| Texto completo | |
| Autor(es): Mostrar menos - |
Delgado, R. M. Gonzalez
[1]
;
Diaz-Garcia, L. A.
[1, 2]
;
de Amorim, A.
[3]
;
Bruzual, G.
[4]
;
Fernandes, R. Cid
[3]
;
Perez, E.
[1]
;
Bonoli, S.
[5, 6, 7]
;
Cenarro, A. J.
[7]
;
Coelho, P. R. T.
[8]
;
Cortesi, A.
[9]
;
Garcia-Benito, R.
[1]
;
Fernandez, R. Lopez
[1]
;
Martinez-Solaeche, G.
[1]
;
Rodriguez-Martin, J. E.
[1]
;
Magris, G.
[10]
;
Mejia-Narvaez, A.
[11]
;
Brito-Silva, D.
[12]
;
Abramo, L. R.
[13]
;
Diego, J. M.
[14]
;
Dupke, R. A.
[15, 16, 17]
;
Hernan-Caballero, A.
[7]
;
Hernandez-Monteagudo, C.
[7, 18, 19]
;
Lopez-Sanjuan, C.
[7]
;
Marin-Franch, A.
[7]
;
Marra, V
[20, 21, 22, 23]
;
Moles, M.
[1, 7]
;
Montero-Dorta, A.
[13, 24]
;
Queiroz, C.
[13]
;
Sodre, Jr., L.
[8]
;
Varela, J.
[7]
;
Ramio, H. Vazquez
[7]
;
Vilchez, J. M.
[1]
;
Baqui, P. O.
[20, 23]
;
Benitez, N.
[1]
;
Cristobal-Hornillos, D.
[7]
;
Ederoclite, A.
[8]
;
de Oliveira, C. Mendes
[8]
;
Civera, T.
[25]
;
Muniesa, D.
[25]
;
Taylor, K.
[8]
;
Tempel, E.
[26]
;
Collaboration, J-PAS
Número total de Autores: 42
|
| Afiliação do(s) autor(es): Mostrar menos - | [1] Inst Astrofis Andalucia CSIC, POB 3004, Granada 18080 - Spain
[2] Acad Sinica Inst Astron & Astrophys ASIAA, 1, Sect 4, Roosevelt Rd, Taipei 10617 - Taiwan
[3] Univ Fed Santa Catarina, Dept Fis, POB 476, BR-88040900 Florianopolis, SC - Brazil
[4] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis IRyA, Campus Morelia, Morelia 58089, Michoacan - Mexico
[5] Basque Fdn Sci, Ikerbasque, Bilbao 48013 - Spain
[6] Donostia Int Phys Ctr DIPC, Manuel Lardizabal Ibilbidea 4, San Sebastian - Spain
[7] Unidad Asociada CSIC, Ctr Estudios Fis Cosmos Aragon CEFCA, Plaza San Juan 1, Teruel 44001 - Spain
[8] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, R Matao 1226, BR-05508090 Sao Paulo - Brazil
[9] Univ Fed Rio de Janeiro, Observ Valongo, BR-20080090 Rio de Janeiro, RJ - Brazil
[10] Ctr Invest Astron CIDA, AP 264, Merida 5101 - Venezuela
[11] Univ Nacl Autonoma Mexico, Inst Astron, AP 70-264, Mexico City 04510, Cdmx - Mexico
[12] Univ Diego Portales, Nucleo Astron, Av Ejercito Libertador 441, Santiago, Region Metropol - Chile
[13] Univ Sao Paulo, Inst Fis, Rua Matao 1371, BR-05508090 Sao Paulo - Brazil
[14] Inst Fis Cantabria CSIC UC, Avda Los Castros S-N, Santander 39005 - Spain
[15] Univ Alabama, Dept Phys & Astron, Box 870324, Tuscaloosa, AL 35487 - USA
[16] Univ Michigan, Dept Astron, 311 West Hall, 1085 South Univ Ave, Ann Arbor, MI 48109 - USA
[17] Minist Ciencia Tecnol Inovacao & Comunicacoes, Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro - Brazil
[18] Inst Astrofis Canarias, Calle Via Lactea S-N, San Cristobal la Laguna 38205 - Spain
[19] Univ La Laguna, Dept Astrofis, San Cristobal la Laguna 38205 - Spain
[20] Univ Fed Espirito Santo, Dept Fis, BR-29075910 Vitoria, ES - Brazil
[21] INAF Osservatorio Astron Trieste, Via Tiepolo 11, I-34131 Trieste - Italy
[22] IFPU Inst Fundamental Phys Universe, Via Beirut 2, I-34151 Trieste - Italy
[23] Univ Fed Espirito Santo, PPGCosmo, Nucleo Astrofis & Cosmol, BR-29075910 Vitoria, ES - Brazil
[24] Univ Tecn Federico Santa Maria, Fis, Avda Espana 1680, Casilla 110, Valparaiso - Chile
[25] Ctr Estudios Fis Cosmos Aragon CEFCA, Plaza San Juan 1, Teruel 44001 - Spain
[26] Univ Tartu, Tartu Observ, Observ 1, EE-61602 Toravere - Estonia
Número total de Afiliações: 26
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Astronomy & Astrophysics; v. 649, MAY 13 2021. |
| Citações Web of Science: | 0 |
| Resumo | |
The Javalambre-Physics of the Accelerating Universe Astrophysical Survey (J-PAS) will soon start imaging thousands of square degrees of the northern sky with its unique set of 56 filters (spectral resolution of R similar to 60). Before the arrival of the final instrument, we observed 1 deg(2) on the AEGIS field with an interim camera with all the J-PAS filters. Taking advantage of these data, dubbed miniJPAS, we aim at proving the scientific potential of the J-PAS to derive the stellar population properties of galaxies via fitting codes for spectral energy distributions (SEDs), with the ultimate goal of performing galaxy evolution studies across cosmic time. One parametric (BaySeAGal) and three non-parametric (MUFFIT, AlStar, and TGASPEX) SED-fitting codes are used to constrain the stellar mass, age, metallicity, extinction, and rest-frame and dust-corrected (u-r) colours of a complete flux-limited sample (r(SDSS) <= 22.5 AB) of miniJPAS galaxies that extends up to z=1. We generally find consistent results on the galaxy properties derived from the different codes, independently of the galaxy spectral type or redshift; this is remarkable considering that 25% of the J-spectra have signal-to-noise ratios (S/N) similar to 3. For galaxies with S/N >= 10, we estimate that the J-PAS photometric system will allow us to derive the stellar population properties of rest-frame (u-r) colour, stellar mass, extinction, and mass-weighted age with a precision of 0.04 +/- 0.02 mag, 0.07 +/- 0.03 dex, 0.2 +/- 0.09 mag, and 0.16 +/- 0.07 dex, respectively. This precision is equivalent to that obtained with spectroscopic surveys of similar S/N. By using the dust-corrected (u-r) colour-mass diagram, a powerful proxy for characterizing galaxy populations, we find: (i) that the fraction of red and blue galaxies evolves with cosmic time, with red galaxies being similar to 38% and similar to 18% of the whole population at z=0.1 and z=0.5, respectively, and (ii) consistent results between codes for the average intrinsic (u-r) colour, stellar mass, age, and stellar metallicity of blue and red galaxies and their evolution up to z=1. At all redshifts, the more massive galaxies belong to the red sequence, and these galaxies are typically older and more metal-rich than their counterparts in the blue cloud. Our results confirm that with J-PAS data we will be able to analyse large samples of galaxies up to z similar to 1, with galaxy stellar masses above log(M-star/M-circle dot)similar to 8.9, 9.5, and 9.9 at z=0.3, 0.5, and 0.7, respectively. The star formation history of a complete sub-sample of galaxies selected at z similar to 0.1 with log(M-star/M-circle dot) > 8.3 constrains the cosmic evolution of the star formation rate density up to z similar to 3, in good agreement with results from cosmological surveys. (AU) | |
| Processo FAPESP: | 18/05392-8 - Uma nova biblioteca de modelos de população estelar puramente teóricos |
| Beneficiário: | Paula Rodrigues Teixeira Coelho |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |
| Processo FAPESP: | 19/10923-5 - Ferramentas de inteligência artificial para grandes levantamentos de galáxias |
| Beneficiário: | Laerte Sodré Junior |
| Modalidade de apoio: | Auxílio à Pesquisa - Regular |