Command over commands Chrisphin Karthick,ARIES-2006-2007

COMMAND
OVER

COMMANDS


An Astronomers data reduction Guide

( IRAF and Linux etc. )



WRITTEN BY


M.CHRISPHIN KARTHICK,

ARIES-2006-2007,

Nainital.




Preface

This guide is good to start for beginner and expert to recall. The most of the topics and commands may available from anywhere or from internet, but here it has written only which is most often used in data reduction . Also ,the last page attached with all the software’s which is required for data reduction for installation purpose and including some important websites which is necessary for an Astronomer. So at the most which is reducing your time to spend on the internet and getting the details. For soft copy and important links log on http://aries.ernet.in/page_chrisphin.html. While Using this guide mean time cross check with the expert if any corrections are there. In this guide if you have any feedback or queries ,please write to chrisphin@aries.ernet.in or chrisphink@yahoo.co.in.

Yours

M.Chrisphin Karthick,






Known is a DROP

Unknown is an OCEAN



Last edited :22 November 2007


Contents


  1. Linux commands

  2. Summary of preprocessing

  3. IRAF Commands
    (Before Basic reduction )

  4. Setting observatory

  5. Setting Air mass

  6. Basic Reduction

  7. Alignment

  8. Cosmic ray reduction through MIDAS

  9. Cosmic ray reduction through IRAF

  10. Aperture Photometry

  11. Spectroscopy reduction

Wavelength Calibration

Flux Calibration

Some more hints on spectroscopy reduction

  1. LATEX Introduction

  2. Ellipse Fitting

  3. Iraf Installation

How it's works



Appendix


I. General

II. Air mass Calculation Program

III. FEAR - FeAr Line List 3000A-10,000A by D. Willmarth

IV. Spectrum Extinction file for IAO (spec_ext.dat)

V. Extinction Coefficients for ARIES

VI. Site Characteristics of HCT

VII. Extinction and Sky Brightness for HCT

VIII. H-alpha filter response curve for HCT

IX. Fe-Ar wavelength identification-1

  1. Fe-Ar wavelength identification-2

  2. Fe-Ne wavelength identification

  3. Standard calibration data for extinction from IRAF



TOP

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> <destinatio----whole directory

>mv <source> <destination>-------for move

>mv  <source>  <destination>----for renaming also

>pwd----------------present working directory

  1. <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>

>dvips <latexoutputfile> -o <newfilename.ps>

(OR) >dvips -o <.ps> <latexoutputfile.dvi>

>gv < .ps>

>man commandname-------for 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 -af----to display all the processes running on the host

UID PID PPID C STIME TTY TIME CMD

501 3618 3545 0 11:00 pts/1 00:00:00 ps -af

> du -k---To report size (in kBytes) of all enclosed directories (recursive)

> du -ms *-----To report size (in kBytes) of all enclosed directories (non-recursive)

> users-----------To 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@IPaddress

then mget* or mput*

or >scp –r username@IPaddress: pathway of file or folder

>yum install softwarename---for installing anything in new fedora version.


For creating webpage


>mozilla

then from file GO EDIT PAGE then from edit page file GO COMPOSURE PAGE

now start work .


to get the details of memory capacity of all ....

chrisphin > df

Filesystem 1K-blocks Used Available Use% Mounted on

/dev/sda8 12096724 8125824 3356416 71% /

/dev/sda6 101086 11153 84714 12% /boot

/dev/sda10 18326876 77888 17318024 1% /data

none 253436 0 253436 0% /dev/shm

/dev/sda5 10231392 1241840 8989552 13% /dos

/dev/sda7 25197220 19620160 4297084 83% /home



working from another computer to our computer then...type..

xhost+

>ssh -X chrisphin @ 202.141.125.144


chrisphin>ls -lrt to know the recent downloaded file.

total 101456

drwxr-xr-x 2 chrisphin chrisphin 4096 Mar 19 2001 lib

drwxrwxr-x 3 chrisphin chrisphin 4096 Nov 4 2005 updatednews

drwxrwxr-- 7 chrisphin chrisphin 4096 Jul 27 09:52 images

-rw-rw-r-- 1 chrisphin chrisphin 1937248 Jul 27 09:52 Firefox_wallpaper.png

drwxrwxr-x 2 chrisphin chrisphin 4096 Jul 27 12:31 uparm



>clear---------to clear the terminal

>setup---------to set up the configuration of computer.





for .fits file getting details from the terminal...type

>more <filename>

cosmic > more csa104b02.fits

SIMPLE = T / Fits standard

BITPIX = -32 / Bits per pixel

NAXIS = 2 / Number of axes

NAXIS1 = 1024 / Axis length

NAXIS2 = 1024 / Axis length

EXTEND = T / File may contain extensions

ORIGIN = 'ESO-MIDAS' / FITS file originator

DATE = '2006-07-31T08:43:32' / Date FITS file was generated

IRAF-TLM= '10:41:08 (03/08/2006)' / Time of last modification

OBJECT = 'sa104 ' / Name of the object observed

COMMENT NOST 100-2.0: Hanisch,R. et al. 2001, Astron. & Astrophys. 376, 559


CRPIX1 = 1. / Reference pixel

CRVAL1 = 1. / Coordinate at reference pixel

CDELT1 = 1. / Coord. incr. per pixel (original value)

CTYPE1 = ' ' / Units of coordinate

CRPIX2 = 1. / Reference pixel

CRVAL2 = 1. / Coordinate at reference pixel

CDELT2 = 1. / Coord. incr. per pixel (original value)

CTYPE2 = ' ' / Units of coordinate

BUNIT = ' ' / Units of data values

DATAMAX = 437.2375 / Maximum data value

RA = 12:42:22 / MIDAS desc.: O_POS(1)

DEC = 00:40:00 / MIDAS desc.: O_POS(2)

DATE-OBS= '2006-05-03T17:01:25' / MIDAS desc.: O_TIME(1)

TM-START= 0. / MIDAS desc.: O_TIME(5)

EXPTIME = 260. / MIDAS desc.: O_TIME(7)

EPOCH = 2000

ST = 13.085

UT = 17.02361

AIRMASS = 1.146693

UTMIDDLE= '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

>ls

chrisphin default

>cd chrisphin

>ls

>vi bookmark.html

chrisphin>firefox&


>mplayer <filename.avi>------To play the .avi format movie.

chrisphin > bc -lq---------For using terminal as a calculator

1+1

2

:quit


writting a program and executing:

>vi <filename>

.................

:wq

Some version problem while transforming tex file (gvim to vi somethinlg like that)

in vi file u may come across the problem of ^M

then

:%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:

  1. .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.



example:

[chrisphin@aries25 ~]$ aries

[chrisphin@aries25 ariesasper25oct06fits]$


To know that which shell we are working :

[chrisphin@aries25 ~]$ echo $SHELL

/bin/csh

for changing the shell type

[chrisphin@aries25 ~]$chsh

password:

changing the shell type

>csh

then 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

>su

password

>xcdroast

(but before that confirm that whether it is installed xcdroast in /usr/bin)





Installation of real player in linux

download the file

then

> 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 pasword that 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.c

or

>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 rm-r="rm-r -i"

alias g="gomidas"


:wq


chrisphin~>source .bashrc


For bringing scroll bar into iraf the command is as follow and also
midas wavelength calibration files is as attachment see the
attachment below thanks:.....
xgterm -sb -fn 10*20 &

TOP

1.1-Printer Configuration for ARIES


adding a printer or printer settings:

go to system setting-printing


printer name:DN2420

networked jet direct

202.141.125.4 port:9100

HP

LASER JET 2420(if not any 2300)

finish.


TOP

2.Summary of pre-processing:


  1. Converting file into fits format.

  2. Setting Observatory*

  3. Setting Airmass*

  4. Making Master bias-----Bias subtraction

  5. 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)}

  1. Align it.

  2. Trim it.

  3. Cosmic rays removal.

  4. 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.fits-------bias_nth frame

fl_r1.fits------flat_filter nth frame

mbi.fits------master bias

mfl_r.fits—master flat_filter

nfl_r.fits ----normalized flat_filter

b-bias substracted---bobject_r1.fits--or--b_object_r1.fits

n-normalised--------nobject_r1.fits

a-aligned------------aobject_r1.fits

c-cosmic reduced--cobject_r1.fits

s-summed-----------sobject_r1.fits

u-unit exposure-----uobject_r1.fits

sc-scaled-------------scobject_r1.fits

sk-sky substracted---skobject_r1.fits


Spectroscopy:

wobject.fits---wavelength calibrated

fobject.fits----flux calibrated



Regarding folder:

  1. floder name as yyyy_mm_dd

  2. for original data

  3. all preprocessing

  4. outside the ----current working.


TOP

03-IRAF 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 bias

2.epar flatcombine—for flat

3.epar imcombine---for object at last only(after pre-processing 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 lines will be produced...in corner side of the spectrum.


In spectro....disp command wont work.....only display ...will work.


*********************************************************************************



TO view the full details of one .fits file


>imhead <filename> l+ | page

or)

>imhead <filename> lo+


to bring control bar in the iraf terminal

press

ctrl+right click--------in 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 name

Filter: <filter Name>

where wr2fits is an executable file....which is in the computer.written only for the image name and filter for ARIES.


[chrisphin@aries25 22mar07]$ wr2fits bi*

Totally are to be processed

Please enter the default parameters :

Image info : bias

Filter : none

1 ) Input file: bi_1.fts

outputfile: bi_1.fits

2) Input file: bi_2.fts

outputfile: bi_2.fits



ob1.fits ,ob2.fits....if v you want to make a list then :


> ob *.fits >>jude

> !emacs jude &



cl> show version

NOAO/IRAF V2.12.2-EXPORT


cl>show printer

lp


cl> refer photometry


cl> help [a-z]*




For saving the Graph:


:.snap epsfl

To 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> e

disp aobject_r1.fits

frame to be written into (1:4) (2):

z1=1380.411 z2=1612.45

im> display zs- zr- z1=1500 z2=3000

image 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

image to be displayed (tn1156r01.fits): ctn1156a01.fits

frame to be written into (1:4) (2): 1

z1=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=<1500

z2=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 =STDOUT

then 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 take the extension of .imh)then the storage space you will get more .Then convert that into fits format

by 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 written

Actually this imh file stores at /iraf/imdirs/chrisphin.So before take into another computer better to change it into fits format.



About imexam:

>imexam


go to the ds9 image....and placing the cursor on a star.press


a----for statitics details

r---radial plot

e---contour plot

c—coloumn plot

l---line plot

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 displayed

frame = 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)


:wq

For trimming;

PACKAGE = ccdred

TASK = ccdproc

images = @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

(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.fits---15min }----imageu1.fits----45min—

imageu3.fits---15min }

The task is

>epar imcombine

PACKAGE = 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)

:go

Others are all by default only change the above darkened.

Note: Change the exposure time in imheader for the output




TOP

04.Setting observatory

cl>noao

no>epar observatory

PACKAGE = noao

TASK = observatory


command = set Command (set|list|images)

obsid = ARIES Observatory to set, list, or image default

images = List of images

(verbose= yes) Verbose output?


(observa= obspars) Observatory identification

(name = ARIES) Observatory name

(longitu= 280.514) Observatory longitude (degrees)

(latitud= 29.36) Observatory latitude (degrees)

(altitud= 1950.) Observatory altitude (meters)

(timezon= -5.5) Observatory time zone

(mode = ql)


override= obspars Observatory identification


:go

Observatory 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



TOP

05. Setting Airmass

for hct one prog has written it is /home/chrisphin/bin/airmass1 this will do by itself.


for that

>noao

>astutil

>asthedit

as> asthedit

Images to be operated upon ( wobject.fits):

File of commands (/home/chrisphin/bin/airmas1):

17.76111111111111

2006.19367569143

2453807.2400463

10.37416111111111

1.12053504889221


then check the imheader;

as> imhead wobject.fits lo+


(in the last row it will join)


LONG = 281.0358

LAT = 32.7795

UT = '17:45:40'

EP = 2006.19367569143

JD = 2453807.2400463

ST = '10:22:26.98'

RAP = '12:27:53.73'

DAP = '44:07:42.71'

HA = 2.09076388888889

AIRMASS = 1.12053504889221


before setting airmass confirm that respective observatory has been set.how to set it is given .

as> setairmass

Input images (csa104*.fits): fn*.fits


# Image UT middle effective begin middle end updated

# SETAIRMASS: Observatory parameters for ARIES

# latitude = 29.36

fn4449a1.fits 18:23:41.0 1.1303 1.1281 1.1303 1.1325 yes

fn4449a2.fits 18:31:14.0 1.1439 1.1393 1.1439 1.1487 yes

as> epar setairmass

PACKAGE = astutil

TASK = setairmass


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 = date-obs) Observation date keyword

(exposur= exptime) Exposure time keyword (seconds)

(airmass= airmass) Airmass keyword (output)

(utmiddl= utmiddle) Mid-observation UT keyword (output)

(scale = 750.) The atmospheric scale height

(show = yes) Print the airmasses and mid-UT?

:go


TOP


06-Basic Reduction


from terminal

>xgterm.fedora&

>ds9&


then from xgterm terminal

chrisphin > cl

NOAO PC-IRAF Revision 2.12.2-EXPORT Sun Jan 25 16:09:03 MST 2004

This is the EXPORT version of PC-IRAF 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:


dataio. language. obsolete. softools. tables.

dbms. lists. plot. stsdas. utilities.

images. noao. proto. system.

cl> noao

artdata. digiphot. nobsolete. onedspec.

astcat. focas. nproto. rv.

astrometry. imred. observatory surfphot.

astutil. mtlocal. obsutil. twodspec.

no> im

argus. crutil. echelle. iids. kpnocoude. specred.

bias. ctioslit. generic. irred. kpnoslit. vtel.

ccdred. dtoi. hydra. irs. quadred.

im> cc

badpiximage ccdmask flatcombine mkskyflat

ccdgroups ccdproc mkfringecor setinstrument

ccdhedit ccdtest mkillumcor zerocombine

ccdinstrument combine mkillumflat

ccdlist darkcombine mkskycor

cc> ls


then go to the respective file.

In the upcoming task commands consider only about the darken region others are all default


  1. epar zerocombine---------for making master bias

PACKAGE = ccdred

TASK = zerocombine

input = b*.fits List of zero level images to combine-------all 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

(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 ccdclip

mbias1.fits is the combination of median and none)

Jul 26 14:13: IMCOMBINE


combine = median, scale = none, zero = none, weight = none

reject = minmax, nlow = 0, nhigh = 1

blank = 0.

Images

bias1.fits

bias2.fits

bias3.fits

bias4.fits

bias5.fits

bias6.fits


Output image = mbias.fits, ncombine = 6


for substracting master bias from all the images use ccdproc command. or if you wants to do it one by one then use imarith command

>imarith inputimage – mbias.fits outputimage


>ls *.fits >>list

Just to do all at one time make a list and do at one stroke.

cc>epar ccdproc

PACKAGE = ccdred

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


then running as...

sa104b07.fits: Jul 26 14:43 Zero level correction image is mbias.fits

sa104r01.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 flatcombine-----do it for same filter images alone in one for flat combine using this

PACKAGE = ccdred

TASK = flatcombine


input = bflat_r* List of flat field images to combine--------bias subtracted all flat images of one particular 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

combine = median, scale = mode, zero = none, weight = none

reject = avsigclip, mclip = yes, nkeep = 1

lsigma = 3., hsigma = 3.

blank = 1.

Images Exp Mode Scale

bflata1.fits 200.0 2408. 2.217

bflata2.fits 200.0 7314. 0.730

bflata3.fits 70.0 6295. 0.848


Output image = mfla.fits, ncombine = 3


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.)


cc> imarith bobject_r1.fits / nfl_r.fits nobject_r1.fits


(like that do it for all with respect to their filter flat)


cc>ls bn* >list2

cc> imarith @list2 / nflr.fits f//@list2





Hint: Repalcing bad pixel

  1. epar imreplace

PACKAGE = imutil

TASK = imreplace


images = bflat_r* Images to be edited

value = 1. Replacement pixel value

(imagina= 0.) Imaginary component for complex

(lower = 0.) Lower limit of replacement window

(upper = INDEF) Upper limit of replacement window

(radius = 0.) Replacement radius

(mode = ql)


:go


OR –if you wants to replace particular portion --open the image and note down the that particular coordinates


replacing bad pixel...........

cc> disp test_5430.fits 1

z1=-1.380593 z2=1.359507

cc>imreplace test_5430.fits[1051:1055,955:959] 3.5

cc>epar imreplace

PACKAGE = imutil

TASK = imreplace


images = test_5430.fits[1051:1055,955:959] Images to be edited

value = 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)


:go

TOP

07-Alignment


first display the respective frame....in ds9.alway stry to choose the red filter frame as are reference one.

cc> disp nobject_r1.fits

frame to be written into (1:16) (2):1

z1=1.951634 z2=15.75021


to create an file type :

cc> epar imexam

PACKAGE = 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 output

frame = 1 display frame

image = image name

(logfile= al.co) logfile

(keeplog= yes) log output results


:go

Log 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 1000-28,000. The 28,000 value is with respect to our aries.then “q”

cc>emacs al.co

then 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


then it becomes



282.88 393.49

286.26 438.66

420.94 550.00

462.09 658.93

507.39 741.35

601.68 613.98

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 2

z1=0.9973257 z2=15.23859


cc> tvmark

Default frame number for display (:16) (2):

Input coordinate list (al.co):


cc> imexam

Log file al.co open


then selct the respective stars in order.

then quit from the image

cc> emacs al.co

then 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 shown above)


282.88 393.49 283.33 396.57

286.26 438.66 286.75 441.81

420.94 550.00 421.38 553.07

462.09 658.93 462.56 662.05

507.39 741.36 507.83 744.34

601.68 613.98 602.13 617.12


and save it.

For cut---------> (ctrl+x) + rk

For paste ----->(ctrl+x) + ry

cc> epar geomap


PACKAGE = immatch

TASK = geomap

input = al.co The input coordinate files

database= al.co_db The output database file

xmin = 1. Minimum x reference coordinate value

xmax = 1024. Maximum x reference coordinate value

ymin = 1. Minimum y reference coordinate value

ymax = 1024. Maximum y reference coordinate value

(interac= no) Fit transformation interactively ?


:go

Coordinate list: al.co Transform: al.co

Results file: tobject_r2.fits

Coordinate mapping status

X fit ok. Y fit ok.

Xin and Yin fit rms: 0.01747025 0.04828498

Coordinate 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 geotran

PACKAGE = immatch

TASK = geotran

input = nobject_r2.fits Input data

output = aobject_r2.fits Output data

database= al.co_db Name of GEOMAP database file

transfor= 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 = tvmark

frame = 1 Default frame number for display

coords = 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 pixels

More




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 will display)


TOP

08-Cosmic ray reduction through MIDAS


Go to the respective file.where the reducing fits files contains.


chrisphin>inmidas

ESO-MIDAS version 06FEBpl1.0 on PC/Linux

Midas 015>

Midas 015> set/con daophot----only once at the time of starting


***** DAOPHOT application package version April 1991 enabled *****

commands available:

ALLSTAR/DAOPHOT Do simultaneous multiple-profile-fitting

DAOPHOT/DAOPHOT Do stellar photometry in 2-dimensional images

DAOMID/DAOPHOT Convert DAOPHOT tables to MIDAS tables

MIDDAO/DAOPHOT Convert MIDAS tables to DAOPHOT tables


Midas 016> indisk/fits aobjectr_1.fits aobject_r1.bdf


no CDELTi nor CDi_j matrix found... STEPi set to 1.0

FITS file: tfbn4449b1.fits converted to: tfbn4449b1.bdf


(Midas 020> help fil/cosmic

FILTER/COSMIC )


Midas 021> daophot

Revised 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

WATCH PROGRESS = 1.00 FITTING RADIUS = 2.00

PSF RADIUS = 15.00 VARIABLE PSF = 0.00

FRACTIONAL-PIXEL EXPANSION = 0.00 ANALYTIC MODEL PSF = 1.00

EXTRA PSF CLEANING PASSES = 5.00 PERCENT ERROR (in %) = 0.75

PROFILE ERROR (in %) = 5.00


Command: at aobject_r1

ngc 4449


Picture size: 1024 1024

Command:sky


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 filter

we process frame in 2 chunks ...

expanding frame - Th, 18 May 2006 14:37:08

working on chunk 1 - Th, 18 May 2006 14:37:09

working on chunk 2 - Th, 18 May 2006 14:37:09

Beginning of the cosmic rays removal


Midas 026> outdisk/fits cobject_r1.bdf cobject_r1.fits

FITS file cfbn4449b1.fits will have 1 extensions

cfbn4449b1.bdf written to FITS file cfbn4449b1.fits

--------------------------------------------------------------------------------------------------------

( To check whether mistakenly some stars are deleted are not.This mask.fits give only the removed part...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.bdf

Beginning of the median filter

we process frame in 2 chunks ...

expanding frame - Th, 18 May 2006 14:38:03

working on chunk 1 - Th, 18 May 2006 14:38:03

working on chunk 2 - Th, 18 May 2006 14:38:03

Beginning of the cosmic rays removal

Midas 028> outdisk/fits mask.bdf mask.fits

FITS file mask.fits will have 1 extensions

mask.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.bdf

Warning: <COMMENT1> of invalid type - not stored

Warning: <COMMENTX> of invalid type - not stored

rot-long = 6.283185, rotlat = 0.000000 - axes not orthogonal!

FITS file: TAfe34_a2.fits converted to: Tafe34_a2.bdf


Midas 018> help fil/cosmic

FILTER/COSMIC 21-NOV-1991 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), read-out-noise (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 Long-Slit spectra of extended sources, the algorithm may be


hit return to continue, 'q' + return to quit Midas 018> help fil/cosmic

FILTER/COSMIC 21-NOV-1991 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), read-out-noise (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 Long-Slit 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).

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 (Imax-sky) is greater than rc*(Iaver-sky), 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 fine-tuning. 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/MEDIAN

Examples:

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 21-NOV-1991

PM,MR

Enter SKY,G,RON,NS,RC:


TOP

09-Cosmic ray reduction through IRAF

cc> disp aobject_r1.fits

frame to be written into (1:16) (1):

z1=102.8171 z2=133.1152

cc> 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 1.708 109.1 115.2

cc> crutil

cosmicrays crcombine crfix crmedian

craverage credit crgrow crnebula

cr> epar cosmic

input = aobject_b1.fits List of images in which to detect cosmic rays

output = ctobject_b1.fits List of cosmic ray replaced output images (optio

(crmasks= ) List of bad pixel masks (optional)


(thresho= 11.) Detection threshold above mean


:go

aobject_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.

1.if it is blended (following gaussian distribution)....then it is a star.


press "s"

see the plotting

come 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 ....

TOP

10-Aperture Photometry


first make a coordinate file by selecting 10 or 15 stars....here i have selected first 5----standard stars..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

:go

log file open

(Now select the stars ...it will be in the file named ' co ' )

>imexam

SA- 104----MEAN 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 .


cl> noao

artdata. digiphot. mtlocal. observatory surfphot.

astrometry. focas. nobsolete. onedspec. twodspec.

astutil. imred. nproto. rv.

no> digi

apphot. daophot. photcal. ptools.

di> daophot

addstar daotest nstar pexamine psf

allstar datapars@ pcalc pfmerge psort

centerpars@ findpars@ pconcat phot pstselect

daoedit fitskypars@ pconvert photpars@ seepsf

daofind group pdump prenumber setimpars

daopars@ grpselect peak pselect substar


da> epar phot

PACKAGE = apphot

TASK = phot


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 counts-----sigma value

(datamin= 0.2375) Minimum good data value-------------------------sky-5*sigma

(datamax= 28000.) Maximum good data value--------------Saturation level ...

(noise = poisson) Noise model

(ccdread= ) CCD readout noise image header keyword

(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


:q

PACKAGE = daophot

TASK = centerpars


(calgori= none) Centering algorithm

(cbox = 6.44) Centering box width in scale units-----------------2*3.74-- - - ie..2*FWHM

(cthresh= 0.) Centering threshold in sigma above background

(minsnra= 1.) Minimum signal-to-noise 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.) K-sigma rejection criterion in skysigma

(mkcente= no) Mark the computed center

(mode = ql)


:q

PACKAGE = daophot

TASK = fitskypars


(salgori= mode) Sky fitting algorithm----constant---for 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 units-----5(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

(snrejec= 50) Maximum number of sky fitting rejection iteratio

(sloreje= 3.) Lower K-sigma rejection limit in sky sigma

(shireje= 3.) Upper K-sigma 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 HELP

nstant|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 units----for knots--

(dannulu= 0.) Width of sky annulus in scale units---for 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 K-sigma rejection limit in sky sigma

(shireje= 3.) Upper K-sigma 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

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 the

1.vector plot(wher vector plot shows the total diameter ..but take only the radius)

2.from the flux------fluctuationn 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)...20----final radius(4FWHM).---.5--interval


:q

then from the main....phot pakage


:go


Centering algorithm (centroid) (CR or value): (just type enter for all )

New centering algorithm: centroid

Centering box width in scale units (5.) (CR or value):

New centering box width: 5. scale units 5. pixels

Sky fitting algorithm (centroid) (CR or value):

Sky fitting algorithm: centroid

Inner radius of sky annulus in scale units (20.) (CR or value):

New inner radius of sky annulus: 20. scale units 20. pixels

Width of the sky annulus in scale units (10.) (CR or value):

New width of the sky annulus: 10. scale units 10. pixels

File/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

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. pixels

Standard deviation of background in counts (1.3) (CR or value):

New standard deviation of background: 1.3 counts

Minimum good data value (INDEF) (CR or value):

New minimum good data value: INDEF counts

Maximum 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. it means 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

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: centroid

Centering box width in scale units (5.) (CR or value):

New centering box width: 5. scale units 5. pixels

Sky fitting algorithm (centroid) (CR or value):

Sky fitting algorithm: centroid

Inner radius of sky annulus in scale units (20.) (CR or value):

New inner radius of sky annulus: 20. scale units 20. pixels

Width of the sky annulus in scale units (10.) (CR or value):

New width of the sky annulus: 10. scale units 10. pixels

File/list of aperture radii in scale units (19) (CR or value):

Aperture radius 1: 19. scale units 19. pixels

Standard deviation of background in counts (1.3) (CR or value):

New standard deviation of background: 1.3 counts

Minimum good data value (INDEF) (CR or value):

New minimum good data value: INDEF counts

Maximum 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 it make one file like ' mag ' with only needed parameters instead of all.

through the command...


ap>epar txdump

PACKAGE = apphot

TASK = txdump

textfile= *.mag.2 Input apphot/daophot text database(s)

fields = ID,XCENTER,YCENTER,MAG,MERR,IMAGE,RAPERT,FLUX Fields to be extracted

expr = yes Boolean expression for record selection

(headers= no) Print the field headers ?

(paramet= yes) Print the parameters if headers is yes ?

(mode = ql) Mode of task



ap> txdump >mag

Input 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 1.1434

2 364.319 688.529 12.815 0.004 csa104r01.fits 1.1434

3 401.578 604.448 13.608 0.007 csa104r01.fits 1.1434


(then the file is look like above mentioned where the last one is AIRMASS--here airmass included after that manually)


Then open the terminal go to that file.

cosmic > emacs mag& (this & symbol allowed to open two emacs windows )

[3] 6794

1 351.529 867.175 14.850 0.015 csa104b02.fits 1.1467

2 364.414 688.483 12.978 0.005 csa104b02.fits 1.1467

3 401.631 604.402 14.223 0.009 csa104b02.fits 1.1467

4 511.751 492.538 15.646 0.025 csa104b02.fits 1.1467

5 263.457 436.599 15.279 0.019 csa104b02.fits 1.1467

6 855.151 553.466 INDEF INDEF csa104b02.fits 1.1467

7 943.576 663.904 11.166 0.002 csa104b02.fits 1.1467

8 612.870 812.539 14.962 0.016 csa104b02.fits 1.1467

9 745.028 914.030 14.606 0.013 csa104b02.fits 1.1467

10 844.448 691.592 15.543 0.024 csa104b02.fits 1.1467

1 351.498 868.058 15.001 0.013 csa104b03.fits 1.5842

2 364.394 689.294 13.147 0.005 csa104b03.fits 1.5842

3 401.589 605.307 14.345 0.009 csa104b03.fits 1.5842

4 511.650 493.542 15.734 0.019 csa104b03.fits 1.5842

""""" """" """"" """""" '''''

cosmic > emacs magb1&

[4] 6795

1 14.850 0.015 csa104b02.fits 1.1467

1 15.001 0.013 csa104b03.fits 1.5842

1 15.068 0.013 csa104b04.fits 1.7020

1 15.217 0.014 csa104b05.fits 1.8460

1 15.410 0.017 csa104b06.fits 2.0781

1 15.478 0.019 csa104b07.fits 2.2980

(like this open two emacs and from the main (mag) take only the --one particular star-- one particular filter ---all frames(magb1)---as shown above.

or the simple command is from the terminal go to the respective file and type ......

cosmic > awk '{if($1==2) print ($1,$4,$5,$6,$7)}' mag

2 12.978 0.005 csa104b02.fits 1.1467

2 13.147 0.005 csa104b03.fits 1.5842

2 13.232 0.005 csa104b04.fits 1.7020

2 13.349 0.005 csa104b05.fits 1.8460

2 13.512 0.006 csa104b06.fits 2.0781

2 13.620 0.006 csa104b07.fits 2.2980

2 12.815 0.004 csa104r01.fits 1.1434

2 12.813 0.004 csa104r02.fits 1.1541

2 12.897 0.004 csa104r03.fits 1.5146

2 12.930 0.004 csa104r04.fits 1.6622

2 13.133 0.005 csa104r05.fits 1.7988

2 13.168 0.005 csa104r06.fits 1.9445

2 13.226 0.005 csa104r07.fits 2.2243

2 12.568 0.004 csa104v01.fits 1.1416

2 12.568 0.004 csa104v02.fits 1.1505

2 13.366 0.005 csa104v03.fits 1.5406

2 12.776 0.004 csa104v04.fits 1.7619

2 12.889 0.004 csa104v05.fits 1.9012

2 12.960 0.004 csa104v06.fits 2.1544

2 13.017 0.005 csa104v07.fits 2.3898

then it will list out the 2nd stars of all the frames and filter.as shown above.then

cosmic > emacs magb2&

[1] 10224

cosmic > emacs magv2&

[2] 10225

[1] Done emacs magb2

cosmic > 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 work

cosmic > 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 2.6.9-1.667smp


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 on-line reference manual.

The gnuplot FAQ is available from

http://www.gnuplot.info/faq/


Send comments and requests for help to

<gnuplot-info@lists.sourceforge.net>

Send bugs, suggestions and mods to

<gnuplot-bugs@lists.sourceforge.net>

Terminal type set to 'x11'

After inside the gnuplot if you want to list out the files to see then type

gnuplot>!ls

gnuplot>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 in yaxis.nothing but in the x axis AIRMASS in yaxis MAGNITUDE

For saving the plot

gnuplot>set term post

gnuplot>set output “filename.ps”

gnuplot>pl “data_filename”

gnuplot> y(x)=m*x+c

gnuplot> fit y(x) "magv1" u 5:2 via m,c

then in the terminal details will come .

Iteration 0

WSSR : 835.669 delta(WSSR)/WSSR : 0

delta(WSSR) : 0 limit for stopping : 1e-05

lambda : 1.4634


initial set of free parameter values


m = 1

c = 1

/


Iteration 1

WSSR : 37.2229 delta(WSSR)/WSSR : -21.4504

delta(WSSR) : -798.446 limit for stopping : 1e-05

lambda : 0.14634


resultant parameter values


m = 4.82373

c = 4.76338

/


Iteration 2

WSSR : 0.1378 delta(WSSR)/WSSR : -269.122

delta(WSSR) : -37.0851 limit for stopping : 1e-05

lambda : 0.014634


resultant parameter values


m = 0.671102

c = 13.3427

/


Iteration 3

WSSR : 0.00507841 delta(WSSR)/WSSR : -26.1345

delta(WSSR) : -0.132722 limit for stopping : 1e-05

lambda : 0.0014634


resultant parameter values


m = 0.361653

c = 13.9148

/


Iteration 4

WSSR : 0.00507835 delta(WSSR)/WSSR : -1.21954e-05

delta(WSSR) : -6.19328e-08 limit for stopping : 1e-05

lambda : 0.00014634


resultant parameter values


m = 0.361441

c = 13.9152

**/


Iteration 5

WSSR : 0.00507835 delta(WSSR)/WSSR : -6.83184e-16

delta(WSSR) : -3.46945e-18 limit for stopping : 1e-05

lambda : 0.0014634


resultant parameter values


m = 0.361441

c = 13.9152


After 5 iterations the fit converged.

final sum of squares of residuals : 0.00507835

rel. change during last iteration : -6.83184e-16


degrees of freedom (ndf) : 4

rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313

variance 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 c

m 1.000

c -0.966 1.000

gnuplot> 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 star details.like...below then you can see the percentage of error will be less now.


1 14.324 0.011 csa104v01.fits 1.1416

1 14.337 0.011 csa104v02.fits 1.1505

#1 15.183 0.014 csa104v03.fits 1.5406

1 14.508 0.011 csa104v04.fits 1.7619

1 14.637 0.011 csa104v05.fits 1.9012

1 14.728 0.013 csa104v06.fits 2.1544

1 14.752 0.012 csa104v07.fits 2.3898

*******************************************************************************

Fri Aug 4 15:50:26 2006

FIT: 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


Iteration 0

WSSR : 0.07522 delta(WSSR)/WSSR : 0

delta(WSSR) : 0 limit for stopping : 1e-05

lambda : 1.4634


initial set of free parameter values


m = 0.26786

c = 14.1777

190,0-1 After 4 iterations the fit converged.

final sum of squares of residuals : 0.00507835

rel. change during last iteration : -6.80346e-09


degrees of freedom (ndf) : 4

rms of residuals (stdfit) = sqrt(WSSR/ndf) : 0.0356313

variance of residuals (reduced chisquare) = WSSR/ndf : 0.00126959


Final set of parameters Asymptotic Standard Error

======================= ==========================


m = 0.361441 +/- 0.03095 (8.563%)

c = 13.9152 +/- 0.05608 (0.403%)


correlation matrix of the fit parameters:

m c

m 1.000

c -0.966 1.000

Also it will create an log file to save this information.onitself as fit.log file.

awk '{print($5-0.36*$7)}' obsmag


TOP

11-Spectroscopy reduction

Hints:

1.First do everything with the specred....means u cant do apall with onedspec command.....so enter in to specred then to onedspec.

2.you cant do everything with specred .because ,while calibrating u have to mention the place (filename where it is located ..like onestds$spec50cal )it is available only in the onedspec so onedspec is important....unless we are keeping the file in our own place)


For deleting the .imh file

>imdel <filename.imh>


Requirements:

1.object-167 l

2.Standard two(Oke 1990)-1340 l

3.comparision(Fe-Ar)

4.flat (Halogen lamp)

5.bias

*Grism with respct to wavelength coverage.

Part-1.basic Steps

changing the name into .fits file.

>pc120001

>epar rename

files = pc* list of files to be renamed

newname = fits new file name or field name

(field = extn) field to be modified (all|ldir|root|extn)

(mode = ql)

:go

>imhead pc120047.fits

pc120047.fits[500,3500][ushort]: NGC 4216

cc> e

mv pc120047.fits n4216-2.fits

cl> noao

artdata. digiphot. nobsolete. onedspec.

astcat. focas. nproto. rv.

astrometry. imred. observatory surfphot.

astutil. mtlocal. obsutil. twodspec.

no> im

argus. crutil. echelle. iids. kpnocoude. specred.

bias. ctioslit. generic. irred. kpnoslit. vtel.

ccdred. dtoi. hydra. irs. quadred.

im> cc

badpiximage ccdmask flatcombine mkskyflat

ccdgroups ccdproc mkfringecor setinstrument

ccdhedit ccdtest mkillumcor zerocombine

ccdinstrument combine mkillumflat

ccdlist darkcombine mkskycor

cc> specred

aidpars@ apresize dispcor response skysub

apall apscatter dofibers sapertures skytweak

apdefault@ apsum dopcor sarith slist

apedit aptrace doslit scombine specplot

apfind autoidentify fitprofs scopy specshift

apfit background identify sensfunc splot

apflatten bplot illumination setairmass standard

apmask calibrate msresp1d setjd telluric

apnormalize continuum refspectra sfit

aprecenter deredden reidentify sflip


sp> ls

(go into the respective file)




sp> epar imcombine


PACKAGE = immatch

TASK = imcombine

(the changable parameters are):

input = bias*.fits List of images to combine

output = mbias.fits List of output images

(combine= median) Type of combine operation

(reject = avsigclip) Type of rejection

(rdnoise= 4.8) ccdclip: CCD readout noise (electrons)

(gain = 1.22) ccdclip: CCD gain (electrons/DN)

:go

Jun 13 11:41: IMCOMBINE

combine = median, scale = none, zero = none, weight = none

reject = avsigclip, mclip = yes, nkeep = 1

lsigma = 3., hsigma = 3.

blank = 0.

Images Offsets

bias1.fits 0 0

bias2.fits 0 0

bias3.fits 0 0

bias4.fits 0 0

bias5.fits 0 0

bias6.fits 0 0

bias7.fits 0 0


Output image = mbias.fits, ncombine = 7

cc> display mbias.fits

frame to be written into (1:16) (1):

z1=273.2498 z2=299.


sp>imstat mbias.fits[3:480,243:3200] means x,y limitation

# IMAGE NPIX MEAN STDDEV MIN MAX

mbias.fits[3:480,243:3200] 1413924 349.2 49.55 259. 834.


sp> imarith g19b2b-2.fits - 349.2 bg19b2b-2.fits


(just like do for all images....exept fe-ar)


sp> imstat bhal?.fits

# IMAGE NPIX MEAN STDDEV MIN MAX

bhal1.fits 1750000 8221. 9342. -349.2 52146.

bhal2.fits 1750000 8226. 9349. -349.2 52172.

bhal3.fits 1750000 8238. 9363. -349.2 52271.

bhal4.fits 1750000 8231. 9356. -349.2 52320.

bhal5.fits 1750000 8247. 9373. -349.2 52336.

(then take mean of mean)....here ..the mean is 8233

sp>imarith bhal1fits / 8233 nbhal1.fits

(like that do for all)

sp> epar imcombine


PACKAGE = immatch

TASK = imcombine

input = nbhal*.fits List of images to combine

output = fnbhal.fits List of output images

(combine= median) Type of combine operation

(reject = avsigclip) Type of rejection

:go

Jun 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 = 5

sp> epar response

calibrat= fnbhal.fits Longslit calibration images

normaliz= fnbhal.fits Normalization spectrum images

response= rfnbhal.fits Response function images

(functio= spline3) Fitting function

(order = 3) Order of fitting function

:go

Fit the normalization spectrum for fnbhal.fits interactively (yes):no

sp>imarith bm106-1.fits / rfnbhal.fits fbm106-1.fits


TOP

Part-2.Wavelength Calibartion

sp>epar apall


(better do not give the output name...it will take automatically with extension of .ms.imh)



# EXTRACTION PARAMETERS


(backgro= median) Background to subtract-----earlier 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 fbm106-1? (yes):

Resize apertures for fbm106-1? (yes):

Edit apertures for fbm106-1? (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..that

using the s & t

where s—for marking level..

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 to reduce 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.fits

on>splot nobject_spec.imh

on>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 identify

images = 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 fe-ar 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

To extend on Y axis-------shift+y

fo marking------------------m

to come back and do again--r

f---j---f----q---Then the fitted curve will appear...delete the points (by "d")which is apart from the line.and try to reduce reduce the RMS value.

l---j----f-- (here f=j ..so use f itself)

q

(f-fitting, j-risidual plot,l=longitudinal plot, l-it 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 as reference.


sp> hedit nobject_1_spec.imh field=REFSPEC1 value=fear_spec.imh

hedit fm106-1-spec.imh field=REFSPEC1 value=fear-spec.imh

add fm106-1-spec.imh,REFSPEC1 = fear-spec.imh

update fm106-1-spec.imh ? (yes):

bm106-1_spec.imh updated


sp> epar dispcor

input = nobject-1_spec.imh List of input spectra

output = wobject-1_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 = 3500

After 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 specshift

PACKAGE = specred

TASK = specshift


spectra = List of spectra

shift = 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 spectra

output = List of output spectra

redshift= 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

TOP

Part-3.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



input = Dstd_2.ms.imh Input image file root name

output = 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= 3.6800000000000E-20) 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 input

star_nam= feige34 Star name in calibration list

airmass = Airmass

exptime = Exposure time (seconds)

mag = Magnitude of star

magband = Magnitude type

teff = Effective temperature or spectral type

answer = 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 4.6598E-13 50.000 3417.

3250.00 4.3944E-13 50.000 2187.5

3300.00 4.4222E-13 50.000 1189.7

3350.00 4.2912E-13 50.000 885.67

3400.00 4.0899E-13 50.000 786.2

3450.00 3.8639E-13 50.000 778.63

3500.00 3.6185E-13 50.000 993.41

3550.00 3.5173E-13 50.000 512.38

3600.00 3.3271E-13 50.000 387.07

3650.00 3.1775E-13 50.000 152.9

3700.00 3.0357E-13 50.000 51.126



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 within IRAF has to be specified..needed..hence for setting these...follow the below...



sp> help onedstd


Standard stars in onedstds$spec50cal/ (3200A - 10200A)


bd284211 eg247 feige34 g191b2b hz44

eg139 eg71 feige66 gd140 pg0823546

eg158 feige110 feige67 hilt600 wolf1346



sp> epar sens


PACKAGE = onedspec

TASK = sensfunc



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

(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 device

answer = 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 9

then “ r “--- replot

d “---delete the deviated points in the below figure.

f “ --fit

r “ --replot

Now you can see RMS value has been reduced.

After finishing “ q “---quit



sp> epar cali


Here the input is dispersion corrected object.


PACKAGE = onedspec

TASK = calibrate


input = Dn1569_1.ms.imh Input spectra to calibrate

output = Fn1569_1.ms.imh Output calibrated spectra

(extinct= yes) Apply extinction correction?

(flux = yes) Apply flux calibration?

(extinct= /home/observer/chris/bin/spec_ext.dat) Extinction file

(observa= )_.observatory) Observatory of observation

(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 = Airmass

exptime = Exposure time (seconds)

(mode = ql)


:go




Fn1569_1.ms.imh: NGC-1569

Cn1569_1.imh: NGC-1569

Extinction correction applied

Flux calibration applied

The above warning because of trimmming may be..



Then sploting the final wavelength and flux calibrated spectrum will appear.

TOP

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 ray then 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 apertures

where “ d” for delete the apeture....so if any cosmic ray prsent and aperture goes for that ...then pres f for 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 another peak...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.

in the splot graph

by typing k,k two times u can get the value of fwhm....and others.


for saving the graph

:.snap epsfl

To 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 options

a Add point to constrain fit

c Print the coordinates and fit of point nearest the cursor

d Delete data point nearest the cursor

f Fit the data and redraw or overplot

g 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 y

h-l Graph keys. Defaults are h=(x,y), i=(y,x), j=(x,r), k=(x,d), l=(x,n)

o Overplot the next graph

q Exit the interactive curve fitting. Carriage return will also exit.

r Redraw graph

s Set sample range with the cursor

t Initialize the sample range to all points

v Change the weight of the point nearest the cursor

u Undelete the deleted point nearest the cursor

w Set the graph window. For help type 'w' followed by '?'.

x Change the x value of the point nearest the cursor

y Change the y value of the point nearest the cursor

z Delete sample region nearest cursor

I Interrupt task immediately



2. INTERACTIVE CURVE FITTING COLON COMMANDS


The parameters are listed or set with the following commands which may be

abbreviated. To list the value of a parameter type the command alone.


: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 manipulating

the 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 to

put 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 specify

the axes types for the horizontal and vertical axes by a pair of comma

separated types from the following:


d Ratio (y / f)

f Fitted values

r Residuals of fit (y - f)

n Nonlinear part of data (linear component of fit subtracted)

x Indepedent variable

y 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(*)

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 graph

e - Equiv. width, integ flux, center x - Connects 2 cursor positions

f - Arithmetic functions: log, sqrt... y - Plot std star flux from calib file

g - Get new image and plot z - Expand x range by factor of 2

h - Equivalent widths(*) ) - Go to next spectrum in image

i - Write current image as new image ( - Go to previous spectrum in image

j - Fudge a point to Y-cursor value # - Select new line/aperture

k - Profile fit to single line(*) % - Select new band

l - Convert to F-lambda $ - Toggle wavelength/pixel scale

m - Mean, RMS, snr in marked region - - Subtract deblended fit

n - Convert to F-nu , - Down slide spectrum

o - Toggle overplot of following plot . - Up slide spectrum

p - Convert to wavelength scale I - Interrupt task immediately

q - 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

: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


TOP

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.tex

This 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.dvi

This is dvips(k) 5.92b Copyright 2002 Radical Eye Software (www.radicaleye.com)

' TeX output 2006.11.01:1541' -> hct_obsp_new.ps


> gv hct_obsp_new.ps

>ps2pdf hct_obsp_new.ps hct_obsp_new.pdf

>xpdf hct_obsp_new.pdf


for a short cut.......you can open a vi editer and put all the commands which has to be executed and then execute that file which will do all the work by one stroke.

>vi l

latex hct_obsp_new.tex

dvips -o hct_obsp_new.ps hct_obsp_new.dvi

gv 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 Wolf-Rayet Galaxies }\\

\vspace{1.0cm}

\bf Chrisphin.K, B.B.Sanwal,D.K.sahu, M.Singh\\\small \bf Aryabhatta Research Institute of Observational Sciences(ARIES)\\Manora Peak,Nainital. \\

\vspace{0.5cm}

{\small

\it email: chrisphin@aries.ernet.in}

\end{center}

\bigskip

\begin{abstract}


\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.

\section----for 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$2k-----------2K x 2K

H$\alpha$ \& H$\alpha$ ----H


In escape mode...

5dd---deleting 5lines.like that any number of lines..

u---undo

5yy---5 lines copying

p-----paste.

for cutting- use the same command for deleting-dd

redo-ctrl+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}|}

\hline

Sl.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\\

\hline

& & & & & &\\ \hline

& & & & & &\\ \hline

& & & & & &\\ \hline

& & & & & &\\ \hline

\end{tabular}


\newpage

\vskip 2cm

if you want to jump to 30 th line in vi editor..

then type

:30

and all the commnad s is possible to execute from..the same terminal..by typing..

:!latex <filename>

:!dvips -o filename.ps filename.dvi


Finding the SFR the expression is:


SFR$_{H\alpha} (M_\odot year^{-1})= 7.9 \times 10^{-42} L_{H\alpha}$


\hspace*{0.1in} –while beginnning sentence giving space.


for inserting the fgure:


\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.

TOP


13.Ellipse Fitting

chrisphin > cl

NOAO PC-IRAF Revision 2.12.2-EXPORT Sun Jan 25 16:09:03 MST 2004

This is the EXPORT version of PC-IRAF 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:


dataio. language. obsolete. softools. tables.

dbms. lists. plot. stsdas. utilities.

images. noao. proto. system.

cl> stsdas



+------------------------------------------------------------+

| 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 e-mail to help@stsci.edu |

| |

+------------------------------------------------------------+

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


is> epar ellipse

PACKAGE = isophote

TASK = ellipse


input = n4449B.fits input image name------ cleaned galaxy image

output = b output table name

(dqf = .c1h) data quality file name or extension

(inellip= ) table with input ellipses for no-fit 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) memory-intensive (versus disk-intensive) ?

(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 semi-major axis lenght

(minsma = 0.) minimum semi-major axis lenght

(maxsma = INDEF) maximum semi-major axis lenght

(step = 0.1) sma step between successive ellipses

(linear = no) linear sma step ?

(maxrit = INDEF) maximum sma lenght for iterative mode

(recente= yes) allows finding routine to re-center x0-y0 ?

(xylearn= yes) updates pset with new x0-y0 ?

(physica= yes) physical coordinate system ?

(mode = al)


:q

then press :e by placing the cursor on control

Image Reduction and Analysis Facility

PACKAGE = 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 k-sigma threshold

(soft = no) soft stop ?

(mode = al)


:q


PACKAGE = isophote

TASK = samplepar


(integrm= bi-linear) area integration mode

(usclip = 3.) sigma-clip criterion for upper deviant points

(lsclip = 3.) sigma-clip criterion for lower deviant points

(nclip = 0) number of sigma-clip 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)

: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)

:q

then

:go

Running object locator... Done.

Can not find object. Please, enter initial

guess for starting isophote center:

X0: 485

Y0: 545

#


# Semi- Isophote Ellipticity Position Grad. Data Flag Iter. Stop

# major mean Angle rel. code

# axis intensity error

#(pixel) (degree)

#

10.00 852.25(322.98) 0.200(INDEF) 20.00(INDEF) INDEF 56 0 2 4

11.00 902.56(479.69) 0.200(INDEF) 20.00(INDEF) INDEF 62 0 1 4

9.09 812.00(227.45) 0.200(INDEF) 20.00(INDEF) INDEF 51 0 2 4

8.26 787.88(183.00) 0.200(INDEF) 20.00(INDEF) INDEF 46 0 1 4

7.51 774.51(167.34) 0.200(INDEF) 20.00(INDEF) INDEF 42 0 1 4

6.83 773.30(158.86) 0.200(INDEF) 20.00(INDEF) INDEF 38 0 1 4

6.21 775.17(152.67) 0.200(INDEF) 20.00(INDEF) 19.53 35 0 1 4

5.64 785.31(142.66) 0.200(INDEF) 20.00(INDEF) 3.560 32 0 1 4

5.13 799.19(133.24) 0.200(INDEF) 20.00(INDEF) 2.546 29 0 1 4

4.67 814.31(122.95) 0.200(INDEF) 20.00(INDEF) 2.284 26 0 1 4

4.24 825.31(112.12) 0.200(INDEF) 20.00(INDEF) 3.023 24 0 1 4

3.86 836.47(102.91) 0.200(INDEF) 20.00(INDEF) 2.839 22 0 1 4

3.50 845.04( 95.28) 0.200(INDEF) 20.00(INDEF) 3.571 20 0 1 4

3.19 852.90( 88.52) 0.200(INDEF) 20.00(INDEF) 3.795 18 0 1 4

2.90 855.50( 83.38) 0.200(INDEF) 20.00(INDEF) 11.16 17 0 1 4

2.63 863.26( 77.85) 0.200(INDEF) 20.00(INDEF) 3.675 15 0 1 4

2.39 865.60( 73.17) 0.200(INDEF) 20.00(INDEF) INDEF 14 0 1 4

2.18 871.25( 68.40) 0.200(INDEF) 20.00(INDEF) 4.825 13 0 1 4

1.98 872.41( 64.20) 0.200(INDEF) 20.00(INDEF) 3.854 13 0 1 4

1.80 874.40( 59.60) 0.200(INDEF) 20.00(INDEF) 12.15 13 0 1 4

1.64 876.17( 55.01) 0.200(INDEF) 20.00(INDEF) 12.71 13 0 1 4

1.49 877.63( 50.27) 0.200(INDEF) 20.00(INDEF) 14.17 13 0 1 4

1.35 879.08( 46.06) 0.200(INDEF) 20.00(INDEF) 13.07 13 0 1 4

1.23 880.09( 42.18) 0.200(INDEF) 20.00(INDEF) 17.21 13 0 1 4

1.12 880.76( 38.58) 0.200(INDEF) 20.00(INDEF) 23.35 13 0 1 4

1.02 881.15( 34.98) 0.200(INDEF) 20.00(INDEF) 37.93 13 0 1 4

0.92 881.38( 31.62) 0.200(INDEF) 20.00(INDEF) 56.84 13 0 1 4

0.84 881.55( 28.60) 0.200(INDEF) 20.00(INDEF) 68.24 13 0 1 4

0.76 881.68( 25.89) 0.200(INDEF) 20.00(INDEF) 82.65 13 0 1 4

0.69 881.77( 23.45) 0.200(INDEF) 20.00(INDEF) 104.1 13 0 1 4

0.63 881.84( 21.25) 0.200(INDEF) 20.00(INDEF) 134.5 13 0 1 4

0.57 881.88( 19.26) 0.200(INDEF) 20.00(INDEF) 186.7 13 0 1 4

0.52 881.90( 17.47) 0.200(INDEF) 20.00(INDEF) 287.5 13 0 1 4

0.00 881.45

0.01 CPU seconds.

0.00 minutes elapsed.

>ls


now if you see list b.tab file has been created.to view that file type

>tprint b.tab




>epar isoexam

PACKAGE = isophote

TASK = isoexam


table = b.tab isophote table

(dqf = .c1h) data quality file name or extension

(device = red) graphics output device

(icomman= ) image cursor

(gcomman= ) graphics cursor

(mode = al)


:q



>epar isoimap

PACKAGE = isophote

TASK = isoimap


image = n4449B.fits input image

table = b.tab input table

(fulltab= yes) use full range of `SMA' from table ?

(minsma = 1.) minimum semi-major axis

(maxsma = 1.) maximum semi-major axis

(nlevels= 3) number of levels

(color = r) overlay color

(frame = 1) image display frame

(mode = al)

:q

is> epar isomap


PACKAGE = isophote

TASK = isomap


image = n4449B.fits input image

table = b.tab input table

floor = minimum contouring level

ceiling = 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 table

xaxis = RSMA x axis

yaxis = MAG y axis

(device = stdgraph) output graphics device

(mode = al)


:go

(will give the plot for mag vs SMA *1/4)


>epar isopall

input = b.tab input table

xaxis = RSMA x axis

(device = stdgraph) output graphics device

(mode = al)


:go


(will give the plot for all)


is>ttools

tt>tprint


tt> ?

gtedit tabkey tcreate tiimage tprint tstat

gtpar@ tabpar tdelete tinfo tproduct ttranspose

imtab taextract tdiffer tintegrate tproject tunits

keypar tainsert tdump titable tquery tupar

keyselect tcalc tedit tjoin tread tximage

keytab tchcol texpand tlcol trebin txtable

parkey tcheck thedit tlinear tscopy

partab tchsize thistogram tmatch tselect

tabim tcopy thselect tmerge tsort


tt> tcalc

Input table: b.tab

Output column name: magb

Arithmetic expression: -2.5*log10(INTENS)


(then in the output table b.tab one more column has fomed with magb)

like that find out for v&r



tt> tproj

Input tables (b): v

Output tables (b1): v1

Column names (sma,magb): sma,magv


this will give the output table with only two colum as sma and magv from original table.

tt> tmerge

list of tables: b1,v1,r1

name of output table: bvr

merge or append? (merge|append) (merge):


This will give the output as with the common one (ie..sma)and the individual magnitudes.


tt> tcalc

Input table (r.tab): bvr

Output column name (magr): b-v

Arithmetic expression (-2.5*log10(INTENS)): magb-magv


then the output is.....


# row SMA magb magv magr b-v

# pixel


1 10.00 -7.326419 -8.350383 -8.977684 1.023964

2 11.00 -7.388693 -8.402966 -9.018461 1.014274

3 12.10 -7.452424 -8.45775 -9.061924 1.005327




tt> tcalc

Input table (bvr):

Output column name (b-v): v-r

Arithmetic expression (magb-magv): magv-magr

tt> tprint bvr

# row SMA magb magv magr b-v

# pixel


1 10.00 -7.326419 -8.350383 -8.977684 1.023964

2 11.00 -7.388693 -8.402966 -9.018461 1.014274

v-r

#


1 0.6273012

2 0.6154947



for making a model using the table parameters

tt> epar bmodel


PACKAGE = isophote

TASK = bmodel


table = b.tab isophote table

output = bm.fits output (model) image

(parent = b.fits) parent image

(fulltab= yes) use full range of `SMA' from table ?

(minsma = 1.) minimum modelling SMA

(maxsma = 1.) maximum modelling SMA

(backgr = 0.) background value

(interp = spline) interpolation algorithm

(highar = no) add higher harmonics ?

(verbose= no) print info ?

(mode = ql)


:go


then the model image will appear.


tt> imarith b.fits - bm.fits subb.fits


(substracting from parent image to model image)



# Table bvr.tab Tue 14:13:23 25-Jul-2006


# row SMA magb magv magr b-v v-r

# pixel


1 10.00 -7.326419 -8.350383 -8.977684 1.023964 0.6273012

2 11.00 -7.388693 -8.402966 -9.018461 1.014274 0.6154947

3 12.10 -7.452424 -8.45775 -9.061924 1.005327 0.6041737

4 13.31 -7.509982 -8.501146 -9.105608 0.9911642 0.6044617

5 14.64 -7.515865 -8.498053 -9.102729 0.9821873 0.6046762

6 16.11 -7.441709 -8.417347 -9.020638 0.9756379 0.6032915

7 17.72 -7.267367 -8.255603 -8.88203 0.9882355 0.6264277

8 19.49 -7.105531 -8.133438 -8.783742 1.027907 0.6503038

9 21.44 -7.025736 -8.073084 -8.733415 1.047348 0.6603308

10 23.58 -6.970555 -8.024835 -8.691433 1.054279 0.6665983

11 25.94 -6.88339 -7.956075 -8.63653 1.072685 0.6804547

12 28.53 -6.819172 -7.901899 -8.59342 1.082727 0.6915207

13 31.38 -6.815528 -7.881151 -8.569758 1.065623 0.6886077

14 34.52 -6.778287 -7.84915 -8.545932 1.070863 0.6967816

15 37.97 -6.768456 -7.825531 -8.517666 1.057076 0.6921344

16 41.77 -6.690573 -7.758854 -8.461597 1.068281 0.7027435

17 45.95 -6.576372 -7.672137 -8.395837 1.095766 0.7236996

18 50.54 -6.378003 -7.54169 -8.303526 1.163687 0.7618356

19 55.60 -6.272883 -7.465623 -8.244529 1.192739 0.7789059

20 61.16 -6.192893 -7.405949 -8.197833 1.213056 0.7918844

21 67.28 -6.070224 -7.315245 -8.131417 1.245021 0.8161726

22 74.00 -5.980441 -7.250807 -8.084737 1.270366 0.83393

23 81.40 -6.003924 -7.328994 -8.150055 1.32507 0.8210607

24 89.54 -5.761503 -7.09622 -7.970737 1.334717 0.8745165

25 98.50 -5.668857 -7.030812 -7.924924 1.361955 0.8941116

26 108.35 -5.626123 -6.995907 -7.896285 1.369784 0.9003778

27 119.18 -5.520816 -6.929633 -7.853443 1.408817 0.92381

28 131.10 -5.454289 -6.885037 -7.822189 1.430748 0.9371519

29 144.21 -5.391116 -6.846087 -7.797658 1.454971 0.9515715

30 158.63 -5.330243 -6.807044 -7.771194 1.476801 0.9641504

31 174.49 -5.270195 -6.777694 -7.752686 1.507499 0.9749918

32 191.94 -5.173338 -6.724012 -7.715868 1.550674 0.9918556

33 211.14 -5.134089 -6.704271 -7.702201 1.570182 0.99793

34 232.25 -5.115785 -6.693449 -7.693737 1.577663 1.000288




# Table b.tab Tue 13:37:45 25-Jul-2006


# row SMA INTENS INT_ERR PIX_VAR RMS ELLIP ELLIP_ERR PA

# pixel degrees


1 10.00 852. 43.2 457. 323. 0.2000 INDEF 20.00

2 11.00 903. 60.9 678. 480. 0.2000 INDEF 20.00

# row PA_ERR X0 X0_ERR Y0 Y0_ERR GRAD GRAD_ERR GRAD_R_ERR

# degrees pixel pixel pixel pixel


1 INDEF 485.00 INDEF 545.00 INDEF -0.04 INDEF INDEF

2 INDEF 485.00 INDEF 545.00 INDEF -0.032 INDEF INDEF


# row RSMA MAG MAG_LERR MAG_UERR TFLUX_E TFLUX_C TMAG_E

# pixel**1/4


1 1.77828 -7.33 0.0564 0.0536 202146. 254556. -13.3

2 1.82116 -7.39 0.0759 0.0709 247010. 306532. -13.5


# row TMAG_C NPIX_E NPIX_C A3 A3_ERR B3 B3_ERR A4

#


1 -13.5 251 317 -78.8 93.8 -98.5 105. 334.

2 -13.7 301 377 -303. 343. -349. 369. 623.


# row A4_ERR B4 B4_ERR NDATA NFLAG NITER STOP A_BIG SAREA

# pixel


1 272. -31.2 57.6 56 0 2 4 356. 2.0

2 548. -10.4 227. 62 0 1 4 137. 2.0


# row magb

#


1 -7.326419

2 -7.388693




is> tprint b1.tab



# Table b1.tab Tue 13:54:28 25-Jul-2006


# row SMA magb

# pixel


1 10.00 -7.326419

2 11.00 -7.388693

3 12.10 -7.452424


TOP


14-Iraf Installation

FOR REDHAT FEDORA


Download these three files first.


Create iraf tree.(using root in / )

/iraf

/ \

(AS) /iraf /irafbin

/ \

(IB) bin.redhat noao.bin.redhat (NB)


Put the files in the respective as shown in above figure .gunzip it and untar it,by the command,within the respective folder.


Simply

rm -rf iraf/ irafbin/ x11iraf/ extern/

echo 'making directroy structure'

mkdir iraf

mkdir irafbin

mkdir irafbin/bin.redhat

mkdir irafbin/noao.bin.redhat

mkdir extern

mkdir x11iraf

mkdir extern/stsdas

mkdir extern/stsdas/bin.redhat

mkdir extern/tables

mkdir extern/tables/bin.redhat

mkdir extern/fitsutil

echo 'Unpacking the file system'

cd /iraf/iraf

tar -zxf /iraf/redhat.package/as.pcix.gen.gz

cd /iraf/irafbin/bin.redhat

tar -zxf /iraf/redhat.package/ib.rhux.x86.gz

cd /iraf/irafbin/noao.bin.redhat

tar -zxf /iraf/redhat.package/nb.rhux.x86.gz

cd /iraf/x11iraf

tar -zxf /iraf/redhat.package/x11iraf-v1.3.1-bin.redhat.tar.gz

cd /iraf/extern/stsdas

tar -zxf /iraf/redhat.package/stsdas33.tar.gz

cd /iraf/extern/stsdas/bin.redhat

tar -zxf /iraf/redhat.package/stsdas33.bin.rh.tar.gz

cd /iraf/extern/tables

tar -zxf /iraf/redhat.package/tables33.tar.gz

cd /iraf/extern/tables/bin.redhat

tar -zxf /iraf/redhat.package/tables33.bin.rh.tar.gz

echo 'installing the x11'

cd /iraf/x11iraf

./install

echo 'installing the iraf'

cd /iraf/iraf/unix/hlib

./install

cd /iraf

echo 'please check the /iraf/iraf/unix/hlib/extern.pkg'



Of course then move the downloaded

Xgterm.fedora &ds9 to the /usr/local/bin.


***********************************************************************

Part-3


[chrisphin@aries25 ~]$ mkiraf

-- creating a new uparm directory

Terminal types: xgterm,xterm,gterm,vt640,vt100,etc.

Enter terminal type: xgterm

A 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

  1. /iraf/iraf/unix/hlib

  1. extern.pkg

edit the earlier commands like shown below...

# External (non core-system) 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.


reset noao = iraf$noao/

task noao.pkg = noao$noao.cl


reset tables = /iraf/extern/tables/

task tables.pkg = tables$tables.cl


reset stsdas = /iraf/extern/stsdas/

task stsdas.pkg = stsdas$stsdas.cl


reset helpdb = "lib$helpdb.mip\

,noao$lib/helpdb.mip\

,tables$lib/helpdb.mip\

,stsdas$lib/helbdb.mip\

"


keep


That's it.

TOP

14.1-How it's works

[root@aries25 chrisphin]#mkdir iraf

[root@aries25 chrisphin]#cd iraf


within this put this folder iraf.V2.12a.tgz


[root@aries25 iraf]# gunzip iraf.V2.12a.tgz

[root@aries25 iraf]# ls

iraf.V2.12a.tar

[root@aries25 iraf]# tar -xvpf iraf.V2.12a.tar

iraf.install

redhat.package/

redhat.package/as.pcix.gen.gz

redhat.package/tables33.bin.rh.tar.gz

redhat.package/ib.rhux.x86.gz

redhat.package/x11iraf-v1.3.1-bin.redhat.tar.gz

redhat.package/xgterm.fedora

redhat.package/tables33.tar.gz

redhat.package/stsdas33.bin.rh.tar.gz

redhat.package/stsdas33.tar.gz

redhat.package/nb.rhux.x86.gz

[root@aries25 iraf]# ./iraf.install

removing the existing directory structure for iraf

making directroy structure

Unpacking the file system

installing the x11


X11IRAF V1.3 Installation

=========================



Binary Installation:

--------------------


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 ]



Manual Page Installation:

-------------------------


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 ]



Application Default Resource Installation:

------------------------------------------


The app-defaults 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.


System app-defaults directory (/usr/lib/X11/app-defaults):...[ OK ]



Client Display Library (CDL) Installation:

------------------------------------------


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.


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 ======================

========================================================================


New iraf root directory (/iraf/iraf):

Default root image storage directory (/iraf/imdirs):

Local unix commands directory (/usr/local/bin):


========================================================================

===================== Verifying System Settings ======================

========================================================================


Hostname = aries25.upso.ernet.i OS version = Linux 2.6.9-1.667smp

Architecture = redhat HSI arch = redhat

New iraf root = /iraf/iraf Old iraf root = /iraf/iraf

New imdir = /iraf/imdirs Old imdir = /d0/imdirs

Local 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)

*** 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 ]

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 ]



========================================================================

===================== Post-Install Configuration =====================

========================================================================


The system should be fully functional at this point however some

post-install configuration may be required to make use of all the

features such as networking or tape access. Additional software such

as external packages or display servers will need to be installed

separately. Some minimal configuration can be accomplished now but

you should consult the IRAF Site Manager's Guide for a more complete

discussion of IRAF system management, configuration of printers, etc.


Proceed to post-install configuration stage? (yes):

IRAF Networking Config

----------------------


IRAF Networking can be used to access a remote image, tape device,

display server, or other network service. It's configuration is not

a requirement for normal IRAF operations and it can be updated at any

time by editing the IRAF dev$hosts file with new entries.


In this stage we will add an entry for the current platform to the

hosts file. In a local network installation this script should be run

on each system to add a networking entry as well as to install other

system files needed by IRAF.


Configure IRAF Networking on this machine? (yes):

Recommended dev$hosts file entry used for this machine:


aries25 aries25.upso.ern : aries25.upso.ernet.in!/iraf/iraf/bin.redhat/irafks.e


Proceed with this entry? (yes):


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 ]

------------------------------------------------------------------------



Tapecap Device File Config

--------------------------


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 PC-IRAF and Sun/IRAF support multiple OS versions

and so the proper template file must be used. This configuration will

allow you to setup a default tapecap for this system, it may be skipped

if 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 this

system IRAF will fallback to use just dev$tapecap. In cases where

the node name changes, this installation is shared with another

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 used

for all IRAF systems.


Do you wish to create a default dev$tapecap link? (yes):

Tapecap symlink 'tapecap' exists and is ok.

------------------------------------------------------------------------



Delete Unneeded HSI Binaries

----------------------------


The following bin directories in the iraf$unix directories were

found to be unused on this machine:


( 4768 Kb) /iraf/iraf/unix/bin.freebsd

( 2040 Kb) /iraf/iraf/unix/bin.linux

( 3540 Kb) /iraf/iraf/unix/bin.linuxppc

( 3460 Kb) /iraf/iraf/unix/bin.macosx

( 2480 Kb) /iraf/iraf/unix/bin.sunos

( 2432 Kb) /iraf/iraf/unix/bin.suse


The contents of these directories may be safely deleted to reclaim

about 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 this

installation, but is strictly only required if you plan to develop this

code. The sources may be deleted from the system without affecting the

runtime environment (including help pages, compilation of external pack-

ages or local task development) allowing you to reclaim 50-60Mb of disk

space for the system. Stripping sources is recommended for systems very

short on space, leaving it on the system will allow IRAF site support to

send code fixes and compilation instructions as needed to fix problems

which have no other workaround.


Do you wish to strip the system of sources? (no):

========================================================================

===================== Post-Install Verification ======================

========================================================================



Display Server Availability

---------------------------


Display Servers Found on This Machine:


( Date: 6 10:02 /usr/local/bin/ximtool ) /usr/local/bin/ximtool

( Date: 6 10:02 /usr/local/bin/ximtool-alt ) /usr/local/bin/ximtool-alt

( Date: 8 2004 /usr/local/bin/ds9 ) /usr/local/bin/ds9


------------------------------------------------------------------------


Graphics Terminal Availability

------------------------------


Graphics Terminals Found on This Machine:


( Date: 6 10:02 /usr/local/bin/xgterm ) /usr/local/bin/xgterm

( Date: 14 2004 /usr/bin/xterm ) /usr/bin/xterm




========================================================================

Congratulations! IRAF has been successfully installed on this system.

========================================================================


To begin using the system simply log in as any user and from the

directory you wish to use as your iraf login directory type:


% mkiraf # create a login.cl file

% cl # start IRAF


The 'iraf' user is already configured with a login.cl file so a simple

'cl' command is sufficient to start the system.


Additional information can be found at the IRAF web site:


http://iraf.noao.edu


Please contact site support with any questions or problems at


iraf@noao.edu



========================================================================

================ 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 directory

Terminal types: xgterm,xterm,gterm,vt640,vt100,etc.

Enter terminal type: xgterm

A 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

  1. /iraf/iraf/unix/hlib

  1. extern.pkg

edit the earlier commands like shown below...

# External (non core-system) 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.


reset noao = iraf$noao/

task noao.pkg = noao$noao.cl


reset tables = /iraf/extern/tables/

task tables.pkg = tables$tables.cl


reset stsdas = /iraf/extern/stsdas/

task stsdas.pkg = stsdas$stsdas.cl


reset helpdb = "lib$helpdb.mip\

,noao$lib/helpdb.mip\

,tables$lib/helpdb.mip\

,stsdas$lib/helbdb.mip\

"


keep


That's it.

HAVE A FUN.

TOP

I-General


For Aries 40 inch:


Readout Noise: 5.3 e-

Gain : 10 e-/ADU

Saturation level:28000


For HCT:

Readout noise is : 4.8

Gain is : 1.22

Saturation level : 63000




CALCULATING AIRMASS THROUGH MIDAS:

Midas 016> compute/airmass 13,23,35.2 36,07,59.5 ? 300 79,28,00 29,21,36 2006,5,03 17,20,00

Julian date: 2.453859222222E+06

Local mean sidereal time: 13 : 23 : 44.155

Airmass: 1.00707E+00

Midas 017>


Midas 016> compute/airmass RA DEC S.T EXPOTIME LONG LATI YYYY/M/DD UT


If dont know the ST just type ? in that place


TOP
II.Airmass Calculation Program


# Define variables.


# observatory = "IAO"


long = 281:02.15

lat = 32:46.77


ut = sexstr ((@'tm_start'+0.1) / 3600.)

# obd = sexstr(@'date-obs')a

# This is for 2k2nov15 (yy:mm:dd)

ep = epoch ('2006-03-12',ut)

jd = julday ('2006-03-12',ut)

st = mst ('2006-03-12',ut, long)

rap = ra_precess (ra, dec, ep, 2000)

dap = dec_precess (ra, dec, ep, 2000)

HA = rap - st

airmass = airmass (rap, dap, st, lat)

# print(obd)

print(ut)

print(ep)

print(jd)

print(st)

print(airmass)

# airmass = eairmass (ra, dec, mst, itime, obsdb (observat, "latitude"))


TOP

III.FEAR - FeAr Line List 3000A-10,000A by D. Willmarth

# units Angstroms


3443.8762 FeI

3722.5625 FeI

3859.9114 FeI

4033.8093 ArII

4158.5905 ArI

4198.3036 FeI

4348.0640 ArII

4427.3039 FeI

4545.0519 ArII

4657.9012 ArII

4764.8646 ArII

4879.8635 ArII

4965.0795 ArII

5167.4873 FeI

5227.1697 FeI

5269.5366 FeI

5328.0376 FeI

5371.4892 FeI

5606.7330 ArI

5912.0853 ArI

6032.1274 ArI

6114.9234 ArII

6416.3071 ArI

6677.2817 ArI

6752.8335 ArI

6871.2891 ArI

6965.4307 ArI

7067.2181 ArI

7272.9359 ArI

7383.9805 ArI

7635.1060 ArI

TOP

IV.Spectrum Extinction file for IAO (spec_ext.dat)


3000. 0.709266663

3050. 0.666614115

3100. 0.62731874

3150. 0.591068327

3200. 0.557584167

3250. 0.526616693

3300. 0.497942328

3350. 0.471360266

3400. 0.446689993

3450. 0.423768848

3500. 0.402450085

3550. 0.382601142

3600. 0.364102066

3650. 0.346844196

3700. 0.330728948

3750. 0.315666676

3800. 0.301575929

3850. 0.288382441

3900. 0.27601853

3950. 0.264422387

4000. 0.253537506

4050. 0.24331215

4100. 0.233698964

4150. 0.224654481

4200. 0.21613881

4250. 0.208115265

4300. 0.200550109

4350. 0.193412289

4400. 0.186673149

4450. 0.180306271

4500. 0.174287245

4550. 0.168593511

4600. 0.163204208

4650. 0.158099994

4700. 0.153262973

4750. 0.14867653

4800. 0.144325256

4850. 0.140194833

4900. 0.136271924

4950. 0.13254416

5000. 0.129000008

5050. 0.125628695

5100. 0.122420244

5150. 0.119365282

5200. 0.116455086

5250. 0.113681495

5300. 0.111036889

5350. 0.108514145

5400. 0.106106579

5450. 0.103807941

5500. 0.101612359

5550. 0.0995143577

5600. 0.0975087583

5650. 0.0955907404

5700. 0.0937557369

5750. 0.0919994786

5800. 0.0903179497

5850. 0.0887073651

5900. 0.0871641561

5950. 0.0856849775

6000. 0.0842666626

6050. 0.0829062387

6100. 0.0816008821

6150. 0.0803479403

6200. 0.0791449174

6250. 0.0779894367

6300. 0.0768792704

6350. 0.0758122951

6400. 0.0747865066

6450. 0.0738000199

6500. 0.0728510395

6550. 0.0719378665

6600. 0.0710588917

6650. 0.0702125877

6700. 0.0693975165

6750. 0.0686122924

6800. 0.0678556263

6850. 0.0671262667

6900. 0.0664230511

6950. 0.0657448545

7000. 0.0650906265

7050. 0.0644593537

7100. 0.0638500676

7150. 0.0632618666

7200. 0.062693879

7250. 0.0621452704

7300. 0.0616152622

7350. 0.0611030944

7400. 0.0606080554

7450. 0.0601294637

7500. 0.0596666671

7550. 0.05921904

7600. 0.0587859936

7650. 0.0583669618

7700. 0.0579614006

7750. 0.057568796

7800. 0.0571886562

7850. 0.0568205081

7900. 0.0564638972

7950. 0.0561183989

8000. 0.0557835922

8050. 0.0554590896

8100. 0.0551445074

8150. 0.0548394881

8200. 0.0545436852

8250. 0.0542567633

8300. 0.0539784022

8350. 0.0537083037

8400. 0.0534461737

8450. 0.0531917289

8500. 0.0529447012

8550. 0.0527048372

8600. 0.0524718799

8650. 0.052245602

8700. 0.0520257652

8750. 0.0518121608

8800. 0.051604569

8850. 0.0514027961

8900. 0.0512066409

8950. 0.0510159172

9000. 0.0508304499

9050. 0.0506500639

9100. 0.0504745916

9150. 0.0503038764

9200. 0.050137762

9250. 0.0499760993

9300. 0.0498187467

9350. 0.0496655703

9400. 0.0495164357

9450. 0.0493712127

9500. 0.0492297821

9550. 0.0490920246

9600. 0.0489578284

9650. 0.0488270782

9700. 0.048699677

9750. 0.0485755131

9800. 0.0484544933

9850. 0.0483365245

9900. 0.0482215099

9950. 0.0481093638

10000. 0.0480000004

10050. 0.0478933342

10100. 0.0477892905

10150. 0.047687795

10200. 0.0475887656

10250. 0.0474921316

10300. 0.0473978296

10350. 0.0473057851

10400. 0.0472159423

10450. 0.0471282303


TOP

V.Extinction Coefficients for ARIES

The extinction coeff. measured for Dec2, 2005 is given below for each filter.


U 0.458727+/-0.010090

B 0.245316+/- 0.010248

V 0.134039+/-0.004601

R 0.091876+/-0.002154

I 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.




slope error intercept error

BVbv 0.994553 0.01317 -0.346141 0.01704

VvBV 0.0179182086 0.0177878 -3.2054812 0.01676718

RIri 1.04770505 0.0323265 0.531954765 0.007405

UBub 0.86043411 0.0232752 -1.61161196 0.05531368

VIvi 0.99450880 0.023112 0.5001866 0.016288

VvVI 0.018754551 0.0165158 -3.2085557 0.01765941

VRvr 0.947630703 0.030370 0.01078140 0.017623

VRvr 0.934882 0.02597 0.0220804 0.01542

VvVR 0.0364902467 0.0308615 -3.2083962 0.016983876

UuUB -0.1290 0.03 -5.4014 0.02




The extinction correction u can give like this.

u0=u-Ku * X

b0=b-Kb * X

v0=v-Kv * X

r0=r-Kr * X

i0=i-Ki *X


where, ubvri are the observed magnitudes(without any correction)

u0, b0,v0,r0, i0 are th extinction corrected using the above relation

Ku,Kb,Kv,Kr,Ki are the extinctions coeffs. which is given above for

each filters. X is the respective airmasses.


then the eqns. for giving transformation coeffs. is given below.


(U-B) = a1 * (u0-b0)+a2

(B-V) = b1 * (b0-v0)+b2

(V-I) = c1 * (v0-i0)+c2

(V-R) = d1 * (v0-r0)+d2

(R-I) = e1 * (r0-i0)+e2


V-v0 = f1 * (B-V)+f2

V-v0 = g1 * (V-R)+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 from

the 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.


TOP

VI.Site Characteristics of HCT


        1. Latitude

32d46m46s N

        1. Longitude

78d57m51s E

        1. Altitude

4500 meters above msl

        1. Seismicity

Low

        1. Wind Speed

Median 2.2 m/s (8 kmph) at night

        1. Wind Direction

Prevailing south-south-easterly


Low ambient temperature and very low humidity

        1. Annual precipitation of rain & snow

< 7 cm

        1. Precipitable water vapour

< 2 mm between October and April

        1. Number of spectroscopic nights

~ 260 per year

        1. Number of photometric nights

~ 190 per year

        1. Median seeing

< 1 arcsec


Uniform distribution of useful nights round the year

        1. Longitudinal advantage

(79d E) Canary Islands (20d W); Eastern Australia(157d E)


Good accessibility round the yer

TOP

VII.Extinction and Sky Brightness for HCT

        1. Mean Extinction Values (2000 December - 2003 January)

                1. U

          0.353 +/- 0.037

                1. B

          0.209 +/- 0.029

                1. V

          0.121 +/- 0.032

                1. R

          0.0823 +/- 0.037

                1. I

          0.0497 +/- 0.027

        2. Mean night sky brightness (1995 & 2002)

        1. U

23.64 +/- 0.57

        1. B

22.94 +/- 0.50

        1. V

21.52 +/- 0.21

        1. R

20.20 +/- 0.35

        1. I

18.60 +/- 0.21


TOP

VIII .H-alpha filter response curve for HCT




TOP

IX.Fe-Ar wavelength identification-1



TOP
X.Fe-Ar wavelength identification-2


TOP

XI.Fe-Ne wavelength identification



TOP

XII.Standard calibration data for extinction from IRAF


The onedstds$ directory contains standard calibration data for extinction and

sensitivity calibration as used in the ONEDSPEC, TWODSPEC, and the various

IMRED packages.



EXTINCTION TABLES

(eg extinction = onedstds$kpnoextinct.dat)


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 3200-8370A 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,

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

3300-7550A 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 (6050-10000A) 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 6500A-7500A 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 3300-7550A for the secondary standards, published

in Hamuy et al., 1992, PASP, 104, 533. This directory

also contains the fluxes of the secondaries in the red

(6020-10300A) 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 6500A-7500A 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 M

but for U, B, R, and I the star magnitudes must be in the same bandpass.

--------------------------------------------------------------------------------

Standard stars in onedstds$bstdscal/


hr718 hr3454 hr3982 hr4468 hr4534

hr5191 hr5511 hr7001 hr7596 hr7950

hr8634 hr9087 hd15318 hd74280 hd100889

hd188350 hd198001 hd214923 hd224926


--------------------------------------------------------------------------------

Standard stars in onedstds$ctiocal/


bd25 eg139 feige56 l2415 l93080

bd73632 eg149 feige98 l2511 l97030

bd8 eg158 g16350 l3218 lds235

cd32 eg248 g2631 l3864 lds749

eg11 eg274 g9937 l4364 ltt4099

eg21 f15 h600 l4816 ltt8702

eg26 f25 hz2 l6248 ross627

eg31 f56 hz4 l7379 w1346

eg54 f98 hz15 l7987 w485a

eg63 f110 kopf27 l8702 wolf1346

eg76 feige110 l377 l9239 wolf485a

eg79 feige15 l1020 l9491

eg99 feige25 l1788 l74546


--------------------------------------------------------------------------------

Standard stars in onedstds$ctionewcal/:


Combined red and blue 3300A-10000A:


cd32 f56 l2415 l4364 l7987

eg21 h600 l3218 l4816 l9239

eg274 l1020 l377 l6248 l9491

f110 l1788 l3864 l7379 l745


Blue 3300A-7550A:


cd32blue f56blue l2415blue l4364blue l7987blue

eg21blue h600blue l3218blue l4816blue l9239blue

eg274blue l1020blue l377blue l6248blue l9491blue

f110blue l1788blue l3864blue l7379blue


Red 6050A-10000A:


cd32red f56red l2415red l4364red l7987red

eg21red h600red l3218red l4816red l9239red

eg274red l1020red l377red l6248red l9491red

f110red l1788red l3864red l7379red l745red


--------------------------------------------------------------------------------

Standard stars in onedstds$iidscal/


40erib eg50 eg149 g16350 hz4 lds235b

amcvn eg54 eg158 g191b2b hz7 lds749b

bd253941 eg63 eg162 g2610 hz14 lft1655

bd284211 eg67 eg182 g2631 hz15 lp414101

bd332642 eg71 eg184 g4718 hz29 ltt13002

bd404032 eg76 eg193 g88 hz43 ltt16294

bd73632 eg77 eg247 g9937 hz44 ltt4099

bd7781 eg79 eg248 gd128 kopff27 ltt8702

bd82015 eg91 feige15 gd140 l13633 ross627

eg11 eg98 feige24 gd190 l140349 ross640

eg20 eg99 feige25 gh7112 l14094 sa29130

eg26 eg102 feige34 grw705824 l151234b sao131065

eg28 eg119 feige56 grw708247 l74546a ton573

eg29 eg129 feige92 grw738031 l8702 wolf1346

eg31 eg139 feige98 he3 l93080 wolf485a

eg33 eg144 feige110 hiltner102 l97030

eg39 eg145 g12627 hiltner600 lb1240

eg42 eg148 g14563 hz2 lb227


--------------------------------------------------------------------------------

Standard stars in onedstds$irscal/


bd082015 eg50 feige34 hd117880 hd60778 hr7001

bd174708 eg71 feige56 hd161817 hd74721 hz44

bd253941 eg139 feige92 hd17520 hd84937 kopff27

bd262606 eg158 feige98 hd192281 hd86986 wolf1346

bd284211 eg247 feige110 hd19445 he3

bd332642 feige15 g191b2b hd217086 hiltner102

bd404032 feige25 hd109995 hd2857 hiltner600


--------------------------------------------------------------------------------

Standard stars in onedstds$oke1990/


bd284211 feige110 feige67 g191b2b g249 gd248 ltt9491 eg71

bd75325 feige34 g13831 g19374 gd108 hz21 eg158 eg247


--------------------------------------------------------------------------------

Standard stars in onedstds$redcal/


40erib eg63 eg139 eg248 gd140 hz44 ltt16294

amcvn eg67 eg144 feige24 gd190 l13633 ltt4099

bd7781 eg76 eg145 g12627 grw705824 l14094 ltt8702

bd73632 eg79 eg148 g14563 grw708247 l151234b ross627

bd174708 eg91 eg149 g16350 grw738031 l74546a ross640

bd262606 eg98 eg162 g191b2b hd19445 l93080 sa29130

eg20 eg99 eg182 g2610 hd84937 l97030 sao131065

eg33 eg102 eg184 g2631 he3 lds235b wolf1346

eg50 eg119 eg193 g4718 hz29 lds749b wolf485a

eg54 eg129 eg247 g9937 hz43 lft1655


--------------------------------------------------------------------------------

Standard stars in onedstds$spec16cal/:


Combined red and blue 3300A-10300A:


hd15318 hd74280 hd114330 hd188350 hd214923

hd30739 hd100889 hd129956 hd198001 hd224926

hr1544 hr4468 hr5501 hr7596 hr8634

hr3454 hr4963 hr718 hr7950 hr9087


Blue 3300A-7550A:


hd15318blue hd74280blue hd114330blue hd188350blue hd214923blue

hd30739blue hd100889blue hd129956blue hd198001blue hd224926blue

hr1544blue hr4468blue hr5501blue hr7596blue hr8634blue

hr3454blue hr4963blue hr718blue hr7950blue hr9087blue


Red 6020A-10300A:


hd15318red hd74280red hd114330red hd188350red hd214923red

hd30739red hd100889red hd129956red hd198001red hd224926red

hr1544red hr4468red hr5501red hr7596red hr8634red

hr3454red hr4963red hr718red hr7950red hr9087red


--------------------------------------------------------------------------------

Standard stars in onedstds$spec50cal/ (3200A - 8100 A)


bd284211 eg247 feige34 hd192281 pg0205134 pg0934554 wolf1346

cygob2no9 eg42 feige66 hd217086 pg0216032 pg0939262

eg139 eg71 feige67 hilt600 pg0310149 pg1121145

eg158 eg81 g191b2b hz14 pg0823546 pg1545035

eg20 feige110 gd140 hz44 pg0846249 pg1708602


Standard stars in onedstds$spec50cal/ (3200A - 10200A)


bd284211 eg247 feige34 g191b2b hz44

eg139 eg71 feige66 gd140 pg0823546

eg158 feige110 feige67 hilt600 wolf1346


--------------------------------------------------------------------------------

Standard stars in onedstds$spechayescal/


bd284211 eg139 feige67 hd217086 pg0216032 pg0939262

cygob2no9 eg158 feige110 hiltner600 pg0310149 pg1121145

eg42 eg247 g191b2b hz14 pg0823546 pg1545035

eg71 feige34 gd140 hz44 pg0846249 pg1708602

eg81 feige66 hd192281 pg0205134 pg0934554 wolf1346











110