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<div style="font-family:"Segoe UI",Helvetica,Arial,sans-serif"><span id="docs-internal-guid-86d1851e-9600-8d8e-733d-c5fa57d08efb"><span id="docs-internal-guid-9e838874-b9fd-c26f-7292-368ffed344e3">
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<div style="text-align:center"><span style="font-size:11pt; font-family:Cambria; background-color:rgb(255,255,255); vertical-align:baseline; white-space:pre-wrap"><span id="docs-internal-guid-748f50ce-f689-54d2-9b41-5a3c77a9e486"><span id="docs-internal-guid-44741882-f788-0e32-c8e8-2b168c3681ef"><span id="docs-internal-guid-d5bed97d-3f42-6ae7-0034-104ccf7b3897"><span id="docs-internal-guid-498729f8-679a-0a20-28d6-2d9b55698270">
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 28pt; color: rgb(192, 0, 0); background-color: transparent; font-weight: 700; vertical-align: baseline;">Spring 2018 Colloquium</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 16pt; background-color: transparent; font-weight: 700; vertical-align: baseline;">Department of Physics & Astronomy, TAMU-Commerce</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 16pt; color: rgb(192, 0, 0); background-color: transparent; font-weight: 700; vertical-align: baseline;">Mar 29, Thursday, 4-5 PM in Science Building 127</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 14pt; background-color: transparent; vertical-align: baseline;">(coffee and cookies will be served at 3:50 PM)</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 18pt; color: rgb(0, 176, 80); background-color: transparent; font-weight: 700; vertical-align: baseline;">Astronomy</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 18pt; color: rgb(0, 0, 255); background-color: transparent; font-weight: 700; vertical-align: baseline;">The HII Region Discovery Survey</span><span style="font-size: 18pt; color: rgb(0, 0, 255); background-color: transparent; font-weight: 700; vertical-align: baseline;"><br class="kix-line-break">
</span><span style="font-size: 14pt; background-color: transparent; font-weight: 700; vertical-align: baseline;">Dr. Dana Balser</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 14pt; background-color: transparent; font-weight: 700; vertical-align: baseline;">National Radio Astronomy Observatory</span></p>
<p dir="ltr" style="line-height: 1.38; margin-top: 0pt; margin-bottom: 0pt;"><span style="font-size: 14pt; background-color: transparent; font-weight: 700; vertical-align: baseline;"></span></p>
<img src="https://lh4.googleusercontent.com/iWedVqwtbo1hoSpAK7NS9U_uYq6GeuSaT_0CstAArUpfAsjlW4R6s05zRNz9lNc7TAnGGAF01zUVV2YC9rsWLXwPVwoai_yTVWDHRaBO8Jqv_6n_LgVTXt8E7XAqkbN91Q_mlesF" width="127" height="128" style="border: none; transform: rotate(0.00rad); -webkit-transform: rotate(0.00rad);">
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<span style="font-size: 11pt; font-family: Arial; vertical-align: baseline;">Dr. Balser earned his BS (1983) and MS (1986) degrees in Engineering Physics and Physics, respectively, at the University of Maine. He earned his Ph.D. degree (1994) in Astronomy
at Boston University studying the abundance of 3He in the Milky Way Galaxy. Dr. Balser was a Jansky postdoc (1994-1997) at the National Radio Astronomy Observatory (NRAO) in Green Bank, WV. In 1997, he became an assistant scientist at the NRAO and helped
to commission the GBT. In 2006, he moved to NRAO in Charlottesville, VA (headquarters) and is doing research in Galactic structure and abundances. More information about Dr. Balser and his research can be found at
</span><a href="https://urldefense.proofpoint.com/v2/url?u=http-3A__www.cv.nrao.edu_-7Edbalser_&d=DwMFAw&c=oqyuZuih6ykib6aKiBq22_bich4AVfYGoLertJN0bEc&r=hjwEO_XYlnwAQWUGeaCrW47w4mK-Al28-BKyRvaivBs&m=WzRIVzKd7LMOOo2fFRh-9tcG7c7RZmN4oHdwKdPQ4No&s=9HBhtHUdz8laAL87F37n72NdbsGdKrBCGnirS-ipveU&e=" style="text-decoration-line: none;"><span style="font-size: 11pt; font-family: Arial; color: rgb(17, 85, 204); text-decoration-line: underline; vertical-align: baseline;">www.cv.nrao.edu/~dbalser/</span></a><span style="font-size: 11pt; font-family: Arial; vertical-align: baseline;">.</span><span style="font-size: 11pt; vertical-align: baseline;">
</span></p>
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<span style="font-size: 11pt; background-color: transparent; vertical-align: baseline;"></span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:4pt;"><span style="font-size: 12pt; background-color: transparent; font-weight: 700; vertical-align: baseline;">Abstract</span></p>
<p dir="ltr" style="line-height:1.38;margin-top:0pt;margin-bottom:0pt;text-align: justify;">
<span style="font-size: 12pt; font-family: Arial; vertical-align: baseline;">HII regions are zones of ionized gas surrounding massive, bright stars. They are the most luminous objects in the Milky Way at mid-infrared to radio wavelengths and can be seen across
the entire Galactic disk. They are the archetypical tracers of Galactic spiral structure. Because of their short lifetimes their chemical abundances indicate the present state of the interstellar medium and reveal the elemental enrichment caused by the nuclear
processing of many stellar generations. The HII Region Discovery Survey (HRDS) uses primarily the Green Bank Telescope (GBT) and the Australia Telescope Compact Array (ATCA) to observe radio recombination line (RRL) and continuum emission to detect new HII
regions. The goal is to increase the sample of HII regions across the Galactic disk. The HRDS strategy,
</span><span style="font-family: Arial; font-size: 12pt;">status, and preliminary results will be discussed.</span></p>
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