Line Intensity Measurements in 14N216O and Their Treatment Using the Effective Dipole Moment Approach

Daumont, Ludovic; Auwera, J. Vander; Teffo, J.-L.; Perevalov, V.I.; Tashkun, S.A.

doi:10.1006/jmsp.2001.8400

Cited by 45 publications

(10 citation statements)

References 22 publications

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“…An interactive multi-line fitting program was used to reproduce the spectrum [18]. As isolated lines are exceptions, the first step of the analysis consisted in the manual determination of the spectral sections of overlapping or nearby transitions that could be fitted independently.…”

Section: Experiments and Line List Constructionmentioning

confidence: 99%

Empirical line parameters of methane in the 1.63–1.48μm transparency window by high sensitivity Cavity Ring Down Spectroscopy

et al. 2010

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We have completed the spectral coverage of the 1.58 m transparency window of methane by high sensitivity Cavity Ring Down Spectroscopy at room temperature. The achieved sensitivity ( min~3 10-10 cm-1) allowed measuring line intensities as weak as 310-29 cm/molecule i.e. three orders of magnitude smaller than the intensity cut off of the HITRAN line list of methane. The complete list contains a total of 16223 transitions between 6165 and 6750 cm-1. Their intensity values vary over six orders of magnitude from 1.6×10-29 to 2.5×10-23 cm/molecule. By comparison with a spectrum of CH 3 D recorded separately by Fourier Transform Spectroscopy, transitions due to CH 3 D in "natural" abundance in our methane sample were identified. The relative contribution of the CH 3 D isotopologue estimated by simulation of the CH 3 D and methane spectra at low resolution has showed that the CH 3 D absorption may contribute to the absorption in the region by up to 30%.

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Section: Experiments and Line List Constructionmentioning

confidence: 99%

Empirical line parameters of methane in the 1.63–1.48μm transparency window by high sensitivity Cavity Ring Down Spectroscopy

et al. 2010

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“…This RMS value is close to the estimated uncertainty of our experimental intensity values. The line intensities calculated using this last M 006 value lead to It is interesting to note that the values obtained for the homogeneous isotopic species,15 N 2 16 O and 14 N 2 16 O, are close but differ significantly from those of the non homogeneous isotopologues 14 N 15 N 16 O, 15 N 14 N 16 O.…”

mentioning

confidence: 73%

“…Using the eigenfunctions of the 00 0 6 state provided by the effective Hamiltonian model [12,13], the effective dipole moment parameter M 006 has been fitted (see Refs. [14,15] for the definition of this parameter). Two fits were performed.…”

Section: Discussionmentioning

confidence: 99%

Rotational analysis of 6ν3 and 6ν3+ν2−ν2 bands of 14N216O from ICLAS spectra between 12,760 and 12,900 cm−1

Milloud

Perevalov

Tashkun

et al. 2011

Journal of Quantitative Spectroscopy and Radiative Transfer

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“…These include DMS, CS 2 , CH 3 Cl, OCS, and N 2 O. The absorption cross sections of CH 3 Cl, OCS, and N 2 O were derived from the corresponding line lists from the HITRAN database (Gordon et al 2017), derived for CH 3 Cl by Bray et al (2011), andNikitin et al (2016); for OCS by Bouanich et al (1986), Golebiowski et al (2014), Müller et al (2005), Auwera & Fayt (2006), Sung et al (2009), Toth et al (2010), andRégalia-Jarlot et al (2002); and for N 2 O by Daumont et al (2001). For DMS and CS 2 , we use the absorption cross sections provided directly by HITRAN (Sharpe et al 2004;Gordon et al 2017;Kochanov et al 2019); we assume the same cross sections across all pressures owing to the limited data available.…”

Section: Modeling and Retrieval Of Transmission Spectramentioning

confidence: 99%

Habitability and Biosignatures of Hycean Worlds

Madhusudhan,

Piette,

Constantinou

2021

Preprint

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We investigate a new class of habitable planets composed of water-rich interiors with massive oceans underlying H 2 -rich atmospheres, referred to here as Hycean worlds. With densities between those of rocky super-Earths and more extended mini-Neptunes, Hycean planets can be optimal candidates in the search for exoplanetary habitability and may be abundant in the exoplanet population. We investigate the bulk properties (masses, radii, and temperatures), potential for habitability, and observable biosignatures of Hycean planets. We show that Hycean planets can be significantly larger compared to previous considerations for habitable planets, with radii as large as 2.6 R ⊕ (2.3 R ⊕ ) for a mass of 10 M ⊕ (5 M ⊕ ). We construct the Hycean habitable zone (HZ), considering stellar hosts from late M to sun-like stars, and find it to be significantly wider than the terrestrial-like HZ. While the inner boundary of the Hycean HZ corresponds to equilibrium temperatures as high as ∼500 K for late M dwarfs, the outer boundary is unrestricted to arbitrarily large orbital separations. Our investigations include tidally locked 'Dark Hycean' worlds that permit habitable conditions only on their permanent nightsides and 'Cold Hycean' worlds that see negligible irradiation. Finally, we investigate the observability of possible biosignatures in Hycean atmospheres. We find that a number of trace terrestrial biomarkers which may be expected to be present in Hycean atmospheres would be readily detectable using modest observing time with the James Webb Space Telescope (JWST). We identify a sizable sample of nearby potential Hycean planets that can be ideal targets for such observations in search of exoplanetary biosignatures.

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Line Intensity Measurements in 14N216O and Their Treatment Using the Effective Dipole Moment Approach

Cited by 45 publications

References 22 publications

Empirical line parameters of methane in the 1.63–1.48μm transparency window by high sensitivity Cavity Ring Down Spectroscopy

Empirical line parameters of methane in the 1.63–1.48μm transparency window by high sensitivity Cavity Ring Down Spectroscopy

Rotational analysis of 6ν3 and 6ν3+ν2−ν2 bands of 14N216O from ICLAS spectra between 12,760 and 12,900 cm−1

Habitability and Biosignatures of Hycean Worlds

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