For objects in the calibrated object lists, the
photometric pipeline sets a number of flags that indicate the status
of each object, warn of possible problems with the image itself, and
warn of possible problems in the measurement of various quantities
associated with the object. For yet more details, refer to Robert Lupton's
Possible problems associated with individual pixels in the reduced
images ("corrected frames") are traced in the
Objects in the catalog have two major sets of flags:
- The status flags, called status in the
PhotoObjAll table, with information needed to discount
duplicate detections of the same object in the catalog.
- The object flags, called flags in the
PhotoObjAll table, with information
about the success of measuring the object's location, flux, or
The "status" of an object
The catalogs contain multiple detections of objects from
overlapping CCD frames. For most applications, remove duplicate
detections of the same objects by considering only those which have
the "primary" flag set in the status entry of the
PhotoObjAll table and its Views.
A description of status is provided on the details page. The details of
determining primary status and of the remaining flags stored in
status are found on the algorithms page describing the
resolution of overlaps (resolve).
The photometric pipeline's flags describe how certain measurements
were performed for each object, and which measurements are considered
unreliable or have failed altogether. You must interpret the
flags correctly to obtain meaningful results.
For each object, there are 59 flags stored as bit fields in a single 64-bit
table column called flags in the PhotoObjAll table (and its Views). There are two versions of the flag variable for each
- Individual flags for each filter u, g, r, i, z. These are called flags_u, etc.
- A single combination of the per-filter flags appropriate for the whole
object, called flags.
Note: This differs from the tsObj files in the DAS, where the individual filter flags are stored as vectors in two separate 32-bit columns called flags and flags2, and the overall flags are stored in a scalar called objc_flags.
Here we describe which flags should be checked for which measurements,
including whether you need to look at the flag in each filter, or at
the general flags.
Clean sample of point sources
In a given band, first select objects with PRIMARY status and
apply the SDSS star-galaxy separation. Then, define the following
DEBLEND_PROBLEMS = PEAKCENTER || NOTCHECKED || (DEBLEND_NOPEAK && psfErr>0.2)
INTERP_PROBLEMS = PSF_FLUX_INTERP || BAD_COUNTS_ERROR ||
(INTERP_CENTER && CR)
Then include only objects that satisfy the following in the band in
BINNED1 && !BRIGHT && !SATURATED && !EDGE && (!BLENDED || NODEBLEND) &&
!NOPROFILE && !INTERP_PROBLEMS && !DEBLEND_PROBLEMS
If you are very picky, you probably will want not to include the
NODEBLEND objects. Note that selecting
PRIMARY objects implies !BRIGHT && (!BLENDED ||
NODEBLEND || nchild == 0)
These are used in the SDSS quasar target selection code which is
quite sensitive to outliers in the stellar locus.
If you want to select very rare outliers in color space, especially
single-band detections, add cuts to MAYBE_CR and
MAYBE_EGHOST to the above list.
Clean sample of galaxies
As for point sources, but don't cut on EDGE (large galaxies
often run into the edge). Also, you may not need to worry about the
INTERP problems. The BRIGHTEST_GALAXY_CHILD may be
useful if you are looking at bright galaxies; it needs further
If you want to select (or reject against) moving objects
(asteroids), cut on the DEBLENDED_AS_MOVING flag, and then cut
on the motion itself. See the the
SDSS Moving Objects Catalog for more details. An interesting
experiment is to remove the restriction on the
DEBLENDED_AS_MOVING flag to find objects with very small proper
motion (i.e., those beyond Saturn).
Descriptions of all flags
Flags that affect the object's status
These flags must be considered to reject duplicate catalog
entries of the same object. By using only objects with
PRIMARY status (see above), you automatically
account for the most common cases: those objects which are BRIGHT, or
which have been deblended (decomposed) into one or more child objects
which are listed individually.
In the tables, Flag names link to detailed descriptions. The "In Flags?"
column indicates that this flag will be set in the general flags column if this flag is set in any of the
filters. "Bit" is the number of the bit.
To find the hexadecimal values used for testing if a flag is set, please see this table.
||detected at >=5 sigma in original imaging frame
||detected in 2x2 binned frame; often outskirts
of bright galaxies, scattered light, low surface brightness galaxies
||detected in 4x4 binned frame; few are genuine astrophysical objects
||BINNED1 | BINNED2 | BINNED4
||duplicate detection of > 200 sigma objects, discard.
||Object has more than one peak, there was an attempt to deblend
it into several CHILD objects. Discard unless NODEBLEND is set.
||Object is a blend, but was not deblended because it is:
- too close to an edge (EDGE already set),
- too large (TOO_LARGE), or
- a child overlaps an edge (EDGE will be set).
||Object is part of a BLENDED "parent" object. May be BLENDED itself.
Flags that indicate problems with the raw data
These flags are mainly informational and important only for some
objects and science applications.
||contains saturated pixels; affects star-galaxy separation
||as SATURATED, affected pixels close to the center
||object was too close to edge of frame to be measured; should not affect
||like EDGE, but for rare cases when one-half of a CCD failed
||object is near EDGE, but so large that it was deblended
anyway. Otherwise, it might have been missed.
||object contains interpolated-over pixels (bad columns, cosmic
rays, bleed trails); should not affect photometry for
single bad column or cosmic ray
||interpolated pixel(s) within 3 pix of the center. Photometry
may be affected.
||more than 20% of PSF flux is interpolated over. May cause
outliers in color-color plots, e.g.
||interpolation affected many pixels; PSF flux error is
inaccurate and likely underestimated.
||object contains cosmic rays which have been interpolated over;
should not affect photometry
||object may be a cosmic ray; not interpolated
over. Useful in searches for single-filter detections.
||object may be an electronics ghost of a bright star. Be
suspicious about faint single-filter detections.
Flags that indicate problems with the image
These flags may be hints that an object may not be real or that a
measurement on the object failed.
||could not determine a centroid in this band; used centroid in
||used brightest pixel as centroid; hint that an object may not
||object is a CHILD of a DEBLEND but has no peak; hint that an
object may not be real
||only 0 or 1 entries for the radial flux profile; photometric
quantities derived from profile are suspect
||object contains pixels which were not checked for peaks by
deblender; deblending may be unreliable
||as NOTCHECKED, but affected pixels are near object's center
||object is larger than outermost radiale profile bin (r
> 4arcmin), or a CHILD in a deblend is > 1/2
frame. Very large object, poorly determined sky, or bad
deblend. Photometry questionable.
||local sky measurement failed, object photometry is meaningless
Problems associated with specific quantities
Some flags simply indicate that the quantity in question could not be
measured. Others indicate more subtle aspects of the measurements,
particularly for Petrosian
||Stokes Q and U (isophotal shape parameters) undetermined
||no isophotal fits performed
||Petrosian radius measured at very low surface
brightness. Petrosian magnitude still usable.
||no Petrosian radius could be determined. Petrosian magnitude
||Petrosian radius larger than extracted radial profile. Happens
for noisy sky or low S/N objects.
||more than 1 value was found for the Petrosian radius.
|MANY_R50 / MANY_R90
||object's radial profile dips below 0 and more than one radius
was found enclosing 50%/90% of the light. Rare.
||Petrosian radius hits edge of frame. Petrosian quantities
should still be reasonable.
||object recognised to be moving between different
filters. For most purposes, consider only this flag to
find moving objects.
||candidate for moving object. Does not mean it did move
- consider DEBLENDED_AS_MOVING instead! Not useful.
||candidate moving object (MOVED) but was not deblended as moving
||object detected in too few bands for motion determination
||even though detected, no good centroid found in enough bands
for motion determination
||A "moving" object's velocity is consistent with zero.
||motion inconsistent with straight line, not deblended as moving
||in a complicated blend, child's motion was inconsistent with
straight line and parent was not deblended as moving
||nominal motion moves object off atlas image in this band
||'adaptive' moment are actually unweighted for this object. NB:
to find out if a moment measurement failed entirely, check the
||centroid shifted too far during calculation of moments,
moment calculation failed and M_e1,M_e2 give the value
of the shift
||moment calculation did not converge
||PSF moments are unweighted.
All flags so far indicate some problem or failure of a
measurement. The following flags provide information about the
processing, but do not indicate a severe problem or failure.
Informational flags related to deblending
Further informational flags
||last bin in radial profile < 0; usually can be ignored
||object is undetected in r-band; this band was used
to determine Petrosian and Model radii
||object is part of extended wing of a bright star
||object was extended and centroid was determined on 2x2 binned
frame. Avoid for astrometric work, e.g.