HIGH-RESOLUTION 1.6 {mu}m SPECTRA OF FeH IN M AND L DWARFS {sup ,}

Journal Article · Fri Oct 15 00:00:00 EDT 2010 · Astronomical Journal (New York, N.Y. Online)

DOI:https://doi.org/10.1088/0004-6256/140/4/919· OSTI ID:21443233

Hargreaves, Robert J; Bernath, Peter F ^[1]; Hinkle, Kenneth H ^[2]; Bauschlicher, Charles W ^[3]; Wende, Sebastian ^[4]; Seifahrt, Andreas ^[5]

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1. Department of Chemistry, University of York, Heslington, York, YO10 5DD (United Kingdom)
2. National Optical Astronomy Observatory, P.O. Box 26732, Tucson, AZ 85726 (United States)
3. NASA Ames Research Centre, Mailstop 230-3, Moffett Field, CA 94035 (United States)
4. Institut fuer Astrophysik, Georg-August-Universitaet Goettingen, Friedrich-Hund-Platz 1, 37077 Goettingen (Germany)
5. Department of Physics, University of California, One Shields Avenue, Davis, CA 95616 (United States)

Near-infrared bands due to the iron monohydride (FeH) molecule are a characteristic feature of late-M and -L dwarfs. We have created a line list at 2200 K for the FeH E {sup 4{Pi}}-A {sup 4{Pi}} electronic transition near 1.58 {mu}m (6300 cm{sup -1}) based on laboratory spectra and an ab initio calculation of the band strength. A variety of M and L dwarfs were observed near 1.6 {mu}m with high spectral resolution (R {approx} 70,000) using the Phoenix spectrograph on the 8.1 m Gemini South telescope. The FeH E-A transition made a surprisingly strong contribution to the observed spectral energy distributions and needs to be included in modeling of late-M and L dwarfs.

• OSTI ID: 21443233
• Journal Information: Astronomical Journal (New York, N.Y. Online), Vol. 140, Issue 4; Other Information: DOI: 10.1088/0004-6256/140/4/919; ISSN 1538-3881
• Country of Publication: United States
• Language: English

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