A H<sup>13</sup>CN/HN<sup>13</sup>C linelist, model atmospheres and synthetic spectra for carbon stars

Harris, G. J.; Larner, FC; Tennyson, Jonathan; Kaminsky, B.; Pavlenko, Ya. V.; Jones, H. R. A.

doi:10.1111/j.1365-2966.2008.13642.x

Cited by 59 publications

(44 citation statements)

References 19 publications

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“…The molecular line-lists for H 2 O, CO, CH 4 , and NH 3 in our model were obtained from Freedman et al (2008) and references therein. Our line-lists for CO 2 , C 2 H 2 , and HCN were obtained from Wattson & Rothman (1986), Rothman et al (2005), and Harris et al (2008), respectively. Our CIA opacities were obtained from Borysow et al (1997) and Borysow (2002).…”

Section: Resultsmentioning

confidence: 99%

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

Ranjan

Charbonneau

Désert

et al. 2014

ApJ

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We probe the structure and composition of the atmospheres of 5 hot Jupiter exoplanets using the Hubble Space Telescope Wide Field Camera 3 (WFC3) instrument. We use the G141 grism (1.1-1.7 µm) to study and CoRoT-1b in transit, TrES-3b in secondary eclipse, and WASP-4b in both. This wavelength region includes a predicted absorption feature from water at 1.4 µm, which we expect to be nondegenerate with the other molecules that are likely to be abundant for hydrocarbon-poor (e.g. solar composition) hot Jupiter atmospheres. We divide our wavelength regions into 10 bins. For each bin we produce a spectrophotometric light curve spanning the time of transit and/or eclipse. We correct these light curves for instrumental systematics without reference to an instrument model. For our transmission spectra, our mean 1 − σ precision per bin corresponds to variations of 2.1, 2.8, and 3.0 atmospheric scale heights for TrES-2b, TrES-4b, and CoRoT-1b, respectively. We find featureless spectra for these three planets. We are unable to extract a robust transmission spectrum for WASP-4b. For our dayside emission spectra, our mean 1 − σ precision per bin corresponds to a planet-to-star flux ratio of 1.5 × 10 −4 and 2.1 × 10 −4 for WASP-4b and TrES-3b, respectively. We combine these estimates with previous broadband measurements and conclude that for both planets isothermal atmospheres are disfavored. We find no signs of features due to water. We confirm 1 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

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Section: Resultsmentioning

confidence: 99%

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

Ranjan

Charbonneau

Désert

et al. 2014

ApJ

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“…To model H 13 CN, energies and transition probabilities by Harris et al (2008) are used. A total of 602 levels and 4622 radiative transitions are included.…”

Section: A Model Molecule For Hcnmentioning

confidence: 99%

Ro-vibrational excitation of an organic molecule (HCN) in protoplanetary disks

Bruderer

Harsono

Dishoeck

2015

A&A

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Context. Organic molecules are important constituents of protoplanetary disks. Their ro-vibrational lines observed in the near-and mid-infrared are commonly detected toward T Tauri disks. These lines are the only way to probe the chemistry in the inner few au where terrestrial planets form. To understand this chemistry, accurate molecular abundances have to be determined. This is complicated by excitation effects that include radiative pumping. Most analyses so far have made the assumption of local thermal equilibrium (LTE), which may not be fulfilled because of the high gas densities required to collisionally thermalize the vibrational levels of the molecules. Aims. The non-LTE excitation effects of hydrogen cyanide (HCN) are studied to evaluate (i) how the abundance determination is affected by the LTE assumption; (ii) whether the ro-vibrational excitation is dominated by collisions or radiative pumping; and (iii) which regions of protoplanetary disks are traced by certain vibrational bands. Methods. Starting from estimates for the collisional rate coefficients of HCN, non-LTE slab models of the HCN emission were calculated to study the importance of different excitation mechanisms. Using a new radiative transfer model, the HCN emission from a full two-dimensional disk was then modeled to study the effect of the non-LTE excitation, together with the line formation. We ran models tailored to the T Tauri disk AS 205 (N) where HCN lines in both the 3 μm and 14 μm bands have been observed by VLT-CRIRES and the Spitzer Space Telescope. Results. Reproducing the observed 3 μm/14 μm flux ratios requires very high densities and kinetic temperatures (n > 10 14 cm −3 and T > 750 K), if only collisional excitation is accounted for. Radiative pumping can, however, excite the lines easily out to considerable radii ∼10 au. Consequently, abundances derived from LTE and non-LTE models do not differ by more than a factor of about 3. Models with both a strongly enhanced abundance within ∼1 au (jump abundance) and constant abundance can reproduce the current observations, but future observations with the MIRI instrument on JWST and METIS on the E-ELT can easily distinguish between the scenarios and test chemical models. Depending on the scenario, ALMA can detect rotational lines within vibrationally excited levels. Conclusions. Pumping by the continuum radiation field can bring HCN close enough to the LTE so that no big deviations in derived abundances are introduced with the LTE assumption, but the line profiles are substantially altered. In non-LTE models, accounting for collisional and radiative excitation, the emitting region can be much larger than in LTE models. Because HCN can be radiatively pumped to considerable radii, deriving a small emitting region from observations can thus point to the chemical abundance structure (e.g., jump abundance). Owing to their level structure, CO 2 and C 2 H 2 are expected to act in a similar way, facilitating studies of the warm inner disk chemistry.

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“…The line lists and partition function together with auxil- iary data including the potential parameters and dipole moment functions, as well as the absorption spectrum given in cross section format , can all be obtained also from www.exomol.com. As a potentially more accurate alternative we provide an energy file where some theoretical energies are replaced with their experimental counterparts, where available, following a similar approach used by Harris et al (2008); Barber et al (2014) and Paulose et al (2015). By taking the advantage of the two-file structure of our line lists, this approach improves the frequencies without affecting the intensities.…”

Section: Line Listmentioning

confidence: 99%

ExoMol molecular line lists – XIII. The spectrum of CaO

Yurchenko

Blissett

Asari

et al. 2016

Mon. Not. R. Astron. Soc.

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An accurate line list for calcium oxide is presented covering transitions between all bound ro-vibronic levels from the five lowest electronic states3 Π, and b 3 Σ + . The ro-vibronic energies and corresponding wavefunctionts were obtained by solving the fully coupled Schrödinger equation. Ab initio potential energy, spin-orbit, and electronic angular momentum curves were refined by fitting to the experimental frequencies and experimentally derived energies available in the literature. Using our refined model we could (i) reassign the vibronic states for a large portion of the experimentally derived energies [van Groenendael A., Tudorie M., Focsa C., Pinchemel B., Bernath P. F., 2005, J. Mol. Spectrosc., 234, 255], (ii) extended this list of energies to J = 79 − 118 and (iii) suggest a new description of the resonances from the A 1 Σ + -X 1 Σ + system. We used high level ab initio electric dipole moments reported previously [Khalil H., Brites V., Le Quere F., Leonard C., 2011, Chem. Phys., 386, 50] to compute the Einstein A coefficients. Our work is the first fully coupled description of this system. Our line list is the most complete catalogue of spectroscopic transitions available for 40 Ca 16 O and is applicable for temperatures up to at least 5000 K. CaO has yet to be observed astronomically but its transitions are characterised by being particularly strong which should facilitate its detection. The CaO line list is made available in an electronic form as supplementary data to this article and at www.exomol.com.

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A H¹³CN/HN¹³C linelist, model atmospheres and synthetic spectra for carbon stars

Abstract: ???The definitive version is available at www.blackwell-synergy.com???. Copyright Blackwell Publishing DOI: 10.1111/j.1365-2966.2008.13642.

Cited by 59 publications

References 19 publications

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

Ro-vibrational excitation of an organic molecule (HCN) in protoplanetary disks

ExoMol molecular line lists – XIII. The spectrum of CaO

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A H13CN/HN13C linelist, model atmospheres and synthetic spectra for carbon stars

Abstract: ???The definitive version is available at www.blackwell-synergy.com???. Copyright Blackwell Publishing DOI: 10.1111/j.1365-2966.2008.13642.

Cited by 59 publications

References 19 publications

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

ATMOSPHERIC CHARACTERIZATION OF FIVE HOT JUPITERS WITH THE WIDE FIELD CAMERA 3 ON THEHUBBLE SPACE TELESCOPE

Ro-vibrational excitation of an organic molecule (HCN) in protoplanetary disks

ExoMol molecular line lists – XIII. The spectrum of CaO

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Resources

About

A H¹³CN/HN¹³C linelist, model atmospheres and synthetic spectra for carbon stars