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Start Over Author "Costantin, A" Publisher oxford university press (oup)
20 results on '"Costantin, A"'

1. Near-infrared spectroscopic indices for unresolved stellar populations. III. Composite indices definition as age and metallicity tracers and model comparison

Author

Gasparri, D, Morelli, L, Cuomo, V, Ivanov, V D, Pizzella, A, François, P, Coccato, L, Corsini, E M, Costantin, L, Bontà, Elena Dalla, Méndez-Abreu, J, Aguerri, J A L, Gasparri, D, Morelli, L, Cuomo, V, Ivanov, V D, Pizzella, A, François, P, Coccato, L, Corsini, E M, Costantin, L, Bontà, Elena Dalla, Méndez-Abreu, J, and Aguerri, J A L

Abstract

Recent advances in the stellar population studies of unresolved galaxies in the NIR domain demonstrated that it contains several line-strength indices to be potentially used as diagnostics for stellar population properties. Reduction of the extinction and possibility to disentangle different stellar populations dominating different spectral ranges are obviously beneficial. To this aim, we have investigated the connections between 19 Lick/IDS indices and 39 NIR indices measured in the central regions of 32 galaxies observed with X-shooter. We adopted a systematic approach deriving a correlation matrix using all the optical and NIR indices measured for the galaxies and building new NIR composite indices to maximise their correlations with the best age and metallicity optical tracers. We found that the new T1 and [AlFeCr] composite indices are promising age and metallicity diagnostics in NIR, respectively. We finally tested the T1 and [AlFeCr] indices with the predictions of simple stellar populations models and we found that models show a general agreement with the data. Some fine tuning and further comparison between models and data, that are now largely available, is necessary to reach the prediction level of the optical line-strength indices.

Published
2024
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2. Near-infrared spectroscopic indices for unresolved stellar populations. III. Composite indices definition as age and metallicity tracers and model comparison

Author

Gasparri, D, primary, Morelli, L, additional, Cuomo, V, additional, Ivanov, V D, additional, Pizzella, A, additional, François, P, additional, Coccato, L, additional, Corsini, E M, additional, Costantin, L, additional, Bontà, E Dalla, additional, Méndez-Abreu, J, additional, and Aguerri, J A L, additional

Published
2024
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3. The bar rotation rate as a diagnostic of dark matter content in the centre of disc galaxies

Author

C Buttitta, E M Corsini, J A L Aguerri, L Coccato, L Costantin, V Cuomo, V P Debattista, L Morelli, and A Pizzella

Subjects
Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies: individual: NGC 4264, galaxies: formation, galaxies: individual: NGC 4277, galaxies: structure, FOS: Physical sciences, galaxies: bar, galaxies: kinematics and dynamics, Astrophysics - Astrophysics of Galaxies, Astronomy and Astrophysics
Abstract

We investigate the link between the bar rotation rate and dark matter content in barred galaxies by concentrating on the cases of the lenticular galaxies NGC4264 and NGC4277. These two gas-poor galaxies have similar morphologies, sizes, and luminosities. But, NGC4264 hosts a fast bar, which extends to nearly the corotation, while the bar embedded in NGC4277 is slow and falls short of corotation. We derive the fraction of dark matter $f_{\rm DM, bar}$ within the bar region from Jeans axisymmetric dynamical models by matching the stellar kinematics obtained with the MUSE integral-field spectrograph and using SDSS images to recover the stellar mass distribution. We build mass-follows-light models as well as mass models with a spherical halo of dark matter, which is not tied to the stars. We find that the inner regions of NGC4277 host a larger fraction of dark matter ($f_{\rm DM, bar} = 0.53 \pm 0.02$) with respect to NGC4264 ($f_{\rm DM, bar} = 0.33 \pm 0.04$) in agreement with the predictions of theoretical works and the findings of numerical simulations, which have found that fast bars live in baryon-dominated discs, whereas slow bars experienced a strong drag from the dynamical friction due to a dense DM halo. This is the first time that the bar rotation rate is coupled to $f_{\rm DM, bar}$ derived from dynamical modelling., Accepted for publication on MNRAS, 12 pages

Published
2023
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4. Lack of influence of the environment in the earliest stages of massive galaxy formation

Author

Marianna Annunziatella, Pablo G Pérez-González, Ángela García Argumánez, Guillermo Barro, Belén Alcalde Pampliega, Luca Costantin, Anton M Koekemoer, and Rosa M Mérida

Subjects
Astrofísica, Astronomía, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate how the environment affects the assembly history of massive galaxies. For that purpose, we make use of SHARDS and HST spectro-photometric data, whose depth, spectral resolution, and wavelength coverage allow to perform a detailed analysis of the stellar emission as well as obtaining unprecedentedly accurate photometric redshifts. This expedites a sufficiently accurate estimate of the local environment and a robust derivation of the star formation histories of a complete sample of 332 massive galaxies ($\mathrm{>10^{10}M_{\odot}}$) at redshift $1\leq z \leq 1.5$ in the GOODS-N field. We find that massive galaxies in this redshift range avoid the lowest density environments. Moreover, we observed that the oldest galaxies in our sample with with mass-weighted formation redshift $\mathrm{\overline{z}_{M-w} \geq 2.5}$, avoid the highest density regions, preferring intermediate environments. Younger galaxies, including those with active star formation, tend to live in denser environments ($\Sigma = \mathrm{5.0_{1.1}^{24.8}\times 10^{10}M_{\odot}Mpc^{-2}}$). This behavior could be expected if those massive galaxies starting their formation first would merge with neighbors and sweep their environment earlier. On the other hand, galaxies formed more recently ($\overline{z}_{M-w} < 2.5$) are accreted into large scale structures at later times and we are observing them before sweeping their environment or, alternatively, they are less likely to affect their environment. However, given that both number and mass surface densities of neighbor galaxies is relatively low for the oldest galaxies, our results reveal a very weak correlation between environment and the first formation stages of the earliest massive galaxies., Comment: Accepted for publication in MNRAS

Published
2022
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5. The bar rotation rate as a diagnostic of dark matter content in the centre of disc galaxies

Author

Buttitta, C, Corsini, E M, Aguerri, J A L, Coccato, L, Costantin, L, Cuomo, V, Debattista, Victor P, Morelli, L, Pizzella, A, Buttitta, C, Corsini, E M, Aguerri, J A L, Coccato, L, Costantin, L, Cuomo, V, Debattista, Victor P, Morelli, L, and Pizzella, A

Abstract

We investigate the link between the bar rotation rate and dark matter content in barred galaxies by concentrating on the cases of the lenticular galaxies NGC 4264 and NGC 4277. These two gas-poor galaxies have similar morphologies, sizes, and luminosities. But, NGC 4264 hosts a fast bar, which extends to nearly the corotation, while the bar embedded in NGC 4277 is slow and falls short of corotation. We derive the fraction of dark matter fDM, bar within the bar region from Jeans axisymmetric dynamical models by matching the stellar kinematics obtained with the MUSE integral-field spectrograph and using SDSS images to recover the stellar mass distribution. We build mass-follows-light models as well as mass models with a spherical halo of dark matter, which is not tied to the stars. We find that the inner regions of NGC 4277 host a larger fraction of dark matter (fDM, bar = 0.53 ± 0.02) with respect to NGC 4264 (fDM, bar = 0.33 ± 0.04) in agreement with the predictions of theoretical works and the findings of numerical simulations, which have found that fast bars live in baryon-dominated discs, whereas slow bars experienced a strong drag from the dynamical friction due to a dense DM halo. This is the first time that the bar rotation rate is coupled to fDM, bar derived from dynamical modelling.

Published
2023
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6. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author

Jin, Shoko, primary, Trager, Scott C, additional, Dalton, Gavin B, additional, Aguerri, J Alfonso L, additional, Drew, J E, additional, Falcón-Barroso, Jesús, additional, Gänsicke, Boris T, additional, Hill, Vanessa, additional, Iovino, Angela, additional, Pieri, Matthew M, additional, Poggianti, Bianca M, additional, Smith, D J B, additional, Vallenari, Antonella, additional, Abrams, Don Carlos, additional, Aguado, David S, additional, Antoja, Teresa, additional, Aragón-Salamanca, Alfonso, additional, Ascasibar, Yago, additional, Babusiaux, Carine, additional, Balcells, Marc, additional, Barrena, R, additional, Battaglia, Giuseppina, additional, Belokurov, Vasily, additional, Bensby, Thomas, additional, Bonifacio, Piercarlo, additional, Bragaglia, Angela, additional, Carrasco, Esperanza, additional, Carrera, Ricardo, additional, Cornwell, Daniel J, additional, Domínguez-Palmero, Lilian, additional, Duncan, Kenneth J, additional, Famaey, Benoit, additional, Fari na, Cecilia, additional, Gonzalez, Oscar A, additional, Guest, Steve, additional, Hatch, Nina A, additional, Hess, Kelley M, additional, Hoskin, Matthew J, additional, Irwin, Mike, additional, Knapen, Johan H, additional, Koposov, Sergey E, additional, Kuchner, Ulrike, additional, Laigle, Clotilde, additional, Lewis, Jim, additional, Longhetti, Marcella, additional, Lucatello, Sara, additional, Méndez-Abreu, Jairo, additional, Mercurio, Amata, additional, Molaeinezhad, Alireza, additional, Monguió, Maria, additional, Morrison, Sean, additional, Murphy, David N A, additional, de Arriba, Luis Peralta, additional, Pérez, Isabel, additional, Pérez-Ràfols, Ignasi, additional, Picó, Sergio, additional, Raddi, Roberto, additional, Romero-Gómez, Mercè, additional, Royer, Frédéric, additional, Siebert, Arnaud, additional, Seabroke, George M, additional, Som, Debopam, additional, Terrett, David, additional, Thomas, Guillaume, additional, Wesson, Roger, additional, Worley, C Clare, additional, Alfaro, Emilio J, additional, Prieto, Carlos Allende, additional, Alonso-Santiago, Javier, additional, Amos, Nicholas J, additional, Ashley, Richard P, additional, Balaguer-Nú nez, Lola, additional, Balbinot, Eduardo, additional, Bellazzini, Michele, additional, Benn, Chris R, additional, Berlanas, Sara R, additional, Bernard, Edouard J, additional, Best, Philip, additional, Bettoni, Daniela, additional, Bianco, Andrea, additional, Bishop, Georgia, additional, Blomqvist, Michael, additional, Boeche, Corrado, additional, Bolzonella, Micol, additional, Bonoli, Silvia, additional, Bosma, Albert, additional, Britavskiy, Nikolay, additional, Busarello, Gianni, additional, Caffau, Elisabetta, additional, Cantat-Gaudin, Tristan, additional, Castro-Ginard, Alfred, additional, Couto, Guilherme, additional, Carbajo-Hijarrubia, Juan, additional, Carter, David, additional, Casamiquela, Laia, additional, Conrado, Ana M, additional, Corcho-Caballero, Pablo, additional, Costantin, Luca, additional, Deason, Alis, additional, de Burgos, Abel, additional, De Grandi, Sabrina, additional, Di Matteo, Paola, additional, Domínguez-Gómez, Jesús, additional, Dorda, Ricardo, additional, Drake, Alyssa, additional, Dutta, Rajeshwari, additional, Erkal, Denis, additional, Feltzing, Sofia, additional, Ferré-Mateu, Anna, additional, Feuillet, Diane, additional, Figueras, Francesca, additional, Fossati, Matteo, additional, Franciosini, Elena, additional, Frasca, Antonio, additional, Fumagalli, Michele, additional, Gallazzi, Anna, additional, García-Benito, Rubén, additional, Fusillo, Nicola Gentile, additional, Gebran, Marwan, additional, Gilbert, James, additional, Gledhill, T M, additional, Delgado, Rosa M González, additional, Greimel, Robert, additional, Guarcello, Mario Giuseppe, additional, Guerra, Jose, additional, Gullieuszik, Marco, additional, Haines, Christopher P, additional, Hardcastle, Martin J, additional, Harris, Amy, additional, Haywood, Misha, additional, Helmi, Amina, additional, Hernandez, Nauzet, additional, Herrero, Artemio, additional, Hughes, Sarah, additional, Irsic, Vid, additional, Jablonka, Pascale, additional, Jarvis, Matt J, additional, Jordi, Carme, additional, Kondapally, Rohit, additional, Kordopatis, Georges, additional, Krogager, Jens-Kristian, additional, Barbera, Francesco La, additional, Lam, Man I, additional, Larsen, Søren S, additional, Lemasle, Bertrand, additional, Lewis, Ian J, additional, Lhomé, Emilie, additional, Lind, Karin, additional, Lodi, Marcello, additional, Longobardi, Alessia, additional, Lonoce, Ilaria, additional, Magrini, Laura, additional, Apellániz, Jesús Maíz, additional, Marchal, Olivier, additional, Marco, Amparo, additional, Martin, Nicolas F, additional, Matsuno, Tadafumi, additional, Maurogordato, Sophie, additional, Merluzzi, Paola, additional, Miralda-Escudé, Jordi, additional, Molinari, Emilio, additional, Monari, Giacomo, additional, Morelli, Lorenzo, additional, Mottram, Christopher J, additional, Naylor, Tim, additional, Negueruela, Ignacio, additional, Onorbe, Jose, additional, Pancino, Elena, additional, Peirani, Sébastien, additional, Peletier, Reynier F, additional, Pozzetti, Lucia, additional, Rainer, Monica, additional, Ramos, Pau, additional, Read, Shaun C, additional, Rossi, Elena Maria, additional, Röttgering, Huub J A, additional, Rubi no-Martín, Jose Alberto, additional, Montes, Jose Sabater, additional, Juan, José San, additional, Sanna, Nicoletta, additional, Schallig, Ellen, additional, Schiavon, Ricardo P, additional, Schultheis, Mathias, additional, Serra, Paolo, additional, Shimwell, Timothy W, additional, Simón-Díaz, Sergio, additional, Smith, Russell J, additional, Sordo, Rosanna, additional, Sorini, Daniele, additional, Soubiran, Caroline, additional, Starkenburg, Else, additional, Steele, Iain A, additional, Stott, John, additional, Stuik, Remko, additional, Tolstoy, Eline, additional, Tortora, Crescenzo, additional, Tsantaki, Maria, additional, Van der Swaelmen, Mathieu, additional, van Weeren, Reinout J, additional, Vergani, Daniela, additional, Verheijen, Marc A W, additional, Verro, Kristiina, additional, Vink, Jorick S, additional, Vioque, Miguel, additional, Walcher, C Jakob, additional, Walton, Nicholas A, additional, Wegg, Christopher, additional, Weijmans, Anne-Marie, additional, Williams, Wendy L, additional, Wilson, Andrew J, additional, Wright, Nicholas J, additional, Xylakis-Dornbusch, Theodora, additional, Youakim, Kris, additional, Zibetti, Stefano, additional, and Zurita, Cristina, additional

Published
2023
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9. Differential attenuation in star-forming galaxies at 0.3 ≲ z ≲ 1.5 in the SHARDS/CANDELS field

Author

Rodríguez-Muñoz, L, primary, Rodighiero, G, additional, Pérez-González, P G, additional, Talia, M, additional, Baronchelli, I, additional, Morselli, L, additional, Renzini, A, additional, Puglisi, A, additional, Grazian, A, additional, Zanella, A, additional, Mancini, C, additional, Feltre, A, additional, Romano, M, additional, Vidal García, A, additional, Franceschini, A, additional, Alcalde Pampliega, B, additional, Cassata, P, additional, Costantin, L, additional, Domínguez Sánchez, H, additional, Espino-Briones, N, additional, Iani, E, additional, Koekemoer, A, additional, Lumbreras-Calle, A, additional, and Rodríguez-Espinosa, J M, additional

Published
2021
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12. Erratum: Deconstructing double-barred galaxies in 2D and 3D. I. Classical nature of the dominant bulges

Author

B. Thorne, L. Costantin, A. de Lorenzo-Cáceres, and J. Mendez-Abreu

Subjects
Physics, Space and Planetary Science, Bulge, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Table (information), Astrophysics::Galaxy Astrophysics, Galaxy
Abstract

This is an Erratum for the paper Deconstructing double-barred galaxies in 2D and 3D. I. Classical nature of the dominant bulges (2019, MNRAS, 484, 665), where we presented two-dimensional multi-component photometric decompositions of a sample of 17 double-barred galaxies, as well as statistical three-dimensional deprojections of their bulges, inner bars, and outer bars. We have detected a bug in the code used to create the tables with the results of the photometric decompositions. Due to this bug, the photometric parameters for the bars of nine galaxies listed in Tables A1- A8 of the original paper are not correct: The inner bars in NGC357, NGC718, NGC2950, NGC2962, NGC3941, NGC3945, NGC4503, and the inner and outer bars in NGC2681 and NGC4725. Our subsequent calculations of the contribution of each structure (bulge, bars, disc) to the total galaxy light and the three-dimensional deprojections of the bars are also affected. Tables 1 to 9 in this Erratum show the correct parameters for all galaxies, and therefore they should be used instead of Table 2 and tables A1-A8 of the original paper.

Published
2019
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18. Morpho-kinematic properties of field S0 bulges in the CALIFA survey

Author

Méndez-Abreu, J., primary, Aguerri, J. A. L., additional, Falcón-Barroso, J., additional, Ruiz-Lara, T., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Catalán-Torrecilla, C., additional, Zhu, L., additional, Sánchez-Blazquez, P., additional, Florido, E., additional, Corsini, E. M., additional, Wild, V., additional, Lyubenova, M., additional, van de Ven, G., additional, Sánchez, S. F., additional, Bland-Hawthorn, J., additional, Galbany, L., additional, García-Benito, R., additional, García-Lorenzo, B., additional, Delgado, R. M. González, additional, López-Sánchez, A. R., additional, Marino, R. A., additional, Márquez, I., additional, Ziegler, B., additional, and collaboration, the CALIFA, additional

Published
2017
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19. Towards a new classification of galaxies: principal component analysis of CALIFA circular velocity curves

Author

Kalinova, V., primary, Colombo, D., additional, Rosolowsky, E., additional, Kannan, R., additional, Galbany, L., additional, García-Benito, R., additional, González Delgado, R., additional, Sánchez, S. F., additional, Ruiz-Lara, T., additional, Méndez-Abreu, J., additional, Catalán-Torrecilla, C., additional, Sánchez-Menguiano, L., additional, de Lorenzo-Cáceres, A., additional, Costantin, L., additional, Florido, E., additional, Kodaira, K., additional, Marino, R. A., additional, Läsker, R., additional, and Bland-Hawthorn, J., additional

Published
2017
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