The NOIRLab Source Catalog (NSC) is a catalog of nearly all of the public imaging data in NOIRLab's Astro Data Archive. These images from telescopes in both hemispheres nearly cover the entire sky. While the large majority of these data were obtained for PI-led projects, only a fraction have been released to the community via well-calibrated and easily accessible catalogs. The NSC remedies this situation by creating a catalog of sources from most of the public data taken on CTIO-4m+DECam as well as KPNO-4m+Mosaic3 and some from the Bok-2.3+90Prime. The second NSC public data release (DR2) contains over 3.9 billion unique objects, 68 billion individual source measurements, covers ~35,000 square degrees of the sky, has depths of ~23rd magnitude in most broadband filters with ~1-2% photometry, accurate proper motions, and an astrometric accuracy of ~2 mas. The NSC will be useful for exploring stellar streams, dwarf satellite galaxies, variable stars, hight proper otion objects, QSO variability, and transients. Browse these pages to learn more about NSC DR2 and how to access the data. The NSC DR2 paper (Nidever et al. 2020) describes the catalog in detail, including the source extraction, calibration, combination, quality assurance, and science use cases. Also, see Nidever et al. 2018 for NSC DR1 information.
|NSC DR2 at a glance|
|Area covered||35,273 deg2|
|Bands||u, g, r, i, z, Y, VR|
|Median Depth (95th%)||22.6, 23.6, 23.2, 22.8, 22.3, 21.0, 23.3 mag|
|Median seeing||1.35, 1.30, 1.18, 1.03, 1.01, 0.99, 1.15 arcsec|
|Number of exposures||412,116|
|Number of objects||3,932,838,064|
|Number of individual measurements||67,822,619,019|
|Photometric calibraton accuracy||~1-2%|
|Astrometric zero-point accuracy||~2 mas|
- Local Group Dwarf Galaxies. The Milky Way is orbited by faint dwarf galaxies satellite that can be challenging to detect. The best method to discovery these objects has been with resolved stellar populations as recently demonstrated by Bechtol et al. (2015) and Drlica-Wagner et al. (2015) using DECam data from the Dark Energy Survey. The NSC includes data of resolved stellar populations for regions of the sky previously unexplored for dwarf galaxies.
- Stellar Streams. The Milky Way halo hosts a number of stellar streams from tidally stripped galaxies and globular clusters. One of the most famous streams is the Sagittarius stellar stream that stretches more than 360 degrees around the sky. Under the currently-favored hierarchical galaxy formation model, galaxies like our Milky Way are formed through the continual merging and accretion of smaller galaxies. The streams that we currently see are relics of this process. Studying these streams we can help us understand how our galaxy was formed and what its accretion history is. The NSC covers regions of the sky that have not yet been explored for stellar streams.
- High Proper Motion Objects. The NSC DR2's accurate proper motions and unrivaled combination of depth and areal coverage make it a unique resource for discovering rare moving objects such as late-type L and T subdwarfs (e.g, Kirkpatrick et al. 2014, Zhang et al. 2018). The NSC can measure motions to several magnitudes beyond the Gaia limit for sources of all colors, enabling proper motion studies in the Galactic halo, such as searches for hypervelocity stars being ejected from the Milky Way (e.g., Boubert et al. 2018).
- Solar System Objects. The NSC temporal information can be used to detect solar system objects and there is a large interest in finding near earth objects that could potentially impact the earth. In addition, there is a big search for Planet 9 and if it exists the proof could be lurking inside the NSC.
Many astronomical objects vary with time either in their brightness or position in the sky. The temporal
information in the NSC can be used to investigate the photometric astrometric variability of objects. The NSC
has ~10,000 square degrees with tens of exposures, ~1,000 square degrees with hundreds of exposures and ~50 square degrees
with thousands of exposures. NSC DR2 also includes eight precomputed photometric variability metrics to make easier
to select variable objects with 23 million objects already flagged as being variable at the 10 sigma level.
Variable stars, such as RR Lyrae, are essentially standard candles and are used to explore stellar structures in the Milky Way halo.
Active Galactic Nuclei (AGN) host supermassive black holes at the centers of galaxies and investigating their photometric variability can be used to study the accretion history of material onto the black hole as well as estimate the black hole mass.
Transient events, like supernova explosions can be used to study interesting astrophysical phenomena as well as the expansion of the universe.
The NSC information can be used to study all of these phenomena across essentially the entire sky.
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- Coverage. Coverage information for each nside=4096 healpix pixel with a resolution of ~1 arcmin. This gives coverage fraction and depth for each band. 172,157,952 rows.
- Chip. Information for each unique chip image with astrometric correction terms and uncertainties. 24,416,997 rows.
- Exposure. Information for each unique exposure with zero-point values and uncertainties. 412,116 rows.
- Object. Information on each unique object with average photometric and astrometric values. 3,932,838,064 rows.
- Measurement. Information on each individual source measurement. 67,822,619,019 rows.
- Reduction. All of the images were reduced by the NOAO Community Pipeline. The instrumentally calibrated ("InstCal") images with the instrumental signature removed were used for further analysis to create the NSC catalogs.
- Measurement. Source Extractor was run on each individual chip image to extract aperture photometry and morphological parameters. The SExtractor configuration parameters are available here and were modified slightly for each image (seeing, gain, saturation level and circular aperture sizes). In the future, we plan to perform PSF photometry on individual exposures and stacked images.
- Calibration. The zero-point for each exposure was obtained by using publicly available catalogs. For grizY exposures above -29 degrees declination the Pan-STARRS1 DR1 catalog was used. For the soutern exposures in griz bands, zeropoints were derived using ATLAS-Refcat2 stars. For u-band exposures below 0 degree declination, zeropoints were derived using Skymapper DR1. VR-band exposures were calibrated using the average of the r-band (PS1 in the north and ATLAS-Refcat2 in the south) and Gaia DR2 G magnitudes. Finally, model magnitudes were used for u-band exposures with positive declinations using GALEX, Gaia DR2 and 2MASS photometry, and for Y-band exposures with declinations below -29 deg using 2MASS photometry. Extinction values to construct dereddened colors were calculated using the Schlegel, Finkbeiner & David (1998) reddening map and RJCE method (Rayleigh-Jeans Color Excess, Majewski et al. 2011), using 2MASS, Spitzer and WISE infrared photometry, in higher extinction regions. The astrometry of each chip (the WCS) was calibrated using the Gaia DR2 catalog and corrections for proper motion to the epoch of the observation.
- Combination. Quality cuts were used to remove exposures with poor seeing, bad zero-points, large spatial variations in the zero-point, or poor astrometric calibration. Furthermore, quality cuts were also applied to the individual source meaurements that were affected by bad pixels, truncated at the edge, or had low signal-to-noise (S/N<5). Finally, measurements from multiple overlapping exposures were combined on a HEALPix (nside=128) pixel basis. The grouping algorithm of measurements into objects was substantially upgraded in DR2 to better handle faster moving stars and more robustly measure proper motions. First, the NSC DR2 measurements in a single HEALPix were clustered using DBSCAN with a clustering distance of 0.4 seconds to create object "seeds". Second, any remaining measurements were crossmatched to the seeds using a radius of three times their astrometric uncertainty. The second step is needed because DBSCAN does not take positional uncertainties into account. Average magnitudes and morphological parameters (in each band), proper motions, and photometric variability metrics were then computed for each object.
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