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
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 (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 χ2 of the W1 profile fit 214-220 F7.1 --- snr2 ? Signal to noise ratio for W2 filter 222-230 E9.3 --- chi2W2 ? Reduced χ2 of the W2 profile fit 232-238 F7.1 --- snr3 ? Signal to noise ratio for W3 filter 240-248 E9.3 --- chi2W3 ? Reduced χ2 of the W3 profile fit 250-257 F8.1 --- snr4 ? Signal to noise ratio for W4 filter 259-267 E9.3 --- chi2W4 ? Reduced χ2 of the W4 profile fit 269-277 E9.3 --- chi2 All-band combined reduced χ2 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 ? Proper motion in RA 421-427 I7 mas/yr e_pmRA ? Mean error on pmRA 429-435 I7 mas/yr pmDE ? Proper motion in DE 437-443 I7 mas/yr e_pmDE ? Mean error on pmDE 445-453 E9.3 --- chi2W1_pm ? Reduced χ2 of the W1 profile fit including motion estimation 455-463 E9.3 --- chi2W2_pm ? Reduced χ2 of the W2 profile fit including motion estimation 465-473 E9.3 --- chi2W3_pm ? Reduced χ2 of the W3 profile fit including motion estimation 475-483 E9.3 --- chi2W4_pm ? Reduced χ2 of the W4 profile fit including motion estimation 485-493 E9.3 --- chi2pm ? Combined reduced χ2 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-σ in RA and Dec (sigra, sigdec) and the co-σ sigradec with the formulae: Δ = (sigra2-sigdec2)2 + 4*sigradec2 eeMaj2 = 0.5*(sigra2+sigdec2+sqrt(Δ)) eeMin2 = 0.5*(sigra2+sigdec2-sqrt(Δ)) 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.
History: From http://wise2.ipac.caltech.edu/docs/release/allwise/expsup/sec2_1a.html
(End) Laurent Cambresy [CDS] 29-Jan-2014
|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|