------------------------------------------------------------------------
From: Robert Blum  blum@ctiowe.ctio.noao.edu 
Mime-Version: 1.0
To: gcnews@aoc.nrao.edu
Subject: submit srgd.abs to appear in the ApJ Feb 1999



------------- End Forwarded Message -------------

%astro-ph/9809345
%http://www.ctio.noao.edu/ftp/pub/blum/sgrd.ps
%\documentstyle[12pt,aasms4]{article}
 \documentstyle[12pt,aaspp4]{article}
%\tighten

\begin{document}

% ---------------defos-----------------------------------------------------

\def\zz{\hang\noindent}

\def\kms{km s$^{-1}$}
\def\pix{pix$^{-1}$}
\def\deg{$^\circ$}

\def\mic{{$\mu$m}}

\def\h2o{H$_2$O}

\def\ak{{\it $A_K$}}

\def\teff{$T_{\rm eff}$}

\def\aple{$\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$
}
\def\apge{$\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}}$
}

%TABLES
%\begin{table}
%\dummytable\label{stars}
%\end{table}

%\vglue 1.5in
% -------------------------------------------------------------------------

\title{2 \mic \ Narrow--Band Imaging of the Sagittarius D H~II Region}

\author{R. D. Blum\altaffilmark{1}} 
\affil{Cerro Tololo Interamerican Observatory, Casilla 603, La Serena, Chile\\
rblum@noao.edu}

\author{A. Damineli\altaffilmark{2}}
\affil{JILA, University of Colorado\\Campus Box 440, Boulder, CO,
80309\\damineli@casa.colorado.edu}

\altaffiltext{1}{Hubble Fellow}
\altaffiltext{2}{Permanent address: IAG-USP, Av. Miguel Stefano 4200, 
04301-904, Sao Paulo, Brazil}

%\centerline{{\it submitted for publication in the} ApJ}

\begin{abstract}
We present 2 \mic \ narrow--band images of the core H~II region in the
Galactic star forming region Sagittarius D. The emission--line images
are centered on 2.17 \mic \ (Br$\gamma$) and 2.06 \mic \ (He~I). The H~II
region appears at the edge of a well defined dark cloud, and the
morphology suggests a blister geometry as pointed out 
in earlier radio continuum work. There is a deficit of
stars in general in front of the associated dark cloud
indicating the H~II region is located in-between the
Galactic center and the sun. The lesser spatial extent of the He~I
line emission relative to Br$\gamma$ places the effective
temperature of the ionizing radiation field below 40,000~K. The He~I 
2.06 \mic \ to Br$\gamma$ ratio and Br$\gamma$ / far infrared dust
emission put \teff \ at about 36,500~K to 40,000~K 
as derived from ionization models.

\end{abstract}

--Herd_of_Hippopotamuses_250_000
Content-Type: TEXT/plain; name="gcnews.abs"; charset=us-ascii
Content-Description: gcnews.abs
Content-MD5: zZGy/EYg6i0gQzWFdmy0Hw==

%astro-ph/9809345
%http://www.ctio.noao.edu/ftp/pub/blum/sgrd.ps
%\documentstyle[12pt,aasms4]{article}
 \documentstyle[12pt,aaspp4]{article}
%\tighten

\begin{document}

% ---------------defos-----------------------------------------------------

\def\zz{\hang\noindent}

\def\kms{km s$^{-1}$}
\def\pix{pix$^{-1}$}
\def\deg{$^\circ$}

\def\mic{{$\mu$m}}

\def\h2o{H$_2$O}

\def\ak{{\it $A_K$}}

\def\teff{$T_{\rm eff}$}

\def\aple{$\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$<$}}}$
}
\def\apge{$\mathrel{\hbox{\rlap{\hbox{\lower4pt\hbox{$\sim$}}}\hbox{$>$}}}$
}

%TABLES
%\begin{table}
%\dummytable\label{stars}
%\end{table}

%\vglue 1.5in
% -------------------------------------------------------------------------

\title{2 \mic \ Narrow--Band Imaging of the Sagittarius D H~II Region}

\author{R. D. Blum\altaffilmark{1}} 
\affil{Cerro Tololo Interamerican Observatory, Casilla 603, La Serena, Chile\\
rblum@noao.edu}

\author{A. Damineli\altaffilmark{2}}
\affil{JILA, University of Colorado\\Campus Box 440, Boulder, CO,
80309\\damineli@casa.colorado.edu}

\altaffiltext{1}{Hubble Fellow}
\altaffiltext{2}{Permanent address: IAG-USP, Av. Miguel Stefano 4200, 
04301-904, Sao Paulo, Brazil}

%\centerline{{\it submitted for publication in the} ApJ}

\begin{abstract}
We present 2 \mic \ narrow--band images of the core H~II region in the
Galactic star forming region Sagittarius D. The emission--line images
are centered on 2.17 \mic \ (Br$\gamma$) and 2.06 \mic \ (He~I). The H~II
region appears at the edge of a well defined dark cloud, and the
morphology suggests a blister geometry as pointed out 
in earlier radio continuum work. There is a deficit of
stars in general in front of the associated dark cloud
indicating the H~II region is located in-between the
Galactic center and the sun. The lesser spatial extent of the He~I
line emission relative to Br$\gamma$ places the effective
temperature of the ionizing radiation field below 40,000~K. The He~I 
2.06 \mic \ to Br$\gamma$ ratio and Br$\gamma$ / far infrared dust
emission put \teff \ at about 36,500~K to 40,000~K 
as derived from ionization models.

\end{abstract}

--Herd_of_Hippopotamuses_250_000--