HIGH-RESOLUTION 1.6 μm SPECTRA OF FeH IN M AND L DWARFS

被引：38

作者：

Hargreaves, Robert J. ^{[1
]}

Hinkle, Kenneth H. ^{[2
]}

Bauschlicher, Charles W., Jr. ^{[3
]}

Wende, Sebastian ^{[4
]}

Seifahrt, Andreas ^{[5
]}

Bernath, Peter F. ^{[1
]}

机构：

[1] Univ York, Dept Chem, York YO10 5DD, N Yorkshire, England

[2] Assoc Univ Res Astron Inc, Natl Opt Astron Observ, Tucson, AZ 85726 USA

[3] NASA, Ames Res Ctr, Moffett Field, CA 94035 USA

[4] Univ Gottingen, Inst Astrophys, D-37077 Gottingen, Germany

[5] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

来源：

ASTRONOMICAL JOURNAL | 2010年 / 140卷 / 04期

基金：

美国国家科学基金会; 澳大利亚研究理事会; 英国科学技术设施理事会;

关键词：

brown dwarfs; infrared: stars; stars:; individual; (DENIS; 1048-39; GJ; 191; 406; 644C; LHS; 292; 2065; 3003; LP; 944-20; 2MASS J1507-16); stars: low-mass; BASIS-SETS; INFRARED SPECTRUM; SKY SURVEY; TRANSITION; STARS; ATOMS; SUNSPOT;

D O I：

10.1088/0004-6256/140/4/919

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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(4)Pi-A(4). electronic transition near 1.58 mu m (6300 cm(-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 similar to 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.

引用

页码：919 / 924

页数：6

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