Linking Stellar Mass and Star Formation in Spitzer MIPS 24 μm Galaxies
Linking Stellar Mass and Star Formation in Spitzer MIPS 24 μm Galaxies
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将斯皮策 MIPS 24 μm 星系中的恒星质量与恒星形成联系起来
DOI：
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发表时间：
2005
期刊：
影响因子：
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通讯作者：
P. Pérez
中科院分区：
文献类型：
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作者：
K. Caputi;H. Dole;G. Lagache;R. McLure;J. Puget;G. Rieke;J. Dunlop;E. Floc’h;C. Papovich;P. Pérez
我们给出了在GOODS/CDFS中构成大部分24 μm背景的大多数源的深k < 21.5（织女星）识别、红移和恒星质量。我们鉴定的样品由747个Spitzer MIPS 24 μm天体组成，其中包括GOODS-South场中通量为Sν(24 μm) > 83 μJy的24 μm源的~94% （Spitzer/GTO 24 μm目录的~80%完备性极限）；36%的星系具有光谱红移（大部分在z < 1.5），其余的星系具有非常好的光度红移质量，中位数为|dz| = |zspec - zphot|/(1 + zspec) = 0.02。我们发现MIPS 24 μm星系的红移范围为z ~ 0 ~ 4，其中28%的星系位于高红移z ~ 1.5。我们确定在z ~ 1.9的红移分布中存在一个凸起，表明在这些红移处存在大量具有多环芳烃发射的星系。24 μm星系群的范围从中等光度（1010 L☉< LIR < 1011 L☉）和低到中等组合恒星质量（109 M☉≤M≤1011 M☉）的来源，到红移z ~ 2-3的大质量（M≥1011 M☉）超亮星系（LIR > 1012 L☉）。红移2 > z > 3的大质量恒星形成星系具有非常高的恒星形成速率（SFR > 500 M☉y -1），其中一些星系能够在一次爆发寿命（~0.01-0.1 Gyr）内形成≈1010-1011 M☉的质量。在较低的红移z > 2处，也存在大质量的恒星形成星系，但它们似乎是在很长的时间尺度上，或者是静止的，或者是在多次适度的爆发中形成恒星。在红移z ~ 1-2处，类暴模式在单个事件中产生整个星系的能力被限制在一些较低质量（M≤7 × 1010 M☉）的系统中，并且在z≤1时基本上可以忽略不计。我们的结果支持这样一种假设：恒星的形成活动与聚集的恒星质量和红移是不同的，而爆发模式的相对重要性从高红移到低红移的过程是缩小的。
We present deep Ks < 21.5 (Vega) identifications, redshifts, and stellar masses for most of the sources composing the bulk of the 24 μm background in the GOODS/CDFS. Our identified sample consists of 747 Spitzer MIPS 24 μm objects and includes ~94% of all the 24 μm sources in the GOODS-South field that have fluxes Sν(24 μm) > 83 μJy (the ~80% completeness limit of the Spitzer/GTO 24 μm catalog); 36% of our galaxies have spectroscopic redshifts (mostly at z < 1.5), and the remaining ones have photometric redshifts of very good quality, with a median of |dz| = |zspec - zphot|/(1 + zspec) = 0.02. We find that MIPS 24 μm galaxies span the redshift range z ~ 0-4 and that a substantial fraction (28%) lie at high redshifts z ≳ 1.5. We determine the existence of a bump in the redshift distribution at z ~ 1.9, indicating the presence of a significant population of galaxies with PAH emission at these redshifts. The 24 μm galaxy population ranges from sources with intermediate luminosities (1010 L☉ < LIR < 1011 L☉) and low-to-intermediate assembled stellar masses (109 M☉ ≲ M ≲ 1011 M☉) at z ≲ 0.8, to massive (M ≳ 1011 M☉) hyperluminous galaxies (LIR > 1012 L☉) at redshifts z ~ 2-3. Massive star-forming galaxies at redshifts 2 ≲ z ≲ 3 are characterized by very high star formation rates (SFR > 500 M☉ yr-1), and some of them are able to construct a mass of ≈1010-1011 M☉ in a single burst lifetime (~0.01-0.1 Gyr). At lower redshifts z ≲ 2, massive star-forming galaxies are also present but appear to be building their stars on long timescales, either quiescently or in multiple modest burstlike episodes. At redshifts z ~ 1-2, the ability of the burstlike mode to produce entire galaxies in a single event is limited to some lower (M ≲ 7 × 1010 M☉) mass systems, and it is basically negligible at z ≲ 1. Our results support a scenario in which star formation activity is differential with assembled stellar mass and redshift, and where the relative importance of the burstlike mode proceeds in a downsizing way from high to low redshifts.
z ~ 2 8 处两个发光亚毫米星系的中红外光谱
DOI：
10.1086/431217
发表时间：
2005
期刊：
The Astrophysical Journal Letters
影响因子：
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作者：
Valiante;Genzel;Tacconi;Lehnert
通讯作者：
Lehnert