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9 results on '"Goicoechea, Javier R. [0000-0001-7046-4319]"'

1. Gas phase Elemental abundances in Molecular cloudS (GEMS) VII. Sulfur elemental abundance

Author

Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Universidad Complutense de Madrid, Fundación Ramón Areces, Ministerio de Universidades (España), Fuente, A. [0000-0001-6317-6343], Rivière-Marichalar, P. [0000-0003-0969-8137], Navarro-Almaida, D. [0000-0002-8499-7447], Kramer; C. [0000-0002-4908-4925], Bachiller, R. [0000-0002-5331-5386], Goicoechea, Javier R. [0000-0001-7046-4319], Jiménez-Serra, I. [0000-0003-4493-8714], Martín-Doménech, R. [0000-0001-6496-9791], Spezzano, S. [0000-0002-6787-5245], Muñoz-Caro, G. [0000-0001-7003-7368], Fuente, A., Rivière-Marichalar, P., Beitia-Antero, L., Caselli, P., Wakelam, V., Esplugues, G., Rodríguez-Baras, M., Navarro-Almaida, D., Gerin, M., Kramer; C., Bachiller, R., Goicoechea, Javier R., Jiménez-Serra, Izaskun, Loison, J. C., Ivlev, A., Martín-Doménech, R., Spezzano, S., Roncero, Octavio, Muñoz-Caro, G., Cazaux, S., Marcelino, Nuria, Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Universidad Complutense de Madrid, Fundación Ramón Areces, Ministerio de Universidades (España), Fuente, A. [0000-0001-6317-6343], Rivière-Marichalar, P. [0000-0003-0969-8137], Navarro-Almaida, D. [0000-0002-8499-7447], Kramer; C. [0000-0002-4908-4925], Bachiller, R. [0000-0002-5331-5386], Goicoechea, Javier R. [0000-0001-7046-4319], Jiménez-Serra, I. [0000-0003-4493-8714], Martín-Doménech, R. [0000-0001-6496-9791], Spezzano, S. [0000-0002-6787-5245], Muñoz-Caro, G. [0000-0001-7003-7368], Fuente, A., Rivière-Marichalar, P., Beitia-Antero, L., Caselli, P., Wakelam, V., Esplugues, G., Rodríguez-Baras, M., Navarro-Almaida, D., Gerin, M., Kramer; C., Bachiller, R., Goicoechea, Javier R., Jiménez-Serra, Izaskun, Loison, J. C., Ivlev, A., Martín-Doménech, R., Spezzano, S., Roncero, Octavio, Muñoz-Caro, G., Cazaux, S., and Marcelino, Nuria

Abstract

Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30m large program aimed at determining the elemental abundances of carbon (C), oxygen (O), nitrogen (N), and sulfur (S) in a selected set of prototypical star-forming filaments. In particular, the elemental abundance of S remains uncertain by several orders of magnitude and its determination is one of the most challenging goals of this program. We have carried out an extensive chemical modeling of the fractional abundances of CO, HCO$^+$, HCN, HNC, CS, SO, H$_2$S, OCS, and HCS$^+$ to determine the sulfur depletion toward the 244 positions in the GEMS database. These positions sample visual extinctions from A$_V$ $\sim$ 3 mag to $>$50 mag, molecular hydrogen densities ranging from a few 10$^3$~cm$^{-3}$ to 3$\times$10$^6$~cm$^{-3}$, and T$_k$ $\sim$ 10$-$35 K. Most of the positions in Taurus and Perseus are best fitted assuming early-time chemistry, t=0.1 Myr, $\zeta_{H_2}$$\sim$ (0.5$-$1)$\times$10$^{-16}$ s$^{-1}$, and [S/H]$\sim$1.5$\times$10$^{-6}$. On the contrary, most of the positions in Orion are fitted with t=1~Myr and $\zeta_{H_2}$$\sim$ 10$^{-17}$ s$^{-1}$. Moreover, $\sim$40% of the positions in Orion are best fitted assuming the undepleted sulfur abundance, [S/H]$\sim$1.5$\times$10$^{-5}$. Our results suggest that sulfur depletion depends on the environment. While the abundances of sulfur-bearing species are consistent with undepleted sulfur in Orion, a depletion factor of $\sim$20 is required to explain those observed in Taurus and Perseus. We propose that differences in the grain charge distribution in the envelopes of the studied clouds might explain these variations. The shocks associated with past and ongoing star formation could also contribute to enhance [S/H] in Orion.

Published
2023

2. The extremely sharp transition between molecular and ionized gas in the Horsehead nebula

Author

Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Hernández-Vera, C. [0009-0009-2320-7243], Guzmán, V. V. [0000-0003-4784-3040], Goicoechea, Javier R. [0000-0001-7046-4319], #NODATA#, Le Petit, F. [0000-0001-8738-6724], Gerin, M. [0000-0002-2418-7952], Bron, E. [0000-0003-1532-7818], Roueff, E. [0000-0002-4949-8562], Schirmer, T. [0000-0002-8086-4890], Carpenter, J. [0000-0003-2251-0602], Gratier, P. [0000-0002-6636-4304], Hernández-Vera, C., Guzmán, V. V., Goicoechea, Javier R., Maillard, V., Pety, J., Le Petit, F., Gerin, M., Bron, E., Roueff, E., Abergel, A., Schirmer, T., Carpenter, J., Gratier, P., Gordon, K., Misselt, K., Agencia Nacional de Investigación y Desarrollo (Chile), Fondo Nacional de Desarrollo Científico y Tecnológico (Chile), Ministerio de Ciencia e Innovación (España), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Hernández-Vera, C. [0009-0009-2320-7243], Guzmán, V. V. [0000-0003-4784-3040], Goicoechea, Javier R. [0000-0001-7046-4319], #NODATA#, Le Petit, F. [0000-0001-8738-6724], Gerin, M. [0000-0002-2418-7952], Bron, E. [0000-0003-1532-7818], Roueff, E. [0000-0002-4949-8562], Schirmer, T. [0000-0002-8086-4890], Carpenter, J. [0000-0003-2251-0602], Gratier, P. [0000-0002-6636-4304], Hernández-Vera, C., Guzmán, V. V., Goicoechea, Javier R., Maillard, V., Pety, J., Le Petit, F., Gerin, M., Bron, E., Roueff, E., Abergel, A., Schirmer, T., Carpenter, J., Gratier, P., Gordon, K., and Misselt, K.

Abstract

(Abridged) Massive stars can determine the evolution of molecular clouds with their strong ultraviolet (UV) radiation fields. Moreover, UV radiation is relevant in setting the thermal gas pressure in star-forming clouds, whose influence can extend from the rims of molecular clouds to entire star-forming galaxies. Probing the fundamental structure of nearby molecular clouds is therefore crucial to understand how massive stars shape their surrounding medium and how fast molecular clouds are destroyed, specifically at their UV-illuminated edges, where models predict an intermediate zone of neutral atomic gas between the molecular cloud and the surrounding ionized gas whose size is directly related to the exposed physical conditions. We present the highest angular resolution (~$0.5$", corresponding to $207$ au) and velocity-resolved images of the molecular gas emission in the Horsehead nebula, using CO J=3-2 and HCO$^+$ J=4-3 observations with ALMA. We find that CO and HCO$^+$ are present at the edge of the cloud, very close to the ionization (H$^+$/H) and dissociation fronts (H/H$_2$), suggesting a very thin layer of neutral atomic gas (<$650$ au) and a small amount of CO-dark gas ($A_V=0.006-0.26$ mag) for stellar UV illumination conditions typical of molecular clouds in the Milky Way. The new ALMA observations reveal a web of molecular gas filaments with an estimated thermal gas pressure of $P_{\mathrm{th}} = (2.3 - 4.0) \times 10^6$ K cm$^{-3}$, and the presence of a steep density gradient at the cloud edge that can be well explained by stationary isobaric PDR models with pressures consistent with our estimations. However, in the HII region and PDR interface, we find $P_{\mathrm{th,PDR}} > P_{\mathrm{th,HII}}$, suggesting the gas is slightly compressed. Therefore, dynamical effects cannot be completely ruled out and even higher angular observations will be needed to unveil their role.

Published
2023

3. Neural network-based emulation of interstellar medium models

Author

Centre National de la Recherche Scientifique (France), Agence Nationale de la Recherche (France), Ministerio de Ciencia e Innovación (España), NASA Jet Propulsion Laboratory, Universities Space Research Association (US), Palud, Pierre [0000-0002-5850-6325], Einig, Lucas [0000-0003-4250-7638], Le Petit, Franck [0000-0001-8738-6724], Bron, Emeric [0000-0003-1532-7818], #NODATA#, Chanussot, Jocelyn [0000-0003-4817-2875], Pety, Jérôme [0000-0003-3061-6546], Thouvenin, Pierre-Antoine [0000-0003-1246-9458], Bešlić, Ivana [0000-0003-0583-7363], Santa-María, Miriam G. [0000-0002-3941-0360], Orkisz, Jan H. [0000-0002-3382-9208], Ségal, Léontine E. [0009-0002-3993-5754], Zakardjian, Antoine [0000-0002-4240-6012], Gerin, Maryvonne [0000-0002-2418-7952], Goicoechea, Javier R. [0000-0001-7046-4319], Gratier, Pierre [0000-0002-6636-4304], Levrier, François [0000-0002-3065-9944], Liszt, Harvey S. [0000-0002-6116-1911], Le Bourlot, Jacques [0000-0003-3920-8063], Roueff, Antoine [0000-0002-7498-4407], Sievers, Albrecht [0000-0003-0151-2924], Palud, Pierre, Einig, Lucas, Le Petit, Franck, Bron, Emeric, Chainais, Pierre, Chanussot, Jocelyn, Pety, Jérôme, Thouvenin, Pierre-Antoine, Languignon, David, Bešlić, Ivana, Santa-María, Miriam G., Orkisz, Jan H., Ségal, Léontine E., Zakardjian, Antoine, Bardeau, Sébastien, Gerin, Maryvonne, Goicoechea, Javier R., Gratier, Pierre, Guzman, Viviana V., Hughes, Annie, Levrier, François, Liszt, Harvey S., Le Bourlot, Jacques, Roueff, Antoine, Sievers, Albrecht, Centre National de la Recherche Scientifique (France), Agence Nationale de la Recherche (France), Ministerio de Ciencia e Innovación (España), NASA Jet Propulsion Laboratory, Universities Space Research Association (US), Palud, Pierre [0000-0002-5850-6325], Einig, Lucas [0000-0003-4250-7638], Le Petit, Franck [0000-0001-8738-6724], Bron, Emeric [0000-0003-1532-7818], #NODATA#, Chanussot, Jocelyn [0000-0003-4817-2875], Pety, Jérôme [0000-0003-3061-6546], Thouvenin, Pierre-Antoine [0000-0003-1246-9458], Bešlić, Ivana [0000-0003-0583-7363], Santa-María, Miriam G. [0000-0002-3941-0360], Orkisz, Jan H. [0000-0002-3382-9208], Ségal, Léontine E. [0009-0002-3993-5754], Zakardjian, Antoine [0000-0002-4240-6012], Gerin, Maryvonne [0000-0002-2418-7952], Goicoechea, Javier R. [0000-0001-7046-4319], Gratier, Pierre [0000-0002-6636-4304], Levrier, François [0000-0002-3065-9944], Liszt, Harvey S. [0000-0002-6116-1911], Le Bourlot, Jacques [0000-0003-3920-8063], Roueff, Antoine [0000-0002-7498-4407], Sievers, Albrecht [0000-0003-0151-2924], Palud, Pierre, Einig, Lucas, Le Petit, Franck, Bron, Emeric, Chainais, Pierre, Chanussot, Jocelyn, Pety, Jérôme, Thouvenin, Pierre-Antoine, Languignon, David, Bešlić, Ivana, Santa-María, Miriam G., Orkisz, Jan H., Ségal, Léontine E., Zakardjian, Antoine, Bardeau, Sébastien, Gerin, Maryvonne, Goicoechea, Javier R., Gratier, Pierre, Guzman, Viviana V., Hughes, Annie, Levrier, François, Liszt, Harvey S., Le Bourlot, Jacques, Roueff, Antoine, and Sievers, Albrecht

Abstract

The interpretation of observations of atomic and molecular tracers in the galactic and extragalactic interstellar medium (ISM) requires comparisons with state-of-the-art astrophysical models to infer some physical conditions. Usually, ISM models are too time-consuming for such inference procedures, as they call for numerous model evaluations. As a result, they are often replaced by an interpolation of a grid of precomputed models. We propose a new general method to derive faster, lighter, and more accurate approximations of the model from a grid of precomputed models. These emulators are defined with artificial neural networks (ANNs) designed and trained to address the specificities inherent in ISM models. Indeed, such models often predict many observables (e.g., line intensities) from just a few input physical parameters and can yield outliers due to numerical instabilities or physical bistabilities. We propose applying five strategies to address these characteristics: 1) an outlier removal procedure; 2) a clustering method that yields homogeneous subsets of lines that are simpler to predict with different ANNs; 3) a dimension reduction technique that enables to adequately size the network architecture; 4) the physical inputs are augmented with a polynomial transform to ease the learning of nonlinearities; and 5) a dense architecture to ease the learning of simple relations. We compare the proposed ANNs with standard classes of interpolation methods to emulate the Meudon PDR code, a representative ISM numerical model. Combinations of the proposed strategies outperform all interpolation methods by a factor of 2 on the average error, reaching 4.5% on the Meudon PDR code. These networks are also 1000 times faster than accurate interpolation methods and require ten to forty times less memory. This work will enable efficient inferences on wide-field multiline observations of the ISM.

Published
2023

4. Formation of the methyl cation by photochemistry in a protoplanetary disk

Author

Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Ministerio de Ciencia e Innovación (España), University of Ontario, Canadian Space Agency, National Research Council of Canada, German Research Foundation, European Commission, San Jose State University Research Foundation, Japan Society for the Promotion of Science, Berné, Olivier [0000-0002-1686-8395], Martin-Drumel, Marie Aline [0000-0002-5460-4294], Schroetter, Ilane [0000-0002-1099-7401], Goicoechea, Javier R. [0000-0001-7046-4319], Jacovella, Ugo [0000-0003-2152-261X], Gans, Bérenger [0000-0001-9658-2436], Dartois, Emmanuel [0000-0003-1197-7143], Coudert, Laurent H. [0000-0003-0498-6957], Bergin, Edwin [0000-0003-4179-6394], #NODATA#, Cami, Jan [0000-0002-2666-9234], Roueff, Evelyne [0000-0002-4949-8562], Black, John H. [0000-0001-7221-7207], Asvany, Oskar [0000-0003-2995-0803], Peeters, Els [0000-0002-2541-1602], Canin, Amelie [0000-0002-7830-6363], Trahin, Boris [0000-0001-5875-5340], Joblin, Christine [0000-0003-1561-6118], Schlemmer, Stephan [0000-0002-1421-7281], Cernicharo, José [0000-0002-3518-2524], Bernard-Salas, Jeronimo [0000-0002-8452-8675], Boersma, Christiaan [0000-0002-4836-217X], Cuadrado, Sara [0000-0002-7393-1813], Dicken, Daniel [0000-0003-0589-5969], Elyajouri, Meriem [0000-0002-6086-2337], Fuente, Asunción [0000-0001-6317-6343], Le Gal, Romane [0000-0003-1837-3772], Okada, Yoko [0000-0002-6838-6435], Onaka, Takashi [0000-0002-8234-6747], Pound, Marc W. [0000-0002-7269-342X], Röllig, Markus [0000-0001-6205-2242], Schefter, Bethany [0000-0001-5080-8030], Tabone, Benoit [0000-0002-1103-3225], Van De Putte, Dries [0000-0002-5895-8268], Vicente, Sílvia [0000-0001-8973-0752], Berné, Olivier, Martin-Drumel, Marie Aline, Schroetter, Ilane, Goicoechea, Javier R., Jacovella, Ugo, Gans, Bérenger, Dartois, Emmanuel, Coudert, Laurent H., Bergin, Edwin, Alarcon, Felipe, Cami, Jan, Roueff, Evelyne, Black, John H., Asvany, Oskar, Habart, Emilie, Peeters, Els, Canin, Amelie, Trahin, Boris, Joblin, Christine, Schlemmer, Stephan, Thorwirth, Sven, Cernicharo, José, Gerin, Maryvonne, Tielens, Alexander, Zannese, Marion, Abergel, Alain, Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Chown, Ryan, Cuadrado, Sara, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Gordon, Karl D., Issa, Lina, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Le Gal, Romane, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Sidhu, Ameek, Tabone, Benoit, Van De Putte, Dries, Vicente, Sílvia, Wolfire, Mark G., Centre National D'Etudes Spatiales (France), Centre National de la Recherche Scientifique (France), Ministerio de Ciencia e Innovación (España), University of Ontario, Canadian Space Agency, National Research Council of Canada, German Research Foundation, European Commission, San Jose State University Research Foundation, Japan Society for the Promotion of Science, Berné, Olivier [0000-0002-1686-8395], Martin-Drumel, Marie Aline [0000-0002-5460-4294], Schroetter, Ilane [0000-0002-1099-7401], Goicoechea, Javier R. [0000-0001-7046-4319], Jacovella, Ugo [0000-0003-2152-261X], Gans, Bérenger [0000-0001-9658-2436], Dartois, Emmanuel [0000-0003-1197-7143], Coudert, Laurent H. [0000-0003-0498-6957], Bergin, Edwin [0000-0003-4179-6394], #NODATA#, Cami, Jan [0000-0002-2666-9234], Roueff, Evelyne [0000-0002-4949-8562], Black, John H. [0000-0001-7221-7207], Asvany, Oskar [0000-0003-2995-0803], Peeters, Els [0000-0002-2541-1602], Canin, Amelie [0000-0002-7830-6363], Trahin, Boris [0000-0001-5875-5340], Joblin, Christine [0000-0003-1561-6118], Schlemmer, Stephan [0000-0002-1421-7281], Cernicharo, José [0000-0002-3518-2524], Bernard-Salas, Jeronimo [0000-0002-8452-8675], Boersma, Christiaan [0000-0002-4836-217X], Cuadrado, Sara [0000-0002-7393-1813], Dicken, Daniel [0000-0003-0589-5969], Elyajouri, Meriem [0000-0002-6086-2337], Fuente, Asunción [0000-0001-6317-6343], Le Gal, Romane [0000-0003-1837-3772], Okada, Yoko [0000-0002-6838-6435], Onaka, Takashi [0000-0002-8234-6747], Pound, Marc W. [0000-0002-7269-342X], Röllig, Markus [0000-0001-6205-2242], Schefter, Bethany [0000-0001-5080-8030], Tabone, Benoit [0000-0002-1103-3225], Van De Putte, Dries [0000-0002-5895-8268], Vicente, Sílvia [0000-0001-8973-0752], Berné, Olivier, Martin-Drumel, Marie Aline, Schroetter, Ilane, Goicoechea, Javier R., Jacovella, Ugo, Gans, Bérenger, Dartois, Emmanuel, Coudert, Laurent H., Bergin, Edwin, Alarcon, Felipe, Cami, Jan, Roueff, Evelyne, Black, John H., Asvany, Oskar, Habart, Emilie, Peeters, Els, Canin, Amelie, Trahin, Boris, Joblin, Christine, Schlemmer, Stephan, Thorwirth, Sven, Cernicharo, José, Gerin, Maryvonne, Tielens, Alexander, Zannese, Marion, Abergel, Alain, Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Chown, Ryan, Cuadrado, Sara, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Gordon, Karl D., Issa, Lina, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Le Gal, Romane, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Sidhu, Ameek, Tabone, Benoit, Van De Putte, Dries, Vicente, Sílvia, and Wolfire, Mark G.

Abstract

Forty years ago, it was proposed that gas-phase organic chemistry in the interstellar medium can be initiated by the methyl cation CH3+ (refs. 1–3), but so far it has not been observed outside the Solar System 4,5. Alternative routes involving processes on grain surfaces have been invoked 6,7. Here we report James Webb Space Telescope observations of CH3+ in a protoplanetary disk in the Orion star-forming region. We find that gas-phase organic chemistry is activated by ultraviolet irradiation.

Published
2023

5. HCN emission from translucent gas and UV-illuminated cloud edges revealed by wide-field IRAM 30m maps of Orion B GMC: Revisiting its role as tracer of the dense gas reservoir for star formation

Author

Ministerio de Ciencia e Innovación (España), Agence Nationale de la Recherche (France), Centre National de la Recherche Scientifique (France), NASA Jet Propulsion Laboratory, Santa-Maria, Miriam G. [0000-0002-3941-0360], Goicoechea, Javier R. [0000-0001-7046-4319], Pety,J. [0000-0003-3061-6546], Gerin, M. [0000-0002-2418-7952], Orkisz, J. H. [0000-0002-3382-9208], Le Petit, F. [0000-0001-8738-6724], Einig, L. [0000-0003-4250-7638], Palud, P. [0000-0002-5850-6325], Bešlić, I. [0000-0003-0583-7363], Segal, L. [0009-0002-3993-5754], #NODATA#, Bron, E. [0000-0003-1532-7818], Chainais, P. [0000-0003-4377-7584], Chanussot, J. [0000-0003-4817-2875], Gratier, P. [000-0002-6636-4304], Guzmán, V. V. [0000-0003-4784-3040], Levrier, F. [0000-0002-3065-9944], Lis, D. C. [0000-0002-0500-4700], Liszt, H. S. [0000-0002-6116-1911], Le Bourlot, J. [0000-0003-3920-8063], Oya, Y. [0000-0002-0197-8751], Peretto, N. [0000-0002-6893-602X], Roueff, E. [0000-0002-4949-8562], Roueff, A. [0000-0002-7498-4407], Yamamoto, S. [0000-0002-9865-0970], Santa-Maria, Miriam G., Goicoechea, Javier R., Pety,J., Gerin, M., Orkisz, J. H., Le Petit, F., Einig, L., Palud, P., Souza Magalhaes, V. de, Bešlić, I., Segal, L., Bardeau, S., Bron, E., Chainais, P., Chanussot, J., Gratier, P., Guzmán, V. V., Hughes, A., Languignon, D., Levrier, F., Lis, D. C., Liszt, H. S., Le Bourlot, J., Oya, Y., Öberg, K., Peretto, N., Roueff, E., Roueff, A., Sievers, A., Thouvenin, P. -A., Yamamoto, S., Ministerio de Ciencia e Innovación (España), Agence Nationale de la Recherche (France), Centre National de la Recherche Scientifique (France), NASA Jet Propulsion Laboratory, Santa-Maria, Miriam G. [0000-0002-3941-0360], Goicoechea, Javier R. [0000-0001-7046-4319], Pety,J. [0000-0003-3061-6546], Gerin, M. [0000-0002-2418-7952], Orkisz, J. H. [0000-0002-3382-9208], Le Petit, F. [0000-0001-8738-6724], Einig, L. [0000-0003-4250-7638], Palud, P. [0000-0002-5850-6325], Bešlić, I. [0000-0003-0583-7363], Segal, L. [0009-0002-3993-5754], #NODATA#, Bron, E. [0000-0003-1532-7818], Chainais, P. [0000-0003-4377-7584], Chanussot, J. [0000-0003-4817-2875], Gratier, P. [000-0002-6636-4304], Guzmán, V. V. [0000-0003-4784-3040], Levrier, F. [0000-0002-3065-9944], Lis, D. C. [0000-0002-0500-4700], Liszt, H. S. [0000-0002-6116-1911], Le Bourlot, J. [0000-0003-3920-8063], Oya, Y. [0000-0002-0197-8751], Peretto, N. [0000-0002-6893-602X], Roueff, E. [0000-0002-4949-8562], Roueff, A. [0000-0002-7498-4407], Yamamoto, S. [0000-0002-9865-0970], Santa-Maria, Miriam G., Goicoechea, Javier R., Pety,J., Gerin, M., Orkisz, J. H., Le Petit, F., Einig, L., Palud, P., Souza Magalhaes, V. de, Bešlić, I., Segal, L., Bardeau, S., Bron, E., Chainais, P., Chanussot, J., Gratier, P., Guzmán, V. V., Hughes, A., Languignon, D., Levrier, F., Lis, D. C., Liszt, H. S., Le Bourlot, J., Oya, Y., Öberg, K., Peretto, N., Roueff, E., Roueff, A., Sievers, A., Thouvenin, P. -A., and Yamamoto, S.

Abstract

We present 5 deg^2 (~250 pc^2) HCN, HNC, HCO+, and CO J=1-0 maps of the Orion B GMC, complemented with existing wide-field [CI] 492 GHz maps, as well as new pointed observations of rotationally excited HCN, HNC, H13CN, and HN13C lines. We detect anomalous HCN J=1-0 hyperfine structure line emission almost everywhere in the cloud. About 70% of the total HCN J=1-0 luminosity arises from gas at A_V < 8 mag. The HCN/CO J=1-0 line intensity ratio shows a bimodal behavior with an inflection point at A_V < 3 mag typical of translucent gas and UV-illuminated cloud edges. We find that most of the HCN J=1-0 emission arises from extended gas with n(H2) ~< 10^4 cm^-3, even lower density gas if the ionization fraction is > 10^-5 and electron excitation dominates. This result explains the low-A_V branch of the HCN/CO J=1-0 intensity ratio distribution. Indeed, the highest HCN/CO ratios (~0.1) at A_V < 3 mag correspond to regions of high [CI] 492 GHz/CO J=1-0 intensity ratios (>1) characteristic of low-density PDRs. Enhanced FUV radiation favors the formation and excitation of HCN on large scales, not only in dense star-forming clumps. The low surface brightness HCN and HCO+ J=1-0 emission scale with I_FIR (a proxy of the stellar FUV radiation field) in a similar way. Together with CO J=1-0, these lines respond to increasing I_FIR up to G0~20. On the other hand, the bright HCN J=1-0 emission from dense gas in star-forming clumps weakly responds to I_FIR once the FUV radiation field becomes too intense (G0>1500). The different power law scalings (produced by different chemistries, densities, and line excitation regimes) in a single but spatially resolved GMC resemble the variety of Kennicutt-Schmidt law indexes found in galaxy averages. As a corollary for extragalactic studies, we conclude that high HCN/CO J=1-0 line intensity ratios do not always imply the presence of dense gas.

Published
2023

6. Deep learning denoising by dimension reduction: Application to the ORION-B line cubes

Author

Centre National de la Recherche Scientifique (France), Agence Nationale de la Recherche (France), Centre National D'Etudes Spatiales (France), Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), Universities Space Research Association (US), Einig, Lucas [0000-0003-4250-7638], Pety, Jérôme [0000-0003-3061-6546], #NODATA#, Chanussot, Jocelyn [0000-0003-4817-2875], Gerin, Maryvonne [0000-0002-2418-7952], Orkisz, Jan H. [0000-0002-3382-9208], Palud, Pierre [0000-0002-5850-6325], Santa-María, Miriam G. [0000-0002-3941-0360], Bešlić, Ivana [0000-0003-0583-7363], Bron, Emeric E. [0000-0003-1532-7818], Chainais,Pierre [0000-0003-4377-7584], Goicoechea, Javier R. [0000-0001-7046-4319], Gratier, Pierre [0000-0002-6636-4304], Lis, Dariuscz C. [0000-0002-0500-4700], Le Bourlot,Jacques [0000-0003-3920-8063], Le Petit, Franck [0000-0001-8738-6724], Roueff, Evelyne [0000-0002-4949-8562], Sievers, Albrecht [0000-0003-0151-2924], Thouvenin, Pierre-Antoine [0000-0003-1246-9458], Einig, Lucas, Pety, Jérôme, Roueff, Antoine, Vandame, Paul, Chanussot, Jocelyn, Gerin, Maryvonne, Orkisz, Jan H., Palud, Pierre, Santa-María, Miriam G., Souza Magalhaes, Victor de, Bešlić, Ivana, Bardeau, Sébastien, Bron, Emeric E., Chainais,Pierre, Goicoechea, Javier R., Gratier, Pierre, Guzman Veloso, Viviana, Hughes, Annie, Kainulainen, Jouni, Languignon, David, Lallement, Rosine, Levrier, François, Lis, Dariuscz C., Liszt, Harvey, Le Bourlot,Jacques, Le Petit, Franck, Öberg,Karin Danielsson, Peretto, Nicolas, Roueff, Evelyne, Sievers, Albrecht, Thouvenin, Pierre-Antoine, Tremblin, Pascal, Centre National de la Recherche Scientifique (France), Agence Nationale de la Recherche (France), Centre National D'Etudes Spatiales (France), Ministerio de Ciencia e Innovación (España), National Aeronautics and Space Administration (US), Universities Space Research Association (US), Einig, Lucas [0000-0003-4250-7638], Pety, Jérôme [0000-0003-3061-6546], #NODATA#, Chanussot, Jocelyn [0000-0003-4817-2875], Gerin, Maryvonne [0000-0002-2418-7952], Orkisz, Jan H. [0000-0002-3382-9208], Palud, Pierre [0000-0002-5850-6325], Santa-María, Miriam G. [0000-0002-3941-0360], Bešlić, Ivana [0000-0003-0583-7363], Bron, Emeric E. [0000-0003-1532-7818], Chainais,Pierre [0000-0003-4377-7584], Goicoechea, Javier R. [0000-0001-7046-4319], Gratier, Pierre [0000-0002-6636-4304], Lis, Dariuscz C. [0000-0002-0500-4700], Le Bourlot,Jacques [0000-0003-3920-8063], Le Petit, Franck [0000-0001-8738-6724], Roueff, Evelyne [0000-0002-4949-8562], Sievers, Albrecht [0000-0003-0151-2924], Thouvenin, Pierre-Antoine [0000-0003-1246-9458], Einig, Lucas, Pety, Jérôme, Roueff, Antoine, Vandame, Paul, Chanussot, Jocelyn, Gerin, Maryvonne, Orkisz, Jan H., Palud, Pierre, Santa-María, Miriam G., Souza Magalhaes, Victor de, Bešlić, Ivana, Bardeau, Sébastien, Bron, Emeric E., Chainais,Pierre, Goicoechea, Javier R., Gratier, Pierre, Guzman Veloso, Viviana, Hughes, Annie, Kainulainen, Jouni, Languignon, David, Lallement, Rosine, Levrier, François, Lis, Dariuscz C., Liszt, Harvey, Le Bourlot,Jacques, Le Petit, Franck, Öberg,Karin Danielsson, Peretto, Nicolas, Roueff, Evelyne, Sievers, Albrecht, Thouvenin, Pierre-Antoine, and Tremblin, Pascal

Abstract

Context. The availability of large bandwidth receivers for millimeter radio telescopes allows the acquisition of position-position-frequency data cubes over a wide field of view and a broad frequency coverage. These cubes contain much information on the physical, chemical, and kinematical properties of the emitting gas. However, their large size coupled with inhomogenous signal-to-noise ratio (SNR) are major challenges for consistent analysis and interpretation.Aims. We search for a denoising method of the low SNR regions of the studied data cubes that would allow to recover the low SNR emission without distorting the signals with high SNR.Methods. We perform an in-depth data analysis of the 13 CO and C 17 O (1 -- 0) data cubes obtained as part of the ORION-B large program performed at the IRAM 30m telescope. We analyse the statistical properties of the noise and the evolution of the correlation of the signal in a given frequency channel with that of the adjacent channels. This allows us to propose significant improvements of typical autoassociative neural networks, often used to denoise hyperspectral Earth remote sensing data. Applying this method to the 13 CO (1 -- 0) cube, we compare the denoised data with those derived with the multiple Gaussian fitting algorithm ROHSA, considered as the state of the art procedure for data line cubes.Results. The nature of astronomical spectral data cubes is distinct from that of the hyperspectral data usually studied in the Earth remote sensing literature because the observed intensities become statistically independent beyond a short channel separation. This lack of redundancy in data has led us to adapt the method, notably by taking into account the sparsity of the signal along the spectral axis. The application of the proposed algorithm leads to an increase of the SNR in voxels with weak signal, while preserving the spectral shape of the data in high SNR voxels.Conclusions. The proposed algorithm that combines a detailed ana

Published
2023

7. Gas kinematics around filamentary structures in the Orion B cloud

Author

Agence Nationale de la Recherche (France), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), l'Observatoire de Paris, Ministerio de Ciencia, Innovación y Universidades (España), Swedish Research Council, Orkisz, Jan H. [0000-0002-3382-9208], Pety, Jérôme [0000-0003-3061-6546], Roueff, Antoine [0000-0002-7498-4407], Marchal, Antoine [0000-0002-5501-232X], Levrier, François [0000-0002-3065-9944], Miville-Deschênes, Marc-Antoine [0000-0002-7351-6062], Goicoechea, Javier R. [0000-0001-7046-4319], Roueff, Evelyne [0000-0002-4949-8562], Santa-Maria, Miriam G. [0000-0002-3941-0360], Bron, Emeric [0000-0003-1532-7818], Chainais, Pierre [0000-0003-4377-7584], Chanussot, Jocelyn [0000-0003-4817-2875], Gratier, Pierre [0000-0002-6636-4304], Guzman, Viviana [0000-0003-4784-3040], Le Bourlot,Jacques [0000-0003-3920-8063], Liszt, Harvey [0000-0002-6116-1911], Gaudel, Mathilde, Orkisz, Jan H., Gerin, Maryvonne, Pety, Jérôme, Roueff, Antoine, Marchal, Antoine, Levrier, François, Miville-Deschênes, Marc-Antoine, Goicoechea, Javier R., Roueff, Evelyne, Le Petit, Franck, Souza Magalhaes, Victor de, Palud, Pierre, Santa-Maria, Miriam G., Vono, Maxime, Bardeau, Sébastien, Bron, Emeric, Chainais, Pierre, Chanussot, Jocelyn, Gratier, Pierre, Guzman, Viviana, Hughes, Annie, Kainulainen, Jouni, Languignon, David, Le Bourlot,Jacques, Liszt, Harvey, Öberg, Karin, Peretto, Nicolas, Sievers, Albrecht, Tremblin, Pascal, Agence Nationale de la Recherche (France), Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), l'Observatoire de Paris, Ministerio de Ciencia, Innovación y Universidades (España), Swedish Research Council, Orkisz, Jan H. [0000-0002-3382-9208], Pety, Jérôme [0000-0003-3061-6546], Roueff, Antoine [0000-0002-7498-4407], Marchal, Antoine [0000-0002-5501-232X], Levrier, François [0000-0002-3065-9944], Miville-Deschênes, Marc-Antoine [0000-0002-7351-6062], Goicoechea, Javier R. [0000-0001-7046-4319], Roueff, Evelyne [0000-0002-4949-8562], Santa-Maria, Miriam G. [0000-0002-3941-0360], Bron, Emeric [0000-0003-1532-7818], Chainais, Pierre [0000-0003-4377-7584], Chanussot, Jocelyn [0000-0003-4817-2875], Gratier, Pierre [0000-0002-6636-4304], Guzman, Viviana [0000-0003-4784-3040], Le Bourlot,Jacques [0000-0003-3920-8063], Liszt, Harvey [0000-0002-6116-1911], Gaudel, Mathilde, Orkisz, Jan H., Gerin, Maryvonne, Pety, Jérôme, Roueff, Antoine, Marchal, Antoine, Levrier, François, Miville-Deschênes, Marc-Antoine, Goicoechea, Javier R., Roueff, Evelyne, Le Petit, Franck, Souza Magalhaes, Victor de, Palud, Pierre, Santa-Maria, Miriam G., Vono, Maxime, Bardeau, Sébastien, Bron, Emeric, Chainais, Pierre, Chanussot, Jocelyn, Gratier, Pierre, Guzman, Viviana, Hughes, Annie, Kainulainen, Jouni, Languignon, David, Le Bourlot,Jacques, Liszt, Harvey, Öberg, Karin, Peretto, Nicolas, Sievers, Albrecht, and Tremblin, Pascal

Abstract

Understanding the initial properties of star-forming material and how they affect the star formation process is key. From an observational point of view, the feedback from young high-mass stars on future star formation properties is still poorly constrained. In the framework of the IRAM 30m ORION-B large program, we obtained observations of the translucent and moderately dense gas, which we used to analyze the kinematics over a field of 5 deg^2 around the filamentary structures. We used the ROHSA algorithm to decompose and de-noise the C18O(1-0) and 13CO(1-0) signals by taking the spatial coherence of the emission into account. We produced gas column density and mean velocity maps to estimate the relative orientation of their spatial gradients. We identified three cloud velocity layers at different systemic velocities and extracted the filaments in each velocity layer. The filaments are preferentially located in regions of low centroid velocity gradients. By comparing the relative orientation between the column density and velocity gradients of each layer from the ORION-B observations and synthetic observations from 3D kinematic toy models, we distinguish two types of behavior in the dynamics around filaments: (i) radial flows perpendicular to the filament axis that can be either inflows (increasing the filament mass) or outflows and (ii) longitudinal flows along the filament axis. The former case is seen in the Orion B data, while the latter is not identified. We have also identified asymmetrical flow patterns, usually associated with filaments located at the edge of an HII region. This is the first observational study to highlight feedback from HII regions on filament formation and, thus, on star formation in the Orion B cloud. This simple statistical method can be used for any molecular cloud to obtain coherent information on the kinematics.

Published
2022

8. PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Author

National Aeronautics and Space Administration (US), University of Maryland, University of Michigan, University of Toledo, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Natural Sciences and Engineering Research Council of Canada, Ministerio de Ciencia e Innovación (España), German Research Foundation, Japan Society for the Promotion of Science, San Jose State University Research Foundation, Berné, Olivier [0000-0002-1686-8395], Habart, Émilie [0000-0001-9136-8043], Peeters, Els [0000-0002-2541-1602], Abergel, Alain [0000-0003-2364-2260], Bergin, Edwin A. [0000-0003-4179-6394], Bernard-Salas, Jeronimo [0000-0002-8452-8675], Bron, Emeric [0000-0003-1532-7818], Cami, Jan [0000-0002-2666-9234], Dartois, Emmanuel [0000-0003-1197-7143], Fuente, Asunción [0000-0001-6317-6343], Goicoechea, Javier R. [0000-0001-7046-4319], Gordon, Karl D. [0000-0001-5340-6774], Okada, Yoko [0000-0002-6838-6435], Onaka, Takashi [0000-0002-8234-6747], Robberto, Massimo [0000-0002-9573-3199], Röllig, Markus [0000-0001-6205-2242], Tielens, Alexander G.G.M. [0000-0003-0306-0028], Vicente, Sílvia [0000-0001-8973-0752], Wolfire, Mark G. [0000-0003-0030-9510], Alarcón, Felipe [0000-0002-2692-7862], Boersma, C. [0000-0002-4836-217X], Canin, Amélie [0000-0002-7830-6363], Chown, Ryan [0000-0001-8241-7704], Dicken, Daniel [0000-0003-0589-5969], Le Gal, Romane [0000-0003-1837-3772], Pound, Marc W. [0000-0002-7269-342X], Trahin, Boris [0000-0001-5875-5340], Sidhu, Ameek [0000-0003-3771-4990], Van De Putte, Dries [0000-0002-5895-8268], Cuadrado, Sara [0000-0002-7393-1813], Guilloteau, Claire [0000-0001-5800-9647], Maragkoudakis, Alexandros [0000-0003-2552-3871], Schefter, Bethany R. [0000-0001-5080-8030], Schirmer, Thiébaut [0000-0002-8086-4890], Aleman, Isabel [0000-0002-7989-9041], Allamandola, Louis [0000-0002-6049-4079], Auchettl, Rebecca [0000-0001-9296-0751], Antonio Baratta, Giuseppe [0000-0002-3688-160X], Bejaoui, Salma [0000-0001-8646-9464], Bera, Partha P. [0000-0003-0843-3209], Bilalbegović, Goranka [0000-0002-1058-6610], Black, John H. [0000-0001-7221-7207], Boulanger, Francois [0000-0003-1097-6042], Bouwman, Jordy [0000-0002-3615-1703], Brandl, Bernhard [0000-0001-9737-169X], Brünken, Sandra [0000-0001-7175-4828], Burkhardt, Andrew [0000-0003-0799-0927], Candian, Alessandra [0000-0002-5431-4449], Cernicharo, José [0000-0002-3518-2524], Chakraborty, Shubhadip [0000-0002-2982-6450], Champion, Jason [0000-0002-9256-8917], Colgan, Sean W.J. [0000-0001-6275-7437], Cooke, Ilsa R. [0000-0002-0850-7426], Coutens, Audrey [0000-0003-1805-3920], Cox, Nick L.J. [0000-0002-7926-4492], Demyk, Karine [0000-0002-5019-8700], Donovan Meyer, Jennifer [0000-0002-3106-7676], Engrand, Cécile [0000-0002-0396-5583], Foschino, Sacha [0000-0003-2455-2355], Gavilan, Lisseth [0000-0001-8645-8415], Gerin, Maryvonne [0000-0002-2418-7952], Godard, Marie [0000-0002-7276-4021], Gottlieb, Carl A. [0000-0003-2845-5317], Guillard, Pierre [0000-0002-2421-1350], Gusdorf, Antoine [0000-0002-0354-1684], Hartigan, Patrick [0000-0002-5380-549X], He, Jinhua [0000-0002-3938-4393], Herbst, Eric [0000-0002-4649-2536], Hornekaer, Liv [0000-0003-0828-3642], Janot-Pacheco, Eduardo [0000-0003-0079-3912], Joblin, Christine [0000-0003-1561-6118], Kaufman, Michael [0000-0002-2521-1985], Kemper, Francisca [0000-0003-2743-8240], Kendrew, Sarah [0000-0002-7612-0469], Kirsanova, Maria S. [0000-0003-4338-9055], Klaassen, Pamela [0000-0001-9443-0463], Knight, Collin [0000-0003-2968-3522], Kwok, Sun [0000-0001-7708-081X], Labiano, Álvaro [0000-0002-0690-8824], Lai, Thomas S.Y. [0000-0001-8490-6632], Lee, Timothy J. [0000-0002-2598-2237], Lefloch, Bertrand [0000-0002-9397-3826], Le Petit, Franck [0000-0001-8738-6724], Li, Aigen [0000-0002-1119-642X], Linz, Hendrik [0000-0002-8115-8437], MacKie, Cameron J. [0000-0003-2885-2021], Madden, Suzanne C. [0000-0003-3229-2899], Mascetti, Joëlle [0000-0002-8585-9118], McGuire, Brett A. [0000-0003-1254-4817], Merino, Pablo [0000-0002-0267-4020], Micelotta, Elisabetta R. [0000-0002-6555-5109], Morse, Jon A. [0000-0001-5895-2256], Berné, Olivier, Habart, Émilie, Peeters, Els, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Bron, Emeric, Cami, Jan, Dartois, Emmanuel, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Okada, Yoko, Onaka, Takashi, Robberto, Massimo, Röllig, Markus, Tielens, Alexander G.G.M., Vicente, Sílvia, Wolfire, Mark G., Alarcón, Felipe, Boersma, C., Canin, Amélie, Chown, Ryan, Dicken, Daniel, Languignon, David, Le Gal, Romane, Pound, Marc W., Trahin, Boris, Simmer, Thomas, Sidhu, Ameek, Van De Putte, Dries, Cuadrado, Sara, Guilloteau, Claire, Maragkoudakis, Alexandros, Schefter, Bethany R., Schirmer, Thiébaut, Cazaux, Stéphanie, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Antonio Baratta, Giuseppe, Bejaoui, Salma, Bera, Partha P., Bilalbegović, Goranka, Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Burkhardt, Andrew, Candian, Alessandra, Cernicharo, José, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W.J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L.J., Demyk, Karine, Donovan Meyer, Jennifer, Engrand, Cécile, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Joblin, Christine, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S.Y., Lee, Timothy J., Lefloch, Bertrand, Le Petit, Franck, Li, Aigen, Linz, Hendrik, MacKie, Cameron J., Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Misselt, Karl, Morse, Jon A., National Aeronautics and Space Administration (US), University of Maryland, University of Michigan, University of Toledo, Centre National de la Recherche Scientifique (France), Centre National D'Etudes Spatiales (France), Natural Sciences and Engineering Research Council of Canada, Ministerio de Ciencia e Innovación (España), German Research Foundation, Japan Society for the Promotion of Science, San Jose State University Research Foundation, Berné, Olivier [0000-0002-1686-8395], Habart, Émilie [0000-0001-9136-8043], Peeters, Els [0000-0002-2541-1602], Abergel, Alain [0000-0003-2364-2260], Bergin, Edwin A. [0000-0003-4179-6394], Bernard-Salas, Jeronimo [0000-0002-8452-8675], Bron, Emeric [0000-0003-1532-7818], Cami, Jan [0000-0002-2666-9234], Dartois, Emmanuel [0000-0003-1197-7143], Fuente, Asunción [0000-0001-6317-6343], Goicoechea, Javier R. [0000-0001-7046-4319], Gordon, Karl D. [0000-0001-5340-6774], Okada, Yoko [0000-0002-6838-6435], Onaka, Takashi [0000-0002-8234-6747], Robberto, Massimo [0000-0002-9573-3199], Röllig, Markus [0000-0001-6205-2242], Tielens, Alexander G.G.M. [0000-0003-0306-0028], Vicente, Sílvia [0000-0001-8973-0752], Wolfire, Mark G. [0000-0003-0030-9510], Alarcón, Felipe [0000-0002-2692-7862], Boersma, C. [0000-0002-4836-217X], Canin, Amélie [0000-0002-7830-6363], Chown, Ryan [0000-0001-8241-7704], Dicken, Daniel [0000-0003-0589-5969], Le Gal, Romane [0000-0003-1837-3772], Pound, Marc W. [0000-0002-7269-342X], Trahin, Boris [0000-0001-5875-5340], Sidhu, Ameek [0000-0003-3771-4990], Van De Putte, Dries [0000-0002-5895-8268], Cuadrado, Sara [0000-0002-7393-1813], Guilloteau, Claire [0000-0001-5800-9647], Maragkoudakis, Alexandros [0000-0003-2552-3871], Schefter, Bethany R. [0000-0001-5080-8030], Schirmer, Thiébaut [0000-0002-8086-4890], Aleman, Isabel [0000-0002-7989-9041], Allamandola, Louis [0000-0002-6049-4079], Auchettl, Rebecca [0000-0001-9296-0751], Antonio Baratta, Giuseppe [0000-0002-3688-160X], Bejaoui, Salma [0000-0001-8646-9464], Bera, Partha P. [0000-0003-0843-3209], Bilalbegović, Goranka [0000-0002-1058-6610], Black, John H. [0000-0001-7221-7207], Boulanger, Francois [0000-0003-1097-6042], Bouwman, Jordy [0000-0002-3615-1703], Brandl, Bernhard [0000-0001-9737-169X], Brünken, Sandra [0000-0001-7175-4828], Burkhardt, Andrew [0000-0003-0799-0927], Candian, Alessandra [0000-0002-5431-4449], Cernicharo, José [0000-0002-3518-2524], Chakraborty, Shubhadip [0000-0002-2982-6450], Champion, Jason [0000-0002-9256-8917], Colgan, Sean W.J. [0000-0001-6275-7437], Cooke, Ilsa R. [0000-0002-0850-7426], Coutens, Audrey [0000-0003-1805-3920], Cox, Nick L.J. [0000-0002-7926-4492], Demyk, Karine [0000-0002-5019-8700], Donovan Meyer, Jennifer [0000-0002-3106-7676], Engrand, Cécile [0000-0002-0396-5583], Foschino, Sacha [0000-0003-2455-2355], Gavilan, Lisseth [0000-0001-8645-8415], Gerin, Maryvonne [0000-0002-2418-7952], Godard, Marie [0000-0002-7276-4021], Gottlieb, Carl A. [0000-0003-2845-5317], Guillard, Pierre [0000-0002-2421-1350], Gusdorf, Antoine [0000-0002-0354-1684], Hartigan, Patrick [0000-0002-5380-549X], He, Jinhua [0000-0002-3938-4393], Herbst, Eric [0000-0002-4649-2536], Hornekaer, Liv [0000-0003-0828-3642], Janot-Pacheco, Eduardo [0000-0003-0079-3912], Joblin, Christine [0000-0003-1561-6118], Kaufman, Michael [0000-0002-2521-1985], Kemper, Francisca [0000-0003-2743-8240], Kendrew, Sarah [0000-0002-7612-0469], Kirsanova, Maria S. [0000-0003-4338-9055], Klaassen, Pamela [0000-0001-9443-0463], Knight, Collin [0000-0003-2968-3522], Kwok, Sun [0000-0001-7708-081X], Labiano, Álvaro [0000-0002-0690-8824], Lai, Thomas S.Y. [0000-0001-8490-6632], Lee, Timothy J. [0000-0002-2598-2237], Lefloch, Bertrand [0000-0002-9397-3826], Le Petit, Franck [0000-0001-8738-6724], Li, Aigen [0000-0002-1119-642X], Linz, Hendrik [0000-0002-8115-8437], MacKie, Cameron J. [0000-0003-2885-2021], Madden, Suzanne C. [0000-0003-3229-2899], Mascetti, Joëlle [0000-0002-8585-9118], McGuire, Brett A. [0000-0003-1254-4817], Merino, Pablo [0000-0002-0267-4020], Micelotta, Elisabetta R. [0000-0002-6555-5109], Morse, Jon A. [0000-0001-5895-2256], Berné, Olivier, Habart, Émilie, Peeters, Els, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Bron, Emeric, Cami, Jan, Dartois, Emmanuel, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Okada, Yoko, Onaka, Takashi, Robberto, Massimo, Röllig, Markus, Tielens, Alexander G.G.M., Vicente, Sílvia, Wolfire, Mark G., Alarcón, Felipe, Boersma, C., Canin, Amélie, Chown, Ryan, Dicken, Daniel, Languignon, David, Le Gal, Romane, Pound, Marc W., Trahin, Boris, Simmer, Thomas, Sidhu, Ameek, Van De Putte, Dries, Cuadrado, Sara, Guilloteau, Claire, Maragkoudakis, Alexandros, Schefter, Bethany R., Schirmer, Thiébaut, Cazaux, Stéphanie, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Antonio Baratta, Giuseppe, Bejaoui, Salma, Bera, Partha P., Bilalbegović, Goranka, Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Burkhardt, Andrew, Candian, Alessandra, Cernicharo, José, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W.J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L.J., Demyk, Karine, Donovan Meyer, Jennifer, Engrand, Cécile, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Joblin, Christine, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S.Y., Lee, Timothy J., Lefloch, Bertrand, Le Petit, Franck, Li, Aigen, Linz, Hendrik, MacKie, Cameron J., Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Misselt, Karl, and Morse, Jon A.

Abstract

Massive stars disrupt their natal molecular cloud material through radiative and mechanical feedback processes. These processes have profound effects on the evolution of interstellar matter in our Galaxy and throughout the universe, from the era of vigorous star formation at redshifts of 1-3 to the present day. The dominant feedback processes can be probed by observations of the Photo-Dissociation Regions (PDRs) where the far-ultraviolet photons of massive stars create warm regions of gas and dust in the neutral atomic and molecular gas. PDR emission provides a unique tool to study in detail the physical and chemical processes that are relevant for most of the mass in inter-and circumstellar media including diffuse clouds, proto-planetary disks, and molecular cloud surfaces, globules, planetary nebulae, and star-forming regions. PDR emission dominates the infrared (IR) spectra of star-forming galaxies. Most of the Galactic and extragalactic observations obtained with the James Webb Space Telescope (JWST) will therefore arise in PDR emission. In this paper we present an Early Release Science program using the MIRI, NIRSpec, and NIRCam instruments dedicated to the observations of an emblematic and nearby PDR: the Orion Bar. These early JWST observations will provide template data sets designed to identify key PDR characteristics in JWST observations. These data will serve to benchmark PDR models and extend them into the JWST era. We also present the Science-Enabling products that we will provide to the community. These template data sets and Science-Enabling products will guide the preparation of future proposals on star-forming regions in our Galaxy and beyond and will facilitate data analysis and interpretation of forthcoming JWST observations.

Published
2022

9. Formation of interstellar SH+ from vibrationally excited H2: Quantum study of S+ + H2 ⇄ SH+ + H reaction and inelastic collision

Author

Octavio Roncero, Javier R. Goicoechea, François Lique, Alexandre Zanchet, Niyazi Bulut, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Institut Universitaire de France, Turkish Academy of Sciences, Zanchet, Alexandre [0000-0002-0471-5658], Lique, François [0000-0002-0664-2536], Roncero, Octavio [0000-0002-8871-4846], Goicoechea, Javier R. [0000-0001-7046-4319], Bulut, Niyazi [0000-0003-2863-7700], Instituto de Física Fundamental [Madrid] (IFF), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Laboratoire Ondes et Milieux Complexes (LOMC), Centre National de la Recherche Scientifique (CNRS)-Université Le Havre Normandie (ULH), Normandie Université (NU)-Normandie Université (NU), Firat University, Zanchet, Alexandre, Lique, François, Roncero, Octavio, Goicoechea, Javier R., and Bulut, Niyazi

Subjects
Physics, [PHYS]Physics [physics], Photodissociation, Inelastic collision, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Potential energy, Molecular physics, Molecular processes, ISM: molecules, 3. Good health, Photon-dominated region (PDR), Reaction rate constant, Space and Planetary Science, Yield (chemistry), Excited state, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Collisional excitation, ComputingMilieux_MISCELLANEOUS, molecules [ISM], Bar (unit)
Abstract

8 pags., 7 figs., 4 tabs., The rate constants for the formation, destruction, and collisional excitation of SH are calculated from quantum mechanical approaches using two new SH potential energy surfaces (PESs) of A″ and A″ electronic symmetry. The PESs were developed to describe all adiabatic states correlating to the SH(ς) + H(S) channel. The formation of SH through the S + H reaction is endothermic by ≈9860 K, and requires at least two vibrational quanta on the H molecule to yield significant reactivity. Quasi-classical calculations of the total formation rate constant for H(v? =? 2) are in very good agreement with the quantum results above 100 K. Further quasi-classical calculations are then performed for v? =? 3, 4, and 5 to cover all vibrationally excited H levels significantly populated in dense photodissociation regions (PDR). The new calculated formation and destruction rate constants are two to six times larger than the previous ones and have been introduced in the Meudon PDR code to simulate the physical and illuminating conditions in the Orion bar prototypical PDR. New astrochemical models based on the new molecular data produce four times larger SH column densities, in agreement with those inferred from recent ALMA observations of the Orion bar., The research leading to these results has received funding from MICIU under grants No. FIS2017-83473-C2 and AYA2017- 85111-P. FL acknowledges financial support from the Institut Universitaire de France. NB acknowledges the computing facilities by TUBITAK-TRUBA.

Published
2019

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