Large format heterodyne arrays for observing far-infrared lines with SOFIA

C. Walker, C. Kulesa, J. Kloosterman, D. Lesser, T. Cottam, Christopher Groppi, J. Zmuidzinas, M. Edgar, S. Radford, P. Goldsmith, W. Langer, H. Yorke, J. Kawamura, I. Mehdi, D. Hollenbach, J. Stutzki, H. Huebers, J. R. Gao, C. Martin

Research output: Chapter in Book/Report/Conference proceedingConference contribution

3 Scopus citations

Abstract

In the wavelength regime between 60 and 300 microns there are a number of atomic and molecular emission lines that are key diagnostic probes of the interstellar medium. These include transitions of [CII], [NII], [OI], HD, H 2D+, OH, CO, and H2O, some of which are among the brightest global and local far-infrared lines in the Galaxy. In Giant Molecular Clouds (GMCs), evolved star envelopes, and planetary nebulae, these emission lines can be extended over many arc minutes and possess complicated, often self absorbed, line profiles. High spectral resolution (R> 105) observations of these lines at sub-arcminute angular resolution are crucial to understanding the complicated interplay between the interstellar medium and the stars that form from it. This feedback is central to all theories of galactic evolution. Large format heterodyne array receivers can provide the spectral resolution and spatial coverage to probe these lines over extended regions. The advent of large format (~100 pixel) spectroscopic imaging cameras in the far-infrared (FIR) will fundamentally change the way astronomy is performed in this important wavelength regime. While the possibility of such instruments has been discussed for more than two decades, only recently have advances in mixer and local oscillator technology, device fabrication, micromachining, and digital signal processing made the construction of such instruments tractable. These technologies can be implemented to construct a sensitive, flexible, heterodyne array facility instrument for SOFIA. The instrument concept for StratoSTAR: Stratospheric Submm/THz Array Receiver includes a common user mounting, control system, IF processor, spectrometer, and cryogenic system. The cryogenic system will be designed to accept a frontend insert. The frontend insert and associated local oscillator system/relay optics would be provided by individual user groups and reflect their scientific interests. Rapid technology development in this field makes SOFIA the ideal platform to operate such a modular, continuously evolving instrument.

Original languageEnglish (US)
Title of host publicationMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V
DOIs
StatePublished - 2010
EventMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V - San Diego, CA, United States
Duration: Jun 29 2010Jul 2 2010

Publication series

NameProceedings of SPIE - The International Society for Optical Engineering
Volume7741
ISSN (Print)0277-786X

Other

OtherMillimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V
CountryUnited States
CitySan Diego, CA
Period6/29/107/2/10

Keywords

  • SOFIA
  • TeraHertz
  • array receiver
  • heterodyne
  • submillimeter

ASJC Scopus subject areas

  • Electronic, Optical and Magnetic Materials
  • Condensed Matter Physics
  • Computer Science Applications
  • Applied Mathematics
  • Electrical and Electronic Engineering

Fingerprint Dive into the research topics of 'Large format heterodyne arrays for observing far-infrared lines with SOFIA'. Together they form a unique fingerprint.

  • Cite this

    Walker, C., Kulesa, C., Kloosterman, J., Lesser, D., Cottam, T., Groppi, C., Zmuidzinas, J., Edgar, M., Radford, S., Goldsmith, P., Langer, W., Yorke, H., Kawamura, J., Mehdi, I., Hollenbach, D., Stutzki, J., Huebers, H., Gao, J. R., & Martin, C. (2010). Large format heterodyne arrays for observing far-infrared lines with SOFIA. In Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V [77410Z] (Proceedings of SPIE - The International Society for Optical Engineering; Vol. 7741). https://doi.org/10.1117/12.857811