Command over commands Chrisphin Karthick,ARIES-2006-2007 1-Linux commands From open terminal: >ls --To list out >mkdir foldername-------making a directory >rm -f (directory name) -----removing directory >rm -rf (directory name)----for removing subdirectories also (* always represents for bulk files or folders) >cp <source> <destination>--------for copy >cp –r <source> <destination>----whole directory >mv <source> <destination>-------for move >mv <source> <destination>----for renaming also >pwd----------------present working directory >cd <directoryname>-------changing directory >cd --------------------------->coming out to the home. >cd .. -------------------->coming out one step back from the source directory gzip file-----for making .zip >gunzip filename.gz ---------for unzip >gunzip *.gz--for unzipping lot of files >tar -xvpf filename.tar ---for untar>tar -xvf <filename>----- to extract the tar file >tar -zxvf <filename> To extract the tar and zipped file >tar -cvf filename.tar filename making tar >zcat <filename.tar.gz> | tar xvf - ---------for removing zip and tar in one time the command is > find . -name "filename"--------For finding one file within the computer (or) >lpr -P <printerName> <filename> ---------for printing >lpr <filename>-----------if you don’t want mention particular printer ---by default printer printing >lpq---to list out the printing materials: ( it will come as file name and with its number) >lprm <therespectivenumber>---to stop the priniting material: >gthump <photo filename>----For viewing photo: alt+Esc------To switch over to another window; alt+tab--------To view and select the alternate window: ctrl+alt+backspace ---------for logout >reboot-------to reboot the computer. to run latex ; >latex <file name>1
111
Embed
Command over commands Chrisphin Karthick,ARIES20062007 · **If the bookmark has been hidden by sekecting aniother profile to retrive it go to chrisphin>cd .mozilla/ ... Chrisphin
This document is posted to help you gain knowledge. Please leave a comment to let me know what you think about it! Share it to your friends and learn new things together.
Transcript
Command over commands Chrisphin Karthick,ARIES20062007
1Linux commandsFrom open terminal:>ls To list out >mkdir foldernamemaking a directory>rm f (directory name) removing directory >rm rf (directory name)for removing subdirectories also(* always represents for bulk files or folders)>cp <source> <destination>for copy >cp –r <source> <destination>whole directory>mv <source> <destination>for move>mv <source> <destination>for renaming also>pwdpresent working directory>cd <directoryname>changing directory>cd >coming out to the home.>cd .. >coming out one step back from the source directorygzip filefor making .zip >gunzip filename.gz for unzip >gunzip *.gzfor unzipping lot of files>tar xvpf filename.tar for untar >tar xvf <filename> to extract the tar file>tar zxvf <filename> To extract the tar and zipped file>tar cvf filename.tar filename making tar>zcat <filename.tar.gz> | tar xvf for removing zip and tar in one time the command is > find . name "filename"For finding one file within the computer (or) >lpr P <printerName> <filename> for printing>lpr <filename>if you don’t want mention particular printer by default printer printing>lpqto list out the printing materials: ( it will come as file name and with its number)>lprm <therespectivenumber>to stop the priniting material: >gthump <photo filename>For viewing photo:alt+EscTo switch over to another window; alt+tabTo view and select the alternate window: ctrl+alt+backspace for logout>rebootto reboot the computer.to run latex; >latex <file name>
1
Command over commands Chrisphin Karthick,ARIES20062007
>dvips <latexoutputfile> o <newfilename.ps> (OR) >dvips o <.ps> <latexoutputfile.dvi> >gv < .ps>>man commandnamefor help on any commands.> xpdf <file name>to open pdf document:(OR)> gv <file name>> ooffice <filename.ppt>to open ppt:>ps2pdf <filename.ps> <filename.pdf>To change .ps file to .pdf file>du s to check disk space in a directory 13026152 >ps afto display all the processes running on the hostUID PID PPID C STIME TTY TIME CMD501 3618 3545 0 11:00 pts/1 00:00:00 ps af> du kTo report size (in kBytes) of all enclosed directories (recursive)> du ms *To report size (in kBytes) of all enclosed directories (nonrecursive)> usersTo list login IDs of users currently logged in to the system
Transwering data's from one computer to another:>ps –aux | grep <filename>listing out the particular file running on the terminal ID>ftp <that computer number>means >ftp IPaddress OR>gftp username@IPaddress or generally >sftp username@IPaddressthen mget* or mput*or >scp –r username@IPaddress: pathway of file or folder>yum install softwarenamefor installing anything in new fedora version.
For creating webpage
>mozillathen from file GO EDIT PAGE then from edit page file GO COMPOSURE PAGEnow start work .
to get the details of memory capacity of all ....chrisphin > dfFilesystem 1Kblocks Used Available Use% Mounted on
2
Command over commands Chrisphin Karthick,ARIES20062007
>clearto clear the terminal>setupto set up the configuration of computer.
for .fits file getting details from the terminal...type>more <filename>cosmic > more csa104b02.fitsSIMPLE = T / Fits standardBITPIX = 32 / Bits per pixelNAXIS = 2 / Number of axesNAXIS1 = 1024 / Axis lengthNAXIS2 = 1024 / Axis lengthEXTEND = T / File may contain extensionsORIGIN = 'ESOMIDAS' / FITS file originatorDATE = '20060731T08:43:32' / Date FITS file was generatedIRAFTLM= '10:41:08 (03/08/2006)' / Time of last modificationOBJECT = 'sa104 ' / Name of the object observedCOMMENT NOST 1002.0: Hanisch,R. et al. 2001, Astron. & Astrophys. 376, 559
3
Command over commands Chrisphin Karthick,ARIES20062007
CRPIX1 = 1. / Reference pixelCRVAL1 = 1. / Coordinate at reference pixelCDELT1 = 1. / Coord. incr. per pixel (original value)CTYPE1 = ' ' / Units of coordinateCRPIX2 = 1. / Reference pixelCRVAL2 = 1. / Coordinate at reference pixelCDELT2 = 1. / Coord. incr. per pixel (original value)CTYPE2 = ' ' / Units of coordinateBUNIT = ' ' / Units of data valuesDATAMAX = 437.2375 / Maximum data valueRA = 12:42:22 / MIDAS desc.: O_POS(1)DEC = 00:40:00 / MIDAS desc.: O_POS(2)DATEOBS= '20060503T17:01:25' / MIDAS desc.: O_TIME(1)TMSTART= 0. / MIDAS desc.: O_TIME(5)EXPTIME = 260. / MIDAS desc.: O_TIME(7)EPOCH = 2000ST = 13.085UT = 17.02361AIRMASS = 1.146693UTMIDDLE= '17:03:35.0'
Notes:always name the file without space.(if space is ther mv or cp or any command wont work)ex:file name: optical telescope.doc (wrong)file name : opticaltelescope.doc (right)
**If the bookmark has been hidden by sekecting aniother profile to retrive it go to chrisphin>cd .mozilla/.mozilla>ls>cd firefox>lschrisphin default>cd chrisphin>ls>vi bookmark.htmlchrisphin>firefox&
>mplayer <filename.avi>To play the .avi format movie.chrisphin > bc lqFor using terminal as a calculator1+12:quit
4
Command over commands Chrisphin Karthick,ARIES20062007
writting a program and executing:>vi <filename>.................:wqSome version problem while transforming tex file (gvim to vi somethinlg like that)in vi file u may come across the problem of ^Mthen :%s/^M/ /g>c++ <filename> (for combiling)>.a/. out
sort all the files w.r.t.to time:>ls lrt
>vol for volume.
Using as super user >su >user name:>password:
while deleting press shift+delete (by right click)...then it wont go to the recycle bin.(in windows)
For making use of alias command:>vi .cshrc
alias x "ds9 &; xgterm.fedora & "alias hedit "/home/chrisphin/bin/./hedit"alias aries "cd /home/chrisphin/data/ariesasper25oct06fits"~~:wq>source .cshrc>rehash .cshrc>now execute the respective it will work.
5
Command over commands Chrisphin Karthick,ARIES20062007
To know that which shell we are working :[chrisphin@aries25 ~]$ echo $SHELL/bin/cshfor changing the shell type[chrisphin@aries25 ~]$chshpassword:changing the shell type >cshthen for making alias commands......]vi .cshrc or vi .bashrc depends on the shell........then inside vi editor type
alias x “xgterm&;ds9&;”:wq
To configure the computer IP address:>cd /sbin>ls ifco*> ./ifconfig(Then number and other details will come)
for writing into cd:go to the root >supassword>xcdroast(but before that confirm that whether it is installed xcdroast in /usr/bin)
6
Command over commands Chrisphin Karthick,ARIES20062007
Installation of real player in linuxdownload the filethen> chmod a+x <filename.bin> (making executable by changing the mode)
> ./<filename.bin>that,s it.
>xmms&For hearing songs linux the command is
(for installing anything like this ...download RPM file and double click it it will ask for root paswordthat is it it will install automatically.(in fedora core 5 version..that also noneed type yum install<installing file> it will install)
How to write and execute the c programme:1.make a folder within that...within that make one file...programm file ...write by vi editer.that file extensions with .c(for c) or .cpp (for c++)...like file.c or file.cpp>gcc o o_file file.cor >c++ file.cpp
For making alias commands:
chrisphin~>vi .bashrc
PS1="\u\w"\> (this command is for setting the prompt)alias x="xgterm.fedora & ds9&"alias e="emacs &"alias rm="rm i"alias rmr="rmr i"alias g="gomidas"
:wq
chrisphin~>source .bashrc
For bringing scroll bar into iraf the command is as follow and also
7
Command over commands Chrisphin Karthick,ARIES20062007
midas wavelength calibration files is as attachment see the attachment below thanks:.....xgterm sb fn 10*20 &
1.1Printer Configuration for ARIES
adding a printer or printer settings:go to system settingprinting
printer name:DN2420networked jet direct202.141.125.4 port:9100HPLASER JET 2420(if not any 2300)finish.
2.Summary of preprocessing:
1. Converting file into fits format.2. Setting Observatory*3. Setting Airmass*4. Making Master biasBias subtraction5. Making Master flat and then Normalized flat for respective filter divide it.
i. e.,{The final image= (raw image – master bias) / normalized flat(how to normalise a flat...take the mean counts of master flat and divide the master flat by that)}
6. Align it.7. Trim it.8. Cosmic rays removal.9. Cleaned image is ready.
(*In the above mentioned steps where 2 and 3 you can do it later also if needed).
Easy way to handling the file and folder name :In this book Prefix given to the file as...object_r1.fits object _filter nth frame.(here example taken as r—filter)bi_1.fitsbias_nth framefl_r1.fitsflat_filter nth framembi.fitsmaster biasmfl_r.fits—master flat_filter
8
Command over commands Chrisphin Karthick,ARIES20062007
Regarding folder:1. floder name as yyyy_mm_dd2. for original data3. all preprocessing4. outside the current working.
03IRAF Commands (Before data reduction )
Hint & Summarise:Before starting reduction....what are things to be noted in mind.Depends which telescope data you are using..change the signal to noise ratio.....and gain....value asked in ....while 1.epar zerocombine—for bias2.epar flatcombine—for flat3.epar imcombinefor object at last only(after preprocessing individual frames )4.
epar display.....it should be fill = yes) scale image to fit display window
otherwise it will be without binning..it will show the bigger image.
While spectro reduction ...better to cut the unwanted portion.....means trimming...other wise unwanted
9
Command over commands Chrisphin Karthick,ARIES20062007
lines will be produced...in corner side of the spectrum.
In spectro....disp command wont work.....only display ...will work.
to bring control bar in the iraf terminal pressctrl+right clickin the cursor>e ........typing like this we can get the earlier commands
to come out or interupt: ctrl+c
Converting fts file to fits file .From the terminal[chrisphin@aries25 22mar07]$ wr2fits <imagename>Image info: image nameFilter: <filter Name>where wr2fits is an executable file....which is in the computer.written only for the image name andfilter for ARIES.
[chrisphin@aries25 22mar07]$ wr2fits bi*Totally are to be processedPlease enter the default parameters : Image info : bias Filter : none1 ) Input file: bi_1.fts outputfile: bi_1.fits2) Input file: bi_2.fts outputfile: bi_2.fits
10
Command over commands Chrisphin Karthick,ARIES20062007
ob1.fits ,ob2.fits....if v you want to make a list then :
> ob *.fits >>jude> !emacs jude &
cl> show versionNOAO/IRAF V2.12.2EXPORT
cl>show printerlp
cl> refer photometry
cl> help [az]*
For saving the Graph:
:.snap epsflTo make a list :
suppose there are frames like.flr1.fits,flr2.fits...................flr9.fits
you wants to make a list (for bias subtraction..for all at a time...through epar ccdproc..then.)
>ls flr* >list
im> edisp aobject_r1.fits frame to be written into (1:4) (2): z1=1380.411 z2=1612.45im> display zs zr z1=1500 z2=3000image to be displayed (tn1156r01.fits): frame to be written into (1:4) (2): z1=1500. z2=3000.im> display zs zr z1=230 z2=900
11
Command over commands Chrisphin Karthick,ARIES20062007
image to be displayed (tn1156r01.fits): ctn1156a01.fits frame to be written into (1:4) (2): 1z1=230. Z2=900.Where z1 be the the sky counts.And z2 be the object counts.Simply the range must be in betweeen these values.For the above command while displaying where the sky count shows the z1=<1500z2=some thing like 2350 to 2620....so it has given that z1=1500 z2=3000
while combining the images if you want to see the details on the screen itself, then give in the place.....
logfile =STDOUTthen you can see the output there itself.HINT:Always try to make the output file in the form of .imh (means leave automatically it will takethe extension of .imh)then the storage space you will get more .Then convert that into fits formatby the command “wfits”
cc> wfits mbi.imh FITS filename(s) (mbi): Image 1: mbi.imh > mbi.fits bias_img Size = 2048 x 2048 pixtype=real bitpix=32 blkfac=fixed scaling=none 3 Header 5826 Data logical (2880 byte) records writtenActually this imh file stores at /iraf/imdirs/chrisphin.So before take into another computer better tochange it into fits format.
About imexam:>imexam
go to the ds9 image....and placing the cursor on a star.press
Command over commands Chrisphin Karthick,ARIES20062007
w—logfile will close. while displaying the images if it fills the images full of window of ds9(SAO)then go to the display and change the below shown ( darken region) no to yes.now display it will be o.k. cc> epar display
PACKAGE = tv TASK = display image = image to be displayedframe = 1 frame to be written into(bpmask = BPM) bad pixel mask(bpdispl= none) bad pixel display (none|overlay|interpolate)(bpcolor= red) bad pixel colors(overlay= ) overlay mask(ocolors= green) overlay colors(erase = yes) erase frame(border_= no) erase unfilled area of window(select_= yes) display frame being loaded(repeat = no) repeat previous display parameters(fill = yes) scale image to fit display window(zscale = yes) display range of greylevels near median(contras= 0.25) contrast adjustment for zscale algorithm(zrange = yes) display full image intensity range(zmask = ) sample mask(nsample= 1000) maximum number of sample pixels to use(xcenter= 0.5) display window horizontal center(ycenter= 0.5) display window vertical center(xsize = 1.) display window horizontal size(ysize = 1.) display window vertical size(xmag = 1.) display window horizontal magnification(ymag = 1.) display window vertical magnification(order = 0) spatial interpolator order (0=replicate, 1=linea(z1 = ) minimum greylevel to be displayed(z2 = ) maximum greylevel to be displayed(ztrans = linear) greylevel transformation (linear|log|none|user)(lutfile= ) file containing user defined look up table(mode = ql)
13
Command over commands Chrisphin Karthick,ARIES20062007
:wqFor trimming;PACKAGE = ccdred TASK = ccdprocimages = @list List of CCD images to correct(output = T//@list) List of output CCD images(ccdtype= ) CCD image type to correct(max_cac= 0) Maximum image caching memory (in Mbytes)(noproc = no) List processing steps only?
(fixpix = no) Fix bad CCD lines and columns?(oversca= no) Apply overscan strip correction?(trim = yes) Trim the image?(zerocor= no) Apply zero level correction?(darkcor= no) Apply dark count correction?(flatcor= no) Apply flat field correction?(illumco= no) Apply illumination correction?(fringec= no) Apply fringe correction?(readcor= no) Convert zero level image to readout correction?(scancor= no) Convert flat field image to scan correction?
(readaxi= line) Read out axis (column|line)(fixfile= ) File describing the bad lines and columns(biassec= ) Overscan strip image section(trimsec= [25:999,25:999]) Trim data section(zero = ) Zero level calibration image(dark = ) Dark count calibration image(flat = ) Flat field images(illum = ) Illumination correction images(fringe = ) Fringe correction images(minrepl= 1.) Minimum flat field value(scantyp= shortscan) Scan type (shortscan|longscan)(nscan = 1) Number of short scan lines
(interac= no) Fit overscan interactively?(functio= legendre) Fitting function(order = 1) Number of polynomial terms or spline pieces(sample = *) Sample points to fit
14
Command over commands Chrisphin Karthick,ARIES20062007
(naverag= 1) Number of sample points to combine(niterat= 1) Number of rejection iterations(low_rej= 3.) Low sigma rejection factor(high_re= 3.) High sigma rejection factor(grow = 0.) Rejection growing radius(mode = ql)
if you want to be “ y ' section to be reamain then [x1:x2,*]then for apeture photometry small correction:
where in midas if you want use as the terminal for all the commands..then before command type $...ex:> $ls
For summing the subexposures images (for the same filter)Ex: imageu1.fits 15min }image u2.fits15min }imageu1.fits45min—imageu3.fits15min } The task is>epar imcombinePACKAGE = immatch TASK = imcombine
input = image*.fits List of images to combine* represents all the images with output = fnbhal.fits List of output images (combine= sum) Type of combine operation(rdnoise= 4.8) ccdclip: CCD readout noise (electrons)(gain = 1.22) ccdclip: CCD gain (electrons/DN):goOthers are all by default only change the above darkened.Note: Change the exposure time in imheader for the output
15
Command over commands Chrisphin Karthick,ARIES20062007
:goObservatory identification (obspars):Using observatory parameters from observatory task# Observatory parameters for ARIES observatory = obspars timezone = 5.5 altitude = 1950. latitude = 29.36 longitude = 280.5140000000001 name = ARIES
16
Command over commands Chrisphin Karthick,ARIES20062007
05. Setting Airmass for hct one prog has written it is /home/chrisphin/bin/airmass1 this will do by itself.
for that >noao>astutil>astheditas> astheditImages to be operated upon ( wobject.fits): File of commands (/home/chrisphin/bin/airmas1): 17.761111111111112006.193675691432453807.240046310.374161111111111.12053504889221
then check the imheader;as> imhead wobject.fits lo+
images = nobj* Input images(observa= obspars) Observatory for images(intype = beginning) Input keyword time stamp(outtype= effective) Output airmass time stamp
(ra = ra) Right ascension keyword (hours)(dec = dec) Declination keyword (degrees)(equinox= epoch) Equinox keyword (years)(st = st) Local sidereal time keyword (hours)(ut = ut) Universal time keyword (hours)(date = dateobs) Observation date keyword(exposur= exptime) Exposure time keyword (seconds)(airmass= airmass) Airmass keyword (output)(utmiddl= utmiddle) Midobservation UT keyword (output)(scale = 750.) The atmospheric scale height(show = yes) Print the airmasses and midUT?
:go
06Basic Reduction
from terminal>xgterm.fedora&>ds9&
then from xgterm terminalchrisphin > cl NOAO PCIRAF Revision 2.12.2EXPORT Sun Jan 25 16:09:03 MST 2004 This is the EXPORT version of PCIRAF V2.12 supporting most PC systems.
Welcome to IRAF. To list the available commands, type ? or ??. To get detailed information about a command, type `help command'. To run a command or load a package, type its name. Type `bye' to exit a package, or `logout' to get out of the CL. Type `news' to find out what is new in the version of the system you are using. The following
18
Command over commands Chrisphin Karthick,ARIES20062007
then go to the respective file.In the upcoming task commands consider only about the darken region others are all default
cc>epar zerocombinefor making master biasPACKAGE = ccdred TASK = zerocombine input = b*.fits List of zero level images to combineall bias images by * mark(output = mbias.fits) Output zero level name(combine= median) Type of combine operation(reject = none) Type of rejection(ccdtype= ) CCD image type to combine(process= no) Process images before combining?(delete = no) Delete input images after combining?(clobber= no) Clobber existing output image?(scale = none) Image scaling(statsec= ) Image section for computing statistics(nlow = 0) minmax: Number of low pixels to reject(nhigh = 1) minmax: Number of high pixels to reject
19
Command over commands Chrisphin Karthick,ARIES20062007
(nkeep = 1) Minimum to keep (pos) or maximum to reject (neg)(mclip = yes) Use median in sigma clipping algorithms?(lsigma = 3.) Lower sigma clipping factor(hsigma = 3.) Upper sigma clipping factor(rdnoise= 5.3) ccdclip: CCD readout noise (electrons)(gain = 10) ccdclip: CCD gain (electrons/DN)(snoise = 0.) ccdclip: Sensitivity noise (fraction)(pclip = 0.5) pclip: Percentile clipping parameter(blank = 0.) Value if there are no pixels(mode = ql)
(if you are giving type of rejection is avgclip then no need of giving ccd parameters???correct it...this.)cc> imstat mbias* IMAGE NPIX MEAN STDDEV MIN MAX mbias.fits 1048576 1.949 0.9981 3. 7. mbias1.fits 1048576 1.934 0.8802 2. 6.(above mbias.fits is the combination of median and ccdclipmbias1.fits is the combination of median and none)
for substracting master bias from all the images use ccdproc command. or if you wants to do it one by onethen use imarith command>imarith inputimage – mbias.fits outputimage
>ls *.fits >>listJust to do all at one time make a list and do at one stroke.cc>epar ccdproc PACKAGE = ccdred
20
Command over commands Chrisphin Karthick,ARIES20062007
TASK = ccdproc images = @list List of CCD images to correct(output = b//@list) List of output CCD images(ccdtype= ) CCD image type to correct(max_cac= 0) Maximum image caching memory (in Mbytes)(noproc = no) List processing steps only?(fixpix = no) Fix bad CCD lines and columns?(oversca= no) Apply overscan strip correction?(trim = no) Trim the image?(zerocor= yes) Apply zero level correction?(darkcor= no) Apply dark count correction?(flatcor= no) Apply flat field correction?(illumco= no) Apply illumination correction?(fringec= no) Apply fringe correction?(readcor= no) Convert zero level image to readout correction?(scancor= no) Convert flat field image to scan correction? (readaxi= line) Read out axis (column|line)(fixfile= ) File describing the bad lines and columns(biassec= ) Overscan strip image section(trimsec= ) Trim data section(zero = mbias.fits) Zero level calibration image(dark = ) Dark count calibration image(flat = ) Flat field images(illum = ) Illumination correction images(fringe = ) Fringe correction images(minrepl= 1.) Minimum flat field value(scantyp= shortscan) Scan type (shortscan|longscan)(nscan = 1) Number of short scan lines(interac= no) Fit overscan interactively?(functio= legendre) Fitting function(order = 1) Number of polynomial terms or spline pieces(sample = *) Sample points to fit (naverag= 1) Number of sample points to combine(niterat= 1) Number of rejection iterations(low_rej= 3.) Low sigma rejection factor(high_re= 3.) High sigma rejection factor(grow = 0.) Rejection growing radius(mode = ql)
:go
21
Command over commands Chrisphin Karthick,ARIES20062007
then running as...sa104b07.fits: Jul 26 14:43 Zero level correction image is mbias.fitssa104r01.fits: Jul 26 14:43 Zero level correction image is mbias.fits
then the result will come with substracted with the name of b<filename>.fits.ex: bobject_r1.fits
now the images are all bias substracted...from master bias.fits.cc> epar flatcombinedo it for same filter images alone in one for flat combine using thisPACKAGE = ccdred TASK = flatcombine
input = bflat_r* List of flat field images to combinebias subtracted all flat images of oneparticular filter
(output = mfl_r.fits) Output flat field root name(combine= median) Type of combine operation(reject = avsigclip) Type of rejection(ccdtype= ) CCD image type to combine(process= no) Process images before combining?(subsets= no) Combine images by subset parameter?(delete = no) Delete input images after combining?(clobber= no) Clobber existing output image?(scale = mode) Image scaling(statsec= ) Image section for computing statistics(nlow = 1) minmax: Number of low pixels to reject(nhigh = 1) minmax: Number of high pixels to reject(nkeep = 1) Minimum to keep (pos) or maximum to reject (neg)(mclip = yes) Use median in sigma clipping algorithms?(lsigma = 3.) Lower sigma clipping factor(hsigma = 3.) Upper sigma clipping factor(rdnoise= 5.3) ccdclip: CCD readout noise (electrons)(gain = 10) ccdclip: CCD gain (electrons/DN)(snoise = 0.) ccdclip: Sensitivity noise (fraction)(pclip = 0.5) pclip: Percentile clipping parameter(blank = 1.) Value if there are no pixels(mode = ql)
;go
Jul 26 14:57: IMCOMBINE
22
Command over commands Chrisphin Karthick,ARIES20062007
like that do it individually for all the different filters.
For normalisation:cc> imstat mfl_r.fits # IMAGE NPIX MEAN STDDEV MIN MAX mfla.fits 1048576 5411. 173.7 1.957 8428.cc> imarith mfl_r.fits / 5411. nfl_r.fits (like that do it for other filter.)
images = test_5430.fits[1051:1055,955:959] Images to be editedvalue = 3.5 Replacement pixel value(imagina= 0.) Imaginary component for complex(lower = INDEF) Lower limit of replacement window(upper = INDEF) Upper limit of replacement window(radius = 0.) Replacement radius(mode = ql)
24
Command over commands Chrisphin Karthick,ARIES20062007
07Alignment
first display the respective frame....in ds9.alway stry to choose the red filter frame as are referenceone.cc> disp nobject_r1.fitsframe to be written into (1:16) (2):1z1=1.951634 z2=15.75021
to create an file type :cc> epar imexamPACKAGE = tv TASK = imexamine input = nobject_r1.fits images to be examined(output = ) output root image name(ncoutpu= 101) Number of columns in image output(nloutpu= 101) Number of lines in image outputframe = 1 display frameimage = image name(logfile= al.co) logfile(keeplog= yes) log output results
:goLog file al.co open
Then in image selct some number of stars by placing 'cursor 'in the middle of a star and press 'a' ....it will give the details of stars in xgterm.the peak value should be within the range of 100028,000. The 28,000 value is with respect to ouraries.then “q”cc>emacs al.cothen delete all other parameter except (the darken region) colum and line cordinates.# [1] nobject_r1.fits hz44# COL LINE COORDINATES R MAG FLUX SKY PEAK E PA BETA ENCLOSED MOFFAT DIRECT 282.88 393.49 282.88 393.49 9.88 15.82 4713. 5.721 318.2 0.20 88 4.08 3.26 3.27 3.29 286.26 438.66 286.26 438.66 10.73 17.45 1044. 5.796 61.75 0.11 39 6.84 3.04 4.01 3.60 420.94 550.00 420.94 550.00 10.52 12.95 66003. 6.676 4326. 0.26 88 3.00 3.13 3.50 3.50 462.09 658.93 462.09 658.93 10.43 15.96 4136. 5.934 259. 0.03 79 3.00 3.11 3.48 3.48 507.39 741.35 507.39 741.35 11.09 16.68 2137. 6.053 134.1 0.10 57 13.0 3.25 3.57 3.72 601.68 613.98 601.68 613.98 11.82 17.62 898.9 5.984 48.34 0.17 67 12.0 3.56 4.00 3.97
25
Command over commands Chrisphin Karthick,ARIES20062007
then save it and close come out.then display the another frame which is going to be aligned wrt reference.cc> display nobject_r2.fits 2z1=0.9973257 z2=15.23859
cc> tvmarkDefault frame number for display (:16) (2): Input coordinate list (al.co):
cc> imexamLog file al.co open
then selct the respective stars in order. then quit from the imagecc> emacs al.cothen the emacs will open like 282.88 393.49 286.26 438.66 420.94 550.00 462.09 658.93 507.39 741.36 601.68 613.98 # [1] nobject_r1.fits hz44# COL LINE COORDINATES R MAG FLUX SKY PEAK E PA BETA ENCLOSED MOFFAT DIRECT 283.33 396.57 283.33 396.57 10.60 15.85 4571. 5.693 303.9 0.21 87 3.00 3.07 3.53 3.53 286.75 441.81 286.75 441.81 11.76 17.64 881.7 5.672 58.21 0.77 27 10.4 3.22 3.79 3.95 421.38 553.07 421.38 553.07 10.65 12.95 65882. 5.804 4333. 0.26 88 22.4 3.11 3.55 3.56 462.56 662.05 462.56 662.05 11.02 16.02 3906. 5.856 248.3 0.43 79 24.3 3.25 3.65 3.67 507.83 744.34 507.83 744.34 10.76 16.75 1994. 6.031 138.5 0.32 75 12.4 3.10 3.48 3.60 602.13 617.12 602.13 617.12 10.66 17.83 735.4 5.956 52.11 52.6 78 5.65 3.11 3.52 3.54
then delete the unwanted make it like the bottom one.....(by taking only the darkened part shownabove)
26
Command over commands Chrisphin Karthick,ARIES20062007
and save it.For cut> (ctrl+x) + rkFor paste >(ctrl+x) + rycc> epar geomap
PACKAGE = immatch TASK = geomap input = al.co The input coordinate filesdatabase= al.co_db The output database filexmin = 1. Minimum x reference coordinate valuexmax = 1024. Maximum x reference coordinate valueymin = 1. Minimum y reference coordinate valueymax = 1024. Maximum y reference coordinate value(interac= no) Fit transformation interactively ?
:goCoordinate list: al.co Transform: al.co Results file: tobject_r2.fitsCoordinate mapping status X fit ok. Y fit ok. Xin and Yin fit rms: 0.01747025 0.04828498Coordinate mapping parameters Mean Xref and Yref: 426.8733 566.07 Mean Xin and Yin: 427.33 569.16 X and Y shift: 0.4870407 3.221664 (xin yin) X and Y scale: 0.9999283 0.9994867 (xin / xref yin / yref) X and Y axis rotation: 359.979 0.000 (degrees degrees)cc> epar geotranPACKAGE = immatch TASK = geotran
27
Command over commands Chrisphin Karthick,ARIES20062007
input = nobject_r2.fits Input dataoutput = aobject_r2.fits Output datadatabase= al.co_db Name of GEOMAP database filetransfor= al.co Names of coordinate transforms in database file
Transforming image nobject_r2.fits to image aobject_r2.fits Using transform al.co in database al.co_db
THAT IS IT HAVE FUN.PACKAGE = tv TASK = tvmarkframe = 1 Default frame number for displaycoords = al.co Input coordinate list(logfile= ) Output log file(autolog= no) Automatically log each marking command(outimag= ) Output snapped image(deletio= ) Output coordinate deletions list (command= ) Image cursor: [x y wcs] key [cmd](mark = circle) The mark type(radii = 0) Radii in image pixels of concentric circles(lengths= 0) Lengths and width in image pixels of concentric (font = raster) Default font(color = 255) Gray level of marks to be drawn(label = no) Label the marked coordinates(number = yes) Number the marked coordinates(nxoffse= 0) X offset in display pixels of number(nyoffse= 0) Y offset in display pixels of number(pointsi= 3) Size of mark type point in display pixelsMore
after alignment check by displaying all the images into different frames.then pressing center in the ds9 display.(then only everthing will be according to centre it willdisplay)
28
Command over commands Chrisphin Karthick,ARIES20062007
08Cosmic ray reduction through MIDAS
Go to the respective file.where the reducing fits files contains.
chrisphin>inmidasESOMIDAS version 06FEBpl1.0 on PC/LinuxMidas 015>Midas 015> set/con daophotonly once at the time of starting
***** DAOPHOT application package version April 1991 enabled *****commands available:ALLSTAR/DAOPHOT Do simultaneous multipleprofilefittingDAOPHOT/DAOPHOT Do stellar photometry in 2dimensional imagesDAOMID/DAOPHOT Convert DAOPHOT tables to MIDAS tablesMIDDAO/DAOPHOT Convert MIDAS tables to DAOPHOT tables
no CDELTi nor CDi_j matrix found... STEPi set to 1.0FITS file: tfbn4449b1.fits converted to: tfbn4449b1.bdf
(Midas 020> help fil/cosmicFILTER/COSMIC )
Midas 021> daophotRevised version W A R N I N G
This version of DAOPHOT can be used for frames with a maximum size of 4100 * 4100 (= 16810000) pixels. In case your frame is larger than this value, DAOPHOT will not be able to process it. In such case, please contact your local MIDAS support person. READ NOISE (ADU; 1 frame) = 5.00 GAIN (e/ADU; 1 frame) = 10.00 OW GOOD DATUM (in sigmas) = 7.00 HIGH GOOD DATUM (in ADU) = 30000.00 FWHM OF OBJECT = 2.50 THRESHOLD (in sigmas) = 4.00 LS (LOW SHARPNESS CUTOFF) = 0.20 HS (HIGH SHARPNESS CUTOFF) = 1.00 LR (LOW ROUNDNESS CUTOFF) = 1.00 HR (HIGH ROUNDNESS CUTOFF) = 1.00
29
Command over commands Chrisphin Karthick,ARIES20062007
Approximate sky value for this frame = 111.2 Standard deviation of sky brightness = 3.58
Command: exit(0.53=5.3/10 ie...readout noise in ADU.)
Midas 025> fil/cosmic aobject_r1.bdf cobject_r1.bdf 111.2,10,0.53,4,2 (fil/cosmic aobject_r1.bdf cobject_r1.bdf skyvalue,Gain,Readout Noise/Gain,4,2 )Beginning of the median filterwe process frame in 2 chunks ...expanding frame Th, 18 May 2006 14:37:08working on chunk 1 Th, 18 May 2006 14:37:09working on chunk 2 Th, 18 May 2006 14:37:09Beginning of the cosmic rays removal
Midas 026> outdisk/fits cobject_r1.bdf cobject_r1.fitsFITS file cfbn4449b1.fits will have 1 extensionscfbn4449b1.bdf written to FITS file cfbn4449b1.fits( To check whether mistakenly some stars are deleted are not.This mask.fits give only the removedpart...so from that by plotting Intensity profile (pressing 's'from Ds9)we can easily find out)Midas 027> fil/cosmic aobject_r1.bdf cobject_r1.bdf 111.2,10,0.53,4,2 mask.bdfBeginning of the median filterwe process frame in 2 chunks ...expanding frame Th, 18 May 2006 14:38:03
30
Command over commands Chrisphin Karthick,ARIES20062007
working on chunk 1 Th, 18 May 2006 14:38:03working on chunk 2 Th, 18 May 2006 14:38:03Beginning of the cosmic rays removalMidas 028> outdisk/fits mask.bdf mask.fitsFITS file mask.fits will have 1 extensionsmask.bdf written to FITS file mask.fits
Hints:For getting help Midas 020> help fil/cosmic FILTER/COSMIC )
While staring for the next one no need to type again>set/con daophot
Instead directly start from indisk/fits ......................Problem in midas:Midas 016> indisk/fits TAfe34_a2.fits TAfe34_a2.bdfWarning: <COMMENT1> of invalid type not storedWarning: <COMMENTX> of invalid type not storedrotlong = 6.283185, rotlat = 0.000000 axes not orthogonal!FITS file: TAfe34_a2.fits converted to: Tafe34_a2.bdf
Midas 018> help fil/cosmicFILTER/COSMIC 21NOV1991 PM,MR
Purpose: Remove cosmic ray events on a single CCD image and replace them by a local median value.Syntax: FILTER/COSMIC inframe outframe sky,gain,ron,[ns,rc] [mask] inframe = raw input frame outframe = output frame sky,gain,ron,ns,rc = sky level (sky), inverse gain factor (e/ADU) (gain), readoutnoise (in ADU) (ron), threshold for the detection of cosmic rays (ns), and critical ratio for discrimination of objects and cosmic rays (rc). The detection threshold is in units of the theoretical noise sigma of each pixel; it's default value is 4. The default for `rc' is 2.
31
Command over commands Chrisphin Karthick,ARIES20062007
mask = name of an optional frame containing the value 1 for cosmic rays and 0 for all other pixels.
Note: a) The algorithm works as follows: 1. The input image is filtered in the following way: FILTER/MEDIAN inframe middumma 1,1,0.0 NA For LongSlit spectra of extended sources, the algorithm may be
hit return to continue, 'q' + return to quit Midas 018> help fil/cosmicFILTER/COSMIC 21NOV1991 PM,MR
Purpose: Remove cosmic ray events on a single CCD image and replace them by a local median value.Syntax: FILTER/COSMIC inframe outframe sky,gain,ron,[ns,rc] [mask] inframe = raw input frame outframe = output frame sky,gain,ron,ns,rc = sky level (sky), inverse gain factor (e/ADU) (gain), readoutnoise (in ADU) (ron), threshold for the detection of cosmic rays (ns), and critical ratio for discrimination of objects and cosmic rays (rc). The detection threshold is in units of the theoretical noise sigma of each pixel; it's default value is 4. The default for `rc' is 2. mask = name of an optional frame containing the value 1 for cosmic rays and 0 for all other pixels.Note: a) The algorithm works as follows: 1. The input image is filtered in the following way: FILTER/MEDIAN inframe middumma 1,1,0.0 NA For LongSlit spectra of extended sources, the algorithm may be
more efficient if the median filter works only along the slit. 2. The input image is compared with the filtered image. All pixels with an intensity I greater than Im+ns*sigma are suspicious and may be cosmic rays (Im is the filtered intensity of a pixel and sigma is given by: sigma**2 = ron**2+I/gain).
32
Command over commands Chrisphin Karthick,ARIES20062007
3. All suspicious pixels are grouped into sets of contiguous points. In each of these sets, the pixel with the maximum intensity Imax is selected. If (Imaxsky) is greater than rc*(Iaversky), Iaver being an average of the intensities of the first eight neighbours of that pixel, the whole set of points is considered as a cosmic ray event. 4. The intensities of the pixels affected by cosmic rays are replaced by a median value calculated over the nearest neighbours of the group to which they belong. b) In many situations, rc is the most critical parameter and requires careful finetuning. If it is choosen too small, small sources such as stars may be affected. If rc is too large, the filter may not remove weak partical hits superimposed to reasonably well exposed extended sources.See also: FILTER/MEDIANExamples: FILTER/COSMIC ccd ccdclean 150,1,4,4,2.3 cosmask Apply cosmic filtering to image `ccd.bdf' and store result frame
hit return to continue, 'q' + return to quit as `ccdclean.bdf'; save a 0/1 mask in `cosmask.bdf'.Midas 019> FILTER/COSMIC 21NOV1991 PM,MREnter SKY,G,RON,NS,RC:
33
Command over commands Chrisphin Karthick,ARIES20062007
09Cosmic ray reduction through IRAFcc> disp aobject_r1.fitsframe to be written into (1:16) (1): z1=102.8171 z2=133.1152cc> imexam
Then in Ds 9 image select isolated field and press 'm' cc> imexam (sky)# SECTION NPIX MEAN MEDIAN STDDEV MIN MAX [684:688,774:778] 25 109.7 110. 1.995 106.3 113.8 [112:116,382:386] 25 112.7 112.8 2.597 108.5 117.1 [244:248,210:214] 25 111.5 111.6 2.64 106. 116.7 [276:280,114:118] 25 111.7 111.6 1.704 108.7 115.1 [390:394,72:76] 25 110.4 110.5 2.229 104.2 114.3 [768:772,118:122] 25 110.2 110. 2.837 105.4 118.1 [906:910,148:152] 25 110.4 110.4 3.277 104.8 117.3 [960:964,638:642] 25 109.7 109.1 1.615 107.2 112.3 [908:912,866:870] 25 109.5 109.6 2.201 104.4 113.9 [44:48,832:836] 25 112.5 112.8 1.708 109.1 115.2cc> crutil cosmicrays crcombine crfix crmedian craverage credit crgrow crnebula cr> epar cosmicinput = aobject_b1.fits List of images in which to detect cosmic raysoutput = ctobject_b1.fits List of cosmic ray replaced output images (optio(crmasks= ) List of bad pixel masks (optional)
(thresho= 11.) Detection threshold above mean
:goaobject_b1.fits Review parameters for a particular image? (no|yes|NO|YES) (yes): yes
Then the figure will come.
* here the threshold is mean of standard deviation multiply with 5.here it is 2.2*5=11
then the figure will come place the cursor over any particular point and press "s"then the plot will come.
1.if the plot is so sharp (peak) then it must be cosmic ray.
34
Command over commands Chrisphin Karthick,ARIES20062007
1.if it is blended (following gaussian distribution)....then it is a star.
press "s"see the plottingcome back by pressing "s"then delete "d"for undelete “u”then for quit “q”also flux ratio also important.this is nothing but.....the ratio between the cosmic ray flux and sky flux ....normally this value ....
10Apeture Photometry
first make a coordinate file by selecting 10 or 15 stars....here i have selected first 5standardstars..then 3 faint stars..and made a file in the name of ' co ' like that.>epar imexam
(logfile= co) logfile(keeplog= yes) log output results:golog file open(Now select the stars ...it will be in the file named ' co ' )>imexamSA 104MEAN OF MEAN OF FWHM(Direct)STD DEV (for the five standard stars)(for the darken region)(by pressing 'a')(by pressing 'm')r01 3.4 2.6
like that for each frame find out the value through imexam command.and make a note of it .
image = cobject_r1.fits The input image(s)skyfile = The input sky file(s)(coords = co) The input coordinate files(s) (default: image.coo.?)(output = default) The output photometry file(s) (default: image.mag.?)(plotfil= ) The output plots metacode file(datapar= ) Data dependent parameters(centerp= ) Centering parameters(fitskyp= ) Sky fitting parameters(photpar= ) Photometry parameters(interac= no) Interactive mode ?
in the above darken region place the cursor and type :e Then for datapar
da> epar phot
PACKAGE = daophot TASK = datapars
(scale = 1.) Image scale in units per pixel(fwhmpsf= 3.74) FWHM of the PSF in scale units(emissio= yes) Features are positive ?(sigma = 0.0015) Standard deviation of background in countssigma value(datamin= 0.2375) Minimum good data valuesky5*sigma(datamax= 28000.) Maximum good data valueSaturation level ...(noise = poisson) Noise model(ccdread= ) CCD readout noise image header keyword
36
Command over commands Chrisphin Karthick,ARIES20062007
(gain = ) CCD gain image header keyword(readnoi= 5.3) CCD readout noise in electrons(epadu = 10.) Gain in electrons per count(exposur= ) Exposure time image header keyword(airmass= ) Airmass image header keyword(filter = ) Filter image header keyword(obstime= ) Time of observation image header keyword(itime = 1.) Exposure time(xairmas= INDEF) Airmass
:qPACKAGE = daophot TASK = centerpars
(calgori= none) Centering algorithm(cbox = 6.44) Centering box width in scale units2*3.74 ie..2*FWHM(cthresh= 0.) Centering threshold in sigma above background(minsnra= 1.) Minimum signaltonoise ratio for centering algo(cmaxite= 10) Maximum iterations for centering algorithm(maxshif= 1.) Maximum center shift in scale units(clean = no) Symmetry clean before centering(rclean = 1.) Cleaning radius in scale units(rclip = 2.) Clipping radius in scale units(kclean = 3.) Ksigma rejection criterion in skysigma(mkcente= no) Mark the computed center(mode = ql)
:q PACKAGE = daophot TASK = fitskypars
(salgori= mode) Sky fitting algorithmconstantfor knots.default for others.(annulus= 12.88) Inner radius of sky annulus in scale units—4 to 5times FWHM for stars (dannulu= 5) Width of sky annulus in scale units5(interm of pixel i think)for stars(skyvalu= 0.) User sky value(smaxite= 10) Maximum number of sky fitting iterations(sloclip= 0.) Lower clipping factor in percent(shiclip= 0.) Upper clipping factor in percent
37
Command over commands Chrisphin Karthick,ARIES20062007
(snrejec= 50) Maximum number of sky fitting rejection iteratio(sloreje= 3.) Lower Ksigma rejection limit in sky sigma(shireje= 3.) Upper Ksigma rejection limit in sky sigma(khist = 3.) Half width of histogram in sky sigma(binsize= 0.1) Binsize of histogram in sky sigma(smooth = no) Boxcar smooth the histogram(rgrow = 0.) Region growing radius in scale units(mksky = no) Mark sky annuli on the display(mode = ql)
What? choose: |median|mode|centroid|gauss|crosscor|ofilter|histplot|radplot|co ESC? for HELPnstant|file|mean|
then for the knots....it differs...(only for fitskypars)..only this fitskypars nothing else.
PACKAGE = daophot TASK = fitskypars
(salgori= constant) Sky fitting algorithm(annulus= 0.) Inner radius of sky annulus in scale unitsfor knots (dannulu= 0.) Width of sky annulus in scale unitsfor knots(skyvalu= 0.15) User sky value(smaxite= 10) Maximum number of sky fitting iterations(sloclip= 0.) Lower clipping factor in percent(shiclip= 0.) Upper clipping factor in percent(snrejec= 50) Maximum number of sky fitting rejection iterations(sloreje= 3.) Lower Ksigma rejection limit in sky sigma(shireje= 3.) Upper Ksigma rejection limit in sky sigma(khist = 3.) Half width of histogram in sky sigma(binsize= 0.1) Binsize of histogram in sky sigma(smooth = no) Boxcar smooth the histogram(rgrow = 0.) Region growing radius in scale units(mksky = no) Mark sky annuli on the display(mode = ql)
:q
da> disp zs zr z1=.1 z2=1
38
Command over commands Chrisphin Karthick,ARIES20062007
image to be displayed (nca_sr.fits): frame to be written into (1:4) (1): z1=0.1 z2=1.
While doing aperture for knots check from the1.vector plot(wher vector plot shows the total diameter ..but take only the radius)2.from the fluxfluctuationn in the flux....sudden rise and fall on the flux.3.from magnitude error.
PACKAGE = apphot TASK = photpars
(weighti= constant) Photometric weighting scheme for wphot(apertur= 10:20:.5) List of aperture radii in scale units(2FWHM:4FWHM:Interval)(zmag = 25.) Zero point of magnitude scale (start:end:interval)(mkapert= no) Draw apertures on the display(mode = ql)
Darken region explains :10—initial(FWHM)...20final radius(4FWHM)..5interval
:qthen from the main....phot pakage
:go
Centering algorithm (centroid) (CR or value): (just type enter for all ) New centering algorithm: centroidCentering box width in scale units (5.) (CR or value): New centering box width: 5. scale units 5. pixelsSky fitting algorithm (centroid) (CR or value): Sky fitting algorithm: centroidInner radius of sky annulus in scale units (20.) (CR or value): New inner radius of sky annulus: 20. scale units 20. pixelsWidth of the sky annulus in scale units (10.) (CR or value): New width of the sky annulus: 10. scale units 10. pixelsFile/list of aperture radii in scale units (10:20:.5) (CR or value): Aperture radius 1: 10. scale units 10. pixels
Aperture radius 2: 10.5 scale units 10.5 pixels Aperture radius 3: 11. scale units 11. pixels Aperture radius 4: 11.5 scale units 11.5 pixels Aperture radius 5: 12. scale units 12. pixels
39
Command over commands Chrisphin Karthick,ARIES20062007
Aperture radius 6: 12.5 scale units 12.5 pixels Aperture radius 7: 13. scale units 13. pixels Aperture radius 8: 13.5 scale units 13.5 pixels Aperture radius 9: 14. scale units 14. pixels Aperture radius 10: 14.5 scale units 14.5 pixels Aperture radius 11: 15. scale units 15. pixels Aperture radius 12: 15.5 scale units 15.5 pixels Aperture radius 13: 16. scale units 16. pixels Aperture radius 14: 16.5 scale units 16.5 pixels Aperture radius 15: 17. scale units 17. pixels Aperture radius 16: 17.5 scale units 17.5 pixels Aperture radius 17: 18. scale units 18. pixels Aperture radius 18: 18.5 scale units 18.5 pixels Aperture radius 19: 19. scale units 19. pixels Aperture radius 20: 19.5 scale units 19.5 pixels Aperture radius 21: 20. scale units 20. pixelsStandard deviation of background in counts (1.3) (CR or value): New standard deviation of background: 1.3 countsMinimum good data value (INDEF) (CR or value): New minimum good data value: INDEF countsMaximum good data value (28000.) (CR or value): New maximum good data value: 28000. counts
then it has been created one file as cobject_r1.fits.mag.1 by default.open and check it for which aperture it has constant value.and take that aperture value(example:19) put it into the coming ...>!vi cobject_r1.fits.mag.1 csa104b04.fits 351.540 867.290 1 co 1 \ 351.575 867.344 0.035 0.054 0.015 0.019 0 NoError \ 40.63198 1.279863 0.4462133 1562 9 0 NoError \ 1. INDEF INDEF INDEF \ 10.00 21848.62 314.3839 9074.581 15.105 0.012 0 NoError *\ 10.50 23208.14 346.9878 9109.336 15.101 0.012 0 NoError *\ 11.00 24588.55 380.2554 9138.025 15.098 0.012 0 NoError *\ " " 17.50 48452.44 962.6317 9338.808 15.074 0.013 0 NoError *\ 18.00 50711.02 1017.86 9353.36 15.073 0.013 0 NoError *\ 18.50 53070.39 1075.453 9372.596 15.070 0.013 0 NoError *\ 19.00 55497.81 1134.713 9392.172 15.068 0.013 0 NoError *\ 19.50 57950.38 1194.741 9405.702 15.068 0.013 0 NoError *\
here you can see the the difference in 19th aperture onwards (darken region)become constant. itmeans that the star is ending and sky is starting.that is the value we want.Hint:if the output somewhare gives INDEF and BAD PIXELS..then reduce the DATAMIN value ..yet..now giving the output it will be fine. ap> epar phot
40
Command over commands Chrisphin Karthick,ARIES20062007
then place that value in .....photmetry prameters...then execute new file has been created.(weighti= constant) Photometric weighting scheme for wphot(apertur= 19) List of aperture radii in scale units(zmag = 25.) Zero point of magnitude scale(mkapert= no) Draw apertures on the display(mode = ql)
:q:go
After that simply type enter …..enter
Centering algorithm (centroid) (CR or value): New centering algorithm: centroidCentering box width in scale units (5.) (CR or value): New centering box width: 5. scale units 5. pixelsSky fitting algorithm (centroid) (CR or value): Sky fitting algorithm: centroidInner radius of sky annulus in scale units (20.) (CR or value): New inner radius of sky annulus: 20. scale units 20. pixelsWidth of the sky annulus in scale units (10.) (CR or value): New width of the sky annulus: 10. scale units 10. pixelsFile/list of aperture radii in scale units (19) (CR or value): Aperture radius 1: 19. scale units 19. pixelsStandard deviation of background in counts (1.3) (CR or value): New standard deviation of background: 1.3 countsMinimum good data value (INDEF) (CR or value): New minimum good data value: INDEF countsMaximum good data value (28000.) (CR or value): New maximum good data value: 28000. count
new file name as...... cobject_r1.fits.mag.2
Now all the frames with the extension of .mag.2 is last one.collect all the file like this and edit itmake one file like ' mag ' with only needed parameters instead of all.through the command...
ap>epar txdumpPACKAGE = apphot TASK = txdumptextfile= *.mag.2 Input apphot/daophot text database(s)fields = ID,XCENTER,YCENTER,MAG,MERR,IMAGE,RAPERT,FLUX Fields to be extractedexpr = yes Boolean expression for record selection(headers= no) Print the field headers ?
41
Command over commands Chrisphin Karthick,ARIES20062007
(paramet= yes) Print the parameters if headers is yes ?(mode = ql) Mode of task
ap> txdump >magInput apphot/daophot text database(s) (*.mag.2): Fields to be extracted (ID,XCENTER,YCENTER,MAG,MERR,IMAGE,AIRMASS): Boolean expression for record selection (yes): ap> vi mag 1 351.556 867.093 14.467 0.011 csa104r01.fits 1.14342 364.319 688.529 12.815 0.004 csa104r01.fits 1.14343 401.578 604.448 13.608 0.007 csa104r01.fits 1.1434
(then the file is look like above mentioned where the last one is AIRMASShere airmass includedafter that manually)
then it will list out the 2nd stars of all the frames and filter.as shown above.thencosmic > emacs magb2&[1] 10224cosmic > emacs magv2&[2] 10225[1] Done emacs magb2cosmic > emacs magr2&[3] 10226[2] Done emacs magv2
copy and paste the respective files.into this.then plotting the graph through the terminal and get the cofficient
This gnuplot type from the terminal where you wants to workcosmic > gnuplot G N U P L O T Version 4.0 patchlevel 0 last modified Thu Apr 15 14:44:22 CEST 2004 System: Linux 2.6.91.667smp
43
Command over commands Chrisphin Karthick,ARIES20062007
Copyright (C) 1986 1993, 1998, 2004 Thomas Williams, Colin Kelley and many others
This is gnuplot version 4.0. Please refer to the documentation for command syntax changes. The old syntax will be accepted throughout the 4.0 series, but all save files use the new syntax. Type `help` to access the online reference manual. The gnuplot FAQ is available from http://www.gnuplot.info/faq/
Send comments and requests for help to <gnuplot[email protected]> Send bugs, suggestions and mods to <gnuplot[email protected]>Terminal type set to 'x11'After inside the gnuplot if you want to list out the files to see then typegnuplot>!lsgnuplot>plot " magv1" u 5:2 plot”datafile”using coloum no in x:y
then the plotted graph will come.using the data magv1 colum no: 5 in x axis and colum no 2 inyaxis.nothing but in the x axis AIRMASS in yaxis MAGNITUDEFor saving the plotgnuplot>set term post gnuplot>set output “filename.ps”gnuplot>pl “data_filename” gnuplot> y(x)=m*x+cgnuplot> fit y(x) "magv1" u 5:2 via m,cthen in the terminal details will come .Iteration 0WSSR : 835.669 delta(WSSR)/WSSR : 0delta(WSSR) : 0 limit for stopping : 1e05lambda : 1.4634
initial set of free parameter values
m = 1c = 1/
44
Command over commands Chrisphin Karthick,ARIES20062007
After 5 iterations the fit converged.final sum of squares of residuals : 0.00507835rel. change during last iteration : 6.83184e16
degrees of freedom (ndf) : 4rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313variance of residuals (reduced chisquare) = WSSR/ndf : 0.00126959
Final set of parameters Asymptotic Standard Error======================= ==========================
m = 0.361441 +/ 0.03095 (8.563%) (here this is the coefficient)c = 13.9152 +/ 0.05608 (0.403%)
correlation matrix of the fit parameters:
m cm 1.000c 0.966 1.000gnuplot> replot y(x) then it will plot the line over the graph.if the plot is not good ......the percentage of error is too much then put the # mark infront of the stardetails.like...below then you can see the percentage of error will be less now.
46
Command over commands Chrisphin Karthick,ARIES20062007
*******************************************************************************Fri Aug 4 15:50:26 2006FIT: data read from "magv1" u 5:2 #datapoints = 6 residuals are weighted equally (unit weight)
function used for fitting: y(x)fitted parameters initialized with current variable values
m = 0.26786c = 14.1777 190,01 After 4 iterations the fit converged.final sum of squares of residuals : 0.00507835rel. change during last iteration : 6.80346e09
degrees of freedom (ndf) : 4rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313variance of residuals (reduced chisquare) = WSSR/ndf : 0.00126959
Final set of parameters Asymptotic Standard Error======================= ==========================
Command over commands Chrisphin Karthick,ARIES20062007
m 1.000c 0.966 1.000Also it will create an log file to save this information.onitself as fit.log file.awk '{print($50.36*$7)}' obsmag
11 Spectroscopy reduction Hints:1.First do everything with the specred....means u cant do apall with onedspec command.....so enter in tospecred then to onedspec.2.you cant do everything with specred .because ,while calibrating u have to mention the place (filenamewhere it is located ..like onestds$spec50cal )it is available only in the onedspec so onedspec isimportant....unless we are keeping the file in our own place)
For deleting the .imh file >imdel <filename.imh>
Requirements:1.object167 l2.Standard two(Oke 1990)1340 l3.comparision(FeAr)4.flat (Halogen lamp)5.bias*Grism with respct to wavelength coverage.
Part1.basic Steps changing the name into .fits file.>pc120001 >epar renamefiles = pc* list of files to be renamednewname = fits new file name or field name(field = extn) field to be modified (all|ldir|root|extn)(mode = ql):go>imhead pc120047.fitspc120047.fits[500,3500][ushort]: NGC 4216cc> emv pc120047.fits n42162.fitscl> noao artdata. digiphot. nobsolete. onedspec. astcat. focas. nproto. rv.
48
Command over commands Chrisphin Karthick,ARIES20062007
PACKAGE = immatch TASK = imcombine (the changable parameters are): input = bias*.fits List of images to combineoutput = mbias.fits List of output images(combine= median) Type of combine operation
49
Command over commands Chrisphin Karthick,ARIES20062007
Command over commands Chrisphin Karthick,ARIES20062007
(then take mean of mean)....here ..the mean is 8233sp>imarith bhal1fits / 8233 nbhal1.fits (like that do for all)sp> epar imcombine
PACKAGE = immatch TASK = imcombine input = nbhal*.fits List of images to combineoutput = fnbhal.fits List of output images(combine= median) Type of combine operation(reject = avsigclip) Type of rejection:goJun 14 11:28: IMCOMBINE combine = median, scale = none, zero = none, weight = none reject = avsigclip, mclip = yes, nkeep = 1 lsigma = 3., hsigma = 3. blank = 0. Images nbhal1.fits nbhal2.fits nbhal3.fits nbhal4.fits nbhal5.fits
Output image = fnbhal.fits, ncombine = 5sp> epar responsecalibrat= fnbhal.fits Longslit calibration imagesnormaliz= fnbhal.fits Normalization spectrum imagesresponse= rfnbhal.fits Response function images(functio= spline3) Fitting function(order = 3) Order of fitting function:goFit the normalization spectrum for fnbhal.fits interactively (yes):nosp>imarith bm1061.fits / rfnbhal.fits fbm1061.fitssp>onedspec
51
Command over commands Chrisphin Karthick,ARIES20062007
Part2.Wavelength Calibartionsp>epar apall
(better do not give the output name...it will take automatically with extension of .ms.imh)
# EXTRACTION PARAMETERS
(backgro= median) Background to subtractearlier it was fit but for median works fine.(skybox = 1) Box car smoothing length for sky(weights= variance) Extraction weights (none|variance)(pfit = fit2d) Profile fitting type (fit1d|fit2d)(clean = yes) Detect and replace bad pixels?(saturat= 63000.) Saturation level(readnoi= 4.87) Read out noise sigma (photons)(gain = 1.22) Photon gain (photons/data number)(lsigma = 4.) Lower rejection threshold(usigma = 4.) Upper rejection threshold(nsubaps= 1) Number of subapertures per aperture(mode = ql)mbias.fits
:go Recenter apertures for fbm1061? (yes): Resize apertures for fbm1061? (yes): Edit apertures for fbm1061? (yes): (then the graph will appear)
then set the aperture giving lower and upper limit .By pressing "l" lower limit.By pressing "u" upper limit.
Then for background subtraction....press "b"Then "f ":sample 25:20,20:25 (or).......in wavelengh calibartion for sky substraction just to mark the limits...instead of typing :sample.....type simly by the keys..thatusing the s & t where s—for marking level..
52
Command over commands Chrisphin Karthick,ARIES20062007
where t –for unmarking..Then..." f "change the order to 3 by:order 3(now RMS value will be reduced)" q "yes,yes,yes,...
Then the fitted curve will appear...delete the points (by "d")which is apart from the line.and try toreduce reduce the RMS value.Then for quit.." q "write the apertures to database:yes,yes,...Then the spectrum of object will be shown.( for a group of images also we can do at one time...one by one...in the input list of images by giving*.fits)
Do this apall for the standard star also...
on>splot nobject.fitson>splot nobject_spec.imhon>apall fear1 out=fear_spec refer=nobject.fits recen trac back interac(so now fear_spec.imh file has been created)(here also by group we can create spectra by giving *.fits).
sp>epar identifyimages = fear_spec Images containing features to be identified(section= middle line) Section to apply to two dimensional images(databas= database) Database in which to record feature data(coordli= /home/chrisphin/bin/fear.dat) User coordinate list(functio= legendre) Coordinate function:go(then the graph of comparision fear will open)Then using *commands and comparing the paper ....plot the wavelength on it.minimum should be 12.
*Note:to extend on x axis shift+x
53
Command over commands Chrisphin Karthick,ARIES20062007
To extend on Y axisshift+yfo markingmto come back and do againrfjfqThen the fitted curve will appear...delete the points (by "d")which is apart fromthe line.and try to reduce reduce the RMS value.ljf (here f=j ..so use f itself)q(ffitting, jrisidual plot,l=longitudinal plot, lit will plot remaining wavelengths on its own)(" i " will delete the all lines which is marked already)then in xgterm....writing the data structures in database?yes
This identification only one time is enough which can be used for all.Just hedit and add to all this asreference.
sp> epar dispcorinput = nobject1_spec.imh List of input spectraoutput = wobject1_spec.imh List of output spectra(lineari= yes) Linearize (interpolate) spectra?(databas= database) Dispersion solution database(ignorea= yes) Ignore apertures?(incase if u have selected different apertures)
:go
TTFbn1569_3.ms.imh: REFSPEC1 = 'TFbcp_2.ms.imh 1.'Dn1569_3.ms.imh: ap = 1, w1 = 2524.67, w2 = 7955.183, dw = 1.552019, nw = 3500After dispersion correction make it all subexposures as one using the command “ sarith “ one by one
For atmospheric line correction s type: better to do this after flux calibration (in case if we are interested in flux calibration also.)First identify the differnce between actual to the observed atmospheric lines then using
>epar specshiftPACKAGE = specred
54
Command over commands Chrisphin Karthick,ARIES20062007
TASK = specshift
spectra = List of spectrashift = 0. Shift to add to dispersion coordinates(apertur= ) List of apertures to shift(verbose= no) Print verbose information?(mode = ql)
For doppler corection:>epar dop
PACKAGE = specred TASK = dopcor
input = List of input spectraoutput = List of output spectraredshift= Redshift or velocity (Km/s)(isveloc= no) Is the redshift parameter a velocity?(add = no) Add to previous dispersion correction?(dispers= yes) Apply dispersion correction?(flux = no) Apply flux correction?(factor = 3.) Flux correction factor (power of 1+z)(apertur= ) List of apertures to correct(verbose= no) Print corrections performed?(mode = ql):go
Part3.Flux Calibiration
Before starting the Flux calibartaion....set airmass and set the observatory parameters.
sp> epar standard
Here the input is dispersion corrected standard star.{ in this... the symbol )_.observatory meant that it will take the information from main}
PACKAGE = onedspec TASK = standard
55
Command over commands Chrisphin Karthick,ARIES20062007
input = Dstd_2.ms.imh Input image file root nameoutput = std Output flux file (used by SENSFUNC)(samesta= yes) Same star in all apertures?(beam_sw= no) Beam switch spectra?(apertur= ) Aperture selection list(bandwid= INDEF) Bandpass widths(bandsep= INDEF) Bandpass separation(fnuzero= 3.6800000000000E20) Absolute flux zero point(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file(caldir = onedstds$/spec50cal/) Directory containing calibration data(observa= )_.observatory) Observatory for data(interac= yes) Graphic interaction to define new bandpasses(graphic= stdgraph) Graphics output device(cursor = ) Graphics cursor inputstar_nam= feige34 Star name in calibration listairmass = Airmassexptime = Exposure time (seconds)mag = Magnitude of starmagband = Magnitude typeteff = Effective temperature or spectral typeanswer = no (no|yes|NO|YES|NO!|YES!)(mode = ql)
:go
Dstd_2.ms.imh[*,1,1](1): Star name in calibration list (g191b2b): Dstd_2.ms.imh[1]: Edit bandpasses? (no|yes|NO|YES|NO!|YES!) (no):
Now you can see the file std has been created with the details of [Dstd_2.ms.imh] 1 3401 600.00 3.602 349.000 3749.000 G19B2B 3200.00 4.6598E13 50.000 3417. 3250.00 4.3944E13 50.000 2187.5 3300.00 4.4222E13 50.000 1189.7 3350.00 4.2912E13 50.000 885.67 3400.00 4.0899E13 50.000 786.2 3450.00 3.8639E13 50.000 778.63 3500.00 3.6185E13 50.000 993.41 3550.00 3.5173E13 50.000 512.38
56
Command over commands Chrisphin Karthick,ARIES20062007
hint:Even after sploting ...if the graph doesnt come press “a” two times.
Then the scale will change to bring the picture.
By typing the below you can get the location where the respective standard star location is...
for getting standard ....observatory is needed also airmass also location of the caldirectory withinIRAF has to be specified..needed..hence for setting these...follow the below...
sp> help onedstd
Standard stars in onedstds$spec50cal/ (3200A 10200A)
standard= std Input standard star data file (from STANDARD)sensitiv= sens Output root sensitivity function imagename(apertur= ) Aperture selection list(ignorea= yes) Ignore apertures and make one sensitivity function?(logfile= logfile) Output log for statistics information(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file(newexti= extinct.dat) Output revised extinction file
57
Command over commands Chrisphin Karthick,ARIES20062007
(observa= )_.observatory) Observatory of data(functio= spline3) Fitting function(order = 6) Order of fit(interac= yes) Determine sensitivity function interactively?(graphs = sr) Graphs per frame(marks = plus cross box) Data mark types (marks deleted added)(colors = 2 1 3 4) Colors (lines marks deleted added)(cursor = ) Graphics cursor input(device = stdgraph) Graphics output deviceanswer = yes (no|yes|NO|YES)(mode = ql):go
Fit aperture 1 interactively? (no|yes|NO|YES) (no|yes|NO|YES) (yes):
Then the graph will open.
Change the order to 9.:ord 9then “ r “ replot“ d “delete the deviated points in the below figure.“ f “ fit “ r “ replotNow you can see RMS value has been reduced.After finishing “ q “quit
Command over commands Chrisphin Karthick,ARIES20062007
(ignorea= yes) Ignore aperture numbers in flux calibration?(sensiti= sens) Image root name for sensitivity spectra(fnu = no) Create spectra having units of FNU?airmass = Airmassexptime = Exposure time (seconds)(mode = ql)
:go
Fn1569_1.ms.imh: NGC1569 Cn1569_1.imh: NGC1569 Extinction correction applied Flux calibration appliedThe above warning because of trimmming may be..
Then sploting the final wavelength and flux calibrated spectrum will appear.
Some more hints on spectroscopy reduction:
1.Removing unwanted lined by the bad pixel:After splotting find out the line ...and place the cursor then press the “ x “ on both the end of the raythen press “ r “ ...then it will be removed.2.EQW:For finding the equalent width press “ e “ on both the ends.3. “ f “ for finding the apertureswhere “ d” for delete the apeture....so if any cosmic ray prsent and aperture goes for that ...then pres ffor finding apeture then dlete the another unwanted aperture.
while doing apall if 2 or 3 features wanted to extract at one time then use shift + it will take to anotherpeak...then extract..4.While epar identification better to use spline 3....and always order 3 is nice. “ j “ fo residual plot.After getting spectrum...There are 4 atmospheric lines....2 are in absorbtion...whar e the 7605 is visible clearly.....then 6870..then in epar splot select the band number as 2.then splotting you will get again 2 lines.6300,6364.
59
Command over commands Chrisphin Karthick,ARIES20062007
in the splot graphby typing k,k two times u can get the value of fwhm....and others.
for saving the graph:.snap epsflTo get the list of help commands press ? from graphical window.then it will give the list in xgterm window like .................
1. INTERACTIVE CURVE FITTING CURSOR OPTIONS
? Print optionsa Add point to constrain fitc Print the coordinates and fit of point nearest the cursord Delete data point nearest the cursorf Fit the data and redraw or overplotg Redefine graph keys. Any of the following data types may be along either axis. x Independent variable y Dependent variable f Fitted value r Residual (y f) d Ratio (y / f) n Nonlinear part of yhl Graph keys. Defaults are h=(x,y), i=(y,x), j=(x,r), k=(x,d), l=(x,n)o Overplot the next graphq Exit the interactive curve fitting. Carriage return will also exit.r Redraw graphs Set sample range with the cursort Initialize the sample range to all pointsv Change the weight of the point nearest the cursoru Undelete the deleted point nearest the cursorw Set the graph window. For help type 'w' followed by '?'.x Change the x value of the point nearest the cursory Change the y value of the point nearest the cursorz Delete sample region nearest cursorI Interrupt task immediately
2. INTERACTIVE CURVE FITTING COLON COMMANDS
The parameters are listed or set with the following commands which may beabbreviated. To list the value of a parameter type the command alone.
60
Command over commands Chrisphin Karthick,ARIES20062007
:show [file] Show the values of all the parameters:vshow [file] Show the values of all the parameters verbosely:xyshow [file] Show the x, y, y fit, and weight data values:evaluate <value> Print the fit at the specified value:errors [file] Print the errors of the fit (default STDOUT):function [value] Fitting function (chebyshev, legendre, spline3, spline1):grow [value] Rejection growing radius:naverage [value] Sample averaging or medianing window:order [value] Fitting function order:low_reject [value] Low rejection threshold:high_reject [value] High rejection threshold:niterate [value] Number of rejection iterations:sample [value] Sample ranges:markrej [value] Mark rejected points?
Additional commands are available for setting graph formats and manipulatingthe graphics. Use the following commands for help.
:/help Print help for graph formatting option:.help Print help for general graphics options
3. INTERACTIVE CURVE FITTING GRAPH KEYS
The graph keys are h, i, j, k, and l. The graph keys may be redefined toput any combination of axes types along either graph axis with the 'g' key.To define a graph key select the desired key to redefine and then specifythe axes types for the horizontal and vertical axes by a pair of commaseparated types from the following:
d Ratio (y / f)f Fitted valuesr Residuals of fit (y f)n Nonlinear part of data (linear component of fit subtracted)x Indepedent variabley Dependent variable (data being fit)
? This display r Redraw the current window/ Cycle thru short help on stat line s Smooth (boxcar)a Autoexpand between cursors t Fit continuum(*)
61
Command over commands Chrisphin Karthick,ARIES20062007
b Toggle base plot level to 0.0 u Adjust coordinate scale(*)c Clear and redraw full spectrum v Velocity scale (toggle)d Deblend lines using profile models w Window the graphe Equiv. width, integ flux, center x Connects 2 cursor positionsf Arithmetic functions: log, sqrt... y Plot std star flux from calib fileg Get new image and plot z Expand x range by factor of 2h Equivalent widths(*) ) Go to next spectrum in imagei Write current image as new image ( Go to previous spectrum in imagej Fudge a point to Ycursor value # Select new line/aperturek Profile fit to single line(*) % Select new bandl Convert to Flambda $ Toggle wavelength/pixel scalem Mean, RMS, snr in marked region Subtract deblended fitn Convert to Fnu , Down slide spectrumo Toggle overplot of following plot . Up slide spectrump Convert to wavelength scale I Interrupt task immediatelyq Quit and exit <space> Cursor position and flux
(*) For 'h' key: Measure equivalent widths a Left side for width at 1/2 flux l Left side for continuum = 1 b Right side for width at 1/2 flux r Right side for continuum = 1 c Both sides for width at 1/2 flux k Both sides for continuum = 1
(*) For 'k' key: Second key may be used to select profile type g Gaussian, l Lorentzian, v Voigt, all others Gaussiank
(*) For 't' key: Fit the continuum with ICFIT and apply to spectrum / = normalize by the continuum fit = subtract the continuum fit (residuals) f = replace spectrum by the continuum fit c = clean spectrum of rejected points n = do the fitting but leave the spectrum unchanged q = quit without fitting or modifying spectrum
(*) For 'u' key: Adjust the coordinate scale by marking features d = apply doppler correction to bring marked feature to specified coord. l = set linear (in wavelength) coordinates based on two marked features z = apply zero point shift to bring marked feature to specified coordinate
The colon commands do not allow abbreviations.
:# <comment> Add comment to log file
62
Command over commands Chrisphin Karthick,ARIES20062007
:dispaxis <val> Change summing parameter for 2D images:log Enable logging to save_file:nolog Disable logging to save_file :nsum <val> Change summing parameter for 2D images:show Show full output of deblending and equiv. width measurments:units <value> Change coordinate units (see below)
:label <label> <format> Add label at cursor position:mabove <label> <format> Add tick mark and label above spectrum:mbelow <label> <format> Add tick mark and label below spectrum The label must be quoted if it contains blanks. A label beginning with % (i.e. %.2f) is treated as a format for the x cursor position. The optional format is a gtext string (see help on "cursors"). The labels are not remembered between redraws.
:auto [yes|no] Enable/disable autodraw option:zero [yes|no] Enable/disable zero baseline option:xydraw [yes|no] Enable/disable xydraw option:hist [yes|no] Enable/disable histogram line type option:nosysid [yes|no] Enable/disable system ID option:wreset [yes|no] Enable/disable window reset for new spectra option:flip [yes|no] Enable/disable dispersion coordinate flip:overplot [yes|no] Enable/disable permanent overplot mode
:/help Get help on GTOOLS options:.help Get help on cursor mode options
63
Command over commands Chrisphin Karthick,ARIES20062007
12.LATEX Introduction While doing latex to ps do it one folder so the all sub created file will be within the folder itself. >vi hct_obsp_new.tex> latex hct_obsp_new.texThis is TeX, Version 3.14159 (Web2C 7.4.5) Output written on hct_obsp_new.dvi (5 pages, 10872 bytes).Transcript written on hct_obsp_new.log.[chrisphin@aries25 ~/hct_form]$ dvips o hct_obsp_new.ps hct_obsp_new.dviThis is dvips(k) 5.92b Copyright 2002 Radical Eye Software (www.radicaleye.com)' TeX output 2006.11.01:1541' > hct_obsp_new.ps
for a short cut.......you can open a vi editer and put all the commands which has to be executed andthen execute that file which will do all the work by one stroke.>vi llatex hct_obsp_new.texdvips o hct_obsp_new.ps hct_obsp_new.dvigv hct_obsp_new.ps:wq>chmod 777 l>./l
General format example:\documentstyle[a4,12pt,psfig]{article}\textheight 18.0cm\textwidth 16.0cm\topmargin 1.0cm\begin{document}\begin{center}{\Large \bf Photometric and Spectrophotometric studies on WolfRayet Galaxies }\\\vspace{1.0cm}\bf Chrisphin.K, B.B.Sanwal,D.K.sahu, M.Singh\\\small \bf Aryabhatta Research Institute ofObservational Sciences(ARIES)\\Manora Peak,Nainital. \\
64
Command over commands Chrisphin Karthick,ARIES20062007
\end{abstract}\end{document}Latex.....commmand.....\item ...........for point..s 1,2,3....like that.if infront of the letter if we put % symbol then it wont come.\sectionfor subsection\section*then it wont put any number...like 2.1,2.2,...like that.
Some commmands quite often used by astronomers in Latex:
HeII 4686$ \AA $He II 4686 A° 2k$\times$2k2K x 2KH$\alpha$ \& H$\alpha$ H
In escape mode...5dddeleting 5lines.like that any number of lines..uundo5yy5 lines copyingppaste.for cutting use the same command for deletingddredoctrl+r
above all is in escape mode.Type <return> to proceed, S to scroll future error messages,R to run without stopping, Q to run quietly,I to insert something,H for help, X to quit.? X\begin{tabular}{|p{.35in}|p{.9in}|p{1.1in}|p{1.1in}|p{0.6in}|p{0.5in}|p{0.3in}|}\hlineSl.No.&Objects Name& RA (hh mm ss) at J2000.0. & Dec (dd mm ss) at J2000.0.& $V$/int.$V$ mag & Filter & Min. S/N\\
65
Command over commands Chrisphin Karthick,ARIES20062007
\newpage\vskip 2cmif you want to jump to 30 th line in vi editor..then type:30and all the commnad s is possible to execute from..the same terminal..by typing..:!latex <filename>:!dvips o filename.ps filename.dvi
\usepackage{graphicx}\begin{document}\label{firstpage}\begin{figure}\vbox{\includegraphics[height=12cm,width=12cm,angle=90]{/home/chrisphin/spectrum/final_figure/2_n1569.ps}\includegraphics[height=12cm,width=12cm,angle=90]{/home/chrisphin/spectrum/final_figure/2_m33.ps}}\caption{Nuclear Spectrum of NGC 1569 and NGC Mrk 33 respectively}\end{figure}
angle if needed only.
66
Command over commands Chrisphin Karthick,ARIES20062007
13.Ellipse Fittingchrisphin > cl NOAO PCIRAF Revision 2.12.2EXPORT Sun Jan 25 16:09:03 MST 2004 This is the EXPORT version of PCIRAF V2.12 supporting most PC systems.
Welcome to IRAF. To list the available commands, type ? or ??. To get detailed information about a command, type `help command'. To run a command or load a package, type its name. Type `bye' to exit a package, or `logout' to get out of the CL. Type `news' to find out what is new in the version of the system you are using. The following commands or packages are currently defined:
++ | Space Telescope Science Data Analysis System | | STSDAS Version 3.3, November 11, 2004 | | | | Space Telescope Science Institute, Baltimore, Maryland | | Copyright (C) 2003 Association of Universities for | | Research in Astronomy, Inc.(AURA) | | See stsdas$copyright.stsdas for terms of use. | | For help, send email to [email protected] | | | ++ analysis. describe fitsio. hst_calib. problems toolbox. contrib. examples graphics. playpen. sobsolete. st> an dither. fourier. isophote. restore. fitting. gasp. nebular. statistics. an> is bmodel geompar@ isomap magpar@ controlpar@ isoexam isopall samplepar@ ellipse isoimap isoplot
67
Command over commands Chrisphin Karthick,ARIES20062007
is> epar ellipsePACKAGE = isophote TASK = ellipse
input = n4449B.fits input image name cleaned galaxy imageoutput = b output table name(dqf = .c1h) data quality file name or extension (inellip= ) table with input ellipses for nofit mode(geompar= ) geometric parameters (pset)(control= ) algorithm control parameters (pset)(samplep= ) sampling control parameters (pset)(magpar = ) magnitude scale parameters (pset)(interac= no) interactive ?(device = red) graphics output device(icomman= ) image cursor(gcomman= ) graphics cursor(masksz = 5) pixel square mask size (`m' cursor key)(region = no) region masking mode ?(memory = yes) memoryintensive (versus diskintensive) ?(verbose= yes) list summary at STDOUT ?(mode = al) (bring the cursor in geompar and press :e then this will come fill the respective.normally the geompar and control is the important.)
PACKAGE = isophote TASK = geompar
(x0 = INDEF) initial isophote center X(y0 = INDEF) initial isophote center Y(ellip0 = 0.2) initial ellipticity(pa0 = 20.) initial position angle (degrees)(sma0 = 10.) initial semimajor axis lenght(minsma = 0.) minimum semimajor axis lenght(maxsma = INDEF) maximum semimajor axis lenght(step = 0.1) sma step between successive ellipses(linear = no) linear sma step ?
68
Command over commands Chrisphin Karthick,ARIES20062007
(maxrit = INDEF) maximum sma lenght for iterative mode(recente= yes) allows finding routine to recenter x0y0 ?(xylearn= yes) updates pset with new x0y0 ?(physica= yes) physical coordinate system ?(mode = al)
:qthen press :e by placing the cursor on control Image Reduction and Analysis FacilityPACKAGE = isophote TASK = controlpar
(conver = 0.05) convergency criterion (maximum harmonic amplitud(minit = 10) minimun no. of iterations at each sma(maxit = 50) maximun no. of iterations at each sma(hcenter= no) hold center fixed ?(hellip = no) hold ellipticity fixed ?(hpa = no) hold position angle fixed ?(wander = INDEF) maximum wander in successive isophote centers(maxgerr= 0.5) maximum acceptable gradient relative error(olthres= 1.) object locator's ksigma threshold(soft = no) soft stop ?(mode = al)
:q
PACKAGE = isophote TASK = samplepar
(integrm= bilinear) area integration mode(usclip = 3.) sigmaclip criterion for upper deviant points(lsclip = 3.) sigmaclip criterion for lower deviant points(nclip = 0) number of sigmaclip iterations(fflag = 0.5) acceptable fraction of flagged data points (sdevice= none) graphics device for ploting intensity samples(tsample= none) tables with intensity samples(absangl= yes) sample angles refer to image coord. system ? (harmoni= none) optional harmonic numbers to fit(mode = al)
69
Command over commands Chrisphin Karthick,ARIES20062007
:q
PACKAGE = isophote TASK = magpar
(mag0 = 0.) magnitude of reference source(refer = 1.) intensity of reference source (zerolev= 0.) intensity of zero (bias) level (mode = al):qthen:goRunning object locator... Done.Can not find object. Please, enter initialguess for starting isophote center:X0: 485Y0: 545#
Command over commands Chrisphin Karthick,ARIES20062007
(fulltab= yes) use full range of `SMA' from table ?(minsma = 1.) minimum semimajor axis(maxsma = 1.) maximum semimajor axis(nlevels= 3) number of levels(color = r) overlay color(frame = 1) image display frame(mode = al):qis> epar isomap
PACKAGE = isophote TASK = isomap
image = n4449B.fits input imagetable = b.tab input tablefloor = minimum contouring levelceiling = maximum contouring level(nlevels= 3) number of levels(device = stdgraph) graphics device(mode = al):q
>epar isoplot
PACKAGE = isophote TASK = isoplot
input = b.tab input tablexaxis = RSMA x axisyaxis = MAG y axis(device = stdgraph) output graphics device(mode = al)
:go(will give the plot for mag vs SMA *1/4)
>epar isopallinput = b.tab input tablexaxis = RSMA x axis
72
Command over commands Chrisphin Karthick,ARIES20062007
Command over commands Chrisphin Karthick,ARIES20062007
tar zxf /iraf/redhat.package/stsdas33.tar.gzcd /iraf/extern/stsdas/bin.redhattar zxf /iraf/redhat.package/stsdas33.bin.rh.tar.gzcd /iraf/extern/tablestar zxf /iraf/redhat.package/tables33.tar.gzcd /iraf/extern/tables/bin.redhattar zxf /iraf/redhat.package/tables33.bin.rh.tar.gzecho 'installing the x11' cd /iraf/x11iraf./installecho 'installing the iraf' cd /iraf/iraf/unix/hlib./installcd /irafecho 'please check the /iraf/iraf/unix/hlib/extern.pkg'
Of course then move the downloaded Xgterm.fedora &ds9 to the /usr/local/bin.
[chrisphin@aries25 ~]$ mkiraf creating a new uparm directoryTerminal types: xgterm,xterm,gterm,vt640,vt100,etc.Enter terminal type: xgtermA new LOGIN.CL file has been created in the current directory.You may wish to review and edit this file to change the defaults.and then for externing the package of stsdas go to >cd /iraf/iraf/unix/hlib>vi extern.pkg
edit the earlier commands like shown below...# External (non coresystem) packages. To install a new package, add the
# two statements to define the package root directory and package task,# then add the package helpdb to the `helpdb' list.
The local commands directory is the place where the commands such as 'xgterm' and 'ximtool' will be installed. This should be a directory in a common search path such as /usr/local/bin.
Local commands directory (/usr/local/bin):
Installing new binaries in /usr/local/bin ...[ OK ]
Man pages are available for each of the X11IRAF tasks, some tasks will also provide online documentation. Manual pages may be installed either in the main system directory or in a local directory as long as that is accessible through a MANPATH environment variable.
Local man page directory (/usr/share/man/man1):[ OK ]
The appdefaults directory contains the default X resources for the XGterm task. This is not required for the program to work but provides for more readable menu entries, fonts, etc. The directory is normally part of the X11 tree but may be any directory specified in an XFILESEARCHPATH environment variable.
81
Command over commands Chrisphin Karthick,ARIES20062007
System appdefaults directory (/usr/lib/X11/appdefaults):...[ OK ]
The CDL is an interface for C/Fortran programs to display images to XImtool and compatible display servers. This library is not required in the runtime system for XImtool but can be useful for developing local applications needing a display capability. The local lib directory is the place where the CDL library file will be installed, the local include directory is where the needed nclude files for the library will be installed.
Would you like to install this library? (yes):Local lib directory (/usr/local/lib):
Installing CDL libraries in /usr/local/lib ...[ OK ]
Local include directory (/usr/local/include):
Installing include files in /usr/local/include ...[ OK ]
Installation complete.
installing the iraf
IRAF V2.12.1 System Installation ================================
Welcome to the IRAF installation script. This script will first prompt you for several needed path names. The system will be verified for proper structure before the actual install begins, all error must must be corrected before you will be allowed to continue. Recommend ations for fixing problems will be made but no corrective action will be taken directly. Once properly installed, you will be allowed to do some minimal configuration.
82
Command over commands Chrisphin Karthick,ARIES20062007
For each prompt: hit <CR> to accept the default value, 'q' to quit, or 'help' or '?' to print an explanation of the prompt.
============================================================================================= Query for System Settings ==============================================================================================
============================================================================================= Verifying System Settings ==============================================================================================
Hostname = aries25.upso.ernet.i OS version = Linux 2.6.91.667smpArchitecture = redhat HSI arch = redhatNew iraf root = /iraf/iraf Old iraf root = /iraf/irafNew imdir = /iraf/imdirs Old imdir = /d0/imdirsLocal bin dir = /usr/local/bin
Checking definition of iraf root directory ... [ OK ]Checking iraf root and imdir directory ... [ OK ]Checking iraf directory write permissions ... [ OK ]Checking for iraf user account ... [ WARN ]
*** No 'iraf' user was found in the /etc/passwd file. The iraf *** user should be created before installing the system to ensure *** all files are owned by the iraf user, and the have the proper *** environment defined for installation and maintanence.
Checking file ownerships ... [ WARN ]
*** (root dir owned by 312, iraf files owned by 312)
83
Command over commands Chrisphin Karthick,ARIES20062007
*** The iraf tree should be owned by the iraf user so it can *** be updated and maintained properly. *** *** To fix this, login as root, set the iraf environment, and *** issue the commands: *** *** cd /iraf *** chown R iraf . # change dir owner *** cd $hbin # go to HSI bin dir *** chown 0 alloc.e # fix alloc.e ownership *** chmod 4755 alloc.e # fix permissions
Checking file permissions ... [ OK ]Checking proper iraf tree structure in /iraf ... Checking for 'iraf' subdir ... [ OK ] Checking for 'irafbin' subdir ... [ OK ] Checking for 'irafbin/bin.redhat' subdir ... [ OK ] Checking for 'irafbin/noao.bin.redhat' subdir ... [ OK ]Checking Core system binary directory ... [ OK ]Checking NOAO package binary directory ... [ OK ]Checking that local bin directory exists ... [ OK ]Checking for existing commands directory... [ OK ]
Proceed with installation? (yes):================================================================================================= Begin Installation =================================================================================================
Editing Paths Editing the iraf user .login/.cshrc paths ... [ OK ]Editing iraf/imdir paths into system files ... [ OK ]
Checking File Permissions Checking iraf file permissions ... [ OK ]Creating root imdir at /iraf/imdirs ... [ OK ]Reset /tmp sticky bit setting ... [ OK ]
84
Command over commands Chrisphin Karthick,ARIES20062007
Setting tape device permissions ... [ OK ]Checking alloc.e permissions ... [ OK ]
Creating File Links Checking for /iraf symlink ... [ OK ]Checking /usr/include directory ... [ OK ]Creating <iraf.h> symlink ... [ OK ]Creating iraf command links in local bin dir ... [ OK ]Marking system update time hlib$utime ... [ OK ]
Creating Graphics Device Files Creating /dev/imt1 fifo pipes for image display ... [ OK ]Creating /dev/imt fifo pipes link ... [ OK ]Checking /usr/local/lib directory ... [ OK ]Creating /usr/local/lib/imtoolrc link ... [ OK ]Checking if termcap file contains an XGterm entry ... [ OK ]Checking graphcap file for XGterm/imtool entries ... [ OK ]
The system should be fully functional at this point however somepostinstall configuration may be required to make use of all thefeatures such as networking or tape access. Additional software suchas external packages or display servers will need to be installedseparately. Some minimal configuration can be accomplished now butyou should consult the IRAF Site Manager's Guide for a more completediscussion of IRAF system management, configuration of printers, etc.
Proceed to postinstall configuration stage? (yes): IRAF Networking Config
IRAF Networking can be used to access a remote image, tape device,
85
Command over commands Chrisphin Karthick,ARIES20062007
display server, or other network service. It's configuration is nota requirement for normal IRAF operations and it can be updated at anytime by editing the IRAF dev$hosts file with new entries.
In this stage we will add an entry for the current platform to thehosts file. In a local network installation this script should be runon each system to add a networking entry as well as to install othersystem files needed by IRAF.
Configure IRAF Networking on this machine? (yes):Recommended dev$hosts file entry used for this machine:
Creating backup of default dev$hosts file...Initializing dev$hosts file ...Host 'aries25.upso.ernet.in' has been added to the network configuration file...Checking that iraf networking is properly enabled ... [ OK ]
By default IRAF will search for a dev$tapecap.<node> file (where<node> is the system name) when looking for a tape configuration file.Platforms such as PCIRAF and Sun/IRAF support multiple OS versionsand so the proper template file must be used. This configuration willallow you to setup a default tapecap for this system, it may be skippedif this machine has no tape drive attached.
Create a default tapecap file? (yes):Creating default file 'tapecap.aries25.upso.ern' from tapecap.linux...
In the event a dev$tapecap.<node> file is not found on thissystem IRAF will fallback to use just dev$tapecap. In cases wherethe node name changes, this installation is shared with another
86
Command over commands Chrisphin Karthick,ARIES20062007
machine or in a local network, or any case where a tapecap.<node>is not found, the dev$tapecap file will be the default tapecap usedfor all IRAF systems.
Do you wish to create a default dev$tapecap link? (yes):Tapecap symlink 'tapecap' exists and is ok.
The contents of these directories may be safely deleted to reclaimabout 18 Mb of disk space without affecting the IRAF runtime system.
Do you wish to delete these unused HSI binaries? (yes):Delete HSI binaries in bin.freebsd ... [ OK ]Delete HSI binaries in bin.linux ... [ OK ]Delete HSI binaries in bin.linuxppc ... [ OK ]Delete HSI binaries in bin.macosx ... [ OK ]Delete HSI binaries in bin.sunos ... [ OK ]Delete HSI binaries in bin.suse ... [ OK ]
Strip IRAF System Sources
Source code for all IRAF tasks and interfaces is included with thisinstallation, but is strictly only required if you plan to develop this
87
Command over commands Chrisphin Karthick,ARIES20062007
code. The sources may be deleted from the system without affecting theruntime environment (including help pages, compilation of external packages or local task development) allowing you to reclaim 5060Mb of diskspace for the system. Stripping sources is recommended for systems veryshort on space, leaving it on the system will allow IRAF site support tosend code fixes and compilation instructions as needed to fix problemswhich have no other workaround.
Do you wish to strip the system of sources? (no):============================================================================================= PostInstall Verification ==============================================================================================
Display Server Availability
======================================================================================== Installation Completed With No Errors =======================================================================================
please check the /iraf/iraf/unix/hlib/extern.pkg Thanx chrisphin[root@aries25 iraf]#exit
[chrisphin@aries25 ~]$ mkiraf creating a new uparm directoryTerminal types: xgterm,xterm,gterm,vt640,vt100,etc.Enter terminal type: xgtermA new LOGIN.CL file has been created in the current directory.You may wish to review and edit this file to change the defaults.and then for externing the package of stsdas go to
89
Command over commands Chrisphin Karthick,ARIES20062007
>cd /iraf/iraf/unix/hlib>vi extern.pkg
edit the earlier commands like shown below...# External (non coresystem) packages. To install a new package, add the
# two statements to define the package root directory and package task,# then add the package helpdb to the `helpdb' list.
Command over commands Chrisphin Karthick,ARIES20062007
V.Extinction Coefficients for ARIESThe extinction coeff. measured for Dec2, 2005 is given below for each filter.
U 0.458727+/0.010090B 0.245316+/ 0.010248V 0.134039+/0.004601R 0.091876+/0.002154I 0.050587+/0.002275
The transformation coeff. for the same night is given below. The first colum is the equation used, second column is the slope, then error in slope, then intercept, error in intercept.
The extinction correction u can give like this.u0=uKu * Xb0=bKb * Xv0=vKv * Xr0=rKr * Xi0=iKi *X
where, ubvri are the observed magnitudes(without any correction)u0, b0,v0,r0, i0 are th extinction corrected using the above relationKu,Kb,Kv,Kr,Ki are the extinctions coeffs. which is given above for
97
Command over commands Chrisphin Karthick,ARIES20062007
each filters. X is the respective airmasses.
then the eqns. for giving transformation coeffs. is given below.
Vv0 = f1 * (BV)+f2Vv0 = g1 * (VR)+g2......This way u can make any combination of eqns. here a1,a2,b1,b2,c1,c2.... etc are the std coeffs. which is given above.u can directly use those coefficients. and UBVRI are the std magnitude fromthe Landolt.
After rearranging the last two eqns, u can get the final std V mag. then from V std mag,u can get std mag for any other filters.
Location, Nainital is situated at 29 degree 24' north latitude and 79 degree 28' east longitude. Altitude,1938 Meters or 6360 ft, above sea level.
98
Command over commands Chrisphin Karthick,ARIES20062007
VI.Site Characteristics of HCT
Latitude 32d46m46s N
Longitude78d57m51s E
Altitude4500 meters above msl
SeismicityLow
Wind SpeedMedian 2.2 m/s (8 kmph) at night
Wind DirectionPrevailing southsoutheasterly
Low ambient temperature and very lowhumidity
Annual precipitation of rain & snow< 7 cm
Precipitable water vapour< 2 mm between October and April
Number of spectroscopic nights~ 260 per year
Number of photometric nights~ 190 per year
Median seeing< 1 arcsec
Uniform distribution of useful nights roundthe year
Command over commands Chrisphin Karthick,ARIES20062007
VII.Extinction and Sky Brightness for HCT
Mean Extinction Values (2000 December 2003 January)
U0.353 +/ 0.037
B0.209 +/ 0.029
V0.121 +/ 0.032
R0.0823 +/ 0.037
I0.0497 +/ 0.027
Mean night sky brightness (1995 & 2002)
U23.64 +/ 0.57
B22.94 +/ 0.50
V21.52 +/ 0.21
R20.20 +/ 0.35
I18.60 +/ 0.21
100
Command over commands Chrisphin Karthick,ARIES20062007
VIII .Halpha filter response curve for HCT
101
Command over commands Chrisphin Karthick,ARIES20062007
IX.FeAr wavelength identification1
102
Command over commands Chrisphin Karthick,ARIES20062007
X.FeAr wavelength identification2
103
Command over commands Chrisphin Karthick,ARIES20062007
XI.FeNe wavelength identification
104
Command over commands Chrisphin Karthick,ARIES20062007
XII.Standard calibration data for extinction from IRAF
The onedstds$ directory contains standard calibration data for extinction andsensitivity calibration as used in the ONEDSPEC, TWODSPEC, and the variousIMRED packages.
ctioextinct.dat CTIO extinction table for ONEDSPEC (in Angstroms) The CTIO extinction curve distributed with IRAF comes from the work of Stone & Baldwin (1983 MN 204, 347) and Baldwin & Stone (1984 MN 206, 241). The first of these papers lists the points from 32008370A while the second extended the flux calibration from 6056 to 10870A but the derived extinction curve was not given in the paper. The IRAF table follows SB83 out to 6436, the redder points presumably come from BS84 with averages used in the overlap region.
More recent CTIO extinction curves are shown as Figures in Hamuy et al (92, PASP 104, 533 ; 94 PASP 106, 566).
Steve Heathcote, Mon, 19 Jul 1999
kpnoextinct.dat KPNO extinction table for ONEDSPEC (in Angstroms)
MISCELLANEOUS
ctio Directory containing CTIO decker comb positions and neutral density filter curves (used with NDPREP).
FLUX STANDARD DIRECTORIES (eg caldir = onedstds$iidscal/)
blackbody Directory for using blackbody flux distributions in various magnitude bands.
bstdscal Directory of the brighter KPNO IRS standards (i.e. those with HR numbers) at 29 bandpasses, data from various sources transformed to the Hayes and Latham system,
105
Command over commands Chrisphin Karthick,ARIES20062007
unpublished. ctiocal Directory containing fluxes for the southern tertiary standards as published by Baldwin & Stone, 1984, MNRAS, 206, 241 and Stone and Baldwin, 1983, MNRAS, 204, 347. ctionewcal Directory containing fluxes at 50A steps in the blue range 33007550A for the tertiary standards of Baldwin and Stone derived from the revised calibration of Hamuy et al., 1992, PASP, 104, 533. This directory also contains the fluxes of the tertiaries in the red (605010000A) at 50A steps as will be published in PASP (Hamuy et al 1994). The combined fluxes are obtained by gray shifting the blue fluxes to match the red fluxes in the overlap region of 6500A7500A and averaging the red and blue fluxes in the overlap. The separate red and blue fluxes may be selected by following the star name with "red" or "blue"; i.e. CD 32 blue. iidscal Directory of the KPNO IIDS standards at 29 bandpasses, data from various sources transformed to the Hayes and Latham system, unpublished. irscal Directory of the KPNO IRS standards at 78 bandpasses, data from various sources transformed to the Hayes and Latham system, unpublished (note that in this directory the brighter standards have no values the `bstdscal' directory must be used for these standards at this time). oke1990 Directory of spectrophotometric standards observed for use with the HST, Table VII, Oke 1990, AJ, 99. 1621 (no correction was applied). An arbitrary 1A bandpass is specified for these smoothed and interpolated flux "points". Users may copy and modify these files for other bandpasses. redcal Directory of standard stars with flux data beyond 8370A. These stars are from the IRS or the IIDS directory but have data extending as far out into the red as the literature permits. Data from various sources. spechayescal The KPNO spectrophotometric standards at the Hayes flux points, Table IV, Spectrophotometric Standards, Massey et al., 1988, ApJ 328, p. 315. spec16cal Directory containing fluxes at 16A steps in the blue range 33007550A for the secondary standards, published in Hamuy et al., 1992, PASP, 104, 533. This directory
106
Command over commands Chrisphin Karthick,ARIES20062007
also contains the fluxes of the secondaries in the red (602010300A) at 16A steps as will be published in PASP (Hamuy et al 1994). The combined fluxes are obtained by gray shifting the blue fluxes to match the red fluxes in the overlap region of 6500A7500A and averaging the blue and red fluxes in the overlap. The separate red and blue fluxes may be selected by following the star name with "red" or "blue"; i.e. HR 1544 blue. spec50cal The KPNO spectrophotometric standards at 50 A intervals. The data are from (1) Table V, Spectrophotometric Standards, Massey et al., 1988, ApJ 328, p. 315 and (2) Table 3, The Kitt Peak Spectrophotometric Standards: Extension to 1 micron, Massey and Gronwall, 1990, ApJ 358, p. 344.
STANDARD STAR MENUS
Blackbody calibrations in onedstds$blackbody/
U B V R I J H K L Lprime M
Magnitude conversions are available between V, J, H, K, L, Lprime, and Mbut for U, B, R, and I the star magnitudes must be in the same bandpass.Standard stars in onedstds$bstdscal/