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

Robert J. Hargreaves; Kenneth H. Hinkle; Charles W. Bauschlicher; Sebastian Wende; Andreas Seifahrt; Peter F. Bernath

doi:10.1088/0004-6256/140/4/919

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

Robert J. Hargreaves, Kenneth H. Hinkle, Charles W. Bauschlicher, Sebastian Wende, Andreas Seifahrt, Peter F. Bernath

Chemistry

Research output: Contribution to journal › Article › peer-review

Abstract

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.

Original language	English
Pages (from-to)	919-924
Number of pages	6
Journal	ASTRONOMICAL JOURNAL
Volume	140
Issue number	4
DOIs	https://doi.org/10.1088/0004-6256/140/4/919
Publication status	Published - Oct 2010

Keywords

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

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10.1088/0004-6256/140/4/919

http://iopscience.iop.org/1538-3881/140/4/919/

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title = "HIGH-RESOLUTION 1.6 mu m SPECTRA OF FeH IN M AND L DWARFS",

abstract = "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.",

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

author = "Hargreaves, {Robert J.} and Hinkle, {Kenneth H.} and Bauschlicher, {Charles W.} and Sebastian Wende and Andreas Seifahrt and Bernath, {Peter F.}",

year = "2010",

month = oct,

doi = "10.1088/0004-6256/140/4/919",

language = "English",

volume = "140",

pages = "919--924",

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T1 - HIGH-RESOLUTION 1.6 mu m SPECTRA OF FeH IN M AND L DWARFS

AU - Hargreaves, Robert J.

AU - Hinkle, Kenneth H.

AU - Bauschlicher, Charles W.

AU - Wende, Sebastian

AU - Seifahrt, Andreas

AU - Bernath, Peter F.

PY - 2010/10

Y1 - 2010/10

N2 - 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.

AB - 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.

KW - brown dwarfs

KW - infrared: stars

KW - stars: individual (DENIS 1048-39, GJ 191, GJ 406, GJ 644C, LHS

KW - 292, LHS 2065, LHS 3003, LP 944-20, 2MASS J1507-16)

KW - stars: low-mass

KW - BASIS-SETS

KW - INFRARED SPECTRUM

KW - SKY SURVEY

KW - TRANSITION

KW - STARS

KW - ATOMS

KW - SUNSPOT

UR - http://www.scopus.com/inward/record.url?scp=78049286901&partnerID=8YFLogxK

U2 - 10.1088/0004-6256/140/4/919

DO - 10.1088/0004-6256/140/4/919

M3 - Article

SN - 0004-6256

VL - 140

SP - 919

EP - 924

JO - ASTRONOMICAL JOURNAL

JF - ASTRONOMICAL JOURNAL

IS - 4

ER -

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

Abstract

Keywords

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