RRA - SETTING HRI FIELD AND SOURCE FLAGS
filename: flagset.hri
Date: 3 oct 94
originat: deh
tlm: 9 apr 95 (s/n for cutoff)
tlm: 29 jun 95 (let 'p' spawn 'i')
1.0 GENERAL
2.0 PROCEDURE
3.0 DESCRIPTION of each flag
4.0 FLAG MATRIX
5.0 SPECIFICATION FOR SMOOTHED ARRAYS
6.0 RECOVERY OF MATCHED SOURCE LIST
7.0 DERIVATION OF BACKGROUND
8.0 SPECIFICATION OF 'ASSOCIATED WITH NEAREST NEIGHBOUR'
1.0 GENERAL
This is meant to expound on the outlined methods of setting flags which were
devised at the MPE meeting in September. We have added the source 'a' flag
after the MPE meeting in Feb 95.
There are 3 logical steps to setting flags:
1 - Before visual inspection. this is done so as to minimize the work required
in step 2. SASS parameters are used to set some flags.
2 - During visual inspection (VI)
3 - After VI - since some flags will spawn others.
Obviously the step 3 operations can be incorporated into the step 2 process
so long as they are 'invisible' to the operator.
Reminder: all flags are F or T, true when something is suspect.
2.0 PROCEDURE
- 2.1 Step 1
All of these are straightforward database operations once
the conditions have been decided.
Field Flags:
B background
The algorithm for deciding if the BG is high is given in
section 7. We generate a histogram of absolute background levels and
then see if the average exceeds some arbitrary threshold, currently
set at level '8'.
D deferred
if there are no sources (e.g. in 12" detect), set the Field D flag, deferred.
S SOURCE LIST MISSING
check for empty or missing source file
Source Flags:
u UN-UNIQUE
if detection matches detection with smaller cell, set u.
n NOT CHECKED
if S/N is < (tbd) 4 sigma, set n
a ASSOCIATED WITH (NEAREST) NEIGHBOR
a test involving radius of extended circle and PRF radius
if this test is met, set a, and i.
d DETECTOR STRUCTURE
if EPI is > 0.01, set d, i, p and v.
e EXTENDED
if SIZCOR is > 1.2, set e, i, and p
v VARIABILITY SUSPECT
perform the two var tests described in section 3 for the v flag.
Step 1 will also require other preparatory tasks. Among these
will be the creation of a blocked array which will then be smoothed with
a Gaussian (details given below). Another task will be the recovery of the
matched source table (section 6) and the creation of 'new columns' for each
source. These new columns will contain the source numbers from the matched
source table for each detect cell size. Although this is a bit wasteful of
space, it will make retrieval tests significantly easier.
- 2.2 Step 2 and 3 Visual Inspection
We suspect it will be most efficient to combine steps 2 and 3
so that the operator will see the ramifications of each decision. This
means that flags spawned by other flags should be changed immediately
and so displayed.
FIELD: Based on our V&V experience, it is useful to first view the
whole field. This may be done with a blocked photon display, although
smoothing (see section 5) or expansion may be useful. In V&V, we used
xexamine in PROS which allowed zooming in on a region of interest.
Current plans are to have a 512 blocked photon display for the whole field
AND a 512 smoothed array of the inner portion of the HRI field of view.
The operator should answer the following:
D deferred
are there problems I don't want to deal with now?
A ASPECT SUSPECT
is there evidence that the aspect has problems
E EXTENDED EMISSION IN THE FIELD
Is there substantial extended emission?
M MISSED SOURCE(S)
Did one or more sources get missed? (overlay ALL unique sources)
D query should be pretty obvious and quick. The A question is
usually manifest by all sources showing the same elliptical structure
or by all sources being double. E should be fairly obvious. M is the
last of the field queries as it requires the same display as the
beginning of the source flags...the overlay of detect positions. The
search for missed sources will be done on the two arrays described in
section 5.
SOURCE: The primary source flags to consider for n=f, u=f, (but
see section 5.4 for precise selection) are:
c CONFUSED DETECT ALGORITHM
Is there one detection for two close sources?
f FALSE DETECTION
Is this detection not a real source?
m MULTIPLE DETECTIONS FOR A SINGLE SOURCE
Were there (spurious) multiple detections for only one source?
w WITHIN EXTENDED EMISSION
Is the source within extended emission?
If the operator sees a particular problem, the secondary flags i, n,
and p may be set. The operator can focus on deciding if the source is
real, if it is confused, if there are multiple detections, and if the
source is within extended emission. Note that many 'm' sources will
also be 'f' sources; i.e. one of the reasons a detection may be false is
that it is a spurious detection in the wings of a strong source.
3.0 DESCRIPTIONS
- 3.1 FIELD FLAGS
_______________
A asp_susp Step 2 only aspect is suspect
For the HRI, this condition can only be easily spotted if
there is a sufficiently strong source which is seen to be elliptical
whereas it is known (apriori) that it is unresolved. OR If there are
two or more sources which have the same apparent ellipticity.
Extremely pathological cases of double images etc will also require
setting this flag, but these are expected to be rare.
Determination of bad aspect by VI is perhaps the most difficult
process in flag setting. We do not wish to flag aspect when there is
a small residual ellipticity caused by wobble (usually < 5"); therefore,
if ellipticity is found, the magnitude should be estimated as >5" before
setting the A flag.
There is also a potential ambiguity between the field
"suspect-aspect" flag A and the source "confused" flag c - what's the
difference between a confused source (i.e. two real sources 3 to 10"
apart) and a source that appears as a close double image due to bad
aspect? If there is only once source strong enough to see elliptical
or double structure, there is no obvious method of determining the
actual situation.
Finally, if there are no strong sources near the field
center, it will be difficult to see any evidence of bad aspect.
Subsequent Action: Whenever this flag is set, all source flags i,p,v
are automatically set.
---------------------------------------------------------------------
B bkg_susp Step 1: test of background level
Step 3: if E (extended emission) flag is set.
In step 1, the algorithm (section 7) will automatically set B.
If the extended emission flag (field flag E) is set by the operator, B
gets set automatically.
Subsequent Action: none.
---------------------------------------------------------------------
D deferred Step 1: if SASS failed running detect
Step 2: the usual method
If, for any reason, the operator believes that a proper
treatment would take too much time, or new software is required etc,
the field can be deferred.
Subsequent Action: Whenever this flag is set, all source flags n
are automatically set.
---------------------------------------------------------------------
E ext_emis Step 2: substantial extended emission
This is subjective, and will normally be set for clusters of
galaxies, supernova remnants, etc. It requires enough extended
emission to affect source measurements and background calculations.
As a guideline, we recommend that the size of the extended emission
exceeds the size of the largest detect cell (2') by a factor of two
or so, i.e. the emission patch be of order 5' or greater.
Subsequent Action: Whenever this flag is set, field flag B is
automatically set.
---------------------------------------------------------------------
F fals_det Step 3: f source flag set for >= 1 source.
Whenever a source is "deleted" with the false detection flag,
this field flag is set as a general field indicator.
Subsequent Action: none
---------------------------------------------------------------------
M src_mis Step 2: There are one or more missed sources
In order to avoid numerous fake (marginal) sources, this flag
should only be used when it is very obvious that a source is missed by
detect. There will always be sophisticated algorithms that can find
probable sources not detected by SASS, but that is not what we are
concerned with here. A moderately blocked field will probably be the
best method for this test. The operator will click the mouse on these
missed sources and thereby record the position and some measure of the
counts.
Subsequent Action: none
---------------------------------------------------------------------
S slis_mis Step 1: check for missing or empty source file
Subsequent Action: Normally (tbd) the D field flag should be set.
---------------------------------------------------------------------
- 3.2 SOURCE FLAGS
________________
a assoc_nn Step 1: Source associated with a close neighbour
This flag was invented for the PSPC during construction of the
original MPE CAT. For the PSPC, it involved a test to see if two sources
were within a certain distance of each other. This distance depended on
the PRF (function of hardness ratio and off-axis distance), the extent
parameter, and a fudge factor determined by trial and error. Details
for the HRI are described in section 8.
Subsequent Action: set the i flag.
---------------------------------------------------------------------
c confused Step 2: detect confounded by close sources
This is evident only by visual inspection, as e.g. two close
sources with only one detection between them.
Subsequent Action: Whenever this flag is set, also set i, p, and v.
---------------------------------------------------------------------
d det_struct Step 1: set if EPI is > 0.01
EPI is the edge priximity indicator. It is zero if the source
is clear of the edge or detector hotspots. APR95, set threshold to be
0.01 instead of zero. Values of 10^-4 were found, and 0.01 was deemed a
reasonable value for d and spawning i, p, and v.
Subsequent Action: Whenever this flag is set, automatically set
i, p, and v.
---------------------------------------------------------------------
e extended Step 1: set if SIZCOR > 1.2
Note that we have changed the original threshold (>0)
since on inspection, SIZCOR is often just above one, but not
significantly so.
Subsequent Action: Whenever this flag is set, automatically set
i, and p. If the VARIABILITY parameter is "POSSIBLE", then the
v flag should be set.
---------------------------------------------------------------------
f false Step 2: source reality is doubtful
This can be determined only by visual inspection.
Subsequent Action: Whenever this flag is set, set the Field F flag.
---------------------------------------------------------------------
i inten_susp Step 1: if Source a or d is set
Step 2: possible to set by visual inspection
Step 3: if Field A is set; if Src c, e or w is set
The normal mode will be the automatic operations of steps 1
and 3; however there may be other conditions.
Subsequent Action: none
---------------------------------------------------------------------
m mult_det Step 2: multiple detections occurred
Multiple detections occurred for a single source. For the HRI,
this condition will normally be understood to mean 'for the same cell
size'. Occasionally however, a larger cell detection is far enough
removed in position so that it is not matched with the small cell
detection even though by VI, it is obviously the same source. In such
a case, both detections get the m flag, but the erroneous position
detection also gets the false flag set. The VI operator should pay
attention to the position flag whenver he sets m.
Subsequent Action: none
---------------------------------------------------------------------
n not_checked Step 1: If s/n of detection is < tbd (4) sigma
Step 3: If Field is Deferred
The question of s/n threshold has not been addressed
definitivly. We can reduce the amount of VI operator effort by not
examining the large number of detections near threshold; these
detections are difficult to evaluate and would probably be the cause
of significant dispersion in the results since subjective judgement
would be required. For the HRI, the SAO group agrees that the S/N
threshold should be set at 5 sigma, but this may be revised downward.
* During testing in early April 95, we decided to try with s/n = 4 for
threshold. Strickly speaking, n means "not visually checked".
Subsequent Action: none.
---------------------------------------------------------------------
p pos_susp Step 1: if source flag d is set
Step 2: may be set by VI
Step 3: if Field A, Source c, d, or e is set.
For the most part p will be set by other flags: field A,
and source flags c, d, and e. It may also be set manually
during VI.
Subsequent Action: set the 'i' source flag.
---------------------------------------------------------------------
u un_uniq Step 1: based on SASS detection matching
We will recover the matching of numbered detections with the
different cell sizes, which produces letter designated sources. Then,
whenever a detection is matched with a detection made with a smaller
detect cell, the U flag will be set. This is the only method of
recovering a unique source list (i.e. in the database retrieval, do
not take detections with the U flag set to True).
There is, however, a complication when a S/N threshold is set
for the N flag. For sources that are extended or off-axis, a S/N <
threshold may be obtained for the 12" detection whereas the 24" (or
larger) detections will often have S/N > threshold. Therefore, the U
flag by itself can not be the sole criterion for desirability.
Subsequent Action: none
---------------------------------------------------------------------
v varflg_susp Step 1: compare VAR for source and BG;
if Field A or Source d is set
Step 3: if source flag c is set
One needs to make a few tests of the VAR parameter which
has the possible values:
POSSIBLE probability that source is constant < 0.01
NEGATIVE >= 0.01
TOO_FEW less than 50 counts
NEAR_EDGE OFFAX > allowed max (probably 12')
Note that VAR is generated only for detections with the 12" and 24"
detect cells.
a) If the e source flag is set, and VAR=POS, then set the v flag.
b) If VAR(src)=POS *AND* VAR(bkg)=POS, then set the v flag.
Subsequent Action: none.
---------------------------------------------------------------------
w within_ext Step 2: VI
This flag describes a discrete source embedded in extended
emission, e.g. a pulsar within a SNR or an AGN in a cluster. Note
that while w implies the presence of extended emission, it may not
be so strong or extended as to warrant the setting of the field E
flag. It is also possible to have a strong unresolved source in
weak extended emission so that w is set, but not the source flag e.
Subsequent Action: Whenever this flag is set, the 'i' source flag should
be set.
---------------------------------------------------------------------
4.0 FLAG MATRIX
The field flags are upper case, source flages lower case. An
"x" in a given position means the flag for that column should be
automatically set whenever the flag for that row is set, i.e. the
flags along the left border spawn the flags in the indicated columns.
THEN....------->
A B D E F M S a c d e f i m n p u v w
......................................................................
IF... A x x x
B
D x
......................................................................
E x
F
M
......................................................................
S
a x
......................................................................
c x x x
d x x x
e x x x?
......................................................................
f x
i
m
......................................................................
n
p x
u
......................................................................
v
w x
The x? above means set the v flag if variability was labelled as
"possible" in the SASS output.
5.0 SPECIFICATION FOR DISPLAYS
For the visual inspection (VI), a smoothed array is required
because with only photons, weak sources are difficult to evaluate.
Since we do not want to loose much resolution (to sort out close
sources) we believe that two 512 arrays are required: one for the
central part of the field with a resolution close to the instrumental,
and the other of the whole field, with a lower resolution which will
still be adequate for the outer parts of the field. To improve the
S/N ratio, we choose PHA channels 1-8 since 9-15 is mostly noise.
- 5.1 High Resolution Map
We choose a blocking of 4, which results in 2" pixels, and a
FOV=17'. To get 3 pixels per beam, we choose a Gaussain with
sigma=1.27 pixels (2.55") which corresponds to FWHM= 6.0". However,
during testing, we found that this function was too small....the
results were very similar to the blocked photon array. Therefore we
changed the recommendation for Gauss: sigma = 1.7 pixels (3.4"), or
FWHM=8.0". With a blocking factor of 4, the original size is reduced
to a 2048, and to get 512x512 around the center, we choose 769:1280
(for the IRAF designation of section).
.......following paragraph to be deleted once testing verifies above.....
For rh150004, Cen A, even when the 90 detections were reduced
to 12 unique sources with S/N > 5, the jumble in the center precluded
evaluation with the standard blocked image/overlay. Only when a
smoothed image and contour diagram was constructed (block=3, 1.5"
pixels, Sigma Gaussian = 2 pixels, FWHM circa 7") which was a 512x512,
were we able to evaluate the features in the galaxy and jet, and find
a missed source. We suggest that such a smoothed array be made for
each field to be used in source evaluation during VI.
Which of these two choices is tbd.
..........................................................................
- 5.2 Whole Field
Experimenting with fields rolled close to 45 degrees, we found
that a blocking factor of 10 (i.e. 5" pixels) was satisfactory.
Current thinking is to have this be a photon array, i.e. not
smoothed. However, if smoothing is to be implemented, similar
considerations as in section 5.1 lead to Gauss sigma = 1.27 pixels
(6.37"), for a FWHM=15" (3 pix). The section specification is
[155:666].
- 5.3 Graphic Plane overlay
We require a somewhat complex coding for the source position
overlays. First, we want to identify the unique sources which have
s/n > 4. These should be marked in a prominent colour (e.g. cyan)
with either the smallest detect cell box with s/n > 4 OR (tbd) all
detect cells with s/n > 4. Next, we need to mark those sources with
s/n < 4 with a less prominent colour (e.g. blue). Although operators
will not normally examine these sources, they need to be clearly
indicated so that they will not be considered to be 'missed sources'.
Until evaluation is performed, we expect that these overlays will be
useful on both displays, and should be suppressable by the operator.
- 5.4 A note on selecting sources
For both eventual default database retrieval and for choosing
which sources to mark for the operator, we will need a combination of
the source match table, n and u flags. In discussions with MC, we
assume that the source match table (retrieved as per section 6) will be
incorporated into the source table for easy conditional tests. This means
that there will be 5 additional columns for each source, with entries
being source numbers. The 'best' source list will consist of s/n > 4,
which, for us means n=false (thereby also leaving out sources from
deferred fields) AND u=false. However, if u=true, it is imperative to
check (test) to see if the smaller detect cell has n=f. If it does not,
then we will accept the source in question even though u=true.
6.0 RECOVERY OF MATCHED SOURCE LIST
filename: matchsrc.doc
Date: 18 nov 94
originat: deh - from JC email
tlm:
Subject: INSTRUCTIONS FOR RETRIEVING MATCHED SOURCE LIST FOR HRI
- 6.1.0 Get the ...trl file from the FITS
For RDF, using IRAF/PROS, this is done so:
1. get into iraf and pros "xray.xdataio"
with "cl, xray, xdataio"
2. xd> xrfits
input fits filename> /pool14/jcc/srclist/rh110267n00_prt.fits
Output filename:
Override output filename with internal IRAF name? (yes):
For rev0 or other environments, details will differ.
- 6.2.0 Run the AWK script:
To use this task, just type the command: "matchsrc input_filename".
If the input_filename is missing, the program is smart enough to
ask you to re-try it. The input file should be same as OUTPUT.trl
in ROSAT HRI PRT FITS file, but you don't have to name it as "OUTPUT.trl".
Two output files are created :
matchpg.txt - the pages of the match source summary
matchnum.txt- the list of the match source numbers
except the first left one.
It is in a numerical order with one column
in each row, as you requested.
Also, each output file contains "Sequence Number", so the users know
where the data came from originally.
For the RRA, one can either parse the ..pg.txt file if you
need complete information (which sources go with which), or if you
just want to set the "un-unique" flag, you can use the list of
detection numbers in the ...num.txt file.
- 6.3 The AWK script
# ************************************************************
# Module: matchsrc
# Project: Rosat Results Archive - SAO RSDC
# Purpose: Capture the pages of the match source summary and
# the source numbers for which a detection has been
# made with a smaller detection cell.
# Author: JCC at SAO - Nov. 1994
# Updated: {n} -- --
# ************************************************************
rm -f ttmpdmp*
nawk '
BEGIN { if (ARGC != 2)
{print("*** Please use the command: *** ")
print("*** matchsrc input_filename *** ")
exit}
}' $*
# capture the pages of the match source summary
rm -f tmp
echo $1 >> tmp
root=`cat tmp`
echo $root |
awk '{
{if (NR==1)
{ {if ($1 ~ /^$/) exit }
ii = 0
tii = 1
print ("*****************************")
print ("Possible Source Match Summary")
print ("*****************************\n")}}
{if ($1 ~/Sequence/)
print (substr($0,9,length($0)), "\n\n")}
{if ($1 ~/Possible/ )
{ii = NR
tii = NR}}
{if ((ii>= tii) && ($1 !~ /composite/))
{ print substr($0,11,length($0))
++ii}}
{if ($1 ~ /composite/)
{ print substr($0,11,length($0))
exit}}
}' $root > matchpg.txt
rm -f tmp
# read the numbers of match sources and remove the dashes
awk '
{if ($1 ~ /Sequence/) print }
{if ($1 ~ /^[A-Za-z]$|^[A-Za-z][A-Za-z]$/)
{ $1=""
{for (jj=2; jj<=NF;++jj)
{if ($jj ~ /^----$/)
{$jj = "" }}
print $0 } }
}' matchpg.txt > ttmpdmp
# write the numbers of match sources
awk '
{if ($1 ~ /Sequence/) print }
{if ((NF >= 2) || ($1 !~ /Sequence/))
{for (kk=NF; kk>=2; kk=kk-1)
{kkk = kk - 1
{if ($kkk ~ /^[0-9]+$/)
{print $kk} } } }
}' ttmpdmp > ttmpdmp2
# remove duplicates and write it in a
# numerical order
awk '
{if ($1 ~ /Sequence/)
{print}
else {
{source[NR] = $1
{for (jk=NR-1; jk>=1; jk=jk-1)
{if (source[NR] == source[jk])
{source[NR] = ""
break}}}
{if (source[NR] !~ /^$/)
{print source[NR]}}
}}}' ttmpdmp2 | sort +0n -1n > ttmpdmp3
# output the results to matchnum.txt
awk '{
if ($1 ~ /Sequence/) {
print ("\n### ",$0,"\n")
print("***************************************************************")
print("SOURCES for which a detection has been made with a smaller cell")
print("***************************************************************\n")
}
else
print
}' ttmpdmp3 > matchnum.txt
rm -f ttmpdmp*
7.0 DERIVATION OF BACKGROUND
The HRI background, when high, is suppressed by SASS.
However, it may be useful to have a user warning flag which will alert
them to total high rates.... be it from anamalous background or
estended emission from SNR or clusters. We do not have the experience
to decide exactly what threshold to use, but suggest a value of 8
(units are 10^-7 cts/pix/sec). This quantity exists in the .TSI
record.
A possible alternative is to make some test on the histogram
of background. However, if we use just the time averaged value, there
are two ways to get it. One is to recover from the ASCII
printout/copy. It comes from SASS output in slightly different
units...cts/sec/sqarcmin. The other is to use the script written by
Primini.
filename: instr
Date: 13 dec 94
originat: fap/deh
tlm:
Subject: INSTRUCTIONS FOR FINDING THE AVERAGE BACKGROUND FOR HRI
From fap@cfa239.harvard.edu Mon Dec 12 14:39:25 1994
A shell script called hiback.sh which runs fdump and awk to determine
the average background level in an HRI observation from the TSI
records in the _bas.fits file. Eventual use should probably redirect
output to a file or...??
If you don't have ftools, you can probably find another way to get the
appropriate columns from the TSI list.
a command such as:
hiback.sh /proj/rev0/mo/rfits_3_0_new/rh110267/rh110267n00_bas.fits
will produce a histogram showing the time at each level. 1 is low, 14
or so is high. Units are cts/sec/pixel
2 557.998
3 740
4 430
5 120
6 150
7 110
8 10
1 30
Average Background Level: 3.46183
Our initial guess is that if is GT 8, it should be flagged.
However, it might be that a smaller value is warranted, or one might
like to look at the behaviour of the histogram. We do not have a good
sense of how these look for many sequences.
Here is the script 'hiback.sh'
fdump "$1[4]" STDOUT "TIME,FAILED,HIBACK" "-" prhead=no page=no |
awk -f hiback.awk
Here is the AWK, 'hiback.awk'
# awk program to compile histogram of high background levels in TSI
# file.
#
# 11/21/94 fap
#
BEGIN{
TIME = 0.0;
FAILED= 1;
HIBACK= -1;
TOTAL = 0.0;
}
NR>3{
deltaT = $2 - TIME;
if(FAILED==0){
bkhist[HIBACK] += deltaT;
TOTAL += deltaT;
}
TIME = $2;
FAILED = $3;
HIBACK = $4;
}
END{
for (bklev in bkhist) {
print bklev, bkhist[bklev];
avbk += bklev*bkhist[bklev]/TOTAL;
}
print "Average Background Level: ",avbk
}
8.0 SPECIFICATION OF 'ASSOCIATED WITH NEAREST NEIGHBOR'
The rationale for the 'a' source flag comes from the MPE
experience with the PSPC. We envisage two close detections (with the
same size detect cell) which, although fulfilling all SASS tests to
qualify as separate sources, may, in fact, be close enough to affect
the determination of intensity of either or both. Therefore, we
require an algorithm which will identify 'associated' sources.
Although it is conceivable that one of a pair of associated sources
may be flagged (by the operator) as a false detection, we choose to
leave the automatically generated 'a' flag. Hence the definition to
the user should specify that "two detections were found....", (not,
"two sources were found...") and in the spirit of "intensity suspect",
the user may demonstrate that the SASS intensity is, after all,
reliable in such a case.
- 8.1 Input parameters
The basic parameters for the HRI will be the 50% power radius
of the PRF(theta) and the radius of the extended circle. We realize
that the latter quantity is not a reliable measure of the extent of
a source. However, it appears to be the only available measure of
source extent.
To parametrize the PRF we have two options. The first would
be to solve for the 50% power radius as given in section 3.2 of the
HRI CAL report. We could double this number to get a radius that was
closer to 90%. Alternately, we could use the SASS parameter, CRAD,
which, according to the RDF/Rev2 output, purports to be the 90%
encircled energy radius (the DPG defines CRAD as 3.0 * sigma of PRF).
Because of the uncertainty as to the genesis of CRAD, and because it
appears to be too large near the field center (20"), we opt for 2*50%
radius.
The HRI report gives:
r(50)=(2.35/2)SQRT{sig(hri)^2+sig(asp)^2+[sig(mir)+a*theta^b]2} arcsec
with sig(hri)= 0.74 arcsec
sig(asp)= 1.0
sig(mir)= 1.3
a = 0.0205
b = 2.349
theta is the off-axis angle in arcmin
Figure 9 of the HRI report plots this function, showing that it goes
from 2.1" (center) to approx 25" at the edge of the detector.
Since we recommend twice this value, the leading coefficient simply
becomes 2.35
For the extent parameter, we will use the SASS parameter,
REC, radius of the extended circle (which encloses all contiguous
detection cells above threshold). Unlike the PSPC, this is a raw
observable, not a deconvolved estimate of true source extent.
- 8.2 Derived Parameter
Therefore, in order to determine if a 'nearest neighbor' is
likely to disrupt the intensity measurement of a source (counts within
CRAD), we define ARAD (association radius) as:
ARAD = 2 * r(50)
If SIZCOR < 1.2 (i.e. no evidence of extent), this will be the
only new parameter for this source. However, if SIZCOR >= 1.2, then
we define a new circle with center XEC(L2) and YEC(L2) and radius REC.
The reason we must maintain REC with its appropriate center position
can be seen by considering a point source near the edge of a large
cluster of galaxies. For a discrete (external) source which lies
outside the cluster, but not very far from the embedded point source,
we do not want to erroneously assign 'a' to the external source.
- 8.3 Procedure for setting the 'a' flag
There may be better methods of achieving this result, but the
following 'brute force' approach has the advantage of simple coding
and few conditionals.
1) For each source, generate the new parameter ARAD, as specified
above.
2) For each source (s), perform the following test with every other
source (i) detected with the same detect cell size.
a) If 'a(s)' flag is true, (exit).
b) Calculate the distance, d, between s and i (convenient to use L2 pixels).
c) If d < ARAD(s) + ARAD(i), then set both s and i aflag to true. (exit)
d) If SIZCOR(i) >= 1.2, AND distance between s and
XEC(i), YEC(i) < REC(i) + ARAD(s),
set aflag(s) = true; (exit)
e) exit
(exit) means go on to the next source.
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