AMAZE -: I.: The evolution of the mass-metallicity relation at z>3

被引：875

作者：

Maiolino, R. ^{[1
]}

Nagao, T. ^{[2
]}

Grazian, A. ^{[1
]}

Cocchia, F. ^{[1
]}

Marconi, A. ^{[3
]}

Mannucci, F. ^{[4
]}

Cimatti, A. ^{[5
]}

Pipino, A. ^{[6
]}

Ballero, S. ^{[7
]}

Calura, F. ^{[7
]}

Chiappini, C. ^{[10
,11
]}

Fontana, A. ^{[1
]}

Granato, G. L. ^{[8
]}

Matteucci, F. ^{[7
]}

Pastorini, G. ^{[3
]}

Pentericci, L.

Risaliti, G. ^{[9
]}

Salvati, M. ^{[9
]}

Silva, L. ^{[10
]}

机构：

[1] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[2] Natl Inst Nat Sci, Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan

[3] Univ Florence, Dipartimento Astron, I-50125 Florence, Italy

[4] INAF Ist Radioastron, I-50125 Florence, Italy

[5] Univ Bologna, Dipartimento Astron, I-40127 Bologna, Italy

[6] Univ Oxford, Oxford OX1 3RH, England

[7] Univ Trieste, Dipartimento Astron, I-34131 Trieste, Italy

[8] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[9] INAF Osservatorio Astrofis Arcetri, I-50125 Florence, Italy

[10] INAF Osservatorio Astron Trieste, I-34131 Trieste, Italy

[11] Univ Geneva, Observ Geneva, CH-1290 Sauverny, Switzerland

来源：

ASTRONOMY & ASTROPHYSICS | 2008年 / 488卷 / 02期

关键词：

ISM : abundances; galaxies : abundances; galaxies : evolution; galaxies : high-redshift; galaxies : starburst;

D O I：

10.1051/0004-6361:200809678

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We present initial results of an ESO-VLT large programme (AMAZE) aimed at determining the evolution of the mass-metallicity relation at z > 3 by means of deep near-IR spectroscopy. Gas metallicities are measured, for an initial sample of nine star forming galaxies at z similar to 3.5, by means of optical nebular lines redshifted into the near-IR. Stellar masses are accurately determined by using Spitzer-IRAC data, which sample the rest-frame near-IR stellar light in these distant galaxies. When compared with previous surveys, the mass-metallicity relation inferred at z similar to 3.5 shows an evolution much stronger than observed at lower redshifts. The evolution is prominent even in massive galaxies, indicating that z similar to 3 is an epoch of major action in terms of star formation and metal enrichment also for massive systems. There are also indications that the metallicity evolution of low mass galaxies is stronger relative to high mass systems, an effect which can be considered the chemical version of the galaxy downsizing. The mass-metallicity relation observed at z similar to 3.5 is difficult to reconcile with the predictions of some hierarchical evolutionary models. Such discrepancies suggest that at z > 3 galaxies are assembled mostly with relatively un-evolved sub-units, i.e. small galaxies with low star formation efficiency. The bulk of the star formation and metallicity evolution probably occurs once small galaxies are already assembled into bigger systems.

引用

页码：463 / 479

页数：17

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AMAZE -: I.: The evolution of the mass-metallicity relation at z&gt;3

AMAZE -: I.: The evolution of the mass-metallicity relation at z>3