The links below point to a set
of directories containing molecular hydrogen absorption models, idl programs
and selected atomic and molecular data for the analysis of absorption lines
in FUSE and STIS spectra.
The content of these pages have been prepared by Stephan R. McCandliss at the request of potential users. He has no formal connected to the FUSE observatory, except as a guest-investigator. You are free to use and modify, for your own nefarious purpose, any programs you find here. By downloading you accept full responsibility for the risk and result. If you find something of use here, then a citation (see below) will be greatly appreciated -- SRM March 5, 2003.
Accepted by PASP 03-05-2003. H2ools reference.
(03-09-2003) Templates with v''<=3 are now available.
(02-06-2003) The directory structure below H2tautemplates has been reorganized to accommodate templates with v''>0.
(02-06-2003) I have determined that the b=1km/sec templates are undersampled with the current wavelength grid spacing of 0.01 Angstroms. The b=1km/sec templates should not be used for quantitative work. Here are how the equivalent widths, numerically integrated from the templates for a range of Nflambda, compare to theory for various doppler parameters. See the reference for details.
(04-30-2002) Byteswapped templates now available for those of you with linux machines courtesy of Pat Romano at Ohio State.
idl program listing
CAMMforPeter.pro-- is a main
program. It calls most of the other programs in this directory.
It won't work until you get all the data and procedure file names correctly
named. Imbedded within this program are calls to make a synthetic
spectrum. The program starts with a selected atlas model, which
is then attenuated with extinction by dust, and absorption by atomic and
molecular hydrogen. Orbital concatenations of individual FUSE
spectral segments are then joined after interpolating onto a common wavelength
A bigplot is then produced with the synthetic spectrum overlaid. Atomic and molecular
line positions are also overlaid. The bigplot is a postscript file and is best viewed with gv on unix machines. On other operating systems you will have to experiment.
ariread.pro -- and its friends feiiread.pro,
niiread.pro, etc... read in the Morton atomic data stored under the
. CAMMfor Peter.pro uses this information to overplot line identifications.
The data can also be used to compute an absorption line
spectrum for the given atomic species, but you will have to write it yourself.
atlas.pro -- reads in the Kurucz stellar models.
convolute.pro -- is used by newjoin.pro to find the segment shifts before joining the spectral segments.
fm.pro -- is a simple Fitzpatrick and Massa extinction routine.
h1abs.pro -- computes an atomic
hydrogen absorption spectrum and can handle
multiple velocity components.
h2data.pro -- reads in the molecular hydrogen data stored under h1h2data
h2label.pro -- does what h2data.pro does and then overplots a label with a tick marker proportional to the line core optical depth on a previously displayed plot. It is very useful for making molecular hydrogen line identifications.
hline.pro -- and its companion vline.pro is a program witten by Eric Burgh to overplot a horizontial (vertical) line on a previously displayed plot.
make_kernel.pro -- was written by Brian Wolven . It makes up a kernel for convolving
the synthetic spectrum to a desired FWHM.
new_join.pro -- Computes a weighted shifted average of all the spectral segments. Works pretty well but use caution.
rescol.pro -- produces a ten element
color table with the color indices of :
0=white, 1=brown, 2=red, 3=orange, 4=yellow, 5=green, 6=blue, 7=violet, 8=grey, 9=black