Zobrazeno 1 - 10
of 3 227
pro vyhledávání: '"García Rojas, A."'
Autor:
Akras, Stavros, Monteiro, Hektor, Walsh, Jeremy R., Konstantinou, Lydia, Gonçalves, Denise R., Garcia-Rojas, Jorge, Boumis, Panos, Aleman, Isabel
Publikováno v:
A&A, 689, A14 (2024)
We report the first spatially resolved detection of the near-infrared [C I] $\lambda$8727 emission from the outer pair of low-ionization structures in the planetary nebula NGC 7009 from data obtained by the Multi Unit Spectroscopic Explorer integral
Externí odkaz:
http://arxiv.org/abs/2409.00371
Autor:
Méndez-Delgado, J. E., Kreckel, K., Esteban, C., García-Rojas, J., Carigi, L., Sander, A. A. C., Palla, M., Chruślińska, M., De Looze, I., Relaño, M., van der Giessen, S. A., Reyes-Rodríguez, E., Sánchez, S. F.
In stars, metallicity is usually traced using Fe, while in nebulae, O serves as the preferred proxy. Both elements have different nucleosynthetic origins and are not directly comparable. Additionally, in ionized nebulae, Fe is heavily depleted onto d
Externí odkaz:
http://arxiv.org/abs/2408.06215
Autor:
Gómez-Llanos, V., García-Rojas, J., Morisset, C., Monteiro, H., Jones, D., Wesson, R., Boffin, H. M. J., Corradi, R. L. M.
Publikováno v:
A&A 689, A228 (2024)
(Abridged) The abundance discrepancy problem in planetary nebulae (PNe) has long puzzled astronomers. NGC6153, with its high Abundance Discrepancy Factor (ADF~10), provides an opportunity to understand the chemical structure and ionisation processes
Externí odkaz:
http://arxiv.org/abs/2407.06385
Autor:
Reyes-Rodríguez, E., Méndez-Delgado, J. E., García-Rojas, J., Binette, L., Nemer, A., Esteban, C., Kreckel, K.
Context. Carbon is the fourth most abundant element in the universe and its distribution is critical to understanding stellar evolution and nucleosynthesis. In optical studies of ionized nebulae, the only way to determine the C/H abundance is by usin
Externí odkaz:
http://arxiv.org/abs/2404.18581
Autor:
Mainieri, Vincenzo, Anderson, Richard I., Brinchmann, Jarle, Cimatti, Andrea, Ellis, Richard S., Hill, Vanessa, Kneib, Jean-Paul, McLeod, Anna F., Opitom, Cyrielle, Roth, Martin M., Sanchez-Saez, Paula, Smiljanic, Rodolfo, Tolstoy, Eline, Bacon, Roland, Randich, Sofia, Adamo, Angela, Annibali, Francesca, Arevalo, Patricia, Audard, Marc, Barsanti, Stefania, Battaglia, Giuseppina, Aran, Amelia M. Bayo, Belfiore, Francesco, Bellazzini, Michele, Bellini, Emilio, Beltran, Maria Teresa, Berni, Leda, Bianchi, Simone, Biazzo, Katia, Bisero, Sofia, Bisogni, Susanna, Bland-Hawthorn, Joss, Blondin, Stephane, Bodensteiner, Julia, Boffin, Henri M. J., Bonito, Rosaria, Bono, Giuseppe, Bouche, Nicolas F., Bowman, Dominic, Braga, Vittorio F., Bragaglia, Angela, Branchesi, Marica, Brucalassi, Anna, Bryant, Julia J., Bryson, Ian, Busa, Innocenza, Camera, Stefano, Carbone, Carmelita, Casali, Giada, Casali, Mark, Casasola, Viviana, Castro, Norberto, Catelan, Marcio, Cavallo, Lorenzo, Chiappini, Cristina, Cioni, Maria-Rosa, Colless, Matthew, Colzi, Laura, Contarini, Sofia, Couch, Warrick, D'Ammando, Filippo, D., William d'Assignies, D'Orazi, Valentina, da Silva, Ronaldo, Dainotti, Maria Giovanna, Damiani, Francesco, Danielski, Camilla, De Cia, Annalisa, de Jong, Roelof S., Dhawan, Suhail, Dierickx, Philippe, Driver, Simon P., Dupletsa, Ulyana, Escoffier, Stephanie, Escorza, Ana, Fabrizio, Michele, Fiorentino, Giuliana, Fontana, Adriano, Fontani, Francesco, Sanchez, Daniel Forero, Franois, Patrick, Galindo-Guil, Francisco Jose, Gallazzi, Anna Rita, Galli, Daniele, Garcia, Miriam, Garcia-Rojas, Jorge, Garilli, Bianca, Grand, Robert, Guarcello, Mario Giuseppe, Hazra, Nandini, Helmi, Amina, Herrero, Artemio, Iglesias, Daniela, Ilic, Dragana, Irsic, Vid, Ivanov, Valentin D., Izzo, Luca, Jablonka, Pascale, Joachimi, Benjamin, Kakkad, Darshan, Kamann, Sebastian, Koposov, Sergey, Kordopatis, Georges, Kovacevic, Andjelka B., Kraljic, Katarina, Kuncarayakti, Hanindyo, Kwon, Yuna, La Forgia, Fiorangela, Lahav, Ofer, Laigle, Clotilde, Lazzarin, Monica, Leaman, Ryan, Leclercq, Floriane, Lee, Khee-Gan, Lee, David, Lehnert, Matt D., Lira, Paulina, Loffredo, Eleonora, Lucatello, Sara, Magrini, Laura, Maguire, Kate, Mahler, Guillaume, Majidi, Fatemeh Zahra, Malavasi, Nicola, Mannucci, Filippo, Marconi, Marcella, Martin, Nicolas, Marulli, Federico, Massari, Davide, Matsuno, Tadafumi, Mattheee, Jorryt, McGee, Sean, Merc, Jaroslav, Merle, Thibault, Miglio, Andrea, Migliorini, Alessandra, Minchev, Ivan, Minniti, Dante, Miret-Roig, Nuria, Ibero, Ana Monreal, Montano, Federico, Montet, Ben T., Moresco, Michele, Moretti, Chiara, Moscardini, Lauro, Moya, Andres, Mueller, Oliver, Nanayakkara, Themiya, Nicholl, Matt, Nordlander, Thomas, Onori, Francesca, Padovani, Marco, Pala, Anna Francesca, Panda, Swayamtrupta, Pandey-Pommier, Mamta, Pasquini, Luca, Pawlak, Michal, Pessi, Priscila J., Pisani, Alice, Popovic, Lukav C., Prisinzano, Loredana, Raddi, Roberto, Rainer, Monica, Rebassa-Mansergas, Alberto, Richard, Johan, Rigault, Mickael, Rocher, Antoine, Romano, Donatella, Rosati, Piero, Sacco, Germano, Sanchez-Janssen, Ruben, Sander, Andreas A. C., Sanders, Jason L., Sargent, Mark, Sarpa, Elena, Schimd, Carlo, Schipani, Pietro, Sefusatti, Emiliano, Smith, Graham P., Spina, Lorenzo, Steinmetz, Matthias, Tacchella, Sandro, Tautvaisiene, Grazina, Theissen, Christopher, Thomas, Guillaume, Ting, Yuan-Sen, Travouillon, Tony, Tresse, Laurence, Trivedi, Oem, Tsantaki, Maria, Tsedrik, Maria, Urrutia, Tanya, Valenti, Elena, Van der Swaelmen, Mathieu, Van Eck, Sophie, Verdiani, Francesco, Verdier, Aurelien, Vergani, Susanna Diana, Verhamme, Anne, Vernet, Joel, Verza, Giovanni, Viel, Matteo, Vielzeuf, Pauline, Vietri, Giustina, Vink, Jorick S., Vazquez, Carlos Viscasillas, Wang, Hai-Feng, Weilbacher, Peter M., Wendt, Martin, Wright, Nicholas, Ye, Quanzhi, Yeche, Christophe, Yu, Jiaxi, Zafar, Tayyaba, Zibetti, Stefano, Ziegler, Bodo, Zinchenko, Igor
The Wide-field Spectroscopic Telescope (WST) is proposed as a new facility dedicated to the efficient delivery of spectroscopic surveys. This white paper summarises the initial concept as well as the corresponding science cases. WST will feature simu
Externí odkaz:
http://arxiv.org/abs/2403.05398
Abundance determinations in planetary nebulae (PNe) are crucial for understanding stellar evolution and the chemical evolution of the host galaxy. We discuss the complications involved when the presence of a metal-rich phase is suspected in the nebul
Externí odkaz:
http://arxiv.org/abs/2311.14244
Ionized nebulae are key to understanding the chemical composition and evolution of the Universe. Among these nebulae, H~{\sc ii} regions and planetary nebulae are particularly important as they provide insights into the present and past chemical comp
Externí odkaz:
http://arxiv.org/abs/2311.10280
Autor:
Méndez-Delgado, J. Eduardo, Esteban, César, García-Rojas, Jorge, Kreckel, Kathryn, Peimbert, Manuel
In a very recent work, [1] claim that the scenario of temperature inhomogeneities proposed by [2] ($t2$ > 0) is not able to explain the O$^{2+}$/H$^{+}$ abundance discrepancy observed between the calculations based on the optical [OIII] collisional e
Externí odkaz:
http://arxiv.org/abs/2310.01197
Autor:
Méndez-Delgado, J. E., Esteban, C., García-Rojas, J., Arellano-Córdova, K. Z., Kreckel, K., Gómez-Llanos, V., Egorov, O. V., Peimbert, M., Orte-García, M.
We present a first study based on the analysis of the DEep Spectra of Ionized REgions Database (DESIRED). This is a compilation of 190 high signal-to-noise ratio optical spectra of HII regions and other photoionized nebulae, mostly observed with 8-10
Externí odkaz:
http://arxiv.org/abs/2305.13136
Autor:
Méndez-Delgado, J. Eduardo, Esteban, César, García-Rojas, Jorge, Kreckel, Kathryn, Peimbert, Manuel
HII regions, ionized nebulae where massive star formation has taken place, exhibit a wealth of emission lines that are the fundamental basis for estimating the chemical composition of the Universe. For more than 80 years, a discrepancy of at least a
Externí odkaz:
http://arxiv.org/abs/2305.11578