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1. 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

2. 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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3. 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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4. Photochemical hazes can trace the C/O ratio in exoplanet atmospheres

Author: Corrales, Lia, Gavilan, Lisseth, Teal, D. J., and Kempton, Eliza M. -R.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: Photochemical hazes are suspected to obscure molecular features, such as water, from detection in the transmission spectra of exoplanets with atmospheric temperatures < 800 K. The opacities of laboratory produced organic compounds (tholins) from Khare et al. (1984) have become a standard for modeling haze in exoplanet atmospheres. However, these tholins were grown in an oxygen-free, Titan-like environment that is very different from typical assumptions for exoplanets, where C/O~0.5. This work presents the 0.13-10 micron complex refractive indices derived from laboratory transmission measurements of tholins grown in environments with different oxygen abundances. With the increasing uptake of oxygen, absorption increases across the entire wavelength range, and a scattering feature around 6 micron shifts towards shorter wavelengths and becomes more peaked around 5.8 micron, due to a C=O stretch resonance. Using GJ 1214b as a test-case, we examine the transmission spectra of a sub-Neptune planet with C/O ratios of solar, 1, and 1000 to evaluate the effective differences between our opacities and those of Khare. For an atmosphere with solar hydrogen and helium abundances, we find a difference of 200-1500 ppm, but for high-metallicity (Z=1000) environments, the difference may only be 20 ppm. The 1-2 micron transmission data for GJ 1214b rule out the Titan-like haze model, and are more consistent with C/O=1 and C/O=solar haze models. This work demonstrates that using haze opacities that are more consistent with underlying assumptions about bulk atmospheric composition are important for building self-consistent models that appropriately constrain the atmospheric C/O ratio, even when molecular features are obscured., Comment: accepted to ApJL
Published: 2023
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5. 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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6. RotNet: Fast and Scalable Estimation of Stellar Rotation Periods Using Convolutional Neural Networks

Author: Johnson, J. Emmanuel, Sundaresan, Sairam, Daylan, Tansu, Gavilan, Lisseth, Giles, Daniel K., Silva, Stela Ishitani, Jungbluth, Anna, Morris, Brett, and Muñoz-Jaramillo, Andrés
Subjects: Astrophysics - Solar and Stellar Astrophysics, Computer Science - Machine Learning
Abstract: Magnetic activity in stars manifests as dark spots on their surfaces that modulate the brightness observed by telescopes. These light curves contain important information on stellar rotation. However, the accurate estimation of rotation periods is computationally expensive due to scarce ground truth information, noisy data, and large parameter spaces that lead to degenerate solutions. We harness the power of deep learning and successfully apply Convolutional Neural Networks to regress stellar rotation periods from Kepler light curves. Geometry-preserving time-series to image transformations of the light curves serve as inputs to a ResNet-18 based architecture which is trained through transfer learning. The McQuillan catalog of published rotation periods is used as ansatz to groundtruth. We benchmark the performance of our method against a random forest regressor, a 1D CNN, and the Auto-Correlation Function (ACF) - the current standard to estimate rotation periods. Despite limiting our input to fewer data points (1k), our model yields more accurate results and runs 350 times faster than ACF runs on the same number of data points and 10,000 times faster than ACF runs on 65k data points. With only minimal feature engineering our approach has impressive accuracy, motivating the application of deep learning to regress stellar parameters on an even larger scale, Comment: Accepted for the Machine Learning and the Physical Sciences Workshop, NeurIPS 2020
Published: 2020

7. The Need for Laboratory Measurements and Ab Initio Studies to Aid Understanding of Exoplanetary Atmospheres

Author: Fortney, Jonathan J., Robinson, Tyler D., Domagal-Goldman, Shawn, Del Genio, Anthony D., Gordon, Iouli E., Gharib-Nezhad, Ehsan, Lewis, Nikole, Sousa-Silva, Clara, Airapetian, Vladimir, Drouin, Brian, Hargreaves, Robert J., Huang, Xinchuan, Karman, Tijs, Ramirez, Ramses M., Rieker, Gregory B., Tennyson, Jonathan, Wordsworth, Robin, Yurchenko, Sergei N, Johnson, Alexandria V, Lee, Timothy J., Dong, Chuanfei, Kane, Stephen, Lopez-Morales, Mercedes, Fauchez, Thomas, Lee, Timothy, Marley, Mark S., Sung, Keeyoon, Haghighipour, Nader, Robinson, Tyler, Horst, Sarah, Gao, Peter, Kao, Der-you, Dressing, Courtney, Lupu, Roxana, Savin, Daniel Wolf, Fleury, Benjamin, Venot, Olivia, Ascenzi, Daniela, Milam, Stefanie, Linnartz, Harold, Gudipati, Murthy, Gronoff, Guillaume, Salama, Farid, Gavilan, Lisseth, Bouwman, Jordy, Turbet, Martin, Benilan, Yves, Henderson, Bryana, Batalha, Natalie, Jensen-Clem, Rebecca, Lyons, Timothy, Freedman, Richard, Schwieterman, Edward, Goyal, Jayesh, Mancini, Luigi, Irwin, Patrick, Desert, Jean-Michel, Molaverdikhani, Karan, Gizis, John, Taylor, Jake, Lothringer, Joshua, Pierrehumbert, Raymond, Zellem, Robert, Batalha, Natasha, Rugheimer, Sarah, Lustig-Yaeger, Jacob, Hu, Renyu, Kempton, Eliza, Arney, Giada, Line, Mike, Alam, Munazza, Moses, Julianne, Iro, Nicolas, Kreidberg, Laura, Blecic, Jasmina, Louden, Tom, Molliere, Paul, Stevenson, Kevin, Swain, Mark, Bott, Kimberly, Madhusudhan, Nikku, Krissansen-Totton, Joshua, Deming, Drake, Kitiashvili, Irina, Shkolnik, Evgenya, Rustamkulov, Zafar, Rogers, Leslie, and Close, Laird
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: We are now on a clear trajectory for improvements in exoplanet observations that will revolutionize our ability to characterize their atmospheric structure, composition, and circulation, from gas giants to rocky planets. However, exoplanet atmospheric models capable of interpreting the upcoming observations are often limited by insufficiencies in the laboratory and theoretical data that serve as critical inputs to atmospheric physical and chemical tools. Here we provide an up-to-date and condensed description of areas where laboratory and/or ab initio investigations could fill critical gaps in our ability to model exoplanet atmospheric opacities, clouds, and chemistry, building off a larger 2016 white paper, and endorsed by the NAS Exoplanet Science Strategy report. Now is the ideal time for progress in these areas, but this progress requires better access to, understanding of, and training in the production of spectroscopic data as well as a better insight into chemical reaction kinetics both thermal and radiation-induced at a broad range of temperatures. Given that most published efforts have emphasized relatively Earth-like conditions, we can expect significant and enlightening discoveries as emphasis moves to the exotic atmospheres of exoplanets., Comment: Submitted as an Astro2020 Science White Paper
Published: 2019

8. Evolution of Titan s high-altitude aerosols under ultraviolet irradiation

Author: Carrasco, Nathalie, Tigrine, Sarah, Gavilan, Lisseth, Nahon, Laurent, and Gudipati, Murthy S.
Subjects: Astrophysics - Earth and Planetary Astrophysics
Abstract: The Cassini-Huygens space mission revealed that Titan s thick brownish haze is initiated high in the atmosphere at about 1000 km of altitude, before a slow transportation down to the surface. Close to the surface at altitudes below 130 km, the Huygens probe provided information on the chemical composition of the haze. So far we do not have insights on a possible photochemical evolution of the aerosols composing the haze during their descent. We address here this atmospheric aerosol aging process, simulating in the laboratory how solar vacuum-ultraviolet (VUV) irradiation affects the aerosol optical properties as probed by infrared spectroscopy. An important evolution is found, which could explain the apparent contradiction between the nitrogen-poor infrared spectroscopic signature observed by Cassini below 600 km of altitude in Titan s atmosphere, and a high nitrogen content as measured by the Aerosol Collector and Pyroliser of Huygens probe at the surface of Titan.
Published: 2018
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9. The Need for Laboratory Measurements and Ab Initio Studies to Aid Understanding of Exoplanetary Atmospheres

Author: Fortney, Jonathan J, Robinson, Tyler D, Domagal-Goldman, Shawn, Genio, Anthony D Del, Gordon, Iouli E, Gharib-Nezhad, Ehsan, Lewis, Nikole, Sousa-Silva, Clara, Airapetian, Vladimir, Drouin, Brian, Hargreaves, Robert J, Huang, Xinchuan, Karman, Tijs, Ramirez, Ramses M, Rieker, Gregory B, Tennyson, Jonathan, Wordsworth, Robin, Yurchenko, Sergei N, Johnson, Alexandria V, Lee, Timothy J, Dong, Chuanfei, Kane, Stephen, Lopez-Morales, Mercedes, Fauchez, Thomas, Lee, Timothy, Marley, Mark S, Sung, Keeyoon, Haghighipour, Nader, Robinson, Tyler, Horst, Sarah, Gao, Peter, Kao, Der-you, Dressing, Courtney, Lupu, Roxana, Savin, Daniel Wolf, Fleury, Benjamin, Venot, Olivia, Ascenzi, Daniela, Milam, Stefanie, Linnartz, Harold, Gudipati, Murthy, Gronoff, Guillaume, Salama, Farid, Gavilan, Lisseth, Bouwman, Jordy, Turbet, Martin, Benilan, Yves, Henderson, Bryana, Batalha, Natalie, Jensen-Clem, Rebecca, Lyons, Timothy, Freedman, Richard, Schwieterman, Edward, Goyal, Jayesh, Mancini, Luigi, Irwin, Patrick, Desert, Jean-Michel, Molaverdikhani, Karan, Gizis, John, Taylor, Jake, Lothringer, Joshua, Pierrehumbert, Raymond, Zellem, Robert, Batalha, Natasha, Rugheimer, Sarah, Lustig-Yaeger, Jacob, Hu, Renyu, Kempton, Eliza, Arney, Giada, Line, Mike, Alam, Munazza, Moses, Julianne, Iro, Nicolas, Kreidberg, Laura, Blecic, Jasmina, Louden, Tom, Molliere, Paul, Stevenson, Kevin, Swain, Mark, Bott, Kimberly, Madhusudhan, Nikku, Krissansen-Totton, Joshua, Deming, Drake, Kitiashvili, Irina, Shkolnik, Evgenya, Rustamkulov, Zafar, Rogers, Leslie, and Close, Laird
Subjects: astro-ph.EP
Abstract: We are now on a clear trajectory for improvements in exoplanet observationsthat will revolutionize our ability to characterize their atmosphericstructure, composition, and circulation, from gas giants to rocky planets.However, exoplanet atmospheric models capable of interpreting the upcomingobservations are often limited by insufficiencies in the laboratory andtheoretical data that serve as critical inputs to atmospheric physical andchemical tools. Here we provide an up-to-date and condensed description ofareas where laboratory and/or ab initio investigations could fill critical gapsin our ability to model exoplanet atmospheric opacities, clouds, and chemistry,building off a larger 2016 white paper, and endorsed by the NAS ExoplanetScience Strategy report. Now is the ideal time for progress in these areas, butthis progress requires better access to, understanding of, and training in theproduction of spectroscopic data as well as a better insight into chemicalreaction kinetics both thermal and radiation-induced at a broad range oftemperatures. Given that most published efforts have emphasized relativelyEarth-like conditions, we can expect significant and enlightening discoveriesas emphasis moves to the exotic atmospheres of exoplanets.
Published: 2019

10. Polyaromatic disordered carbon grains as carriers of the UV bump: FUV to mid-infrared spectroscopy of laboratory analogs

Author: Gavilan, Lisseth, Le, Kim Cuong, Pino, Thomas, Alata, Ivan, Giuliani, Alexandre, and Dartois, Emmanuel
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: A multiwavelength study of laboratory carbons with varying degrees of hydrogenation and sp$^2$ hybridization is required to characterize the structure of the carbonaceous carriers of interstellar and circumstellar extinction. Analogs to carbonaceous interstellar dust encountered in various phases of the interstellar medium have been prepared in the laboratory. Thin films have been measured in transmission in the vacuum ultraviolet (VUV; 120 - 210 nm) within the atmospheric pressure experiment (APEX) chamber of the DISCO beam line at the SOLEIL synchrotron radiation facility. Spectra of these films were further measured through the UV-Vis (210 nm - 1 $\mu$m) and in the mid-infrared (3 - 15 $\mu$m). Tauc optical gaps, E$_g$, are derived from the visible spectra. The major spectral features are fitted through the VUV to the mid infrared to obtain positions, full-widths at half maximum (FWHM), and integrated intensities. These are plotted against the position of the $\pi$-$\pi^*$ electronic transitions peak. Unidentified or overlapping features in the UV are identified by correlations with complementary infrared data. A correlation between the optical gap and position of the $\pi$-$\pi^*$ electronic transitions peak is found. The latter is also correlated to the position of the sp$^3$ carbon defect band at ~8 $\mu$m, the aromatic C=C stretching mode position at ~6 $\mu$m, and the H/C ratio. Our study suggests that carriers of the interstellar UV bump should exhibit infrared bands akin to the A/B classes of the aromatic infrared bands, while the circumstellar bump carriers should exhibit bands corresponding to the B/C classes., Comment: 20 pages, 101 figures. Accepted for publication in Astronomy & Astrophysics (24 July 2017)
Published: 2017
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11. X-ray induced deuterium enrichment on N-rich organics in protoplanetary disks: an experimental investigation using synchrotron light

Author: Gavilan, Lisseth, Remusat, Laurent, Roskosz, Mathieu, Popescu, Horia, Jaouen, Nicolas, Sandt, Christophe, Jager, Cornelia, Henning, Thomas, Simionovici, Alexandre, Lemaire, Jean Louis, Mangin, Denis, and Carrasco, Nathalie
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The deuterium enrichment of organics in the interstellar medium, protoplanetary disks and meteorites has been proposed to be the result of ionizing radiation. The goal of this study is to quantify the effects of soft X-rays (0.1 - 2 keV), a component of stellar radiation fields illuminating protoplanetary disks, on the refractory organics present in the disks. We prepared tholins, nitrogen-rich complex organics, via plasma deposition and used synchrotron radiation to simulate X-ray fluences in protoplanetary disks. Controlled irradiation experiments at 0.5 and 1.3 keV were performed at the SEXTANTS beam line of the SOLEIL synchrotron, and were followed by ex-situ infrared, Raman and isotopic diagnostics. Infrared spectroscopy revealed the loss of singly-bonded groups (N-H, C-H and R-N$\equiv$C) and the formation of sp$^3$ carbon defects. Raman analysis revealed the introduction of defects and structural amorphization. Finally, tholins were measured via secondary ion mass spectrometry (SIMS), revealing that significant D-enrichment is induced by X-ray irradiation. Our results are compared to previous experimental studies involving the thermal degradation and electron irradiation of organics. The penetration depth of soft X-rays in $\mu$m-sized tholins leads to volume rather than surface modifications: lower energy X-rays (0.5 keV) induce a larger D-enrichment than 1.3 keV X-rays, reaching a plateau for doses larger than 5 $\times$ 10$^{27}$ eV cm$^{-3}$. Our work provides experimental evidence of a new non-thermal pathway to deuterium fractionation of organic matter., Comment: 14 pages, 23 figures. Accepted for publication in ApJ
Published: 2017
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12. 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

13. Expanding Heliophysics to Engage in Interdisciplinary Star-Planet Interactions Studies

Author: Garcia-Sage, Katherine, primary, Farrish, Alison O., additional, Airapetian, Vladimir S., additional, Cohen, Ofer, additional, Domagal-Goldman, Shawn, additional, Dong, Chuanfei, additional, Gronoff, Guillaume, additional, Halford, Alexa, additional, Mandell, Avi, additional, Sciola, Anthony, additional, Toffoletto, Frank, additional, Vievering, Juliana, additional, Acharya, Anshuman, additional, Adams, Danica, additional, Ahmed, Md Redyan, additional, Alexander, David, additional, Bali, Komal, additional, Barclay, Thomas, additional, Bott, Kimberly, additional, Chamberlin, Phillip, additional, Chen, Thomas Y., additional, Chen, Li-Jen, additional, Chirakkil, Krishnaprasad, additional, Curry, Shannon, additional, Danchi, William C., additional, Derr, Jason, additional, Dewey, Ryan, additional, DiBraccio, Gina, additional, Drake, Jeremy, additional, Egert, Austin, additional, Gavilan, Lisseth, additional, Gennaro, D’Angelo, additional, Holt, Timothy Richard, additional, Howaida, Parvin, additional, Hu, Junxiang, additional, Hughes, Andrea, additional, Jin, Meng, additional, Kalra, Archit, additional, Kane, Stephen, additional, Kohler, Erika, additional, Lazio, Joseph, additional, Lee, Yuni, additional, Lingam, Manasvi, additional, Luhmann, Janet, additional, Lyra, Wladimir, additional, Mandt, Kathleen E., additional, Mayyasi, Majd, additional, Meadows, Victoria, additional, Meziane, Karim, additional, Millot, Marius, additional, Molaverdikhani, Karan, additional, Pawlowski, David, additional, Quintana, Elisa, additional, Rau, Gioia, additional, Redfield, Seth, additional, Romanelli, Norberto, additional, Schlecker, Martin, additional, Schwieterman, Edward, additional, Segura, Antigona, additional, Stassun, Keivan, additional, Turner, Neal, additional, Wang, Liang, additional, and Youngblood, Allison, additional
Published: 2023
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14. 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

15. The evolution of Titan’s high-altitude aerosols under ultraviolet irradiation

Author: Carrasco, Nathalie, Tigrine, Sarah, Gavilan, Lisseth, Nahon, Laurent, and Gudipati, Murthy S.
Published: 2018
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16. Photochemical Hazes Can Trace the C/O Ratio in Exoplanet Atmospheres

Author: Corrales, Lía, primary, Gavilan, Lisseth, additional, Teal, D. J., additional, and Kempton, Eliza M.-R., additional
Published: 2023
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17. Laboratory Astrophysics Studies of the Evolution of Organic Matter with the COSmIC Facility.

Author: Salama, Farid, Sciamma-O'Brien, Ella, Bejaoui, Salma, Gavilan, Lisseth, and Dubois, David
Subjects: Astrophysics
Abstract: Understanding the origin of organic matter in astrophysical environments ranging from circumstellar (CS) outflows to diffuse and dense interstellar (IS) clouds to protoplanetary disks and planetary bodies has become a central objective in astrophysics. Experimental facilities dedicated to the formation and characterization of laboratory analogs generated under conditions relevant to the targeted environments have been developed in the past recent years. Recent advances achieved in laboratory astrophysics using COSmIC’s laboratory data in synergy with observational data will be presented. These results include the use of laboratory spectra to search for IS organic molecules and ions in astronomical spectra, the formation of laboratory analogs of CS and IS dust grains and planetary atmospheres aerosols from molecular precursors.
Published: 2019

18. Laboratory Astrophysics at NASA Ames: Recent Results and Advances

Author: Salama, Farid, Sciamma-O'brien, Ella, Bejaoui, Salma, Gavilan, Lisseth, and Dubois, David
Subjects: Astrophysics
Abstract: The Cosmic SImulation Chamber (COSmIC) facility was developed at NASA Ames to study, in the laboratory, neutral and ionized molecules and nanoparticles under the low temperature and high vacuum conditions representative of interstellar, circumstellar and planetary environments. COSmIC is composed of a Pulsed Discharge Nozzle expansion that generates a plasma in a free supersonic jet expansion coupled to highsensitivity, complementary in situ diagnostic tools, used for the detection and characterization of the species present in the expansion: a Cavity Ring Down Spectroscopy and fluorescence spectroscopy systems operating in the UV-Visible range, and a Reflectron Time-Of-Flight Mass Spectrometer (ReTOF-MS). We will present recent advances that were achieved in laboratory astrophysics using COSmIC. These include advances in the domain of the diffuse interstellar bands (DIBs) and in the formation of dust grains and aerosols from their gas-phase molecular precursors in environments as varied as circumstellar outflows and planetary atmospheres. An extension of the spectral response of the facility into the infrared (IR) range is in progress with the addition of a high-resolution near-IR to mid-IR CRDS system that will allow to further investigate cosmic molecules and grains with COSmIC. Acquisition of laser induced fluorescence spectra of cosmic molecule analogs and the laser induced incandescence spectra of cosmic grain analogs are also planned. Preliminary results in these fronts will presented and the implications of the on-going studies for astronomy will be addressed.
Published: 2019

19. Raman Spectroscopic Study of Pyrene in Cosmic Dust Analogues: Evolution from the Gas to the Solid Phase

Author: Gavilan, Lisseth, primary, Ricketts, Claire L., additional, Bejaoui, Salma, additional, Ricca, Alessandra, additional, Boersma, Christiaan, additional, Salama, Farid, additional, and Mattioda, Andrew L., additional
Published: 2022
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20. 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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21. Simultaneous Bright- and Dark-Field X-ray Microscopy at X-ray Free Electron Lasers

Author: Dresselhaus-Marais, Leora E., Kozioziemski, Bernard, Holstad, Theodor S., Ræder, Trygve Magnus, Seaberg, Matthew, Nam, Daewoong, Kim, Sangsoo, Breckling, Sean, Chollet, Matthieu, Cook, Philip K., Folsom, Eric, Galtier, Eric, Gavilan, Lisseth, Gonzalez, Arnulfo, Gorhover, Tais, Guillet, Serge, Haldrup, Kristoffer, Howard, Marylesa, Katagiri, Kento, Kim, Seonghan, Kim, Sunam, Kim, Sungwon, Kim, Hyunjung, Knudsen, Erik Bergback, Kuschel, Stephan, Lee, Hae-Ja, Lin, Chuanlong, McWilliams, R. Stewart, Nagler, Bob, Ozaki, Norimasa, Pal, Dayeeta, Pedro, Ricardo Pablo, Nielsen, Martin Meedom, Saunders, Alison M., Schoofs, Frank, Sekine, Toshimori, Simons, Hugh, van Driel, Tim, Wang, Bihan, Yang, Wenge, Yildirim, Can, Poulsen, Henning Friis, and Eggert, Jon H.
Subjects: Condensed Matter - Materials Science, Materials Science (cond-mat.mtrl-sci), FOS: Physical sciences
Abstract: The structures, strain fields, and defect distributions in solid materials underlie the mechanical and physical properties across numerous applications. Many modern microstructural microscopy tools characterize crystal grains, domains and defects required to map lattice distortions or deformation, but are limited to studies of the (near) surface. Generally speaking, such tools cannot probe the structural dynamics in a way that is representative of bulk behavior. Synchrotron X-ray diffraction based imaging has long mapped the deeply embedded structural elements, and with enhanced resolution, Dark Field X-ray Microscopy (DFXM) can now map those features with the requisite nm-resolution. However, these techniques still suffer from the required integration times due to limitations from the source and optics. This work extends DFXM to X-ray free electron lasers, showing how the $10^{12}$ photons per pulse available at these sources offer structural characterization down to 100 fs resolution (orders of magnitude faster than current synchrotron images). We introduce the XFEL DFXM setup with simultaneous bright field microscopy to probe density changes within the same volume. This work presents a comprehensive guide to the multi-modal ultrafast high-resolution X-ray microscope that we constructed and tested at two XFELs, and shows initial data demonstrating two timing strategies to study associated reversible or irreversible lattice dynamics.
Published: 2022
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22. A Laboratory-driven Multiscale Investigation of X-Ray Induced Mass Loss and Photochemical Evolution in Cosmic Carbon and Silicate Dust

Author: Gavilan, Lisseth, primary, Ho, Phay J., additional, Gorti, Uma, additional, Ogasawara, Hirohito, additional, Jäger, Cornelia, additional, and Salama, Farid, additional
Published: 2022
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23. ANUBIS - A Probe-Class UVO Space Observatory

Author: Scowen, Paul, Morse, Jon, Ardila, David, Balasubramanian, Bala, Bally, John, Devereux, Nick, Dyster, John, Figer, Don, Finkelstein, Steven, France, Kevin, Gavilan, Lisseth, Gorjian, Varoujan, Green, James, Grillmair, Carl, Hartigan, Patrick, Hendrix, Amanda, Howk, Chris, Hu, Renyu, Hutchings, John, Jansen, Rolf Kafka, Stella, Kasting, Jim, Larruquert, Juan Ignacio, Matthews, Gary, McCandliss, Stephan, McGrath, Melissa, Nikzad, Shouleh, Raymond, John, Sahai, Raghvendra, Siegmund, Ossy, Shkolnik, Evgenya, Stahl, Phil, Tripp, Todd, Turner, Neal, Willacy, Karen, Williams, Ben, Windhorst, Rogier, and Yanatsis, Dave
Abstract: 14 pags., 1 fig., 1 tab., We propose a next generation Probe-class UV-optical (UVO) observatory called ANUBIS that is capable of conducting wide-field imaging and far-ultraviolet (FUV) spectroscopic surveys to address critical topics in modern astrophysics and planetary science.
Published: 2019

24. The advent of soot nanostructure and soot evolution in a premixed low pressure ethylene flame by Raman, Far-UV to mid-IR spectroscopies and High Resolution Electron Transmission Microscopy (HRTEM)

Author: Le, Kim Cuong, Pre, Pascaline, Gavilan, Lisseth, Deldicque, Damien, Dartois, Emmanuel, Rouzaud, Jean Noël, PINO, THOMAS, Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Valorisation Energie-matière des Résidus et Traitement des Emissions (GEPEA-VERTE), Laboratoire de génie des procédés - environnement - agroalimentaire (GEPEA), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-Université de Nantes (UN)-Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN)-Institut Universitaire de Technologie Saint-Nazaire (IUT Saint-Nazaire), Université de Nantes (UN)-Institut Universitaire de Technologie - La Roche-sur-Yon (IUT La Roche-sur-Yon), Université de Nantes (UN)-Ecole Nationale Vétérinaire, Agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Université Bretagne Loire (UBL)-Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN)-Université de Nantes (UN)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Institut Universitaire de Technologie Saint-Nazaire (IUT Saint-Nazaire), Université de Nantes (UN)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-Ecole Nationale Vétérinaire, Agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Centre National de la Recherche Scientifique (CNRS)-Université Bretagne Loire (UBL)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Institut Universitaire de Technologie - La Roche-sur-Yon (IUT La Roche-sur-Yon), Université de Nantes (UN), Département Systèmes Energétiques et Environnement (IMT Atlantique - DSEE), IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de géologie de l'ENS (LGENS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDE.IE]Environmental Sciences/Environmental Engineering, [SPI.FLUID]Engineering Sciences [physics]/Reactive fluid environment, ComputingMilieux_MISCELLANEOUS, [SPI.MAT]Engineering Sciences [physics]/Materials
Abstract: International audience
Published: 2018

25. Evolution of soot nanostructure in premixed low pressure ethylene flame

Author: Le, Kim Cuong, Pre, Pascaline, Gavilan, Lisseth, Deldicque, Damien, Dartois, Emmanuel, Rouzaud, Jean Noël, PINO, THOMAS, Institut des Sciences Moléculaires d'Orsay (ISMO), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Valorisation Energie-matière des Résidus et Traitement des Emissions (GEPEA-VERTE), Laboratoire de génie des procédés - environnement - agroalimentaire (GEPEA), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS)-Ecole Polytechnique de l'Université de Nantes (EPUN), Université de Nantes (UN)-Université de Nantes (UN)-Institut Universitaire de Technologie - Nantes (IUT Nantes), Université de Nantes (UN)-Institut Universitaire de Technologie Saint-Nazaire (IUT Saint-Nazaire), Université de Nantes (UN)-Institut Universitaire de Technologie - La Roche-sur-Yon (IUT La Roche-sur-Yon), Université de Nantes (UN)-Ecole Nationale Vétérinaire, Agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Université Bretagne Loire (UBL)-Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Ecole Nationale Vétérinaire, Agroalimentaire et de l'alimentation Nantes-Atlantique (ONIRIS)-Université Bretagne Loire (UBL), Département Systèmes Energétiques et Environnement (IMT Atlantique - DSEE), IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de géologie de l'ENS (LGENS), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Département des Géosciences - ENS Paris, École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Institut d'astrophysique spatiale (IAS), and Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDE.IE]Environmental Sciences/Environmental Engineering, [SPI.FLUID]Engineering Sciences [physics]/Reactive fluid environment, [SPI.GPROC]Engineering Sciences [physics]/Chemical and Process Engineering, ComputingMilieux_MISCELLANEOUS, [SPI.MAT]Engineering Sciences [physics]/Materials
Abstract: International audience
Published: 2018

26. Optical indices of organic aerosols for oxidizing atmospheres of Earth-like exoplanets

Author: Gavilan, Lisseth, Broch, Laurent, Carrasco, Nathalie, Fleury, Benjamin, Vettier, Ludovic, BROCH, LAURENT, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Laboratoire de Chimie et Physique - Approche Multi-échelle des Milieux Complexes (LCP-A2MC), Université de Lorraine (UL), Jet Propulsion Laboratory (JPL), California Institute of Technology (CALTECH)-NASA, and Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)
Subjects: [SDU] Sciences of the Universe [physics], [SDU]Sciences of the Universe [physics], [CHIM] Chemical Sciences, [CHIM]Chemical Sciences
Abstract: International audience; Photochemical haze is likely produced in most planetary atmospheres. Optical indices are required to evaluate the haze contribution to the climate of aplanet. Unfortunately few experimental data exist and most of them have been measured with laboratory analogs of Titan’s haze, which can only be amodel scenario fortotally reduced atmospheres. In the present work we studythe optical indices in the UV-Vis range ofanalogs of planetary organic haze produced with CO2/CH4ratios varying between 1 and 4 in order to provide appropriate optical indices for a large range of Earth-like oxidizingatmospheres. Oxidized analogues are found as much as four times better absorbers in the UVthan the reduced ones.
Published: 2018

27. High-resolution study of oscillator strengths and predissociation rates for 13C18O

Author: Eidelsberg, Michèle, Lemaire, jean-Louis, Federman, Steven R., Heays, Alan N., Stark, Glenn, Lyons, James R., Gavilan, Lisseth, De Oliveira, Nelson, Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Toledo], University of Toledo, Leiden Observatory [Leiden], Universiteit Leiden, Department of Physics [Wellesley], Wellesley College, School of Earth and Space Exploration [Tempe] (SESE), Arizona State University [Tempe] (ASU), PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ligne DESIRS [Saint Aubin], Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), and Universiteit Leiden [Leiden]
Subjects: [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], spectroscopy, molecular data, TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, ultraviolet, ISM
Abstract: International audience; We carried out experiments at the SOLEIL synchrotron facility to acquire data for modelling CO photochemistry in the vacuum ultraviolet. We report oscillator strengths and predissociation rates for four vibrational bands associated with transitions from the v = 0 level of the X1 Σ+ ground state to the v = 0–3 vibrational levels of the core excited W1Π Rydberg state, and for three overlapping bands associated with the 4pπ, 5pπ, and 5pσ Rydberg states between 92.9 and 93.4 nm in 13C18O. These results complete those obtained in the same conditions for 12C16O, 13C16O, and 12C18O recently published by us, and extend the development of a comprehensive database of line positions, oscillator strengths, and linewidths of photodissociating transitions for CO isotopologues. Absorption spectra were recorded using the Vacuum UltraViolet Fourier Transform Spectrometer (VUV-FTS) installed on the Dichroïsme Et Spectroscopie par Interaction avec le Rayonnement Synchrotron (DESIRS) beamline at SOLEIL. The resolving power of the measurements, R = 300 000 to 400 000, allows the analysis of individual line strengths and widths within the bands. Gas column densities in the differentially pumped system were calibrated using the B-X (0–0) band at 115.1 nm in 13C18O.
Published: 2017

28. Organic Aerosols in Anoxic and Oxic Atmospheres of Earth-like Exoplanets: VUV-MIR Spectroscopy of CHON Tholins

Author: Gavilan, Lisseth, primary, Carrasco, Nathalie, additional, Hoffmann, Søren Vrønning, additional, Jones, Nykola C., additional, and Mason, Nigel J., additional
Published: 2018
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29. COMPLETE PHOTOABSORPTION LINELIST FOR CO AND ITS ISOTOPOLOGUES BETWEEN 101 AND 115 NM

Author: Heays, Alan, primary, de Oliveira, Nelson, additional, Ubachs, Wim, additional, Lyons, James, additional, Federman, Steven, additional, Stark, Glenn, additional, Gavilan, Lisseth, additional, Eidelsberg, Michele, additional, and Lemaire, Jean, additional
Published: 2018
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30. High-resolution spectroscopy of the A1Π(v′=0-10)−X1Σ+(v′′=0) bands in 13C18O: term values, ro-vibrational oscillator strengths and Hönl–London corrections

Author: Lemaire, Jean-Louis, Eidelsberg, Michèle, Heays, Alan, Gavilan, Lisseth, Federman, Steven, Stark, G., Lyons, James R., De Oliveira, Nelson, Joyeux, Denis, Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Toledo], University of Toledo, Wellesley College, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Ligne DESIRS [Saint Aubin], Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Universiteit Leiden [Leiden], and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; Our knowledge of astronomical environments containing CO depends on accurate molecular data to reproduce and interpret observations. The constant improvement in UV space instrumentation, both in sensitivity and resolution, requires increasingly detailed laboratory data. Following a long-term experimental campaign at the SOLEIL Synchrotron facility, we have acquired complete datasets on the CO isotopologues in the vacuum ultraviolet. Absorption spectra were recorded using the Fourier-transform spectrometer installed on the DESIRS beamline, providing a resolving power R > 106 in the 8–12 eV range. Such resolution allows the analysis of individual line positions and strengths in electronic transitions and the location of perturbations. We continue our previous work on A–X bands of 12C16O and 13C16O, reporting here measurements for the 13C18O isotopologue.
Published: 2016

31. High-resolution spectroscopy of the A1Π(v′=0-10)−X1Σ+(v′′=0) bands in 13C18O

Author: Lemaire, Jean-Louis, Eidelsberg, Michèle, Heays, Alan, Gavilan, Lisseth, Federman, Steven, Stark, Glenn, Lyons, James R., De Oliveira, Nelson, Joyeux, Denis, Institut des Sciences Moléculaires d'Orsay (ISMO), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Department of Physics and Astronomy [Toledo], University of Toledo, Wellesley College, ASU School of Earth and Space Exploration (SESE), Arizona State University [Tempe] (ASU), Synchrotron SOLEIL (SSOLEIL), Centre National de la Recherche Scientifique (CNRS), Cardon, Catherine, Universiteit Leiden, and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)
Subjects: [PHYS.PHYS.PHYS-AO-PH]Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph], TheoryofComputation_ANALYSISOFALGORITHMSANDPROBLEMCOMPLEXITY, [PHYS.PHYS.PHYS-AO-PH] Physics [physics]/Physics [physics]/Atmospheric and Oceanic Physics [physics.ao-ph]
Abstract: International audience; Ultraviolet spectrographs on space-borne astronomical facilities are used to study CO photochemistry primarily through observations of the A-X Fourth Positive Band System. Absorption from 12C16O, 13C16O, 12C18O, and 12C1712C16O. In our ongoing experiments on the DESIRS beam-line at the SOLEIL Synchrotron, we are acquiring the necessary data on oscillator strengths and term values for other isotopologues. Here we present our latest results involving A-X bands in 13C18O.
Published: 2016

32. Influence of traces elements in the organic chemistry of upper atmosphere of Titan

Author: Mathé, Christophe, Carrasco, Nathalie, Trainer, Melissa Grady, Gautier, Thomas, Gavilan, Lisseth, Dubois, David, Li, Xiang, Cardon, Catherine, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), NASA Goddard Space Flight Center (GSFC), Center for Space Sciences and Technology (CSST), University of Maryland [Baltimore County] (UMBC), University of Maryland System-University of Maryland System, and Universities Space Research Association (USRA)
Subjects: [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; In the upper atmosphere of Titan, complex chemistry leads to the formation of organic aerosols. Since the work of Khare et al. in 1984, several experiments investigated the formation of Titan aerosols, so called tholins, in the laboratory. It has been suggested that nitrogen-containing compounds may contribute significantly to the aerosols formation process. In this study, we focused on the influence of pyridine, the simplest nitrogenous aromatic hydro- carbon, on the chemistry of Titan's atmosphere and on aerosol formation.To assess the effect of pyridine on aerosol formation chemistry, we used two different experimental setups : a capaci- tively coupled radio-frequency (electronic impact), and a VUV Deuterium lamp (photochemistry) in a collaboration between LATMOS (Guyancourt) and NASA-GSFC (Greenbelt), respectively. Aerosols produced with both setups were first analyzed using a FTIR-ATR (Fourier Transform Infrared spectroscopy - Attenuated Total Reflection) with a spectral range of 4000-800 cm−1 to characterize their optical properties. Next the samples were analysed using a Bruker Autoflex Speed MALDI mass spectrometer with a m/z range up to 2000 Da in order to infer their composition.Infrared spectroscopy analysis showed that tholins produced with a nitrogen-methane gas mixture (95:5) and nitrogen- pyridine gas mixture (99:250ppm) present very similar spectra features. Tholins produced with a mixture of nitrogen- methane-pyridine (99:1:250ppm) do not present aliphatic CH2 or CH3 vibrational signatures. This could indicate a cyclic polymerization by a pyridine skeleton. Mass spectrometry is still in progress to confirm this.
Published: 2016

33. XUV complex refractive indices of aerosols in the atmospheres of Titan and the primitive Earth

Author: Gavilan, Lisseth, Carrasco, Nathalie, Neumann, Maciej, Esser, Norbert, Fleury, Benjamin, Dahoo, Pierre-Richard, Popescu, Horia, Jaouen, Nicolas, Cardon, Catherine, PLANETO - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Leibniz-Institut für Analytische Wissenschaften - ISAS - e.V., Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Synchrotron SOLEIL (SSOLEIL), and Centre National de la Recherche Scientifique (CNRS)
Subjects: [SDU.OCEAN]Sciences of the Universe [physics]/Ocean, Atmosphere, [SDU.OCEAN] Sciences of the Universe [physics]/Ocean, Atmosphere, [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP] Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP]
Abstract: International audience; The complex refractive indices of tholins, simulating aerosols in the atmosphere of Titan and the primitive earth, have been measured over a wide spectral range, including the soft X-ray, vacuum-ultraviolet (VUV), and UV-Visible. The soft X-ray and VUV spectral ranges are in particular relevant to radiative transfer models of solar irradiation of primitive atmospheres (Lammer et al. 2008) and may elucidate the (anti-)greenhouse potential of photochemical aerosols.Thin films were grown using the PAMPRE capacitively coupled plasma setup (Szopa et al. 2006; Carrasco et al. 2009). Gas mixtures consisting of CH4/N2 with 5:95 ratios were used to simulate Titan's atmospheric composition. For the primitive Earth, gas mixtures of N2/CO2/H2 and N2/CO2/CH4 were used as described in Fleury et al. (2014).State-of-the-art laboratory techniques were used to determine the refractive indices of such tholin films. These include VUV ellipsometry (performed in collaboration with the Metrology Light Source in Berlin) and synchrotron X-ray spectroscopy (performed at the SEXTANTS beamline of the SOLEIL synchrotron). While VUV spectroscopy reveals new electronic transitions due to plasmon resonances in tholins, X-ray spectra reveal the C and O absorption edges of these solids. The refractive indices are compared to results from Khare et al. (1984). Implications on the optical properties of these aerosol analogs on the radiative modeling of primitive atmospheres will be discussed.
Published: 2016

34. Organic Aerosols in the Presence of CO 2 in the Early Earth and Exoplanets: UV–Vis Refractive Indices of Oxidized Tholins

Author: Gavilan, Lisseth, primary, Broch, Laurent, additional, Carrasco, Nathalie, additional, Fleury, Benjamin, additional, and Vettier, Ludovic, additional
Published: 2017
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35. X-Ray-induced Deuterium Enrichment of N-rich Organics in Protoplanetary Disks: An Experimental Investigation Using Synchrotron Light

Author: Gavilan, Lisseth, primary, Remusat, Laurent, additional, Roskosz, Mathieu, additional, Popescu, Horia, additional, Jaouen, Nicolas, additional, Sandt, Christophe, additional, Jäger, Cornelia, additional, Henning, Thomas, additional, Simionovici, Alexandre, additional, Lemaire, Jean Louis, additional, Mangin, Denis, additional, and Carrasco, Nathalie, additional
Published: 2017
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36. High-Resolution Study of 13C16O A-X (v′=0-9) Bands Using the VUV-FTS at SOLEIL: Revised Term Values

Author: Gavilan, Lisseth, Lemaire, Jean Louis, Eidelsberg, Michele, Federman, Steven R., Stark, Glenn, Heays, Alan N., Fillion, Jean-Hugues, Lyons, James R., and de Oliveira, Nelson
Abstract: We present high-resolution absorption spectral measurements of the A 1Pi – X 1Sigma+ band system of 13C16O. These were recorded with the VUV Fourier transform spectrometer (VUV-FTS) installed on the DESIRS beamline at the SOLEIL synchrotron. This work includes revised term values that extend to higher J′ values than previous measurements for most v′ levels and lower J′ values for v′=0. We confirm previously observed perturbations of the rotational levels in greater detail and present evidence for new perturbations. The accuracy in the wavelength determination and term values is on average within 0.01 cm−1, improving upon previous measurements.
Published: 2024
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37. HIGH-RESOLUTION SPECTROSCOPY OF THE A1Π(v′=0-10)−X1Σ+(v′′=0) BANDS IN 13C18O

Author: Federman, Steven, primary, Joyeux, Denis, additional, de Oliveira, Nelson, additional, Lyons, James, additional, Stark, Glenn, additional, Gavilan, Lisseth, additional, Heays, Alan, additional, Eidelsberg, Michele, additional, and Lemaire, Jean, additional
Published: 2016
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38. UV Photolysis of Hydrogenated Amorphous Carbons of Astrophysical Interest

Author: Dartois, Emmanuel, primary, Jallat, Aurélie, additional, Alata, Ivan, additional, Gavilan, Lisseth, additional, Cruz-Diaz, Gustavo A., additional, Chabot, Marin, additional, Beroff, Karine, additional, and Muñoz Caro, Guillermo M., additional
Published: 2016
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39. The formation of molecular hydrogen on interstellar silicates : FROM EXPERIMENTS TO OBSERVATIONS

Author: Gavilan, Lisseth, Institut d'astrophysique spatiale (IAS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Sud - Paris 11 (UP11), Observatoire de Paris, Lemaire, Jean-Louis, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Barbet, Virginie
Subjects: astronomy, Cosmochimie, Molécules interstellaires, Hydrogène interstellaire, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract: The goal of this thesis is to understand the formation of molecular hydrogen in the interstellar medium (ISM) via laboratory experiments and astronomical observations. The experiments are performed with FORMOLISM, an ultra-high vacuum setup to study the formation of molecules in the ISM. We are interested in the energy disposal during the exhothermic recombination of two H atoms on a cryogenically cooled surface (< 10 K). Resonance Enhanced Multi-Photon Ionization ( REMPI 2 + 1) spectroscopy is used to probe the population of rovibrational levels in the ground electronic state of molecular hydrogen after formation. We have tested different surfaces of astrophysical relevance : amorphous and crystalline silicates, porous amorphous solid water, and a bare silicate pre-dosed with hydrogen molecules. We have confirmed the formation enhancement of molecular hydrogen on a surface pre-dosed with molecules and quantified D₂formation as a non-thermal desorption mechanism. We have also measured the ortho-to-para ratio of newly formed molecular hydrogen on p-ASW, finding that it corresponds to the value expected at statistical equilibrium at high temperature. Silicate analog surfaces (forsterite and fayalite) have been fabricated to test the influence of their morphology and chemical composition on hydrogen formation. We have found that newly formed molecular hydrogen leaves rotationally cooler (with respect to the molecular beam rotational temperature) from crystalline surfaces, and that it is unaffected when it scatters from amorphous surfaces. We have also detected nuclear spin conversion of molecular hydrogen absorbed on bare silicates. Observational predictions from these experiments are tested using long slit near infrared spectroscopy available at the VLT and Keck telescopes. Planetary nebulae with H₂ and X-ray emission were chosen as ideal targets. H₂transitions have been detected throughout our targets. The intensity distribution of these transitions will be compared to models of formation pumping spectra. In addition, part of this thesis addresses the VUV high-resolution spectroscopy of CO and its isotopologues, using the Fourier Transform Spectrometer at the SOLEIL synchroton. This complements the work on hydrogen in the wider context of the astrochemistry of small molecules., L'objectif de cette thèse est de comprendre la formation de l'hydrogène moléculaire dans le milieu interstellaire (MIS) via des expériences de laboratoire et des observations astronomiques. Les expériences ont été réalisées avec FORMOLISM, un montage fonctionnant dans l'ultra-vide pour étudier la formation de molécules dans le MIS. On s'intéresse à la distribution en énergie de molécules d'hydrogène formées sur une surface refroidie par cryogénie (< 10 K). La technique de Resonance Enhanced Multi-Photon Ionization (REMPI 2 + 1) est utilisée pour sonder la population des niveaux rovibrationnels de l'état électronique fondamental de l'hydrogène moléculaire. Nous avons examiné différentes surfaces d'intérêt astrophysique : des silicates amorphes et cristallins, et de la glace d'eau solide amorphe poreuse (p-ASW). Nous avons confirmé l'augmentation du taux de formation de l'hydrogène moléculaire sur une surface recouverte au préalable des molécules d'hydrogène et nous avons quantifié la formation D₂en tant que mécanisme de désorption non-thermique. Nous avons mesuré le rapport ortho-para de l'hydrogène moléculaire nouvellement formée sur la surface de p-ASW, qui correspond à la valeur attendue à l'équilibre statistique à haute température (> 100 K). Nous avons fabriqué au laboratoire de nouvelles surfaces de silicates (forstérite et fayalite) pour examiner l'impact de leur morphologie et de leur composition chimique sur la formation de l'hydrogène moléculaire. On a observé l'abaissement de la température de rotation des molécules d'hydrogène formées (par rapport à la température de rotation du jet moléculaire) émergeant de surfaces cristallines. Nous avons également étudié la conversion de spin nucléaire des molécules d'hydrogène absorbées sur une surface de sillicate. Les prédictions observationnelles qui on été déduites de ces expériences ont été testées par spectroscopie à longue fente dans l'infrarouge proche disponible au VLT et au Keck. Des nébuleuses planétaires présentant simultanément des émissions de H₂ont été détectées sur certains de nos objets. La distribution d'intensité de ces raies est comparée à des modèles théoriques de formation H₂dans l'espace. Une partie de cette thèse traite également de la spectroscopie VUV à haute résolution de CO et de ses isotopes, en utilisant le spectromètre à transformée de Fourier disponible au synchroton SOLEIL. Cela complète le travail sur l'hydrogène dans le contexte plus large de l'astrochimie de petites molécules.
Published: 2013

40. OSCILLATOR STRENGTHS AND PREDISSOCIATION RATES FOR W−X BANDS AND THE 4P5P COMPLEX IN 13C18O

Author: Federman, Steven, primary, Joyeux, Denis, additional, de Oliveira, Nelson, additional, Smith, Peter, additional, Lyons, James, additional, Gavilan, Lisseth, additional, Heays, Alan, additional, Stark, Glenn, additional, Lemaire, Jean, additional, and Eidelsberg, Michele, additional
Published: 2015
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41. UV Photolysis of Hydrogenated Amorphous Carbons of Astrophysical Interest.

Author: Dartois, Emmanuel, Jallat, Aurélie, Alata, Ivan, Gavilan, Lisseth, Cruz-Diaz, Gustavo A., Chabot, Marin, Beroff, Karine, and Muñoz Caro, Guillermo M.
Subjects: GAS phase reactions, AMORPHOUS carbon, PHOTOLYSIS (Chemistry), HYDROCARBONS, GRAIN
Abstract: In the gas phase, most of the ionized or neutral molecules detected in the interstellar and circumstellar media contain at least one carbon atom. Carbon chemistry plays thus a dominant role in the understanding of the structure and evolution of the interstellar medium (ISM). One particular zone of interest to observe small carbonaceous radicals and molecules, are the sharp molecular clouds edges exposed to energetic photons. These photon-dominated regions are rich in these hydrocarbons (like CCH, c-C3H2, C4H), and provide tests for the chemistry models in the diffuse to molecular transition. The pure gas phase models generally fail in reproducing the abundance of many of the observed species, and several authors suggest such abundances may arise from the products of the VUV photodissociation of carbonaceous grains or PAHs. Hydrogenated amorphous carbons (a-C:H or HAC), abundantly observed in the ISM, could also be at the origin of many of these small carbonaceous radicals. Experimentally, this work investigates the production and release of hydrocarbons from the VUV photolysis of a-C:H interstellar analogues under ultra-high vacuum. The experimental results are applied to a Photon Dominated Region model to constrain the impact of this release on the observed gas phase species. [ABSTRACT FROM AUTHOR]
Published: 2017
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42. OSCILLATOR STRENGTHS AND PREDISSOCIATION RATES FOR W−X BANDS AND THE 4P5P COMPLEX IN 13C16O AND 12C18O

Author: Federman, Steven, primary, Joyeux, Denis, additional, de Oliveira, Nelson, additional, Smith, Peter, additional, Lyons, James, additional, Gavilan, Lisseth, additional, Heays, Alan, additional, Stark, Glenn, additional, Lemaire, Jean, additional, and Eidelsberg, Michele, additional
Published: 2014
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43. STUDY OF THE PERTURBED W 1Π(v=1) STATE OF CO IN FIVE ISOTOPOLOGUES

Author: Heays, Alan, primary, Joyeux, Denis, additional, de Oliveira, Nelson, additional, Gavilan, Lisseth, additional, Smith, Peter, additional, Lyons, James, additional, Federman, Steven, additional, Stark, Glenn, additional, Lemaire, Jean, additional, and Eidelsberg, Michele, additional
Published: 2014
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44. High-Resolution Study of 13C16O A–X(v′ = 0–9) Bands Using the VUV-FTS at SOLEIL: Revised Term Values

Author: Gavilan, Lisseth, primary, Lemaire, Jean Louis, additional, Eidelsberg, Michèle, additional, Federman, S. R., additional, Stark, Glenn, additional, Heays, Alan N., additional, Fillion, Jean-Hugues, additional, Lyons, James R., additional, and de Oliveira, Nelson, additional
Published: 2013
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45. Experiments on molecular hydrogen formation on cold ISM dust

Author: Gavilan, Lisseth, primary, Lemaire, Jean Louis, additional, and Vidali, Gianfranco, additional
Published: 2012
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46. 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

47. 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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