HITRAN HAWKS and HITEMP: high-temperature molecular database

Rothman, Laurence S.; Wattson, R. B.; Gamache, R. R.; Schroeder, Jessica; McCann, Andrew

doi:10.1117/12.211919

Cited by 85 publications

(56 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…We included absorption of water and CO, whose absorption properties were taken from the (old) HITEMP database (Rothman et al 1995). Although the water data in this database is not the most up-to-date, a line-by-line comparison in K-band with the new HITEMP database (Rothman et al 2010) yielded only differences many times smaller than the errors on the measured eclipse depths, which we neglect for this qualitative assessment.…”

Section: Atmospheric Modelsmentioning

confidence: 99%

The GROUSE project

Mooij

Kok

Nefs

et al. 2011

A&A

View full text Add to dashboard Cite

Context. Only recently it has become possible to measure the thermal emission from hot-Jupiters at near-Infrared wavelengths using ground-based telescopes, by secondary eclipse observations. This allows the planet flux to be probed around the peak of its spectral energy distribution, which is vital for the understanding of its energy budget. Aims. The aim of the reported work is to measure the eclipse depth of the planet HAT-P-1b at 2.2 μm. This planet is an interesting case, since the amount of stellar irradiation it receives falls in between that of the two best studied systems (HD 209458 and HD 189733), and it has been suggested to have a weak thermal inversion layer. Methods. We have used the LIRIS instrument on the William Herschel Telescope (WHT) to observe the secondary eclipse of HAT-P-1b in the K s -band, as part of our Ground-based secondary eclipse (GROUSE) project. The observations were done in staring mode, while significantly defocusing the telescope to avoid saturation on the K = 8.4 star. With an average cadence of 2.5 s, we collected 6520 frames during one night. Results. The eclipse is detected at the 4-σ level, the measured depth being 0.109 ± 0.025%. The uncertainties are dominated by residual systematic effects, as estimated from different reduction/analysis procedures. The measured depth corresponds to a brightness temperature of 2136 +150 −170 K. This brightness temperature is significantly higher than those derived from longer wavelengths, making it difficult to fit all available data points with a plausible atmospheric model. However, it may be that we underestimate the true uncertainties of our measurements, since it is notoriously difficult to assign precise statistical significance to a result when systematic effects are important.

show abstract

Section: Atmospheric Modelsmentioning

confidence: 99%

The GROUSE project

Mooij

Kok

Nefs

et al. 2011

A&A

View full text Add to dashboard Cite

show abstract

“…Comparisons of computer simulations with experimental data by Rodrigues et al (1999) have shown that including line-mixing into the calculations can result in a decrease of absorption coefficients by up to a factor of 2. Line-mixing parameters for CO 2 are included in the HITRAN database (Rothman et al 2005), but not in the HiTemp database (Rothman et al 1995) used for the absorption coefficients in the model. Hence, a Voigt profile was assumed for all lines at all pressures during the calculations of the absorption coefficients (von Paris et al 2008).…”

Section: B1 Performed Runsmentioning

confidence: 99%

“…In this way, the continuum is no longer restricted to the atmospheric window region (between 8 and 12 μm) and incorporates contributions from H 2 O self as well as foreign continua and, for the first time in the context of exoplanet 1D models, the CO 2 foreign continuum in the IR; 6. the temperature-pressure grid for the absorption coefficient calculations in the IR has been extended to T = 100 K and p = 1000 bar. This was done as described by von Paris et al (2008), using line parameters from Rothman et al (1995); 7. the model has been further modified to account for changing pressure levels during the calculations. Under some conditions described here, the atmospheric content of water or carbon dioxide is controlled by the surface temperature caused by evaporation or condensation.…”

Section: Computational Detailsmentioning

confidence: 99%

The extrasolar planet Gliese 581d: a potentially habitable planet?

Paris

Gebauer

Godolt

et al. 2010

A&A

View full text Add to dashboard Cite

Aims. The planetary system around the M star Gliese 581 contains at least three close-in potentially low-mass planets, Gl 581c, d, and e. In order to address the question of the habitability of Gl 581d, we performed detailed atmospheric modeling studies for several planetary scenarios. Methods. A 1D radiative-convective model was used to calculate temperature and pressure profiles of model atmospheres, which we assumed to be composed of molecular nitrogen, water, and carbon dioxide. The model allows for changing surface pressures caused by evaporation/condensation of water and carbon dioxide. Furthermore, the treatment of the energy transport has been improved in the model to account in particular for high CO 2 , high-pressure Super-Earth conditions. Results. For four high-pressure scenarios of our study, the resulting surface temperatures were above 273 K, indicating a potential habitability of the planet. These scenarios include three CO 2 -dominated atmospheres (95% CO 2 concentration with 5, 10, and 20 bar surface pressure) and a high-pressure CO 2 -enriched atmosphere (5% CO 2 concentration with 20 bar surface pressure). For all other considered scenarios, the calculated Gl 581d surface temperatures were below the freezing point of water, suggesting that Gl 581d would not be habitable then. The results for our CO 2 -dominated scenarios confirm very recent model results by Wordsworth et al. (2010). However, our model calculations imply that also atmospheres that are not CO 2 -dominated (i.e., 5% vmr instead of 95% vmr) could result in habitable conditions for Gl 581d.

show abstract

“…[120] Apart from the HITRAN and JPL spectral line catalogs, line parameters from HiTemp [Rothman et al, 1995], SAO [Chance et al, 1994], or GEISA [JacquinetHusson et al, 1999] spectral line catalogs can be used in MIRART.…”

Section: A6 Modular Infrared Atmospheric Radiative Transfer (Mirart)mentioning

confidence: 99%

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

et al. 2005

View full text Add to dashboard Cite

[1] We compare a number of radiative transfer models for atmospheric sounding in the millimeter and submillimeter wavelength range, check their consistency, and investigate their deviations from each other. This intercomparison deals with three different aspects of radiative transfer models: (1) the inherent physics of gaseous absorption lines and how they are modeled, (2) the calculation of absorption coefficients, and (3) the full calculation of radiative transfer for different geometries, i.e., up-looking, down-looking, and limblooking. The correctness and consistency of the implementations are tested by comparing calculations with predefined input such as spectroscopic data, line shape, continuum absorption model, and frequency grid. The absorption coefficients and brightness temperatures calculated by the different models are generally within about 1% of each other. Furthermore, the variability or uncertainty of the model results is estimated if (except for the atmospheric scenario) the input such as spectroscopic data, line shape, and continuum absorption model could be chosen freely. Here the models deviate from each other by about 10% around the center of major absorption lines. The main cause of such discrepancies is the variability of reported spectroscopic data for line absorption and of the continuum absorption model. Further possible causes of discrepancies are different frequency and pressure grids and differences in the corresponding interpolation routines, as well as differences in the line shape functions used, namely a prefactor of (n/n 0 ) or (n/n 0 ) 2 of the Van-Vleck-Weisskopf line shape function. Whether or not the discrepancies affect retrieval results remains to be investigated for each application individually.Citation: Melsheimer, C., et al. (2005), Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range, Radio Sci., 40, RS1007,

show abstract

HITRAN HAWKS and HITEMP: high-temperature molecular database

Cited by 85 publications

References 0 publications

The GROUSE project

The GROUSE project

The extrasolar planet Gliese 581d: a potentially habitable planet?

Intercomparison of general purpose clear sky atmospheric radiative transfer models for the millimeter/submillimeter spectral range

Contact Info

Product

Resources

About