ACDS V10.0 - Detailed Description of VII/225B

ACDS V10.0 - Sun Jan 19 19:12:26 CET 2025

| # Detailed Description of VII/225B : The Canada-France Redshift Survey (CFRS) (Lilly+, 1995) |

Note : this is the description file of the original catalog. This HTML page corresponds well to the original description, but some minor changes in the format may have been introduced in the FITS output files in order to allow for arithmetic operations on quantities such as coordinates and times. h:m:s and d:m:s units are normally converted into degrees, and YYYY-MM-DD into julian days.
Similarly, some slight changes may have been introduced in the units; the value given in the HTML files supersedes the value indicated in the ReadMe file for this catalogue.

    VII/225B            The Canada-France Redshift Survey (CFRS)      (Lilly+, 1995)
    ================================================================================
    The Canada-France Redshift Survey
         Lilly S.J., Le Fevre O., Crampton D., Hammer F., Tresse L.
        <Astrophys. J. 455, 50; 455, 60; 455, 75; 455, 88; 455, 96 (1995)>
        =1995ApJ...455...50L
        =1995ApJ...455...60L
        =1995ApJ...455...75L
        =1995ApJ...455...88H
        =1995ApJ...455...96C
    ================================================================================
    ADC_Keywords: Galaxies, photometry ; Galaxies, spectra ; Redshifts

    Keywords: galaxies: distances and redshifts - techniques: spectroscopic

    Description:
        The Canada-France Redshift Survey (CFRS) is a collaboration between
        astronomers in Canada and France: Simon Lilly (University of Toronto),
        Olivier Le Fevre and Francois Hammer (Observatoire de Paris Meudon),
        David Crampton (Dominion Astrophysical Observatory, Victoria),
        Laurence Tresse (Cambridge University), and David Schade and Dan Hudon
        (University of Toronto). The survey is based primarily on observations
        with the 3.6m Canada-France-Hawaii Telescope (CFHT) on Mauna Kea,
        Hawaii. The CFRS consists of spectra of over 1000 faint objects
        selected to have 17.5 < I(AB) < 22.5 in five regions of sky. The
        survey is providing the first systematic study of normal galaxies at
        redshifts z > 0.5, corresponding to look-back times of greater than
        50% of the age of the Universe. Observations of CFRS galaxies have
        also been made with the Hubble Space Telescope and the survey will
        form the basis of future studies with a number of other ground-based
        and space facilities. We have written a lay-persons guide to the CFRS
        and the main scientific results that are emerging from it.

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × catalog.dat      124     1010   The Canada-France Redshift Survey catalogue

    See also:
     http://www.astro.utoronto.ca/~lilly/CFRS : The CFRS Home Page
     J/ApJ/464/79  : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996)
     J/ApJ/481/49  : CFRS XIV. Field galaxies up to z=1 (Hammer+ 1997)
     J/ApJ/517/148 : ISO observations of the CFRS field (Flores+, 1999)
     J/AJ/122/621  : Galaxy morphology in the CFRS (van den Bergh, 2001)

    Byte-by-byte Description of file:  catalog.dat

       Bytes Format Units   Label     Explanations

       1-  7  A7    ---     CFRS      CFRS identification number (6)
           8  A1    ---     f_CFRS    [*] when the galaxy appears in the parts XI/XIV
                                       (catalogs J/ApJ/464/79 or J/ApJ/481/49)
      10- 11  I2    h       RAh       Right ascension (J2000) (1)
      13- 14  I2    min     RAm       Right ascension (J2000)
      16- 20  F5.2  s       RAs       Right ascension (J2000)
          22  A1    ---     DE-       Declination sign (J2000)
      23- 24  I2    deg     DEd       Declination (J2000)
      26- 27  I2    arcmin  DEm       Declination (J2000)
      29- 32  F4.1  arcsec  DEs       Declination (J2000)
      35- 39  F5.2  mag     Imag      Isophotal IAB (see CFRS-I, 1995ApJ...455...50L)
      42- 46  F5.2  mag     V-I       ?=99.99 (V-I)AB colour in 3 arcsec aperture
                                     (see CFRS-I, 1995ApJ...455...50L)
      49- 53  F5.2  ---     Q         Image compactness parameter Q (1 = star)
                                     (see CFRS-I, 1995ApJ...455...50L) (2)
      56- 61  F6.4  ---     z         ?=9.999 Redshift (0.000=star) (3)
      64- 65  I2    ---     Class     Confidence class of spectroscopic
                                    identification (4)
      68- 71  I4    0.1nm   Lam1      ? Spectroscopic feature (5)
          72  A1    ---     Cont1     [12Ca?]? Spectroscopic feature (5)
      73- 76  I4    0.1nm   Lam2      ? Spectroscopic feature (5)
          77  A1    ---     Cont2     [1Cb?]? Spectroscopic feature (5)
      78- 81  I4    0.1nm   Lam3      ? Spectroscopic feature (5)
          82  I1    ---     Cont3     [1]? Spectroscopic feature (5)
      83- 86  I4    0.1nm   Lam4      ? Spectroscopic feature (5)
          87  A1    ---     Cont4     [1a?]? Spectroscopic feature (5)
      88- 91  I4    0.1nm   Lam5      ? Spectroscopic feature (5)
      92- 93  A2    ---     Cont5     [1a? ]? Spectroscopic feature (5)
      94- 97  I4    0.1nm   Lam6      ? Spectroscopic feature (5)
          98  A1    ---     Cont6     [1] Spectroscopic feature (5)
      99-102  I4    0.1nm   Lam7      ? Spectroscopic feature (5)
     104-107  I4    0.1nm   Lam8      ? Spectroscopic feature (5)
     109-124  A16   ---     Com       Comments

    Note (1): These should be accurate to about 1 arcsec or better
         (see CFRS-I, 1995ApJ...455...50L)
    Note (2): The Q parameter (Le Fevre et al., 1986A&A...154...92L)
        represents the inverse of the ratio of central surface brightness of
        the object in question and a star of the same isophotal magnitude.
    Note (3): The r.m.s. redshift uncertainty is 0.0013
         (see CFRS-III, 1995ApJ...455...75L)
    Note (4): This is quite involved but is essential for the successful
        use of the catalogue. Nearly all the CFRS spectra were reduced and
        identified independently by three individuals before a final
        identification was made. The Confidence Class represents the consensus
        confidence of these three individuals in the correctness of the final
        identification (see CFRS-II, 1995ApJ...455...60L)

        Classes 0-4 represent normal stars and galaxies, with increasing
        levels of confidence in the identification:
          1: probability of 50% that the measurement was correct
          2: probability of more than 75% that the measurement was correct
          3: measurement at least 95% secure
          4: unquestionably correct identification

        Class 8 represents a single line redshift in which the continuum shape
        around the line supports its identification with [OII] 3727 (see
        CFRS-III, 1995ApJ...455...75L)

        Class 9 represents a single line redshift in which the continuum test
        could not be done, or (rarely) where it gave ambiguous results. The
        line is assumed to be [OII] 3727.

        One of the above notations plus 10 (e.g. 14) indicates that the object
        had broad emission lines and is thus presumably a QSO or broad-line AGN.

        One of the above notations plus 90 (e.g. 94) indicates that the object
        is in the "supplementary" catalogue. Objects went in to the supplementary
        catalogue if a redshift had been measured but the spectrum would
        otherwise have been rejected for one of a number of objective (and
        quantified) observational reasons (see CFRS-II, 1995ApJ...455...60L):
          (a) Spectrum on CCD defect.
          (b) Object too near the end of slit.
          (c) Object displaced off of slit.
          (d) Reexamination of photometry resulted in magnitude below survey limit.

        Objects in the supplementary catalogue are liable to be biased towards
        "easy" objects. No such bias should be present in the remaining
        "statistically complete" catalogue.

        Repeated observations of objects (independently reduced and identified)
        confirmed our a priori assent of probabilities that individual
        spectroscopic identifications were CORRECT (see CFRS-III,
        1995ApJ...455...75L)

               ------------------------------------------------------------
               Class     fraction   confirmation
                         of sample     rate
               ------------------------------------------------------------
               Class 4     35%         100%
               Class 8      3%         100% (the line was always confirmed)
               Class 9      3%         100% (the line was always confirmed)
               Class 3     33%          97%
               Class 2     10%          80%
                       ----------------
               Class 1      5%          50%
               Class 0     10%           -
               ------------------------------------------------------------

        In all the CFRS science analyses, the Class 1 unreliable
        "identifications" have been treated as being "unidentified"
    Note (5): Features noted in the spectra. These are largely self-explanatory,
    Note (5): Features noted in the spectra. These are largely self-explanatory,
        except that a "1" indicates that the continuum shape supported the
        identification in cases in which the number of distinct features was
        small and a "2" indicates the multiple features of an M star.
          C indicates continuum
          b indicates break
          a for 4863a line
          ? for uncertainty
        It should be noted that the listed features were "seen" at the
        indicated redshift. They are not necessarily all of such strength as
        to significantly confirm the redshift.
    Note (6): the CFRS identification is of the form HH.NNNN, where
        HH represents the field hour:
        00 for the field at 0000-00 (1995ApJ...455...60L,  90 sources)
        03 for the field at 0300+00 (1995ApJ...455...88H, 272 sources)
        10 for the field at 1000+25 (1995ApJ...455...60L, 210 sources)
        14 for the field at 1415+52 (1995ApJ...455...75L, 239 sources)
        22 for the field at 2215+00 (1995ApJ...455...75L, 199 sources)

    History:
        Copied at http://www.astro.utoronto.ca/~lilly/CFRS
      * 13-Aug-2002: Added the '*' for galaxies also studied in papers XI and XIV.
      * 30-May-2008: Added the files "astro.dat" and "photo.dat"
        from http://www.oamp.fr/people/tresse/cfrs/cfrs.html

    References:
        Lilly S.J. et al.,  Paper I      =1995ApJ...455...50L
        Le Fevre O. et al.. Paper II     =1995ApJ...455...60L, Cat. J/ApJ/455/60
        Lilly et al.,       Paper III    =1995ApJ...455...75L, Cat. J/ApJ/455/75
        Hammer F. et al.,   Paper IV     =1995ApJ...455...88H, Cat. J/ApJ/455/88
        Crampton D. et al., Paper V      =1995ApJ...455...96C
        Lilly S. J. et al., Paper VI     =1995ApJ...455..108L
        Hammer F. et al.,   Paper VII    =1995MNRAS.276.1085H
        Le Fevre O. et al., Paper VIII   =1996ApJ...461..534L
        Schade D. et al.,   Paper IX     =1995ApJ...451L...1S
        Schade D. et al.,   Paper X      =1996MNRAS.278...95S
        Schade D. et al.,   Paper XI     =1996ApJ...464...79S, Cat. J/ApJ/464/79
        Tresse L. et al.,   Paper XII    =1996MNRAS.281..847T
        Le Fevre et al.,    Paper XIII   =1996BCFHT..34...10L
        Hammer et al.,      Paper XIV    =1997ApJ...481...49H, Cat. J/ApJ/481/49
    ================================================================================
    (End)                                   Francois Ochsenbein [CDS]    13-Nov-2001