ACDS V10.0 - Sat Apr 27 06:40:53 CEST 2019
|  | 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., et al.
    <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      561     1000  *Sample of the AllWISE data release
                             (among 747,634,026 sources)
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)
 319-322  I4    ---     nW1       ? Frame detection count in W1 (w1nm) (5)
 324-327  I4    ---     mW1       ? Integer frame coverage in W1 (w1m) (6)
 329-332  I4    ---     nW2       ? Frame detection count in W2 (w2nm) (5)
 334-337  I4    ---     mW2       ? Integer frame coverage in W2 (w2m) (6)
 339-342  I4    ---     nW3       ? Frame detection count in W3 (w3nm) (5)
 344-347  I4    ---     mW3       ? Integer frame coverage in W3 (w3m) (6)
 349-352  I4    ---     nW4       ? Frame detection count in W4 (w4nm) (5)
 354-357  I4    ---     mW4       ? Integer frame coverage in W4 (w4m) (6)
 359-362  I4    ---     satnum    Minimum sample at which saturation occurs
                                   in each band
 364-374  F11.7 deg     RA_pm     ? Right ascension at epoch MJD=55400.0
                                     (2010.5589) from the profile-fitting
                                     measurement model that includes motion.
 376-386  F11.7 deg     DE_pm     ? Declination at epoch MJD=55400.0
                                     (2010.5589) from the profile-fitting
                                     measurement model that includes motion.
 388-394  F7.4  arcsec  eRApm   ? error on RA_pm
 396-402  F7.4  arcsec  eDEpm   ? error on DE_pm
 404-411  F8.4  arcsec  cosig_pm  ? co-sigma of the equatorial position
                                     uncertainties
 413-419  I7    mas/yr  pmRA      ? Apparent motion in RA (9)
 421-427  I7    mas/yr  e_pmRA    ? Mean error on pmRA (9)
 429-435  I7    mas/yr  pmDE      ? Apparent motion in DE (9)
 437-443  I7    mas/yr  e_pmDE    ? Mean error on pmDE (9)
 445-453  E9.3  ---    chi2W1_pm  ? Reduced {chi}2 of the W1 profile fit
                                     including motion estimation
 455-463  E9.3  ---    chi2W2_pm  ? Reduced {chi}2 of the W2 profile fit
                                     including motion estimation
 465-473  E9.3  ---    chi2W3_pm  ? Reduced {chi}2 of the W3 profile fit
                                     including motion estimation
 475-483  E9.3  ---    chi2W4_pm  ? Reduced {chi}2 of the W4 profile fit
                                     including motion estimation
 485-493  E9.3  ---     chi2pm    ? Combined reduced {chi}2 profile fit
                                     including motion estimation
 495-499  A5    ---     qpm       ? Motion estimation quality (pmcode) (7)
 501-504  A4    ---     qph       [ABCUXZ] Photometric quality flag (8)
 506-507  I2    ---     fdet      [0-15] Bit-encoded integer indicating bands
                                   in which a source has a w?snr>2 detection
 509-512  I4    ---     fmoon     Scattered moonlight contamination flag
 514-520  F7.3  ---     covW1     ? Mean pixel coverage in W1
 522-528  F7.3  ---     covW2     ? Mean pixel coverage in W2
 530-536  F7.3  ---     covW3     ? Mean pixel coverage in W3
 538-544  F7.3  ---     covW4     ? Mean pixel coverage in W4
 546-555  I10   ---     2Mkey     ? 2MASS PSC association (not identification)
 557-561  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
================================================================================
(End)             Laurent Cambresy [CDS]                             29-Jan-2014