A31 --- ONames Other names (6)
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Note (1): Usually, but not always, the same name as was used in the FUSE
observation log (see text).
Note (2): From the Veron-Cetty & Veron (2000, see Cat. VII/224) catalogue
of QSOs and Seyferts or NED if not present in the catalogue.
Note (3): Note that for QSOs NED gives QSO on its summary line, but in
the body of the information each QSO is classified as either
Sey1, Opt.var. or (in a few cases) E2 or E4. We use the QSO
classification in these cases.
QSO or BLLac = quasars;
Sey# = Seyfert where a number between 1 and 2 gives the numerical
subclassification;
Gal: mmm = Galaxy with mmm the morphological classification;
Gal:HII = The three Tololo objects, which are galaxies whose light
is dominated by H II regions;
BCG = Blue Compact Galaxy;
BCD = Blue Compact Dwarf;
StrBrst = a starburst galaxy;
HII(ggg) = bright H II regions inside another galaxy, whose name is
given by ggg;
sdO = for PG 0832+675 and vZ 1128.
Note (4): Each identification has two parts - a target ID within the
observing program and a visit number.
Note (5): The time that the observation log specifies.
Note (6): We established the following order of preference for the prefix
indicating the source catalogue: NGC, 3C, Mrk, PG, and Ton.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Rank Object ranking number
7- 22 A16 --- Name Object name
24- 27 A4 --- Chan Channels used (1)
29- 33 F5.1 ks Exp Effective exposure time (2)
35 A1 --- f_Exp [d] Flag on Exp (3)
37- 41 F5.2 10-16W/m2/nm Flux The 10-pixel bin flux in units
of 10-14erg/cm2/s/Å
43- 46 F4.2 10-16W/m2/nm RMS The 10-pixel bin RMS noise in units
of 10-14erg/cm2/s/Å
48- 51 F4.1 --- S/N The S/N per 20 km/s resolution element
53- 56 F4.1 --- S/NF Final rebinning Signal-to-Noise ratio
58- 59 I2 --- Bin Final rebinning near the O VI line
61 I1 --- Q A O VI quality factor (4)
63- 65 A3 --- Order The global and local polynomial orders (5)
67- 78 A12 --- Shape Continuum shape (6)
80- 90 A11 --- IGM InterGalactic medium absorption flag (7)
92- 98 A7 --- GHGrp Geller & Huchra (1983, Cat. VII/84)
galaxy group intersected by sightline
100-107 A8 --- TGrp Tully (1988, Cat. VII/145) galaxy groups
intersected by sightline (in notes.dat)
109-110 A2 --- JMax Highest detected rotational level
of H2 (9)
112 A1 --- H2 [y/n] H2 lines contaminate the
O VI (1031.926) absorption
114 A1 --- f_LoV-MW Flag on LoV-MW (11)
116-119 I4 km/s LoV-MW ? Lower Milky Way LSR velocity
121-123 I3 km/s UpV-MW ? Upper Milky Way LSR velocity
125 A1 --- f_UpV-MW Flag on UpV-MW (12)
127-129 I3 10-13m EW-MW ? Milky Way equivalent width
in units of milliAngstroms
131-132 I2 10-13m e_EW-MW ? Statistical error in EW-MW
134-135 I2 10-13m E_EW-MW ? Systematic error in EW-MW
137 A1 --- f_EW-MW [j] Flag on EW-MW (13)
139-141 A3 --- HVC High-velocity O VI component
classification
143 A1 --- f_LoV-HVC Flag on LoV-HVC (11)
145-148 I4 km/s LoV-HVC ? Lower High Velocity Cloud LSR velocity
150-153 I4 km/s UpV-HVC ? Upper High Velocity Cloud LSR velocity
155 A1 --- f_UpV-HVC Flag on UpV-HVC (12)
157-159 I3 10-13m EW-HVC ? High Velocity Cloud equivalent width
in units of milliAngstroems
161-162 I2 10-13m e_EW-HVC ? Statistical error in EW-HVC
164-165 I2 10-13m E_EW-HVC ? Systematic error in EW-HVC
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Note (1): The number of LiF1A and LiF2B channels used to create the
final spectrum; a "f" implies no flux in the LiF2B channel,
a "d" implies LiF2B was not used because it differs from LiF1A;
Note (2): The sum of the LiF1A exposure time(s) plus half the LiF2B
exposure time(s);
Note (3): Indicates guest observer objects that we did not recalibrate
because either the continuum is too complicated to measure
Galactic O VI, or because the source is too faint.
Note (4): Quality flag as follows:
4 = spectra in which the O VI (1031.926) line can be clearly
measured. This pertains to most spectra with S/N>14.
3 = good data where a confident measurement can be obtained (S/N=9-14)
2 = (S/N=5-9) for spectra where we think that the measurement is
acceptable, but where some problems start to appear - such
as uncertainty about the range of integration or even about
whether certain features are or are not O VI.
1 = (S/N=3-5) for spectra for which the measurement is unreliable,
but for which we still list the results; these should be
treated carefully.
0 = pertains both to spectra with very low S/N (S/N<3) and spectra
in which the continuum near O VI (1031.926) was too uncertain
or where intergalactic absorption overlapped the Galactic O VI
lines (see Section 3.10).
Note (5): Cases where a local fit was not possible because the continuum
had too much curvature or there were interfering features, no
separate local fit was done and are indicated by having an
``x'' as the order of the local continuum fit.
Note (6): For objects where the O VI (1031.926) line sits in the wing of
Lyβ absorption associated with the background object, or
where the spectrum shows large fluctuations, this number is
lower than the continuum flux elsewhere in the spectrum. Then
the continuum value over most of the spectrum is given between
square brackets, after the word describing the continuum shape.
Note (7): InterGalactic medium absorption flag as follows:
NoGrp = no intervening group
NoGrpLyb?? = no intervening group; possible Lyβ
GrpNoIGM = intervening group, no features
Grp = intervening group but low S/N
Unid = unidentified feature
GrpLyb = confirmed Lyβ from identified group
GrpLyb? = intervening group, probable Lyβ
GrpLyb?? = intervening group, possible Lyβ
IntrLyb = intrinsic Lyβ seen
IntrLyb?? = intrinsic possible Lyβ seen
Lyb = confirmed Lyβ, no known group
ContamLyb = contaminating Lyβ
Note (9): A dash indicates no H2 was found.
Note (11): Flag on LoV-MW as follows:
[ = The separation between the Galactic and high-velocity absorption
at the negative-velocity edge is unclear and thus was based on
a rule rather than on features in the spectrum (see text).
x = The separation between the Galactic and high-velocity component
at the negative-velocity edge is not clear, but it appears to
be possible to discern separate components.
Note (12): Flag on UpV-MW:
] = The separation between the Galactic and high-velocity absorption
at the positive-velocity edge is unclear and thus was based on a
rule rather than on features in the spectrum (see text).
x = The separation between the Galactic and high-velocity component
at the positive-velocity edge is not clear, but it appears to be
possible to discern separate components.
Note (13): 'j' indicates that the equivalent width listed for Mrk771
is based on the O VI 1037.617 line.
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Byte-by-byte Description of file: notes.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Code Code (TGrp number)
5- 40 A36 --- Group Galaxy groups intersected
43- 44 A2 --- --- [v=]
45- 48 I4 km/s Vel ? Velocity
49- 51 A3 --- --- [±]
52- 54 I3 km/s e_Vel ? rms uncertainty on Vel
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Bauer [CDS] 16-Jun-2003