A NEWFIRM Survey of the SDWFS/NDWFS Field
Anthony Gonzalez (U Florida)
Mark Brodwin (NOAO)
Daniel Stern (JPL/Caltech)
Jamie Bock (JPL/Caltech)
Michael Brown (Monash U.)
Shane Bussman (U. Arizona)
Asantha Cooray (UC-Irvine)
Mark Dickinson (NOAO)
Peter Eisenhardt (JPL/Caltech)
Buell Jannuzi (NOAO)
Yen-Ting Lin (Princeton/Catolica)
S. Adam Stanford (IGPP/LLNL, UC Davis)
Ian Sullivan (Caltech)
Mike Zemcov (JPL)
Infrared Bootes Imaging Survey: Data Release 2
The Infrared Bootes Imaging Survey is a near-infrared imaging survey covering the entire Spitzer Deep Wide-Field Survey (SDWFS) region, which corresponds to the Bootes field of the NOAO Deep Wide-Field Survey. regions. This public release includes data from 52 subfields that together span the region, and that overlap with one another by roughly 2 arcmin on each side. We provide both the final reduced images and J-band selected, line matched catalogs for all subfields. Along with these images, we also provide weight maps from the SWARP software, and flag images denoting regions with poor data. Specifically, in the flag images regions in which the weights are less that 25% of the median value are given a value of 1001, while all other pixels have a value of 0. The typical field reaches a 5-sigma depth of roughly J=22, H=20.8, Ks=19.5 within a 3 arcsecond diameter aperture. We note however that the depth is variable, and that our team obtained significantly deeper data in some subfields. The zeropoints for the images, which are on the Vega system(**see addendum below**), were calibrated using 2MASS photometry and stellar locus regression(High et al. 2009, AJ, 138, 110) was used to ensure accurate colors for the three bands. The quoted FWHM values are taken directly from Source Extractor.
The catalogs provide all basic astrometric, photometric, and shape information, including magnitudes within a series of 13 apertures ranging in diameter from 1-20 arcsec. We also use a curve of growth analysis for bright stars in each field to compute an estimate of the correction necessary to convert to total magnitude for each aperture. These values, which are not applied to the catalog, are included at the end of the catalog headers.
The paper describing the survey is in preparation, and should be available in early 2011. If you use the images or catalogs from the survey in your research or publications, we ask that you please cite either this paper: ``The Infrared Bootes Imaging Survey", Gonzalez et al. 2011 (in prep). If you have additional questions, please feel free to contact the PI via email (Anthony Gonzalez).
Addendum (3/9/2011): There is one important clarification regarding the zeropoints. The zeropoints derived from the stellar locus regression are such that they provide accurate mean colors for the stellar locus. Due to color terms, these zeropoints do not yield m=0 for Vega. To obtain true Vega magnitudes with m=0 for Vega in all bands requires subtraction of 0.056 mag in J and 0.007 mag in H (Ks is unchanged). This is true for both the images and photometric catalogs.