| Texto completo | |
| Autor(es): Mostrar menos - |
Niemiec, A.
[1]
;
Jullo, E.
[1]
;
Montero-Dorta, A. D.
[2]
;
Prada, F.
[3]
;
Rodriguez-Torres, S.
[4]
;
Perez, E.
[3]
;
Klypin, A.
[5]
;
Erben, T.
[6]
;
Makler, M.
[7]
;
Moraes, B.
[8]
;
Pereira, M. E. S.
[9]
;
Shan, H.
[6]
Número total de Autores: 12
|
| Afiliação do(s) autor(es): | [1] Aix Marseille Univ, LAM, CNRS, F-13388 Marseille - France
[2] Univ Sao Paulo, Dept Fis Matemat, Inst Fis, Rua Matao 1371, BR-05508090 Sao Paulo - Brazil
[3] CSIC, Inst Astrofis Andalucia, Glorieta Astron, E-18080 Granada - Spain
[4] Univ Autonoma Madrid, Dept Fis Teor, E-28049 Madrid - Spain
[5] New Mexico State Univ, Dept Astron, Las Cruces, NM 88003 - USA
[6] Argelander Inst Astron, Hugel 71, D-53121 Bonn - Germany
[7] Ctr Brasileiro Pesquisas Fis, Rua Dr Xavier Sigaud 150, BR-22290180 Rio De Janeiro, RJ - Brazil
[8] UCL, Dept Phys & Astron, London WC1E 6BT - England
[9] Brandeis Univ, 415 South St, Waltham, MA 02453 - USA
Número total de Afiliações: 9
|
| Tipo de documento: | Artigo Científico |
| Fonte: | Monthly Notices of the Royal Astronomical Society; v. 477, n. 1, p. L1-L5, JUN 2018. |
| Citações Web of Science: | 4 |
| Resumo | |
In Montero-Dorta et al., we show that luminous red galaxies (LRGs) from the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS) at z similar to 0.55 can be divided into two groups based on their star formation histories. So-called fast-growing LRGs assemble 80 per cent of their stellar mass at z similar to 5, whereas slow-growing LRGs reach the same evolutionary state at z similar to 1.5. We further demonstrate that these two subpopulations present significantly different clustering properties on scales of similar to 1-30 Mpc. Here, we measure the mean halo mass of each subsample using the galaxy-galaxy lensing technique, in the similar to 190 deg(2) overlap of the LRG catalogue and the CS82 and CFHTLenS shear catalogues. We show that fast- and slow-growing LRGs have similar lensing profiles, which implies that they live in haloes of similar mass: log(M-halo(fast)/h(-1)M(circle dot)) = 12.85(-0.26)(+0.16) and log(M-halo(slow)/h(-1)M(circle dot)) = 12.92(-0.22)(+0.16). This result, combined with the clustering difference, suggests the existence of galaxy assembly bias, although the effect is too subtle to be definitively proven, given the errors on our current weak-lensing measurement. We show that this can soon be achieved with upcoming surveys like DES. (AU) | |
| Processo FAPESP: | 16/23567-4 - Unificando evolução de galáxias e cosmologia com os grandes levantamentos astrofísicos |
| Beneficiário: | Antonio David Montero Dorta |
| Modalidade de apoio: | Bolsas no Brasil - Pós-Doutorado |