The determination of an accurate isotope dependent potential energy surface for water from extensive ab initio calculations and experimental data

By H. Partridge, D. Schwenke. 1997

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CDSD-1000, the high-temperature carbon dioxide spectroscopic databank (2003, methodology): “To account for the principal isotopic species of water we used the energy levels and transition moments calculated by Partridge and Schwenke [149].”
IUPAC Critical Evaluation of the Rotational-Vibrational Spectra of Water Vapor. Part II. Energy Levels and Transition Wavenumbers for HD16O, HD17O, and HD18O (2010, background): “Observed, MARVEL predicted, and variationally determined spectra of HD(16)O (VTT [118]), HD(17)O [116,140], and HD(18)O [116,140] are reported in Table 5”
Evolutionary Models for Very Low-Mass Stars and Brown Dwarfs with Dusty Atmospheres (2000, methodology): “This arises from the use of different H2O line lists: Miller et al. (1994) in NextGen and the recent AMES list (Partridge and Schwenke, 1997) in DUSTY models.”
Irradiated planets (2001, background): “The opacities include H 2 O and TiO lines by Partridge & Schwenke (1997), CH 4 lines from the HITRAN and GEISA databases (Rothman et al. 1992; Husson et al. 1992), and H 2 , N 2 , Ar, CH 4 , and CO 2 collision induced absorption (CIA) opacities according to (Borysow et al. 1997a,b; Borysow &…”
Low-Temperature Opacities (2005, methodology): “For the opacities computed for this paper we have chosen to use the molecular line data from Partridge & Schwenke (1997), which have been commonly used by various authors, includingAllard et al. (2001).”
DMRG+QTT approach to computation of the ground state for the molecular Schrödinger operator (2010, background): “A lot of successful approaches exist for the particular molecules (see, for example, [31, 34, 46]), which are based on the interpolation of multivariate functions.”
Infrared Spectra and Spectral Energy Distributions of Late M and L Dwarfs (2000, methodology): “MODELS, SYNTHETIC SPECTRA, AND COMPARISON PROCESS The Ames-Dusty 2000 models used for this work were calculated as described in L00 and are based on the Ames and TiO line lists by Partridge & Schwenke (1997) andH2OSchwenke (1998).”
The HITRAN molecular spectroscopic database: edition of 2000 including updates through 2001 (2003, background): “For the second isotopologue, H218O, the calculated positions predicted by Partridge and Schwenke [19] have occasionally been superseded using observed upper levels from Chevillard et al. [20].”
The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought (2005, unknown): “The situation has decidedly improved in the past years, in large part due to the great efforts by a few groups to compute ab initio line lists (e.g., Partridge & Schwenke 1997; Harris et al. 2002), and it now seems quite satisfactory regarding oxygen-rich mixtures, such as TiO (see reviews by…”
Dust in the Photospheric Environment: Unified Cloudy Models of M, L, and T Dwarfs (2002, methodology): “We have also tried other H2O data such as by Partridge & Schwenke (1997) and found that the differences with the HITEMP data are rather minor (typically, ∆log gf 0.1 and ∆ω 0.1 cm−1).”
New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit (2015, methodology): “This stems from the use of the more complete and accurate water linelist of Barber et al. (2006), compared to previously used ones, namely Miller et al. (1994) in NextGen and Partridge & Schwenke (1997) in Dusty/Cond.”
THE ATMOSPHERIC SIGNATURES OF SUPER-EARTHS: HOW TO DISTINGUISH BETWEEN HYDROGEN-RICH AND HYDROGEN-POOR ATMOSPHERES (2008, background): “We include the dominant sources of molecular line opacity in the IR: CH4, CO, NH3, (Freedman et al. 2007, and references therein), H2O (Freedman et al. 2007; Partridge & Schwenke 1997), CO2, O2, and O3 (Rothman et al. 2005).”
The Limiting Effects of Dust in Brown Dwarf Model Atmospheres (2001, background): “…& Borysow 1997; Borysow & Frommhold 1986c, 1987b; Gruszka & Borysow 1997, and references therein), (iii) ab initio line lists for H2O and TiO by Partridge & Schwenke (1997); Schwenke (1998), (iv) CO from the line list by Goorvitch & Chackerian (1994a,b), Goorvitch (1994), (v) most other…”