A variationally computed line list for hot NH3

By Sergei N. Yurchenko, R. Barber, Jonathan Tennyson. 2010

293 citations recorded by the source corpus.

A B S T R A C T We present ‘BYTe’, a comprehensive ‘hot’ line list for the ro-vibrational transitions of ammonia, 14 NH 3, in its ground electronic state. This line list has been computed variationally using the program suite TROVE , a new spectroscopically determined potential energy surface and an ab initio dipole moment surface. BYTe, is designed to be used at all temperatures up to 1500 K. It comprises 1138 323 351 transitions in the frequency range from 0 to 12 000 cm −1 , constructed from 1373 897 energy levels below 18 000 cm −1 having J values ≤36. Comparisons with laboratory data confirm the accuracy of the line list which is suitable for modelling a variety of astrophysical problems including the atmospheres of extrasolar planets and brown dwarfs.

Subfields: Astronomy and Astrophysics, Instrumentation, Spectroscopy

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Citations in the corpus

A Population Study of Gaseous Exoplanets (2017, methodology): “We modeled the transmission spectra using a variety of possible molecular opacities, namely H2O, CH4, CO, CO2, NH3, TiO, and VO.”
Retrieving scattering clouds and disequilibrium chemistry in the atmosphere of HR 8799e (2020, methodology): “The following absorber species were included: CO, CO2 and H2O (from Rothman et al. 2010), CH4 (Yurchenko & Tennyson 2014), NH3 (Yurchenko et al. 2011), H2S (Rothman et al. 2013), Na and K (Piskunov et al. 1995, with Allard wings, see Mollière et al. 2019 for more details), PH3 (Sousa-Silva et al.…”
NEGLECTED CLOUDS IN T AND Y DWARF ATMOSPHERES (2012, background): “Recent work by Saumon et al. (2012) has modeled a range of brown dwarfs using improved line lists for ammonia from Yurchenko et al. (2011) and an improved treatment of the pressure-induced opacity of H2 collisions from Richard et al. (2012).”
ExoMol molecular line lists – XXXV. A rotation-vibration line list for hot ammonia (2019, background): “Notable amongst these are the BYTe line list of Yurchenko et al. (2011) and the HSL-pre3 line list (Huang & Lee 2013) of Sung et al. (2012).”
Total internal partition sums for 166 isotopologues of 51 molecules important in planetary atmospheres: Application to HITRAN2016 and beyond (2017, background): “[56] and those for (15)NH3 are from Yurchenko et al.”
Exoplanetary Atmospheres: Key Insights, Challenges, and Prospects (2019, background): “The spectral range of the HST WFC3 G141 grism of 1.1-1.7 µm contains strong spectral bands of key volatile species such as H2O, CH4, NH3, and HCN, making it a prime instrument for molecular spectroscopy of exoplanetary atmospheres.”
MASSES, RADII, AND CLOUD PROPERTIES OF THE HR 8799 PLANETS (2012, methodology): “First we use a new molecular line list for ammonia (Yurchenko et al. 2011).”
Mass–Metallicity Trends in Transiting Exoplanets from Atmospheric Abundances of H2O, Na, and K (2019, background): “…consider absorption due to H2O (Rothman et al. 2010), Na (Allard et al. 2019), K (Allard et al. 2016), CH4 (Yurchenko & Tennyson 2014), NH3 (Yurchenko et al. 2011), HCN (Barber et al. 2014), CO (Rothman et al. 2010), and H2-H2 and H2-He collision induced absorption (CIA; Richard et al.…”
H2O abundances and cloud properties in ten hot giant exoplanets (2018, methodology): “In particular, our CH4, HCN, and NH3 molecular line data are from EXOMOL (Tennyson et al. 2016; Yurchenko et al. 2011; Barber et al. 2014; Yurchenko & Tennyson 2014) and the line data for H2O, CO, and CO2 are obtained from HITEMP (Rothman et al. 2010).”
DETECTION OF AN ATMOSPHERE AROUND THE SUPER-EARTH 55 CANCRI E (2015, methodology): “The transmission spectra are generated using cross sections based on the line lists from ExoMol (Tennyson & Yurchenko 2012; Barber et al. 2006; Yurchenko et al. 2011; Barton et al. 2013; Yurchenko & Tennyson 2014; Barber et al. 2014), HITRAN (Rothman et al. 2009, 2013) and HITEMP (Rothman et al.…”
ExoMol: molecular line lists for exoplanet and other atmospheres (2012, methodology): “We have developed new procedures for this (Yurchenko et al. 2008, 2011b) which are both efficient and retain the predictive nature of the underlying ab initio PES. b. Post hoc by replacing calculated energy levels with observed ones.”
TAU-REX I: A NEXT GENERATION RETRIEVAL CODE FOR EXOPLANETARY ATMOSPHERES (2014, background): “…ExoMol provides computed line lists valid over extended temperature ranges for a variety of molecules including water (Barber et al. 2006), ammonia (Yurchenko et al. 2011), methane Yurchenko & Tennyson (2014) and a variety of diatomic molecules (Yadin et al. 2012; Barton et al. 2013; Barber et al.…”
GASEOUS MEAN OPACITIES FOR GIANT PLANET AND ULTRACOOL DWARF ATMOSPHERES OVER A RANGE OF METALLICITIES AND TEMPERATURES (2014, methodology): “For H2 CIA we use Richard et al. (2012) in place of previous work by Borysow (2002).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “This system allows for the user to choose, for the low temperature opacities, between either Ferguson et al. (2005) or Freedman et al. (2008) with updates to ammonia opacity from Yurchenko et al. (2011) and the pressureinduced opacity for molecular hydrogen from Frommhold et al. (2010).”