1,112 results on '"ABERGEL, A."'
Search Results
2. MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
- Author
-
Sierra L. Grant, Ewine F. van Dishoeck, Benoît Tabone, Danny Gasman, Thomas Henning, Inga Kamp, Manuel Güdel, Pierre-Olivier Lagage, Giulio Bettoni, Giulia Perotti, Valentin Christiaens, Matthias Samland, Aditya M. Arabhavi, Ioannis Argyriou, Alain Abergel, Olivier Absil, David Barrado, Anthony Boccaletti, Jeroen Bouwman, Alessio Caratti o Garatti, Vincent Geers, Adrian M. Glauser, Rodrigo Guadarrama, Hyerin Jang, Jayatee Kanwar, Fred Lahuis, Maria Morales-Calderón, Michael Mueller, Cyrine Nehmé, Göran Olofsson, Eric Pantin, Nicole Pawellek, Tom P. Ray, Donna Rodgers-Lee, Silvia Scheithauer, Jürgen Schreiber, Kamber Schwarz, Milou Temmink, Bart Vandenbussche, Marissa Vlasblom, L. B. F. M. Waters, Gillian Wright, Luis Colina, Thomas R. Greve, Kay Justannont, and Göran Östlin
- Subjects
Protoplanetary disks ,Planet formation ,Astrophysics ,QB460-466 - Abstract
We present JWST-MIRI Medium Resolution Spectrometer (MRS) spectra of the protoplanetary disk around the low-mass T Tauri star GW Lup from the MIRI mid-INfrared Disk Survey Guaranteed Time Observations program. Emission from ^12 CO _2 , ^13 CO _2 , H _2 O, HCN, C _2 H _2 , and OH is identified with ^13 CO _2 being detected for the first time in a protoplanetary disk. We characterize the chemical and physical conditions in the inner few astronomical units of the GW Lup disk using these molecules as probes. The spectral resolution of JWST-MIRI MRS paired with high signal-to-noise data is essential to identify these species and determine their column densities and temperatures. The Q branches of these molecules, including those of hot bands, are particularly sensitive to temperature and column density. We find that the ^12 CO _2 emission in the GW Lup disk is coming from optically thick emission at a temperature of ∼400 K. ^13 CO _2 is optically thinner and based on a lower temperature of ∼325 K, and thus may be tracing deeper into the disk and/or a larger emitting radius than ^12 CO _2 . The derived ${N}_{{\mathrm{CO}}_{2}}$ / ${N}_{{{\rm{H}}}_{2}{\rm{O}}}$ ratio is orders of magnitude higher than previously derived for GW Lup and other targets based on Spitzer-InfraRed-Spectrograph data. This high column density ratio may be due to an inner cavity with a radius in between the H _2 O and CO _2 snowlines and/or an overall lower disk temperature. This paper demonstrates the unique ability of JWST to probe inner disk structures and chemistry through weak, previously unseen molecular features.
- Published
- 2023
- Full Text
- View/download PDF
3. 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
4. MINDS. The Detection of 13CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk
- Author
-
Grant, Sierra L., van Dishoeck, Ewine F., Tabone, Benoît, Gasman, Danny, Henning, Thomas, Kamp, Inga, Güdel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M., Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, Caratti o Garatti, Alessio, and Glauser, Adrian Michael
- Abstract
We present JWST-MIRI Medium Resolution Spectrometer (MRS) spectra of the protoplanetary disk around the low-mass T Tauri star GW Lup from the MIRI mid-INfrared Disk Survey Guaranteed Time Observations program. Emission from 12CO213CO2, H2O, HCN, C2H2, and OH is identified with 13CO2 being detected for the first time in a protoplanetary disk. We characterize the chemical and physical conditions in the inner few astronomical units of the GW Lup disk using these molecules as probes. The spectral resolution of JWST-MIRI MRS paired with high signal-to-noise data is essential to identify these species and determine their column densities and temperatures. The Q branches of these molecules, including those of hot bands, are particularly sensitive to temperature and column density. We find that the 12CO2 emission in the GW Lup disk is coming from optically thick emission at a temperature of ∼400 K. 13CO2 is optically thinner and based on a lower temperature of ∼325 K, and thus may be tracing deeper into the disk and/or a larger emitting radius than 12CO2. The derived N CO 2 / N H 2 O ratio is orders of magnitude higher than previously derived for GW Lup and other targets based on Spitzer-InfraRed-Spectrograph data. This high column density ratio may be due to an inner cavity with a radius in between the H2O and CO2 snowlines and/or an overall lower disk temperature. This paper demonstrates the unique ability of JWST to probe inner disk structures and chemistry through weak, previously unseen molecular features., The Astrophysical Journal Letters, 947 (1), ISSN:1967-2014, ISSN:2041-8213
- Published
- 2023
5. 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
- Full Text
- View/download PDF
6. MINDS. The Detection of 13 CO2 with JWST-MIRI Indicates Abundant CO2 in a Protoplanetary Disk.
- Author
-
Grant, Sierra L., van Dishoeck, Ewine F., Tabone, Benoît, Gasman, Danny, Henning, Thomas, Kamp, Inga, Güdel, Manuel, Lagage, Pierre-Olivier, Bettoni, Giulio, Perotti, Giulia, Christiaens, Valentin, Samland, Matthias, Arabhavi, Aditya M., Argyriou, Ioannis, Abergel, Alain, Absil, Olivier, Barrado, David, Boccaletti, Anthony, Bouwman, Jeroen, and o Garatti, Alessio Caratti
- Published
- 2023
- Full Text
- View/download PDF
7. Interacting Dirac materials
- Author
-
Banerjee, Saikat, Abergel, David, Ågren, Hans, Aeppli, G., Balatsky, Alexander V., Banerjee, Saikat, Abergel, David, Ågren, Hans, Aeppli, G., and Balatsky, Alexander V.
- Abstract
We investigate the extent to which the class of Dirac materials in two-dimensions provides general statements about the behavior of both fermionic and bosonic Dirac quasiparticles in the interacting regime. For both quasiparticle types, we find common features for the interaction induced renormalization of the conical Dirac spectrum. We perform the perturbative renormalization analysis and compute the self-energy for both quasiparticle types with different interactions and collate previous results from the literature whenever necessary. Guided by the systematic presentation of our results in table1, we conclude that long-range interactions generically lead to an increase of the slope of the single-particle Dirac cone, whereas short-range interactions lead to a decrease. The quasiparticle statistics does not qualitatively impact the self-energy correction for long-range repulsion but does affect the behavior of short-range coupled systems, giving rise to different thermal power-law contributions. The possibility of a universal description of the Dirac materials based on these features is also mentioned., QC 20200826
- Published
- 2020
- Full Text
- View/download PDF
8. Interacting Dirac materials
- Author
-
Banerjee, S, primary, Abergel, D S L, additional, Ågren, H, additional, Aeppli, G, additional, and Balatsky, A V, additional
- Published
- 2020
- Full Text
- View/download PDF
9. The role of spin–orbit coupling in topologically protected interface states in Dirac materials
- Author
-
D S L Abergel, Jonathan M Edge, and Alexander V Balatsky
- Subjects
Dirac materials ,interface states ,persistent currents ,topological protection ,73.20.-r ,73.40.-c ,Science ,Physics ,QC1-999 - Abstract
We highlight the fact that two-dimensional (2D) materials with Dirac-like low energy band structures and spin–orbit coupling (SOC) will produce linearly dispersing topologically protected Jackiw–Rebbi modes at interfaces where the Dirac mass changes sign. These modes may support persistent spin or valley currents parallel to the interface, and the exact arrangement of such topologically protected currents depends crucially on the details of the SOC in the material. As examples, we discuss buckled 2D hexagonal lattices such as silicene or germanene, and transition metal dichalcogenides such as ${\rm Mo}{{{\rm S}}_{2}}$ .
- Published
- 2014
- Full Text
- View/download PDF
10. Infrared absorption by graphene–hBN heterostructures
- Author
-
D S L Abergel, J R Wallbank, Xi Chen, M Mucha-Kruczyński, and Vladimir I Fal'ko
- Subjects
Science ,Physics ,QC1-999 - Abstract
We propose a theory of optical absorption in monolayer graphene–hexagonal boron nitride (hBN) heterostructures. In highly oriented heterostructures, the hBN underlay produces a long-range moiré superlattice potential for the graphene electrons which modifies the selection rules for absorption of incoming photons in the infrared to visible frequency range. The details of the absorption spectrum modification depend on the relative strength of the various symmetry-allowed couplings between the graphene electrons and the hBN, and the resulting nature of the reconstructed band structure.
- Published
- 2013
- Full Text
- View/download PDF
11. Robustness of topologically protected transport in graphene–boron nitride lateral heterostructures
- Author
-
Abergel, D S L, primary
- Published
- 2016
- Full Text
- View/download PDF
12. Robustness of topologically protected transport in graphene–boron nitride lateral heterostructures
- Author
-
David Abergel
- Subjects
Materials science ,FOS: Physical sciences ,Hexagonal boron nitride ,02 engineering and technology ,01 natural sciences ,law.invention ,chemistry.chemical_compound ,law ,Lattice (order) ,Mesoscale and Nanoscale Physics (cond-mat.mes-hall) ,0103 physical sciences ,Ribbon ,General Materials Science ,010306 general physics ,Condensed Matter - Mesoscale and Nanoscale Physics ,Condensed matter physics ,Graphene ,Heterojunction ,021001 nanoscience & nanotechnology ,Condensed Matter Physics ,3. Good health ,Zigzag ,chemistry ,Boron nitride ,0210 nano-technology ,Graphene nanoribbons - Abstract
Previously, graphene nanoribbons set in lateral heterostructures with hexagonal boron nitride were predicted to support topologically protected states at low energy. We investigate how robust the transport properties of these states are against lattice disorder. We find that forms of disorder that do not couple the two valleys of the zigzag graphene nanoribbon do not impact the transport properties at low bias, indicating that these lateral heterostructures are very promising candidates for chip-scale conducting interconnects. Forms of disorder that do couple the two valleys, such as vacancies in the graphene ribbon, or substantial inclusions of armchair edges at the graphene-hexagonal boron nitride interface will negatively affect the transport. However, these forms of disorder are not commonly seen in current experiments., Main text is eight pages with four figures, RevTeX. Supplementary material included
- Published
- 2016
13. Two-photon absorption in gapped bilayer graphene with a tunable chemical potential
- Author
-
Brinkley, M K, primary, Abergel, D S L, additional, and Clader, B D, additional
- Published
- 2016
- Full Text
- View/download PDF
14. The role of spin–orbit coupling in topologically protected interface states in Dirac materials
- Author
-
Abergel, D S L, primary, Edge, Jonathan M, additional, and Balatsky, Alexander V, additional
- Published
- 2014
- Full Text
- View/download PDF
15. Infrared absorption by graphene–hBN heterostructures
- Author
-
Abergel, D S L, primary, Wallbank, J R, additional, Chen, Xi, additional, Mucha-Kruczyński, M, additional, and Fal'ko, Vladimir I, additional
- Published
- 2013
- Full Text
- View/download PDF
16. On spectral properties of bilayer graphene: the effect of an SiC substrate and infrared magneto-spectroscopy.
- Author
-
Mucha-Kruczyński, M, Abergel, D S L, McCann, E, and Fal’ko, V I
- Published
- 2009
- Full Text
- View/download PDF
17. A variational Bayesian approach for unsupervised super-resolution using mixture models of point and smooth sources applied to astrophysical map-making
- Author
-
Ayasso, Hacheme, primary, Rodet, Thomas, additional, and Abergel, Alain, additional
- Published
- 2012
- Full Text
- View/download PDF
18. 50 nm thick AlN film-based piezoelectric cantilevers for gravimetric detection
- Author
-
Ivaldi, P, primary, Abergel, J, additional, Matheny, M H, additional, Villanueva, L G, additional, Karabalin, R B, additional, Roukes, M L, additional, Andreucci, P, additional, Hentz, S, additional, and Defaÿ, E, additional
- Published
- 2011
- Full Text
- View/download PDF
19. Irradiated bilayer graphene
- Author
-
Abergel, D S L, primary and Chakraborty, Tapash, additional
- Published
- 2010
- Full Text
- View/download PDF
20. Hi-GAL: The Herschel Infrared Galactic Plane Survey
- Author
-
Molinari, S., primary, Swinyard, B., additional, Bally, J., additional, Barlow, M., additional, Bernard, J.-P., additional, Martin, P., additional, Moore, T., additional, Noriega-Crespo, A., additional, Plume, R., additional, Testi, L., additional, Zavagno, A., additional, Abergel, A., additional, Ali, B., additional, André, P., additional, Baluteau, J.-P., additional, Benedettini, M., additional, Berné, O., additional, Billot, N. P., additional, Blommaert, J., additional, Bontemps, S., additional, Boulanger, F., additional, Brand, J., additional, Brunt, C., additional, Burton, M., additional, Campeggio, L., additional, Carey, S., additional, Caselli, P., additional, Cesaroni, R., additional, Cernicharo, J., additional, Chakrabarti, S., additional, Chrysostomou, A., additional, Codella, C., additional, Cohen, M., additional, Compiegne, M., additional, Davis, C. J., additional, de Bernardis, P., additional, de Gasperis, G., additional, Di Francesco, J., additional, di Giorgio, A. M., additional, Elia, D., additional, Faustini, F., additional, Fischera, J. F., additional, Fukui, Y., additional, Fuller, G. A., additional, Ganga, K., additional, Garcia-Lario, P., additional, Giard, M., additional, Giardino, G., additional, Glenn, J:, additional, Goldsmith, P., additional, Griffin, M., additional, Hoare, M., additional, Huang, M., additional, Jiang, B., additional, Joblin, C., additional, Joncas, G., additional, Juvela, M., additional, Kirk, J., additional, Lagache, G., additional, Li, J. Z., additional, Lim, T. L., additional, Lord, S. D., additional, Lucas, P. W., additional, Maiolo, B., additional, Marengo, M., additional, Marshall, D., additional, Masi, S., additional, Massi, F., additional, Matsuura, M., additional, Meny, C., additional, Minier, V., additional, Miville-Deschênes, M.-A., additional, Montier, L., additional, Motte, F., additional, Müller, T. G., additional, Natoli, P., additional, Neves, J., additional, Olmi, L., additional, Paladini, R., additional, Paradis, D., additional, Pestalozzi, M., additional, Pezzuto, S., additional, Piacentini, F., additional, Pomarès, M., additional, Popescu, C. C., additional, Reach, W. T., additional, Richer, J., additional, Ristorcelli, I., additional, Roy, A., additional, Royer, P., additional, Russeil, D., additional, Saraceno, P., additional, Sauvage, M., additional, Schilke, P., additional, Schneider-Bontemps, N., additional, Schuller, F., additional, Schultz, B., additional, Shepherd, D. S., additional, Sibthorpe, B., additional, Smith, H. A., additional, Smith, M. D., additional, Spinoglio, L., additional, Stamatellos, D., additional, Strafella, F., additional, Stringfellow, G., additional, Sturm, E., additional, Taylor, R., additional, Thompson, M. A., additional, Tuffs, R. J., additional, Umana, G., additional, Valenziano, L., additional, Vavrek, R., additional, Viti, S., additional, Waelkens, C., additional, Ward-Thompson, D., additional, White, G., additional, Wyrowski, F., additional, Yorke, H. W., additional, and Zhang, Q., additional
- Published
- 2010
- Full Text
- View/download PDF
21. 50 nm thick AlN film-based piezoelectric cantilevers for gravimetric detection
- Author
-
Luis Guillermo Villanueva, Matthew H. Matheny, J. Abergel, P. Ivaldi, P. Andreucci, Michael L. Roukes, Emmanuel Defay, R. B. Karabalin, and Sebastien Hentz
- Subjects
Detection limit ,Cantilever ,Materials science ,business.industry ,Mechanical Engineering ,chemistry.chemical_element ,Nanotechnology ,Nitride ,Piezoelectricity ,Electronic, Optical and Magnetic Materials ,Low noise ,chemistry ,Mechanics of Materials ,Aluminium ,Optoelectronics ,Gravimetric analysis ,Electrical and Electronic Engineering ,Allan variance ,business - Abstract
Due to low power operation, intrinsic integrability and compatibility with CMOS processing, aluminum nitride (AlN) piezoelectric (PZE) microcantilevers are a very attractive paradigm for resonant gas sensing. In this paper, we theoretically investigate their ultimate limit of detection and enunciate design rules for performance optimization. The reduction of the AlN layer thickness is found to be critical. We further report the successful development and implementation in cantilever structures with a 50 nm thick active PZE AlN layer. Material characterizations demonstrate that the PZE e_(31) coefficient can remain as high as 0.8 C m^(−2). Electrically transduced frequency responses of the fabricated devices are in good agreement with analytical predictions. Finally, we demonstrate the excellent frequency stability with a 10^(−8) minimum Allan deviation. This exceptionally low noise operation allows us to expect a limit of detection as low as 53 zg µm^(−2) and demonstrate the strong potential of AlN PZE microcantilevers for high resolution gas detection.
- Published
- 2011
22. Electron wave and quantum optics in graphene.
- Author
-
Chakraborti, Himadri, Gorini, Cosimo, Knothe, Angelika, Liu, Ming-Hao, Makk, Péter, Parmentier, François D, Perconte, David, Richter, Klaus, Roulleau, Preden, Sacépé, Benjamin, Schönenberger, Christian, and Yang, Wenmin
- Published
- 2024
- Full Text
- View/download PDF
23. An optimal Bayesian strategy for comparing Wiener–Hunt deconvolution models in the absence of ground truth.
- Author
-
Harroué, B, Giovannelli, J-F, and Pereyra, M
- Subjects
GIBBS sampling ,MEASUREMENT errors ,IMAGE reconstruction ,BIG data ,COVARIANCE matrices - Abstract
This paper considers the quantitative comparison of several alternative models to perform deconvolution in situations where there is no ground truth data available. With applications to very large data sets in mind, we focus on linear deconvolution models based on a Wiener filter. Although comparatively simple, such models are widely prevalent in large scale setting such as high-resolution image restoration because they provide an excellent trade-off between accuracy and computational effort. However, in order to deliver accurate solutions, the models need to be properly calibrated in order to capture the covariance structure of the unknown quantity of interest and of the measurement error. This calibration often requires onerous controlled experiments and extensive expert supervision, as well as regular recalibration procedures. This paper adopts an unsupervised Bayesian statistical approach to model assessment that allows comparing alternative models by using only the observed data, without the need for ground truth data or controlled experiments. Accordingly, the models are quantitatively compared based on their posterior probabilities given the data, which are derived from the marginal likelihoods or evidences of the models. The computation of these evidences is highly non-trivial and this paper consider three different strategies to address this difficulty—a Chib approach, Laplace approximations, and a truncated harmonic expectation—all of which efficiently implemented by using a Gibbs sampling algorithm specialised for this class of models. In addition to enabling unsupervised model selection, the output of the Gibbs sampler can also be used to automatically estimate unknown model parameters such as the variance of the measurement error and the power of the unknown quantity of interest. The proposed strategies are demonstrated on a range of image deconvolution problems, where they are used to compare different modelling choices for the instrument's point spread function and covariance matrices for the unknown image and for the measurement error. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
24. Ephemeral walls for natural, flexible living.
- Author
-
Gatóo, Ana, Ramage, Michael H., and Bakker, Ron
- Published
- 2024
- Full Text
- View/download PDF
25. Robustness of topologically protected transport in graphene–boron nitride lateral heterostructures.
- Author
-
D S L Abergel
- Published
- 2017
- Full Text
- View/download PDF
26. Polycyclic Aromatic Hydrocarbon Emission in the Central Regions of Three Seyferts and the Implication for Underlying Feedback Mechanisms.
- Author
-
Zhang, Lulu, García-Bernete, Ismael, Packham, Chris, Donnan, Fergus R., Rigopoulou, Dimitra, Hicks, Erin K. S., Davies, Ric I., Shimizu, Taro T., Alonso-Herrero, Almudena, Almeida, Cristina Ramos, Pereira-Santaella, Miguel, Ricci, Claudio, Bunker, Andrew J., Leist, Mason T., Rosario, David J., García-Burillo, Santiago, Muñoz, Laura Hermosa, Combes, Francoise, Imanishi, Masatoshi, and Labiano, Alvaro
- Published
- 2024
- Full Text
- View/download PDF
27. Enhancing thermal comfort in buildings through the integration of phase change material on the building envelope: a simulation study.
- Author
-
Bordoloi, U and Das, B
- Published
- 2024
- Full Text
- View/download PDF
28. The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies at z ∼ 8.5–14.5.
- Author
-
Finkelstein, Steven L., Leung, Gene C. K., Bagley, Micaela B., Dickinson, Mark, Ferguson, Henry C., Papovich, Casey, Akins, Hollis B., Arrabal Haro, Pablo, Davé, Romeel, Dekel, Avishai, Kartaltepe, Jeyhan S., Kocevski, Dale D., Koekemoer, Anton M., Pirzkal, Nor, Somerville, Rachel S., Yung, L. Y. Aaron, Amorín, Ricardo O., Backhaus, Bren E., Behroozi, Peter, and Bisigello, Laura
- Published
- 2024
- Full Text
- View/download PDF
29. High harmonic generation in graphene quantum dots.
- Author
-
Zafar, Ahmal Jawad, Mitra, Aranyo, and Apalkov, Vadym
- Published
- 2024
- Full Text
- View/download PDF
30. ALMA Lensing Cluster Survey: Full Spectral Energy Distribution Analysis of z ∼ 0.5–6 Lensed Galaxies Detected with millimeter Observations.
- Author
-
Uematsu, Ryosuke, Ueda, Yoshihiro, Kohno, Kotaro, Toba, Yoshiki, Yamada, Satoshi, Smail, Ian, Umehata, Hideki, Fujimoto, Seiji, Hatsukade, Bunyo, Ao, Yiping, Bauer, Franz Erik, Brammer, Gabriel, Dessauges-Zavadsky, Miroslava, Espada, Daniel, Jolly, Jean-Baptiste, Koekemoer, Anton M., Kokorev, Vasily, Magdis, Georgios E., Oguri, Masamune, and Sun, Fengwu
- Subjects
SPECTRAL energy distribution ,GALACTIC evolution ,GALAXIES ,REDSHIFT ,STARBURSTS ,ACTIVE galactic nuclei ,STAR formation - Abstract
Sub/millimeter galaxies are a key population for the study of galaxy evolution because the majority of star formation at high redshifts occurred in galaxies deeply embedded in dust. To search for this population, we have performed an extensive survey with Atacama Large Millimeter/submillimeter Array (ALMA), called the ALMA Lensing Cluster Survey (ALCS). This survey covers 133 arcmin
2 area and securely detects 180 sources at z ∼ 0.5–6 with a flux limit of ∼0.2 mJy at 1.2 mm. Here, we report the results of multiwavelength spectral energy distribution analysis of the whole ALCS sample, utilizing the observed-frame UV to millimeter photometry. We find that the majority of the ALCS sources lie on the star-forming main sequence, with a smaller fraction showing intense starburst activities. The ALCS sample contains high infrared-excess sources ( IRX = log (L dust / L UV) > 1 ), including two extremely dust-obscured galaxies (IRX > 5). We also confirm that the ALCS sample probes a broader range in lower dust mass than conventional submillimeter galaxy samples in the same redshift range. We identify six heavily obscured active galactic nucleus (AGN) candidates that are not detected in the archival Chandra data in addition to the three X-ray AGNs reported by Uematsu et al. (2023). The inferred AGN luminosity density shows a possible excess at z = 2–3 compared with that determined from X-ray surveys below 10 keV. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
31. Spin and charge persistent currents in a Kane Mele α - T 3 quantum ring.
- Author
-
Islam, Mijanur and Basu, Saurabh
- Published
- 2024
- Full Text
- View/download PDF
32. Resolved Measurements of the CO-to-H2 Conversion Factor in 37 Nearby Galaxies.
- Author
-
Chiang, I-Da, Sandstrom, Karin M., Chastenet, Jérémy, Bolatto, Alberto D., Koch, Eric W., Leroy, Adam K., Sun, Jiayi, Teng, Yu-Hsuan, and Williams, Thomas G.
- Subjects
STARBURSTS ,STELLAR density (Stellar population) ,GALAXIES ,STELLAR mass ,STAR formation ,GRAVITATION - Abstract
We measure the CO-to-H
2 conversion factor (αCO ) in 37 galaxies at 2 kpc resolution, using the dust surface density inferred from far-infrared emission as a tracer of the gas surface density and assuming a constant dust-to-metal ratio. In total, we have ∼790 and ∼610 independent measurements of αCO for CO (2–1) and (1–0), respectively. The mean values for αCO (2–1) and αCO (1–0) are 9.3 − 5.4 + 4.6 and 4.2 − 2.0 + 1.9 M ⊙ pc − 2 (K km s − 1) − 1 , respectively. The CO-intensity-weighted mean is 5.69 for αCO (2–1) and 3.33 for αCO (1–0) . We examine how αCO scales with several physical quantities, e.g., the star formation rate (SFR), stellar mass, and dust-mass-weighted average interstellar radiation field strength ( U ¯ ). Among them, U ¯ , ΣSFR , and the integrated CO intensity (WCO ) have the strongest anticorrelation with spatially resolved αCO . We provide linear regression results to αCO for all quantities tested. At galaxy-integrated scales, we observe significant correlations between αCO and WCO , metallicity, U ¯ , and ΣSFR . We also find that αCO in each galaxy decreases with the stellar mass surface density (Σ⋆ ) in high-surface-density regions (Σ⋆ ≥ 100 M⊙ pc−2 ), following the power-law relations α CO (2 – 1) ∝ Σ ⋆ − 0.5 and α CO (1 – 0) ∝ Σ ⋆ − 0.2 . The power-law index is insensitive to the assumed dust-to-metal ratio. We interpret the decrease in αCO with increasing Σ⋆ as a result of higher velocity dispersion compared to isolated, self-gravitating clouds due to the additional gravitational force from stellar sources, which leads to the reduction in αCO . The decrease in αCO at high Σ⋆ is important for accurately assessing molecular gas content and star formation efficiency in the centers of galaxies, which bridge "Milky Way–like" to "starburst-like" conversion factors. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
33. Detection of Extragalactic Anomalous Microwave Emission in NGC 2903 Using KVN Single-dish Observations.
- Author
-
Poojon, Panomporn, Chung, Aeree, Hoang, Thiem, Baek, Junhyun, Nakanishi, Hiroyuki, Hirota, Tomoya, and Tsai, Chao-Wei
- Subjects
SPECTRAL energy distribution ,STAR formation ,MICROWAVES ,MOLECULAR clouds ,STARBURSTS - Abstract
We present the results of the single-dish observations using the Korean VLBI Network to search for anomalous microwave emission (AME) in nearby galaxies. The targets were selected from 'Mapping the dense molecular gas in the strongest star-forming galaxies' (MALATANG), a legacy survey project of the James Clerk Maxwell Telescope. The MALATANG galaxies are good representatives of local galaxies with enhanced nuclear activity associated with star formation and/or active galactic nuclei (AGNs), providing IR-bright galaxy samples; thus, they are good candidates for AME hosts. Combining with ancillary data, we investigated the radio–IR spectral energy distribution (SED), while searching for AME signals in five galaxies. The AME in NGC 2903 was well detected at a significant confidence level, whereas that in NGC 2146 and M82 was marginal. NGC 1068 and Arp 299 indicated no significant hints, and we provide upper limits for the AME. The best-fit SED exhibited local peaks of the AME components at higher frequencies and with stronger peak fluxes than those in previous studies. This suggested that AME originates from denser environments such as molecular clouds or photodissociation regions rather than warm neutral/ionized medium as commonly suggested by previous studies. Further, our AME-detected targets were observed to exhibit higher specific star formation rates than the other extragalactic AME hosts. Furthermore, AME favored starburst galaxies among our sample rather than AGN hosts. Consequently, this might imply that AGNs are excessively harsh environments for tiny dust to survive. [ABSTRACT FROM AUTHOR]
- Published
- 2024
- Full Text
- View/download PDF
34. Enhanced Subkiloparsec-scale Star Formation: Results from a JWST Size Analysis of 341 Galaxies at 5 < z < 14.
- Author
-
Morishita, Takahiro, Stiavelli, Massimo, Chary, Ranga-Ram, Trenti, Michele, Bergamini, Pietro, Chiaberge, Marco, Leethochawalit, Nicha, Roberts-Borsani, Guido, Shen, Xuejian, and Treu, Tommaso
- Subjects
STAR formation ,GALAXIES ,SUPERMASSIVE black holes ,GALACTIC redshift - Abstract
We present a comprehensive search and analysis of high-redshift galaxies in a suite of nine public JWST extragalactic fields taken in Cycle 1, covering a total effective search area of ∼ 358 arcmin 2 . Through conservative (8 σ) photometric selection, we identify 341 galaxies at 5 < z < 14, with 109 having spectroscopic redshift measurements from the literature, including recent JWST NIRSpec observations. Our regression analysis reveals that the rest-frame UV size–stellar mass relation follows R eff ∝ M * 0.19 ± 0.03 , similar to that of star-forming galaxies at z ∼ 3, but scaled down in size by ∼0.7 dex. We find a much slower rate for the average size evolution over the redshift range, R
eff ∝ (1 + z)−0.4±0.2 , than that derived in the literature. A fraction (∼13%) of our sample galaxies are marginally resolved even in the NIRCam imaging (≲100 pc), located at ≳1.5 σ below the derived size–mass slope. These compact sources exhibit a high star formation surface density ΣSFR > 10 M⊙ yr−1 kpc−2 , a range in which only <0.01% of the local star-forming galaxy sample is found. For those with available NIRSpec data, no evidence of ongoing supermassive black hole accretion is observed. A potential explanation for the observed high [O iii ]-to-H β ratios could be high shock velocities, likely originating within intense star-forming regions characterized by high ΣSFR . Lastly, we find that the rest-frame UV and optical sizes of our sample are comparable. Our results are consistent with these early galaxies building up their structures inside out and being yet to exhibit the strong color gradient seen at lower redshift. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
35. Two-photon absorption in gapped bilayer graphene with a tunable chemical potential.
- Author
-
M K Brinkley, D S L Abergel, and B D Clader
- Published
- 2016
- Full Text
- View/download PDF
36. PASSAGES: The Wide-ranging, Extreme Intrinsic Properties of Planck-selected, Lensed Dusty Star-forming Galaxies.
- Author
-
Kamieneski, Patrick S., Yun, Min S., Harrington, Kevin C., Lowenthal, James D., Wang, Q. Daniel, Frye, Brenda L., Jiménez-Andrade, Eric F., Vishwas, Amit, Cooper, Olivia, Pascale, Massimo, Foo, Nicholas, Berman, Derek, Englert, Anthony, and Garcia Diaz, Carlos
- Subjects
GALAXIES ,RADIATION pressure ,GALAXY formation ,STARBURSTS ,OPTICAL images - Abstract
The PASSAGES (Planck All-Sky Survey to Analyze Gravitationally-lensed Extreme Starbursts) collaboration has recently defined a sample of 30 gravitationally lensed dusty star-forming galaxies (DSFGs). These rare, submillimeter-selected objects enable high-resolution views of the most extreme sites of star formation in galaxies at cosmic noon. Here, we present the first major compilation of strong lensing analyses using lenstool for PASSAGES, including 15 objects spanning z = 1.1–3.3, using complementary information from 0.″6-resolution 1.1 mm Atacama Large Millimeter/submillimeter Array and 0.″4 5 cm Jansky Very Large Array continuum imaging, in tandem with 1.6 μ m Hubble and optical imaging with Gemini-S. Magnifications range from μ = 2 to 28 (median μ = 7), yielding intrinsic infrared luminosities of L
IR = 0.2–5.9 × 1013 L⊙ (median 1.4 × 1013 L⊙ ) and inferred star formation rates of 170–6300 M⊙ yr−1 (median 1500 M⊙ yr−1 ). These results suggest that the PASSAGES objects comprise some of the most extreme known starbursts, rivaling the luminosities of even the brightest unlensed objects, further amplified by lensing. The intrinsic sizes of far-infrared continuum regions are large (Re = 1.7–4.3 kpc; median 3.0 kpc) but consistent with LIR – Re scaling relations for z > 1 DSFGs, suggesting a widespread spatial distribution of star formation. With modestly high angular resolution, we explore if these objects might be maximal starbursts. Instead of approaching Eddington-limited surface densities, above which radiation pressure will disrupt further star formation, they are safely sub-Eddington—at least on global, galaxy-integrated scales. [ABSTRACT FROM AUTHOR]- Published
- 2024
- Full Text
- View/download PDF
37. JWST: Deuterated PAHs, PAH Nitriles, and PAH Overtone and Combination Bands. I. Program Description and First Look.
- Author
-
Boersma, C., Allamandola, L. J., Esposito, V. J., Maragkoudakis, A., Bregman, J. D., Temi, P., Lee, T. J., Fortenberry, R. C., and Peeters, E.
- Subjects
POLYCYCLIC aromatic hydrocarbons ,NITRILES ,STAR-branched polymers ,SPACE telescopes ,INTERSTELLAR molecules ,INFRARED astronomy - Abstract
A first look is taken at the NIRSpec 1–5 μ m observations from James Webb Space Telescope program 1591 that targets seven objects along the low-mass stellar life cycle with polycyclic aromatic hydrocarbon (PAH) emission. Spectra extracted from a 1.″5 radius circular aperture are explored, showing a wealth of features, including the 3 μ m PAH complex, the PAH continuum, and atomic and molecular emission lines from H i, He, H
2 , and other species. CO2 - and H2 O-ice absorption and CO emission is also seen. Focusing on the bright-PDR position in M17, the PAH CH stretch falls at 3.29 μ m (FWHM = 0.04 μ m). Signs of its 1.68 μ m overtone are confused by line emission in all targets. Multicomponent decomposition reveals a possible aliphatic deuterated PAH feature centered at 4.65 μ m (FWHM = 0.02 μ m), giving [D/H]alip. = 31% ± 12.7%. However, there is little sign of its aromatic counterpart between 4.36 and 4.43 μ m. There is also little sign of PAH nitrile emission between 4.34 and 4.39 μ m. A PAH continuum rises from ∼1 to 3.2 μ m, after which it jumps by about a factor of 2.5 at 3.6 μ m, with bumps at 3.8, 4.04, and 4.34 μ m adding structure. The CO2 absorption band in M17 is matched with 10:1 H2 O:CO2 ice at 10 K. The v = 0 pure rotational molecular hydrogen population diagram reveals >2200 K UV-pumped gas. The hydrogen Pfund series runs from levels 10 to >30. Considering Br α /Br β = 0.381 ± 0.01966 and Case B recombination results in AV ≃ 8. CO emission in IRAS 21282+5050 originates from 258 K gas. In-depth spectral–spatial analysis of all features and targets is planned for a series of forthcoming papers. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
38. Heterogeneous anomalous transport in cellular and molecular biology.
- Author
-
Waigh, Thomas Andrew and Korabel, Nickolay
- Subjects
CYTOLOGY ,INELASTIC neutron scattering ,MOLECULAR biology ,GLOBULAR proteins ,NUCLEAR magnetic resonance ,CELL motility ,MACHINE learning - Abstract
It is well established that a wide variety of phenomena in cellular and molecular biology involve anomalous transport e.g. the statistics for the motility of cells and molecules are fractional and do not conform to the archetypes of simple diffusion or ballistic transport. Recent research demonstrates that anomalous transport is in many cases heterogeneous in both time and space. Thus single anomalous exponents and single generalised diffusion coefficients are unable to satisfactorily describe many crucial phenomena in cellular and molecular biology. We consider advances in the field of heterogeneous anomalous transport (HAT) highlighting: experimental techniques (single molecule methods, microscopy, image analysis, fluorescence correlation spectroscopy, inelastic neutron scattering, and nuclear magnetic resonance), theoretical tools for data analysis (robust statistical methods such as first passage probabilities, survival analysis, different varieties of mean square displacements, etc), analytic theory and generative theoretical models based on simulations. Special emphasis is made on high throughput analysis techniques based on machine learning and neural networks. Furthermore, we consider anomalous transport in the context of microrheology and the heterogeneous viscoelasticity of complex fluids. HAT in the wavefronts of reaction–diffusion systems is also considered since it plays an important role in morphogenesis and signalling. In addition, we present specific examples from cellular biology including embryonic cells, leucocytes, cancer cells, bacterial cells, bacterial biofilms, and eukaryotic microorganisms. Case studies from molecular biology include DNA, membranes, endosomal transport, endoplasmic reticula, mucins, globular proteins, and amyloids. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
39. Magellanic System Stars Identified in SMACS J0723.3-7327 James Webb Space Telescope Early Release Observations Images.
- Author
-
Summers, Jake, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Holwerda, Benne W., Conselice, Christopher J., Adams, Nathan J., Frye, Brenda L., Diego, Jose M., Willmer, Christopher N. A., Ortiz III, Rafael, Cheng, Cheng, Pigarelli, Alex, Robotham, Aaron, D'Silva, Jordan C. J., Tompkins, Scott, Driver, Simon P., and Yan, Haojing
- Subjects
SPACE telescopes ,LARGE magellanic cloud ,DENSITY of stars ,SPECTRAL energy distribution ,STELLAR parallax ,MAGELLANIC clouds - Abstract
We identify 71 distant stars in James Webb Space Telescope/NIRCam early release observations (ERO) images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small (∼10°) angular separation between SMACS 0723 and the Large Magellanic Cloud (LMC), it is likely that these stars are associated with the LMC outskirts or the Leading Arm. This is further bolstered by a spectral energy distribution (SED) analysis, which suggests an excess of stars at a physical distance of 40–100 kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is ∼2.3 times that of stars in a blank field with similar Galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is ∼6.1 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] = −1.0 and an age of ∼5.0 Gyr. On the assumption that all of the 71 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is ∼740 stars kpc
−3 , which helps trace the density of stars in the LMC outskirts. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
40. Tracing the Total Stellar Mass and Star Formation of High-redshift Protoclusters.
- Author
-
Popescu, Roxana, Pope, Alexandra, Lee, Kyoung-Soo, Alberts, Stacey, Chiang, Yi-Kuan, Lee, Sowon, Brodwin, Mark, McKinney, Jed, and Ramakrishnan, Vandana
- Subjects
STAR formation ,GALACTIC evolution ,GALAXY clusters ,SPECTRAL energy distribution ,GALAXY formation ,STELLAR mass ,GALAXIES - Abstract
As the progenitors of present-day galaxy clusters, protoclusters are excellent laboratories to study galaxy evolution. Since existing observations of protoclusters are limited to the detected constituent galaxies at UV and/or infrared wavelengths, the details of how typical galaxies grow in these young, pre-virialized structures remain uncertain. We measure the total stellar mass and star formation within protoclusters, including the contribution from faint undetected members by performing a stacking analysis of 211 z = 2–4 protoclusters selected as Planck cold sources. We stack Wide-field Infrared Survey Explorer and Herschel/SPIRE images to measure the angular size and the spectral energy distribution of the integrated light from the protoclusters. The fluxes of protoclusters selected as Planck cold sources can be contaminated by line-of-sight interlopers. Using the WebSky simulation, we estimate that a single protocluster contributes 33% ± 15% of the flux of a Planck cold source on average. After this correction, we obtain a total star formation rate of 7.3 ± 3.2 × 10
3 M⊙ yr−1 and a total stellar mass of 4.9 ± 2.2 × 1012 M⊙ . Our results indicate that protoclusters have, on average, 2× more star formation and 4× more stellar mass than the total contribution from individually detected galaxies in spectroscopically confirmed protoclusters. This suggests that much of the total flux within z = 2–4 protoclusters comes from galaxies with luminosities lower than the detection limit of SPIRE (LIR < 3 × 1012 L⊙ ). Lastly, we find that protoclusters subtend a half-light radius of 2.′8 (4.2–5.8 cMpc), which is consistent with simulations. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
41. Investigating the Globally Collapsing Hub–Filament Cloud G326.611+0.811.
- Author
-
He, Yu-Xin, Liu, Hong-Li, Tang, Xin-Di, Qin, Sheng-Li, Zhou, Jian-Jun, Esimbek, Jarken, Pan, Si-Rong, Li, Da-Lei, Zhao, Meng-Ke, Ji, Wei-Guang, and Komesh, Toktarkhan
- Subjects
GRAVITATIONAL collapse ,STAR formation ,HIGH mass stars ,GRAVITATIONAL instability ,FIBERS ,PROTOSTARS - Abstract
We present a dynamics study toward the G326.611+0.811 (G326) hub–filament system (HFS) cloud using new APEX observations of both
13 CO and C18 O (J = 2–1). The G326 HFS cloud constitutes a central hub and at least four hub-composing filaments that are divided into a major branch of filaments (F1 and F2) and a side branch (F3–F5). The cloud holds ongoing high-mass star formation as characterized by three massive dense clumps (i.e., 370–1100 M⊙ and 0.14–0.16 g cm−2 for C1–C3) with high clump-averaged mass infalling rates (>10−3 M⊙ yr−1 ) within the major filament branch, and the associated point sources bright at 70 μ m, typical of young protostars. Along the five filaments, velocity gradients are found in both13 CO and C18 O (J = 2–1) emission, suggesting that filament-aligned gravitational collapse toward the central hub (i.e., C2) is responsible for the high-mass star formation therein. Moreover, a periodic velocity oscillation along the major filament branch is revealed in both13 CO and C18 O (J = 2–1) emission with a characteristic wavelength of ∼3.5 pc and an amplitude of ∼0.31–0.38 km s−1 . We suggest that this pattern of velocity oscillation in G326 could arise from clump-forming gas motion induced by gravitational instabilities. The prevalent velocity gradients, fragmentation of the major branch of filaments, and the ongoing collapse of the three massive dense clumps are indicative that G326 is an HFS undergoing global collapse. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
42. Grain Growth and Dust Segregation Revealed by Multiwavelength Analysis of the Class I Protostellar Disk WL 17.
- Author
-
Han, Ilseung, Kwon, Woojin, Aso, Yusuke, Bae, Jaehan, and Sheehan, Patrick
- Subjects
DUST ,PROTOPLANETARY disks ,GRAVITATIONAL instability ,MOLECULAR clouds ,ORIGIN of planets ,RADIATIVE transfer - Abstract
The first step toward planet formation is grain growth from (sub)micrometer to millimeter/centimeter sizes. Grain growth has been reported not only in Class II protoplanetary disks but also in Class 0/I protostellar envelopes. However, early-stage grain growth occurring in Class 0/I stages has rarely been observed on the protostellar disk scale. Here we present the results from the Atacama Large Millimeter/submillimeter Array Band 3 (λ = 3.1 mm) and 7 (λ = 0.87 mm) archival data of the Class I protostellar disk WL 17 in the ρ Ophiuchus molecular cloud. Disk substructures are found in both bands, but they are different: while a central hole and a symmetric ring appear in Band 3, an off-center hole and an asymmetric ring are shown in Band 7. Furthermore, we obtain an asymmetric spectral index map with a low mean value of α = 2.28 ± 0.02, suggestive of grain growth and dust segregation on the protostellar disk scale. Our radiative transfer modeling verifies these two features by demonstrating that 10 cm sized large grains are symmetrically distributed, whereas 10 μ m sized small grains are asymmetrically distributed. In addition, the analysis shows that the disk is expected to be massive and gravitationally unstable. We thus suggest a single Jupiter-mass protoplanet formed by gravitational instability as the origin of the ring-like structure, grain growth, and dust segregation identified in WL 17. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
43. Circular Practices in Construction.
- Author
-
Hubmann, G and van Maaren, V
- Published
- 2023
- Full Text
- View/download PDF
44. Young Stellar Object Candidates in IC 417.
- Author
-
Rebull, L. M., Anderson III, R. L., Hall, G., Kirkpatrick, J. D., Koenig, X., Odden, C. E., Rodriguez, B., Sanchez, R., Senson, B., Urbanowski, V., Austin, M., Blood, K., Kerman, E., Long, J., and Roosa, N.
- Published
- 2023
- Full Text
- View/download PDF
45. A Recipe for Unbiased Background Modeling in Deep Wide-field Astronomical Images.
- Author
-
Liu, Qing, Abraham, Roberto, Martin, Peter G., Bowman, William P., van Dokkum, Pieter, Janssens, Steven R., Chen, Seery, Keim, Michael A., Lokhorst, Deborah, Pasha, Imad, Shen, Zili, and Zhang, Jielai
- Subjects
SURFACE brightness (Astronomy) ,COVARIANCE matrices ,IMAGE processing ,INTERPLANETARY dust ,ASTRONOMICAL surveys - Abstract
Unbiased sky background modeling is crucial for the analysis of deep wide-field images, but it remains a major challenge in low surface brightness astronomy. Traditional image processing algorithms are often designed to produce artificially flat backgrounds, erasing astrophysically meaningful structures. In this paper, we present three ideas that can be combined to produce wide-field astronomical data that preserve accurate representations of the background sky: (1) Use of all-sky infrared/submillimeter data to remove the large-scale time-varying components while leaving the scattered light from Galactic cirrus intact, with the assumptions of (a) the underlying background has little power on small scales, and (b) the Galactic cirrus in the field is optically thin on large scales; (2) Censoring of frames contaminated by anomalously prominent wings in the wide-angle point-spread function; and (3) Incorporation of spatial covariance in image stacking that controls the local background consistency. We demonstrate these methods using example data sets obtained with the Dragonfly Telephoto Array, but these general techniques are prospective to be applied to improve sky models in data obtained from other wide-field imaging surveys, including those from the upcoming Vera Rubin Telescope. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
46. The Fate of the Interstellar Medium in Early-type Galaxies. II. Observational Evidence for Morphological Quenching.
- Author
-
Leśniewska, Aleksandra, Michałowski, M. J., Gall, C., Hjorth, J., Nadolny, J., Ryzhov, O., and Solar, M.
- Subjects
INTERSTELLAR medium ,GALAXIES ,ELLIPTICAL galaxies ,TYPE I supernovae ,STELLAR populations ,BIPOLAR outflows (Astrophysics) - Abstract
The mechanism by which galaxies stop forming stars and get rid of their interstellar medium (ISM) remains elusive. Here, we study a sample of more than 2000 elliptical galaxies in which dust emission has been detected. This is the largest sample of such galaxies ever analyzed. We infer the timescale for removal of dust in these galaxies and investigate its dependence on physical and environmental properties. We obtain a dust-removal timescale in elliptical galaxies of τ = 2.26 ± 0.18 Gyr, corresponding to a half-life time of 1.57 ± 0.12 Gyr. This timescale does not depend on environment, stellar mass, or redshift. We observe a departure of dusty elliptical galaxies from the relation between star formation rate and dust mass. This is caused by the star formation rates declining faster than the dust masses and indicates that there exists an internal mechanism that affects star formation but leaves the ISM intact. Morphological quenching together with ionization or outflows caused by older stellar populations (Type Ia supernovae or planetary nebulae) is consistent with these observations. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
47. Soft X-Ray-induced Dimerization of Methane.
- Author
-
Reinwardt, S., Baev, I., Cieslik, P., Baev, K., Buhr, T., Perry-Sassmannshausen, A., Schippers, S., Müller, A., Trinter, F., Viefhaus, J., and Martins, M.
- Subjects
DAUGHTER ions ,CHEMICAL reactions ,PLANETARY atmospheres ,DIMERIZATION ,ION traps ,FAR ultraviolet radiation ,SOFT X rays - Abstract
Carbon 1s excitation of methane, CH
4 , has been studied in the gas phase using the ion trap integrated with the photon–ion instrument at PETRA III/DESY and soft X-rays from the beamline P04. The created photoions are stored within the ion trap so that in further steps the photoions can undergo reactions with neutral methane molecules. The ionic photoproducts as well as reaction products created thereby are mass-over-charge analyzed by an ion time-of-flight spectrometer. Besides the photoions, product ions with up to three carbon atoms are found. In contrast to experiments using vacuum ultraviolet radiation, especially highly reactive product ions with a small number of hydrogen atoms such as C 2 H 2 + and C 2 H 3 + are found, which are important precursors for larger hydrocarbons such as C6 H6 . Possible production routes of the product ions are analyzed on the basis of a model that considers the probabilities for photofragmentation and the first subsequent chemical reaction step. The model indicates that the high degree of fragmentation by photons with energies around 280 eV is favoring these products. The results of the measurements show that the products like C 2 H 2 + and C 2 H 3 + can be generated by a single collision of the ionization product with neutral methane. The results suggest that soft X-rays might be important for chemical reactions in planetary atmospheres, which has usually not been taken into account. However, due to the high degree of fragmentation and large cross sections involved, they can have a large influence even when the corresponding photon flux is rather small. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
48. 2 mm Observations and the Search for High-redshift Dusty Star-forming Galaxies.
- Author
-
Cowie, L. L., Barger, A. J., and Bauer, F. E.
- Subjects
GALAXIES ,BLOOD coagulation factor IX ,STAR formation ,GALAXY formation ,ACTINIC flux ,GALACTIC redshift - Abstract
Finding high-redshift (z ≫ 4) dusty star-forming galaxies is extremely challenging. It has recently been suggested that millimeter selections may be the best approach since the negative K-correction makes galaxies at a given far-infrared luminosity brighter at z ≳ 4 than those at z = 2–3. Here we analyze this issue using a deep Atacama Large Millimeter/submillimeter Array (ALMA) 2 mm sample obtained by targeting ALMA 870 μ m priors (these priors were the result of targeting SCUBA-2 850 μ m sources) in the GOODS-S. We construct prior-based 2 mm galaxy number counts and compare them with published blank field-based 2 mm counts, finding good agreement down to 0.2 mJy. Only a fraction of the current 2 mm extragalactic background light is resolved, and we estimate what observational depths may be needed to resolve it fully. By complementing the 2 mm ALMA data with a deep SCUBA-2 450 μ m sample, we exploit the steep gradient with a redshift of the 2 mm–450 μ m flux density ratio to estimate redshifts for those galaxies without spectroscopic or robust optical/near-infrared photometric redshifts. Our observations measure galaxies with star formation rates in excess of 250 M
⊙ yr−1 . For these galaxies, the star formation rate densities fall by a factor of 9 from z = 2–3 to z = 5–6. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
49. The GLASS-JWST Early Release Science Program. II. Stage I Release of NIRCam Imaging and Catalogs in the Abell 2744 Region.
- Author
-
Paris, Diego, Merlin, Emiliano, Fontana, Adriano, Bonchi, Andrea, Brammer, Gabriel, Correnti, Matteo, Treu, Tommaso, Boyett, Kristan, Calabrò, Antonello, Castellano, Marco, Chen, Wenlei, Yang, Lilan, Glazebrook, Karl, Kelly, Patrick, Koekemoer, Anton M., Leethochawalit, Nicha, Mascia, Sara, Mason, Charlotte, Morishita, Takahiro, and Nonino, Mario
- Subjects
CATALOGS ,CATALOGING ,SPACE telescopes ,DATA reduction ,GALACTIC redshift ,GALAXY clusters - Abstract
We present images and a multiwavelength photometric catalog based on all of the JWST NIRCam observations obtained to date in the region of the Abell 2744 galaxy cluster. These data come from three different programs, namely, the GLASS-JWST Early Release Science Program, UNCOVER, and the Director's Discretionary Time program 2756. The observed area in the NIRCam wide-band filters—covering the central and extended regions of the cluster, as well as new parallel fields—is 46.5 arcmin
2 in total. All images in eight bands (F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W) have been reduced adopting the latest calibration and reference files available. Data reduction has been performed using an augmented version of the official JWST pipeline, with improvements aimed at removing or mitigating defects in the raw images and improving the background subtraction and photometric accuracy. We obtain an F444W-detected multiband catalog, including all NIRCam and available Hubble Space Telescope data, adopting forced-aperture photometry on point-spread-function-matched images. The catalog is intended to enable early scientific investigations and is optimized for the study of faint galaxies; it contains 24,389 sources, with a 5 σ limiting magnitude in the F444W band ranging from 28.5 AB to 30.5 AB, as a result of the varying exposure times of the surveys that observed the field. We publicly release the reduced NIRCam images, associated multiwavelength catalog, and the code adopted for 1/ f noise removal with the aim of aiding users in familiarizing themselves with JWST NIRCam data and identifying suitable targets for follow-up observations. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
50. The Origin of Dust Polarization in the Orion Bar.
- Author
-
Le Gouellec, Valentin J. M., Andersson, B-G, Soam, Archana, Schirmer, Thiébaut, Michail, Joseph M., Lopez-Rodriguez, Enrique, Flores, Sophia, Chuss, David T., Vaillancourt, John E., Hoang, Thiem, and Lazarian, Alex
- Subjects
LINEAR polarization ,MAGNETIC fields ,BREWSTER'S angle ,DUST ,TENSILE strength ,GRAIN size - Abstract
The linear polarization of thermal dust emission provides a powerful tool to probe interstellar and circumstellar magnetic fields, because aspherical grains tend to align themselves with magnetic field lines. While the Radiative Alignment Torque (RAT) mechanism provides a theoretical framework for this phenomenon, some aspects of this alignment mechanism still need to be quantitatively tested. One such aspect is the possibility that the reference alignment direction changes from the magnetic field (" B -RAT") to the radiation field k-vector (" k -RAT") in areas of strong radiation fields. We investigate this transition toward the Orion Bar PDR, using multiwavelength SOFIA HAWC+ dust polarization observations. The polarization angle maps show that the radiation field direction is on average not the preferred grain alignment axis. We constrain the grain sizes for which the transition from B -RAT to k -RAT occurs in the Orion Bar (grains ≥ 0.1 μ m toward the most irradiated locations), and explore the radiatively driven rotational disruption that may take place in the high-radiation environment of the Bar for large grains. While the grains susceptible to rotational disruption should be in suprathermal rotation and aligned with the magnetic field, k -RAT aligned grains would rotate at thermal velocities. We find that the grain size at which the alignment shifts from B -RAT to k -RAT corresponds to grains too large to survive the rotational disruption. Therefore, we expect a large fraction of grains to be aligned at suprathermal rotation with the magnetic field, and to potentially be subject to rotational disruption, depending on their tensile strength. [ABSTRACT FROM AUTHOR]
- Published
- 2023
- Full Text
- View/download PDF
Catalog
Discovery Service for Jio Institute Digital Library
For full access to our library's resources, please sign in.