The first release of SDSSMOC includes all data obtained up to Dec 15, 2001. The catalog includes data for 58,117 moving objects from 87 observing runs that roughly cover the area included in the upcoming SDSS Data Release 1 (January 1, 2003). SDSSMOC will be updated about once a month (i.e. once per every dark run), with a time delay of about 1-3 weeks between the observations and public release. This time delay is mandated by the minimum time needed for data processing and quality assurance procedures.
The catalogs includes various identification parameters, SDSS astrometric measurements (position and velocity, with errors), SDSS photometric measurements (five SDSS magnitudes and their errors), and orbital information for previously cataloged asteroids.
WHERE ( (objFlags & (OBJECT_SATUR | OBJECT_BRIGHT | OBJECT_BLENDED)) == 0 && (objFlags & OBJECT_DEBLENDED_AS_MOVING) > 0 && (objc_type == 6) && (psfCounts > 14.5) && (psfCounts < 21.5) && (rowv*rowv + colv*colv > 0.0025) && (rowv*rowv + colv*colv < 0.25) )The first line excludes all saturated and "bright" objects (the latter are always duplicates of physical objects produced by processing software), and the second line requires that the object was recognized as a moving object by SDSS photometric pipeline (Lupton et al. 2002, in prep; see also a paper about SDSS moving objects by Ivezic et al. 2001, hereafter Paper I). The third and fourth lines require that the object is unresolved and brighter than r=21.5, and the last two conditions require that the magnitude of the object's velocity vector is larger than 0.05 deg/day and smaller than 0.5 deg/day. Note that some of these entries are multiple observations of the same objects (see Section 3.3. in Paper I).
The completeness (number of moving objects detected by the software that are included in the catalog, divided by the total number of moving objects recorded in the images, for details see Juric et al. 2001, hereafter Paper II) of this catalog is about 90%, and its contamination rate is about 3% (the number of entries that are not moving objects, but rather instrumental artifacts, for details see Paper I). That is, about 6,000 observed moving objects were missed by the processing software, and about 2,000 catalog entries are instrumental and software artifacts.
Using these supplemental orbital data, the SDSS colors can be used to produce informative plots of asteroid distribution in orbital parameter space; e.g. see a "colorful" plot of asteroid distribution in the proper inclination vs. semi-major axis plane. Details about this plot can be found in Ivezic et al. 2002, Paper III (pdf).
|-- SDSS identification --|
|1||1 - 7||moID||Unique SDSS moving-object ID|
|2||8 - 13||Run||SDSS object IDs, for details see SDSS EDR paper|
|3||14 - 15||Col|
|4||16 - 20||Field|
|5||21 - 26||Object|
|6||27 - 35||rowc||Pixel row|
|7||36 - 44||colc||Pixel col|
|-- Astrometry --|
|8||47 - 59||Time (MJD)||Modified Julian Day|
|9||60 - 70||R.A.||J2000 right ascension of the object at the time of the (r band) SDSS observation|
|10||71 - 81||Dec||J2000 declination of the object at the time of the (r band) SDSS observation|
|11||82 - 92||Lambda||Ecliptic longitude at the time of observation|
|12||93 - 103||Beta||Ecliptic latitude at the time of observation|
|13||104 - 115||Phi||Distance from the opposition at the time of observation|
|14||117 - 124||vMu||The velocity component parallel to the SDSS scanning direction, and its error (deg/day)|
|15||125 - 131||vMu Error|
|16||132 - 139||vNu||The velocity component perpendicular to the SDSS scanning direction, and its error (deg/day)|
|17||140 - 146||vNu Error|
|18||147 - 154
|| The velocity component parallel to the Ecliptic
|19||155 - 162
|| The velocity component perpendicular to the Ecliptic
|-- Photometry --|
|20||164 - 169||u||SDSS u'g'r'i'z' psf magnitudes and corresponding errors|
|21||170 - 174||uErr|
|22||175 - 180||g|
|23||181 - 185||gErr|
|24||186 - 191||r|
|25||192 - 196||rErr|
|26||197 - 202||i|
|27||203 - 207||iErr|
|28||208 - 213||z|
|29||214 - 218||zErr|
|30||219 - 224||a||a* color = 0.89 (g - r) + 0.45 (r - i) - 0.57 (see Paper I)|
|31||225 - 229||aErr|
|32||231 - 236||V||Johnson-V band magnitude, synthetized from SDSS magnitudes|
|33||237 - 242||B||Johnson-B band magnitude, synthetized from SDSS magnitudes|
|-- Identification --|
|34||243 - 244||Identification flag||Has this moving object been linked to a known asteroid (0/1)? See Paper II.|
|35||245 - 250||Numeration||Numeration of the asteroid. If the asteroid is not numbered, or this moving object has not yet been linked to a known asteroid, it's 0.|
|36||251 - 271||Designation||Asteroid designation or name. If this moving object has not yet been linked to a known asteroid, it's '-'|
|37||272 - 274
||Detection counter of this object in SDSS data
|38||275 - 277||Total Detection Count||Total number of SDSS observations of this asteroid|
|39||278 - 286||Flags||Flags that encode SDSSMOC processing information (internal)
|-- Matching information --|
|40||288 - 298||Computed R.A.||Predicted position and magnitude at the time of SDSS observation for an associated known object computed using ASTORB data|
|41||299 - 309||Computed Dec|
|42||310 - 315||Computed App. Mag.|
|43||317 - 324||R||Heliocentric distance at the time of observation|
|44||318 - 325||Geocentric||Geocentric distance at the time of observation|
|45||333 - 338||Phase||Phase angle at the time of observation|
|-- Osculating elements --|
|46||340 - 350||Catalog ID||Identification of the catalog from which the osculating elements and (H, G) values were extracted|
|47||361 - 366||H||Absolute magnitude and slope parameter|
|48||367 - 371||G|
|49||372 - 377||Arc||Arc of observations used to derive the elements|
|50||378 - 391||Epoch||Osculating elements|
|51||392 - 404||a|
|52||405 - 415||e|
|53||416 - 426||i|
|54||427 - 437||Lon. of asc. node|
|55||438 - 448||Arg. of perihelion|
|56||449 - 459||M|
|-- Proper elements --|
|57||461 - 481||Proper elements catalog ID||Identification of the catalog from which the proper elements were extracted|
|58||482 - 494||a'||Proper elements|
|59||495 - 505||e'|
|60||506 - 516||sin(i')|
Unique SDSS moving-object ID (e.g. s0456d) is a coded representation (hash table) of an observation based on SDSS run number and equatorial position on a 1x1 arcsec grid (the limit of 6 digits is stipulated by the Minor Planet Center observation report form). Note that this ID describes SDSS observations, and not physical objects. Thus, the same object can be associated with multiple IDs; one for each SDSS observation.
MJD (TAI) when row 0 of the r frame was read. To get true mean observation time for an object, add (3.0471e-07 * rowc) days to mjd, where rowc is listed in the catalog (field 6) for each object.
Johnson V band magnitude is computed from SDSS photometry using
V = r + 0.44*(g-r) - 0.02
Johnson B band magnitude is computed from SDSS photometry using
B = V + 1.04*(g-r) + 0.19The accuracy of these transformations is better than 0.05 mag (Fukugita et al. 1996, Astronomical Journal, 111, 1748).
Identification for ASTORB file A string of the form ASTORB_YYYYMMDD, where YYYYMMDD is the release date for ASTORB file used in matching.
Identification for file with proper orbital elements A string of the form ASTDYS_?_YYYYMMDD, where YYYYMMDD is the issue date of file used in matching, and ? can be either N (numbered objects) or U (unnumbered objects).
In all string field values blanks have been replaced with underscores. For example, the designation "1998 RH41" is encoded as "1998_RH41", This allows the record to be read as a series of blank-delimited fields.
All magnitudes that were not properly measured were replaced by 99.99, and all errors that were not properly measured were replaced by 9.99.
To this program, save it first in a file called sademo.c, then compile it as
cc sademo.c -o sademoand run it as
./sademo filenamewhere "filename" stands for the catalog file name. The output for file ADR1.dat should look like
> ./sademo ADR1.dat Parsed file ADR1.dat [58118 lines] Total moving objects : 58117 Blue : 22084 Red : 35974 Color unknown : 59 Identified : 12602
Funding for the creation and distribution of the SDSS Archive has been
provided by the Alfred P. Sloan Foundation, the Participating
Institutions, the National Aeronautics and Space Administration, the
National Science Foundation, the U.S. Department of Energy, the Japanese
Monbukagakusho, and the Max Planck Society. The SDSS Web site is
The SDSS is managed by the Astrophysical Research Consortium (ARC) for
the Participating Institutions. The Participating Institutions are The
University of Chicago, Fermilab, the Institute for Advanced Study, the
Japan Participation Group, The Johns Hopkins University, Los Alamos
National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the
Max-Planck-Institute for Astrophysics (MPA), New Mexico State
University, University of Pittsburgh, Princeton University, the United
States Naval Observatory, and the University of Washington.
The SDSS is managed by the Astrophysical Research Consortium (ARC) for the Participating Institutions. The Participating Institutions are The University of Chicago, Fermilab, the Institute for Advanced Study, the Japan Participation Group, The Johns Hopkins University, Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, University of Pittsburgh, Princeton University, the United States Naval Observatory, and the University of Washington.
If you write a paper based on this catalog, please let us know and we will add it to the list of other SDSS-based asteroid publications. This way we will minimize the chance for repeating someone else's work, and will also have a convenient way to access all related papers. The current list is available here.
Thank you very much,
Zeljko Ivezic (1) Mario Juric (1,2,3) Robert Lupton (1) Serge Tabachnik (1) Tom Quinn (4) and the SDSS Collaboration (1) Princeton University (2) Zagreb University (3) Visnjan Observatory (4) The University of Washington
SDSSMOC data files
Each data file has identical format, as described above. As the new data become available, we will update the list below with additional catalogs.
ADR1.dat: the first release (gzip); based on these runs.
Erratum for ADR1.dat: The 'Proper elements catalog ID' field is incorrect. It should be ASTDYS_N_20010915 and ASTDYS_U_20010915, instead of ASTDYS_N_20000601 and ASTDYS_U_20000601, respectively.
Run Lists for Released Catalogs
The files linked below provide basic information about each SDSS observing run used in producing SDSSMOC files. The file names correspond to SDSSMOC file names, with suffix ".dat" replaced by ".runList". Each file has 8 columns that list the run number, run, the starting equatorial position of the (0,0) pixel in camera column 1 (in degrees, RA and Dec), the modified Julian Day for the beginning and the end of the run (MJDstart and MJDend), its node and inclination (in degrees, node and inclination) relative to the equatorial coordinate system (see SDSS EDR paper), and the starting great circle coordinates (so-called mu and nu coordinates, mu is measured along the scan, and nu perpendicularly to the scan) for the (0,0) pixel in camera column 1 (in degrees, mu0 and nu0). The last two quantities are redundant, and can be reproduced using RA, Dec, node, and inclination; they are added for testing coordinate transformations; for convenience, we provide relevant C functions used by SDSS software pipelines.
The sky region covered by a run can be obtained using the above information for the (0,0) pixel in camera column 1, and the layout of the camera. The nu range spanned by the six camera columns, relative to the (0,0) pixel in camera column 1, is (in degrees):
column nuMin nuMax 1: 0.000000 0.225269 2: 0.419741 0.645077 3: 0.839260 1.064554 4: 1.258912 1.484212 5: 1.678480 1.903806 6: 2.098364 2.323656
ADR1.runList: the run list for ADR1.dat
Please send us your comments or suggestions.