Computer Science
Scientific paper
Sep 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004sptz.prop.3423m&link_type=abstract
Spitzer Proposal ID #3423
Computer Science
Scientific paper
Outflows from young stellar objects are the most prominent signs of star formation. Unfortunately, the connection between the strength of the ouflow and the properties of the driving source is not fully understood, and remains an area of intense study. Outflows also drive shocks that can significantly alter the composition of the gas into which they propagate. However, the chemical changes they induce are a sensitive function of the shock velocity and pre-shock density. Because the IRS instrument provides access to a variety of low-lying rotational lines of H2, ground-state rotational transitions of H2O, and several atomic and ionic fine-structure lines, it is particularly well-suited to study these problems. Specifically, we propose to use the H2 S(0) through S(5) lines to obtain the shock luminosity to compare with the mechanical luminosity and the protostellar models of six well-studied outflow sources. Use of these mid-IR H2 lines greatly reduces the uncertainties in the derived luminosity resulting from poorly known extinction corrections. Simultaneously, we propose to use the H2, H2O, [FeI], [SI], [FeII], and [SiII] lines in the IRS band to study the spatial distribution of any fast dissociative and slower non-dissociative shocks that may be present. The high spatial resolution of the IRS will permit us to better determine the filling factor and abundance of hot water in these sources -- something that was not possible with the lower angular resolution of ISO and SWAS. For each of the observed sources we will carry out mapping observations in a ~1'x1' field centered on one lobe of each outflow. The observations will be performed using the IRS in spectral mapping mode. This includes use of the Short-Lo, Short-Hi, and Long-Hi modules to obtain complete coverage throughout the 5.3 - 37.0 micron spectral region. The sensitivity obtained will exceed that possible from an ambient temperature telescope by several orders of magnitude and will allow the detection of all of the key diagnostics.
Bergin Edwin
Forrest William
Kaufman Michael
Melnick G. G.
Neufeld David
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