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1. Water Ortho-to-Para ratio in the coma of comet 67P/Churyumov-Gerasimenko

Author: Cheng, Y. -C., Bockelée-Morvan, D., Roos-Serote, M., Crovisier, J., Debout, V., Erard, S., Drossart, P., Leyrat, C., Capaccioni, F., Filacchione, G., Dubernet, M. -L., and Encrenaz, T.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Abundance ratios of the nuclear-spin isomers of H$_2$O and NH$_3$ have been measured in about two dozen comets, with a mean value corresponding to a nuclear-spin temperature of $\sim$ 30 K. The real meaning of these unequilibrated nuclear-spin abundance ratios is still debated. However, an equilibrated water ortho-to-para ratio (OPR) of 3 is also commonly observed. The H channel of VIRTIS (VIRTIS-H) on board Rosetta provided high-resolution 2.5--2.9 $\mu$m spectra of H$_2$O vapour in the coma of comet 67P/Churyumov-Gerasimenko (67P), which are suitable for the determination of the OPR of water in this comet. A large dataset of VIRTIS-H spectra obtained in limb-sounding viewing geometry was analysed, covering heliocentric distances from 1.24 to 2.73 au and altitudes from a few hundred metres to $>$ 100 km. The OPR, together with the H$_2$O rotational temperature and column density, were derived for each spectra. The weak lines of the $\nu_1$, $\nu_1+\nu_3-\nu_1$ and $\nu_2+\nu_3-\nu_2$ bands in the 2.774--2.910 $\mu$m range were used to calculate by how much the strong $\nu_3$ band centred at 2.67 $\mu$m is attenuated due to optical depth effects, expressed by the attenuation factor $f_{\rm atten}$. Most OPR determinations are strongly affected by opacity effects, as demonstrated by the observed anti-correlation between the OPR and the column density, and the correlation between the OPR and attenuation factor $f_{\rm atten}$. Based on both radiative transfer calculations and OPR values obtained in low-opacity conditions, we derive an OPR of 2.94 $\pm$ 0.06 for comet 67P. The water OPR measured in the coma of 67P is consistent with laboratory experiments showing that water vapour that has thermally desorbed from water ice has a statistical value of 3, regardless of the past formation process of water ice., Comment: 12 pages, 13 figures, not including additional material in the Appendices. Accepted in Astronomy and Astrophysics
Published: 2022
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2. BASECOL2023 scientific content

Author: Dubernet, M. L., primary, Boursier, C., additional, Denis-Alpizar, O., additional, Ba, Y. A., additional, Moreau, N., additional, Zwölf, C. M., additional, Amor, M. A., additional, Babikov, D., additional, Balakrishnan, N., additional, Balança, C., additional, Ben Khalifa, M., additional, Bergeat, A., additional, Bop, C. T., additional, Cabrera-González, L., additional, Cárdenas, C., additional, Chefai, A., additional, Dagdigian, P. J., additional, Dayou, F., additional, Demes, S., additional, Desrousseaux, B., additional, Dumouchel, F., additional, Faure, A., additional, Forrey, R. C., additional, Franz, J., additional, García-Vázquez, R. M., additional, Gianturco, F., additional, Godard Palluet, A., additional, González-Sánchez, L., additional, Groenenboom, G. C., additional, Halvick, P., additional, Hammami, K., additional, Khadri, F., additional, Kalugina, Y., additional, Kleiner, I., additional, Kłos, J., additional, Lique, F., additional, Loreau, J., additional, Mandal, B., additional, Mant, B., additional, Marinakis, S., additional, Ndaw, D., additional, Pirlot Jankowiak, P., additional, Price, T., additional, Quintas-Sánchez, E., additional, Ramachandran, R., additional, Sahnoun, E., additional, Santander, C., additional, Stancil, P. C., additional, Stoecklin, T., additional, Tennyson, J., additional, Tonolo, F., additional, Urzúa-Leiva, R., additional, Yang, B., additional, Yurtsever, E., additional, and Żóltowski, M., additional
Published: 2024
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3. Collisional excitation of water by hydrogen atoms

Author: Daniel, F., Faure, A., Dagdigian, P. J., Dubernet, M. -L., lique, F., and forêts, G. Pineau des
Subjects: Astrophysics - Astrophysics of Galaxies, Physics - Chemical Physics
Abstract: We present quantum dynamical calculations that describe the rotational excitation of H$_2$O due to collisions with H atoms. We used a recent, high accuracy potential energy surface, and solved the collisional dynamics with the close-coupling formalism, for total energies up to 12 000 cm$^{-1}$. From these calculations, we obtained collisional rate coefficients for the first 45 energy levels of both ortho- and para-H$_2$O and for temperatures in the range T = 5-1500 K. These rate coefficients are subsequently compared to the values previously published for the H$_2$O / He and H$_2$O / H$_2$ collisional systems. It is shown that no simple relation exists between the three systems and that specific calculations are thus mandatory.
Published: 2014
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4. On the influence of collisional rate coefficients on the water vapour excitation

Author: Daniel, F., Goicoechea, J. R., Cernicharo, J., Dubernet, M. -L., and Faure, A.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Water is a key molecule in many astrophysical studies. Its high dipole moment makes this molecule to be subthermally populated under the typical conditions of most astrophysical objects. This motivated the calculation of various sets of collisional rate coefficients (CRC) for H$_2$O (with He or H$_2$) which are necessary to model its rotational excitation and line emission. We performed accurate non--local non--LTE radiative transfer calculations using different sets of CRC in order to predict the line intensities from transitions that involve the lowest energy levels of H$_2$O (E $<$ 900 K). The results obtained from the different CRC sets are then compared using line intensity ratio statistics. For the whole range of physical conditions considered in this work, we obtain that the intensities based on the quantum and QCT CRC are in good agreement. However, at relatively low H$_2$ volume density ($n$(H$_2$) $<$ 10$^7$ cm$^{-3}$) and low water abundance ($\chi$(H$_2$O) $<$ 10$^{-6}$), these physical conditions being relevant to describe most molecular clouds, we find differences in the predicted line intensities of up to a factor of $\sim$ 3 for the bulk of the lines. Most of the recent studies interpreting early Herschel Space Observatory spectra used the QCT CRC. Our results show that although the global conclusions from those studies will not be drastically changed, each case has to be considered individually, since depending on the physical conditions, the use of the QCT CRC may lead to a mis--estimate of the water vapour abundance of up to a factor of $\sim$ 3.
Published: 2012
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5. Herschel observations of Extra-Ordinary Sources: Methanol as a probe of physical conditions in Orion KL

Author: Wang, S., Bergin, E. A., Crockett, N. R., Goldsmith, P. F., Lis, D. C., Pearson, J. C., Schilke, P., Bell, T. A., Comito, C., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T. F., Goicoechea, J. R., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. B., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Muller, H. S. P., Murphy, J. A., Neufeld, D. A., Ossenkopf, V., Perault, M., Phillips, T. G., Plume, R., Qin, S. -L., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Yorke, H. W., Yu, S., and Zmuidzinas, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We have examined methanol emission from Orion KL with of the {\em Herschel}/HIFI instrument, and detected two methanol bands centered at 524 GHz and 1061 GHz. The 524 GHz methanol band (observed in HIFI band 1a) is dominated by the isolated $\Delta$J$=$0, K$=-4\rightarrow$-3, v$_t$$=$0 Q branch, and includes 25 E-type and 2 A-type transitions. The 1061 GHz methanol band (observed in HIFI band 4b) is dominated by the $\Delta$J$=$0, K$=7\rightarrow$6, v$_t$$=$0 Q branch transitions which are mostly blended. We have used the isolated E-type v$_t$$=$0 methanol transitions to explore the physical conditions in the molecular gas. With HIFI's high velocity resolution, the methanol emission contributed by different spatial components along the line of sight toward Orion KL (hot core, low velocity flow, and compact ridge) can be distinguished and studied separately. The isolated transitions detected in these bands cover a broad energy range (upper state energy ranging from 80 K to 900 K), which provides a unique probe of the thermal structure in each spatial component. The observations further show that the compact ridge is externally heated. These observations demonstrate the power of methanol lines as probes of the physical conditions in warm regions in close proximity to young stars., Comment: 8 pages, 9 figures, accepted for publication in Astronomy & Astrophysics
Published: 2011
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6. Detection of OH$^+$ and H$_2$O$^+$ towards Orion~KL

Author: Gupta, H., Rimmer, P., Pearson, J. C., Yu, S., Herbst, E., Harada, N., Bergin, E. A., Neufeld, D. A., Melnick, G. J., Bachiller, R., Baechtold, W., Bell, T. A., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Chattopadhyay, G., Comito, C., Cabrit, S., Crockett, N. R., Daniel, F., Falgarone, E., Diez-Gonzalez, M. C., Dubernet, M. -L., Erickson, N., Emprechtinger, M., Encrenaz, P., Gerin, M., Gill, J. J., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Joblin, C., Johnstone, D., Langer, W. D., Larsson, B., Latter, W. B., Lin, R. H., Lis, D. C., Liseau, R., Lord, S. D., Maiwald, F. W., Maret, S., Martin, P. G., Martin-Pintado, J., Menten, K. M., Morris, P., Müller, H. S. P., Murphy, J. A., Nordh, L. H., Olberg, M., Ossenkopf, V., Pagani, L., Pérault, M., Phillips, T. G., Plume, R., Qin, S. -L., Salez, M., Samoska, L. A., Schilke, P., Schlecht, E., Schlemmer, S., Szczerba, R., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Wang, S., Yorke, H. W., Zmuidzinas, J., Boogert, A., Güsten, R., Hartogh, P., Honingh, N., Karpov, A., Kooi, J., Krieg, J. -M., Schieder, R., and Zaal, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report observations of the reactive molecular ions OH$^+$, H$_2$O$^+$, and H$_3$O$^+$ towards Orion KL with Herschel/HIFI. All three $N=1-0$ fine-structure transitions of OH$^+$ at 909, 971, and 1033GHz and both fine-structure components of the doublet {\it ortho}-H$_2$O$^+$ $1_{11}-0_{00}$ transition at 1115 and 1139GHz were detected; an upper limit was obtained for H$_3$O$^+$. OH$^+$ and H$_2$O$^+$ are observed purely in absorption, showing a narrow component at the source velocity of 9 kms$^{-1}$, and a broad blueshifted absorption similar to that reported recently for HF and {\it para}-H$_{2}^{18}$O, and attributed to the low velocity outflow of Orion KL. We estimate column densities of OH$^+$ and H$_2$O$^+$ for the 9 km s$^{-1}$ component of $9 \pm 3 \times 10^{12}$cm$^{-2}$ and $7 \pm 2 \times 10^{12}$cm$^{-2}$, and those in the outflow of $1.9 \pm 0.7 \times 10^{13}$cm$^{-2}$ and $1.0 \pm 0.3 \times 10^{13}$cm$^{-2}$. Upper limits of $2.4\times 10^{12}$cm$^{-2}$ and $8.7\times 10^{12}$cm$^{-2}$ were derived for the column densities of {\it ortho} and {\it para}-H$_3$O$^+$ from transitions near 985 and 1657GHz. The column densities of the three ions are up to an order of magnitude lower than those obtained from recent observations of W31C and W49N. The comparatively low column densities may be explained by a higher gas density despite the assumption of a very high ionization rate., Comment: 5 pages, 1 figure. Accepted to and to be published in the Herschel HIFI special issue of A\&A Letters
Published: 2010
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7. Herschel observations of EXtra-Ordinary Sources (HEXOS): Observations of H2O and its isotopologues towards Orion KL

Author: Melnick, G. J., Tolls, V., Neufeld, D. A., Bergin, E. A., Phillips, T. G., Wang, S., Crockett, N. R., Bell, T. A., Blake, G. A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. D., Lis, D. C., Lord, S. D., Maret, S., Martin, P. G., Menten, K. M., Morris, P., Muller, H. S. P., Murphy, J. A., Ossenkopf, V., Pagani, L., Pearson, J. C., Perault, M., Plume, R., Qin, S. -L., Salez, M., Schilke, P., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Yorke, H. W., Yu, S., and Zmuidzinas, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the detection of more than 48 velocity-resolved ground rotational state transitions of H2(16)O, H2(18)O, and H2(17)O - most for the first time - in both emission and absorption toward Orion KL using Herschel/HIFI. We show that a simple fit, constrained to match the known emission and absorption components along the line of sight, is in excellent agreement with the spectral profiles of all the water lines. Using the measured H2(18)O line fluxes, which are less affected by line opacity than their H2(16)O counterparts, and an escape probability method, the column densities of H2(18)O associated with each emission component are derived. We infer total water abundances of 7.4E-5, 1.0E-5, and 1.6E-5 for the plateau, hot core, and extended warm gas, respectively. In the case of the plateau, this value is consistent with previous measures of the Orion-KL water abundance as well as those of other molecular outflows. In the case of the hot core and extended warm gas, these values are somewhat higher than water abundances derived for other quiescent clouds, suggesting that these regions are likely experiencing enhanced water-ice sublimation from (and reduced freeze-out onto) grain surfaces due to the warmer dust in these sources., Comment: 5 pages, 2 figures
Published: 2010
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8. Reversal of infall in SgrB2(M) revealed by Herschel/HIFI observations of HCN lines at THz frequencies

Author: Rolffs, Rainer, Schilke, Peter, Comito, Claudia, Bergin, E. A., van der Tak, F. F. S., Lis, D. C., Qin, S. -L., Menten, K. M., Guesten, R., Bell, T. A., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N. R., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. D., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Morris, P., Mueller, H. S. P., Murphy, J. A., Ossenkopf, V., Pearson, J. C., Perault, M., Phillips, T. G., Plume, R., Schlemmer, S., Stutzki, J., Trappe, N., Vastel, C., Wang, S., Yorke, H. W., Yu, S., Zmuidzinas, J., Diez-Gonzalez, M. C., Bachiller, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L. H., Gill, J. J., and Chattopadhyay, G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: To investigate the accretion and feedback processes in massive star formation, we analyze the shapes of emission lines from hot molecular cores, whose asymmetries trace infall and expansion motions. The high-mass star forming region SgrB2(M) was observed with Herschel/HIFI (HEXOS key project) in various lines of HCN and its isotopologues, complemented by APEX data. The observations are compared to spherically symmetric, centrally heated models with density power-law gradient and different velocity fields (infall or infall+expansion), using the radiative transfer code RATRAN. The HCN line profiles are asymmetric, with the emission peak shifting from blue to red with increasing J and decreasing line opacity (HCN to H$^{13}$CN). This is most evident in the HCN 12--11 line at 1062 GHz. These line shapes are reproduced by a model whose velocity field changes from infall in the outer part to expansion in the inner part. The qualitative reproduction of the HCN lines suggests that infall dominates in the colder, outer regions, but expansion dominates in the warmer, inner regions. We are thus witnessing the onset of feedback in massive star formation, starting to reverse the infall and finally disrupting the whole molecular cloud. To obtain our result, the THz lines uniquely covered by HIFI were critically important., Comment: A&A, HIFI special issue, accepted
Published: 2010
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9. Herschel observations of deuterated water towards Sgr B2(M)

Author: Comito, Claudia, Schilke, Peter, Rolffs, Rainer, Lis, D. C., Belloche, A., Bergin, E. A., Phillips, T. G., Bell, T. A., Crockett, N. R., Wang, S., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. D., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Mueller, H. S. P., Murphy, J. A., Neufeld, D. A., Ossenkopf, V., Pearson, J. C., Perault, M., Plume, R., Qin, S. -L., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Yorke, H. W., Yu, S., Olberg, M., Szczerba, R., Larsson, B., Liseau, R., Lin, R. H., Samoska, L. A., and Schlecht, E.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: Observations of HDO are an important complement for studies of water, because they give strong constraints on the formation processes -- grain surfaces versus energetic process in the gas phase, e.g. in shocks. The HIFI observations of multiple transitions of HDO in Sgr~B2(M) presented here allow the determination of the HDO abundance throughout the envelope, which has not been possible before with ground-based observations only. The abundance structure has been modeled with the spherical Monte Carlo radiative transfer code RATRAN, which also takes radiative pumping by continuum emission from dust into account. The modeling reveals that the abundance of HDO rises steeply with temperature from a low abundance ($2.5\times 10^{-11}$) in the outer envelope at temperatures below 100~K through a medium abundance ($1.5\times 10^{-9}$) in the inner envelope/outer core, at temperatures between 100 and 200~K, and finally a high abundance ($3.5\times 10^{-9}$) at temperatures above 200~K in the hot core., Comment: A&A HIFI special issue, accepted
Published: 2010
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10. Herschel observations of EXtra-Ordinary Sources: The Terahertz spectrum of Orion KL seen at high spectral resolution

Author: Crockett, N. R., Bergin, E. A., Wang, S., Lis, D. C., Bell, T. A., Blake, G. A., Boogert, A., Bumble, B., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Gusten, R., Hartogh, P., Helmich, F., Herbst, E., Honingh, N., Joblin, C., Johnstone, D., Karpov, A., Kawamura, J. H., Kooi, J., Krieg, J. -M., Langer, W. D., Latter, W. D., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Muller, H. S. P., Murphy, J. A., Neufeld, D. A., Ossenkopf, V., Pearson, J. C., Perault, M., Phillips, T. G., Plume, R., Qin, S. -L., Roelfsema, P., Schieder, R., Schilke, P., Schlemmer, S., Stutzki, J., van der Tak, F. F. S., Tielens, A., Trappe, N., Vastel, C., Yorke, H. W., Yu, S., and Zmuidzinas, J.
Subjects: Astrophysics - Solar and Stellar Astrophysics
Abstract: We present the first high spectral resolution observations of Orion KL in the frequency ranges 1573.4 - 1702.8 GHz (band 6b) and 1788.4 - 1906.8 GHz (band 7b) obtained using the HIFI instrument on board the Herschel Space Observatory. We characterize the main emission lines found in the spectrum, which primarily arise from a range of components associated with Orion KL including the hot core, but also see widespread emission from components associated with molecular outflows traced by H2O, SO2, and OH. We find that the density of observed emission lines is significantly diminished in these bands compared to lower frequency Herschel/HIFI bands., Comment: Accepted for publication in the Herschel HIFI special issue of Astronomy and Astrophysics Letters, 5 pages, 3 figures
Published: 2010
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11. Herschel observations of EXtra-Ordinary Sources: the present and future of spectral surveys with Herschel/HIFI

Author: Bergin, E. A., Phillips, T. G., Comito, C., Crockett, N. R., Lis, D. C., Schilke, P., Wang, S., Bell, T. A., Blake, G. A., Bumble, B., Caux, E., Cabrit, S., Ceccarelli, C., Cernicharo, J., Daniel, F., de Graauw, Th., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Hartogh, P., Helmich, F. P., Herbst, E., Joblin, C., Johnstone, D., Kawamura, J. H., Langer, W. D., Latter, W. B., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Muller, H. S. P., Murphy, J. A., Neufeld, D. A., Ossenkopf, V., Pagani, L., Pearson, J. C., Perault, M., Plume, R., Roelfsema, P., Qin, S. -L., Salez, M., Schlemmer, S., Stutzki, J., Tielens, A. G. G. M., Trappe, N., van der Tak, F. F. S., Vastel, C., Yorke, H. W., Yu, S., and Zmuidzinas, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present initial results from the Herschel GT key program: Herschel observations of EXtra-Ordinary Sources (HEXOS) and outline the promise and potential of spectral surveys with Herschel/HIFI. The HIFI instrument offers unprecedented sensitivity, as well as continuous spectral coverage across the gaps imposed by the atmosphere, opening up a largely unexplored wavelength regime to high-resolution spectroscopy. We show the spectrum of Orion KL between 480 and 560 GHz and from 1.06 to 1.115 THz. From these data, we confirm that HIFI separately measures the dust continuum and spectrally resolves emission lines in Orion KL. Based on this capability we demonstrate that the line contribution to the broad-band continuum in this molecule-rich source is ~20-40% below 1 THz and declines to a few percent at higher frequencies. We also tentatively identify multiple transitions of HD18O in the spectra. The first detection of this rare isotopologue in the interstellar medium suggests that HDO emission is optically thick in the Orion hot core with HDO/H2O ~ 0.02. We discuss the implications of this detection for the water D/H ratio in hot cores., Comment: 6 pages, 5 figures, accepted and to be published in Herschel HIFI special issue of A&A Letters
Published: 2010
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12. Herschel observations of extra-ordinary sources: Detection of Hydrogen Fluoride in absorption towards Orion~KL

Author: Phillips, T. G., Bergin, E. A., Lis, D. C., Neufeld, D. A., Bell, T. A., Wang, S., Crockett, N. R., Emprechtinger, M., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Comito, C., Daniel, F., Dubernet, M. -L., Encrenaz, P., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. D., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Muller, H. S. P., Murphy, J. A., Ossenkopf, V., Pearson, J. C., Perault, M., Plume, R., Qin, S. -L., Schilke, P., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Yorke, H. W., Yu, S., Zmuidzinas, J., Boogert, A., Gusten, R., Hartogh, P., Honingh, N., Karpov, A., Kooi, J., Krieg, J. -M., and Schieder, R.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report a detection of the fundamental rotational transition of hydrogen fluoride in absorption towards Orion KL using Herschel/HIFI. After the removal of contaminating features associated with common molecules ("weeds"), the HF spectrum shows a P-Cygni profile, with weak redshifted emission and strong blue-shifted absorption, associated with the low-velocity molecular outflow. We derive an estimate of 2.9 x 10^13 cm^-2 for the HF column density responsible for the broad absorption component. Using our best estimate of the H2 column density within the low-velocity molecular outflow, we obtain a lower limit of ~1.6 x 10^-10 for the HF abundance relative to hydrogen nuclei, corresponding to 0.6% of the solar abundance of fluorine. This value is close to that inferred from previous ISO observations of HF J=2--1 absorption towards Sgr B2, but is in sharp contrast to the lower limit of 6 x 10^-9 derived by Neufeld et al. (2010) for cold, foreground clouds on the line of sight towards G10.6-0.4., Comment: 5 pages, 3 figures, paper to be published in the Herschel special issue of A&A letters
Published: 2010
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13. Herschel observations of extra-ordinary sources: Detecting spiral arm clouds by CH absorption lines

Author: Qin, S. -L., Schilke, P., Comito, C., Möller, T., Rolffs, R., Müller, H. S. P., Belloche, A., Menten, K. M., Lis, D. C., Phillips, T. G., Bergin, E. A., Bell, T. A., Crockett, N. R., Blake, G. A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Herbst, E., Joblin, C., Johnstone, D., Langer, W. D., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Morris, P., Murphy, J. A., Neufeld, D. A., Ossenkopf, V., Pagani, L., Pearson, J. C., Pérault, M., Plume, R., Salez, M., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Wang, S., Yorke, H. W., Yu, S., Zmuidzinas, J., Boogert, A., Güsten, R., Hartogh, P., Honingh, N., Karpov, A., Kooi, J., Krieg, J. M., Schieder, R., Diez-Gonzalez, M. C., Bachille, R., Martin-Pintado, J., Baechtold, W., Olberg, M., Nordh, L. H., Gill, J. L., and Chattopadhyay, G.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We have observed CH absorption lines ($J=3/2, N=1 \leftarrow J=1/2, N=1$) against the continuum source Sgr~B2(M) using the \textit{Herschel}/HIFI instrument. With the high spectral resolution and wide velocity coverage provided by HIFI, 31 CH absorption features with different radial velocities and line widths are detected and identified. The narrower line width and lower column density clouds show `spiral arm' cloud characteristics, while the absorption component with the broadest line width and highest column density corresponds to the gas from the Sgr~B2 envelope. The observations show that each `spiral arm' harbors multiple velocity components, indicating that the clouds are not uniform and that they have internal structure. This line-of-sight through almost the entire Galaxy offers unique possibilities to study the basic chemistry of simple molecules in diffuse clouds, as a variety of different cloud classes are sampled simultaneously. We find that the linear relationship between CH and H$_2$ column densities found at lower $A_V$ by UV observations does not continue into the range of higher visual extinction. There, the curve flattens, which probably means that CH is depleted in the denser cores of these clouds., Comment: Accepted for publication in A&A, HIFI Special Issue
Published: 2010
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14. Herschel/HIFI measurements of the ortho/para ratio in water towards Sagittarius B2(M) and W31C

Author: Lis, D. C., Phillips, T. G., Goldsmith, P. F., Neufeld, D. A., Herbst, E., Comito, C., Schilke, P., Müller, H. S. P., Bergin, E. A., Gerin, M., Bell, T. A., Emprechtinger, M., Black, J. H., Blake, G. A., Boulanger, F., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Coutens, A., Crockett, N. R., Daniel, F., Dartois, E., De Luca, M., Dubernet, M. -L., Encrenaz, P., Falgarone, E., Geballe, T. R., Godard, B., Giesen, T. F., Goicoechea, J. R., Gry, C., Gupta, H., Hennebelle, P., Hily-Blant, P., Kołos, R., Krełowski, J., Joblin, C., Johnstone, D., Kaźmierczak, M., Lord, S. D., Maret, S., Martin, P. G., Martín-Pintado, J., Melnick, G. J., Menten, K. M., Monje, R., Mookerjea, B., Morris, P., Murphy, J. A., Ossenkopf, V., Pagani, L., Pearson, J. C., Pérault, M., Persson, C., Plume, R., Qin, S. -L., Salez, M., Schlemmer, S., Schmidt, M., Sonnentrucker, P., Stutzki, J., Teyssier, D., Trappe, N., van der Tak, F. F. S., Vastel, C., Wang, S., Yorke, H. W., Yu, S., Zmuidzinas, J., Boogert, A., Erickson, N., Karpov, A., Kooi, J., Maiwald, F. W., Schieder, R., and Zaal, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We present Herschel/HIFI observations of the fundamental rotational transitions of ortho- and para-H$_2^{16}$O and H$_2^{18}$O in absorption towards Sagittarius~B2(M) and W31C. The ortho/para ratio in water in the foreground clouds on the line of sight towards these bright continuum sources is generally consistent with the statistical high-temperature ratio of 3, within the observational uncertainties. However, somewhat unexpectedly, we derive a low ortho/para ratio of $2.35 \pm 0.35$, corresponding to a spin temperature of $\sim$27~K, towards Sagittarius~B2(M) at velocities of the expanding molecular ring. Water molecules in this region appear to have formed with, or relaxed to, an ortho/para ratio close to the value corresponding to the local temperature of the gas and dust., Comment: Accepted for publication in A&A, HIFI Special Issue; 5 pages, 3 figures
Published: 2010
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15. Herschel/HIFI discovery of interstellar chloronium (H$_2$Cl$^+$)

Author: Lis, D. C., Pearson, J. C., Neufeld, D. A., Schilke, P., Müller, H. S. P., Gupta, H., Bell, T. A., Comito, C., Phillips, T. G., Bergin, E. A., Ceccarelli, C., Goldsmith, P. F., Blake, G. A., Bacmann, A., Baudry, A., Benedettini, M., Benz, A., Black, J., Boogert, A., Bottinelli, S., Cabrit, S., Caselli, P., Castets, A., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N. R., Daniel, F., Demyk, K., Dominic, C., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Fuente, A., Gerin, M., Giesen, T. F., Goicoechea, J. R., Helmich, F., Hennebelle, P., Henning, Th., Herbst, E., Hily-Blant, P., Hjalmarson, Å., Hollenbach, D., Jack, T., Joblin, C., Johnstone, D., Kahane, C., Kama, M., Kaufman, M., Klotz, A., Langer, W. D., Larsson, B., Bourlot, J. Le, Lefloch, B., Petit, F. Le, Li, D., Liseau, R., Lord, S. D., Lorenzani, A., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Murphy, J. A., Nagy, Z., Nisini, B., Ossenkopf, V., Pacheco, S., Pagani, L., Parise, B., Pérault, M., Plume, R., Qin, S. -L., Roueff, E., Salez, M., Sandqvist, A., Saraceno, P., Schlemmer, S., Schuster, K., Snell, R., Stutzki, J., Tielens, A., Trappe, N., van der Tak, F. F. S., van der Wiel, M. H. D., van Dishoeck, E., Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Wyrowski, F., Yorke, H. W., Yu, S., Zmuidzinas, J., Delorme, Y., Desbat, J. -P., Güsten, R., Krieg, J. -M., and Delforge, B.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We report the first detection of chloronium, H$_2$Cl$^+$, in the interstellar medium, using the HIFI instrument aboard the \emph{Herschel} Space Observatory. The $2_{12}-1_{01}$ lines of ortho-H$_2^{35}$Cl$^+$ and ortho-H$_2^{37}$Cl$^+$ are detected in absorption towards NGC~6334I, and the $1_{11}-0_{00}$ transition of para-H$_2^{35}$Cl$^+$ is detected in absorption towards NGC~6334I and Sgr~B2(S). The H$_2$Cl$^+$ column densities are compared to those of the chemically-related species HCl. The derived HCl/H$_2$Cl$^+$ column density ratios, $\sim$1--10, are within the range predicted by models of diffuse and dense Photon Dominated Regions (PDRs). However, the observed H$_2$Cl$^+$ column densities, in excess of $10^{13}$~cm$^{-2}$, are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models., Comment: Accepted for publication in A&A, HIFI Special Issue; 4 pages, 2 figures, 1 table
Published: 2010
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16. Herschel observations of ortho- and para-oxidaniumyl (H2O+) in spiral arm clouds toward Sgr B2(M)

Author: Schilke, P., Comito, C., Mueller, H. S. P., Bergin, E. A., Herbst, E., Lis, D. C., Neufeld, D. A., Phillips, T. G., Bell, T. A., Blake, G. A., Cabrit, S., Caux, E., Ceccarelli, C., Cernicharo, J., Crockett, N. R., Daniel, F., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Gerin, M., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Gupta, H., Joblin, C., Johnstone, D., Langer, W. D., Latter, W. B., Lord, S. D., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Murphy, J. A., Ossenkopf, V., Pagani, L., Pearson, J. C., Perault, M., Plume, R., Qin, S. -L., Salez, M., Schlemmer, S., Stutzki, J., Trappe, N., van der Tak, F. F. S., Vastel, C., Wang, S., Yorke, H. W., Yu, S., Erickson, N., Maiwald, F. W., Kooi, J., Karpov, A., Zmuidzinas, J., Boogert, A., Schieder, R., and Zaal, P.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: H2O+ has been observed in its ortho- and para- states toward the massive star forming core Sgr B2(M), located close to the Galactic center. The observations show absorption in all spiral arm clouds between the Sun and Sgr B2. The average o/p ratio of H2O+ in most velocity intervals is 4.8, which corresponds to a nuclear spin temperature of 21 K. The relationship of this spin temperature to the formation temperature and current physical temperature of the gas hosting H2O+ is discussed, but no firm conclusion is reached. In the velocity interval 0 to 60 km/s, an ortho/para ratio of below unity is found, but if this is due to an artifact of contamination by other species or real is not clear., Comment: A&A, HIFI special issue, accepted
Published: 2010
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17. Detection of interstellar oxidaniumyl: abundant H2O+ towards the star-forming regions DR21, Sgr B2, and NGC6334

Author: Ossenkopf, V., Müller, H. S. P., Lis, D. C., Schilke, P., Bell, T. A., Bruderer, S., Bergin, E., Ceccarelli, C., Comito, C., Stutzki, J., Bacman, A., Baudry, A., Benz, A. O., Benedettini, M., Berne, O., Blake, G., Boogert, A., Bottinelli, S., Boulanger, F., Cabrit, S., Caselli, P., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N. R., Daniel, F., Demyk, K., Dieleman, P., Dominik, C., Dubernet, M. L., Emprechtinger, M., Encrenaz, P., Falgarone, E., France, K., Fuente, A., Gerin, M., Giesen, T. F., di Giorgio, A. M., Goicoechea, J. R., Goldsmith, P. F., Güsten, R., Harris, A., Helmich, F., Herbst, E., Hily-Blant, P., Jacobs, K., Jacq, T., Joblin, Ch., Johnstone, D., Kahane, C., Kama, M., Klein, T., Klotz, A., Kramer, C., Langer, W., Lefloch, B., Leinz, C., Lorenzani, A., Lord, S. D., Maret, S., Martin, P. G., Martin-Pintado, J., McCoey, C., Melchior, M., Melnick, G. J., Menten, K. M., Mookerjea, B., Morris, P., Murphy, J. A., Neufeld, D. A., Nisini, B., Pacheco, S., Pagani, L., Parise, B., Pearson, J. C., Pérault, M., Phillips, T. G., Plume, R., Quin, S. -L., Rizzo, R., Röllig, M., Salez, M., Saraceno, P., Schlemmer, S., Simon, R., Schuster, K., van der Tak, F. F. S., Tielens, A. G. G. M., Teyssier, D., Trappe, N., Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Whyborn, N., van der Wiel, M., Yorke, H. W., Yu, S., and Zmuidzinas, J.
Subjects: Astrophysics - Astrophysics of Galaxies
Abstract: We identify a prominent absorption feature at 1115 GHz, detected in first HIFI spectra towards high-mass star-forming regions, and interpret its astrophysical origin. The characteristic hyperfine pattern of the H2O+ ground-state rotational transition, and the lack of other known low-energy transitions in this frequency range, identifies the feature as H2O+ absorption against the dust continuum background and allows us to derive the velocity profile of the absorbing gas. By comparing this velocity profile with velocity profiles of other tracers in the DR21 star-forming region, we constrain the frequency of the transition and the conditions for its formation. In DR21, the velocity distribution of H2O+ matches that of the [CII] line at 158\mu\m and of OH cm-wave absorption, both stemming from the hot and dense clump surfaces facing the HII-region and dynamically affected by the blister outflow. Diffuse foreground gas dominates the absorption towards Sgr B2. The integrated intensity of the absorption line allows us to derive lower limits to the H2O+ column density of 7.2e12 cm^-2 in NGC 6334, 2.3e13 cm^-2 in DR21, and 1.1e15 cm^-2 in Sgr B2., Comment: Accepted for publication in A&A
Published: 2010
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18. Quasi-classical rate coefficient calculations for the rotational (de)excitation of H2O by H2

Author: Faure, A., Crimier, N., Ceccarelli, C., Valiron, P., Wiesenfeld, L., and Dubernet, M. -L.
Subjects: Astrophysics
Abstract: The interpretation of water line emission from existing observations and future HIFI/Herschel data requires a detailed knowledge of collisional rate coefficients. Among all relevant collisional mechanisms, the rotational (de)excitation of H2O by H2 molecules is the process of most interest in interstellar space. To determine rate coefficients for rotational de-excitation among the lowest 45 para and 45 ortho rotational levels of H2O colliding with both para and ortho-H2 in the temperature range 20-2000 K. Rate coefficients are calculated on a recent high-accuracy H2O-H2 potential energy surface using quasi-classical trajectory calculations. Trajectories are sampled by a canonical Monte-Carlo procedure. H2 molecules are assumed to be rotationally thermalized at the kinetic temperature. By comparison with quantum calculations available for low lying levels, classical rates are found to be accurate within a factor of 1-3 for the dominant transitions, that is those with rates larger than a few 10^{-12}cm^{3}s^{-1}. Large velocity gradient modelling shows that the new rates have a significant impact on emission line fluxes and that they should be adopted in any detailed population model of water in warm and hot environments., Comment: 8 pages, 2 figures, 1 table (the online material (4 tables) can be obtained upon request to afaure@obs.ujf-grenoble.fr)
Published: 2007
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19. N2H+ and N2D+ in interstellar molecular clouds. II- Observations

Author: Daniel, F., Cernicharo, J., Roueff, E., Gerin, M., and Dubernet, M. -L.
Subjects: Astrophysics
Abstract: We present observations of the $J$=1--0, 2--1, and 3--2 rotational transitions of N$_2$H$^+$ and N$_2$D$^+$ towards a sample of prototypical dark clouds. The data have been interpreted using non--local radiative transfer models., Comment: 12 pages, 18 figures
Published: 2007

20. The Excitation of N$_2$H$^+$ in Interstellar Molecular Clouds. I - Models

Author: Daniel, F., Cernicharo, J., and Dubernet, M. -L.
Subjects: Astrophysics
Abstract: We present LVG and non-local radiative transfer calculations involving the rotational and hyperfine structure of the spectrum of N$_2$H$^+$ with collisional rate coefficients recently derived by us. The goal of this study is to check the validity of the assumptions made to treat the hyperfine structure and to study the physical mechanisms leading to the observed hyperfine anomalies. We find that the usual hypothesis of identical excitation temperatures for all hyperfine components of the $J$=1-0 transition is not correct within the range of densities existing in cold dense cores, i.e., a few 10$^4$ $\textless$ n(H$_2$) $\textless$ a few 10$^6$ cm$^{-3}$. This is due to different radiative trapping effects in the hyperfine components. Moreover, within this range of densities and considering the typical abundance of N$_2$H$^+$, the total opacity of rotational lines has to be derived taking into account the hyperfine structure. The error made when only considering the rotational energy structure can be as large as 100%. Using non-local models we find that, due to saturation, hyperfine anomalies appear as soon as the total opacity of the $J$=1-0 transition becomes larger than $\simeq$ 20. Radiative scattering in less dense regions enhance these anomalies, and particularly, induce a differential increase of the excitation temperatures of the hyperfine components. This process is more effective for the transitions with the highest opacities for which emerging intensities are also reduced by self-absorption effects. These effects are not as critical as in HCO$^+$ or HCN, but should be taken into account when interpreting the spatial extent of the N$_2$H$^+$ emission in dark clouds., Comment: 13 pages, 12 figures
Published: 2006
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21. Water ortho-to-para ratio in the coma of comet 67P/Churyumov-Gerasimenko

Author: Cheng, Y.-C., primary, Bockelée-Morvan, D., additional, Roos-Serote, M., additional, Crovisier, J., additional, Debout, V., additional, Erard, S., additional, Drossart, P., additional, Leyrat, C., additional, Capaccioni, F., additional, Filacchione, G., additional, Dubernet, M.-L., additional, and Encrenaz, T., additional
Published: 2022
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22. Collisional Excitation Processes Relevant to ISM Studies

Author: Roueff, E., Dubernet, M. L., Flower, D. R., Pottage, J. T., Pfalzner, Susanne, editor, Kramer, Carsten, editor, Straubmeier, Christian, editor, and Heithausen, Andreas, editor
Published: 2004
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23. Water in Star-forming Regions with the Herschel Space Observatory (WISH). I. Overview of Key Program and First Results

Author: van Dishoeck, E. F., Kristensen, L. E., Benz, A. O., Bergin, E. A., Caselli, P., Cernicharo, J., Herpin, F., Hogerheijde, M. R., Johnstone, D., Liseau, R., Nisini, B., Shipman, R., Tafalla, M., van der Tak, F., Wyrowski, F., Aikawa, Y., Bachiller, R., Baudry, A., Benedettini, M., Bjerkeli, P., Blake, G. A., Bontemps, S., Braine, J., Brinch, C., Bruderer, S., Chavarría, L., Codella, C., Daniel, F., de Graauw, Th., Deul, E., di Giorgio, A. M., Dominik, C., Doty, S. D., Dubernet, M. L., Encrenaz, P., Feuchtgruber, H., Fich, M., Frieswijk, W., Fuente, A., Giannini, T., Goicoechea, J. R., Helmich, F. P., Herczeg, G. J., Jacq, T., Jørgensen, J. K., Karska, A., Kaufman, M. J., Keto, E., Larsson, B., Lefloch, B., Lis, D., Marseille, M., McCoey, C., Melnick, G., Neufeld, D., Olberg, M., Pagani, L., Panić, O., Parise, B., Pearson, J. C., Plume, R., Risacher, C., Salter, D., Santiago-García, J., Saraceno, P., Stäuber, P., van Kempen, T. A., Visser, R., Viti, S., Walmsley, M., Wampfler, S. F., and Yıldız, U. A.
Published: 2011
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24. VAMDC as a Resource for Atomic and Molecular Data and the New Release of VALD

Author: Kupka F. and Dubernet M.-L.
Subjects: databases, catalogs, atomic data, molecular data, Astronomy, QB1-991
Abstract: The Virtual Atomic and Molecular Data Centre (VAMDC) is an EU-FP7 project devoted to build a common electronic infrastructure for the exchange and distribution of atomic and molecular data. Within VAMDC scientists from many different disciplines in atomic and molecular physics collaborate with users of their data and also with scientists and engineers from the information and communication technology community. In this presentation, an overview of the current status of VAMDC and its capabilities is provided. In the second part of the presentation I will focus on one of the databases which have become a part of the VAMDC platform, the Vienna Atomic Line Data Base (VALD). VALD has developed into a well-known resource of atomic data for spectroscopy, particularly in astrophysics. A new release, VALD-3, will provide numerous improvements over its predecessor. This particularly relates to the data contents where new sets of atomic data for both precision spectroscopy (i.e., with data for observed energy levels) as well as opacity calculations (i.e., with data involving predicted energy levels) have been included. Data for selected diatomic molecules have been added, and the new system for data distribution and data referencing provides more convenience in using the third release of VALD.
Published: 2011
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25. Atomic and Molecular Databases Open Science for a sustainable world

Author: Dubernet, M. L., primary, Berriman, G.B., additional, Barklem, P., additional, Choi, K., additional, Foster, A., additional, Gordon, I., additional, Hill, C., additional, Kim, J., additional, Kwon, D.H., additional, Linnartz, H., additional, Ralchenko, Yu., additional, Salama, F., additional, Shmagun, H., additional, Schilke, P., additional, Seo, D., additional, Shim, J., additional, Shin, S., additional, Song, M.-Y., additional, Tennyson, J., additional, and Vastel, C., additional
Published: 2021
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26. New H2O–H2O collisional rate coefficients for cometary applications

Author: Boursier, C, primary, Mandal, B, additional, Babikov, D, additional, and Dubernet, M L, additional
Published: 2020
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27. Rotational state dependence of rate constants for the reaction of ions with asymmetric top molecules at very low temperatures: application to the N+/H2O system

Author: Dubernet, M. L. and McCarroll, R.
Published: 1990
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28. Collisional Excitation Processes Relevant to ISM Studies

Author: Roueff, E., primary, Dubernet, M. L., additional, Flower, D. R., additional, and Pottage, J. T., additional
Published: 1997
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29. Citation of evolving data in distributed asynchronous infrastructures

Author: Zwölf, C. M., primary, Moreau, N., additional, Ba, Y. A., additional, and Dubernet, M. L., additional
Published: 2019
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30. New H2O–H2O collisional rate coefficients for cometary applications.

Author: Boursier, C, Mandal, B, Babikov, D, and Dubernet, M L
Subjects: POTENTIAL energy surfaces, BIG data, GEOTHERMAL resources, RADIATIVE transfer, ATMOSPHERIC models
Abstract: We re-introduce a semiclassical methodology based on theories developed for the determination of broadening coefficients. We show that this simple and extremely fast methodology provides results that are in good agreement with results obtained using the more sophisticate MQCT approach. This semiclassical methodology could be an alternative approach which allows to provide large sets of collisional data for very complex molecular systems. It saves time both on the determination of potential energy surfaces and on the collisional dynamical calculations. In addition, this paper provides more complete sets of rotational de-excitation cross-sections and rate coefficients of H2O perturbed by a thermal average of water molecules. Those data can be used in the radiative transfer modelling of cometary atmospheres. [ABSTRACT FROM AUTHOR]
Published: 2020
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31. Rotational excitation of sulfur monoxide by collisions with helium at low temperature.

Author: Lique, F., Spielfiedel, A., Dubernet, M.-L., and Feautrier, N.
Subjects: EXCITON theory, SULFUR, COLLISIONS (Nuclear physics), HELIUM, LOW temperatures, ELECTRONIC excitation
Abstract: We present two new two-dimensional potential-energy surfaces for the SO–He system calculated at SO r distance frozen at its experimental minimum-energy distance. Both are obtained at the RCCSD(T) level using two different basis sets (AVTZ and AVQZ) for the three atoms. Bond functions are placed at mid-distance between the SO center of mass and He for a better description of the van der Waals well. Close-coupling calculations of the collisional excitation cross sections of the fine-structure levels of SO by He are calculated at low energies. The exact level splitting is taken into account. It is found that the results obtained from the two surfaces are very similar, except for some small differences observed in the region of resonances at low energies. The propensity rules between fine-structure levels are studied, it is shown that F-conserving cross sections are much larger for high-N rotational levels than cross sections between F-changing levels, as expected from theoretical considerations. The use of infinite order sudden recoupling techniques from spin-free cross sections is investigated. Excitation rate coefficients among fine-structure levels are calculated at low temperatures. [ABSTRACT FROM AUTHOR]
Published: 2005
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32. Selective hyperfine excitation of N2H+ by He: Potential energy surface, cross sections, and propensity rules.

Author: Daniel, F., Dubernet, M.-L., and Meuwly, Markus
Subjects: *HYPERFINE interactions, *PHYSICS, *HYPERFINE structure, *ELECTRONIC excitation, *PHYSICAL sciences, *DYNAMICS
Abstract: We present potential energy surfaces for the He-N2H+ system adiabatically corrected for the zero-point motion along the intermolecular stretching vibrations v1=0 and v1=1. The potentials are extended to shorter He-N2H+ separations which makes them useful for scattering calculations. Close coupling calculations of the spinless S matrices for the rotational excitation of N2H+ by He are presented, and recoupling techniques to obtain collisional excitation cross sections between the N2H+ hyperfine levels are used. The propensity rules between hyperfine levels are investigated for the case where two nuclear spins are involved. It is found that the only well defined propensity rule is ΔF=ΔF1=Δj and that calculations are required in order to obtain the relative intensities of the two-spin hyperfine cross sections. © 2004 American Institute of Physics. [ABSTRACT FROM AUTHOR]
Published: 2004
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33. Raman Q and S line broadening and shifting coefficients: some commonly used assumptions revisited

Author: Dubernet, M.-L. and Tuckey, P.A.
Published: 1999
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34. Collisional excitation rate coefficients of N2H+ by He

Author: Daniel, F., Dubernet, M.-L, Meuwly, M., Cernicharo, J., Pagani, L., Daniel, F., Dubernet, M.-L, Meuwly, M., Cernicharo, J., and Pagani, L.
Abstract: Using a recoupling technique with close-coupling spin-free calculations de-excitation rate coefficients are obtained among hyperfine transitions for He colliding with N2H+. A recently determined potential energy surface suitable for scattering calculations is used to investigate rate coefficients for temperatures between 5 and 50 K, and for the seven lowest rotational levels of N2H+. Fitting functions are provided for the Maxwellian averaged opacity tensors and for the rotational de-excitation collisional rate coefficients. The fitting functions for the opacity tensors can be used to calculate hyperfine (de)-excitation rate coefficients among elastic and inelastic rotational levels, and among the corresponding magnetic sublevels of the hyperfine structure. Certain dynamical approximations are investigated and found to be invalid
Published: 2017

35. On the effects of an internal barrier on fast four-atom ion–molecule reactions.

Author: Dubernet, M. L., Rebentrost, F., Kompa, K. L., and Levine, R. D.
Subjects: *CHEMICAL reactions, *ADIABATIC invariants, *IONS, *MOLECULES, *POTENTIAL energy surfaces
Abstract: We investigate the influence of an internal barrier on an exothermic adiabatic reaction model between diatomic ions and molecules. Reaction cross-sections are calculated from quasi-classical trajectories for different initial vibrational and rotational states of the reactants and for relative collision energies in the range from 0.01 to 3 eV. It is shown that the height of a late internal barrier strongly influences both the characteristics of the state-selected cross-sections and the energy distributions of the products. In contrast to complex formation in the entrance region according to the Langevin model our analysis emphasizes the role of the full potential energy surface for an understanding of the dynamics of ion–molecule reactions. © 1996 American Institute of Physics. [ABSTRACT FROM AUTHOR]
Published: 1996
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36. Quantum and semiclassical calculations of H[sub 2]-He vibrational line-shape parameters...

Author: Joubert, P., Dubernet, M.-L., Bonamy, J., and Robert, D.
Subjects: *POTENTIAL energy surfaces
Abstract: Investigates the quantum close-coupling (CC) and semiclassical (SC) calculations of broadening and shifting coefficients of rovibrational lines using an ab initio potential energy surface. Comparisons between CC, RB calculations and experimental data; Energy dependence of the broadening and shifting cross-sections.
Published: 1997
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37. The virtual atomic and molecular data centre (VAMDC) consortium

Author: Dubernet, M. L., Antony, B. K., Ba, Y. A., Babikov, Yu L., Bartschat, K., Boudon, V., Braams, B. J., Chung, H-K, Daniel, F., Delahaye, F., Del Zanna, G., de Urquijo, J., Dimitrijevic, M. S., Domaracka, A., Doronin, M., Drouin, B. J., Endres, C. P., Fazliev, A. Z., Gagarin, S. V., Gordon, I. E., Gratier, P., Heiter, Ulrike, Hill, C., Jevremovic, D., Joblin, C., Kasprzak, A., Krishnakumar, E., Leto, G., Loboda, P. A., Louge, T., Maclot, S., Marinkovic, B. P., Markwick, A., Marquart, Thomas, Mason, H. E., Mason, N. J., Mendoza, C., Mihajlov, A. A., Millar, T. J., Moreau, N., Mulas, G., Pakhomov, Yu, Palmeri, P., Pancheshnyi, S., Perevalov, V. I., Piskunov, Nikolai, Postler, J., Quinet, P., Quintas-Sanchez, E., Ralchenko, Yu, Rhee, Y-J, Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T., Sahal-Brechot, S., Scheier, P., Schlemmer, S., Schmitt, B., Stempels, Eric H. C., Tashkun, S., Tennyson, J., Tyuterev, Vl G., Vujcic, V., Wakelam, V., Walton, N. A., Zatsarinny, O., Zeippen, C. J., Zwoelf, C. M., Dubernet, M. L., Antony, B. K., Ba, Y. A., Babikov, Yu L., Bartschat, K., Boudon, V., Braams, B. J., Chung, H-K, Daniel, F., Delahaye, F., Del Zanna, G., de Urquijo, J., Dimitrijevic, M. S., Domaracka, A., Doronin, M., Drouin, B. J., Endres, C. P., Fazliev, A. Z., Gagarin, S. V., Gordon, I. E., Gratier, P., Heiter, Ulrike, Hill, C., Jevremovic, D., Joblin, C., Kasprzak, A., Krishnakumar, E., Leto, G., Loboda, P. A., Louge, T., Maclot, S., Marinkovic, B. P., Markwick, A., Marquart, Thomas, Mason, H. E., Mason, N. J., Mendoza, C., Mihajlov, A. A., Millar, T. J., Moreau, N., Mulas, G., Pakhomov, Yu, Palmeri, P., Pancheshnyi, S., Perevalov, V. I., Piskunov, Nikolai, Postler, J., Quinet, P., Quintas-Sanchez, E., Ralchenko, Yu, Rhee, Y-J, Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T., Sahal-Brechot, S., Scheier, P., Schlemmer, S., Schmitt, B., Stempels, Eric H. C., Tashkun, S., Tennyson, J., Tyuterev, Vl G., Vujcic, V., Wakelam, V., Walton, N. A., Zatsarinny, O., Zeippen, C. J., and Zwoelf, C. M.
Abstract: The Virtual Atomic and Molecular Data Centre (VAMDC) Consortium is a worldwide consortium which federates atomic and molecular databases through an e-science infrastructure and an organisation to support this activity. About 90% of the inter-connected databases handle data that are used for the interpretation of astronomical spectra and for modelling in many fields of astrophysics. Recently the VAMDC Consortium has connected databases from the radiation damage and the plasma communities, as well as promoting the publication of data from Indian institutes. This paper describes how the VAMDC Consortium is organised for the optimal distribution of atomic and molecular data for scientific research. It is noted that the VAMDC Consortium strongly advocates that authors of research papers using data cite the original experimental and theoretical papers as well as the relevant databases.
Published: 2016
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38. The virtual atomic and molecular data centre (VAMDC) consortium

Author: Dubernet, M L, primary, Antony, B K, additional, Ba, Y A, additional, Babikov, Yu L, additional, Bartschat, K, additional, Boudon, V, additional, Braams, B J, additional, Chung, H-K, additional, Daniel, F, additional, Delahaye, F, additional, Zanna, G Del, additional, Urquijo, J de, additional, Dimitrijević, M S, additional, Domaracka, A, additional, Doronin, M, additional, Drouin, B J, additional, Endres, C P, additional, Fazliev, A Z, additional, Gagarin, S V, additional, Gordon, I E, additional, Gratier, P, additional, Heiter, U, additional, Hill, C, additional, Jevremović, D, additional, Joblin, C, additional, Kasprzak, A, additional, Krishnakumar, E, additional, Leto, G, additional, Loboda, P A, additional, Louge, T, additional, Maclot, S, additional, Marinković, B P, additional, Markwick, A, additional, Marquart, T, additional, Mason, H E, additional, Mason, N J, additional, Mendoza, C, additional, Mihajlov, A A, additional, Millar, T J, additional, Moreau, N, additional, Mulas, G, additional, Pakhomov, Yu, additional, Palmeri, P, additional, Pancheshnyi, S, additional, Perevalov, V I, additional, Piskunov, N, additional, Postler, J, additional, Quinet, P, additional, Quintas-Sánchez, E, additional, Ralchenko, Yu, additional, Rhee, Y-J, additional, Rixon, G, additional, Rothman, L S, additional, Roueff, E, additional, Ryabchikova, T, additional, Sahal-Bréchot, S, additional, Scheier, P, additional, Schlemmer, S, additional, Schmitt, B, additional, Stempels, E, additional, Tashkun, S, additional, Tennyson, J, additional, Tyuterev, Vl G, additional, Vujčić, V, additional, Wakelam, V, additional, Walton, N A, additional, Zatsarinny, O, additional, Zeippen, C J, additional, and Zwölf, C M, additional
Published: 2016
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39. Rotational state dependence of ion-polar molecule reactions at very low temperature

Author: Dubernet, M. L. and McCarroll, R.
Published: 1989
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40. VO-Paris Data Centre (VO-PDC)

Author: Le Petit, F., Aboudarham, J., Thuillot, W., Le Sidaner, Pierre, Alimi, J.-M., Désert, J.-M., Barache, C., Berthier, J., Boisson, C., Bouquillon, S., Combes, F., Delahaye, F., Deleflie, F., Di Matteo, P., Domisse, L., Dubernet, M.-L., Erard, S., Gambis, D., Guibert, J., Haigron, R., Hennebelle, P., Jégouzo, I., Henry, F., Heydari-Malayeri, M., Languignon, D., Lambert, S., Mamon, G., Normand, J., Martin, J.-M., Moreau, N., Pérault, M., Rasera, Y., Roueff, E., Roy, F., Royer, F., Sahal-Bréchot, S., Sarkissian, Alain, Sartoretti, P., Schneider, Jodi, Tajhamady, F., Zolotukhin, I., Zwolf, C.-M., Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Centre National de la Recherche Scientifique (CNRS)-Université de Lille-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Observatoire de Paris - Site de Paris (OP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Systèmes de Référence Temps Espace (SYRTE), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université d'Orléans (UO), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), PSL Research University (PSL)-PSL Research University (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), IMPEC - LATMOS, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM]
Abstract: International audience; VO-Paris Data Centre (VO-PDC) is a new data centre that gathers ten laboratories in Paris area (GEPI, IAP, IMCCE, LATMOS, LERMA, LESIA, LPMAA, LUTH, SYRTE, USN). It is specialized in the development of Virtual Observatory services. The objective of this federation is to build a sustainable infrastructure to offer high quality diffusion services to the community. It gives also the opportunity to promote exchanges and to share expertise on the development of VO services between scientists and computer engineers. VO-PDC is a multidisciplinary data center. Its main axes are atomic and molecular physics, VO-Theory, planetology and solar physics. It also develops several services concerning the diffusion of traditional astronomical data, catalogues, as well as geodesy services.
Published: 2011

41. VAMDC: Databases of Calculated Spectral Lines of Ethylene and Methane

Author: ROTGER, Maud, Bourgeois, Marie-Thérèse, Ba, Y. A., Boudon, Vincent, Wenger, Christian, Bonhommeau, David, Daumont, L., Tyuterev, Vladimir G., Dubernet, M.-L., Boudon, Vincent, Virtual Atomic and Molecular Data Center - VAMDC - - EC:FP7:INFRA2009-07-01 - 2012-12-31 - 239108 - VALID, Groupe de spectrométrie moléculaire et atmosphérique - UMR 7331 ( GSMA ), Université de Reims Champagne-Ardenne ( URCA ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Interdisciplinaire Carnot de Bourgogne ( LICB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique ( LERMA ), École normale supérieure - Paris ( ENS Paris ) -Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université de Cergy Pontoise ( UCP ), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique ( CNRS ), European Project : 239108,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-2,VAMDC ( 2009 ), Groupe de spectrométrie moléculaire et atmosphérique (GSMA), Université de Reims Champagne-Ardenne (URCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), European Project: 239108,EC:FP7:INFRA,FP7-INFRASTRUCTURES-2008-2,VAMDC(2009), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), and École normale supérieure - Paris (ENS Paris)
Subjects: [CHIM.THEO]Chemical Sciences/Theoretical and/or physical chemistry, [CHIM.THEO] Chemical Sciences/Theoretical and/or physical chemistry, [ CHIM.THEO ] Chemical Sciences/Theoretical and/or physical chemistry
Published: 2011

42. Herschel/HIFI discovery of interstellar chloronium (H2Cl+) [Letter]

Author: Lis, D. C., Pearson, J. C., Neufeld, D. A., Schilke, P., Mueller, H. S. P., Gupta, H., Bell, T. A., Comito, C., Phillips, T. G., Bergin, E. A., Ceccarelli, C., Goldsmith, P. F., Blake, G. A., Bacmann, A., Baudry, A., Benedettini, M., Benz, A., Black, J., Boogert, A., Bottinelli, S., Cabrit, S., Caselli, P., Castets, A., Caux, E., Cernicharo, J., Codella, C., Coutens, A., Crimier, N., Crockett, N. R., Daniel, F., Demyk, K., Dominic, C., Dubernet, M. -L., Emprechtinger, M., Encrenaz, P., Falgarone, E., Fuente, A., Gerin, M., Giesen, T. F., Goicoechea, J. R., Helmich, F., Hennebelle, P., Henning, Th., Herbst, E., Hily-Blant, P., Hjalmarson, A., Hollenbach, D., Jack, T., Joblin, C., Johnstone, D., Kahane, C., Kama, M., Kaufman, M., Klotz, A., Langer, W. D., Larsson, B., Le Bourlot, J., Lefloch, B., Le Petit, F., Li, D., Liseau, R., Lord, S. D., Lorenzani, A., Maret, S., Martin, P. G., Melnick, G. J., Menten, K. M., Morris, P., Murphy, J. A., Nagy, Z., Nisini, B., Ossenkopf, V., Pacheco, S., Pagani, L., Parise, Berengere, Perault, M., Plume, R., Qin, S. -L., Roueff, E., Salez, M., Sandqvist, A., Saraceno, P., Schlemmer, S., Schuster, K., Snell, R., Stutzki, J., Tielens, A., Trappe, N., van der Tak, F. F. S., van der Wiel, M. H. D., van Dishoeck, E., Vastel, C., Viti, S., Wakelam, V., Walters, A., Wang, S., Wyrowski, F., Yorke, H. W., Yu, S., Zmuidzinas, J., Delorme, Y., Desbat, J. -P., Guesten, R., Krieg, J. -M., and Delforge, B.
Subjects: QB
Abstract: We report the first detection of chloronium, H2Cl+, in the interstellar medium, using the HIFI instrument aboard the Herschel Space Observatory. The 212–101 lines of ortho-HCl+ and ortho-HCl+ are detected in absorption towards NGC 6334I, and the 111–000 transition of para-HCl+ is detected in absorption towards NGC 6334I and Sgr B2(S). The H2Cl+ column densities are compared to those of the chemically-related species HCl. The derived HCl/H2Cl+ column density ratios, ~1–10, are within the range predicted by models of diffuse and dense photon dominated regions (PDRs). However, the observed H2Cl+ column densities, in excess of 1013 cm-2, are significantly higher than the model predictions. Our observations demonstrate the outstanding spectroscopic capabilities of HIFI for detecting new interstellar molecules and providing key constraints for astrochemical models.
Published: 2010

43. On behalf of Consortium (presented by N. Walton, Cambridge, UK) 'VAMDC: Virtual Atomic and Molecular Data Center - Poster

Author: Dubernet, M. L., Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Francois, Francoise
Subjects: [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published: 2010

44. On behalf of Consortium (presented by L. Molina, LPMAA) 'VAMDC: Virtual Atomic and Molecular Data Center - Poster

Author: Dubernet, M. L., Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), and Francois, Francoise
Subjects: [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Published: 2010

45. Virtual Atomic and Molecular Data Center

Author: Dubernet, M. L., Vincent Boudon, Culhane, J. L., Dimitrijevic, M. S., Fazliev, A. Z., Joblin, C., Kupka, F., Leto, G., Pierre Le Sidaner, Loboda, P. A., Mason, H. E., Mason, N. J., Mendoza, C., Mulas, G., Millar, T. J., Nuñez, L. A., Perevalov, V. I., Piskunov, N., Ralchenko, Y., Rixon, G., Rothman, L. S., Roueff, E., Ryabchikova, T. A., Ryabtsev, A., Sahal-Brechot, S., Bernard Schmitt, Schlemmer, S., Tennyson, J., Tyuterev, Vladimir G., Walton, N. A., Valentine Wakelam, Zeippen, C. J., Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique ( LPMAA ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Univers et Théories ( LUTH ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire Interdisciplinaire Carnot de Bourgogne ( LICB ), Université de Bourgogne ( UB ) -Centre National de la Recherche Scientifique ( CNRS ), Mullard Space Science Laboratory ( MSSL ), University College of London [London] ( UCL ), Astronomical Observatory Belgrade, V.E. Zuev Institute of Atmospheric Optics ( IAO ), Siberian Branch of the Russian Academy of Sciences ( SB RAS ), Univ Toulouse UPS, Ctr Etud Spatiale Rayonnements, F-31062 Toulouse 9, France, Centre Etud Spatiale Rayonnements Toulouse, University Vienna, Fac Math, Osserv Astrofis Catania, Ist Nazl Astrofis, Observatoire de Paris - Site de Meudon ( OBSPM ), Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS ), All-Russian Scientific Research Institute of Technical Physics RFNTC VNIITF, Centre for Mathematical Science, Dept Appl Math & Theoret Phys Cambridge, Centre for Mathematical Science, Open university Faculty of Sciences, Universidad de Los Andes Venezuela, CeCalCULA, Corp Parque Tecnol Merida, Ctr Calculo Cient, Universidad de Los Andes Venezuela, Instituto Venezolano Investigaciones Cientificas, Ctr Fis, Caracas, Instituto Venezolano Investigaciones Cientificas, Osservatorio Astronomico di Cagliari, Ist Nazl Astrofis, Osservatorio Astronomico di Cagliari, Queen's UniversityBelfast, Sch Math & Phys, Universidad Industrial de Santander [Bucaramanga] ( UIS ), AMOR 2010, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux ( L3AB ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Observatoire aquitain des sciences de l'univers ( OASU ), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Laboratoire d'Astrophysique de Bordeaux [Pessac] ( LAB ), Université de Bordeaux ( UB ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Bordeaux ( UB ), Laboratoire de Physique Moleculaire pour l'Atmosphere et l'Astrophysique (LPMAA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Interdisciplinaire Carnot de Bourgogne (ICB), Université de Bourgogne (UB)-Centre National de la Recherche Scientifique (CNRS), Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Astronomical Observatory Belgrade (AOB), V.E. Zuev Institute of Atmospheric Optics (IAO), Siberian Branch of the Russian Academy of Sciences (SB RAS), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Universidad de Los Andes [Mérida, Venezuela] (ULA), INAF - Osservatorio Astronomico di Cagliari (OAC), Istituto Nazionale di Astrofisica (INAF), Queen's University [Belfast] (QUB), Universidad Industrial de Santander [Bucaramanga] (UIS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), Francois, Francoise, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Interdisciplinaire Carnot de Bourgogne (LICB), Universidad de Los Andes [Venezuela] (ULA), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.EP] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ PHYS.ASTR.EP ] Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [ SDU.ASTR.EP ] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: (special issue HighRus2009). VAMDC; International audience
Published: 2010

46. Detection of OH+ and H2O+ towards Orion KL

Author: Gupta, H., Rimmer, P., Pearson, J. C., Yu, S., Herbst, E., Harada, N., Bergin, E. A., Neufeld, D. A., Melnick, G. J., Bachiller, R., Baechtold, W., Bell, T. A., Blake, G. A., Caux, E., Ceccarelli, C., Cernicharo, J., Chattopadhyay, G., Comito, C., Cabrit, S., Crockett, N. R., Daniel, F., Falgarone, E., Diez-Gonzalez, M. C., Dubernet, M.-L., Erickson, N., Emprechtinger, M., Encrenaz, P., Gerin, M., Gill, J. J., Giesen, T. F., Goicoechea, J. R., Goldsmith, P. F., Joblin, C., Johnstone, D., Langer, W. D., Larsson, B., Latter, W. B., Lin, R. H., Lis, D. C., Liseau, R., Lord, S. D., Maiwald, F. W., Maret, S., Martin, P. G., Martin-Pintado, J., Menten, K. M., Morris, P., Müller, H. S. P., Murphy, J. A., Nordh, L. H., Olberg, M., Ossenkopf, V., Pagani, L., Pérault, M., Phillips, T. G., Plume, R., Qin, S.-L., Salez, M., Samoska, L. A., Schilke, P., Schlecht, E., Schlemmer, S., Szczerba, R., Stutzki, J., Trappe, N., Van Der Tak, F. F. S., Vastel, C., Wang, S., Yorke, H. W., Zmuidzinas, J., Boogert, A., Güsten, R., Hartogh, P., Honingh, N., Karpov, A., Kooi, J., Krieg, J.-M., Schieder, R., Zaal, P., Faure, Alexandre, Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: ComputingMilieux_MISCELLANEOUS
Abstract: International audience
Published: 2010

47. N2H+ and N2D+ in interstellar molecular clouds. II- Observations

Author: Daniel, Fabien, Cernicharo, José, Roueff, E., Gerin, M., and Dubernet, M. L.
Subjects: clouds: molecules: abundances [ISM], Astrophysics (astro-ph), individual (TMC1, L183) [ISM], Radiative transfer, FOS: Physical sciences, ISM: individual (TMC1, L183), Line: formation: profiles, Astrophysics, ISM: clouds: molecules: abundances, Molecular processes, formation: profiles [Line]
Abstract: Accepted for publication in The Astrophysical Journal (ApJ)., We present observations of the J=1-0, 2-1, and 3-2 rotational transitions of N2H+ and N2D+ towards a sample of prototypical dark clouds. The data have been interpreted using non-local radiative transfer models., The authors acknowledge funding support under grants PNAYA2000-1784, ESP2001-4516, PNAYA2002-10113-E, ESP2002-01627, PNAYA2003-02785, PNAYA2004-0579 and the Madrid DGU PRICIT Program S-0505/ESP-0237 (ASTROCAM).
Published: 2007

48. Latest VO developments at Paris VO Data Center

Author: Le Sidaner, P., Dubernet, M. -L, Simon, G., Aboudarham, J., Baillard, A., Barache, C., Boone, F., Chilingarian, I., Dantel-Fort, M., Desert, J. M., Didelon, P., Egret, D., Guibert, J., Hebrard, G., Lainey, V., Magnard, F., Chiara Marmo, Martin, J. M., Pelat, D., Renié, C., Sarkissian, A., Schneider, J., Theureau, G., Vachier, F., Observatoire de Paris - Site de Paris (OP), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ingénieurs, Techniciens et Administratifs, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Physique solaire, Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, D. Barret, F. Casoli, T. Contini, G. Lagache, A. Lecavelier, and and L. Pagani (eds)
Subjects: [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: International audience; Paris VO Data Center aims at providing VO access to its databases ressources, at participating to international standards developments, at implementing VO compliant simulation codes and data visuali- sation and analysis softwares. We will present some of the latest VO developments involving ressources from Paris VO Data Center, i.e, the first simple spectra access for data of the Nanay radiotelescope observatory, a validator for Simple Spectra Access protocols and its implementation tools, a Cone-search access to the exoplanet catalog, a pipeline for images processing to make them ”science-ready” in vo-format, implemen- tation of Simple Image Access using Geographic Information System in databases. Developments involving other ressources may be found in their own contributions to this meeting.
Published: 2006

49. Influence of a new potential energy surface on the rotational (de)excitation of H2O by H2 at low temperature

Author: Dubernet, M.-L., Daniel, F., Grosjean, A., Faure, A., Valiron, P., Wernli, M., Wiesenfeld, L., Rist, C., Noga, J., Tennyson, J., Laboratoire d'Astrophysique de Grenoble (LAOG), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Abstract: International audience; Aims.Using a newly determined 5D potential energy surface for H2-H2O we provide an extended and revised set of rate coefficients for de-excitation of the lowest 10 para- and 10 ortho- rotational levels of H2O by collisions with para-(j=0) and ortho-H2(j=1), for kinetic temperatures from 5 K to 20 K. Methods: .Our close coupling scattering calculations involve a slightly improved set of coupled channels with respect to previous calculations. In addition, we discuss the influence of several features of this new 5D interaction on the rotational excitation cross sections. Results: . The new interaction potential leads to significantly different rate coefficients for collisions with para-H2 (j=0). In particular the de-excitation rate coefficient for the 110 to 101 transition is increased by up to 300% at 5 K. At 20 K this increase is 75%. Rate coefficients for collisions with ortho-H2(j=1) are modified to a lesser extent, by up to 40%. The influence of the new potential on collisions with both para-(j=0) and ortho-H2(j=1) is expected to become less pronounced at higher temperatures.
Published: 2006
Full Text: View/download PDF

50. VO Paris Federation

Author: Simon, G., Dubernet, M. L., Le Sidaner, P., Aboudarham, J., Barache, C., Berthier, J., Boone, F., Borsenberger, J., Caillat, M., Igor Chilingarian, Crovisier, J., Dantel-Fort, M., Debatz, B., Dedieu, C., Egret, D., Gontier, A. M., Guibert, J., Guillaume, D., Haigron, R., Hennebelle, P., Jegouzo, I., Lainey, V., Le Bourlot, J., Le Petit, F., Martin, J. M., Micheneau, P., Moreau, N., Pelat, D., Perault, M., Prugniel, P., Renié, C., Roques, F., Royer, F., Schneider, J., Tajahmady, F., Theureau, G., Thuillot, W., Tran-Minh, F., Vachier, F., Vetois, J., Viallefond, F., Baillard, A., Bertin, E., Desert, J. M., Ferlet, R., Hebrard, G., Magnard, F., Malapert, J. -C, Marquette, J. B., Marmo, C., Mellier, Y., Sarkissian, A., Mccracken, H., Lesquoy, E., Didelon, P., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ingénieurs, Techniciens et Administratifs, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Pôle Planétologie du LESIA, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Physique solaire, Institut de Mécanique Céleste et de Calcul des Ephémérides (IMCCE), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS), Groupe Astrométrie et Planétologie (GAP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université de Lille-Centre National de la Recherche Scientifique (CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Service d'aéronomie (SA), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), CEA- Saclay (CEA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), C. Gabriel, C. Arviset, D. Ponz and E. Solano, eds., Henry, Florence, and C. Gabriel, C. Arviset, D. Ponz and E. Solano, eds.
Subjects: [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], PADC
Abstract: International audience; VO Paris Federation is a partnership between Paris Obser-vatory, IAP, IPSL and CEA. Its objectives are to provide VO access toits databases ressources, contribute to international standards develop-ments, implement VO compliant simulation codes and data visualisa-tion and analysis software. The various activities are organised into por-tals whose functions are (i) to provide visibility and information on theprojects and (ii) to encourage collaborations. The portals are linked tothematic activities and resources: solar system (ephemerides, astrometry,physical characteristic of small bodies of the solar system, planetology),reference systems, exoplanet database, legacy (archives from the Nan ̧cayRadio Telescope, some specific data from the DENIS and EROS surveys,MAMA), solar physics, stellar and galactic databases and services, atomicand molecular databases and services, simulation codes and data analysis.
Published: 2005

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