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II/307              WISE Preliminary Data Release         (Cutri+ 2011)

WISE Preliminary Data Release Cutri R.M., et al. <IPAC/Caltech (2011) > =2011yCat.2307....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). WISE will produce and release to the world astronomical and educational communities and general public a digital Image Atlas covering the sky in the four survey bands, and a reliable Source Catalog containing accurate photometry and astrometry for over 300 million objects. The WISE Catalog and Atlas will enable a broad variety of research efforts ranging from the search for the closest stars and brown dwarfs to the most luminous galaxies in the Universe. WISE science data products will serve as an important reference data set for planning observations and interpreting data obtained with future ground and space-borne observatories, such as JWST. WISE was launched on 2009-12-14 from Vandenberg SLC2W. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file wise.sam 342 150 Sample of the "slim" version of the WISE preliminary release (among 257,310,278 sources)
See also: http://wise2.ipac.caltech.edu/docs/release/prelim/expsup/ : Explanatory Supplement to the WISE Preliminary Data Release Products Byte-by-byte Description of file: wise.sam
Bytes Format Units Label Explanations
1- 19 A19 --- WISEP WISE Preliminary Release Catalog name, based on J2000 position (designation) 21- 29 F9.5 deg RAdeg Right ascension (J2000) 31- 39 F9.5 deg DEdeg Declination (J2000) 41- 44 F4.2 arcsec eeMaj Semi-major axis of the error ellipse (6) 46- 49 F4.2 arcsec eeMin Semi-minor axis of the error ellipse (6) 51- 53 I3 deg eePA Position angle of the error ellipse (6) 56- 61 F6.3 mag W1mag ? W1 magnitude (3.35um), Vega scale 63- 68 F6.3 mag W2mag ? W2 magnitude (4.6um), Vega scale 70- 75 F6.3 mag W3mag ? W3 magnitude (11.6um), Vega scale 77- 82 F6.3 mag W4mag ? W4 magnitude (22.1um), Vega scale 84- 89 F6.3 mag Jmag ? 2MASS J magnitude (1.2um) 91- 96 F6.3 mag Hmag ? 2MASS H magnitude (1.6um) 98-103 F6.3 mag Kmag ? 2MASS Ks magnitude (2.2um) 106-110 F5.3 mag e_W1mag ? Mean error on W1 magnitude (3.35um) 112-116 F5.3 mag e_W2mag ? Mean error on W2 magnitude (4.6um) 118-122 F5.3 mag e_W3mag ? Mean error on W3 magnitude (11.6um) 124-128 F5.3 mag e_W4mag ? Mean error on W4 magnitude (22.1um) 130-134 F5.3 mag e_Jmag ? Mean error on J magnitude 136-140 F5.3 mag e_Hmag ? Mean error on H magnitude 142-146 F5.3 mag e_Kmag ? Mean error on Ks magnitude 148-166 A19 --- cntr Unique identification number for the source 169-174 F6.1 --- snr1 ? Signal to noise ratio for W1 filter 176-184 E9.3 --- chi2W1 ? Reduced χ2 of the W1 profile fit 186-191 F6.1 --- snr2 ? Signal to noise ratio for W2 filter 193-201 E9.3 --- chi2W2 ? Reduced χ2 of the W2 profile fit 203-208 F6.1 --- snr3 ? Signal to noise ratio for W3 filter 210-218 E9.3 --- chi2W3 ? Reduced χ2 of the W3 profile fit 220-225 F6.1 --- snr4 ? Signal to noise ratio for W4 filter 227-235 E9.3 --- chi2W4 ? Reduced χ2 of the W4 profile fit 238 I1 --- nb Number of PSF components used simultaneously in the profile-fitting 240 I1 --- na [0/1] Active deblending flag (1 if a detection was split into multiple sources) 243-247 F5.3 --- sat1 [0/1] Saturated pixel fraction in W1 (w1sat) 249-253 F5.3 --- sat2 [0/1] Saturated pixel fraction in W2 (w2sat) 255-259 F5.3 --- sat3 [0/1] Saturated pixel fraction in W3 (w3sat) 261-265 F5.3 --- sat4 [0/1] Saturated pixel fraction in W4 (w4sat) 268-271 A4 --- ccf [DdPpHhOo0] Contamination and confusion flag, one per band (cc_flags) (1) 273 I1 --- ex [0/1] Extended source flag (ext_flg) (0 = consistent with point source) 275-278 A4 --- var [0-9] Variability flag, one per band (2) 286-289 I4 --- nW1 Frame detection count in W1 (w1nm) (4) 291-294 I4 --- mW1 Integer frame coverage in W1 (w1m) (5) 296-299 I4 --- nW2 Frame detection count in W2 (w2nm) (4) 301-304 I4 --- mW2 Integer frame coverage in W2 (w2m) (5) 306-309 I4 --- nW3 Frame detection count in W3 (w3nm) (4) 311-314 I4 --- mW3 Integer frame coverage in W3 (w3m) (5) 316-319 I4 --- nW4 Frame detection count in W4 (w4nm) (4) 321-324 I4 --- mW4 Integer frame coverage in W4 (w4m) (5) 326-335 I10 --- 2Mkey ? 2MASS PSC association (not identification!) 337-342 F6.3 arcsec d2M [0,3]? Distance separating the positions of the WISE source and associated 2MASS PSC source
Note (1): 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 (2): 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 "0" indicates insufficient or inadequate data to make a determination (<11 exposures) * values 1 thru 9 indicate increasing probabilities of variation; - values 1-4 are most likely not variable, - values 5-7 are likely variables (but susceptible of false-positive variability) - values >7 have the highest probability of being true variables Note (4): number of individual exposures on which this source was detected with SNR>3 in the 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 (5): number of individual exposures on which a profile-fit measurement of this source was possible. Note (6): 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)
History: From http://wise2.ipac.caltech.edu/docs/release/prelim/expsup/ Acknowledgements: Roc Cutri (IPAC/Caltech) and Laurent Cambresy (CDS)
(End) Francois Ochsenbein [CDS] 23-Jan-2012
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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