The NOAO Source Catalog (NSC) is a catalog of nearly all of the public imaging data in NOAO's 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 first NSC public data release (DR1) contains over 2.9 billion unique objects, 34 billion individual source measurements, covers ~30,000 square degrees of the sky, has depths of ~23rd magnitude in most broadband filters with ~1-2% photometry, and an astrometric accuracy of ~2 mas. The NSC will be useful for exploring stellar streams, dwarf satellite galaxies, as well as variable stars and other transients. Browse these pages to learn more about the NSC and how to access the data. The NSC DR1 overview paper (Nidever et al. 2018) describes the catalog in detail, including its the source extraction, calibration, combination, quality assurance, and science use cases.
|NSC at a glance|
|Area covered||30,382 deg2|
|Bands||u, g, r, i, z, Y, VR|
|Median Depth (10σ)||22.4, 22.9, 22.6, 22.4, 21.6, 20.4, 22.9 mag|
|Median Depth (95th%)||23.1, 23.3, 23.2, 22.9, 22.2, 21.0, 23.1 mag|
|Median seeing||1.35, 1.30, 1.18, 1.03, 1.01, 0.99, 1.15 arcsec|
|Number of exposures||255,454|
|Number of objects||2,930,644,736|
|Number of individual measurements||34,658,213,888|
|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.
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.
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.
Proper motions of objects can be used to study the movements of moving groups of stars in the Milky Way galaxy among other things.
The NSC information can be used to study all of these phenomena across essentially the entire sky.
- 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.
Back to Top
- Coverage. Coverage information for each nside=4096 healpix pixel with a resolution of ~1 arcmin. This gives coverage fraction and depth for each band. 201,326,592 rows.
- Chip. Information for each unique chip image with astrometric correction terms and uncertainties. 12,008,634 rows.
- Exposure. Information for each unique exposure with zero-point values and uncertainties. 255,454 rows.
- Object. Information on each unique object with average photometric and astrometric values. 2,930,644,736 rows.
Information on each individual source measurement. 34,658,213,888 rows.
This table will be available as soon as is feasible.
- 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 -30 degrees declination the Pan-STARRS1 DR1 catalog was used. For the rest of the exposures, model magnitudes were constructed from Gaia DR1, 2MASS, GALEX, and APASS and an extinction term using the Schlegel, Finkbeiner & David (1998) reddening map. The astrometry of each chip was calibrated using the Gaia DR1 catalog.
- 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. Sources were crossmatched and their average magnitudes and morphological parameters (in each band) were computed. Finally, proper motions and the photometric variability in each band were also calculated.
Back to Top