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VII/185 IRAS 1.2 Jy IRAS Redshift Survey (Strauss+ 1990,92,95)
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IRAS 1.2 Jy Redshift Survey Data File
Strauss M., Davis M., Yahil A., Huchra J.P.
<Astrophys. J. 361, 49 (1990)>
=1990ApJ...361...49S
Strauss M., Huchra J.P., Davis M., Yahil A., Fisher K.B., Tonry J.
<Astrophys. J. Suppl. 83, 29 (1992)>
=1992ApJS...83...29S
Fisher K.B., Huchra J.P., Strauss M.A., Davis M., Yahil A., Schlegel D.
<Astrophys. J. Suppl. 100, 69 (1995)>
=1995ApJS..100...69F
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ADC_Keywords: Infrared sources ; Photometry, infrared ; Redshifts
Description:
This is an explanation of the redshift survey of Fisher, Huchra,
Strauss, Davis, Yahil and Schlegel; the data set is described in full
in ApJ 361, 49 (1990). The data for the brighter half are included in
ApJ Supp 1992, 83, 29; the data for the fainter half are included in a
paper submitted for publication to the Astrophysical Journal
Supplement. The survey contains 9897 objects selected from the IRAS
database according to the criteria listed in that paper, briefly:
F60 > 1.2 Jy;
F60^2 > F12 f25;
|b| > 5;
high source density flag at 60 microns not raised.
Thus, the file consists of both galaxies and Galaxian contaminants;
this is explained below. The sample contains ~5320 galaxies, and 14
objects without id's at the present time.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
catalog.dat 132 9897 The data file
exclude.lis 6 1465 Numbers of the lune bins that are excluded
exclude.f 80 281 Fortran program to define excluded regions
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
II/174 : IRAS 2Jy Redshift Survey Data File (Strauss+ 1992)
Byte-by-byte Description of file: catalog.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh *Right Ascension B1950 (hours)
3- 4 I2 min RAm *Right Ascension B1950 (minutes)
5- 8 F4.1 s RAs *Right Ascension B1950 (seconds)
9 A1 --- DE- *Declination B1950 (sign)
10- 11 I2 deg DEd *Declination B1950 (degrees)
12- 13 I2 arcmin DEm *Declination B1950 (minutes)
14- 15 I2 arcsec DEs *Declination B1950 (seconds)
17- 20 I4 [0.1Jy] nf12 *? log_10 of 12 um flux, in 0.1 Jy
21- 24 I4 [0.1Jy] nf25 *? log_10 of 25 um flux, in 0.1 Jy
25- 28 I4 [0.1Jy] nf60 *? log_10 of 60 um flux, in 0.1 Jy
29- 32 I4 [0.1Jy] nf100 *? log_10 of 100 um flux, in 0.1 Jy
34 I1 --- IDtype *[0/4] IRAS PSC identification
35 I1 --- ExtendFlag *[0/8] IRAS PSC flag for
extended objects
36 A1 --- CC *IRAS PSC cirrus flag
37 A1 --- VarFlag * IRAS PSC variability flag
38 A1 --- StatusFlag *? Object identification flag
39 I1 --- fq12 *[1/3]? IRAS PSC Flux qual. flag 12um
40 I1 --- fq25 *[1/3]? IRAS PSC Flux qual. flag 25um
41 I1 --- fq60 *[1/3]? IRAS PSC Flux qual. flag 60um
42 I1 --- fq100 *[1/3]? IRAS PSC Flux qual. flag 100um
43- 54 A12 --- optID *Optical counterpart to the object
55- 59 F5.2 mag mag *? Optical magnitude, where available
61- 65 I5 km/s Hvel *? Heliocentric velocity
66- 68 I3 km/s e_Hvel *? Heliocentric velocity error
69- 72 A4 --- r_Hvel *Code for source of redshift
73- 77 A5 --- Ttype *de Vaucouleurs' T-type
79- 84 A6 --- UGC/ESO * object ID from UGC or ESO catalog
first 5 bytes is number
last byte is letter or blank
90- 95 A6 --- Spectrum *Internal flag coding the optical spect
97-116 A20 --- comments *Miscellaneous comments
117-120 I4 [0.1Jy] pf12 *? log_10 of 12 um flux, in 0.1 Jy
121-124 I4 [0.1Jy] pf25 *? log_10 of 25 um flux, in 0.1 Jy
125-128 I4 [0.1Jy] pf60 *? log_10 of 60 um flux, in 0.1 Jy
129-132 I4 [0.1Jy] pf100 *? log_10 of 100 um flux, in 0.1 Jy
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Note on RAh, RAm, RAs, DE-, DEd, DEm, DEs:
The coordinates for all objects that appear in the IRAS PSC, Version 2,
are from that source, and are given as B1950.0; there are also a few
very large galaxies whose fluxes and coordinates are taken from the
Large Optical Galaxy Catalog (Rice et al. 1988, ApJS, 68, 91).
Note on nf12, nf25, nf60, nf100:
The IRAS fluxes are coded in a compact logarithmic form:
The 12 micron flux is related to the integer nF12 by
F12 = 10.^(nF12/1000 - 1.); similarly for the other fluxes.
The fluxes are taken from the PSC, unless:
1. The object is extended at 60 microns (see extendflag below);
2. The object is variable (see varflag below);
3. The object is of moderate flux quality at 60 microns (see Fq60 below).
In these cases, we have obtained one-dimensional addscan's of the data and
used the zero-crossing flux from the median scan's in all four bands, as
supplied by SCANPI.
Those sources flagged as extended in Rice et al. have fluxes from that
source.
Note on IDtype:
The idtype is taken directly from the PSC;
Idtype ranges from 1 to 4 and states whether an association was found is an
extragalactic catalog (1), stellar catalogs (2), other catalogs (3), or
matches in multiple types of catalogs (4).
Note on ExtendFlag:
The extendflag indicates whether or not an object is flagged as extended
(SES(2) flag) in the psc.
extendflag = 0 Not extended
1 Extended at 12 microns
2 Extended at 25 microns
3 Extended at 12 and 25 microns
4 Extended at 60 microns
5 Extended at 12 and 60 microns
6 Extended at 25 and 60 microns
7 Extended at 12, 25, and 60 microns
8 Extended in Rice et al
Note on CC:
The correlation coefficient is taken from the PSC and represents the best
correlation coefficient between a hours-confirmed scan and the point source
template at 60 microns in the Point Source Data Base; see the Explanatory
Supplement for details. A means 99% or better correlation, B is between 98
and 99% and so on.
Note on VarFlag:
The varflag is a measure of variability in 12 and 25 microns.
n No measure of variability available.
0 No variability measured.
N Variability between 1 and 10%.
1 Variability between 10 and 20%
and so on.
Note on StatusFlag:
The statusflag indicates the identification of the source, and, if it is a
galaxy, the source of the redshift:
Galaxies: O,H,Z,F,B,D. The distinction between these is uninteresting,
although Z indicates a source drawn from John Huchra's private version
of ZCAT.
L: Local Group galaxy. This is given a separate flag.
Non-galaxies:
M: HII region in external galaxy.
S: Star
s: Emission line star
C: Cirrus or dark cloud
P: Planetary nebula
R: Reflection Nebula
? or E: Unidentified field.
These labels are by no means complete; we observed only a fraction of these
sources at the telescope. See Strauss et al. 1990 and Yahil et al. 1991
(ApJ, 372, 380) for a discussion of our estimate of the number of sources
flagged as cirrus that are indeed galaxies.
Note on fq12, fq25, fq60, fq100:
The flux qualities are taken from the PSC; one number between one and three
is given for each band:
1: Not detected
2: Moderate flux quality
3: Good flux quality
If the flux given is from the PSC (as opposed to ADDSCAN), the flux listed
in a band with flux quality 1 will be an upper limit.
Note on optID:
Optical identification is from a matching of the combined UGC, Zwicky, and
NGC catalogs.
Note on mag:
Magnitudes are from the same source, and are not complete.
Note on Hvel, e_Hvel:
Redshifts and errors are either as quoted in the literature, or measured
by us. All are heliocentric.
Note on r_Hvel:
Source is a four-digit number that codes the redshift source from ZCAT.
Note on Ttype:
Ttype is the type of the galaxy from ZCAT.
Note on UGC/ESO:
Unumber is either the UGC or ESO number of the source.
Note on Spectrum:
Spectrum is an internal index for the optical spectrum, if one exists, of
the galaxy in the CfA database.
Note on comments:
Comments are taken from ZCAT.
Note on pf12, pf25, pf60, pf100:
Fluxes of the source as listed in the IRAS Point Source Catalog for those
sources with ADDSCAN fluxes in columns 17-32; they are coded the same way
as the earlier fluxes are.
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Remark:
There is a supplementary file, exclude.lis which contains the number of
the lune bins that are excluded (see Paper 1 for a full description).
There is a series of Fortran programs in exclude.f that should be used
to decide if a given object is in the excluded regions or not. First,
run the program write_lmask, which reads the exclude.lis file and creates
a binary file lmask.lis, which has much faster I/O. This only need be
done once. Your code will need to call init_lmask to read in lmask.lis,
and thereafter zones or not.
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People may contact Michael Strauss at strauss@astro.princeton.edu
if they have questions about these files.
History:
* MCG and PK numbers which were truncated in the original catalogue file
have been replaced at CDS (Francois Ochsenbein, 10-Oct-1997)
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(End) Michael Strauss [IAS] 1995-02-06