Molecular line lists for modelling the opacity of cool stars

Tennyson, Jonathan; Harris, G. J.; Barber, R. J.; Delfa, S. La; Воронин, Б А; Kaminsky, B.; Pavlenko, Ya. V.

doi:10.1080/00268970701196983

Cited by 23 publications

(20 citation statements)

References 92 publications

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“…Furthermore, some of the lines observed in the high frequency end of the spectrum remained unassigned. However new HD 16 O calculations were subsequently provided by Tashkun [29] and by us [30], both based on the use of the PS potential energy [14] and dipole moment surfaces [15].…”

Section: Line Assignment and Energy Levels Derivationmentioning

confidence: 99%

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HDO absorption spectrum above 11500cm−1: Assignment and dynamics

Воронин

Naumenko

Carleer

et al. 2007

Journal of Molecular Spectroscopy

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Section: Line Assignment and Energy Levels Derivationmentioning

confidence: 99%

“…Our new calculations have been performed in Radau coordinates with the DVR3D program suite [31] and a large enough basis to obtain good convergence [30]. Calculations have been made for J 6 15 including all levels up to 25 600 cm À1 ; and for J < 3 the calculations extended up to 34 000 cm À1 .…”

Section: Line Assignment and Energy Levels Derivationmentioning

confidence: 99%

HDO absorption spectrum above 11500cm−1: Assignment and dynamics

Воронин

Naumenko

Carleer

et al. 2007

Journal of Molecular Spectroscopy

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“…We computed the profiles of the NaI and KI resonance doublets in the framework of a quasi-static approach described in Pavlenko et al (2007b) with an upgraded approach from Burrows et al (2003). We computed the CrH and FeH line lists from the work of Burrows et al (2002b) and Dulick et al (2003), respectively, while the water vapour line list was taken from Tennyson et al (2007). We considered the spectroscopic data for atomic absorption of the Vienna Atomic Line Database (VALD; Kupka et al 1999) 5 .…”

Section: Comparison With Theoretical Modelsmentioning

confidence: 99%

VLT X-Shooter spectroscopy of the nearest brown dwarf binary

Lodieu

Osorio

Rebolo

et al. 2015

A&A

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Aims. The aim of the project is to characterise the two components of the brown dwarf system nearest to the Sun, WISE J104915.57−531906.1 (also called Luhman 16AB) at optical and near-infrared wavelengths. Methods. We obtained high signal-to-noise intermediate-resolution (R ∼ 6000−11 000) optical (600−1000 nm) and near-infrared (1000−2480 nm) spectra of each component of Luhman 16AB with the X-Shooter instrument on the Very Large Telescope. Results. We classify the primary and secondary of the Luhman 16 system as L6−L7.5 and T0 ± 1, respectively, in agreement with previous measurements published in the literature. We present measurements of the lithium pseudo-equivalent widths, which appear of similar strength in both components (8.2 ± 1.0 Å for the L and 8.4 ± 1.5 Å for the T component). The presence of lithium ( 7 Li) in both components implies masses lower than 0.06 M , while the comparison with models suggests lower limits of 0.04 M . The detection of lithium in the T component is the first of its kind. Similarly, we assess the strength of other alkali lines (e.g. pseudoequivalent widths of 6−7 Å for RbI and 4−7 Å for CsI) present in the optical and near-infrared regions and compare with estimates for L and T dwarfs. We also derive effective temperatures and luminosities of each component of the binary: −4.66 ± 0.08 dex and 1305K for the L dwarf and −4.68 ± 0.13 dex and 1320K for the T dwarf. According to our radial velocity determinations, the binary does not appear to belong to any of the well-known moving group. Our preliminary theoretical analysis of the optical and J-band spectra indicates that the L-and T-type spectra can be reproduced with a single temperature and gravity but different relative chemical abundances, which strongly affects the spectral energy distribution of L/T transition objects.

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“…Unlike atoms, molecules have a large number of energy levels due to their rotational and vibrational states. Such energy levels lead to band structures where numerous individual transitions take place (Tennyson et al 2007). These individual transition features dominate the M dwarf's spectra at infrared wavelengths.…”

Section: Atomic Line Identification and Pseudo-equivalent Width Measumentioning

confidence: 99%

Intermediate Resolution Near-Infrared Spectroscopy of 36 Late M Dwarfs

Deshpande

Martín

Montgomery

et al. 2012

The Astronomical Journal

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We present observations of 36 late-M dwarfs obtained with the KeckII/NIRSPEC in the J-band at a resolution of ∼ 20,000. We have measured projected rotational velocities, absolute radial velocities, and pseudo-equivalent widths of atomic lines. 12 of our targets did not have previous measurements in the literature.For the other 24 targets, we confirm previously reported measurements. We find that 13 stars from our sample have v sin i below our measurement threshold (12 km s −1 ) whereas four of our targets are fast rotators (v sin i > 30 km s −1 ). As fast rotation causes spectral features to be washed out, stars with low projected rotational velocities are sought for radial velocity surveys.At our intermediate spectral resolution we have confirmed theidentification of neutral atomic lines reported in McLean et al. (2007). We also calculated pseudo-equivalent widths (p-EW) of 12 atomic lines. Our results confirm that the p-EW of K I lines are strongly dependent on spectral types. We observe that the p-EW of Fe I and Mn I lines remain fairly constant with later spectral type. We suggest that those lines are particularly suitable for deriving metallicities for late-M dwarfs.

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Molecular line lists for modelling the opacity of cool stars

Cited by 23 publications

References 92 publications

HDO absorption spectrum above 11500cm−1: Assignment and dynamics

HDO absorption spectrum above 11500cm−1: Assignment and dynamics

VLT X-Shooter spectroscopy of the nearest brown dwarf binary

Intermediate Resolution Near-Infrared Spectroscopy of 36 Late M Dwarfs

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