ACDS V10.0 - Detailed Description of II/328

ACDS V10.0 - Mon Jan 20 09:36:51 CET 2025

| # Detailed Description of II/328 : AllWISE Data Release (Cutri+ 2013) |

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.

    II/328              AllWISE Data Release                           (Cutri+ 2013)
    ================================================================================
    AllWISE Data Release
         Cutri R.M., Wright E.L., Conrow T., Fowler J.W., Eisenhardt P.R.M.,
         Grillmair C., Kirkpatrick J.D., Masci F., McCallon H.L., Wheelock S.L.,
         Fajardo-Acosta S., Yan L., Benford D., Harbut M., Jarrett T., Lake S.,
         Leisawitz D., Ressler M.E., Stanford S.A., Tsai C.-W., Liu F., Helou G.,
         Mainzer A., Gettngs D., Gonzalez A., Hoffman D., Marsh K.A., Padgett D.,
         Skrutskie M.F., Beck R., Papin M., Wittman M.
        <IPAC/Caltech (2013)>
        =2014yCat.2328....0C
    ================================================================================
    ADC_Keywords: Infrared sources ; Photometry, infrared ; Surveys

    Mission_Name: WISE

    Description:
        The Wide-field Infrared Survey Explorer (WISE; see Wright et al.
        2010AJ....140.1868W) is a NASA Medium Class Explorer mission that
        conducted a digital imaging survey of the entire sky in the 3.4, 4.6,
        12 and 22um mid-infrared bandpasses (hereafter W1, W2, W3 and W4).
        The AllWISE program extends the work of the successful Wide-field Infrared
        Survey Explorer mission by combining data from the cryogenic and
        post-cryogenic survey phases to form the most comprehensive view of the
        mid-infrared sky currently available. AllWISE has produced a new Source
        Catalog and Image Atlas with enhanced sensitivity and accuracy compared
        with earlier WISE data releases. Advanced data processing for AllWISE
        exploits the two complete sky coverages to measure source motions for
        each Catalog source, and to compile a massive database of light curves
        for those objects.

    Acknowledging WISE in publications:
        Please include the following in any published material that makes use
        of the WISE data products:

       "This publication makes use of data products from the Wide-field
        Infrared Survey Explorer, which is a joint project of the University of
        California, Los Angeles, and the Jet Propulsion Laboratory/California
        Institute of Technology, funded by the National Aeronautics and Space
        Administration."

    File Summary:

    File Summary:

           FileName      Lrecl  Records   Explanations

    ×                   80        .   This file
    × ReadMe            80        .   This file
    × allwise.sam      553     1000  *Sample of the AllWISE data release
                                 (among 747,634,026 sources)
                                 (updated version, 16-Feb-2021)

    Note on allwise.sam : the catalog described here is a subset of the full AllWISE
         catalog available from IRSA (http://irsa.ipac.caltech.edu/) with a
         selection of the columns of the full catalog.

    See also:
       http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/ : Explanatory
              Supplement to the AllWISE Data Release Products
       II/311 : The WISE All-Sky data Release (Cutri+ 2012)
       II/246 : The 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)

    Byte-by-byte Description of file:  allwise.sam

       Bytes Format Units   Label     Explanations

       1- 19  A19   ---     AllWISE   WISE All-Sky Release Catalog name,
                                        based on J2000 position,
                                        <WISEA JHHMMSS.ss+DDMMSS.s> (designation)
      21- 31  F11.7 deg     RAJ2000   Right ascension (J2000)
      33- 43  F11.7 deg     DEJ2000   Declination (J2000)
      45- 51  F7.4  arcsec  eeMaj     Semi-major axis of the error ellipse (1)
      53- 59  F7.4  arcsec  eeMin     Semi-minor axis of the error ellipse (1)
      61- 65  F5.1  deg     eePA      Position angle of the error ellipse (1)
      67- 72  F6.3  mag     W1mag     ? W1 magnitude (3.35um)
      74- 79  F6.3  mag     W2mag     ? W2 magnitude (4.6um)
      81- 86  F6.3  mag     W3mag     ? W3 magnitude (11.6um)
      88- 93  F6.3  mag     W4mag     ? W4 magnitude (22.1um)
      95-100  F6.3  mag     Jmag      ? 2MASS J magnitude (1.25um)
     102-107  F6.3  mag     Hmag      ? 2MASS H magnitude (1.65um)
     109-114  F6.3  mag     Kmag      ? 2MASS Ks magnitude (2.17um)
     116-120  F5.3  mag     e_W1mag   ? Mean error on W1 magnitude
     122-126  F5.3  mag     e_W2mag   ? Mean error on W2 magnitude
     128-132  F5.3  mag     e_W3mag   ? Mean error on W3 magnitude
     134-138  F5.3  mag     e_W4mag   ? Mean error on W4 magnitude
     140-144  F5.3  mag     e_Jmag    ? Mean error on J magnitude
     146-150  F5.3  mag     e_Hmag    ? Mean error on H magnitude
     152-156  F5.3  mag     e_Kmag    ? Mean error on Ks magnitude
     158-165  F8.3  pix     wx        x-pixel coordinate on the Atlas Image
     167-174  F8.3  pix     wy        y-pixel coordinate on the Atlas Image
     176-194  I19   ---     ID        Unique source ID
     196-202  F7.1  ---     snr1      ? Signal to noise ratio for W1 filter
     204-212  E9.3  ---     chi2W1    ? Reduced {chi}2 of the W1 profile fit
     214-220  F7.1  ---     snr2      ? Signal to noise ratio for W2 filter
     222-230  E9.3  ---     chi2W2    ? Reduced {chi}2 of the W2 profile fit
     232-238  F7.1  ---     snr3      ? Signal to noise ratio for W3 filter
     240-248  E9.3  ---     chi2W3    ? Reduced {chi}2 of the W3 profile fit
     250-257  F8.1  ---     snr4      ? Signal to noise ratio for W4 filter
     259-267  E9.3  ---     chi2W4    ? Reduced {chi}2 of the W4 profile fit
     269-277  E9.3  ---     chi2      All-band combined reduced {chi}2
         279  I1    ---     nb        [1/4] Number of PSF components used
                                         simultaneously in the profile-fitting
         281  I1    ---     na        [0/1] Active deblending flag (1 if a
                                        detection was split into multiple sources)
     283-287  F5.3  ---     sat1      ? Saturated pixel fraction in W1 (w1sat)
     289-293  F5.3  ---     sat2      ? Saturated pixel fraction in W2 (w2sat)
     295-299  F5.3  ---     sat3      ? Saturated pixel fraction in W3 (w3sat)
     301-305  F5.3  ---     sat4      ? Saturated pixel fraction in W4 (w4sat)
     307-310  A4    ---     ccf       [0DHOPdhop] Contamination and confusion
                                         flag, one per band (cc_flags) (2)
         312  I1    ---     ex        [0-5] Extended source flag (ext_flg) (3)
     314-317  A4    ---     var       Variability flag, one per band (var_flg) (4)
     319-321  I3    ---     nW1       ? Frame detection count in W1 (w1nm) (5)
     323-325  I3    ---     mW1       ? Integer frame coverage in W1 (w1m) (6)
     327-329  I3    ---     nW2       ? Frame detection count in W2 (w2nm) (5)
     331-333  I3    ---     mW2       ? Integer frame coverage in W2 (w2m) (6)
     335-337  I3    ---     nW3       ? Frame detection count in W3 (w3nm) (5)
     339-341  I3    ---     mW3       ? Integer frame coverage in W3 (w3m) (6)
     343-345  I3    ---     nW4       ? Frame detection count in W4 (w4nm) (5)
     347-349  I3    ---     mW4       ? Integer frame coverage in W4 (w4m) (6)
     351-354  I4    ---     satnum    Minimum sample at which saturation occurs
                                         in each band
     356-366  F11.7 deg     RA_pm     ? Right ascension at epoch MJD=55400.0
                                         (2010.5589) from the profile-fitting
                                         measurement model that includes motion.
     368-378  F11.7 deg     DE_pm     ? Declination at epoch MJD=55400.0
                                         (2010.5589) from the profile-fitting
                                         measurement model that includes motion.
     380-386  F7.4  arcsec  eRApm   ? Error on RA_pm
     388-394  F7.4  arcsec  eDEpm   ? Error on DE_pm
     396-403  F8.4  arcsec  cosig_pm  ? co-sigma of the equatorial position
                                         uncertainties
     405-411  I7    mas/yr  pmRA      ? Apparent motion in RA (9)
     413-419  I7    mas/yr  e_pmRA    ? Mean error on pmRA (9)
     421-427  I7    mas/yr  pmDE      ? Apparent motion in DE (9)
     429-435  I7    mas/yr  e_pmDE    ? Mean error on pmDE (9)
     437-445  E9.3  ---    chi2W1_pm  ? Reduced {chi}2 of the W1 profile fit
                                         including motion estimation
     447-455  E9.3  ---    chi2W2_pm  ? Reduced {chi}2 of the W2 profile fit
                                         including motion estimation
     457-465  E9.3  ---    chi2W3_pm  ? Reduced {chi}2 of the W3 profile fit
                                         including motion estimation
     467-475  E9.3  ---    chi2W4_pm  ? Reduced {chi}2 of the W4 profile fit
                                         including motion estimation
     477-485  E9.3  ---     chi2pm    ? Combined reduced {chi}2 profile fit
                                         including motion estimation
     487-491  A5    ---     qpm       ? Motion estimation quality (pmcode) (7)
     493-496  A4    ---     qph       [ABCUXZ] Photometric quality flag (8)
     498-499  I2    ---     fdet      [0/15] Bit-encoded integer indicating bands
                                         in which a source has a w?snr>2 detection
     501-504  I4    ---     fmoon     Scattered moonlight contamination flag
     506-512  F7.3  ---     covW1     ? Mean pixel coverage in W1
     514-520  F7.3  ---     covW2     ? Mean pixel coverage in W2
     522-528  F7.3  ---     covW3     ? Mean pixel coverage in W3
     530-536  F7.3  ---     covW4     ? Mean pixel coverage in W4
     538-547  I10   ---     2Mkey     ? 2MASS PSC association (not identification)
     549-553  F5.3  arcsec  d2M       ? Distance separating the positions of the
                                         WISE source and associated 2MASS PSC source

    Note (1): the parameters of the error ellipse are computed from the
         1-{sigma} in RA and Dec (sigra, sigdec) and the co-{sigma} sigradec
         with the formulae:
         {Delta} = (sigra2-sigdec2)2 + 4*sigradec2
         eeMaj2 = 0.5*(sigra2+sigdec2+sqrt({Delta}))
         eeMin2 = 0.5*(sigra2+sigdec2-sqrt({Delta}))
         tan(eePA) = (eeMaj2-sigdec2)/(sigradec*|sigradec|)
                   = (sigradec*|sigradec|)/(eeMaj2-sigra2)

         Conversely, the sigra/sigdec are given by:
         sigra2  = eeMaj2sin2(eePA) + eeMin2cos2(eePA)
         sigdec2 = eeMaj2cos2(eePA) + eeMin2sin2(eePA)
    Note (2): One character per band (W1/W2/W3/W4) that indicates that the
         photometry and/or position measurements of a source may be
         contaminated or biased due to proximity to an image artifact:
     D,d =  Diffraction spike. Source may be a spurious detection of or
         contaminated by a diffraction spike from a nearby bright star on
         the same image
     P,p = Persistence. Source may be a spurious detection of or contaminated
           by a latent image left by a bright star
     H,h = Halo. Source photometry may be a spurious detection of or
           contaminated by the scattered light halo surrounding a nearby
           bright source
     O,o = (letter "o") Optical ghost. Source may be a spurious detection
         of or contaminated by an optical ghost image caused by a nearby bright
         source
     0  = (number zero) Source is unaffected by known artifacts.
    Note (3): Extended source flag.
     0 = The source shape is consistent with a point-source and the source is not
         associated with or superimposed on a 2MASS XSC source
     1 - The profile-fit photometry goodness-of-fit, w?rchi2, is >3.0 in one or
         more bands.
     2 = The source falls within the extrapolated isophotal footprint of a
         2MASS XSC source.
     3 = The profile-fit photometry goodness-of-fit, w?rchi2, is >3.0 in one or
         more bands, and The source falls within the extrapolated isophotal
         footprint of a 2MASS XSC source.
     4 = The source position falls within 5" of a 2MASS XSC source.
    > 5 = The profile-fit photometry goodness-of-fit, w?rchi2, is >3.0 in one or
    >     more bands, and the source position falls within 5" of a 2MASS XSC source.
    Note (4): The variability flag is a 4-character string, one character per
         band, containing a value related to the probability that the source
         flux measured on the individual WISE exposures is variable.
      * value "n" indicates insufficient or inadequate data to make a
        determination  (<6 exposures)
      * values 0 thru 9 indicate increasing probabilities of variation;
        - values 0-5 are most likely not variable,
        - values 6-7 are likely variables (but susceptible of false-positive
          variability)
        - values >7 have the highest probability of being true variables
    Note (5): Integer frame detection count. This column gives the number of
         individual 7.7s exposures on which this source was detected with SNR>3
         in the W1 profile-fit measurement. This number can be zero for sources
         that are well-detected on the coadded Atlas Image, but too faint for
         detection on the single exposures.
    Note (6): number of individual 7.7s W1 exposures on which a profile-fit
         measurement of this source was possible. This number can differ between
         the four bands because band-dependent criteria are used to select
         individual frames for inclusion in the coadded Atlas Images. This column
         is null if there is no frame coverage in this band at the position of
         this source.
    Note (7): five character string that encodes information about factors that
         impact the accuracy of the motion estimation. These include the original
         blend count, whether a blend-swap took place, and the distance in
         hundredths of an arcsecond between the non-motion position and the
         motion mean-observation-epoch position. The format is NQDDD
         where N is the original blend count, Q is either "Y" or "N" for "yes" or
         "no" a blend-swap occurred (i.e., the original primary component was not
         the final primary component), and DDD is the radial distance between the
         non-motion and motion at mean-observation epoch positions in units of
         0.01 arcsec, clipped at 999 (almost 10 arcsec).
    Note (8): Four character flag, one character per band [W1/W2/W3/W4], that
         provides a shorthand summary of the quality of the profile-fit photometry
         measurement in each band, as derived from the measurement signal-to-noise
         ratio:
         A = Source is detected in this band with a flux signal-to-noise ratio
             w?snr>10.
         B = Source is detected in this band with a flux signal-to-noise ratio
             3<w?snr<10.
         C = Source is detected in this band with a flux signal-to-noise ratio
             2<w?snr<3.
         U = Upper limit on magnitude. Source measurement has w?snr<2. The
             profile-fit magnitude w?mpro is a 95% confidence upper limit.
         X = A profile-fit measurement was not possible at this location in this
             band. The value of w?mpro and w?sigmpro will be "null" in this band.
         Z = A profile-fit source flux measurement was made at this location, but
             the flux uncertainty could not be measured. The value of w?sigmpro
             will be "null" in this band. The value of w?mpro will be "null" if
             the measured flux, w?flux, is negative, but will not be "null" if
             the flux is positive. If a non-null magnitude is present, it
             corresponds to the true flux, and not the 95% confidence upper limit.
             This occurs for a small number of sources found in a narrow range of
             ecliptic longitude which were covered by a large number of saturated
             pixels from 3-Band Cryo single-exposures.
    Note (9): CAUTION - Note concerning "proper" motions:
             according to AllWISE documentation, the motions measured are not
             proper motions because they are affected by parallax motions.
             More information is given in:
        http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/sec2_6.html
        #HowToInterpret

    History:
     From http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/sec2_1a.html

     * 05-Feb-2014: First version
     * 16-Feb-2021: Updated version
        + Correction of column eePA: the position angle was wrongly computed as
           being north-of-east instead of east-of-north.
          The correct position angle from the previous version is thus 90-eePA
           (then transformed to match the range [0-180[ instead of ]-90, 90]).
        + Change the nW1, mW1, nW2, mW2, nW3, mW3, nW4, mW4 datatypes from one byte
           to two bytes to cover the full range of possible values
           (affects less than 1% of all rows).
    ================================================================================
    (End)             Laurent Cambresy, Patricia Vannier [CDS]           16-Feb-2021