**
** ROUTINE: taQuasarsTargetSelect
**
**
** Set the appropriate bit in the primary target bit mask for each
** Quasars Working Group target selection criterion this object
** satisfies. This routine is responsible for setting the following
** bits:
**
** It is assumed that the above bits are unset on entry, although other
** bits may be set.
**
** This routine returns the priority of the quasar candidate, in the
** range 0-255. On error, -1 is returned. Zero means it should not
** be targeted. We currently give the same priority (200) to all
** QSO targets.
**
** FYI, the area of a good frame is given by
** area = at_scanSeparation*1361.0*0.396/(3600.0)
** = 3.140533x10^-2 sq. deg
**
** NOTE: Update me after all changes are made (MAS, 09/05/00).
**
**
**
**
******************************************************************************
*******************************************************************************/
int taQuasarsTargetSelect(TA_CALIB_OBJ *obj,
/* MOD: calibrated object to test */
const TA_QUASARS_PARAMS *params
/* IN: tunable parameters*/)
{
float mag[5],err[5];
double syserr[5];
double lowzlimit[5];
int colorindex;
int capobject, index, tmpflag,tmpflag2, TSFLAG;
float MAGLIMIT;
float MIDZBRIGHTLIMIT;
int ta[5], det[5];
int priority = 0;
int inlowzlocus = 0;
int inhighzlocus = 0;
int inmidzlocus = 0;
int inGalaxyplane = 0;
int ImageProb = 0;
int badCol = 0;
int uvx = 0;
int closestpoint = 0;
double ellipsedist = 0.0;
double galdist = 0.0;
int inGalaxyklm = 0;
int inGalaxyklmJunk = 0;
int inGalaxylocus = 0;
double velocity = 0.0;
double velocityError = 0.0;
int targetmidZ = 0;
int inAstarbox = 0;
int inWDbox = 0;
int inWMbox = 0;
int i, nchild;
int intercenter, intercenterI;
int retval = 0;
int badamp = 0;
int rejReason; /* reason for rejecting a quasar
1 = BRIGHT
2 = EDGE
3 = SATUR
4 = BLENDED
5 = bad objc_type
6 = moving
7 = too bright
8 = deblend problem
9 = ERRINTERPCENTER
10 = INTERP_CENTER i' + bright
11 = bad column
12 = A-star
13 = WD
14 = WD+M
15 = galaxy klm
16 = stellar locus ugri
17 = stellar locus griz
18 = high-z uvx
19 = large errors in all bands
20 = mid-z random
21 = galaxy locus
22 = mid-z locus
23 = not OK_SCANLINE
24 = LOCAL_EDGE (e.g. bad u' amplifier)
*/
int accReason; /* reason for accepting quasar
-1 = FIRST
-2 = mid-z
-3 = low-z
-4 = low-z mag outlier
-5 = high-z ugri
-6 = high-z
-7 = high-z mag outlier
-8 = mid-z bright
-9 = FIRST mag outlier
-10 = High-z galaxy
*/
static int icall=0; /* changed after first call */
static int diagReject; /* write diagnostics for all rejected objects */
static int diagAccept; /* write diagnostics for all accepted objects */
static FILE *fp,*fp2; /* diagnostic file pointer */
int run;
int rerun;
int camcol;
char rejstr[80];
char accstr[80];
char temp[6];
sprintf(rejstr,"quasarsReject");
sprintf(accstr,"quasarsAccept");
run = sprintf(temp,"%d",obj->run);
strcat(rejstr,temp);
strcat(accstr,temp);
rerun = sprintf(temp,"%d",obj->rerun);
strcat(rejstr,"_");
strcat(accstr,"_");
strcat(rejstr,temp);
strcat(accstr,temp);
camcol = sprintf(temp,"%d",obj->camCol);
strcat(rejstr,".out");
strcat(accstr,".out");
/* on 1st call, open files for writing accept and reject diagnostics */
if (icall==0) {
diagReject=params->DIAGREJECT;
diagAccept=params->DIAGACCEPT;
if (diagReject) fp=fopen(rejstr,"w") ;
if (diagAccept) fp2=fopen(accstr,"w") ;
}
icall++;
ta[0] = TA_U;
ta[1] = TA_G;
ta[2] = TA_R;
ta[3] = TA_I;
ta[4] = TA_Z;
/*
*************************************************************************
** FATAL Errors
**
** These next sections look for objects with fatal errors. If the
** object is bad, we return 0, which means the object is never
** given a chance to be targeted.
**
*************************************************************************
**/
/**********************************************************************
** Cut "bad" objects
**
** Don't even bother to check objects which are bad. Including
** bright objects, edge objects and those that are flagged as
** saturated.
**
** In fact, these may never get used, since "primary" is defined so
** that these objects are not given the chance to be targeted.
**
** We now reject on status != OK_SCANLINE. This is in order to
** deal with the area problem.
**
** (OK ???, GTR, 09/22/00)
*********************************************************************/
if (obj->objc_flags&AR_DFLAG_BRIGHT) {
/* Output diagnostic information */
rejReason=1;
if (diagReject) {
taQuasarsLog(fp, obj, 0, 0, 0, rejReason);
}
return 0;
}
if (obj->objc_flags&AR_DFLAG_EDGE) {
rejReason=2;
if (diagReject) {
taQuasarsLog(fp, obj, 0, 0, 0, rejReason);
}
return 0;
}
if (obj->objc_flags&AR_DFLAG_SATUR) {
rejReason=3;
if (diagReject) {
taQuasarsLog(fp, obj, 0, 0, 0, rejReason);
}
return 0;
}
if (!(obj->status&AR_OBJECT_STATUS_OK_SCANLINE)) {
rejReason=23;
if (diagReject) {
taQuasarsLog(fp, obj, 0, 0, 0, rejReason);
}
return 0;
}
/**********************************************************************
** Cut blended objects
**
** Do not select things which are blended. Note that we do NOT
** keep NODEBLEND objects, as such objects are likely to have very
** unreliable colors.
**
** (OK, GTR, 09/22/00)
*********************************************************************/
if ((obj->objc_flags & AR_DFLAG_BLENDED)) {
rejReason=4;
if (diagReject) {
taQuasarsLog(fp, obj, 0, 0, 0, rejReason);
}
return 0;
}
/**********************************************************************
** Reject objc_types other than stellar or galaxy
**
** Reject things which don't have either objc_type == 3 (galaxy) or
** objc_type == 6 (stellar), because the other types are all error
** codes.
**
** (OK, GTR, 09/22/00)
*********************************************************************/
if ((obj->objc_type != 3) && (obj->objc_type != 6)) {
rejReason=5;
if (diagReject) {
taQuasarsLog(fp, obj, (double) obj->objc_type, 0, 0, rejReason);
}
return 0;
}
/**********************************************************************
** Disregard moving objects
**
** Objects which are moving are probably asteriods,
** but certainly not quasars. However, their colors can be
** non-solar if the deblend isn't perfect, so we have to reject
** them explicitly.
**
** (Needs more testing, GTR, 10/30/00)
*********************************************************************/
velocity = (sqrt(obj->rowv.val*obj->rowv.val + obj->colv.val*obj->colv.val));
velocityError = (sqrt(obj->rowv.err*obj->rowv.err + obj->colv.err*obj->colv.err));
if ((velocity > params->MAXV) && ((velocity/velocityError) > params->MAXVSIG)) {
rejReason=6;
if (diagReject) {
taQuasarsLog(fp, obj, (double) velocity, (double) velocityError, 0, rejReason);
}
/**** Note: Look to see how many such objects there are, but don't
**** reject them for now. ****/
/*
return 0;
*/
}
/**********************************************************************
** Delete object brighter than i' = IBRIGHT (too bright for the spec.)
**
** While we can take spectra of bright objects, they will bleed
** into neighboring spectra. Therefore we have to set a limit on
** how bright of an object we will take spectra of. Reddening
** correction is NOT applied.
**
** (OK, GTR, 09/22/00)
*********************************************************************/
if (obj->detection[ta[3]].psfCounts.val < params->IBRIGHT) {
rejReason=7;
if (diagReject) {
taQuasarsLog(fp, obj, (double) obj->detection[ta[3]].psfCounts.val, 0, 0, rejReason);
}
/* We no longer return 0 here, since we reject on IBRIGHT elsewhere.
* This way we can have a record of such objects, but we will not
* put fibers on them. */
/* return 0; */
}
/**********************************************************************
** Delete undetected objects
**
** We don't want to throw away good high-z quasar candidates, even
** if they don't meet the official selection criteria. We also
** don't want to keep a zillion QSO_REJECT and QSO_MAG_OUTLIER
** objects, so we have to restrict things somehow. So, we require
** that at least one band be a 5 sigma detection (error less than
** 0.2).
**
** NOTE: What about faint objects with small errors?
**
*********************************************************************/
if (obj->detection[ta[0]].psfCounts.err > 0.2 &&\
obj->detection[ta[1]].psfCounts.err > 0.2 &&\
obj->detection[ta[2]].psfCounts.err > 0.2 &&\
obj->detection[ta[3]].psfCounts.err > 0.2 &&\
obj->detection[ta[4]].psfCounts.err > 0.2) {
rejReason=19;
if (diagReject) {
taQuasarsLog(fp, obj, (double) obj->detection[ta[0]].psfCounts.err,\
(double) obj->detection[ta[1]].psfCounts.err,\
(double) obj->detection[ta[2]].psfCounts.err, rejReason);
}
return 0;
}
/*
*************************************************************************
** End FATAL Error checking, begin non-FATAL Error checking
**
** These objects are rejected, but not if they are also
** FIRST sources.
**
** Before doing that, we need to fill the magnitude and magnitude
** error vectors.
**
*************************************************************************
**/
/**********************************************************************
** Correct magnitudes and errors for galactic reddening
**
** We use the Schlegel maps to correct for galactic reddening. We
** then must add the error in the reddening in quadrature with the
** error in the magnitude.
**
** NOTE: Schlegel says that the error in the reddening correction
** is 15% of the value, which is what is coded. It may be that
** since the errors in different filters are correlated that we now
** overestimate the errors in colors, but this probably does not
** hurt.
**
*********************************************************************/
for (colorindex=0; colorindex<5; colorindex++) {
mag[colorindex] = obj->detection[ta[colorindex]].psfCounts.val-obj->reddening[ta[colorindex]];
err[colorindex] = sqrt(obj->detection[ta[colorindex]].psfCounts.err\
*obj->detection[ta[colorindex]].psfCounts.err\
+0.15*0.15*obj->reddening[ta[colorindex]]\
*obj->reddening[ta[colorindex]]);
}
/**********************************************************************
** Add systematic errors
**
** Despite our best efforts, the photometric errors will not
** incorporate all of the possible error in the determination of
** magnitudes for these objects. As such add some additional error
** based on practical experience.
**
** TODO: Check that these additional errors have reasonable values.
**
*********************************************************************/
syserr[0]=params->SYSUERR;
syserr[1]=params->SYSGERR;
syserr[2]=params->SYSRERR;
syserr[3]=params->SYSIERR;
syserr[4]=params->SYSZERR;
for (colorindex=0; colorindex<5; colorindex++) {
err[colorindex]=sqrt(err[colorindex]*err[colorindex]+syserr[colorindex]*syserr[colorindex]);
}
/**********************************************************************
** Identify objects with image problems, and flag them with ImagProb=1
**
** The various tests that are done here are based on our experience
** and are mostly empirical.
*********************************************************************/
if((obj->objc_flags & AR_DFLAG_CHILD)!=0) {
nchild=1;
} else {
nchild=0;
}
intercenter=0;
intercenterI=0;
/* if object is a child, but its error is small, and if it is not */
/* detected or is flagged as PEAKCENTER or NOTCHECKED or */
/* DEBLEND_NOPEAK, then this is probably a deblending problem. */
for (colorindex=0; colorindex<5; colorindex++) {
tmpflag=obj->detection[ta[colorindex]].flags;
tmpflag2=obj->detection[ta[colorindex]].flags2;
if (tmpflag & AR_DFLAG_BINNED1) {
det[colorindex]=1;
} else {
det[colorindex]=0;
}
if(mag[colorindex]<23 && err[colorindex]