**
** 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 targetted. We would like to give the same priority (200) to all
** QSO targets except FIRST QSO targets which are selected as being
** on a line between two FIRST sources. The latter type of QSO
** receives lower priority (100). In the future the lower priority
** will be replaced by a range of priority.
**
** 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;
int inlocus, inGalaxylocus = 0;
int ImageProb=0, badCol=0, uvx=0;
int ta[5], det[5];
int priority=0;
int closestpoint;
double ellipsedist;
int targetmidZ = 0;
int inAstarbox = 0;
int inWDbox = 0;
int inWMbox = 0;
int i, nchild;
int intercenter, intercenterI;
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.
**
*********************************************************************/
if (obj->objc_flags&(AR_DFLAG_BRIGHT|AR_DFLAG_EDGE|AR_DFLAG_SATUR)) {
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.
**
*********************************************************************/
if ((obj->objc_flags & AR_DFLAG_BLENDED)) {
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.
**
*********************************************************************/
if ((obj->objc_type != 3) && (obj->objc_type != 6)) {
return 0;
}
/**********************************************************************
** Disregard moving objects
**
** Objects which are deblended as 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.
**
*********************************************************************/
if((obj->objc_flags2 & AR_DFLAG2_DEBLENDED_AS_MOVING))
return 0;
/**********************************************************************
** Disregard more moving objects
**
** Throw away things
** that have large velocities (if those velocities are significant
** with respect to the error). This *might* be redundant with the
** above.
**
*********************************************************************/
if( !(obj->objc_flags2 & AR_DFLAG2_BAD_MOVING_FIT) &&
( (fabs(obj->rowv.val) > params->MAXV ) && (fabs(obj->rowv.val)/obj->rowv.err > params->MAXVSIG) ||
(fabs(obj->colv.val) > params->MAXV ) && (fabs(obj->colv.val)/obj->colv.err > params->MAXVSIG)) )
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.
**
** TODO: flag any such object with quasar-like colors with the QSO_REJECT
** flag, so that they might be followed up by others. This will require
** moving this check forward to later in the code.
**
*********************************************************************/
if (obj->detection[ta[3]].psfCounts.val < params->IBRIGHT) 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.
**
*********************************************************************/
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]