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Format of the 1.2-Jy IRAS Redshift Survey
CDS Catalog 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: references Strauss M., Davis M., Yahil A., Huchra J.P.
============================================================================1990ApJ...361...49S Strauss M., Huchra J.P., Davis M., Yahil A., Fisher K.B., Tonry J. 1992ApJS...83...29S Fisher K.B., Huchra J.P., Strauss M.A., Davis M., Yahil A., Schlegel D. 1995ApJS..100...69F 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: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- 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
--------------------------------------------------------------------------------See also: II/174 : IRAS 2Jy Redshift Survey Data File (Strauss+ 1992) Byte-by-Byte Description of file: catalog.dat
-------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 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 -------------------------------------------------------------------------------- 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. -------------------------------------------------------------------------------- Remark: There is a supplementary file, exclude.lis which contains the number of the lune bins that are excluded (see Strauuss et al. 1992, ApJS, 83, 29 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 call the logical function exclude to decide if an object is in the excluded zones or not. -------------------------------------------------------------------------------- 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) ===============================================================================
