#This SM script will generate a list of unresolved objects from the
#tsObj files. This is an example script to illustrate the reading of
#tsObj files.
#Flags for primary target
define TARGET_QSO_HIZ 0
define TARGET_QSO_CAP 1
define TARGET_QSO_SKIRT 2
define TARGET_QSO_FIRST_CAP 3
define TARGET_QSO_FIRST_SKIRT 4
define TARGET_QSO_MAG_OUTLIER 25
define TARGET_GALAXY_RED 5
define TARGET_GALAXY 6
define TARGET_GALAXY_BIG 7
define TARGET_GALAXY_BRIGHT_CORE 8
define TARGET_ROSAT_A 9
define TARGET_ROSAT_B 10
define TARGET_ROSAT_C 11
define TARGET_ROSAT_D 12
define TARGET_STBHB 13
define TARGET_STCARBON 14
define TARGET_STBROWN_DWARF 15
define TARGET_STSUB_DWARF 16
define TARGET_STCATY_VAR 17
define TARGET_STRED_DWARF 18
define TARGET_STWHITE_DWARF 19
define TARGET_SERENDIP_BLUE 20
define TARGET_SERENDIP_FIRST 21
define TARGET_SERENDIP_RED 22
define TARGET_SERENDIP_DISTANT 23
define TARGET_SERENDIP_MANUAL 24
#Flags for secondary target
define TTARGET_LIGHT_TRAP 0
define TTARGET_REDDEN_STD 1
define TTARGET_TEST_TARGET 2
define TTARGET_QA_TARGET 3
define TTARGET_SKY 4
define TTARGET_SPECTROPHOTO_STD 5
define TTARGET_GUIDE_STAR 6
define TTARGET_BUNDLE_HOLE 7
define TTARGET_QUALITY_HOLE 8
define TTARGET_HOT_STD 9
#Photo's flags
define OBJ1_CANONICAL_CENTER 0
define OBJ1_BRIGHT 1
define OBJ1_EDGE 2
define OBJ1_BLENDED 3
define OBJ1_CHILD 4
define OBJ1_PEAKCENTER 5
define OBJ1_NODEBLEND 6
define OBJ1_NOPROFILE 7
define OBJ1_NOPETRO 8
define OBJ1_MANYPETRO 9
define OBJ1_NOPETRO_BIG 10
define OBJ1_DEBLEND_TOO_MANY_PEAKS 11
define OBJ1_CR 12
define OBJ1_MANYR50 13
define OBJ1_MANYR90 14
define OBJ1_BAD_RADIAL 15
define OBJ1_INCOMPLETE_PROFILE 16
define OBJ1_INTERP 17
define OBJ1_SATUR 18
define OBJ1_NOTCHECKED 19
define OBJ1_SUBTRACTED 20
define OBJ1_NOSTOKES 21
define OBJ1_BADSKY 22
define OBJ1_PETROFAINT 23
define OBJ1_TOO_LARGE 24
define OBJ1_DEBLENDED_AS_PSF 25
define OBJ1_DEBLEND_PRUNED 26
define OBJ1_ELLIPFAINT 27
define OBJ1_BINNED1 28
define OBJ1_BINNED2 29
define OBJ1_BINNED4 30
define OBJ1_MOVED 31
define OBJ1_DETECTED 32
define OBJ2_DEBLENDED_AS_MOVING 0
define OBJ2_NODEBLEND_MOVING 1
define OBJ2_TOO_FEW_DETECTIONS 2
define OBJ2_BAD_MOVING_FIT 3
define OBJ2_STATIONARY 4
define OBJ2_PEAKS_TOO_CLOSE 5
define OBJ2_MEDIAN_CENTRE 6
define OBJ2_LOCAL_EDGE 7
define OBJ2_BAD_COUNTS_ERROR 8
define OBJ2_BAD_MOVING_FIT_CHILD 9
define OBJ2_DEBLEND_UNASSIGNED_FLUX 10
define OBJ2_SATUR_CENTER 11
define OBJ2_INTERP_CENTER 12
define OBJ2_DEBLENDED_AT_EDGE 13
define OBJ2_DEBLEND_NOPEAK 14
define OBJ2_PSF_FLUX_INTERP 15
define OBJ2_TOO_FEW_GOOD_DETECTIONS 16
define OBJ2_CENTER_OFF_AIMAGE 17
define OBJ2_DEBLEND_DEGENERATE 18
define OBJ2_BRIGHTEST_GALAXY_CHILD 19
define OBJ2_CANONICAL_BAND 20
define OBJ2_AMOMENT_FAINT 21
define OBJ2_AMOMENT_SHIFT 22
define OBJ2_AMOMENT_MAXITER 23
define OBJ2_MAYBE_CR 24
define OBJ2_MAYBE_EGHOST 25
define OBJ2_NOTCHECKED_CENTER 26
#Flags for object status
define AR_OBJECT_STATUS_SET 0
define AR_OBJECT_STATUS_GOOD 1
define AR_OBJECT_STATUS_DUPLICATE 2
define AR_OBJECT_STATUS_OK_RUN 4
define AR_OBJECT_STATUS_RESOLVED 5
define AR_OBJECT_STATUS_PSEGMENT 6
define AR_OBJECT_STATUS_FIRST_FIELD 8
define AR_OBJECT_STATUS_OK_SCANLINE 9
define AR_OBJECT_STATUS_OK_STRIPE 10
define AR_OBJECT_STATUS_SECONDARY 12
define AR_OBJECT_STATUS_PRIMARY 13
define AR_OBJECT_STATUS_TARGET 14
#Flags for object type
define TYPE_UNK 0
define TYPE_CR 1
define TYPE_DEFECT 2
define TYPE_GALAXY 3
define TYPE_GHOST 4
define TYPE_KNOWNOBJ 5
define TYPE_STAR 6
define TYPE_TRAIL 7
define TYPE_SKY 8
#This run is part of the Equatorial stripe in the Northern Galactic
#Cap. It was part of the EDR, but has been reprocessed here with the
#latest versions of the imaging pipelines. This assumes the
#definition of a data directory, assigned to the variable data_dir
define run 756
define rerun 20
# The following will be used to do aperture photometry based on the
# measured radial profiles. The quantity profileRadii is the
# outer radius of the radii within which the radial profiles are
# measured.
set profileRadii={0 0.564190 1.692569 2.585442 4.406462 \
7.506054 11.576202 18.584032 28.551561 45.503910 \
70.510155 110.530769 172.493530 269.519104 420.510529 \
652.500061}
set profileRadii = profileRadii*0.396 #Convert to arcsec
set ii = 1, (dimen(profileRadii)-1)
set area = PI*(profileRadii[ii]**2 - profileRadii[ii-1]**2)
do column = 1, 6 {
do frame = 11, 800 {
define run_s (sprintf('%06d',$run)
define frame_s (sprintf('%04d',$frame))
define file_name "tsObj-$run_s-$column-$rerun-$frame_s.fit"
table 1 "$!data_dir/$!column/$!file_name"
#The basic command in SM for reading fits binary tables is the
#following: 'read table'. See the data model for a full description
#of each of the quantities read here. Note that many of the
#quantities come in fives, one each for each of the five bands
#(u g r i z, corresponding to indices 0 1 2 3 4). The command here
#reads in only a small fraction of all the outputs available for each
#object.
read table {run rerun camCol field id objc_rowc objc_colc status \
rowv rowvErr colv colvErr psfCounts[0-4] psfCountsErr[0-4] \
objc_type objc_flags objc_flags2 flags[0-4] flags2[0-4] \
reddening[0-4] ra dec primTarget secTarget}
#These are the radial profiles, 15 numbers in each of 5 bands.
read table {profMean[0-74] profErr[0-74]}
#This calculates aperture magnitudes in the five bins (in this case,
#going out to the 7th radial bin, i.e., a radius of 7.4 arcsec).
set dimen(apmag) = 5
set apmagerr = apmag
do band = 0, 4 {
set apmag[$band] = 0
set apmagerr[$band] = 0
do aperture = 0, 6 {
set apmag[$band] = apmag[$band] + \
profMean$(15*$band + $aperture)[jj[0]]*area[$aperture]
set apmagerr[$band] = apmagerr[$band] + \
(profErr$(15*$band + $aperture)[jj[0]]*area[$aperture])**2
}}
# That result is in maggies. Here we convert to magnitudes again:
# (note that this is not expressed in asinh magnitudes; it should be).
set apmagerr = 2.5*sqrt(apmagerr)/apmag/ln(10)
set apmag = (apmag < 0)?(25.):(-2.5*lg(apmag))
#The status flag within the tsObj file gives information to allow a
#unique set of objects to be selected; i.e., objects that are have
#'primary' status have all the book-keeping of the overlaps between
#frames, scanlines, runs, and stripes worked out. In brief, you want
#to include objects flagged as 'primary'. Objects flagged as
#'OK_STRIPE' don't take into account the overlap between adjacent
#stripes; this may be useful if you are considering one stripe at a
#time, in particular, at the edge of the DR1 area.
# Note that 'is_set(x,y)' returns a 1 if the y'th bit is set in x,
# and 0 otherwise.
set primary = is_set(status,$AR_OBJECT_STATUS_PRIMARY)
set ok_stripe = is_set(status,$AR_OBJECT_STATUS_OK_STRIPE)
There is a set of all-important flags output by the pipeline that
describe the processing; look
here for their meaning.
# Here we reject objects that are flagged BRIGHT (a duplicate entry in
# the photo outputs), SATURATED (for which the photometry will clearly
# be unreliable, EDGE (i.e., touching the edge of a frame) or BLENDED
# (we want the child entries). On the latter, an object can be noted
# as a composite (BLENDED), but for a variety of reasons, will not be
# deblended. Note that some of these cuts are redundant
# with the status=primary selection above; in particular, no BRIGHT
# objects are flagged primary. Note that some of these definitions
# here use objc_flags (overall flags based on the union of flags from
# the five bands), and some use flags from one band (i.e., flags3
# refers to the i-band in this example). There are enough flag bits
# that they don't all fit into a single parameter, thus the
# distinction between objc_flags and objc_flags2, and flags3 and
# flags23.
set bright = is_set(objc_flags,$OBJ1_BRIGHT)
set saturated = is_set(flags3,$OBJ1_SATUR)
set edge = is_set(objc_flags,$OBJ1_EDGE)
set blended = is_set(objc_flags,$OBJ1_BLENDED)
set nodeblend = is_set(objc_flags,$OBJ1_NODEBLEND)
# In the example here, we wish to select a sample of objects observed
# at i; we clearly want to confirm that it is detected in i!
set detected = is_set(flags3,$OBJ1_BINNED1)
# These are empirical cuts we've found are effective for rejecting
# small bits of fluff that often appear on deblending large objects;
# such objects are often assigned strange colors. These are explained
# in more detail in the quasar target selection algorithm paper
# (Richards et al 2002).
set deblending_problems = (is_set(flags3,$OBJ1_PEAKCENTER)|| \
is_set(flags3,$OBJ1_NOTCHECKED)|| \
is_set(flags23,$OBJ2_DEBLEND_NOPEAK)|| \
psfCountsErr3>0.2)
set interp_problems = (is_set(flags23,$OBJ2_PSF_FLUX_INTERP)|| \
(is_set(flags23,$OBJ2_INTERP_CENTER)&&\
is_set(flags3,$OBJ1_CR))||\
is_set(flags23,$OBJ2_BAD_COUNTS_ERROR))
# Here is a logical variable that is 1 for sources that are clean in
# the sense described above.
set clean = (detected && !edge && !saturated && primary && \
!blended && !bright &&!deblending_problems && !interp_problems)
# Correction for Galactic reddening (following Schlegel, Finkbeiner,
# and Davis 1998) is straightforward!
set iMag = psfCounts3 - reddening3
# Star-galaxy separation is done based on the difference between the
# psf and model magnitudes; if this is greater than 0.142 in a given
# band, then the quantity 'type' is set to 3; otherwise, it is set to
# 6. objc_type is global over the five bands; it is based on the
# sum of psf and model fluxes over the five bands.
set star = (objc_type==$TYPE_STAR)
# This velocity is based on the change in astrometric position
# between the five bands (observed in the order r i u z g over a
# span of roughly five minutes. Main-belt asteroids move by several
# arcsec in that time; the criteria here is to reject such objects.
set velocity = sqrt(rowv**2 + colv**2)
set velsig = sqrt((rowv/rowvErr)**2 + (colv/colvErr)**2)
set moving = (velocity > 0.2 || velsig > 3)
# As described in the quasar target selection paper, there are some
# bad columns in the data that never properly got masked, which can
# give rise to spurious unusual-colored objects. Here is a filter
# for rejecting them.
set bad_col = ($column==2&&objc_colc<1461&&objc_colc>1451)||\
($column==2&&objc_colc<1388&&objc_colc>1382)||\
($column==5&&objc_colc<1032&&objc_colc>1018)
set clean = clean&&star&&!moving&&!bad_col
# The following defines some flags related to target selection. Note
# that if you are using the BEST tsObj files, this will be based on
# the current version of the target selection code; some of the
# targets may not have been flagged for observation with earlier
# reductions, and therefore will not have spectroscopic observations.
# The CAP and SKIRT quasar target algorithms are the same; this is a
# remnant of a time when we thought we would need separate algorithms in
# regions of high and low stellar density.
set qso_first = (is_set(primTarget,$TARGET_QSO_FIRST_CAP) || \
is_set(primTarget,$TARGET_QSO_FIRST_SKIRT))
set qso_loz = (is_set(primTarget,$TARGET_QSO_CAP) || \
is_set(primTarget,$TARGET_QSO_SKIRT))
set qso_hiz = is_set(primTarget,$TARGET_QSO_HIZ)
set qso_optical = (qso_loz || qso_hiz)
#This is the union of all targetted quasar candidates.
set qso = (qso_first || qso_optical)
#The qso_mag_outlier and qso_reject objects are *not* targetted;
#these are outliers in the stellar locus that are either outside
#the quasar magnitude limits, or are in regions with contamination
from non-quasars (such as white dwarfs).
set qso_mag_outlier = is_set(primTarget,$TARGET_QSO_MAG_OUTLIER)
set qso_reject = is_set(primTarget,$TARGET_QSO_REJECT)
#This selects objects targetted as LRG's. Note that they come in two
#categories (see Eisenstein et al 2001 for the details).
set lrg = (is_set(primTarget,$TARGET_GALAXY_RED) || \
is_set(primTarget,$TARGET_GALAXY_REDII))
#This is the main galaxy sample. GALAXY_BIG and GALAXY_BRIGHT_CORE
#objects are very rare; most are not real galaxies.
set main_gal = (is_set(primTarget,$TARGET_GALAXY) || \
is_set(primTarget,$TARGET_GALAXY_BIG) || \
is_set(primTarget,$TARGET_GALAXY_BRIGHT_CORE))
# These are untiled set of targets.
set rosat = (is_set(primTarget,$TARGET_ROSAT_A) || \
is_set(primTarget,$TARGET_ROSAT_B) || \
is_set(primTarget,$TARGET_ROSAT_C) || \
is_set(primTarget,$TARGET_ROSAT_D) || \
is_set(primTarget,$TARGET_ROSAT_E))
set star = (is_set(primTarget,$TARGET_STBHB) || \
is_set(primTarget,$TARGET_STCARBON) || \
is_set(primTarget,$TARGET_STBROWN_DWARF) || \
is_set(primTarget,$TARGET_STSUB_DWARF) || \
is_set(primTarget,$TARGET_STCATY_VAR) || \
is_set(primTarget,$TARGET_STRED_DWARF) || \
is_set(primTarget,$TARGET_STAR_PN))
# These are blank areas of sky, appropriate for placing a sky fiber.
set sky = is_set(secTarget,$TTARGET_SKY)
#Various categories of serendipity targets, untiled.
set serendip = (is_set(primTarget,$TARGET_SERENDIP_BLUE) || \
is_set(primTarget,$TARGET_SERENDIP_FIRST) || \
is_set(primTarget,$TARGET_SERENDIP_RED) || \
is_set(primTarget,$TARGET_SERENDIP_DISTANT) || \
is_set(primTarget,$TARGET_SERENDIP_MANUAL))
#Various types of standard stars.
set standard_star = (is_set(secTarget,$TTARGET_REDDEN_STD) || \
is_set(secTarget,$TTARGET_SPECTROPHOTO_STD) || \
is_set(secTarget,$TTARGET_HOT_STD))