K–H_{2} line shapes for the spectra of cool brown dwarfs^{⋆}
^{1}
GEPI, Observatoire de Paris, UMR 8111, CNRS, Université Paris VII, 61
avenue de l’Observatoire,
75014
Paris,
France
email:
nicole.allard@obspm.fr
^{2}
Institut d’Astrophysique de Paris, UMR 7095, CNRS, Université
Paris VI, 75014
Paris,
France
^{3}
Laboratoire de Chimie et Physique Quantique, UMR 5626, CNRS,
Université Paul Sabatier, 118 route
de Narbonne, 31400
Toulouse,
France
^{4}
Department of Physics and Astronomy, University of
Louisville, Louisville, Kentucky
40292,
USA
Received: 8 February 2016
Accepted: 24 February 2016
Observations of cooler and cooler brown dwarfs show that the contribution from broadening at many bars pressure is becoming important. The opacity in the red optical to nearIR region under these conditions is dominated by the extremely pressurebroadened wings of the alkali resonance lines, in particular, the K I resonance doublet at 0.77 μm. Collisions with H_{2} are preponderant in brown dwarf atmospheres at an effective temperature of about 1000 K; the H_{2} perturber densities reach several 10^{19} even in Jupitermass planets and exceed 10^{20} for superJupiters and older Y dwarfs. As a consequence, it appears that when the far wing absorption due to alkali atoms in a dense H_{2} atmosphere is significant, accurate pressure broadened profiles that are valid at high densities of H_{2} should be incorporated into spectral models.
Key words: line: profiles / brown dwarfs
The opacity tables are only available at the CDS via anonymous ftp to cdsarc.ustrasbg.fr (130.79.128.5) or via http://cdsarc.ustrasbg.fr/vizbin/qcat?J/A+A/589/A21
© ESO, 2016
1. Introduction
The cooling sequence of brown dwarfs has now been observationally characterized well beyond the transition from T to Y, or corresponding to effective temperatures down to 500 K or lower (Luhman 2014). Such objects are directly comparable to massive giant planets (superJupiters) around a Gyr in age or older and to the closest browndwarf analogs of Jupitermass planets at intermediate ages (Beichman et al. 2014). As a result of strong molecular and quasimolecular absorption at longer wavelengths, among their spectral features best characterized from the ground are the nearinfrared (NIR) flux peaks around 1 μm; these flux peaks are actually emerging from deep photospheric layers at temperatures around 1000 K and pressures of 10 to 100 bars.
Alkali–H_{2} collisional profiles have been the subject of previous studies by Burrows & Volobuyev (2003) and Allard et al. (2003, 2007c,b). Absorption profiles of sodium and potassium perturbed by helium and molecular hydrogen were presented in Burrows & Volobuyev (2003) using multiconfiguration selfconsistent field HartreeFock potentials in the Szudy theory (Szudy & Baylis 1975, 1996). Blue satellites on the line are predicted in the far wing of alkaliHe/H_{2} line profiles; such satellite bands of alkali metals perturbed by rare gas were extensively studied in the past (Allard & Kielkopf 1982 and references therein). A reliable determination of the line profiles that is applicable in all parts of the line at all densities is the Anderson semiclassical theory, which utilizes the Fourier transform of an autocorrelation function (Anderson 1952). In Allard et al. (2003, 2005), Allard & Spiegelman (2006), and Allard et al. (2007b), we used the molecularstructure calculations performed by Rossi & Pascale (1985; hereafter labeled RP85) for the molecular potentials of alkali–H_{2} systems. This approach to calculating the spectral line profile requires the knowledge of molecular potentials with high accuracy because the shape and strength of the line profile are very sensitive to the details of the molecular potential curves describing the K–H_{2} collisions. Ab initio calculations of the potentials of K–H_{2} for different orientations of the molecule have been reported in Santra & Kirby (2005) and Allard et al. (2007c), neglecting the spinorbit coupling (SO). In a previous paper (Allard et al. 1999), we derived a classical path expression for a pressurebroadened atomic spectral line shape that allows for an electric dipole moment that is dependent on the position of perturbers, which is not included in the more usual approximation of Anderson & Talman (1956) and Baranger (1958a,b). This treatment has improved the comparison of synthetic spectra of brown dwarfs with observations (Allard et al. 2003, 2007a).
In Sect. 2 we describe new calculations of the K–H_{2} potential energy surfaces in which the two electrons of H_{2} and the valence electron of potassium are explicit. The improvement over our previous work (Allard et al. 2007b) consists in a better determination of the intermediate and long range part of the K–H_{2} potential and inclusion of spinorbit coupling, which enables a new determination of the line widths of the two components of the doublet (Sect. 3).
In this continuation of previous work (Allard et al. 2003, 2007c), we illustrate the evolution of the absorption spectra of K–H_{2} collisional profiles for the densities and temperatures prevailing in atmosphere of cool brown dwarf stars (Sect. 4). Laboratory measurements are used to validate the new ab initio molecular potentials presented here, and to confirm their implementation in the spectral line profile theory (Sect. 5).
2. K–H_{2} diatomic potentials including spinorbit coupling
We carried out the ab initio calculations of the potentials (hereafter labeled S15) for the C_{2v} (Tshape) symmetry group and the C_{∞v} (linear) symmetry group in a wide range of distances R between the K atom and the center of mass of the molecule H_{2} (Figs. 1–4).
Fig. 1 Potential curves for the A and B states of the K–H_{2} molecule for the C_{∞v} (red curves) and C_{2v} symmetries (black curves). 

Open with DEXTER 
Fig. 2 Potential curves for the X state of the KH_{2} molecule for the C_{∞v} (red curves) and C_{2v} symmetries (black curves). 

Open with DEXTER 
In the calculation of the complex, we kept the bond length of H_{2} fixed at the equilibrium value r_{e} = 1.401 a.u. and the approach is along the z coordinate axis. We followed the same electronic structure calculation schemes as in our previous work (Allard et al. 2007c) on KH_{2}, namely a pseudopotential description of the potassium atom core complemented by a core polarization operator to include the core response. The pseudopotential expressions and Gaussian type basis sets (GTOs) were already published (Allard et al. 2007c). In the former work (Allard et al. 2007c), we had considered configuration interaction (CI) in determinantal spaces generated from a multireference MRPT2 perturbative scheme (Huron et al. 1973), retaining in a final variational CI all determinants with a contribution in the firstorder wavefunction larger than 10^{5} (the reference space itself included all single excitations with respect to the ground state configuration). This provided a result that could be considered a quasifull CI for the three electrons with a residual perturbation less than 10 cm^{1}. However, we noticed some noise in the potential energy definition along the K–H_{2} separation distance grid, which was due to the fact that despite the use of a unique threshold, the selection process was achieved at each distance separately; this did not ensure the continuity of CI spaces from one distance to the next and, thus, generated noise. This was not too serious far from the line center, but could be problematic in the vicinity of the atomic line, namely at intermediate and long distances where the hydrogen influence is small and constant accuracy is required. In order to solve this problem, we thus (i) still reduced the selection threshold, setting it to 0.5 × 10^{5}; and (ii) merged the CI determinantal selections at all distances, performing the final CI with the final overall selection.
Fig. 3 Ab initio potentials (black curves) for the C_{∞v} symmetry compared at intermediate and long range internuclear distance with the pseudopotential results of Rossi & Pascale (1985; red curves); B (full line), A P_{3/2} (dotted line), and A P_{1/2} (dashed line). 

Open with DEXTER 
Fig. 4 Ab initio potentials (black curves) for the C_{2v} symmetry compared with the pseudopotential results of Rossi & Pascale (1985; red curves); B ^{2}A_{1} (full line), A ^{2}B_{1} (dotted line), and A ^{2}B_{2} (dashed line). 

Open with DEXTER 
The spinorbit coupling energy splitting in the 4p level of potassium is 57.72 cm^{1} (Moore 1971). Since we want to address spectral regions close to the line center, we also incorporated SO coupling within a variant of the atominmoleculelike scheme introduced by Cohen & Schneider (1974). This scheme relies on a monoelectronic formulation of the spinorbit coupling operator (1)The total Hamiltonian H_{el} + H_{SO} is expressed in the basis set of the eigenstates (here with ) of the purely electrostatic Hamiltonian H_{el}. The spinorbit coupling between the molecular manyelectron doublet states Φ_{kσ}, approximated at this step as single determinants with the same closed shell H_{2} subpart, is isomorphic to that between the singly occupied molecular spinorbitals φ_{kσ}, correlated with the six p spinorbitals of the alkali atom (k labels the space part and σ = α,β labels the spin projection). The Cohen and Schneider approximation consists in assigning these matrix elements to their asymptotic (atomic) values (2)The scheme makes no a priori assumption about the magnitude of spinorbit coupling versus pure electrostatic interactions and enables general intermediate coupling. The effective spinorbit integral of the 4p shell of potassium is taken empirically as 2/3 times the spinorbit splitting, namely ζ_{4p} = 38.48 cm^{1}.
The main question for the applicability of this scheme in a basis of adiabatic states is the transferability of the atomic SO integrals to the molecular case. The situation can be problematic in the case where the molecular orbitals and/or the CI states undergo significant change and, thus, loose their asymptotic character. In order to improve the transferability of the CohenSchneider scheme, we thus implemented it within a diabatic representation scheme. Namely, we achieved a diabatization of the CI adiabatic states (Cimiraglia et al. 1985), obtaining quasidiabatic states from a unitary transformation of the adiabatic states. The quasidiabatic states (omitting spin mention for convenience at this stage) at a given distance R are obtained by maximizing their overlaps with the asymptotic references, which are defined as the adiabatic states at infinite separation (here R = 50a_{0}), i.e., the quasidiabatic states are defined such that (3)is maximum at each distance R. This criterion ensures that, within a truncated manifold of states, the quasidiabatic states resemble their asymptotic counterparts as much as possible. This process is achieved here including all molecular states correlated with 4s, 4p, and 5s asymptotes, which means that for the symmetries under consideration here, the transformation only affects the three states correlated with the 4s, 4pz, and 5s orbitals, namely states in symmetry C_{∞v} and states in symmetry C_{2v}. Within the unitarytransformed basis, the electronic Hamiltonian is thus no longer diagonal, but its diagonalization yields the same adiabatic energies as initially obtained in the CI process and from which it is unitary transformed. We hereafter designate E_{4s}, E_{4px}, E_{4py}, E_{4pz}, and E_{5s} the diabatic energies of the states (diagonal elements). In the present case, states with orbitals perpendicular to the approach axis have identical adiabatic and diabatic energies (these states are single in their respective symmetries). Hereafter, V_{4s4p}, V_{4s5s} and V_{4p5s} label the offdiagonal elements of the electronic Hamiltonian obtained from diabatization of the or ^{2}A_{1} manifolds.
The total Hamiltonian matrix H = H_{el} + H_{SO} is a 10 × 10 complex matrix written in the basis of the diabatic states components The diagonalization of the above matrix at each internuclear distance provides the spinorbit eigenstates (spanned by coefficients on the diabatic states) and energies. Figures 1–4 present the potential energy surfaces in the C_{∞v} and C_{2v} symmetries.
Fig. 5 Transition dipole moment for the B–X (full line), A ^{2}P_{3/2}–X (dotted line), and A ^{2}P_{1/2}–X (dashed line) transitions of the K–H_{2} molecule for the C_{∞v} (red curves) and C_{2v}symmetries (black curves); B–X (full line), A ^{2}P_{3/2}–X (dotted line), and A ^{2}P_{1/2}–X (dashed line). 

Open with DEXTER 
The transition dipole moments (Fig. 5) between the spinorbit states can be easily determined from those computed between the diabatic CI wavefunctions (4)
3. Spectral line parameters
The Ttype brown dwarf optical spectra are totally controlled by the wings of the most abundant Na I D and K I resonance doublet perturbed by H_{2}, the most abundant form of hydrogen in these deepest, hottest photospheric layers. The cores, on the other hand, are formed in the uppermost, lowest density atmospheric layers dominated by H_{2} collisions. Since in a model atmosphere calculation, the resulting line profile is the integration of the flux in all layers from the deepest to the uppermost, it is important that the centers be adequately represented; i.e., they can be nonLorentzian at the high densities of the innermost layers, while Lorentzian in the upper atmosphere but with different widths than predicted by the hydrogenic van der Waals approximation usually used for the cores (Schweitzer et al. 1996).
In Allard et al. (2007b), spectral line widths of the light alkalies perturbed by He and H_{2} were presented for conditions prevailing in brown dwarf atmospheres. We used the molecularstructure calculations performed by Pascale (1983) for the adiabatic potentials of alkalimetal–He systems, and by Rossi & Pascale (1985) for the molecular potentials of alkaliH_{2} systems. For that purpose, the fine structure was included in these potentials within the atominmoleculelike scheme introduced by Cohen & Schneider (1974) (see Sect. 2). In Fig. 6, we plotted the results obtained in the semiclassical unified theory using the potentials presented in Figs. 1–4. It shows the sensitivity of the halfwidth to the potentials.
The line widths w (HWHM) are linearly dependent on H_{2} density and a power law in temperature given for the ^{2}P_{1/2} transition by (5)and for the ^{2}P_{3/2} transition by (6)The nonlinear dependence on temperature is illustrated in Fig. 6. These expressions may be used to compute the widths for temperatures of stellar or planetary atmospheres from 400 to at least 4000 K.
H_{2} collisions are preponderant in brown dwarf atmospheres and the broadening due to H_{2} is larger than that due to He. We are not aware of other calculations of halfwidths due to K–H_{2} collisions. We could only compare the accurate theory with the broadening that is obtained from a van der Waals potential (vdW) in Fig. 6.
When it is assumed that the main interaction between two atoms is the long range van der Waals interaction of two dipoles, the LindholmFoley theory gives the usual formulae for the width and shift. The van der Waals damping constant is calculated according to the impact theory of the collision broadening.
A few laboratory experiments have measured the width, shift, and asymmetry of the light alkalis broadened by He at low density. For the most part, the alkali resonance lines are so narrow under laboratory conditions that a measurement of their widths requires extremely high spectral resolution and careful allowance for instrumental effects. Furthermore, because the shifts are also small, extremely good stability is required to make an accurate measurement of the dependence of shift on broadening, a process that requires measuring the wavelength of the line over a range of gas densities. Recently published experimental measurements for broadening by H_{2} concerns neutral Na perturbed by H_{2} (Allard et al. 2012b).
Fig. 6 Variation with temperature of the halfwidth of the D2 (blue curves) and D1 (red curves) lines of K I perturbed by H_{2} collisions. New ab initio potentials (full line) and pseudopotentials of Rossi & Pascale (1985; dashed lines), van der Waals potential (black dotted lines). 

Open with DEXTER 
4. Spectral line absorption
The theory of spectral line shapes, especially the unified approach we developed, makes possible accurate models of stellar spectra that account both for the centers of spectral lines and their extreme wings in one consistent treatment. Complete details and the derivation of the theory are provided by Allard et al. (1999).
Fig. 7 Variation with the density of H_{2} of the D2 component. The temperature is 1000 K. 

Open with DEXTER 
The blue satellites in the far wing of alkali–He/H_{2} line profiles are correlated with the maxima in the difference potentials ΔV for the B–X transition (Allard et al. 2003, 2005, 2007c; Allard & Spiegelman 2006; Zhu et al. 2005, 2006). Details on the properties of the K–H_{2} quasimolecular line satellite have been reported in Allard et al. (2003, 2007c). The main difference between our previous work reported in Allard et al. (2003) was to predict a K–H_{2} quasimolecular line satellite closely matching the position and shape of an observed feature in the spectrum of the T1 dwarf ε Indi Ba. Ab initio calculations of the potentials of K–H_{2} (Allard et al. 2007c) enabled a better agreement with the observations (Allard et al. 2007a).
The density effect on the shape of the blue wing is very significant when the H_{2} density becomes larger than 10^{20} cm^{3}. Because of multiple perturber effects, we can notice in Fig. 7 a first line satellite at 1300 cm^{1} and a second line satellite due to K–(H_{2})_{2} that appears as a shoulder about 2700 cm^{1}. The density dependence of the far blue wing is no longer linear. Opacity tables of K–H_{2}, which can be incorporated into atmosphere calculations, are valid for perturber densities lower than 10^{20} cm^{3}. Our line profiles that are valid at higher density need to be used to construct new tables.
Fig. 8 Variation with temperature of the D2 component of the K I resonance doublet perturbed by H_{2}. The density of perturbers is n_{H2} = 10^{21} cm^{3}. 

Open with DEXTER 
Fig. 9 Variation with temperature of the D1 component of the K I resonance doublet perturbed by H_{2}. The density of perturbers is n_{H2} = 10^{21} cm^{3}. 

Open with DEXTER 
Figures 8–9 present the variation with temperature of line profiles calculated for a fixed molecular hydrogen density n_{H2} = 10^{21}.
5. Unified profiles compared to laboratory spectra
We measured the absorption spectrum of K with H_{2} at pressures under 1 bar under controlled conditions in the laboratory to compare with the unified theory calculations and validation of the new potentials. In previous experimental and theoretical work on Na perturbed by H_{2}, we also reported the Naline wings measured similarly (Allard et al. 2012a,b). We also reported the experimental methods for measurement of the line wings. As in that work, the data we report on here are from a series of spectra taken of a K absorption cell with a 30 cm long by 2.2 cm diameter uniformly heated central section.
The room temperature cell was flushed with He, loaded with 99.95% pure K metal, evacuated to 10^{3} Torr with a mechanical pump, and also flushed with H_{2} and heated to remove adsorbed water and volatile impurities. H_{2} was introduced to the evacuated clean cell at 320 K, which was then sealed at an initial pressure on the order of 500 Torr. The cell temperature was monitored with thermocouples to an accuracy of 1 K, and the gas pressure was measured with a capacitive manometer accurate to ± 1 Torr as indicators of a stable environment and to insure there was no significant additional outgassing or leaks while spectral data were collected. The absorption coefficient measurements reported here are in a regime of linear dependence on H_{2} and K density.
A stable tungsten filament light source illuminated the entrance window of the cell through the output of a quasicollimated fiber optical bundle, and transmitted light from the exit window of the cell was collected and sent through an optical fiber to a CzernyTurner spectrometer, thus providing a first order dispersion of 4.3 Å per pixel on a Peltiercooled Kodak (now On Semiconductor) KAF0402E CCD sensor. This low resolution is ideal for a comprehensive survey measurement of the extended Kline wing. We have not measured the Lorentzian core in this work, and focus our attention on the line wing where critical information about the potentials is clearly distinguished. Once raw images were acquired, they were processed by subtracting dark frames and the spectra were extracted from selected regions summed over pixels at the same wavelength. Wavelength calibration against a Hg standard was applied and the 2pixel resolution of the resulting spectra was approximately 8.6 Å or 15 cm^{1} over the region of interest in the Kline wing.
The measured absorption signal was given by (7)where I_{0} is the background and f is the instrument response including spectrograph transmission and CCD efficiency. We made measurements at an elevated temperature where the density of K vapor was sufficient to produce absorption, and at room temperature where there was no absorption, that is where k = 0. The ratio of the two measurements eliminated the unknown background and sensitivity factors, effectively flatfielding the spectra and yielding the absorption coefficient k at temperature T from Eq. (7). We cannot directly measure the absolute absorption cross section because the K number density is not independently known in this method. Furthermore, it was evident from the spectra that there was significant absorption from the K_{2} molecule that is experimentally unavoidable at temperatures of interest. We also took data with Kr buffer gas, which will be reported elsewhere Kielkopf & Allard (in prep.), to remove this molecular background and reveal only the atomic K–H_{2} spectrum. Kr, and all rare gases other than He, have classically inaccessible line wing contributions to the spectral region where the singular K–H_{2} feature occurs, and therefore provide an absorption coefficient only due to K_{2}. It is straightforward then to remove this component by subtraction and leave only the coefficient of absorption due to K–H_{2} in the reduced experimental data.
The result is shown in Fig. 10 for an H_{2} density of 10^{19} cm^{3} at 820 K. The experimental absorption spectrum is linearly scaled to match the theoretical total absorption. A point to note is that the wavelength of the maximum “satellite” feature is the same in both experiment and line shape theory. Although the satellite is broad, the nonclassical region (below 0.69 μm) decreases in strength exponentially and makes a sharply defined shoulder. The experimental data and theoretical profile follow this decrease exactly, within an uncertainty on the order of the spectral bandwidth of ± 15 cm^{1}. The nonclassical region beyond the satellite (toward the blue) follows the theory exactly into the noise floor of the measurement. The wavelength of the satellite is largely dependent on the accuracy of the potential difference of the two contributing states to the transition, while the strength of the absorption as a function of wavelength is dependent on the radial scaling of the potential, the radiative dipole moment shown in Fig. 5, and the accuracy of the spectral line shape theory. The region is clearly far different from a Lorenztian, and the shape of the satellite is not the same as given by simplified theories that do not treat core and wing in a unified way. While the effects seem small since they are a fraction of the total line strength far from the unperturbed line center, for light passing through H_{2} with a long path length of K, the exponential absorption saturates the line center and the spectrum of the escaping radiation is defined by these otherwise subtle effects.
Fig. 10 Comparison of the theoretical profile (dashed blue line) of the D2 component with experimental absorption profile (dotted red line). The corresponding Lorentzian profile is overplotted (dashdotted black line). The density of perturbers is n_{H2} = 10^{19} cm^{3}, T = 820 K. 

Open with DEXTER 
6. Conclusion
Ultracool stellar atmospheres show absorption by alkali resonance lines significantly broadened by collisions with neutral perturbers. In the coolest and densest atmospheres, such as those of T dwarfs, Na I and K I broadened by H_{2} and by He can come to dominate the entire optical spectrum (Burrows et al. 2000). We have performed a theoretical determination of the K I–H_{2} line profiles using a semiclassical collision approach and high quality ab initio potentials. The new models were confirmed by a laboratory measurement in a critical sensitive region on the short wavelength side of the resonance doublet where there is some emission in a typical brown dwarf atmosphere.
Opacity tables were constructed; the complete tables are available on request and at the CDS.
References
 Allard, N. F., & Kielkopf, J. F. 1982, Rev. Mod. Phys., 54, 1103 [NASA ADS] [CrossRef] [Google Scholar]
 Allard, N. F., & Spiegelman, F. 2006, A&A, 452, 351 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, N. F., Royer, A., Kielkopf, J. F., & Feautrier, N. 1999, Phys. Rev. A, 60, 1021 [NASA ADS] [CrossRef] [Google Scholar]
 Allard, N. F., Allard, F., Hauschildt, P. H., Kielkopf, J. F., & Machin, L. 2003, A&A, 411, 473 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, N. F., Allard, F., & Kielkopf, J. F. 2005, A&A, 440, 1195 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, F., Allard, N. F., Homeier, D., et al. 2007a, A&A, 474, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, N. F., Kielkopf, J. F., & Allard, F. 2007b, Eur. Phys. J. D, 44, 507 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, N. F., Spiegelman, F., & Kielkopf, J. F. 2007c, A&A, 465, 1085 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Allard, N. F., Kielkopf, J. F., Spiegelman, F., Tinetti, G., & Beaulieu, J. P. 2012a, in EAS Pub. Ser., 58, 239 [Google Scholar]
 Allard, N. F., Spiegelman, F., Kielkopf, J. F., Tinetti, G., & Beaulieu, J. P. 2012b, A&A, 543, A159 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Anderson, P. W. 1952, Phys. Rev., 86, 809 [NASA ADS] [CrossRef] [Google Scholar]
 Anderson, P. W., & Talman, J. D. 1956, Bell System Tech. Rep., 3117 (Murray Hill, NJ) [Google Scholar]
 Baranger, M. 1958a, Phys. Rev., 111, 481 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Baranger, M. 1958b, Phys. Rev., 111, 494 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Beichman, C., Gelino, C. R., Kirkpatrick, J. D., et al. 2014, ApJ, 783, 68 [NASA ADS] [CrossRef] [Google Scholar]
 Burrows, A., & Volobuyev, M. 2003, ApJ, 583, 985 [NASA ADS] [CrossRef] [Google Scholar]
 Burrows, A. M. S.,Marley, M. S., & Sharp, C. M. 2000, ApJ, 531, 438 [NASA ADS] [CrossRef] [Google Scholar]
 Cimiraglia, R., Malrieu, J.P., Persico, M., & Spiegelmann, F. 1985, J. Phys. B, 18, 3073 [NASA ADS] [CrossRef] [Google Scholar]
 Cohen, J. S., & Schneider, B. 1974, J. Chem. Phys., 61, 3230 [NASA ADS] [CrossRef] [Google Scholar]
 Huron, B., Malrieu, J. P., & Rancurel, P. 1973, J. Chem. Phys., 58, 5745 [NASA ADS] [CrossRef] [Google Scholar]
 Luhman, K. L. 2014, ApJ, 786, L18 [NASA ADS] [CrossRef] [Google Scholar]
 Moore, C. E. 1971, National Standard Reference Data Series, NSRDS 35 Vol. I Atomic Energy Levels as Derived from the Analyses of Optical Spectra, Vol. I. 1H to 23V, NSRDSNBS 35, 358, NSRDS 35 Vol. II Atomic Energy Levels as Derived from the Analyses of Optical Spectra, Vol. II. 24Cr to 41Nb, NSRDSNBS 35, 263, NSRDS 35 Vol. III Atomic Energy Levels as Derived from the Analysis of Optical Spectra. Volume III. 42 Mo to 57La, 72Hf to 89Ac, NSRDSNBS 35, 289 [Google Scholar]
 Pascale, J. 1983, Phys. Rev. A, 28, 632 [NASA ADS] [CrossRef] [Google Scholar]
 Rossi, F., & Pascale, J. 1985, Phys. Rev. A, 32, 2657 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Santra, R., & Kirby, K. 2005, J. Chem. Phys., 123, 214309 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Schweitzer, A., Hauschildt, P. H., Allard, F., & Basri, G. 1996, MNRAS, 283, 821 [NASA ADS] [CrossRef] [Google Scholar]
 Szudy, J., & Baylis, W. 1975, J. Quant. Spectrosc. Rad. Transfer, 15, 641 [NASA ADS] [CrossRef] [Google Scholar]
 Szudy, J., & Baylis, W. 1996, Phys. Rep., 266, 127 [NASA ADS] [CrossRef] [Google Scholar]
 Zhu, C., Babb, J. F., & Dalgarno, A. 2005, Phys. Rev. A, 71, 052710 [NASA ADS] [CrossRef] [Google Scholar]
 Zhu, C., Babb, J. F., & Dalgarno, A. 2006, Phys. Rev. A, 73, 012506 [NASA ADS] [CrossRef] [Google Scholar]
All Figures
Fig. 1 Potential curves for the A and B states of the K–H_{2} molecule for the C_{∞v} (red curves) and C_{2v} symmetries (black curves). 

Open with DEXTER  
In the text 
Fig. 2 Potential curves for the X state of the KH_{2} molecule for the C_{∞v} (red curves) and C_{2v} symmetries (black curves). 

Open with DEXTER  
In the text 
Fig. 3 Ab initio potentials (black curves) for the C_{∞v} symmetry compared at intermediate and long range internuclear distance with the pseudopotential results of Rossi & Pascale (1985; red curves); B (full line), A P_{3/2} (dotted line), and A P_{1/2} (dashed line). 

Open with DEXTER  
In the text 
Fig. 4 Ab initio potentials (black curves) for the C_{2v} symmetry compared with the pseudopotential results of Rossi & Pascale (1985; red curves); B ^{2}A_{1} (full line), A ^{2}B_{1} (dotted line), and A ^{2}B_{2} (dashed line). 

Open with DEXTER  
In the text 
Fig. 5 Transition dipole moment for the B–X (full line), A ^{2}P_{3/2}–X (dotted line), and A ^{2}P_{1/2}–X (dashed line) transitions of the K–H_{2} molecule for the C_{∞v} (red curves) and C_{2v}symmetries (black curves); B–X (full line), A ^{2}P_{3/2}–X (dotted line), and A ^{2}P_{1/2}–X (dashed line). 

Open with DEXTER  
In the text 
Fig. 6 Variation with temperature of the halfwidth of the D2 (blue curves) and D1 (red curves) lines of K I perturbed by H_{2} collisions. New ab initio potentials (full line) and pseudopotentials of Rossi & Pascale (1985; dashed lines), van der Waals potential (black dotted lines). 

Open with DEXTER  
In the text 
Fig. 7 Variation with the density of H_{2} of the D2 component. The temperature is 1000 K. 

Open with DEXTER  
In the text 
Fig. 8 Variation with temperature of the D2 component of the K I resonance doublet perturbed by H_{2}. The density of perturbers is n_{H2} = 10^{21} cm^{3}. 

Open with DEXTER  
In the text 
Fig. 9 Variation with temperature of the D1 component of the K I resonance doublet perturbed by H_{2}. The density of perturbers is n_{H2} = 10^{21} cm^{3}. 

Open with DEXTER  
In the text 
Fig. 10 Comparison of the theoretical profile (dashed blue line) of the D2 component with experimental absorption profile (dotted red line). The corresponding Lorentzian profile is overplotted (dashdotted black line). The density of perturbers is n_{H2} = 10^{19} cm^{3}, T = 820 K. 

Open with DEXTER  
In the text 