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VII/185    IRAS 1.2 Jy IRAS Redshift Survey            (Strauss+ 1990-1995)

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 =1995yCat.7185....0S
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; F602 > 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
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
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
Bytes Format Units Label Explanations
1- 2 I2 h RAh Right Ascension B1950 (hours) (1) 3- 4 I2 min RAm Right Ascension B1950 (minutes) (1) 5- 8 F4.1 s RAs Right Ascension B1950 (seconds) (1) 9 A1 --- DE- Declination B1950 (sign) (1) 10- 11 I2 deg DEd Declination B1950 (degrees) (1) 12- 13 I2 arcmin DEm Declination B1950 (minutes) (1) 14- 15 I2 arcsec DEs Declination B1950 (seconds) (1) 17- 20 I4 10-3[dJy] nf12 ? 12µm flux (2) 21- 24 I4 10-3[dJy] nf25 ? 25µm flux (2) 25- 28 I4 10-3[dJy] nf60 ? 60µm flux (2) 29- 32 I4 10-3[dJy] nf100 ? 100µm flux (2) 34 I1 --- id [0/4] IRAS-PSC association type (9) 35 I1 --- x [0/8] IRAS-PSC extended object flag (3) 36 A1 --- CC [A-L] IRAS-PSC correlation (4) 37 A1 --- v [0-9Vnv] IRAS-PSC variability flag (5) 38 A1 --- s Type of source (statusflag) (6) 39 I1 --- q_nf12 [1/3]? IRAS flux quality flag 12um (7) 40 I1 --- q_nf25 [1/3]? IRAS flux quality flag 25um (7) 41 I1 --- q_nf60 [1/3]? IRAS flux quality flag 60um (7) 42 I1 --- q_nf100 [1/3]? IRAS flux quality flag 100um (7) 43- 53 A11 --- optID Optical counterpart name to the object (8) 54 A1 --- n_optID [M] Unexplained note on optID 55- 59 F5.2 mag mag ? Optical magnitude, where available 61- 65 I5 km/s Hvel ? Heliocentric velocity, from literature (see (VII/193)) or measured by us 66- 68 I3 km/s e_Hvel ? Heliocentric velocity error 69- 72 A4 --- r_Hvel Code for source of redshift in ZCAT (VII/193) 73- 77 A5 --- Ttype de Vaucouleurs' T-type from ZCAT (VII/193) 79- 84 A6 --- UGC/ESO Object ID from UGC or ESO catalog 90- 95 A6 --- Sp Internal flag coding the optical spectrum in the CfA database 97-116 A20 --- Comm Miscellaneous comments from ZCAT (VII/193) 117-120 I4 10-3[dJy] pf12 ? IRAS-PSC 12µm flux (2) 121-124 I4 10-3[dJy] pf25 ? IRAS-PSC 25µm flux (2) 125-128 I4 10-3[dJy] pf60 ? IRAS-PSC 60µm flux (2) 129-132 I4 10-3[dJy] pf100 ? IRAS-PSC 100µm flux (2)
Note (1): The coordinates for all objects that appear in the IRAS PSC, Version 2 (II/125), 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, Cat. VII/109) Note (2): The IRAS fluxes are coded in a compact logarithmic form: nFx=1000*log(10Fx), or Fx=10(nFx/1000-1) for x=12, 25, 60, 100. The fluxes are taken from the PSC, unless: * The object is extended at 60 microns (see the Note (3) below) * The object is variable (see the Note (5) below) * The object is of moderate flux quality at 60 microns (see q_nf60) 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. (VII/109) have fluxes from that source. Note (3): The extendflag indicates whether or not an object is flagged as extended (SES(2) flag) in the IRAS-PSC. Values are: 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 (VII/109) Note (4): 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 60µm 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 (5): 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% 2 = Variability between 20 and 30% 3 = Variability between 30 and 40% 4 = Variability between 40 and 50% 5 = Variability between 50 and 60% 6 = Variability between 60 and 70% 7 = Variability between 70 and 80% 8 = Variability between 80 and 90% 9 = Variability between 90 and 100% Note (6): 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 indicates a Local Group galaxy. * 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 (Cat. VII/185) and Yahil et al. (1991ApJ...372..380Y) for a discussion of our estimate of the number of sources flagged as cirrus that are indeed galaxies. Note (7): 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 (8): Optical identification is from a matching of the combined UGC, Zwicky, and NGC catalogs. Note (9): The idtype is taken directly from the PSC; it ranges from 1 to 4: 1 = association found in an extragalactic catalogs 2 = association found in stellar catalogs 3 = association found in other catalogs 4 = association found in multiple types of catalogs
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. -------------------------------------------------------------------------------- People may contact Michael Strauss at if they have questions about these files. History: * 1995-02-06: Files prepared by Michael Strauss * 1997-10-10: MCG and PK numbers which were truncated in the original catalogue file have been replaced at CDS (Francois Ochsenbein) * 2015-12-11: cosmetic changes at CDS
(End) Michael Strauss [IAS] 1995-02-06
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

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