SDSS DR6 Sources
(Latest revision: 22 July 2017)
The Sloan Digital Sky Survey (SDSS) Data Release 6 (DR6) photometric catalog was downloaded via CasJobs from https://cas.sdss.org/dr6/en/. More information on SDSS DR6 can be found at https://classic.sdss.org/dr6/.
Format: SDSS JHHMMSS.ss+/-DDMMSS.s
Example: SDSS J133840.44+481704.9
There are a total of 217 million objects in the SDSS DR6 photometric catalog, out of which 154 million objects were integrated into NED. This subset was selected using the following "Clean sample" filters based on the recommendations for clean sample of point sources by the SDSS team:
- All objects with SDSS PRIMARY status bit set, and SDSS flags set as follows
- and not BRIGHT
- and (not BLENDED or NODEBLEND)
- and not NOPROFILE
- and not (PEAKCENTER or NOTCHECKED
or (DEBLEND_NOPEAK and r-band PSF mag err > 0.2))
- and not DEBLENDED_AS_MOVING
We did not filter out objects with the SATURATED flag set, because although
SDSS photometry is unreliable for such sources,
this would have omitted useful SDSS positions and size measurements for
galaxies with bright nuclei, including many nearby Seyfert galaxies.
The requirement that Status=PRIMARY excluded objects
with Status=FAMILY that were de-blended by the pipeline into smaller components
(these CHILD objects themselves have Status=PRIMARY),
and also excluded repeated observations with Status=SECONDARY.
SDSS classified each object as either a "galaxy" or "star", depending
on whether the pipeline
determined it to be resolved (extended) or unresolved (a point source).
Along with objects of type "galaxy", objects of type "star" were also
folded into NED,
because this SDSS classification is strictly morphological and includes many
that are actually QSOs and unresolved, compact galaxies. Whenever possible,
both types of SDSS objects
were cross-matched to objects in the previous version of NED
(which had ~10 million objects
total, including ~4 million objects within the SDSS footprint) using our
standard position- and data-matching procedures.
Please see this note
about corrections to the u band (CModel only) and z band (PSF and Model only)
magnitudes and flux densities.
SDSS data in NED include:
- Multiwavelength cross-identifications with observations from tens of thousands of catalogs and journal papers.
(Example: multiwavelength cross-IDs with SDSS J074906.51+451033.9)
- Basic Data, including representative g-band magnitudes, positions, and classifications
(Example: SDSS J133840.44+481704.9)
- Position measurements in the r band (Example: SDSS J133936.13+430238.7)
- Size measurements in the r band using 4 methods: Isophotal, Petrosian, de Vaucouleurs, and Exponential
(Example: SDSS J133934.97+430351.0)
- Photometric measurements in all 5 bands [ugriz], each with 3 methods
(PSF, Model, CModel) for extended objects (Example: SDSS J135554.50+454822.6)
and with one method (PSF) for point sources (Example: SDSS J133933.60+430228.5), have been folded into NED's SEDs
- Links to SDSS SkyServer
pipeline processing flags, spectra and images for each object (Example: SDSS J074906.50+451033.9). Additional links to DR7, DR8, DR9, and DR12 are also
available in the "Detailed Information" section of each SDSS object.
- SDSS measurements for large galaxies, including a subset of objects with
from the standard SDSS pipeline and measurements derived from custom mosaics such as those produced
for selected galaxies in the RC3 by David Hogg at NYU.
With over 1.7 billion detailed photometric measurements (PSF, Model and
CModel magnitudes for galaxies) in five bands, and hundreds of millions of diameter and position measurements, as well as
crucial flags from the pipeline processing, folding in SDSS DR6 (the "Clean Sample" subset described above) expanded NED's tabular database
volume (in 2007) by a factor of ~200.
- While we carefully checked the resulting database of about 163 million
objects, there are certain to be anomalies included. Many SDSS objects,
for example, are parts of galaxies covering a major portion of a spiral arm.
These may be cross-matched to radio sources or H II regions with relatively
large position uncertainties that coincidentally overlap the much smaller
position error ellipses of the SDSS objects.
- Some DR6 objects have either no counterparts among
objects previously in NED, or generally reliable cross-identifications with
objects previously in NED based on observations across the EM spectrum.
However, hundreds of thousands of SDSS objects were determined by our
cross-comparison software to be possible (candidate) matches with other
objects in NED. In addition, there are
many cases in which multiple SDSS objects may be associated with single objects
observed with lower resolution (e.g., radio, UV, or X-ray surveys).