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1. A sensitivity analysis of the modeling of Polycyclic Aromatic Hydrocarbon emission in galaxies

Author

Maragkoudakis, Alexandros, Boersma, Christiaan, Temi, Pasquale, Bregman, Jesse D., Allamandola, Louis J., Esposito, Vincent, Ricca, Alessandra, and Peeters, Els

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We have conducted a sensitivity analysis on the mid-infrared spectral decomposition of galaxies and the modeling of the PAH emission spectrum with the NASA Ames PAH Infrared Spectroscopic Database (PAHdb) to assess the variance on the average galaxy PAH population properties under a grid of different modeling parameters. We find that the SL and SL+LL Spitzer-IRS decomposition with PAHFIT provides consistent modeling and recovery of the 5-15 $\mu$m PAH emission spectrum. For PAHdb modeling, application of a redshift to the calculated spectra to account for anharmonic effects introduces a $15\%$-$20\%$ variance on the derived parameters, while its absence improves the fits by $\sim13\%$. The 4.00-$\alpha$ release of PAHdb achieves the complete modeling of the 6-15 $\mu$m PAH spectrum, including the full 6.2 $\mu$m band, improving the average fitting uncertainty by a factor of 2. The optimal PAHdb modeling configuration requires selection of pure PAHs without applying a redshift to the bands. Although quantitatively the PAHdb-derived parameters change under different modeling configurations or database versions, their variation follows a linear scaling, with previously reported trends remaining qualitatively valid. PAHdb modeling of JWST observations, and JWST observations smoothed and resampled to the Spitzer-IRS resolution and dispersion have consistent PAHdb derived parameters. Decomposition with different codes, such as PAHFIT and CAFE, produce PAH emission spectra with noticeable variation in the 11-15~$\mu$m region, driving a $\sim7\%$ difference in the neutral PAH fraction under PAHdb modeling. A new library of galaxy PAH emission templates is delivered to be utilized in galaxy SED modeling., Comment: 25 pages, 17 figures, 6 tables. Accepted for publication in ApJ

Published
2024

2. The Background Interstellar Medium as Observed from Off-Order Low-Resolution Spitzer-IRS Spectra

Author

Boersma, Christiaan, Bregman, Jesse D., Allamandola, Louis J., Temi, Pasquale, and Maragkoudakis, Alexandros

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Spitzer 'hidden' observations of the background are used to construct a catalog of 4,090 spectra and examine the signature of polycyclic aromatic hydrocarbon (PAH) molecules and their connection to extinction by dust. A strong positive correlation is recovered between WISE12, E(B-V), and the 11.2 $\mu$m PAH band. For 0.06 $\leq$ E(B-V) $\leq$ 5.0, correlations of the 6.2, 11.2, and 12.7 $\mu$m PAH band are positive with E(B-V). Three dust temperature regimes are revealed. Correlations with WISE12 are well-constrained and that with 12.7/11.2 is flat. Decomposition with the NASA Ames PAH IR Spectroscopic Database reveals a tentative positive correlation between the 6.2/11.2 and the PAH ionization fraction, while that with 12.7/11.2 is slightly negative, suggesting PAH structural changes. The relation with PAH size and 6.2/11.2 is negative, while that with 12.7/11.2 is positive. Averaging spectra into five E(B-V) and three T$_{\rm dust}$ bins shows an evolution in PAH emission and variations in 12.7/11.2. Database-fits show an increase in $f_{\rm i}$ and the PAH ionization parameter $\gamma$, but a more stable large PAH fraction. While the largest $\gamma$s are associated with the highest T$_{\rm dust}$, there is no one-to-one correlation. The analysis is hampered by low-quality data at short wavelengths. There are indications that PAHs in the more-diffuse backgrounds behave differently from those in the general interstellar medium. However, they are often still associated with larger scale filamentary cloud-like structures. The spectra and auxiliary data have been made available through the Ames Background Interstellar Medium Spectral Catalog and may guide JWST programs.

Published
2024
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3. PDRs4All VIII: Mid-IR emission line inventory of the Orion Bar

Author

Van De Putte, Dries, Meshaka, Raphael, Trahin, Boris, Habart, Emilie, Peeters, Els, Berné, Olivier, Alarcón, Felipe, Canin, Amélie, Chown, Ryan, Schroetter, Ilane, Sidhu, Ameek, Boersma, Christiaan, Bron, Emeric, Dartois, Emmanuel, Goicoechea, Javier R., Gordon, Karl D., Onaka, Takashi, Tielens, Alexander G. G. M., Verstraete, Laurent, Wolfire, Mark G., Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Cami, Jan, Cuadrado, Sara, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Joblin, Christine, Khan, Baria, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Maragkoudakis, Alexandros, Okada, Yoko, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Tabone, Benoit, Vicente, Sílvia, Zannese, Marion, Colgan, Sean W. J., He, Jinhua, Rouillé, Gaël, Togi, Aditya, Aleman, Isabel, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Bejaoui, Salma, Bera, Partha P., Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Cazaux, Stéphanie, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, Foschino, Sacha, García-Lario, Pedro, Gerin, Maryvonne, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, Herbst, Eric, Hornekaer, Liv, Issa, Lina, Jäger, Cornelia, Janot-Pacheco, Eduardo, Kannavou, Olga, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S. -Y., Floch, Bertrand Le, Petit, Franck Le, Li, Aigen, Linz, Hendrik, Mackie, Cameron J., Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Morse, Jon A., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Omont, Alain, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Rho, Jeonghee, Ricca, Alessandra, Roman-Duval, Julia, Roser, Joseph, Roueff, Evelyne, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Witt, Adolf N., Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Mid-infrared emission features probe the properties of ionized gas, and hot or warm molecular gas. The Orion Bar is a frequently studied photodissociation region (PDR) containing large amounts of gas under these conditions, and was observed with the MIRI IFU aboard JWST as part of the "PDRs4All" program. The resulting IR spectroscopic images of high angular resolution (0.2") reveal a rich observational inventory of mid-IR emission lines, and spatially resolve the substructure of the PDR, with a mosaic cutting perpendicularly across the ionization front and three dissociation fronts. We extracted five spectra that represent the ionized, atomic, and molecular gas layers, and measured the most prominent gas emission lines. An initial analysis summarizes the physical conditions of the gas and the potential of these data. We identified around 100 lines, report an additional 18 lines that remain unidentified, and measured the line intensities and central wavelengths. The H I recombination lines originating from the ionized gas layer bordering the PDR, have intensity ratios that are well matched by emissivity coefficients from H recombination theory, but deviate up to 10% due contamination by He I lines. We report the observed emission lines of various ionization stages of Ne, P, S, Cl, Ar, Fe, and Ni, and show how certain line ratios vary between the five regions. We observe the pure-rotational H$_2$ lines in the vibrational ground state from 0-0 S(1) to 0-0 S(8), and in the first vibrationally excited state from 1-1 S(5) to 1-1 S(9). We derive H$_2$ excitation diagrams, and approximate the excitation with one thermal (~700 K) component representative of an average gas temperature, and one non-thermal component (~2700 K) probing the effect of UV pumping. We compare these results to an existing model for the Orion Bar PDR and highlight the differences with the observations., Comment: 26 pages, 12 figures, 3 tables. Submitted to A&A, under review (1st revision)

Published
2024
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4. A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk

Author

Berné, Olivier, Habart, Emilie, Peeters, Els, Schroetter, Ilane, Canin, Amélie, Sidhu, Ameek, Chown, Ryan, Bron, Emeric, Haworth, Thomas J., Klaassen, Pamela, Trahin, Boris, Van De Putte, Dries, Alarcón, Felipe, Zannese, Marion, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Cami, Jan, Cuadrado, Sara, Dartois, Emmanuel, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Simmer, Thomas, Tabone, Benoit, Tielens, Alexander G. G. M., Vicente, Sílvia, Wolfire, Mark G., Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Baruteau, Clément, Bejaoui, Salma, Bera, Partha P., Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Cazaux, Stéphanie, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, 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, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S. -Y., Lee, Timothy J., Lefloch, Bertrand, Petit, Franck Le, Li, Aigen, Linz, Hendrik, Mackie, Cameron J., Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Morse, Jon A., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roueff, Evelyne, Rouillé, Gaël, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shannon, Matthew J., Simonnin, Adrien, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photo-dissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, impacting planet formation within the disks. We report JWST and Atacama Large Millimetere Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modelling their kinematics and excitation allows us to constrain the physical conditions within the gas. We quantify the mass-loss rate induced by the FUV irradiation, finding it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk.

Published
2024

5. Formation of the Methyl Cation by Photochemistry in a Protoplanetary Disk

Author

Berné, Olivier, Martin-Drumel, Marie-Aline, Schroetter, Ilane, Goicoechea, Javier R., Jacovella, Ugo, Gans, Bérenger, Dartois, Emmanuel, Coudert, Laurent, 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, Jose, 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, Gal, Romane Le, 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.

Subjects
Astrophysics - Astrophysics of Galaxies, Physics - Chemical Physics
Abstract

Forty years ago it was proposed that gas phase organic chemistry in the interstellar medium was initiated by the methyl cation CH3+, but hitherto it has not been observed outside the Solar System. Alternative routes involving processes on grain surfaces have been invoked. Here we report JWST observations of CH3+ in a protoplanetary disk in the Orion star forming region. We find that gas-phase organic chemistry is activated by UV irradiation., Comment: Published in Nature

Published
2024
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6. OH as a probe of the warm water cycle in planet-forming disks

Author

Zannese, Marion, Tabone, Benoît, Habart, Emilie, Goicoechea, Javier R., Zanchet, Alexandre, van Dishoeck, Ewine F., van Hemert, Marc C., Black, John H., Tielens, Alexander G. G. M., Veselinova, A., Jambrina, P. G., Menendez, M., Verdasco, E., Aoiz, F. J., Gonzalez-Sanchez, L., Trahin, Boris, Dartois, Emmanuel, Berné, Olivier, Peeters, Els, He, Jinhua, Sidhu, Ameek, Chown, Ryan, Schroetter, Ilane, Van De Putte, Dries, Canin, Amélie, Alarcón, Felipe, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Cami, Jan, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Vicente, Sílvia, and Wolfire, Mark G.

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

Water is a key ingredient for the emergence of life as we know it. Yet, its destruction and reformation in space remains unprobed in warm gas. Here, we detect the hydroxyl radical (OH) emission from a planet-forming disk exposed to external far-ultraviolet (FUV) radiation with the James Webb Space Telescope. The observations are confronted with the results of quantum dynamical calculations. The highly excited OH infrared rotational lines are the tell-tale signs of H2O destruction by FUV. The OH infrared ro-vibrational lines are attributed to chemical excitation via the key reaction O+H=OH+H which seeds the formation of water in the gas-phase. We infer that the equivalent of the Earth ocean's worth of water is destroyed per month and replenished. These results show that under warm and irradiated conditions water is destroyed and efficiently reformed via gas-phase reactions. This process, assisted by diffusive transport, could reduce the HDO/H2O ratio in the warm regions of planet-forming disks., Comment: Version submitted to Nature Astronomy

Published
2023

7. PDRs4All III: JWST's NIR spectroscopic view of the Orion Bar

Author

Peeters, Els, Habart, Emilie, Berne, Olivier, Sidhu, Ameek, Chown, Ryan, Van De Putte, Dries, Trahin, Boris, Schroetter, Ilane, Canin, Amelie, Alarcon, Felipe, Schefter, Bethany, Khan, Baria, Pasquini, Sofia, Tielens, Alexander G. G. M., Wolfire, Mark G., Dartois, Emmanuel, Goicoechea, Javier R., Maragkoudakis, Alexandros, Onaka, Takashi, Pound, Marc W., Vicente, Silvia, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Cami, Jan, Cuadrado, Sara, Dicken, Daniel, Elyajour, Meriem, Fuente, Asuncion, Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Meshaka, Raphael, Okada, Yoko, Robberto, Massimo, Roellig, Markus, Schirmer, Thiebaut, Tabone, Benoit, Zannese, Marion, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Bejaoui, Salma, Bera, Partha P., Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brunken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Cazaux, Stephanie, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, Foschino, Sacha, Garcia-Lario, Pedro, Gerin, Maryvonne, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jager, Cornelia, Janot-Pacheco, Eduardo, Kaufman, Michael, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Kwok, Sun, Labiano, Alvaro, Lai, Thomas S. -Y., Lee, Timothy J., Lefloch, Bertrand, Petit, Franck Le, Li, Aigen, Linz, Hendrik, Mackie, Cameron J., Madden, Suzanne C., Mascetti, Joelle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Misselt, Karl, Morse, Jon A., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roser, Joseph, Roueff, Evelyne, Rouille, Gael, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

(Abridged) We investigate the impact of radiative feedback from massive stars on their natal cloud and focus on the transition from the HII region to the atomic PDR (crossing the ionisation front (IF)), and the subsequent transition to the molecular PDR (crossing the dissociation front (DF)). We use high-resolution near-IR integral field spectroscopic data from NIRSpec on JWST to observe the Orion Bar PDR as part of the PDRs4All JWST Early Release Science Program. The NIRSpec data reveal a forest of lines including, but not limited to, HeI, HI, and CI recombination lines, ionic lines, OI and NI fluorescence lines, Aromatic Infrared Bands (AIBs including aromatic CH, aliphatic CH, and their CD counterparts), CO2 ice, pure rotational and ro-vibrational lines from H2, and ro-vibrational lines HD, CO, and CH+, most of them detected for the first time towards a PDR. Their spatial distribution resolves the H and He ionisation structure in the Huygens region, gives insight into the geometry of the Bar, and confirms the large-scale stratification of PDRs. We observe numerous smaller scale structures whose typical size decreases with distance from Ori C and IR lines from CI, if solely arising from radiative recombination and cascade, reveal very high gas temperatures consistent with the hot irradiated surface of small-scale dense clumps deep inside the PDR. The H2 lines reveal multiple, prominent filaments which exhibit different characteristics. This leaves the impression of a "terraced" transition from the predominantly atomic surface region to the CO-rich molecular zone deeper in. This study showcases the discovery space created by JWST to further our understanding of the impact radiation from young stars has on their natal molecular cloud and proto-planetary disk, which touches on star- and planet formation as well as galaxy evolution., Comment: 52 pages, 30 figures, submitted to A&A

Published
2023
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8. PDRs4All II: JWST's NIR and MIR imaging view of the Orion Nebula

Author

Habart, Emilie, Peeters, Els, Berné, Olivier, Trahin, Boris, Canin, Amélie, Chown, Ryan, Sidhu, Ameek, Van De Putte, Dries, Alarcón, Felipe, Schroetter, Ilane, Dartois, Emmanuel, Vicente, Sílvia, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Cami, Jan, Cuadrado, Sara, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Tabone, Benoit, Tielens, Alexander G. G. M., Wolfire, Mark G., Zannese, Marion, Ysard, Nathalie, Miville-Deschenes, Marc-Antoine, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Bejaoui, Salma, Bera, Partha P., Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, rew, Candian, Alessandra, Cazaux, Stéphanie, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S. -Y., Lee, Timothy J., Lefloch, Bertrand, Petit, Franck Le, 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., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Omont, Alain, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roser, Joseph, Roueff, Evelyne, Rouillé, Gaël, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Wootten, Alwyn, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The JWST has captured the most detailed and sharpest infrared images ever taken of the inner region of the Orion Nebula, the nearest massive star formation region, and a prototypical highly irradiated dense photo-dissociation region (PDR). We investigate the fundamental interaction of far-ultraviolet photons with molecular clouds. The transitions across the ionization front (IF), dissociation front (DF), and the molecular cloud are studied at high-angular resolution. These transitions are relevant to understanding the effects of radiative feedback from massive stars and the dominant physical and chemical processes that lead to the IR emission that JWST will detect in many Galactic and extragalactic environments. Due to the proximity of the Orion Nebula and the unprecedented angular resolution of JWST, these data reveal that the molecular cloud borders are hyper structured at small angular scales of 0.1-1" (0.0002-0.002 pc or 40-400 au at 414 pc). A diverse set of features are observed such as ridges, waves, globules and photoevaporated protoplanetary disks. At the PDR atomic to molecular transition, several bright features are detected that are associated with the highly irradiated surroundings of the dense molecular condensations and embedded young star. Toward the Orion Bar PDR, a highly sculpted interface is detected with sharp edges and density increases near the IF and DF. This was predicted by previous modeling studies, but the fronts were unresolved in most tracers. A complex, structured, and folded DF surface was traced by the H2 lines. This dataset was used to revisit the commonly adopted 2D PDR structure of the Orion Bar. JWST provides us with a complete view of the PDR, all the way from the PDR edge to the substructured dense region, and this allowed us to determine, in detail, where the emission of the atomic and molecular lines, aromatic bands, and dust originate.

Published
2023
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9. PDRs4All IV. An embarrassment of riches: Aromatic infrared bands in the Orion Bar

Author

Chown, Ryan, Sidhu, Ameek, Peeters, Els, Tielens, Alexander G. G. M., Cami, Jan, Berné, Olivier, Habart, Emilie, Alarcón, Felipe, Canin, Amélie, Schroetter, Ilane, Trahin, Boris, Van De Putte, Dries, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Cuadrado, Sara, Dartois, Emmanuel, Dicken, Daniel, El-Yajouri, Meriem, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Gal, Romane Le, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Vicente, Sílvia, Wolfire, Mark G., Zannese, Marion, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Bejaoui, Salma, Bera, Partha P., Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Cazaux, Stéphanie, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S. -Y., Lee, Timothy J., Lefloch, Bertrand, Petit, Franck Le, 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., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Omont, Alain, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roser, Joseph, Roueff, Evelyne, Rouillé, Gaël, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Wootten, Alwyn, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

(Abridged) Mid-infrared observations of photodissociation regions (PDRs) are dominated by strong emission features called aromatic infrared bands (AIBs). The most prominent AIBs are found at 3.3, 6.2, 7.7, 8.6, and 11.2 $\mu$m. The most sensitive, highest-resolution infrared spectral imaging data ever taken of the prototypical PDR, the Orion Bar, have been captured by JWST. We provide an inventory of the AIBs found in the Orion Bar, along with mid-IR template spectra from five distinct regions in the Bar: the molecular PDR, the atomic PDR, and the HII region. We use JWST NIRSpec IFU and MIRI MRS observations of the Orion Bar from the JWST Early Release Science Program, PDRs4All (ID: 1288). We extract five template spectra to represent the morphology and environment of the Orion Bar PDR. The superb sensitivity and the spectral and spatial resolution of these JWST observations reveal many details of the AIB emission and enable an improved characterization of their detailed profile shapes and sub-components. While the spectra are dominated by the well-known AIBs at 3.3, 6.2, 7.7, 8.6, 11.2, and 12.7 $\mu$m, a wealth of weaker features and sub-components are present. We report trends in the widths and relative strengths of AIBs across the five template spectra. These trends yield valuable insight into the photochemical evolution of PAHs, such as the evolution responsible for the shift of 11.2 $\mu$m AIB emission from class B$_{11.2}$ in the molecular PDR to class A$_{11.2}$ in the PDR surface layers. This photochemical evolution is driven by the increased importance of FUV processing in the PDR surface layers, resulting in a "weeding out" of the weakest links of the PAH family in these layers. For now, these JWST observations are consistent with a model in which the underlying PAH family is composed of a few species: the so-called 'grandPAHs'., Comment: 25 pages, 10 figures, to appear in A&A

Published
2023
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10. OH as a probe of the warm-water cycle in planet-forming disks

Author

Zannese, Marion, Tabone, Benoît, Habart, Emilie, Goicoechea, Javier R., Zanchet, Alexandre, van Dishoeck, Ewine F., van Hemert, Marc C., Black, John H., Tielens, Alexander G. G. M., Veselinova, A., Jambrina, P. G., Menendez, M., Verdasco, E., Aoiz, F. J., Gonzalez-Sanchez, L., Trahin, Boris, Dartois, Emmanuel, Berné, Olivier, Peeters, Els, He, Jinhua, Sidhu, Ameek, Chown, Ryan, Schroetter, Ilane, Van De Putte, Dries, Canin, Amélie, Alarcón, Felipe, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bron, Emeric, Cami, Jan, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Gordon, Karl D., Issa, Lina, Joblin, Christine, Kannavou, Olga, Khan, Baria, 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, Vicente, Sílvia, and Wolfire, Mark G.

Published
2024
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11. The spatially resolved PAH characteristics in the Whirlpool Galaxy (M51a)

Author

Zang, Rong Xuan, Maragkoudakis, Alexandros, and Peeters, Els

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present a detailed study on the spatially resolved polycyclic aromatic hydrocarbon (PAH) emission properties in the (circum)nuclear region (NR) and extranuclear regions (ENRs) of M51a using Spitzer-IRS observations. Correlations among PAH intensity ratios are examined with respect to each other, local physical parameters, galactocentric distance ($R_{g}$), and very small grain (VSG) emission. Additional comparison is performed with the mid-infrared emission features in the H$_{\mathrm{II}}$ regions of M33 and M83. The NR exhibits the strongest correlation among the PAH intensity ratios, whereas ENRs are showing increased scatter attributed to ISM emission. Overall, the radiation field hardness has a higher impact on PAH emission than metallicity, with the latter regulating PAH variance as a function of $R_{g}$. Specifically, the variance of PAH emission with respect to the different physical parameters suggests a higher rate of small/medium PAH processing compared to large PAHs and a higher ratio of small-to-large PAHs formed with increasing galactocentric distance. We find similarities between the 7.7 $\mu$m carriers in M51a's NR and M83's H$_{\mathrm{II}}$ regions, the 8.6 $\mu$m carriers in M51a's NR and M33 H$_{\mathrm{II}}$ regions, and both types of carriers between M51a's ENRs, M33's, and M83's H$_{\mathrm{II}}$ regions. We have identified a positive correlation between PAH/VSG and the PAH intensity ratios. We conclude that the relative abundance of PAHs and VSG is not solely driven by the hardness of the radiation field., Comment: 17 pages, 12 figures, 7 tables. Accepted for publication in MNRAS

Published
2022
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12. PDRs4All: A JWST Early Release Science Program on radiative feedback from massive stars

Author

Berné, Olivier, Habart, Émilie, Peeters, Els, Abergel, Alain, Bergin, Edwin A., Bernard-Salas, Jeronimo, Bron, Emeric, Cami, Jan, Cazaux, Stéphanie, Dartois, Emmanuel, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Okada, Yoko, Onaka, Takashi, Robberto, Massimo, Röllig, Markus, Tielens, Alexander G. G. M., Vicente, Silvia, Wolfire, Mark G., Alarcon, Felipe, Boersma, C., Canin, Ameélie, Chown, Ryan, Dicken, Daniel, Languignon, David, Gal, Romane Le, Pound, Marc W., Trahin, Boris, Simmer, Thomas, Sidhu, Ameek, Van De Putte, Dries, Cuadrado, Sara, Guilloteau, Claire, Maragkoudakis, Alexandros, Schefter, Bethany R., Schirmer, Thiébaut, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Bejaoui, Salma, Bera, Partha P., Bilalbegovic, Goranka, Black, John H., Boulanger, Francois, Bouwman, Jordy, Brandl, Bernhard, Brechignac, Philippe, Brunken, Sandra, Burkhardt, Andrew, Candian, Alessandra, Cernicharo, Jose, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L. J., Demyk, Karine, Meyer, Jennifer Donovan, Engrand, Cécile, Foschino, Sacha, Garcıa-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jaeger, Cornelia, Janot-Pacheco, Eduardo, Joblin, Christine, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Klaassen, Pamela, Knight, Collin, Kwok, Sun, Labiano, Alvaro, Lai, Thomas S. -Y., Lee, Timothy J., Lefloch, Bertrand, Petit, Franck Le, Li, Aigen, Linz, Hendrik, Mackie, Cameron J., Madden, Suzanne C., Mascetti, Joelle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Misselt, Karl, Morse, Jon A., Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Omont, Alain, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roser, Joseph, Roueff, Evelyne, Rouille, Gael, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Sciamma-O'Brien, Ella, Sellgren, Kris, Shannon, Matthew J., Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., and Zhen, Junfeng

Subjects
Astrophysics - Astrophysics of Galaxies
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 datasets 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 datasets 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., Comment: Submitted to PASP

Published
2022
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13. The Star Formation Reference Survey. IV. Stellar mass distribution of local star-forming galaxies

Author

Bonfini, Paolo, Zezas, Andreas, Ashby, Matthew L. N., Willner, Steven P., Maragkoudakis, Alexandros, Kouroumpatzakis, Konstantinos, Sell, Paul. H., and Kovlakas, Konstantinos

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We constrain the mass distribution in nearby, star-forming galaxies with the Star Formation Reference Survey (SFRS), a galaxy sample constructed to be representative of all known combinations of star formation rate (SFR), dust temperature, and specific star formation rate (sSFR) that exist in the Local Universe. An innovative two-dimensional bulge/disk decomposition of the 2MASS/$K_{s}$-band images of the SFRS galaxies yields global luminosity and stellar mass functions, along with separate mass functions for their bulges and disks. These accurate mass functions cover the full range from dwarf galaxies to large spirals, and are representative of star-forming galaxies selected based on their infra-red luminosity, unbiased by AGN content and environment. We measure an integrated luminosity density $j$ = 1.72 $\pm$ 0.93 $\times$ 10$^{9}$ L$_{\odot}$ $h^{-1}$ Mpc$^{-3}$ and a total stellar mass density $\rho_{M}$ = 4.61 $\pm$ 2.40 $\times$ 10$^{8}$ M$_{\odot}$ $h^{-1}$ Mpc$^{-3}$. While the stellar mass of the \emph{average} star-forming galaxy is equally distributed between its sub-components, disks globally dominate the mass density budget by a ratio 4:1 with respect to bulges. In particular, our functions suggest that recent star formation happened primarily in massive systems, where they have yielded a disk stellar mass density larger than that of bulges by more than 1 dex. Our results constitute a reference benchmark for models addressing the assembly of stellar mass on the bulges and disks of local ($z = 0$) star-forming galaxies., Comment: 33 pages, 21 figures, published in MNRAS, 504, 3831-3861 (2021)

Published
2021
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14. The Star Formation Reference Survey-V: the effect of extinction, stellar mass, metallicity, and nuclear activity on star-formation rates based on H$\alpha$ emission

Author

Kouroumpatzakis, Konstantinos, Zezas, Andreas, Maragkoudakis, Alexandros, Willner, Steven P., Bonfini, Paolo, Ashby, Matthew L. N., Sell, Paul H., and Jarrett, Thomas H.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present new H$\alpha$ photometry for the Star-Formation Reference Survey (SFRS), a representative sample of star-forming galaxies in the local Universe. Combining these data with the panchromatic coverage of the SFRS, we provide calibrations of H$\alpha$-based star-formation rates (SFRs) with and without correction for the contribution of [$\rm N_{^{II}}$] emission. We consider the effect of extinction corrections based on the Balmer decrement, infrared excess (IRX), and spectral energy distribution (SED) fits. We compare the SFR estimates derived from SED fits, polycyclic aromatic hydrocarbons, hybrid indicators such as 24 $\mu$m + H$\alpha$, 8 $\mu$m + H$\alpha$, FIR + FUV, and H$\alpha$ emission for a sample of purely star-forming galaxies. We provide a new calibration for 1.4 GHz-based SFRs by comparing to the H$\alpha$ emission, and we measure a dependence of the radio-to-H$\alpha$ emission ratio based on galaxy stellar mass. Active galactic nuclei introduce biases in the calibrations of different SFR indicators but have only a minimal effect on the inferred SFR densities from galaxy surveys. Finally, we quantify the correlation between galaxy metallicity and extinction., Comment: 20 pages, 21 Figures, accepted for publication in MNRAS

Published
2021
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15. Formation of the methyl cation by photochemistry in a protoplanetary disk

Author

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, Jose, 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.

Published
2023
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16. Sub-galactic scaling relations between X-ray luminosity, star-formation rate, and stellar mass

Author

Kouroumpatzakis, Konstantinos, Zezas, Andreas, Sell, Paul, Kovlakas, Konstantinos, Bonfini, Paolo, Willner, Steven, Ashby, Matthew, Maragkoudakis, Alexandros, and Jarrett, Thomas

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

X-ray luminosity ($L_X$) originating from high-mass X-ray binaries (HMXBs) is tightly correlated with the host galaxy's star-formation rate (SFR). We explore this connection at sub-galactic scales spanning ${\sim}$7 dex in SFR and ${\sim}$8 dex in specific SFR (sSFR). There is good agreement with established relations down to ${\rm SFR {\simeq} 10^{-3}\,M_\odot \, yr^{-1}}$, below which an excess of X-ray luminosity emerges. This excess likely arises from low mass X-ray binaries. The intrinsic scatter of the $L_X$-SFR relation is constant, not correlated with SFR. Different star formation indicators scale with $L_X$ in different ways, and we attribute the differences to the effect of star formation history. The SFR derived from H$\alpha$ shows the tightest correlation with X-ray luminosity because H$\alpha$ emission probes stellar populations with ages similar to HMXB formation timescales, but the H$\alpha$-based SFR is reliable only for $\rm sSFR{>}10^{-12}\,M_\odot \, yr^{-1}/M_\odot$., Comment: 19 pages, 13 figures, accepted for publication in MNRAS (2020-04-19)

Published
2020
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17. PDRs4All. VIII. Mid-infrared emission line inventory of the Orion Bar

Author

Van De Putte, Dries, primary, Meshaka, Raphael, additional, Trahin, Boris, additional, Habart, Emilie, additional, Peeters, Els, additional, Berné, Olivier, additional, Alarcón, Felipe, additional, Canin, Amélie, additional, Chown, Ryan, additional, Schroetter, Ilane, additional, Sidhu, Ameek, additional, Boersma, Christiaan, additional, Bron, Emeric, additional, Dartois, Emmanuel, additional, Javier Goicoechea, R., additional, Karl Gordon, D., additional, Onaka, Takashi, additional, Alexander Tielens, G.M., additional, Verstraete, Laurent, additional, Mark Wolfire, G., additional, Abergel, Alain, additional, Edwin Bergin, A., additional, Bernard-Salas, Jeronimo, additional, Cami, Jan, additional, Cuadrado, Sara, additional, Dicken, Daniel, additional, Elyajouri, Meriem, additional, Fuente, Asunción, additional, Joblin, Christine, additional, Khan, Baria, additional, Lacinbala, Ozan, additional, Languignon, David, additional, Le Gal, Romane, additional, Maragkoudakis, Alexandros, additional, Okada, Yoko, additional, Pasquini, Sofia, additional, Marc Pound, W., additional, Robberto, Massimo, additional, Röllig, Markus, additional, Schefter, Bethany, additional, Schirmer, Thiébaut, additional, Tabone, Benoit, additional, Vicente, Sílvia, additional, Zannese, Marion, additional, Sean Colgan, W.J., additional, He, Jinhua, additional, Rouillé, Gaël, additional, Togi, Aditya, additional, Aleman, Isabel, additional, Auchettl, Rebecca, additional, Antonio Baratta, Giuseppe, additional, Bejaoui, Salma, additional, Partha Bera, P., additional, John Black, H., additional, Boulanger, Francois, additional, Bouwman, Jordy, additional, Brandl, Bernhard, additional, Brechignac, Philippe, additional, Brünken, Sandra, additional, Buragohain, Mridusmita, additional, Burkhardt, Andrew, additional, Candian, Alessandra, additional, Cazaux, Stéphanie, additional, Cernicharo, Jose, additional, Chabot, Marin, additional, Chakraborty, Shubhadip, additional, Champion, Jason, additional, Ilsa Cooke, R., additional, Coutens, Audrey, additional, Nick Cox, L.J., additional, Demyk, Karine, additional, Donovan Meyer, Jennifer, additional, Foschino, Sacha, additional, García-Lario, Pedro, additional, Gerin, Maryvonne, additional, Carl Gottlieb, A., additional, Guillard, Pierre, additional, Gusdorf, Antoine, additional, Hartigan, Patrick, additional, Herbst, Eric, additional, Hornekaer, Liv, additional, Issa, Lina, additional, Jäger, Cornelia, additional, Janot-Pacheco, Eduardo, additional, Kannavou, Olga, additional, Kaufman, Michael, additional, Kemper, Francisca, additional, Kendrew, Sarah, additional, Maria Kirsanova, S., additional, Klaassen, Pamela, additional, Kwok, Sun, additional, Labiano, Álvaro, additional, Lai, Thomas S.-Y., additional, Le Floch, Bertrand, additional, Le Petit, Franck, additional, Li, Aigen, additional, Linz, Hendrik, additional, Cameron Mackie, J., additional, Suzanne Madden, C., additional, Mascetti, Joëlle, additional, Brett McGuire, A., additional, Merino, Pablo, additional, Elisabetta Micelotta, R., additional, Jon Morse, A., additional, Mulas, Giacomo, additional, Neelamkodan, Naslim, additional, Ohsawa, Ryou, additional, Omont, Alain, additional, Paladini, Roberta, additional, Elisabetta Palumbo, Maria, additional, Pathak, Amit, additional, Yvonne Pendleton, J., additional, Petrignani, Annemieke, additional, Pino, Thomas, additional, Puga, Elena, additional, Rangwala, Naseem, additional, Rapacioli, Mathias, additional, Rho, Jeonghee, additional, Ricca, Alessandra, additional, Roman-Duval, Julia, additional, Roser, Joseph, additional, Roueff, Evelyne, additional, Salama, Farid, additional, Dinalva Sales, A., additional, Sandstrom, Karin, additional, Sarre, Peter, additional, Sciamma-O'Brien, Ella, additional, Sellgren, Kris, additional, Sachindev Shenoy, S., additional, Teyssier, David, additional, Richard Thomas, D., additional, Adolf Witt, N., additional, Wootten, Alwyn, additional, Ysard, Nathalie, additional, Zettergren, Henning, additional, Zhang, Yong, additional, Ziwei Zhang, E., additional, and Zhen, Junfeng, additional

Published
2024
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19. PDRs4All

Author

Peeters, Els, primary, Habart, Emilie, additional, Berné, Olivier, additional, Sidhu, Ameek, additional, Chown, Ryan, additional, Van De Putte, Dries, additional, Trahin, Boris, additional, Schroetter, Ilane, additional, Canin, Amélie, additional, Alarcón, Felipe, additional, Schefter, Bethany, additional, Khan, Baria, additional, Pasquini, Sofia, additional, Tielens, Alexander G. G. M., additional, Wolfire, Mark G., additional, Dartois, Emmanuel, additional, Goicoechea, Javier R., additional, Maragkoudakis, Alexandros, additional, Onaka, Takashi, additional, Pound, Marc W., additional, Vicente, Sílvia, additional, Abergel, Alain, additional, Bergin, Edwin A., additional, Bernard-Salas, Jeronimo, additional, Boersma, Christiaan, additional, Bron, Emeric, additional, Cami, Jan, additional, Cuadrado, Sara, additional, Dicken, Daniel, additional, Elyajouri, Meriem, additional, Fuente, Asunción, additional, Gordon, Karl D., additional, Issa, Lina, additional, Joblin, Christine, additional, Kannavou, Olga, additional, Lacinbala, Ozan, additional, Languignon, David, additional, Le Gal, Romane, additional, Meshaka, Raphael, additional, Okada, Yoko, additional, Robberto, Massimo, additional, Röllig, Markus, additional, Schirmer, Thiébaut, additional, Tabone, Benoit, additional, Zannese, Marion, additional, Aleman, Isabel, additional, Allamandola, Louis, additional, Auchettl, Rebecca, additional, Baratta, Giuseppe Antonio, additional, Bejaoui, Salma, additional, Bera, Partha P., additional, Black, John H., additional, Boulanger, Francois, additional, Bouwman, Jordy, additional, Brandl, Bernhard, additional, Brechignac, Philippe, additional, Brünken, Sandra, additional, Buragohain, Mridusmita, additional, Burkhardt, Andrew, additional, Candian, Alessandra, additional, Cazaux, Stéphanie, additional, Cernicharo, Jose, additional, Chabot, Marin, additional, Chakraborty, Shubhadip, additional, Champion, Jason, additional, Colgan, Sean W. J., additional, Cooke, Ilsa R., additional, Coutens, Audrey, additional, Cox, Nick L. J., additional, Demyk, Karine, additional, Meyer, Jennifer Donovan, additional, Foschino, Sacha, additional, García-Lario, Pedro, additional, Gerin, Maryvonne, additional, Gottlieb, Carl A., additional, Guillard, Pierre, additional, Gusdorf, Antoine, additional, Hartigan, Patrick, additional, He, Jinhua, additional, Herbst, Eric, additional, Hornekaer, Liv, additional, Jäger, Cornelia, additional, Janot-Pacheco, Eduardo, additional, Kaufman, Michael, additional, Kendrew, Sarah, additional, Kirsanova, Maria S., additional, Klaassen, Pamela, additional, Kwok, Sun, additional, Labiano, Álvaro, additional, Lai, Thomas S.-Y., additional, Lee, Timothy J., additional, Lefloch, Bertrand, additional, Le Petit, Franck, additional, Li, Aigen, additional, Linz, Hendrik, additional, Mackie, Cameron J., additional, Madden, Suzanne C., additional, Mascetti, Joëlle, additional, McGuire, Brett A., additional, Merino, Pablo, additional, Micelotta, Elisabetta R., additional, Misselt, Karl, additional, Morse, Jon A., additional, Mulas, Giacomo, additional, Neelamkodan, Naslim, additional, Ohsawa, Ryou, additional, Paladini, Roberta, additional, Palumbo, Maria Elisabetta, additional, Pathak, Amit, additional, Pendleton, Yvonne J., additional, Petrignani, Annemieke, additional, Pino, Thomas, additional, Puga, Elena, additional, Rangwala, Naseem, additional, Rapacioli, Mathias, additional, Ricca, Alessandra, additional, Roman-Duval, Julia, additional, Roser, Joseph, additional, Roueff, Evelyne, additional, Rouillé, Gaël, additional, Salama, Farid, additional, Sales, Dinalva A., additional, Sandstrom, Karin, additional, Sarre, Peter, additional, Sciamma-O’Brien, Ella, additional, Sellgren, Kris, additional, Shenoy, Sachindev S., additional, Teyssier, David, additional, Thomas, Richard D., additional, Togi, Aditya, additional, Verstraete, Laurent, additional, Witt, Adolf N., additional, Wootten, Alwyn, additional, Ysard, Nathalie, additional, Zettergren, Henning, additional, Zhang, Yong, additional, Zhang, Ziwei E., additional, and Zhen, Junfeng, additional

Published
2024
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20. A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk

Author

Ministerio de Ciencia e Innovación (España), Centre National D'Etudes Spatiales (France), Université Pierre et Marie Curie, Institut Universitaire de France, Centre National de la Recherche Scientifique (France), Canadian Space Agency, Natural Sciences and Engineering Research Council of Canada, San Jose State University Research Foundation, National Aeronautics and Space Administration (US), Japan Society for the Promotion of Science, Royal Society (UK), United Arab Emirates University, National Natural Science Foundation of China, German Research Foundation, Department of Science and Technology (India), Chinese Academy of Sciences, Chinese Academy of Sciences South America Center for Astronomy, Swedish Research Council, #NODATA#, Berné, Olivier, Habart, Emilie, Peeters, Els, Schroetter, Ilane, Canin, Amélie, Sidhu, Ameek, Chown, Ryan, Bron, Emeric, Haworth, Thomas J., Klaassen, Pamela, Trahin, Boris, Abergel, Alain, Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., Zhen, Junfeng, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bera, Partha P., Cami, Jan, Cuadrado, Sara, Dartois, Emmanuel, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Issa, Lina, Joblin, Christine, Black, John H, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Le Gal, Romane, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Boulanger, Francois, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Simmer, Thomas, Tabone, Benoit, Tielens, Alexander G. G.M., Vicente, Sílvia, Wolfire, Mark G., Bouwman, Jordy, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Baruteau, Clément, Bejaoui, Salma, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Le Petit, Franck, Cazaux, Stéphanie, Cernicharo, José, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L J, Demyk, Karine, Li, Aigen, Meyer, Jennifer Donovan, Engrand, Cécile, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Linz, Hendrik, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Mackie, Cameron J., Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S.-Y., Lee, Timothy J., Lefloch, Bertrand, Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Morse, Jon A., Van De Putte, Dries, Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Alarcón, Felipe, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roueff, Evelyne, Rouillé, Gaël, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Zannese, Marion, Sciamma-O'Brien, Ella, Sellgren, Kris, Shannon, Matthew J., Simonnin, Adrien, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, Witt, Adolf N., Ministerio de Ciencia e Innovación (España), Centre National D'Etudes Spatiales (France), Université Pierre et Marie Curie, Institut Universitaire de France, Centre National de la Recherche Scientifique (France), Canadian Space Agency, Natural Sciences and Engineering Research Council of Canada, San Jose State University Research Foundation, National Aeronautics and Space Administration (US), Japan Society for the Promotion of Science, Royal Society (UK), United Arab Emirates University, National Natural Science Foundation of China, German Research Foundation, Department of Science and Technology (India), Chinese Academy of Sciences, Chinese Academy of Sciences South America Center for Astronomy, Swedish Research Council, #NODATA#, Berné, Olivier, Habart, Emilie, Peeters, Els, Schroetter, Ilane, Canin, Amélie, Sidhu, Ameek, Chown, Ryan, Bron, Emeric, Haworth, Thomas J., Klaassen, Pamela, Trahin, Boris, Abergel, Alain, Wootten, Alwyn, Ysard, Nathalie, Zettergren, Henning, Zhang, Yong, Zhang, Ziwei E., Zhen, Junfeng, Bergin, Edwin A., Bernard-Salas, Jeronimo, Boersma, Christiaan, Bera, Partha P., Cami, Jan, Cuadrado, Sara, Dartois, Emmanuel, Dicken, Daniel, Elyajouri, Meriem, Fuente, Asunción, Goicoechea, Javier R., Gordon, Karl D., Issa, Lina, Joblin, Christine, Black, John H, Kannavou, Olga, Khan, Baria, Lacinbala, Ozan, Languignon, David, Le Gal, Romane, Maragkoudakis, Alexandros, Meshaka, Raphael, Okada, Yoko, Onaka, Takashi, Pasquini, Sofia, Boulanger, Francois, Pound, Marc W., Robberto, Massimo, Röllig, Markus, Schefter, Bethany, Schirmer, Thiébaut, Simmer, Thomas, Tabone, Benoit, Tielens, Alexander G. G.M., Vicente, Sílvia, Wolfire, Mark G., Bouwman, Jordy, Aleman, Isabel, Allamandola, Louis, Auchettl, Rebecca, Baratta, Giuseppe Antonio, Baruteau, Clément, Bejaoui, Salma, Brandl, Bernhard, Brechignac, Philippe, Brünken, Sandra, Buragohain, Mridusmita, Burkhardt, Andrew, Candian, Alessandra, Le Petit, Franck, Cazaux, Stéphanie, Cernicharo, José, Chabot, Marin, Chakraborty, Shubhadip, Champion, Jason, Colgan, Sean W. J., Cooke, Ilsa R., Coutens, Audrey, Cox, Nick L J, Demyk, Karine, Li, Aigen, Meyer, Jennifer Donovan, Engrand, Cécile, Foschino, Sacha, García-Lario, Pedro, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Linz, Hendrik, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, Jäger, Cornelia, Janot-Pacheco, Eduardo, Kaufman, Michael, Kemper, Francisca, Kendrew, Sarah, Kirsanova, Maria S., Mackie, Cameron J., Knight, Collin, Kwok, Sun, Labiano, Álvaro, Lai, Thomas S.-Y., Lee, Timothy J., Lefloch, Bertrand, Madden, Suzanne C., Mascetti, Joëlle, McGuire, Brett A., Merino, Pablo, Micelotta, Elisabetta R., Morse, Jon A., Van De Putte, Dries, Mulas, Giacomo, Neelamkodan, Naslim, Ohsawa, Ryou, Paladini, Roberta, Palumbo, Maria Elisabetta, Pathak, Amit, Pendleton, Yvonne J., Petrignani, Annemieke, Pino, Thomas, Puga, Elena, Alarcón, Felipe, Rangwala, Naseem, Rapacioli, Mathias, Ricca, Alessandra, Roman-Duval, Julia, Roueff, Evelyne, Rouillé, Gaël, Salama, Farid, Sales, Dinalva A., Sandstrom, Karin, Sarre, Peter, Zannese, Marion, Sciamma-O'Brien, Ella, Sellgren, Kris, Shannon, Matthew J., Simonnin, Adrien, Shenoy, Sachindev S., Teyssier, David, Thomas, Richard D., Togi, Aditya, Verstraete, Laurent, and Witt, Adolf N.

Abstract

Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photodissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, which affects planet formation within the disks. We report James Webb Space Telescope and Atacama Large Millimeter Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modeling their kinematics and excitation allowed us to constrain the physical conditions within the gas. We quantified the mass-loss rate induced by the FUV irradiation and found that it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk.

Published
2024

21. PDRs4All: III. JWST's NIR spectroscopic view of the Orion Bar.

Author

Peeters, Els, Habart, Emilie, Berné, Olivier, Sidhu, Ameek, Chown, Ryan, Van De Putte, Dries, Trahin, Boris, Schroetter, Ilane, Canin, Amélie, Alarcón, Felipe, Schefter, Bethany, Khan, Baria, Pasquini, Sofia, Tielens, Alexander G. G. M., Wolfire, Mark G., Dartois, Emmanuel, Goicoechea, Javier R., Maragkoudakis, Alexandros, Onaka, Takashi, and Pound, Marc W.

Subjects
INTERSTELLAR medium, CHEMICAL processes, PROTOPLANETARY disks, STARS, GALACTIC evolution, SUPERGIANT stars
Abstract

Context. JWST has taken the sharpest and most sensitive infrared (IR) spectral imaging observations ever of the Orion Bar photodis-sociation region (PDR), which is part of the nearest massive star-forming region the Orion Nebula, and often considered to be the 'prototypical' strongly illuminated PDR. Aims. We investigate the impact of radiative feedback from massive stars on their natal cloud and focus on the transition from the H II region to the atomic PDR – crossing the ionisation front (IF) –, and the subsequent transition to the molecular PDR – crossing the dissociation front (DF). Given the prevalence of PDRs in the interstellar medium and their dominant contribution to IR radiation, understanding the response of the PDR gas to far-ultraviolet (FUV) photons and the associated physical and chemical processes is fundamental to our understanding of star and planet formation and for the interpretation of any unresolved PDR as seen by JWST. Methods. We used high-resolution near-IR integral field spectroscopic data from NIRSpec on JWST to observe the Orion Bar PDR as part of the PDRs4All JWST Early Release Science programme. We constructed a 3″ × 25″' spatio-spectral mosaic covering 0.97– 5.27 μm at a spectral resolution R of ~2700 and an angular resolution of 0.075″–0.173″. To study the properties of key regions captured in this mosaic, we extracted five template spectra in apertures centred on the three H2 dissociation fronts, the atomic PDR, and the H II region. This wealth of detailed spatial-spectral information was analysed in terms of variations in the physical conditions-incident UV field, density, and temperature – of the PDR gas. Results. The NIRSpec data reveal a forest of lines including, but not limited to, He I, H I , and C I recombination lines; ionic lines (e.g. Fe III and Fe II); O I and N I fluorescence lines; aromatic infrared bands (AIBs, including aromatic CH, aliphatic CH, and their CD counterparts); pure rotational and ro-vibrational lines from H2; and ro-vibrational lines from HD, CO, and CH+, with most of them having been detected for the first time towards a PDR. Their spatial distribution resolves the H and He ionisation structure in the Huygens region, gives insight into the geometry of the Bar, and confirms the large-scale stratification of PDRs. In addition, we observed numerous smaller-scale structures whose typical size decreases with distance from θ1 Ori C and IR lines from C I , if solely arising from radiative recombination and cascade, reveal very high gas temperatures (a few 1000 K) consistent with the hot irradiated surface of small-scale dense clumps inside the PDR. The morphology of the Bar, in particular that of the H2 lines, reveals multiple prominent filaments that exhibit different characteristics. This leaves the impression of a 'terraced' transition from the predominantly atomic surface region to the CO-rich molecular zone deeper in. We attribute the different characteristics of the H2 filaments to their varying depth into the PDR and, in some cases, not reaching the C+/C/CO transition. These observations thus reveal what local conditions are required to drive the physical and chemical processes needed to explain the different characteristics of the DFs and the photochemical evolution of the AIB carriers. Conclusions. This study showcases the discovery space created by JWST to further our understanding of the impact radiation from young stars has on their natal molecular cloud and proto-planetary disk, which touches on star and planet formation as well as galaxy evolution. [ABSTRACT FROM AUTHOR]

Published
2024
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22. Anharmonic IR absorption spectra of the prototypical interstellar PAHs phenanthrene, pyrene, and pentacene in their neutral and cation states.

Author

Esposito, Vincent J., Allamandola, Louis J., Boersma, Christiaan, Bregman, Jesse D., Fortenberry, Ryan C., Maragkoudakis, Alexandros, and Temi, Pasquale

Subjects
ABSORPTION spectra, PENTACENE, PHENANTHRENE, POLYCYCLIC aromatic hydrocarbons, PYRENE
Abstract

Combination band and overtone transitions of polycyclic aromatic hydrocarbon (PAH) cations in the 2000–2900 cm-1 (5-3.5 µm) region are implicated as carriers of the 'quasi-continuum' observed in the near-infrared (IR) emission spectra of many astronomical objects. In neutral PAHs, the strongest absorption features are concentrated in the 700–900 cm-1 (14–11 µm) range, which are associated with CH out-of-plane bending motions. Upon ionization, this shifts to the 1000–1600 cm-1 (10–6 µm) range, where bands are associated with C=C stretches and CH in-plane bends. Anharmonicity is required to accurately characterize the IR absorption spectrum of PAHs, indicated herein by the ability to directly assign the bands in high-resolution experimental absorption spectra of neutral and cationic phenanthrene, pyrene, and pentacene. Neutral PAHs are indicated as the source of the strong 3.3 and 11.2 µm astronomical PAH features, while the broad features in the 6–10 µm region and the 'quasi-continuum' from 3.5–5 µm stem from PAH cations. This study reinforces the need for including anharmonicity in the computation of IR absorption and emission spectra of larger and more complex PAHs. This is particularly pertinent to the interpretation of data returned by JWST. [ABSTRACT FROM AUTHOR]

Published
2024
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24. 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

25. 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

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

Author

Berné, Olivier, additional, Habart, Émilie, additional, Peeters, Els, additional, Abergel, Alain, additional, Bergin, Edwin A., additional, Bernard-Salas, Jeronimo, additional, Bron, Emeric, additional, Cami, Jan, additional, Dartois, Emmanuel, additional, Fuente, Asunción, additional, Goicoechea, Javier R., additional, Gordon, Karl D., additional, Okada, Yoko, additional, Onaka, Takashi, additional, Robberto, Massimo, additional, Röllig, Markus, additional, Tielens, Alexander G. G. M., additional, Vicente, Sílvia, additional, Wolfire, Mark G., additional, Alarcón, Felipe, additional, Boersma, C., additional, Canin, Amélie, additional, Chown, Ryan, additional, Dicken, Daniel, additional, Languignon, David, additional, Le Gal, Romane, additional, Pound, Marc W., additional, Trahin, Boris, additional, Simmer, Thomas, additional, Sidhu, Ameek, additional, Van De Putte, Dries, additional, Cuadrado, Sara, additional, Guilloteau, Claire, additional, Maragkoudakis, Alexandros, additional, Schefter, Bethany R., additional, Schirmer, Thiébaut, additional, Cazaux, Stéphanie, additional, Aleman, Isabel, additional, Allamandola, Louis, additional, Auchettl, Rebecca, additional, Antonio Baratta, Giuseppe, additional, Bejaoui, Salma, additional, Bera, Partha P., additional, Bilalbegović, Goranka, additional, Black, John H., additional, Boulanger, Francois, additional, Bouwman, Jordy, additional, Brandl, Bernhard, additional, Brechignac, Philippe, additional, Brünken, Sandra, additional, Burkhardt, Andrew, additional, Candian, Alessandra, additional, Cernicharo, Jose, additional, Chabot, Marin, additional, Chakraborty, Shubhadip, additional, Champion, Jason, additional, Colgan, Sean W. J., additional, Cooke, Ilsa R., additional, Coutens, Audrey, additional, Cox, Nick L. J., additional, Demyk, Karine, additional, Donovan Meyer, Jennifer, additional, Engrand, Cécile, additional, Foschino, Sacha, additional, García-Lario, Pedro, additional, Gavilan, Lisseth, additional, Gerin, Maryvonne, additional, Godard, Marie, additional, Gottlieb, Carl A., additional, Guillard, Pierre, additional, Gusdorf, Antoine, additional, Hartigan, Patrick, additional, He, Jinhua, additional, Herbst, Eric, additional, Hornekaer, Liv, additional, Jäger, Cornelia, additional, Janot-Pacheco, Eduardo, additional, Joblin, Christine, additional, Kaufman, Michael, additional, Kemper, Francisca, additional, Kendrew, Sarah, additional, Kirsanova, Maria S., additional, Klaassen, Pamela, additional, Knight, Collin, additional, Kwok, Sun, additional, Labiano, Álvaro, additional, Lai, Thomas S.-Y., additional, Lee, Timothy J., additional, Lefloch, Bertrand, additional, Le Petit, Franck, additional, Li, Aigen, additional, Linz, Hendrik, additional, Mackie, Cameron J., additional, Madden, Suzanne C., additional, Mascetti, Joëlle, additional, McGuire, Brett A., additional, Merino, Pablo, additional, Micelotta, Elisabetta R., additional, Misselt, Karl, additional, Morse, Jon A., additional, Mulas, Giacomo, additional, Neelamkodan, Naslim, additional, Ohsawa, Ryou, additional, Omont, Alain, additional, Paladini, Roberta, additional, Elisabetta Palumbo, Maria, additional, Pathak, Amit, additional, Pendleton, Yvonne J., additional, Petrignani, Annemieke, additional, Pino, Thomas, additional, Puga, Elena, additional, Rangwala, Naseem, additional, Rapacioli, Mathias, additional, Ricca, Alessandra, additional, Roman-Duval, Julia, additional, Roser, Joseph, additional, Roueff, Evelyne, additional, Rouillé, Gaël, additional, Salama, Farid, additional, Sales, Dinalva A., additional, Sandstrom, Karin, additional, Sarre, Peter, additional, Sciamma-O’Brien, Ella, additional, Sellgren, Kris, additional, Shannon, Matthew J., additional, Shenoy, Sachindev S., additional, Teyssier, David, additional, Thomas, Richard D., additional, Togi, Aditya, additional, Verstraete, Laurent, additional, Witt, Adolf N., additional, Wootten, Alwyn, additional, Ysard, Nathalie, additional, Zettergren, Henning, additional, Zhang, Yong, additional, Zhang, Ziwei E., additional, and Zhen, Junfeng, additional

Published
2022
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28. spatially resolved PAH characteristics in the Whirlpool Galaxy (M51a).

Author

Zang, Rong Xuan, Maragkoudakis, Alexandros, and Peeters, Els

Subjects
*POLYCYCLIC aromatic hydrocarbons, *GALAXIES, *INTERSTELLAR medium
Abstract

We present a detailed study on the spatially resolved polycyclic aromatic hydrocarbon (PAH) emission properties in the (circum)nuclear region (NR) and extranuclear regions (ENRs) of M51a using Spitzer -IRS (infrared spectrograph) observations. Correlations among PAH intensity ratios are examined with respect to each other, local physical parameters, galactocentric distance (R g), and very small grain (VSG) emission. Additional comparison is performed with the mid-infrared emission features in the H  ii regions of M33 and M83. The NR exhibits the strongest correlation among the PAH intensity ratios, whereas ENRs are showing increased scatter attributed to interstellar medium emission. Overall, the radiation field hardness has a higher impact on PAH emission than metallicity, with the latter regulating PAH variance as a function of R g. Specifically, the variance of PAH emission with respect to the different physical parameters suggests a higher rate of small/medium PAH processing compared to large PAHs and a higher ratio of small-to-large PAHs formed with increasing galactocentric distance. We find similarities between the 7.7 |$\mu$| m carriers in M51a's NR and M83's H  ii regions, the 8.6 |$\mu$| m carriers in M51a's NR and M33 H  ii regions, and both types of carriers between M51a's ENRs, M33's, and M83's H  ii regions. We have identified a positive correlation between PAH/VSG and the PAH intensity ratios. We conclude that the relative abundance of PAHs and VSG is not solely driven by the hardness of the radiation field. [ABSTRACT FROM AUTHOR]

Published
2022
Full Text
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29. PDRs4All: A JWST Early Release Science Program on Radiative Feedback from Massive Stars

Author

Olivier Berné, Émilie Habart, Els Peeters, Alain Abergel, Edwin A. Bergin, Jeronimo Bernard-Salas, Emeric Bron, Jan Cami, Emmanuel Dartois, Asunción Fuente, Javier R. Goicoechea, Karl D. Gordon, Yoko Okada, Takashi Onaka, Massimo Robberto, Markus Röllig, Alexander G. G. M. Tielens, Sílvia Vicente, Mark G. Wolfire, Felipe Alarcón, C. Boersma, Amélie Canin, Ryan Chown, Daniel Dicken, David Languignon, Romane Le Gal, Marc W. Pound, Boris Trahin, Thomas Simmer, Ameek Sidhu, Dries Van De Putte, Sara Cuadrado, Claire Guilloteau, Alexandros Maragkoudakis, Bethany R. Schefter, Thiébaut Schirmer, Stéphanie Cazaux, Isabel Aleman, Louis Allamandola, Rebecca Auchettl, Giuseppe Antonio Baratta, Salma Bejaoui, Partha P. Bera, Goranka Bilalbegović, John H. Black, Francois Boulanger, Jordy Bouwman, Bernhard Brandl, Philippe Brechignac, Sandra Brünken, Andrew Burkhardt, Alessandra Candian, Jose Cernicharo, Marin Chabot, Shubhadip Chakraborty, Jason Champion, Sean W. J. Colgan, Ilsa R. Cooke, Audrey Coutens, Nick L. J. Cox, Karine Demyk, Jennifer Donovan Meyer, Cécile Engrand, Sacha Foschino, Pedro García-Lario, Lisseth Gavilan, Maryvonne Gerin, Marie Godard, Carl A. Gottlieb, Pierre Guillard, Antoine Gusdorf, Patrick Hartigan, Jinhua He, Eric Herbst, Liv Hornekaer, Cornelia Jäger, Eduardo Janot-Pacheco, Christine Joblin, Michael Kaufman, Francisca Kemper, Sarah Kendrew, Maria S. Kirsanova, Pamela Klaassen, Collin Knight, Sun Kwok, Álvaro Labiano, Thomas S.-Y. Lai, Timothy J. Lee, Bertrand Lefloch, Franck Le Petit, Aigen Li, Hendrik Linz, Cameron J. Mackie, Suzanne C. Madden, Joëlle Mascetti, Brett A. McGuire, Pablo Merino, Elisabetta R. Micelotta, Karl Misselt, Jon A. Morse, Giacomo Mulas, Naslim Neelamkodan, Ryou Ohsawa, Alain Omont, Roberta Paladini, Maria Elisabetta Palumbo, Amit Pathak, Yvonne J. Pendleton, Annemieke Petrignani, Thomas Pino, Elena Puga, Naseem Rangwala, Mathias Rapacioli, Alessandra Ricca, Julia Roman-Duval, Joseph Roser, Evelyne Roueff, Gaël Rouillé, Farid Salama, Dinalva A. Sales, Karin Sandstrom, Peter Sarre, Ella Sciamma-O’Brien, Kris Sellgren, Matthew J. Shannon, Sachindev S. Shenoy, David Teyssier, Richard D. Thomas, Aditya Togi, Laurent Verstraete, Adolf N. Witt, Alwyn Wootten, Nathalie Ysard, Henning Zettergren, Yong Zhang, Ziwei E. Zhang, Junfeng Zhen, Institut de recherche en astrophysique et planétologie (IRAP), 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), Institut d'astrophysique spatiale (IAS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), University of Western Ontario (UWO), Carl Sagan Center, SETI Institute, University of Michigan [Ann Arbor], University of Michigan System, Analytic and Computational Research, Inc. - Earth Sciences (ACRI-ST), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique et Atmosphères = Laboratory for Studies of Radiation and Matter in Astrophysics and Atmospheres (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-CY Cergy Paris Université (CY), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Observatorio Astronomico Nacional, Madrid, Instituto de Física Fundamental [Madrid] (IFF), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universiteit Gent = Ghent University (UGENT), Space Telescope Science Institute (STSci), Physikalisches Institut [Köln], Universität zu Köln = University of Cologne, Meisei University, The University of Tokyo (UTokyo), Leiden Observatory [Leiden], Universiteit Leiden, Johns Hopkins University (JHU), Instituto de Astrofísica e Ciências do Espaço (IASTRO), University of Maryland [College Park], University of Maryland System, NASA Ames Research Center (ARC), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Signal et Communications (IRIT-SC), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université de Toulouse (UT)-Toulouse Mind & Brain Institut (TMBI), Université Toulouse - Jean Jaurès (UT2J), Université de Toulouse (UT)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université Toulouse Capitole (UT Capitole), Université de Toulouse (UT), Institut National Polytechnique (Toulouse) (Toulouse INP), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], Delft University of Technology (TU Delft), Universidade Federal de Itajubá, Bay Area Environmental Research Institute (BAER), Australian Synchrotron [Clayton], INAF - Osservatorio Astrofisico di Catania (OACT), Istituto Nazionale di Astrofisica (INAF), University of Zagreb, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Département de Physique de l'ENS-PSL, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), University of Colorado [Boulder], Institute for Molecules and Materials [Nijmegen], Radboud University [Nijmegen], Wellesley College, Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut de Physique de Rennes (IPR), Université de Rennes (UR)-Centre National de la Recherche Scientifique (CNRS), University of British Columbia (UBC), National Radio Astronomy Observatory [Charlottesville] (NRAO), National Radio Astronomy Observatory (NRAO), European Space Astronomy Centre (ESAC), Agence Spatiale Européenne = European Space Agency (ESA), Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University-Smithsonian Institution, 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), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Rice University [Houston], Yunnan Observatories, Chinese Academy of Sciences [Changchun Branch] (CAS), Universidad de Chile = University of Chile [Santiago] (UCHILE), University of Virginia, Aarhus University [Aarhus], Friedrich-Schiller-Universität = Friedrich Schiller University Jena [Jena, Germany], Instituto de Astronomia, Geofísica e Ciências Atmosféricas [São Paulo] (IAG), Universidade de São Paulo = University of São Paulo (USP), San Jose State University [San Jose] (SJSU), European Southern Observatory (ESO), Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), Academia Sinica, Institute of Astronomy of the Russian Academy of Sciences (INASAN), Russian Academy of Sciences [Moscow] (RAS), UK Astronomy Technology Centre (UK ATC), Science and Technology Facilities Council (STFC), Telespazio, Services par satellites, Infrared Processing and Analysis Center (IPAC), California Institute of Technology (CALTECH), University of Missouri [Columbia] (Mizzou), University of Missouri System, Max Planck Institute for Astronomy (MPIA), CAS Key Laboratory of Crust–Mantle Materials and Environments [Hefei], School of Earth and Space Sciences [Hefei], University of Science and Technology of China [Hefei] (USTC)-University of Science and Technology of China [Hefei] (USTC)-Chinese Academy of Sciences [Beijing] (CAS), Lawrence Berkeley National Laboratory [Berkeley] (LBNL), University of California [Berkeley] (UC Berkeley), University of California (UC), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut des Sciences Moléculaires (ISM), Université Montesquieu - Bordeaux 4-Université Sciences et Technologies - Bordeaux 1 (UB)-École Nationale Supérieure de Chimie et de Physique de Bordeaux (ENSCPB)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS), Massachusetts Institute of Technology (MIT), Instituto de Ciencia de Materiales de Madrid (ICMM), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, Steward Observatory, University of Arizona, INAF - Osservatorio Astronomico di Cagliari (OAC), United Arab Emirates University (UAEU), National Astronomical Observatory of Japan (NAOJ), Banaras Hindu University [Varanasi] (BHU), University of Amsterdam [Amsterdam] (UvA), Laboratoire de Chimie et Physique Quantiques Laboratoire (LCPQ), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut de Chimie du CNRS (INC)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche « Matière et interactions » (FeRMI), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Université de Toulouse (UT)-Institut National des Sciences Appliquées (INSA)-Centre National de la Recherche Scientifique (CNRS), Universidade Federal do Rio Grande do Sul [Porto Alegre] (UFRGS), University of California [San Diego] (UC San Diego), University of Nottingham, UK (UON), Ohio State University [Columbus] (OSU), Space Science Institute [Boulder] (SSI), Stockholm University, Texas State University, Ritter Astrophysical Research Center, University of Toledo, National Sun Yat-Sen University (NSYSU), Star and Planet Formation Laboratory, ITA, USA, GBR, FRA, DEU, ESP, AUS, BEL, BRA, CHL, TWN, HRV, DNK, JPN, IND, NLD, PRT, CHN, RUS, SWE, National Aeronautics and Space Administration (US), University of Maryland, University of Michigan, 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 José State University Research Foundation, 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, Le Gal, Romane, Pound, Marc W., Trahin, Boris, Sidhu, Ameek, Van De Putte, Dries, Cuadrado, Sara, Guilloteau, Claire, Maragkoudakis, Alexandros, Schefter, Bethany R., Schirmer, Thiébaut, 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, Brünken, Sandra, Burkhardt, Andrew, Candian, Alessandra, Cernicharo, José, 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, Gavilan, Lisseth, Gerin, Maryvonne, Godard, Marie, Gottlieb, Carl A., Guillard, Pierre, Gusdorf, Antoine, Hartigan, Patrick, He, Jinhua, Herbst, Eric, Hornekaer, Liv, 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., Morse, Jon A., Molecular Spectroscopy (HIMS, FNWI), and HIMS (FNWI)

Subjects
Gaseous Nebulae, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, FELIX Infrared and Terahertz Spectroscopy, Star Forming Regions, Astrophysics - Astrophysics of Galaxies, Infrared Telescopes, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, [INFO]Computer Science [cs], Photodissociation Regions, Astrophysics::Earth and Planetary Astrophysics, Polycyclic Aromatic Hydrocarbons, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], James Webb Space Telescope (JWST), Photo-Dissociation Regions (PDRs), Massive stars, Orion Bar, MIRI, NIRSpec, NIRCam, Astrophysics::Galaxy Astrophysics
Abstract

22 pags., 8 figs., 1 tab., 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., Support for JWST-ERS program ID 1288 was provided through grants from the STScI under NASA contract NAS5-03127 to STScI (K.G., D.V.D.P., M.R.), Univ. of Maryland (M.W., M.P.), Univ. of Michigan (E.B., F.A.), and Univ. of Toledo (T.S.-Y.L.). O.B. and E.H. are supported by the Programme National “Physique et Chimie du Milieu Interstellaire” (PCMI) of CNRS/INSU with INC/INP co-funded by CEA and CNES, and through APR grants 6315 and 6410 provided by CNES. E. P. and J.C. acknowledge support from the National Science and Engineering Council of Canada (NSERC) Discovery Grant program (RGPIN-2020-06434 and RGPIN-2021-04197 respectively). E.P. acknowledges support from a Western Strategic Support Accelerator Grant (ROLA ID 0000050636). J.R.G. and S.C. thank the Spanish MCINN for funding support under grant PID2019-106110GB-I00. Work by M.R. and Y.O. is carried out within the Collaborative Research Centre 956, subproject C1, funded by the Deutsche Forschungsgemeinschaft (DFG)—project ID 184018867. T.O. acknowledges support from JSPS Bilateral Program, grant No. 120219939. M.P. and M.W. acknowledge support from NASA Astrophysics Data Analysis Program award #80NSSC19K0573. C.B. is grateful for an appointment at NASA Ames Research Center through the San José State University Research Foundation (NNX17AJ88A) and acknowledges support from the Internal Scientist Funding Model (ISFM) Directed Work Package at NASA Ames titled: “Laboratory Astrophysics—The NASA Ames PAH IR Spectroscopic Database.”

Published
2022
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30. A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk.

Author

Berné O, Habart E, Peeters E, Schroetter I, Canin A, Sidhu A, Chown R, Bron E, Haworth TJ, Klaassen P, Trahin B, Van De Putte D, Alarcón F, Zannese M, Abergel A, Bergin EA, Bernard-Salas J, Boersma C, Cami J, Cuadrado S, Dartois E, Dicken D, Elyajouri M, Fuente A, Goicoechea JR, Gordon KD, Issa L, Joblin C, Kannavou O, Khan B, Lacinbala O, Languignon D, Le Gal R, Maragkoudakis A, Meshaka R, Okada Y, Onaka T, Pasquini S, Pound MW, Robberto M, Röllig M, Schefter B, Schirmer T, Simmer T, Tabone B, Tielens AGGM, Vicente S, Wolfire MG, Aleman I, Allamandola L, Auchettl R, Baratta GA, Baruteau C, Bejaoui S, Bera PP, Black JH, Boulanger F, Bouwman J, Brandl B, Brechignac P, Brünken S, Buragohain M, Burkhardt A, Candian A, Cazaux S, Cernicharo J, Chabot M, Chakraborty S, Champion J, Colgan SWJ, Cooke IR, Coutens A, Cox NLJ, Demyk K, Meyer JD, Engrand C, Foschino S, García-Lario P, Gavilan L, Gerin M, Godard M, Gottlieb CA, Guillard P, Gusdorf A, Hartigan P, He J, Herbst E, Hornekaer L, Jäger C, Janot-Pacheco E, Kaufman M, Kemper F, Kendrew S, Kirsanova MS, Knight C, Kwok S, Labiano Á, Lai TS, Lee TJ, Lefloch B, Le Petit F, Li A, Linz H, Mackie CJ, Madden SC, Mascetti J, McGuire BA, Merino P, Micelotta ER, Morse JA, Mulas G, Neelamkodan N, Ohsawa R, Paladini R, Palumbo ME, Pathak A, Pendleton YJ, Petrignani A, Pino T, Puga E, Rangwala N, Rapacioli M, Ricca A, Roman-Duval J, Roueff E, Rouillé G, Salama F, Sales DA, Sandstrom K, Sarre P, Sciamma-O'Brien E, Sellgren K, Shannon MJ, Simonnin A, Shenoy SS, Teyssier D, Thomas RD, Togi A, Verstraete L, Witt AN, Wootten A, Ysard N, Zettergren H, Zhang Y, Zhang ZE, and Zhen J

Abstract

Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photodissociation regions (PDRs) on the surfaces of protoplanetary disks around low-mass stars, which affects planet formation within the disks. We report James Webb Space Telescope and Atacama Large Millimeter Array observations of a FUV-irradiated protoplanetary disk in the Orion Nebula. Emission lines are detected from the PDR; modeling their kinematics and excitation allowed us to constrain the physical conditions within the gas. We quantified the mass-loss rate induced by the FUV irradiation and found that it is sufficient to remove gas from the disk in less than a million years. This is rapid enough to affect giant planet formation in the disk.

Published
2024
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