The Optical Spectra Catalogs

The data were taken as a part of several different surveys, each of which were broken up into a number of different programs. To select different programs, you should check the survey and programname tags in the specObj files or tables. For example, all the BOSS large-scale structure sample data is taken as part of the boss program in the survey boss.

The essential information (redshifts and classifications) of each object are stored in the specObj file (the specObjAll table in the CAS). The files and tables contain all spectra, which includes bad spectra as well as repeat spectra. To select the best observations of all unique objects, look for objects in specObjAll with the column "sciencePrimary" (called "specprimary" in the SAS flat files) greater than zero (i.e., true). Note that this is equivalent to the specObj view in the database (analogous to the photoObj view of the photoObjAll table for imaging data). sciencePrimary is basically designed to choose the best available unique set of spectra, in the sense that between two (or more) spectra of the same location on the sky sciencePrimary will only be set for one. Any group of spectra which are within 2 arcsec of each other are considered to be of the same object, and only one of them is designated as "sciencePrimary". The object picked as primary is the one that satisfies best the following conditions, in order of importance:

As alluded to in these conditions, there is a sense of "primary"within different surveys. Indeed, in addition to sciencePrimary there are several other indicators of primary-ness that are appropriate if you are only interested in a subset of the data:

sdssPrimary;

Indicates whether the spectrum is primary when considering only data from the SDSS spectrograph (called "specsdss" in the SAS flat files.

legacyPrimary

Indicates whether the spectrum is primary when considering only data from the SDSS Legacy survey (called "speclegacy" in the SAS flat files.

bossPrimary

Indicates whether spectrum is primary when considering only data from the BOSS survey plates (called "specboss" in the SAS flat files).

seguePrimary

Indicates whether spectrum is primary when considering only data from the SEGUE-1 and SEGUE-2 survey plates (called "specsegue" in the SAS flat files).

segue1Primary

Indicates whether spectrum is primary when considering only data from the SEGUE-1 survey plates (called "specsegue1" in the SAS flat files).

segue2Primary

Indicates whether spectrum is primary when considering only data from the SEGUE-2 survey plates (called "specsegue2" in the SAS flat files).

Note that a fiber can be primary even if it is not in a "primary"MJD for its plate as defined below; it just has to be the "best"observation of that location according to the above conditions. For example, if a group of spectra of the same location on the sky are ALL on "bad" plates (failing condition 1), one of them will still be chosen as "sciencePrimary" based on the subsequent criteria. The subsequent criteria are treated similarly.

To test if the spectrum is "good" the primary indicator to use is zWarning, which should be 0 or 16 for the data to be good with no identified problems. This flag is a bitmask, and each set bit has a particular meaning, described in our bitmask documentation. (Bit 4 is MANY_OUTLIERS, which turns out is commonly set even for perfectly good spectra).

For BOSS galaxy targets in DR9, there is a wrinkle. For these galaxy targets, a dominate source of false identifications is due to QSO templates with unphysical fit parameters (e.g., large negative parameters causing a QSO template emission feature to fit a galaxy absorption feature). Thus, for BOSS galaxy targets, the best redshift is the value of the Z_NOQSO field (with uncertainty given by Z_NOQSO_ERR, and warning flag given by ZWARNING_NOQSO), and the best classification is given by CLASS_NOQSO and SUBCLASS_NOQSO.

Other useful quality information is available in the signal-to-noise estimates (snMedian and snMedianAll) and in the estimate of plate quality (plateQuality, which is "good", "marginal" or "bad"). "bad" plates are released in the data set because there are in fact some good redshift determinations and other information in these data, but they should be used with care.

The "plates" file (and the plateX table) contain all observations of all plates, including repeats and including some low signal-to-noise plates. You can restrict that list of plates in the following way:

• To select primary, survey quality plates, look for plates with isPrimary greater than zero (IS_PRIMARY in the flat files)
• To select the best observation of each plate, including plates with no survey quality observations, look for plates with isBest greater than zero
• To select primary, survey quality tiles from SDSS Legacy, look for plates with isTile greater than zero
• To select primary, survey quality tiles from the SEGUE surveys, look for plates with isSegue greater than zero
• To simply check for plate quality, regardless of whether it is a repeat plate, "platequality" classifies plates into "bad", "marginal" and "good".

The PLATEQUALITY string is set for each observation (labeled by its MJD) of each plate. For DR9 plates the definition varies depending on whether the plate is an SDSS plate (that is, has survey set to 'sdss'), a SEGUE-1 plate (that is, has survey set to 'segue1'), a SEGUE-2 plate (that is, has survey set to 'segue2'), or a BOSS plate (survey = 'boss'). For SDSS plates, the conditions are based on the signal-to-noise and the fraction of bad pixels:

      PLATESN2>15 AND FBADPIX<0.05 -> 'good'PLATESN2>9 AND FBADPIX<0.13 -> 'marginal' (if not 'good') otherwise -> 'bad'

For SEGUE-1 plates, the conditions are based on the signal-to-noise of the main sequence turnoff at g=18, except for some special plates:

      for faint plates SN of turnoff @ g=18 > 16 for 'good'for bright plates SN of turnoff @ g=18 > 7.5 for 'good'for low-latitude or test plates, consult $SAS_DIR/data/segue1-hand.par

For SEGUE-2 plates, the conditions are also based on the signal-to-noise of the main sequence turnoff at g=18:

      median(SN for MS-turnoff @ g=18) > 10 -> 'good'otherwise -> 'bad'

For BOSS plates,

  'good' if SN2_G1 > 10.0 and SN2_G2 > 10.0 and SN2_I1 > 22.0 and SN2_I2 > 22.0 and FBADPIX < 0.10 and min(NEXP_*) ≥ 3 otherwise 'bad'

In a few cases, BOSS plates just under threshold were overridden to "good" by hand: plate-MJD 3589-55186, 3834-55569, 3841-55572, 4627-55626, 4718-55750, and 5017-55715 (a special ELG test plate). The isPrimary flag is set for each observation (labeled by its MJD) of each plate. It is "1" if we consider that MJD to be the best observation of that plate, and for it to be an acceptable observation from a science point of view (with PLATEQUALITY either 'marginal' or 'good'). It is "0" either if there is a better observation or if all observations are labeled 'bad'. The isBest flag is set for each observation (labeled by its MJD) of each plate. It is "1" if we consider that MJD to be the best observation of that plate if that observation is PLATEQUAlITY="bad". It is "0" if there is another MJD observation of that plate which is better.

Each spectroscopic object has a classification (CLASS) and a redshift determination (Z) with an associated error (Z_ERR). For galaxies, a velocity dispersion can be determined (down to about 70 km/s). The redshifts are determined by fitting models to each spectrum assuming a large range of possible redshifts. The best model is chosen on the basis of the chi-squared value of the data with respect to the model. In addition, there is a bitmask called ZWARNING which has flags set in suspicious cases. A ZWARNING equal to zero indicates no problems identified. Most bits in that mask are signs of substantial problems, suggesting that the classification and redshift are not to be trusted; the exception is the MANY_OUTLIERS bit, which can be set for successful spectra that either happen to be very high signal-to-noise ratio (e.g. bright stars) or unusual (e.g. some broad-line AGN in galaxies). The classifications are stored in the CLASS and SUBCLASS parameters. They can take the following values:

GALAXY

identified with a galaxy template; can have subclasses:

STARFORMING

set based on whether the galaxy has detectable emission lines that are consistent with star-formation according to the criteria: log₁₀(OIII/H_β) < 0.7 - 1.2*log₁₀(NII/H_α) - 0.4

STARBURST

set if the galaxy is star-forming but has an equivalent width of Hα greater than 50 Å

AGN

set based on whether the galaxy has detectable emission lines that are consistent with being a Seyfert or LINER: log₁₀(OIII/H_β) > 0.7 - 1.2*log₁₀(NII/H_α) - 0.4

QSO

identified with a QSO template

STAR

identified with a stellar template, chosen among the following subclasses: O, OB, B6, B9, A0, A0p, F2, F5, F9, G0, G2, G5, K1, K3, K5, K7, M0V, M2V,M1, M2, M3, M4, M5, M6, M7, M8, L0, L1, L2, L3, L4, L5, L5.5, L9, T2, Carbon, Carbon_lines, CarbonWD, CV

If any galaxies or quasars have lines detected at the 10-sigma level with sigmas > 200 km/sec at the 5-sigma level, the indication "BROADLINE" is appended to their subclass. As examples, the full resolution version of the figure showing the spectra on the Understanding SDSS Spectroscopic Data page lists the CLASSes, SUBCLASSes and error flags of these particular spectra. For each object, there are also detailed quality determinations, a full description of the templates used, and the targeting information. See the CAS table schema or the specObj file datamodel page for full information.