HITEMP, the high-temperature molecular spectroscopic database

By L. Rothman, I. Gordon, R. Barber, H. Dothe, Robert R. Gamache, Aaron Goldman, V. Perevalov, S. Tashkun, Jonathan Tennyson. 2010

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Subfields: Atmospheric Science, Spectroscopy

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Citations in the corpus

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. 2012).”
Total internal partition sums for 166 isotopologues of 51 molecules important in planetary atmospheres: Application to HITRAN2016 and beyond (2017, background): “Comparing Q(296 K) for (12)C(16)O2 with the CDSD value and the UCL value [48] gives 0.”
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 carbon monoxide in the high-resolution day-side spectrum of the exoplanet HD 189733b (2013, methodology): “Line data for the trace gases are taken from HITEMP 2010 for H2O and CO (Rothman et al. 2010), HITRAN 2008 for CH4 (Rothman et al. 2009) and HITEMP 1995 for CO2 (Rothman et al. 1995).”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, background): “It is a program to produce high-resolution spectrum of any gas mixture, in any thermodynamical conditions, from line-by-line (LBL) databases such as HITRAN 2008 (Rothman et al. 2009) and HITEMP 20104 (Rothman et al. 2010).”
CDSD-4000: High-resolution, high-temperature carbon dioxide spectroscopic databank (2011, methodology): “An enhanced and enlarged version of CDSD-1000 is a part of new version of the HITEMP database [20].”
HD 209458b in new light: evidence of nitrogen chemistry, patchy clouds and sub-solar water (2017, methodology): “We consider the main chemical species regarded as spectrally active between 0.3−1.7µm in hot Jupiter atmospheres: H2, He, H2O, CH4, NH3, HCN, CO, CO2, Na and K (Seager & Sasselov 2000; Madhusudhan et al. 2016c).”
An Accurate, Extensive, and Practical Line List of Methane for the HITEMP Database (2020, methodology): “Data from the ExoMol group are regularly used to update the HITRAN and HITEMP databases (Rothman et al. 2010; Gordon et al. 2017; Hargreaves et al. 2019) because the ab initio intensities for some molecules are of exceptional quality.”
Exoplanet Biosignatures: A Review of Remotely Detectable Signs of Life (2017, methodology): “, 2013), HITEMP (Rothman et al., 2010), or ExoMol (Tennyson and Yurchenko, 2012) is used to query line parameters for gases included in the model and calculate absorption cross sections.”
ROVIBRATIONAL LINE LISTS FOR NINE ISOTOPOLOGUES OF THE CO MOLECULE IN THE X1Σ+ GROUND ELECTRONIC STATE (2015, methodology): “At 3000 K, the Q values from the present study are in excellent agreement with the ones derived by Goorvitch, while the value used in the HITRAN and HITEMP databases are approximately 0.18% larger than the present study.”
The ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2016, background): “The latest, 2010, release [76] only contained data on 5 molecules (OH, NO, CO, H2O and CO2) and improved hot line lists are available for all these molecules; an update to HITEMP is currently in progress [77–79].”
ExoMol: molecular line lists for exoplanet and other atmospheres (2012, methodology): “Only in a minority of cases, specifically CO, OH and NO which all form part of the HITEMP database (Rothman et al. 2010), have the line lists been constructed essentially on the basis of experimental data, see for example Goorvitch (1994) and Bernath & Colin (2009).”
Optimal estimation retrievals of the atmospheric structure and composition of HD 189733b from secondary eclipse spectroscopy (2011, methodology): “The molecular line lists used in this study were taken from HITEMP2010 (Rothman et al. 2010) for H2O, the Carbon Dioxide Spectroscopic Databank (CDSD1000) (Tashkun et al. 2003) (also used for HITEMP2010) for CO2, HITEMP1995 (Rothman et al. 1995) for CO, and the Spherical Top Data System (STDS) (Weng”
The 2020 release of the ExoMol database: Molecular line lists for exoplanet and other hot atmospheres (2020, background): “The latest, 2010, release [76] only contained data on 5 molecules (OH, NO, CO, H2O and CO2) and improved hot line lists are available for all these molecules; an update to HITEMP is currently in progress [77–79].”
Low simulated radiation limit for runaway greenhouse climates (2013, methodology): “Firstly, using the most detailed spectral line-list for water (we use HITEMP2010[19]) and correct Rayleigh scattering cross sections for water are essential.”
A SYSTEMATIC RETRIEVAL ANALYSIS OF SECONDARY ECLIPSE SPECTRA. I. A COMPARISON OF ATMOSPHERIC RETRIEVAL TECHNIQUES (2013, methodology): “On that note, we use the HITEMP database (Rothman et al. 2010) to compute the tabulated cross-sections for CO2, CO, and H2O and the STDS database for CH4 (Wenger & Champion 1998).”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: DEPENDENCE ON PLANETARY MASS (2014, positive): “…Kopparapu et al. (2013) obtained new, improved estimates of the boundaries of the HZ by updating Kasting et al. (1993) model with new H2O and CO2 absorption coefficients from updated line- by-line (LBL) databases such as HITRAN 2008 (Rothman et al. 2009) and HITEMP 2010 (Rothman et al. 2010).”