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HERS82CAT Catalog

This study presents the first set of maps and band-merged catalog from the Herschel Stripe 82 Survey (HerS). Observations at 250, 350, and 500 micron (µm) were taken with the Spectral and Photometric Imaging Receiver (SPIRE) instrument onboard the Herschel Space Observatory. HerS covers 79 square degrees along the SDSS Stripe 82 to an average depth of 13.0, 12.9, and 14.8 mJy beam-1 (including confusion) at 250, 350, and 500 um, respectively. HerS was designed to measure correlations with external tracers of the dark matter density field, either point-like (i.e., galaxies selected from radio to X-ray) or extended (i.e., clusters and gravitational lensing), in order to measure the bias and redshift distribution of intensities of infrared-emitting dusty star-forming galaxies and active galactic nuclei. By locating HerS in Stripe 82, the authors maximize the overlap with available and upcoming cosmological surveys. The band-merged catalog contains 3.3 x 104 sources detected at a significance of >~ 3 sigma (including confusion noise). The maps and catalog are available at http://www.astro.caltech.edu/hers/.

This table contains the first HerS band-merged point source catalog based on observations covering 79 deg2 in the equatorial Stripe 82, spanning 13 to 37 degrees (0h 54m to 2h 24m ) in RA, and -2 to +2 degrees in Declination. The SPIRE beams are 18.1, 25.2 and 36.6 arcseconds at 250, 350 and 500 um, respectively. The band-merged catalog was constructed, after filtering, with DESPHOT (Roseboom et al. 2010, MNRAS, 409, 48), using 250-um sources (extracted with STARFINDER: Diolaiti et al. 2000, A&AS, 147, 335) as positional priors. The authors included sources with S/N greater than 3, whose completeness is estimated to be 50% (see Figure 7 of the reference paper), with a false detection rate less than 1%, and which had reasonable residuals (i.e., chi2 < 10). Next, they identified obviously extended sources - 24 in total - where their extended nature resulted in them being broken up into multiple components by the filter, and removed them. This results in a catalog with 32,815 sources at 250 um, of which 13,300 and 3,276 have similarly defined 3-sigma detections at 350 and 500 um, respectively. The authors expect a false positive rate of 1.2 +/- 0.2 deg-2 : thus, across the 79 deg2 of HerS, they expect 96 +/- 16 spurious sources.

The following local extended sources were removed: 

Name, RA, DEC
NGC 0493,20.537458,0.945361
UGC 00890,20.283333,1.373333
UGC 00892,20.319166,-0.544491
NGC 0428,18.232125,0.981556
NGC 0799,30.551407,-0.100629
NGC 0800,30.549358,-0.130432
NGC 0450,18.876840,-0.860973
NGC 0497,20.599064,-0.875207
NGC 0867,34.269910,1.244202
UGC 01725,33.607833,1.469833
NGC 0570,22.244325,-0.948996
UGC 00711,17.153750,1.641667
UGC 00726,17.489833,-1.749694
NGC 0550,21.677292,2.022361
NGC 0585,22.9255833,-0.9333056
UGC 01123,23.533209,-1.032286
2MASX J01434929-0048547,25.955091,-0.815256
NGC 0856,33.409831,-0.717287
UGC 01698,33.082019,-0.811513
CGCG 385-007,17.256708,1.378194
UGC 00790,18.657792,1.180167
2MFGC 01002,19.930083,1.630778
2MFGC 00979,19.642792,1.747889
UGC 00847,19.768317,-0.138572

HERSCHLLOG Catalog

The Herschel Space Observatory (Herschel) is an ESA (European Space Agency) project with instruments funded by ESA member states. It was operated from May 2009 till April 2013, offering unprecedented observational capabilities in the far-infrared and sub-millimeter spectral range (55-671 microns [um]). Herschel carried a 3.5m diameter passively cooled Cassegrain telescope, which was the largest of its kind and utilizes a novel silicon carbide technology. The science payload comprised three instruments: two direct detection cameras/medium resolution spectrometers, the Photodetector Array Camera and Spectrometer (PACS) and the Spectral and Photometric Imaging Receiver (SPIRE), and a very high-resolution heterodyne spectrometer, the Heterodyne Instrument for the Far Infrared or HIFI, whose focal plane units were housed inside a superfluid helium cryostat.

PACS comprised two mutually exclusive sub-instruments: a bolometric camera designed to perform photometry in three spectral bands (70, 100 and 160 um) and an integral field unit grating spectrometer operating over the spectral range from 57 to 210 um with a spectral resolution ranging from 1000 to 5000.

SPIRE comprised a three-band photometer, operating in spectral bands centered on 250, 350 and 500 um, and an imaging Fourier-Transform Spectrometer (FTS), which provided low resolution spectra over the 195-670 um band. Both instruments used germanium bolometers operating at 0.3 K and coupled to the telescope with hexagonally conical feedhorns. The photometer and the spectrometer were not designed to operate simultaneously.

HIFI was designed to obtain spectra with very high resolution (up to 107) in the far-infrared and sub-millimeter wavelengths not directly observable by ground-based telescopes. The HIFI instrument was an heterodyne receiver which provided spectroscopy in the continuous frequency range 480-1250 GHz (240-625 microns) and in the frequency range 1410-1910 GHz (157-213 microns).

Herschel had two Announcement of Opportunities (AOs) for Open Time (OT) observations. The first in-flight AO for Open Time (OT1) was opened on 20 May 2010, with a deadline of 22 July 2010. For OT1, 241 observing programs were accepted and the total allocated observing time amounts to 6576.9 hours. The second in-flight AO for Open Time (OT2) was opened on 9 June 2011, with a deadline of 15 September 2011. There were parallel AOs for Guaranteed Time observations, GT1 and GT2, with separate deadlines.

The Announcement of Opportunity (AO) for Herschel Key Programs (KP) was issued on 1 February 2007, with separate deadlines for guaranteed time (GT) and open time (OT) proposals. The whole Key Program AO process has now been completed, and by coincidence there were exactly the same number of KP GT and OT programs, in both cases 21 programs were awarded observing time. Taken together, these 42 observing programs contained 11,650 astronomical observation requests or AORs (AORs are the primary units of Herschel observing time and are effectively the Herschel 'observation units'). The total allocated observing time for these programs was 11,257.7 hours, corresponding to approximately 57% of the nominally available Herschel routine mission science time.

Herschel successfully made over 37,000 scientific observations before its helium cryogen was exhausted.

The HSA is available at the Herschel Science Centre at http://herschel.esac.esa.int/Science_Archive.shtml, the Herschel help desk is at http://herschel.esac.esa.int/esupport/, the Herschel User Provided Data Products are available at http://herschel.esac.esa.int/UserProvidedDataProducts.shtml, the Herschel Postcard Server is at http://archives.esac.esa.int/hsa/aio/doc/postcardGallery.html, and the Herschel Observation Log is athttp://herschel.esac.esa.int/logrepgen/observationlist.do

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