The near-infrared spectrum of the FeH molecule

Phillips, J. G.; Davis, Sumner P.; Lindgren, B.; Balfour, Walter J.

doi:10.1086/191241

Cited by 89 publications

(85 citation statements)

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“…The J band spectra are dominated by two broad molecular absorptions of H 2 O shortward of 1.17 µm and longward of 1.33 µm (Auman 1967), and by FeH at 1.194 µm and 1.239 µm (Phillips et al 1987). We have also retrieved several narrow absorptions of FeH in the spectra of TWA 22 AB, TWA 5B, KPNO Tau 4, OTS 44, 2M0141, USco CTIO 108B, CT Cha b, HR7329 B, AB Pic b, and Gl 417 B that were previously identified in the spectra of field M-L dwarfs (Cushing et al 2003).…”

Section: Line Identificationmentioning

confidence: 98%

A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy

Chauvin

Lagrange

et al. 2014

A&A

142

204

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Context. At young ages, low surface gravity affects the atmospheric properties of ultracool dwarfs. The impact on medium-resolution near-infrared (NIR) spectra has only been slightly investigated at the M-L transition so far. Aims. We present a library of NIR (1.1-2.45 µm) medium-resolution (R ∼ 1500-2000) integral field spectra of 15 young M6−L0 dwarfs. We aim at deriving updated NIR spectral type, luminosity, and physical parameters (T eff , log g, M, L/L ) for each source. This work also aims at testing the latest generation of BT-SETTL atmospheric models. Methods. We estimated spectral types using spectral indices and the spectra of young objects classified in the optical. We used the 2010 and 2012 releases of the BT-SETTL synthetic spectral grid and cross-checked the results with the DRIFT-PHOENIX models to derive the atmospheric properties of the sources. Results. We do not find significant differences between the spectra of young companions and those of young isolated brown dwarfs in the same spectral type range. We derive infrared spectral types L0 ± 1, L0 ± 1, M9.5 ± 0.5, M9.5 ± 0.5, M9.25 ± 0.25, M8 +0.5 −0.75 , and M8.5 ± 0.5 for AB Pic b, Cha J110913-773444, USco CTIO 108B, GSC 08047-00232 B, DH Tau B, CT Cha b, and HR7329B, respectively. The BT-SETTL and DRIFT-PHOENIX models yield close T eff and log g estimates for each source. The models seem to show a 600 +600 −300 K drop in the effective temperature at the M-L transition. Assuming the former temperatures are correct, we then derive new mass estimates that confirm that DH Tau B, USco CTIO 108B, AB Pic b, KPNO Tau 4, OTS 44, and Cha1109 lie inside or at the boundary of the planetary mass range. We combine the empirical luminosities of the M9.5-L0 sources to the T eff to derive semi-empirical radii estimates that do not match "hot-start" evolutionary models predictions at 1-3 Myr. We use complementary data to demonstrate that atmospheric models are able to reproduce the combined optical and infrared spectral energy distribution, together with the NIR spectra of these sources simultaneously. But the models still fail to represent the dominant features in the optical. This issue raises doubts on the ability of these models to predict effective temperatures from NIR spectra alone. Conclusions. The library provides templates for characterizing other young and late type objects. The study advocates the use of photometric and spectroscopic information over a broad range of wavelengths to study the properties of very low-mass young companions to be detected with the planet imagers (Subaru/SCExAO, LBT/LMIRCam, Gemini/GPI, VLT/SPHERE).

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Section: Line Identificationmentioning

confidence: 98%

A library of near-infrared integral field spectra of young M–L dwarfs

Bonnefoy

Chauvin

Lagrange

et al. 2014

A&A

142

204

View full text Add to dashboard Cite

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“…It was clear from our test syntheses that the DR13 line list could not match well several features in the observed spectra of the target stars. To investigate if the unmatched features were due to FeH, we first tested the line list from Phillips et al (1987) that includes the vibration-rotation transition of the FeH D D 44 -system. The computed FeH lines from this line list were weak and did not improve the matching of the observed spectra.…”

Section: Enhancements To the Apogee Line List For The Study Of M-dwarfsmentioning

confidence: 99%

Chemical Abundances of M-Dwarfs from the Apogee Survey. I. The Exoplanet Hosting Stars Kepler-138 and Kepler-186

Souto

Cunha

García–Hernández

et al. 2017

ApJ

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We report the first detailed chemical abundance analysis of the exoplanet-hosting M-dwarf stars Kepler-138 and Kepler-186 from the analysis of high-resolution (R∼22,500) H-band spectra from the SDSS-IV-APOGEE survey. Chemical abundances of 13 elements-C, O, Na, Mg, Al, Si, K, Ca, Ti, V, Cr, Mn, and Fe-are extracted from the APOGEE spectra of these early M-dwarfs via spectrum syntheses computed with an improved line list that takes into account H 2 O and FeH lines. This paper demonstrates that APOGEE spectra can be analyzed to determine

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“…Seven infra-red bands of the 4 ∆− 4 ∆ system of the FeH molecule were analyzed by Phillips et al (1987) (The rms of the deviations between observed and calculated lines was 0.01 cm −1 ). Their wavenumber ranges are listed in Table 1 in order of the wavelength of the heads.…”

Section: Molecular Datamentioning

confidence: 99%

“…The presence of a molecular band in the umbral spectrum shows up as a peak above the noise produced by random coincidences. All known FeH bands (Phillips et al 1987) within the spectral range of the present umbral spectrum were checked with this procedure (Fawzy 1995). A slightly different version of this method was developed and used by Lambert (1988).…”

Section: Feh Solar Identificationmentioning

confidence: 99%