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A Masing BAaDE’s Window

Published online by Cambridge University Press:  30 December 2019

Lorant O. Sjouwerman ,
Ylva M. Pihlström ,
Adam C. Trapp ,
Michael C. Stroh ,
Luis Henry Quiroga-Nuñez ,
Megan O. Lewis Open the ORCID record for Megan O. Lewis [Opens in a new window] ,
R. Michael Rich ,
Mark R. Morris Open the ORCID record for Mark R. Morris [Opens in a new window] ,
Huib Jan van Langevelde  and
Mark J Claussen
...Show all authors
Lorant O. Sjouwerman
Affiliation:
National Radio Astronomy ObservatoryP.O. Box O, Socorro, NM, U.S.A. email: lsjouwer@nrao.edu
Ylva M. Pihlström
Affiliation:
University of New Mexico, Albuquerque NM, USA
Adam C. Trapp
Affiliation:
University of California, Los Angeles CA, USA
Michael C. Stroh
Affiliation:
University of New Mexico, Albuquerque NM, USA
Luis Henry Quiroga-Nuñez
Affiliation:
Leiden Observatory, Leiden & Joint Institute for VLBI ERIC, Dwingeloo, The Netherlands
Megan O. Lewis
Affiliation:
University of New Mexico, Albuquerque NM, USA
R. Michael Rich
Affiliation:
University of California, Los Angeles CA, USA
Mark R. Morris
Affiliation:
University of California, Los Angeles CA, USA
Huib Jan van Langevelde
Affiliation:
Leiden Observatory, Leiden & Joint Institute for VLBI ERIC, Dwingeloo, The Netherlands
Mark J Claussen
Affiliation:
National Radio Astronomy ObservatoryP.O. Box O, Socorro, NM, U.S.A. email: lsjouwer@nrao.edu
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Abstract

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We report on the Bulge Asymmetries and Dynamic Evolution (BAaDE) survey which has observed 19 000 MSX color selected red giant stars for SiO maser emission at 43 GHz with the VLA and is in the process of observing 9 000 of these stars with ALMA at 86 GHz in the Southern sky. Our setup covers the main maser transitions, as well as those of isotopologues and selected lines of carbon-bearing species. Observations of this set of lines allow a far-reaching catalog of line-of-sight velocities in the dust-obscured regions where optical surveys cannot reach. Our preliminary detection rate is close to 70%, predicting a wealth of new information on the distribution of metal rich stars, their kinematics as function of location in the Galaxy, as well as the occurrence of lines and line ratios between the different transitions in combination with the spectral energy distribution from about 1 to 100 μm. Similar to the OH/IR stars, a clear kinematic signature between disk and bulge stars can be seen. Furthermore, the SiO J = →10 (v=3) line plays a prominent role in the derived maser properties.

Keywords

maserssurveysstars: late-typeGalaxy: kinematics and dynamicsinfrared: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 14 , Symposium S343: Why Galaxies Care About AGB Stars: A Continuing Challenge through Cosmic Time , August 2018 , pp. 334 - 337
Copyright
© International Astronomical Union 2019 

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