Understanding the image processing flags - Details
Introduction
In the process of measuring the properties of all objects detected in the SDSS images, the image-processing software sets an extensive series 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. The present document describes the flags in different categories, and tries to make clear how they can best be used. For full understanding, one should read this in parallel with Robert Lupton's flags document containing even more detailed descriptions of the individual flags.
The SDSS imaging data consist of images in five photometric bands. The measurement of the properties of the objects is carried out in the five bands separately, and flag bits are set in each band. There are enough flag bits to fill up two 32-bit quantities, thus these are encoded in two quantities, called generically flags and flags2. There is one such pair for each of the five bands, u, g, r, i, and z. These are combined in various ways to make flags appropriate for the whole object in all five bands; these are called objc_flags and objc_flags2.
Beware of interpreting the objc_flags blindly! For example, the
NOPETRO
flag is set in objc_flags if the Petrosian radius
cannot be measured in any of u, g, r, i, and z. Imagine our
horror when the SDSS galaxy spectroscopic sample (which is defined in
terms of Petrosian magnitudes in r) had 50% of the objects flagged
NOPETRO
! The reason is because the u and z bands are low S/N,
and many objects had NOPETRO
set in u or z, and therefore in
the objc_flags as well. Only 2% of galaxy targets have NOPETRO
set in r.
Flags that affect the object's resolve status
These flags are used by the resolve software to determine
whether an object is unique within a field. Typically, you should
rely on the RUN_PRIMARY
bit in resolveStatus
rather than use these bits directly.
BINNED
An object that is detected
as greater than a 5 sigma peak (after smoothing with the local PSF) in
a given band is flagged BINNED1
in that band. The object-finder then
masks all detected objects thus far, bins the image 2x2, and runs the
detection algorithm again; objects discovered at this stage are
flagged BINNED2
. This is repeated again (i.e., now binning 4x4);
detections are labeled BINNED4
. Many BINNED2
detections include the
outskirts of bright galaxies, and scattered light from bright stars
(as well as genuine low surface brightness galaxies); very few BINNED4
detections seem to be real astrophysical objects.
DETECTED
Used only
internally in the pipeline, but not written to files. DETECTED
is the OR of BINNED1
, BINNED2
, and BINNED4
, in a
given band. Even if the object is not flagged DETECTED
in a
given band (usually because it was detected only in another band),
photometry is still carried out on it, allowing, e.g., a 3-sigma
detection of a point source.
BRIGHT
As described in the EDR paper, objects detected at more than 200
sigma in the r band have their properties measured twice: once with a
global sky and once with a local sky. The former entry in the SDSS
catalogs is flagged BRIGHT
, and in practice is rarely used to do
science. One should always reject such objects. This will be set in
all the bands, as well as objc_flags.
BLENDED, NODEBLEND, CHILD
Each detected object is
examined to see if it is composite; if it is, it is flagged BLENDED in
all bands, as well as objc_flags. An attempt is made to deblend it.
If for some reason it is not deblended (usually because it is too
close to the edge), it will be flagged NODEBLEND
. Otherwise, its
children will have their properties measured as well, and one wants to
reject BLENDED
objects not flagged DEBLENDED
in order to avoid
duplicate entries. Note that selecting PRIMARY
objects does this, and
the cut on BRIGHT
entries, automatically.
The children of a deblend are flagged CHILD
. It is
possible for multiple peaks to be detected in the CHILD
,
and for it to also be labelled BLENDED
as well. There
are further flags related to deblending that are mostly informational
in nature; see below.
Flags that indicate problems with the raw data
SATURATED, SATURATED_CENTER
The photometry of saturated objects is questionable, needless to say (in
fact, the total PSF counts of mildly saturated stars should not be too
much in error, as it attempts to include all photons, including those
in the saturated core and the bleed trail). The SATURATED
flag is set
in each band that includes saturated pixels; if it is set in any band,
it is also set in objc_flags. Objects that are saturated can be
deblended if they show multiple peaks. Note that a galaxy with a
superposed saturated star in its disk, even if successfully deblended,
will be flagged SATURATED
, as some of the pixels in the object
footprint are indeed saturated.
SATURATED_CENTER
indicates that the saturated pixels are close to
the center of the object. This can be used to distinguish, e.g.,
galaxies which are flagged SATURATED
because of a superposed star,
from those with a very bright Seyfert nucleus, although it still needs
further testing. Note that star-galaxy separation is not very
effective for saturated objects; many saturated stars are
misclassified as galaxies.
EDGE, LOCAL_EDGE, DEBLENDED_AT_EDGE
The photometric pipeline works on one field at a time. An object which is
too close to the edge of a frame is flagged EDGE
in that band. Among
PRIMARY
objects (which have been resolved in overlaps, and thus should
remove most EDGE
objects), only large extended objects should be
flagged EDGE
. Thus, if you are interested in point sources, you will
probably not need to worry about the EDGE
flag (or at least be
suspicious of objects with EDGE
and PRIMARY
set). On rare occasions,
it has happened that half of a chip has gone on the blink; objects
close to the new edge there are flagged LOCAL_EDGE
in the appropriate
band.
The deblending algorithm has to work harder for objects close to the
edge; it runs only for big objects which otherwise might be missed.
If so, the flag DEBLENDED_AT_EDGE
is set. This is an informational
flag; it by itself does not indicate any trouble.
Other pixel-level problems
If the photometric pipeline recognizes a pixel as bad (due to a bad
column, a cosmic ray, or a bleed trail), it is interpolated over. If
this is true for any pixel within the object, it is flagged
INTERP
. This by itself it just informational; if the
interpolation is over a cosmic ray or a single bad column, for
example, the photometry should be essentially perfect. Further flags
give additional information.
-
CR
means that the object contained a cosmic ray that was interpolated over. This does not mean that the object in question is a cosmic ray! Again, the photometry of objects flaggedCR
is usually fine. Thus this is mostly an informational flag. -
MAYBE_CR
is an indication that object may be a cosmic ray. It is not interpolated over; it is set with a threshold lower than the main cosmic-ray finding algorithm. It is a useful flag to trigger on if one is looking, e.g., for objects detected in a single band (such as the high-redshift quasars and T dwarfs, which can show up only in the z band). -
MAYBE_EGHOST
says that the object in question is in a position that it may be an electronics ghost of a bright star in the given band. You should be suspicious of objects with this flag that are faint and detected in only one band. -
INTERP_CENTER
means that the interpolated pixel(s) in question fell within 3 pixels of the center of the object. This is a warning that perhaps the photometry of this object may be affected. You should really get concerned when -
PSF_FLUX_INTERP
is set. This means that more than 20% of the PSF flux is interpolated over in the band in question, which may make one suspicious of the accuracy of the flux. In practice, most objects with this flag set still appear to have perfectly good PSF photometry, but the number of outliers (say, in a color-color plot) is definitely larger than usual. - You should be especially suspicious if
BAD_COUNTS_ERROR
is set in a given band, which says that the interpolation over bad pixels is so significant that you should not believe the PSF flux error; it is probably underestimated.
Flags that indicate problems with the image
CANONICAL_CENTER, PEAKCENTER, DEBLEND_NOPEAK, NOPROFILE, NOTCHECKED, NOTCHECKED_CENTER, TOO_LARGE, BADSKY
Often, in deblending, objects near the edge, and at low S/N, various flags will be set indicating trouble defining the center of the object. This should make one suspicious of its detailed photometric properties. In particular:
CANONICAL_CENTER
: The centroid of a given object is usually determined separately in each band. If in some band, it is impossible to measure the center (due to being at the edge), one uses the center in another band, transformed according to the relative astrometry between the bands, and this flag is set.PEAKCENTER
: If the centroiding algorithm can't find a better center, it will often simply report the position of the peak pixel in a given band. This often happens with little wisps of objects deblended from something bright; the flagPEAKCENTER
is set. It is a hint that this object may not be real. A related flag isDEBLEND_NOPEAK
: indicates that after deblending, the child in question doesn't have a peak. Objects with either of these flags set (especially nominal point sources in a nominally high S/N band) should be treated with suspicion.- An object with
NOPROFILE
set in a given band had (as the name implies) zero or one entries in the radial profile; most photometric quantities measured from it are likely to be suspect. NOTCHECKED
: An object includes pixels which were not checked for peaks by the deblender; this can happen close to the edge, and in the cores of saturated stars. Be suspicious of the performance of the deblender in this case. If the flagNOTCHECKED_CENTER
is also set, the situation is worse; the center of the object is in a not-checked region. This should not happen for anyBINNED1
object.- The flag
TOO_LARGE
indicates an object which is still detected at the outermost point of the radial profile (a radius of over 4 arcmin), or at least one child in a deblend is larger than 1/2 a frame. This is indicative either of a very large object, or a poorly determined sky, or a particularly horrific deblend. The detailed photometry of this object is questionable. BADSKY
: If the local sky is badly determined (as occasionally happens in regions with complex backgrounds), the core of an object can be strongly negative. This is bad; the photometry of such objects is meaningless.
Problems associated with specific quantities
Introduction
Some of these are easy; they simply say that the quantity in question could not be measured. In particular:
NOSTOKES
: Objects whose Q and U (Stokes parameters) were not measured in a given band.ELLIPFAINT
: Objects whose isophotal shape could not be measured.
Three types of measurement generate a lot of flags: Petrosian quantities, the proper motion of objects, and adaptive shape moments. These are described below.
Flags associated with the measurement of Petrosian quantities
The pipeline measures Petrosian radii, fluxes, 50% and 90% radii, and errors for all these quantities. This is described in detail in Appendix A to Strauss et al. (2002), which discusses the flags as well. The Petrosian radius (and there can be more than one of them) is often measured at a fairly low S/N point in the profile of an object. Thus the most common flags that are set (especially at the faint end) are
PETROFAINT
the Petrosian radius is measured at a very low surface brightness level, andNOPETRO
the code was unable to measure the Petrosian radius.
These two often appear together. In this case
(and in the absence of other warning flags such as BADSKY
or
NOPROFILE
, which mean real trouble), the code still returns a
meaningful magnitude (i.e., the total flux within the aperture with
detected counts), so the Petrosian magnitude will still be usable. A
related flag is NOPETRO_BIG
, which indicates that the Petrosian
radius appears to be larger than the outermost point of the extracted
radial profile. This can happen in regions in which the background
sky is noisy, or for low S/N objects.
Other Petrosian flags, mostly informational in nature, include:
MANYPETRO
For galaxies with composite profiles, it is possible for there to be more than one Petrosian radius.MANY_R50, MANY_R90
Galaxies which have a radial profile which dips below zero can have more than one radius including 50% or 90% of the light. This is a rare occurrence.- If the Petrosian radius hits the edge of the frame, the flag
INCOMPLETE_PROFILE
is set. The radial profile, and thus the Petrosian quantities, are still calculated in an unbiased way, and the results should be reasonable.
Flags associated with moving objects
A main-belt asteroid will show a parallax of a few arcseconds between
the r and g exposure in the SDSS camera. The photometric pipeline,
and in particular, the deblending algorithm, explicitly tests for
this, and measures the motion as appropriate. There are quite a few
flags associated with this process. For most purposes, the
only flag you need to examine is DEBLENDED_AS_MOVING
, whose
name should be self-explanatory. If one wants a catalog of moving
objects, for example, cut on this flag, as well as the derived motion
(rowv, colv) and associated errors. It is possible that objects with
small enough motion will have a statistically significant proper
motion, but not trigger this flag; this requires further exploration.
There are no doubt a number of Kuiper Belt objects to be discovered in
the SDSS data!
The remaining flags related to moving objects are mostly informational in nature, but are useful in understanding why a specific object was not deblended as moving:
MOVED
indicates that the object is a candidate to be deblended as moving. This is not a terribly useful flag. In particular, despite its name, it does not mean that the object is actually determined to be moving!NODEBLEND_MOVING
Objects flaggedMOVED
that are not deblended as moving. Not terribly useful.- Objects with detections in only a few bands will not be able to
be tested for motion; they are flagged
TOO_FEW_DETECTIONS
. Even if the object passes this threshold, it may turn out that the centroids are not good in a few of the bands, in which case the flagTOO_FEW_GOOD_DETECTIONS
is also set. BAD_MOVING_FIT
the motion of the object is inconsistent with a straight line and it is not deblended as moving. A related flag isBAD_MOVING_FIT_CHILD
, which states that in a complicated deblend putatively involving both a moving and stationary object, a child's velocity fit is too poor, so the parent wasn't deblended as moving.STATIONARY
the moving object's velocity is consistent with zeroCENTER_OFF_AIMAGE
the nominal motion moves the object right off the edge of the atlas image in some band.
Flags associated with the measurement of adaptive moments
The imaging pipeline carries out the calculations of optimally weighted second moments of objects in order to determine their shapes (especially for weak lensing studies). The flags indicate trouble with this process for a given object in a given band, usually at low S/N and such moment measurements should not be used.
AMOMENT_UNWEIGHTED
(also calledAMOMENT_FAINT
) the calculation of the weights failed, the adaptive moments are calculated without weightsAMOMENT_SHIFT
in the determination of adaptive moments, the centroid is recalculated; if it shifts too far, the flagAMOMENT_SHIFT
is set, and M_e1 and M_e2 give the value of shiftAMOMENT_MAXITER
the moment calculation did not converge
Further flags related to deblending (all informational)
A complicated object may have many peaks in it (think of the core of a globular cluster as the worst-case scenario!). However complicated an object is, the deblender conserves flux, in so much as the flux in each pixel is split among the children. Still, no effort is made to ensure that the sum of the children is exactly equal to the parent, so rounding error could lead to discrepancies of one or two DN. A number of informational flags point out cases where deblending was complicated.
If the number of peaks is larger than 25, the flag
DEBLEND_TOO_MANY_PEAKS
is set (in the parent, *not* the child),
and only the 25 most significant peaks are deblended.
DEBLEND_UNASSIGNED_FLUX
indicates that initially, >5% of the
parent's flux was not assigned to any of the children and that this
flux has been redistributed among them. Thus this is not an indicator
of any problem with the deblender; this is an informational flag
only.
It is occasionally true (especially in complicated deblends) that
some of the peaks are not deblended, for one of two reasons. The
parents in such cases are labelled DEBLEND_PRUNED
. The two
reasons are that these peaks lie too close to other peaks (in which
case the flag PEAKS_TOO_CLOSE
is set), or that the templates
associated with the peak is degenerate with others (in which case
DEBLEND_DEGENERATE
is set -- see deblender
description in DR1 changes document).
In a complicated deblend, especially those involving galaxies,
there can be many children, and it is not always obvious (without
looking at the image by eye) which child is the main galaxy. The flag
BRIGHTEST_GALAXY_CHILD
flags that object which the code
believes to be the brightest galaxy child.
If the deblending algorithm recognizes a given child as unresolved, it
will use that information in the deblend, and flag it as
DEBLENDED_AS_PSF
.
HAS_SATUR_DN
indicates that the object is saturated in this
band and the bleed trail doesn't touch the edge of the frame. In such
cases, an attempt is made to add up all the flux in the bleed trails,
and to include it in the object's photometry. Note: some of the CCDs
saturate at over 65535 DN; for these chips, the bled flux will be
underestimated.
After the regular deblender had completed, photo took another pass
looking for some special cases, and the deblend was modified based on
this analysis are flagged DEBLEND_PEEPHOLE
. Currently, only one
special case is considered: objects that, when merged together, were
consistent with a moving object that the deblender had missed in the
first pass.
Further informational flags
It is often true that the last bin in the radial profile of an
object goes slightly negative. When this happens, the BAD_RADIAL
flag
is set; it can usually be ignored.
The Petrosian and model magnitude calculations make reference to
a canonical band, which defaults to the r band. In the case that the
object is undetected in r, the canonical band is set to the highest
S/N band. The band in question is flagged
CANONICAL_BAND
.
The extended wings around bright stars are subtracted; such
objects are flagged SUBTRACTED
.
For sufficiently extended objects, the PSF-weighted centroid is not optimal,
and the centroid is found using a 2x2-binned images. Such objects are
flagged BINNED_CENTER
; such objects probably should not
be used, e.g.,
as part of a local astrometric reference frame.