NAME:
cormapinp - input a galfa file as correlator map.
SYNTAX:istat=cormapinp(desc, m,han=han,binp=binp,smo=smo)
ARGS:
desc: {} file descriptor from galopen() that points at the file
to use. It will be rewound before inputing.
KEYWORDS:
han: if set then hanning smooth the data on input.
binp[n]:{corget} If the data has already been read in, you can pass
it into the routine via binp keyword. In this case no
hanning smoothing is done
smo : If the smooth keyword is set, then the frequency channels
will be smoothed and then decimated by 7. The 7679 channels
will be reduced to 1097 channels. The header locations that
specify the number of frequency channels will also be updated.
RETURNS:
istat: int 1: got all the strips
0: got part of requested map
-1: got no data.
m[2,pnts/strip,7]:{} array of structures holding the returned
data and header. (see below for a description).
DESCRIPTION:
Input a galfa file and load it into a map structure. If the binp=
keyword is used then you can pass in galfa data that has already been
read in via corgetm. Normally you would open the file with galopen()
and then pass in the descriptor. If the file is to be input, desc will
be rewound before the input.
This routine differs from the interrim correlator cormapinp in
various ways:
1. the old routine would read in an entire map. This routine reads in
an entire file.
2. The galfa files are not necessarily sychronized with the start
of a mapping pattern on the telescope. A single strip on the telescope may
take more than 1 galfa file or may start in the middle of a galfa file.
3. You need to be careful with memory usage. Each file returned
is about 300Mb. You need to keep an eye on the computer memory
usage with top when processing. Don't make a whole lot of
copies of the arrays..
The map information is returned as an array m of structures. The
dimensions of the array are:
m[pol,pntsperstrip,npixels]. pol=2
Each element of the array contains the information for a particular
polarization,sample, and pixel. The following example is for
[0:polA,5:sample,6:beamnum]
eg:
m[0,5,6].h the std header for pola,
m[0,5,6].hf the fits header for pola,
m[0,5,6].d[7679] the data for pola
m[0,5,6].p the total power value for this sample (linear scale).
m[0,5,6].az the azimuth position in degrees at the endedncenter of
each sample.
m[0,5,6].za the zenith angle position in degrees at the end of
each sample.
m[0,5,6].raHr the RA in hours at the middle of each sample.
m[0,5,6].decDeg the declination in degrees at the middle of each sample.
m[0,5,6].calscl the cal scale factore (this value is currently not
loaded.
m.h holds the older header information for this sample. It is mainly
blank. You should probably use the m.hf header for the info
The sample order is how it is found on disc. There is no reordering of
the data.
EXAMPLE:
The standard file is 600 seconds long.
idl
@phil
@galinit
1. open file and input via cormapinp.
file='/share/galfa/galf.20050623.a2055.0008.fits'
istat=galopen(file,desc)
istat=cormapinp(desc,m)
the data would then have:
m[0,4,3].d[*] polA sample 4,beam 3
m[1,4,3].d[*] polB sample 4,beam 3
the headers would be:
m[0,4,3].hf polA header sample 4,beam 3
m[1,4,3].hf polB header sample 4,beam 3
2. open file, input it, and then pass the struct to cormapinp
file='/share/galfa/galf.20050623.a2055.0008.fits'
istat=galopen(file,desc)
istat=corgetm(desc,600,b)
istat=cormapinp(desc,m,b=b)
SEE ALSO:
NOTES:
Current status:
* cormapsclk does not yet work since the cal info is not there.
* i've tried cormapbc and it seems to work ok.
---------------------
modhistory
23jun05: stole from cormapinp interrim cor and updated for galfa.
10jul05: added /smo keyword
14jul05: fixed jdenc computation. was failing 8pm to 12 midnite.
(See /pkg/rsi/local/libao/phil/galfa/cormapinp.pro)
NAME:
galclose - close a gal file for i/o
SYNTAX: galclose,desc
ARGS:
desc: {galdescr} - descriptor to close (returned by galopen)
KEYWORDS:
all: if set then close all open descriptors.
DESCRIPTION:
Files opened with galopen() need to be closed with galclose() so that
the resources are freed up.
EXAMPLE:
filename='/share/wapp11/wapp1.20040121.a1849.0004.fits'
istat=galopen(filename,desc)
.. process the data in the file
galclose,desc .. this closes the file when done with the processing.
(See /pkg/rsi/local/libao/phil/galfa/galclose.pro)
NAME:
galfnamepars - parse a fits filename.
SYNTAX: istat=galfnamepars(filename,nmpars)
ARGS:
filename: string fits filename
RETURNS:
istat: int 1 - fits filename format is ok.
0 - filename is not a standard was fits filename
nmpars: {} return structure with filename parsed into
variables.
DESCRIPTION:
Parse a spectral line was file into its component parts. The
returned structure contains:
help,nmpars,/st
DIR STRING '/share/galfa/',;dir with trailing '/'
;(or blank if no dir in filename)
WAPP STRING 'galfa'
DATE STRING '20050709'
PROJID STRING 'a2004'
SEQNUM LONG 6
FITS STRING 'fits'
(See /pkg/rsi/local/libao/phil/galfa/galfnamepars.pro)
NAME:
galftochdr - convert fits hdr to cor header
SYNTAX: istat=galftochdr(desc,h,hf=hf,nrows=nrows,irec=irec)
ARGS:
desc:{galdesc} gal descriptor returned from galopen()
RETURNS:
istat: int 1 ok, 0 eof, -1 error.
h: {corhdr} correlator header
hf:{galhdr} gal hdr extension..
nrows: long number of rows to advance desc.curpos if you
want to update the position.
pol[2,nbrds]: long codes the pol type polA=1, polB=2 for each
spectra on each board.
iscan : long index into desc.scanI[] for this scans data.
DESCRIPTION:
Read in a fits header for the current group and convert it
to a correlator header. If the file is not positioned at
the start of a group, then move forward to the start of the
next group.
NOTE: this routine does not update the position in the file.
You are left pointing at the input position.
This is a lowlevel routine that is not normally called via
corget().
current data being loaded into b1.h from fits header:
tointerimHdr from fitsHdr
--------------------
STD
h.std.time fits.crval5 convert to ast secs
h.std.date yyyyddd
h.std.azttd fits.ENC_AZIMUTH
h.std.grttd fits.ENC_ELEVATIO
h.std.chttd fits.ENC_ALTEL
h.std.posTmMs fits.ENC_TIME
h.std.grpTotRecs desc.scanI.nbrds
h.std.grpNum
--------------------
COR
h.cor.numbrdsused desc.scanI.nbrds
h.cor.numSbcOut desc.scanI.nsbc
h.cor.lagsbcout desc.scanI.nlags
h.cor.boardId desc.scanI.brdNum
--------------------
PROC
h.proc.srcname fits.OBJECT
h.proc.procname fits.OBSMODE with name translation new to old
--------------------
-
history
25jun04 - if frontend = alfa, force rfnum to be 17
13jul04 - check for eof by row.
18jul04 - added if2.. mixer
09aug04 - added rajcumrd decjcumrd
12aug04 - for spider scans with alfa include the pixel number in iar[5]
taken from the pattern name .
14aug04 - for spider scans load iar[0] with a beamwidth.Use stripLen/6.
20aug04 - added iscan keyword to return to user
22oct04 - updated to new header version. wide band has 512 channels
instead of just 256 V1 has the old 256 channel def.
28oct04 - version 3 header
18jul05 - added object, obs_name
(See /pkg/rsi/local/libao/phil/galfa/galftochdr.pro)
NAME:
galgerrdcd - decode the galfa g_err bitmap convert fits hdr to cor header
SYNTAX: gdcd=galgerrdcd(g_err)
ARGS:
g_err[] :int array of g_err values from header
RETURNS:
gdcd[]: {g_errstr} array of structures with decoded values.
DESCRIPTION:
The g_err status word holds overflow information for the galfa
spectromenter. Pol A and B of the same beam always have the same
bits set. There are six flags in the status word. Each flag is decoded
into a separate integer value. The structure field names, bits in the
mask and description are:
S wbUpShSat B0-1 wide band upshift saturation
F wbFftOvr B2-3 wide band fft overflow
S nbUpShSat B4-5 narrow band upshift saturation
F nbFftOvr B6-7 narrow band fft overflow
L nbLpSat B8-99 narrow band low pass filter saturation
M nbMixSat B10-11 narrow band mixer saturation
adcSat B12-13 adc input saturation
For each field it can take on the value 0 thru 3. These values are:
0 - 0 to 15 errors in previous 1 sec
1 - 16 to 255 errors in previous 1 sec
2 - 256 to 4095 errors in previous 1 sec
3 - > 4096 errors in previous 1 sec
note that pola,b will always have the same errors for a given beam.
(See /pkg/rsi/local/libao/phil/galfa/galgerrdcd.pro)
NAME:
galget - read a group of galfa data records.
SYNTAX: istat=galget(desc,b,rec=rec,han=han)
ARGS:
desc:{galdesc} gal descriptor returned from galopen()
RETURNS:
istat: int 1 ok, 0 eof, -1 error.
b: {galget} data structure holdin data.
DESCRIPTION:
This is the lowlevel routine that reads the data from the fits file.
This routine in normally not called by users. The user interface to the
data in the file is via corget(). corget() will call this routine
automatically when it is passed a galDescriptor rather than a
logical unit number(lun).
18jan04 - added h.dop. set it so that it is doppler update
each sbc even if it is not being done. We will load the
correct frequency, velocity into the header so that this
will be true.
19jan04 - force returned data to always be in increasing freq order.
for now key off of flipped keyword (until cdelta1 is fixed).
02feb04 - switch to use galftochdr() to get/convert the header.
14jul04 - if pol data then acf's, do not flip data
20aug04 - added iscan call to galftochdr.
use indar to return the data arrays independant of the order
they are stored on disc.
(See /pkg/rsi/local/libao/phil/galfa/galget.pro)
NAME:
galimgdisp - display a set of correlator records as an image
SYNTAX: img=galimgdisp(b,clip=clip,brdlist=brdlist,pol=pol,col=col,$
median=median,bpc=bpc,ravg=ravg,nobpc=nobpc,$
win=win,wxlen=wxlen,wylen=wylen,wxpos=wxpos,wypos=wypos,$
samewin=samewin,zx=zx,zy=zy,$
mytitle=mytitle,$
hlind=hlind,hlval=hlval,hldash=hldash,hlvlines=hlvlines,$
useind=useind,ln=ln,chn=chn)
ARGS:
b[nrecs]: {corget} correlator data to make image of
RETURNS:
img[nchns,nrecs]: float image of last brd displayed (before clipping).
KEYWORDS:
wb: if set then take the data from the wide band.
clip[]: float value to clip the normalized data to. Default is
.1 of Tsys (3 sigma for 1 sec integratio for nb).
If clip has 1 value then
normalize to (img > (-clip)) < clip. If two value are
provided, then they will the [min,max].
brdlist: long A single number whose decimal digits specify the boards
to display. eg brds 1,2,3,4 would be: brdlist=1234
The boards are numbered 1 thru 8.
pol: int 1,2, (3,4 if stokes) polarization to plot. default is 1:polA
win: int window number to plot in. default is 1.
wxlen: int xlen of window. default 700
wylen: int ylen of window. default 870
wxpos: int xpos of lower left edge of window.default 445
wypos: int ypos of lower left edge of window.default:35
samewin: if set then use the current dimension for the image win.
If you are calling galimgdisp in a loop then setting this
(after the first call) lets the user dynamically adjust the
window size,position.
zx: int ..-3,-2,2,3,4 zoom factor x dimension. Negative numbers
shrink the image positive numbers expand. Negative number
must divide evenly into the number of channels.
zy: int ..-3,-2,2,3,4 zoom factor y dimension (same format as zx)
col[2]: int .. x columns to use to flatten the image in the time
direction. count 0..numberoflags-1. If multiple boards
plotted then the same cols are used for all boards. The
default is no flattening in the time direction.
chn: if set then plot vs channel number rather than freq
bpc:{corget} if supplied then this data will be used to do the
bandpass correction. The default is to average over
all of the nrecs.
nobpc: if set then no bandpass correction is done.
median: if set and bpc not provided, then bandpass correct using
the median of the nrecs rather than the average.
ravg: long bandpass correct with a running average of ravg spectra
scan : long if provided,then routine will input scans data into
b[] before making image. In this case you must also
supply the lun keyword to tell the routine where to
read from.
lun : int if scan keyword provided, then you must also supply
this keyword. It should contain the lun for the
corfile that you have previously opened.
sl[]:{scanlist} This array can be used for direct access when the
scan keyword is used. The sl[] (scanlist) array is
returned from the sl=getsl(lun) routine. The routine
scans the entire file recording where the scans start.
han: if set and scan keyword set, then hanning smooth the
data on input.
maxrecs: int if lun used then the max records of a scan to input.
default:300
mytitle:string user supplied tittle instead of scan,srcname,az,za
az,za at top of the plot.
hlind[]: ind index into img array (2nd dimension) to draw
horizontal lines.
hlval : float value to use for horizontal lines (in img units)
default is clip value.
hldash : int The dash lengths to used for the horizontal lines.
2*ldash must divide into x dimension.default is 4
hlvlines:int Number of engths to used for the horizontal lines.
default=1
useind[2]:int if provided then use these indices from data array
0 .. lengthsbc -1
default=1
ln :int linenumber for title..0..33 def:3
extra_=e this allows you to input keywords that will be
passed to the plotting routine. eg title=title..
DESCRIPTION:
galimgdisp will display a set of correlator records (usually a scans
worth) as an image. By default it will make a separate image for each
subcorrelator (board). The brdlist keyword lets you choose just 1 brd to
image. The data for the image is taken from polA by default.
Use the pol keyword to make the image from the other polarization.
If you use the /wb keyword then the wide band data will be used.
By default, the image is bandpass normalized by the average of all the
records (sbc/avg(sbc) - 1). If the median keyword is used then
avg(sbc) is replaced by median(sbc). The bpc keyword allows you to input
a separate correlator record to use as the normalization.
The col keyword lets you also flatten the image in the time (record)
dimension by specifying the first/last columns to average and then divide
into all of the other columns (the columns are counted from 0). By default
this is not done.
After bandpass correction and flattening in the record dimension, the
image is clipped (by default) to +/- .1 (tsys) and then scaled
from 0 to 256 for the image display. The clip keyword lets you change the
clipping value.
The zx,zy keywords let you scale the image in the x and y dimensions by
integral amounts. Negative numbers will shrink it by that amount (Note:
the negative numbers must divide evenly into the number of channels in
each brd). -1,0,1 do no scaling. This scaling is only applied for the single
brd displays. The multiple brd displays are always scaled to fit
inside the window (700 by 870 pixels).
After displaying the image, use xloadct to manipulate the color table.
The routine returns the last image displayed (before clipping).
EXAMPLES:
input a scans worth of data.
print,corgetm(desc,600,b,/han) .. input scan with hanning smoothing
1. display the image of all 7 brds.
img=galimgdisp(b)
img=galimgdisp(b,/wb) display the wide band data.
2. display only brd 2, scale y by 2, and x by -2
img=galimgdisp(b,brdlist=1,zx=-2,zy=2)
3. display all 7, clip to .015 Tsys , display polB and median filter the
bandpass correction:
img=galimgdisp(b,pol=2,/median)
4. display all brds 1,2,3,4 , clip to .015 Tsys ,
display polB and median filter the bandpass correction:
img=galimgdisp(b,brdlist=1234,pol=2,/median)
This routine calls imgflat, and imgdisp for the image scaling and display.
NOTE:
When displaying only 1 brd and using zx fopr shrinking the image,
zx must divide into the number of channels. For the narrow only zx=-7
works since 7679/7=1097 and 1097 is prime.
SEE ALSO:
imgdisp,imgflat
(See /pkg/rsi/local/libao/phil/galfa/galimgdisp.pro)
NAME:
galmix - compute galfa lo mixing freqs
SYNTAX: mixI=galmix(skyCfr,narBandCfr,rfiSky,use275=use275,lo1Low=lo1Low,$
print=print)
ARGS:
skyCfr : float sky center frequency as set by first lo.
narBandCfr: float center freq we want for narrow band spectra
rfiSky[n] : float compute the IF locations for these sky frequencies
KEYWORDS:
use275: if set then use 275 Mhz for IF1 (the default is 250 Mhz).
lo1Low: if set then use a low side LO1. The default is a high side LO.
print: if set then print out the values (cals galmixpr())
RETURNS:
mixI[n]: {} structure holding the computed information (see below).
DESCRIPTION:
The user specifies the rf sky center frequency (as set by the first
LO) and the center of the narrow band spectra. The routine will then
compute the first and and 2nd lo's to use. You can select an IF1 of
250 (default) or use 275Mhz (by setting /use275.). If lo1Low is set then
the first LO will be a low side LO (the default is high side).
The array rfiSky contains a set of sky frequencies. The routine
will compute where in the if1, if2 bands these frequencies will fall.
If the /print keyword is set then the data will be printed to stdout.
You can pass mixI to galmixpr to print out the info at a later time.
The structure mixI[n] contains:
IDL> help,mixI,/st
SKYF FLOAT 1385.00 sky center freq (set by 1stLO)
NBF FLOAT 1420.41 narrow band cfr
WBF FLOAT 1439.16 wide band cfr
IF1 FLOAT 250.000 if1 used (250 or 275)
LO1 FLOAT 1635.00 first LO.
LO1SB INT -1 -1--> 1stlo high side,1-->loside
LO2 FLOAT 195.844 2nd lo frequency
RFI_SKY FLOAT 1330.00 rfi sky freq
RFI_IF1 FLOAT 305.000 location in IF1 of rfi
RFI_IF2 FLOAT 109.156 location in IF2 of rfi
EXAMPLE:
1. Center the RF at 1385 and the narrow band at 1420.4058. Use the
250Mhz IF for if1. Also look to see where the two faa radars (1330,1350)
fall in the IF band. This setup could be used for a piggy back
observering with the extra galactic crowd.
skyCfr=1385.
nbCfr =1420.4058
rfiSky=[1330.,1350.] ; look at where the 2 faa radars fall
mixI=galmix(skyCfr,nbCfr,rfiSky,/print)
the output is then :
sky nbCen wbCen if1 rfiSky RfiIf1 rfiIf2 lo1 lo2
1385.00 1420.41 1439.16 250 1330.00 305.00 109.16 1635.000000 195.844238
1385.00 1420.41 1439.16 250 1350.00 285.00 89.16 1635.000000 195.844238
2. use the 275 Mhz IF1. Center the RF and the narrow band center at
1420.4058. This is a typical galactic setup with no piggy backing.
skyCfr=1385.
nbCfr =1420.4058
rfiSky=[1330.,1350.] ; look at where the 2 faa radars fall
mixI=galmix(skyCfr,nbCfr,rfiSky,/print)
SEE ALSO: galmixpr
(See /pkg/rsi/local/libao/phil/galfa/galmix.pro)
NAME:
galmixpr - formatted print of galmix() data.
SYNTAX: galmixpr,mixI,notitle=notitle
ARGS:
mixI[n] : {}float info returned by galmix()
KEYWORDS:
notitle: if set then don't print the title. This is handy if you
are calling galmixpr multiple times and you only want
one heading.
DESCRIPTION:
Print the info returned by galmix() to std out.
EXAMPLE:
1. Center the RF at 1385 and the narrow band at 1420.4058. Use the
250Mhz IF for if1. Also look to see where the two faa radars (1330,1350)
fall in the IF band. This setup could be used for a piggy back
observering with the extra galactic crowd.
skyCfr=1385.
nbCfr =1420.4058
rfiSky=[1330.,1350.] ; look at where the 2 faa radars fall
mixI=galmix(skyCfr,nbCfr,rfiSky)
galmixpr,mixI
the output is then :
sky nbCen wbCen if1 rfiSky RfiIf1 rfiIf2 lo1 lo2
1385.00 1420.41 1439.16 250 1330.00 305.00 109.16 1635.000000 195.844238
1385.00 1420.41 1439.16 250 1350.00 285.00 89.16 1635.000000 195.844238
SEE ALSO: galmix
(See /pkg/rsi/local/libao/phil/galfa/galmixpr.pro)
NAME:
galopen - open a galfa fits files for i/o
SYNTAX: istat=galopen(filename,desc,tmI=tmiI,scanI=scanI)
ARGS:
filename: string filename to open
KEYWORDS:
RETURNS:
istat: int 0 couldn't open file
1 file opened successfully
desc: {galdescr} - descriptor holding info for file i/o.
scanI: {} structure holding info about each record in
file. You can use this to sort out where
different patterns started (without having
to read the entire file).
tmI[6]: {} structure holding timing info:
tmI[i].nm label of where the time was measured
tmI[i].tm time value (from call to systime(1)).
The units are seconds (with fraction). To get the
relative time, you should subtract tmI[0].tm from
all of the .tm values or (tmI.tm - shift(tmI.tm,1)
DESCRIPTION:
Open a gal (galfa) spectral line fits file. Load
the descriptor with the info for the entire file. This
descriptor will be passed to the galxxx corxxx routines to do the
file i/o. This descriptor replaces the standard lun that is
used for the interim correlator data.
The descriptor contains:
help,desc,/st
LUN LONG 0 .. idl lun
FILENAME STRING '/share/wapp11/a9999_wapp1_0027.fits' ..filename
TOTRECS LONG 1 .. total recs (integ) in file
TOTROWS LONG 7216 .. total number of rows in bintable
CURPOS LONG 1 .. position for next read 0 based (row-1)
tmStartFile LONG 0 .. secs since 1970 start of file
rowStartRec lonarr(nrecs)
rowsinrec lonarr(nrecs)
-------------------------------
If the scanI keyword is returned, then the scanI[nrecs] structure array
returned contains:
IDL> help,scanI
SCANI 0 STRUCT = -> Array[600]
IDL> help,scanI,/st
SEQNUM LONG 1203 ; seq number from fits file
OBSMODE STRING 'BASKET' ; pattern used
OBS_NAME STRING 'BASKET' ; step in pattern
OBJECT STRING 'lwb_14_00' ; source name
SEC DOUBLE 1.1209410e+09 ;sec from 1970 start of rec. rounded to
closest sec: round(g_time[0]+g_time[1]*1d-6)
AZ FLOAT 359.382 ; az position (deg)
ZA FLOAT 14.7502 ; za position (deg)
RESTFREQ DOUBLE 1420.2858 ; crval1:rest freq Mhz (narrow band)
NUM LONG 0 ; unused.. user can load
The az,za are taken from the file. They are not interpolated to the
center of the data sample.
EXAMPLE:
1. open a file
filenm='/share/wapp11/wapp1.20040118.a1849.0010.fits'
istat=galopen(filenm,desc)
gallist,desc ; list scan summary
istat=corget(desc,b) ; read a record
corplot,b ; plot it
istat=corinpscan(desc,b,scan=401864155,maxrecs=600) ; input a scan
galclose,desc ; when done.
2. open file, return timing info and scanI
istat=galopen(filenm,desc,scanI=scanI,tmI=tmI)
print,tmI.tm - tmI[0].tm
; look for pattern name of CAL
ind=where(scanI.obsmode eq 'CAL',count)
if count gt 0 then ...
process cal records
endif
(See /pkg/rsi/local/libao/phil/galfa/galopen.pro)
NAME:
galprojfiles - find the files belonging to a project id
SYNTAX: istat=galprojfiles(proj,fileInfo,yymmdd1=yymmdd1,yymmdd2=yymmdd2,$
minsize=minsize,dir=dir)
ARGS:
proj: string proj name to search for
KEYWORDS:
yymmdd1: long limit files to those starting on this date (yymmdd1 included)
yymmdd2: long limit files to those starting on or before this date
(yymmdd2 included)
minsize: long minimum size in bytes for file to return. default is
100000 bytes. file less than this usually have no
data (just a header).
dir : string directory to search thru. def: /share/galfa
RETURNS:
istat: number of files found
fileinfo[istat]: array of file info structures containing the name
and size of the file
DESCRIPTION:
Search through the galfa fits directories looking for files that
belong to a particular project. Return an array of stuctures containing
the filename and file size.
(See /pkg/rsi/local/libao/phil/galfa/galprojfiles.pro)
NAME:
galpwr - return power information for a number of recs
SYNTAX: nrecs=galpwr(desc,reqrecs,pwra,lasthdr,b=b,useb=useb,wb=wb)
ARGS:
desc - descriptor opened via wasopen.
reqrecs - requested records to return
KEYWORDS:
wb - if set then return power from wideband data
useb - if set then the user passes the data in via b= keyword.
desc is ignored and no data is read from disc
b[nrecs] - This can be an input and an output keyword. If /useb is
set, then the user is passing in the spectral data in the
b=b keyword (which means you need to have previously read
it). If /useb is not set, but b=b is provided, then the
spectral data read in will be returned in b.
RETURNS:
pwra - returns an array pwra[nrecs] of {corpwr} struct
nrecs - number of recs found, 0 if at eof, -1 if hdr alignment/io error
b[nrecs] - if keyword b= is supplied, then the input spectral data will
be returned in this keyword.
DESCRIPTION:
Return the total power information for the requested number of
records of a galfa file. The data is returned in the array pwra.
Each element of thearray contains:
pwra[i].scan - scan number.. this is 0 for galfa:
pwra[i].rec - record number in the file (count from 1)
pwra[i].time - seconds from midnight for this record
pwra[i].nbrds- number of boards in use
pwra[i].az - az (deg) end of this record.
pwra[i].za - za (deg) end of this record.
pwra[i].azErr- az (asecs great circle) . not available galfa
pwra[i].zaErr- za (asecs great circle) . not available galfa
pwra[i].pwr[2,8] - total power info. first index in pol1,pol2
2nd index are 8 pixelss (only the 1st 7 are used with
galfa.
There will only be valid data in the first pwra[i].nbrds entries of
pwra.
EXAMPLES:
;
; 1. get the pwr from the entire file
rew,desc
nrecs=galpwr(desc,600,p)
; 2. same thing but also return the spectral records for later use
rew,desc
nrecs=galpwr(desc,600,p,b=b)
; 3. use the spectra data in b we read from 2. to now get the
; wide band data. This is quicker since we don't have to re read
; all the spectral data.
nrecs=galpwr(desc,600,pwb,b=b,/useb)
; 4. read in the spectral data with corgetm and the compute the power.
istat=corgetm(desc,600,b)
nrecs=galpwr(desc,600,p,/useb,b=b)
(See /pkg/rsi/local/libao/phil/galfa/galpwr.pro)
NAME:
galripple - look at ripple in galfa bandpass
SYNTAX: galripple,b,hard=hard,bfit=bfit,win=win,mytitle=mytitle,$
spcar=spcar,deg=deg,fsin=fsin,nospc=nospc,tosmo=tosmo
ARGS:
b: {corget} bandpass to use. Normally you would input a file, average
it, and then pass the averaged spectra in.
KEYWORDS:
hard: if set then user wants hardcopy. This will not plot the
baseline fits.
bfit:{corget} This is the fit from corblauto(). If it is passed in as
a corget structure then it will be used rather than calling
corblauto(). This speed things up if you call the routine
multiple times with the same bandpass.
win : string Window function to use when computing the transform of the
spectrum. Values are:
'cos4' cos^4 window
'han' hanning smoothing.
The default is no windowing.
mytitle: string If supplied then it will be plotted at the top of the
page.
deg : int The deg for the polynomial portion of the fit done by
corblauto().
fsin : int The order of the harmonic fit done by corblauto()
nospc : If set, then don't plot the smoothed bandpass corrected
spectra.
RETURNS:
bfit: {corget} If supplied and the input is not a {corget} then the
corblauto() fit is returned here.
spcar[nchn,2,nbeams]: float this is the transform of the bandpass.
DESCRIPTION:
galripple was used to look at the 174 Khz rippled caused by reflections
in the fiber optics cable. It takes an galfa bandpass as input.
It will then :
1. fit the bandpass with corblauto(). The default is a linear polynomial
and a 7th order harmonic. This gets rid of ripples with a spacing up
to 1 Mhz. You can change the order using deg= and fsin=
2. Divide the bandpass by the fit in 1.
3. Smooth the spectra from 2 by tosmo. The default is 19 channels.
4. if the keyword /nospc is not set then plot the bandpasses from 3. Pol
A and polB are on separate pages.
5. compute the transform of the spectra in 4:
spc=abs(fft(spc3))*2.
The 174 Khz rippled should show up in channel 39 or 40.
Then plot this spc for each pixel. Black in polA, red is polB
EXAMPLES:
istat=corgetm(desc,600,b)
bavg=coravg(b)
galripple,bavg
(See /pkg/rsi/local/libao/phil/galfa/galripple.pro)