Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer
Evolution of the dusty infrared luminosity function from z = 0 to z = 2.3 using observations from Spitzer
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DOI：
10.1051/0004-6361/200913941
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发表时间：
2011-01
影响因子：
6.5
通讯作者：
B. Magnelli;D. Elbaz;R. Chary;M. Dickinson;D. L. Borgne;D. Frayer;C. Willmer
中科院分区：
文献类型：
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作者：
B. Magnelli;D. Elbaz;R. Chary;M. Dickinson;D. L. Borgne;D. Frayer;C. Willmer
目标。利用GOODS南北场24 μ m和70 μ m深像，导出了宇宙时间最后4/5的红外光度函数（LF）的演化。方法.我们使用了一种基于较短波长的先验源位置的提取技术来建立24和70 μ m源目录。大多数（93%）光源具有光谱红移（39%）或光度红移（54%），并且在我们感兴趣的红移范围内（即，1.3<z <2.3）~20%的源具有光谱红移。为了将我们的研究扩展到70 μ m以下，我们进行了叠加分析，并描述了所观察到的L_（24/（1 + z））与L_（70/（1 + z））的相关性。利用光谱能量分布（SED）模板，我们从24和70 μ m的亮度中得到了各个光源的红外光度。然后，我们计算在z~1.55 ± 0.25和z~2.05 ± 0.25处的红外LF。结果我们观察到在红外LF到z~2.3的中断。红外LF从z = 1.3到z = 2.3的红移演化与光度演化成正比于（1 + z）^（1.0 ± 0.9）以及密度演化成正比于（1 + z）^（9 − 1.1 ± 1.5）相一致。在z~2处，亮红外星系（LIRGs：10 ^（11）L_∞ <L_（IR）<10 ^（12）L_∞）仍然是宇宙共动红外光度密度的主要贡献者。在z~2处，LIRGs和超亮红外星系（ULIRGs：10 ^（12）L_（12）L_（12）<L_（IR））分别约占宇宙共动红外光度密度的49%和17%。结合以前对z <1.3的星系采用相同策略的结果，并假设星系的红外光度和恒星形成率（SFR）之间的转换是常数，我们研究了宇宙SFR密度从z = 0到z = 2.3的演化。我们发现宇宙的SFR密度随着红移从z = 0到z = 1.3而强烈增加，但在更高的红移到z = 2.3时几乎是恒定的。作为本文附带的在线资料的一部分，我们提供了GOODS南北场24 μ m和70 μ m的源目录。
Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ~20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L_(24/(1 + z)) vs. L_(70/(1 + z)) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ~ 1.55 ± 0.25 and z ~ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ~ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z)^(1.0 ± 0.9) combined with a density evolution proportional to (1 + z)^9−1.1 ± 1.5). At z ~ 2, luminous infrared galaxies (LIRGs: 10^(11)L_⊙ < L_(IR) < 10^(12) L_⊙) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ~ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10^(12)L_⊙ < L_(IR)) account for ~49% and ~17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.