Tripp abstract for UNLV lab astrophysics meeting

[tripp@fcrao1.astro.umass.edu]

Hello again.

  Here is the abstract for my talk at the upcoming lab astrophysics 
meeting.  I have used the latex template, and I have assumed that simple 
latex commands can be embedded in the abstract.

  The abstract is attached and is also appended in the main email body 
(see below).  Please let me know if you encounter any problems with the 
abstract.

Thanks!
Todd Tripp

=======================================================================
ABSTRACT (Latex)

%
% Sample abstract for submission to NASA LAW 2006.
% See page 181-183 of Leslie Lamport's LaTeX book (second edition)
% for more info.
%
\documentclass{article}

\begin{document}

\title{Ultraviolet and X-ray Spectroscopy of Multiphase Hot Gas in the
Interstellar Medium and the IGM}

\author{Todd M. Tripp, University of Massachusetts}

\date{6 January 2006}

\maketitle

\begin{abstract}
The Space Telescope Imaging Spectrograph and the {\it Far Ultraviolet
Spectroscopic Explorer} have observed a large number of hot stars and
low-redshift QSOs and AGNs for the purpose of studying interstellar
and intergalactic gases and their roles in galaxy evolution and
cosmology. The spectra of these objects show an array of remarkable
absorption lines ranging from cold, molecular gas (e.g., traced by C~I
and H$_{2}$) to highly ionized and hot gas (e.g., traced by O~VI and
Ne~VIII transitions). Many of the gas clouds detected in UV absorption
cannot be studied by any other technique, especially in intergalactic
regions where the densities are likely to be quite low. The O~VI
absorption lines detected in intervening gas clouds have particularly
important implications regarding the chemical enrichment, physical
conditions, and baryonic content of intergalactic gas in the nearby
universe. For example, these absorbers can be used to search for the
``warm-hot intergalactic medium'', a shock-heated phase of the IGM
that is theoretically predicted to be a major baryon reservoir at the
present epoch. In parallel, X-ray telescopes with grating
spectrographs have detected absorption lines of even more highly
ionized species (e.g., O~VII and Ne~IX) that complement the UV
studies. This talk will briefly review studies of the low-z IGM based
on UV and X-ray observations of O~VI and related absorption lines,
including findings on the metallicity, ionization, and cosmological
mass of these systems as well as their relationships with galaxies.
Comments will be interspersed about how these science programs require
and motivate supporting work from laboratory astrophysics.
\end{abstract}

\end{document}
%
% Sample abstract for submission to NASA LAW 2006.
% See page 181-183 of Leslie Lamport's LaTeX book (second edition)
% for more info.
%
\documentclass{article}

\begin{document}

\title{Ultraviolet and X-ray Spectroscopy of Multiphase Hot Gas in the
Interstellar Medium and the IGM}

\author{Todd M. Tripp, University of Massachusetts}

\date{6 January 2006}

\maketitle

\begin{abstract}
The Space Telescope Imaging Spectrograph and the {\it Far Ultraviolet
Spectroscopic Explorer} have observed a large number of hot stars and
low-redshift QSOs and AGNs for the purpose of studying interstellar
and intergalactic gases and their roles in galaxy evolution and
cosmology. The spectra of these objects show an array of remarkable
absorption lines ranging from cold, molecular gas (e.g., traced by C~I
and H$_{2}$) to highly ionized and hot gas (e.g., traced by O~VI and
Ne~VIII transitions). Many of the gas clouds detected in UV absorption
cannot be studied by any other technique, especially in intergalactic
regions where the densities are likely to be quite low. The O~VI
absorption lines detected in intervening gas clouds have particularly
important implications regarding the chemical enrichment, physical
conditions, and baryonic content of intergalactic gas in the nearby
universe. For example, these absorbers can be used to search for the
``warm-hot intergalactic medium'', a shock-heated phase of the IGM
that is theoretically predicted to be a major baryon reservoir at the
present epoch. In parallel, X-ray telescopes with grating
spectrographs have detected absorption lines of even more highly
ionized species (e.g., O~VII and Ne~IX) that complement the UV
studies. This talk will briefly review studies of the low-z IGM based
on UV and X-ray observations of O~VI and related absorption lines,
including findings on the metallicity, ionization, and cosmological
mass of these systems as well as their relationships with galaxies.
Comments will be interspersed about how these science programs require
and motivate supporting work from laboratory astrophysics.
\end{abstract}

\end{document}