A high-accuracy computed water line list

Barber, R. J.; Tennyson, Jonathan; Harris, G. J.; Tolchenov, R.N.

doi:10.1111/j.1365-2966.2006.10184.x

Cited by 642 publications

(612 citation statements)

References 51 publications

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“…Within these files, one for each spin species of H2O, additional comment lines credit the energy level data to Tennyson et al (2001) and the Einstein A-values to Barber et al (2006). Collisional data is divided between two collisional partners: H2 molecules and free electrons (Faure & Josselin 2008).…”

Section: Molecular Datamentioning

confidence: 99%

The physics of water masers observable with ALMA and SOFIA: model predictions for evolved stars

Gray

Baudry

Richards

et al. 2015

Mon. Not. R. Astron. Soc.

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We present the results of models that were designed to study all possible water maser transitions in the frequency range 0-1.91 THz, with particular emphasis on maser transitions that may be generated in evolved-star envelopes and observed with the ALMA and SOFIA telescopes. We used tens of thousands of radiative transfer models of both spin species of H 2 O, spanning a considerable parameter space in number density, kinetic temperature and dust temperature. Results, in the form of maser optical depths, have been summarized in a master table, Table 6. Maser transitions identified in these models were grouped according to loci of inverted regions in the density/kinetic temperature plane, a property clearly related to the dominant mode of pumping. A more detailed study of the effect of dust temperature on maser optical depth enabled us to divide the maser transitions into three groups: those with both collisional and radiative pumping schemes (22,96,209,321,325,395,941 and 1486 GHz), a much larger set that are predominantly radiatively pumped, and another large group with a predominantly collisional pump. The effect of accelerative and decelerative velocity shifts of up to 5 km s −1 was found to be generally modest, with the primary effect of reducing computed maser optical depths. More subtle asymmetric effects, dependent on line overlap, include maximum gains offset from zero shift by >1 km s −1 , but these effects were predominantly found under conditions of weak amplification. These models will allow astronomers to use multi-transition water maser observations to constrain physical conditions down to the size of individual masing clouds (size of a few astronomical units).

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Section: Molecular Datamentioning

confidence: 99%

The physics of water masers observable with ALMA and SOFIA: model predictions for evolved stars

Gray

Baudry

Richards

et al. 2015

Mon. Not. R. Astron. Soc.

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“…This interval is equal to 2B 0 , where B 0 is the rotational constant of the molecule. Barber et al 2006) and ammonia (bottom, Yurchenko et al 2011) as a function of wavelengths and temperature. The figure shows how molecular opacities change in intensity and shape due to the temperature.…”

Section: The 2-18 μM Rangementioning

confidence: 99%

“…Water vapour and methane spectral features are weaker here compared to the IR. We used calculated BT2 line list for water at high temperature (Barber et al 2006) and methane absorption coefficients from Karkoschka and Tomasko (2010). The slope of the continuum is due to Rayleigh scattering by molecular hydrogen Fig.…”

Section: A Modelling Of An Exoplanet Transit Spectrum Between 1 and 1mentioning

confidence: 99%

“…Several databases already provide transitions line lists at high temperature (including positions and absorption Neale et al (1996) coefficients for H + 3 and HITEMP (Rothman et al 2010) for CO and CO 2 . The other molecules were simulated using HITRAN 2008 (Rothman et al 2013) line list cross sections) of a series of molecules of astrophysical and planetological relevance (BT2 for water (Barber et al 2006; Fig. 13), CDSD-4000 for CO 2 (Tashkun and Perevalov 2011), as well as some hot spectra for NH 3 (Hargreaves et al 2011;Yurchenko et al 2011;Zobov et al 2011;Fig.…”

Section: Status Of Current Databases For Hot Temperaturesmentioning

confidence: 99%

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Spectroscopy of planetary atmospheres in our Galaxy

Tinetti

Encrenaz

Coustenis

2013

Astron Astrophys Rev

126

111

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About 20 years after the discovery of the first extrasolar planet, the number of planets known has grown by three orders of magnitude, and continues to increase at neck breaking pace. For most of these planets we have little information, except for the fact that they exist and possess an address in our Galaxy. For about one third of them, we know how much they weigh, their size and their orbital parameters. For less than 20, we start to have some clues about their atmospheric temperature and composition. How do we make progress from here?We are still far from the completion of a hypothetical Hertzsprung-Russell diagram for planets comparable to what we have for stars, and today we do not even know whether such classification will ever be possible or even meaningful for planetary objects. But one thing is clear: planetary parameters such as mass, radius and temperature alone do not explain the diversity revealed by current observations. The chemical composition of these planets is needed to trace back their formation history and evolution, as happened for the planets in our Solar System. As in situ measurements are and will remain off-limits for exoplanets, to study their chemical composition we will have to rely on remote sensing spectroscopic observations of their gaseous envelopes.

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“…The second important advantage of the L-band spectral region is the large number of strong transitions of molecular species such as H 2 O, CH 4 , and other simple molecules present. We primarily target spectroscopic features of water because it is abundant in hot Jupiters, and has many hundreds of well-determined "hot" transitions (Barber et al 2006) that we expect to be prominent in the exoplanet spectrum, but not excited in the telluric spectrum.…”

Section: Towards a Measurement Of The Day-side Spectrum For Hd 189733mentioning

confidence: 99%

A NIR spectrum of a hot Jupiter from the ground: Preliminary results

Mandell¹,

Deming²,

Blake

et al. 2010

Proc. IAU

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Abstract. High resolution NIR spectroscopy offers an excellent complement to the expanding dataset of transit and secondary eclipse observations of exo-planets with Spitzer that have provided the bulk of our understanding of the atmospheres and internal structure of these objects. High-resolution data can quantify the vertical temperature structure by isolating specific spectral lines formed at various depths. The presence of an opaque absorbing layer can also be inferred -and its pressure level determined quantitatively -via its effect on spectral line intensities.We have analyzed data for a single secondary eclipse of the bright transiting exo-planet host star HD189733 at L-band wavelengths (3 − 4 µm) using the NIRSPEC instrument on Keck-II. We utilize a sophisticated first-order telluric absorption modeling technique that, combined with a calibration star, has already been proven to remove the effects of varying atmospheric transmittance and allow us to reach unprecedented S/N. We are conducting validation of the final data reduction products and developing high-resolution atmospheric models for comparison, but we have already been able to rule out emission from methane as reported by Swain et al. (2010). We present preliminary results and discuss future plans for analysis and observations.

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A high-accuracy computed water line list

Cited by 642 publications

References 51 publications

The physics of water masers observable with ALMA and SOFIA: model predictions for evolved stars

The physics of water masers observable with ALMA and SOFIA: model predictions for evolved stars

Spectroscopy of planetary atmospheres in our Galaxy

A NIR spectrum of a hot Jupiter from the ground: Preliminary results

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