Air-Broadening of H2O as a Function of Temperature: 696 - 2163 cm(exp -1)

The temperature dependence of air-broadened halfwidths are reported for some 500 transitions in the (000)-(000) and (010)-(000) bands of H2(16)O using gas sample temperatures ranging from 241 to 388 K. These observations were obtained from infrared laboratory spectra recorded at 0.006 to 0.011 cm(exp-1) resolution with the McMath-Pierce Fourier transform spectrometer located at Kitt Peak. The experimental values of the temperature dependence exponents, eta, were grouped into eight subsets and fitted to empirical functions in a semi-global procedure. Overall, the values of eta were found to decrease with increasing rotational quantum number J. The number of measurements (over 2200) and transitions (586) involved exceeds by a large margin that of any other comparable reported study

CRIRES-POP: A library of high resolution spectra in the near-infrared

New instrumental capabilities and the wealth of astrophysical information extractable from the near-infrared wavelength region have led to a growing interest in the field of high resolution spectroscopy at 1-5 mu. We aim to provide a library of observed high-resolution and high signal-to-noise-ratio near-infrared spectra of stars of various types throughout the Hertzsprung-Russell diagram. This is needed for the exploration of spectral features in this wavelength range and for comparison of reference targets with observations and models. High quality spectra were obtained using the CRIRES near-infrared spectrograph at ESO's VLT covering the range from 0.97 to 5.3 mu at high spectral resolution. Accurate wavelength calibration and correction for of telluric lines were performed by fitting synthetic transmission spectra for the Earth's atmosphere to each spectrum individually. We describe the observational strategy and the current status and content of the library which includes 13 objects. The first examples of finally reduced spectra are presented. This publication will serve as a reference paper to introduce the library to the community and explore the extensive amount of material.Comment: accepted for publication in A&A; see also the project webpage http://www.univie.ac.at/crirespo

The properties of V838 Mon in 2002 November

We present the results of modelling the 0.45--1 micron spectral energy distribution of V838 Mon for 2002 November. Synthetic spectra were calculated using the NextGen model atmospheres of Hauschildt et al. (1999), which incorporate line lists for H2O, TiO, CrH, FeH, CO, and MgH, as well as the VALD atomic line list. Fits to the observed spectra show that, in 2002 November, the effective temperature of V838 Mon was approximately 2000 +/-100 K. Our theoretical spectra show a comparatively weak dependence on log g. Preliminary analysis of the hot star observed together with V838 Mon shows it to be a normal B3V dwarf.Comment: 7 pages, 4 figs, accepted by A&

SPECTROSCOPY FOR HOT SUPER-EARTH EXOPLANETS

Author Institution: Department of Chemistry \& Biochemistry, Old Dominion University, 4541 Hampton Boulevard, Norfolk, VA, 23529-0126, USASpectroscopic observations of exoplanets are now possible by transit methods and direct emission. Spectroscopic requirements for exoplanet atmospheres will be reviewed based on existing measurements and model predictions for hot Jupiters and super-Earths. Super-Earths are exoplanets with masses in the range of about 2 to 10 Earth masses (i.e., between the size of Earth and Neptune). Many of them have very short orbital periods like hot Jupiters and are also hot because of proximity to their parent star. For example, Kepler-10b has a mass of 4.54 times that of Earth, a density of 8.74 g cm$^{-3}$ and a surface temperature of 1833 K. More than thirty super-Earths have been discovered and the most interesting objects are rocky planets such as Kepler-10b and CoRoT-7b. Schaefer \textit{et al.} have calculated the chemical equilibrium composition of super-Earths with temperatures in the range 500-4000 K based on the vaporization of silicate rocks similar to those of the Earth's continental crust and bulk silicate Earth. In addition to H$_2$O, CO$_2$, CH$_4$, CO and H$_2$ found in hot Jupiters, additional species such as SO$_2$, O$_2$, HCl, HF, NaCl, KCl, KF, KOH and NaOH are expected to be present. Similar to our previous work on hot ammonia \textbf{735}, 111.} and hot methane 2012, Hot Methane Line Lists for Exoplanet and Brown Dwarf Atmospheres, \textit{Astrophys. J.} \textbf{757}, 46.}, emission spectra of hot SO$_2$ will be presented. Continuing work on NaCl and KCl emission spectra will also be covered

THE ELECTRONIC STRUCTURE OF THE LnX AND LnX+LnX^{+} (X = O,H,F,Cl,Br,I) MOLECULES

Author Institution: Department of Chemistry, Massachusetts Institute of Technology Cambridge; Department of Chemistry, University of British Columbia; Department of Chemistry, Massachusetts Institute of Technology CambridgeA Ligand Field based samiempirical model for the description of the electronic structure of the law lying states of Rare Earth halides, hydrides, and oxides will be presented. The theory leads to an ordering of ionic molecular configurations corresponding to groups of states characterized by ``large"" and ``small"" orbitals. These configurations, composed of many states, are shown to be directly related to the states of the free ion. $Ln^{n+}$. Spectroscopic constants such as vibrational frequencies, bond lengths, and hyperfine splittings, as well as symmetry and position of energy levels of the few molecules of this class that have been studied will be compared to the predictions of the theory