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Register a new userHigh-Resolution Measurements of Intersystem Bands of Carbon Monoxide toward X Persei
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Yaron Sheffer
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In an echelle spectrum of X Per acquired with the Space Telescope Imaging Spectrograph we have identified individual rotational lines of 11 triplet-singlet (intersystem) absorption bands of ^12CO. Four bands provide first detections for interstellar clouds. From a comparison with the zeta Oph sight line we find that X Per is obscured by a higher 12CO column density of 1.4 x 10^16 cm-2. Together with the high spectral resolution of 1.3 km s-1, this allows (i) an improved measurement of previously published f-values for seven bands, and (ii) an extraction of the first astrophysical oscillator strengths for d-X (8-0), (9-0), and (10-0), as well as for e-X (12-0). The ^13CO d-X (12-0) band, previously suspected to exist toward zeta Oph, is now readily resolved and modeled. Our derived intersystem f-values for ^12CO include a few mild (leq 34%) disagreements with recent predictions from a perturbation analysis calculated for the interstellar excitation temperature. Overall, the comparison confirms the superiority of employing multiple singlet levels in the calculations of mixing coefficients over previous single-level predictions.
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Yakiv V. Pavlenko Main Astronomicaln Observatory of Academy of Sciences of Ukraine
, Golosiiv woods
2002
We compare the observational and theoretical spectra of the $Delta v$ = 2 CO bands in a range of M dwarfs. We investigate the dependence of theoretical spectra on effective temperatures as well as carbon abundance. In general we find that the synthetic CO bands fit the observed data extremely well and are excellent diagnostics. In particular the synthetic spectra reasonably match observations and the best fit temperatures are similar to those found by empirical methods. We also examine the CDC isotopic ratio. We find that fundamental $^{13}$CO bands around 2.345 and 2.375 $mu$m are good discriminators for the CDC ratio in M dwarfs. The 2.375 $mu$m is more useful because it doesnt suffer such serious contamination by water vapour transitions. Our current dataset does not quite have the wavelength coverage to perform a reliable determination of the CDC ratio in M dwarfs. For this we recommend observing the region 2.31--2.40 $mu$m at a resolution of better than 1000. Alternatively the observational problems of contamination by water vapour at 2.345 $mu$m maybe solved by observing at resolutions of around 50000. We also investigated the possibility of using the $Delta v$ = 1 CO bands around 4.5 $mu$m. We find that the contamination due to water vapour is even more of a problem at these wavelengths.
The goal is to determine the composition of Plutos atmosphere and to constrain the nature of surface-atmosphere interactions. We perform high--resolution spectroscopic observations in the 2.33--2.36 $mu$m range, using CRIRES at the VLT. We obtain (i) the first detection of gaseous methane in this spectral range, through lines of the $ u_3$ + $ u_4$ and $ u_1$ + $ u_4$ bands (ii) strong evidence (6-$sigma$ confidence) for gaseous CO in Pluto. For an isothermal atmosphere at 90 K, the CH$_4$ and CO column densities are 0.75 and 0.07 cm-am, within factors of 2 and 3, respectively. Using a physically--based thermal structure model of Plutos atmosphere also satisfying constraints from stellar occultations, we infer CH$_4$ and CO mixing ratios q$_{CH_4}$= 0.6$^{+0.6}_{-0.3}$% (consistent with results from the 1.66 $mu$m range) and q$_{CO}$ = 0.5$^{+1}_{-0.25}$$times10^{-3}$. The CO atmospheric abundance is consistent with its surface abundance. As for Triton, it is probably controlled by a thin, CO-rich, detailed balancing layer resulting from seasonal transport and/or atmospheric escape.
We report the detection of fully resolved absorption lines of A-X bands from interstellar 12C17O and 12C18O, through high-resolution spectroscopy of X Per with the Space Telescope Imaging Spectrograph. The first ultraviolet measurement of an interstellar 12C17O column density shows that its isotopomeric ratio is 12C16O/12C17O = 8700 pm 3600. Simultaneously, the second ultraviolet detection of interstellar 12C18O establishes its isotopomeric ratio at 3000 pm 600. These ratios are about five times higher than local ambient oxygen isotopic ratios in the ISM. Such severe fractionation of rare species shows that both 12C17O and 12C18O are destroyed by photodissociation, whereas 12C16O avoids destruction through self-shielding. This is to be contrasted with our ratio of 12C16O/13C16O = 73 pm 12 toward X Per, which is indistinguishable from 12C/13C, the result of a balance between photodissociation of 13C16O and its preferential formation via the isotope exchange reaction between CO and C^+.
We report on experimental results obtained from collisions of slow highly charged Ar9+ ions with a carbon monoxide dimer (CO)2 target. A COLTRIMS setup and a Coulomb explosion imaging approach are used to reconstruct the structure of the CO dimers. The three dimensional structure is deduced from the 2-body and 3-body dissociation channels from which both the intermolecular bond length and the relative orientation of the two molecules are determined. For the 3-body channels, the experimental data are interpreted with the help of a classical model in which the trajectories of the three emitted fragments are numerically integrated. We measured the equilibrium intermolecular distance to be Re = 4.2 A. The orientation of both CO molecules with respect to the dimer axis is found to be quasi-isotropic due to the large vibrational temperature of the gas jet.
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