Line Intensities and Molecular Opacities of the FeH F 4Δi-X 4Δi Transition

By M. Dulick, C. Bauschlicher, Adam Burrows, C. Sharp, R. S. Ram, P. F. Bernath. 2003

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We calculate new line lists and opacities for the F 4Δi-X 4Δi transition of FeH. The 0-0 band of this transition is responsible for the Wing-Ford band seen in M-type stars, sunspots, and brown dwarfs. The new Einstein A-values for each line are based on a high-level ab initio calculation of the electronic transition dipole moment. The necessary rotational line strength factors (Hönl-London factors) are derived for both the Hund's case (a) and (b) coupling limits. A new set of spectroscopic constants was derived from the existing FeH term values for v = 0, 1, and 2 levels of the X and F states. Using these constants, extrapolated term values were generated for v = 3 and 4 and for J-values up to 50.5. The line lists (including Einstein A-values) for the 25 vibrational bands with v ≤ 4 were generated using a merged list of experimental and extrapolated term values. The FeH line lists were used to compute the molecular opacities for a range of temperatures and pressures encountered in L and M dwarf atmospheres. Good agreement was found between the computed and observed spectral energy distribution of the L5 dwarf 2MASS-1507.

Subfields: Atmospheric Science, Atomic and Molecular Physics, and Optics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/6a05291ef5e639b68c5e330a6ac880564539a718

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Citations in the corpus

Line and Mean Opacities for Ultracool Dwarfs and Extrasolar Planets (2007, methodology): “We rely on lists tabulated by Dulick et al. (2003) and discussed in more detail by Sharp & Burrows (2007).”
THE SDSS-III APOGEE SPECTRAL LINE LIST FOR H-BAND SPECTROSCOPY (2015, methodology): “FeH For DR12, several FeH line lists were tested, including lines from Langhoff & Bauschlicher (1990) as implemented in the Uppsala spectral synthesis code BSYN, and Dulick et al. (2003) as implemented by Kurucz in fehfx.asc (Kurucz web site, http://kurucz.harvard.edu/molecules/).”
The Spectra of T Dwarfs. II. Red Optical Data (2003, background): “While opacity data from Burrows et al. (2002b) clearly show a CrH band head at this wavelength, its visibility depends on the relative abundance of CrH to FeH, as their opacities are roughly equal in strength at these wavelengths (Dulick et al. 2003).”
The First Substellar Subdwarf? Discovery of a Metal-poor L Dwarf with Halo Kinematics (2003, background): “The J-band spectrum, shown in detail in Figure 2b, is far more rich, with atomic lines of K i (1.1690, 1.1773, 1.2543, and 1.2522 lm) and Fe i (1.1528, 1.1886, 1.1976, 1.2128, and 1.3210 lm), and strong molecular bands of FeH (1.194 and 1.239 lm) and H2O (1.3 lm) observed.”
An Infrared Spectroscopic Sequence of M, L, and T Dwarfs (2004, background): “…effect may occur in the J band since the 0–1 band of FeH at 1.19 m is strong in the spectra of L dwarfs (Cushing et al. 2003; McLean et al. CUSHING, RAYNER, & VACCA1122 Vol. 623 2003) and the cross sections of CrH and FeH are also approximately equal at these wavelengths (Dulick et al. 2003).”
ExoMol: molecular line lists for exoplanet and other atmospheres (2012, methodology): “In the case of FeH Dulick et al. (2003) present results on rovibronic transitions within the F 4∆ –”
GASEOUS MEAN OPACITIES FOR GIANT PLANET AND ULTRACOOL DWARF ATMOSPHERES OVER A RANGE OF METALLICITIES AND TEMPERATURES (2014, unknown): “…(1994); HITRAN’08a isotopes;b CO HITEMP’10c; Tipping (1976) CO2 Huang et al. (2014); Huang et al. (2013) CrH Burrows et al. (2002) FeH Dulick et al. (2003); Hargreaves et al. (2010) H2O Partridge & Schwenke (1997); Gamache et al. (1998); HITRAN’08a isotopes H2S Kissel et al.…”
COUNTING LOW-MASS STARS IN INTEGRATED LIGHT (2011, methodology): “The FeH linelist is from the work of Dulick et al. (2003), but with a partition function tabulated by Kurucz specifically for this project.”
Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres (2006, methodology): “Table 1 lists the species considered in this work and gives the sections where the species are discussed in detail, including several condensates addressed with the Mie theory.”
L and T Dwarf Models and the L to T Transition (2005, background): “Though theorists have gradually responded to this challenge (Partridge & Schwenke 1997; Burrows et al. 2002a; Dulick et al. 2003; Burrows & Volobuyev 2003), their remain significant deficits in the relevant molecular databases.”
The effective temperature scale of M dwarfs (2013, methodology): “…line list computed by Barber et al. (2006), TiO, VO, CaH line lists by Plez (1998), MgH by (Weck et al. 2003, Story et al. 2003), FeH and CrH by (Dulick et al. 2003, Chowdhury et al. 2006), NH3 by Yurchenko et al. (2011), CO2 (Tashkun et al. 2004), and H2 Collision Induced Absorption (CIA) by…”