Evolution of infrared luminosity functions of galaxies in the AKARI NEP-deep field - Revealing the cosmic star formation history hidden by dust
Evolution of infrared luminosity functions of galaxies in the AKARI NEP-deep field - Revealing the cosmic star formation history hidden by dust
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DOI：
10.1051/0004-6361/200913182
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发表时间：
2009-12
影响因子：
6.5
通讯作者：
T. Goto;T. Takagi;H. Matsuhara;T. Takeuchi;C. Pearson;C. Pearson;C. Pearson;T. Wada;T. Nakagawa;O. Ilbert;E. Floc’h;S. Oyabu;Y. Ohyama;M. Malkan;Ho-Gyu Lee;M. Lee;H. Inami;H. Inami;H. Inami;N. Hwang;H. Hanami;M. Im;K. Imai;T. Ishigaki;S. Serjeant;H. Shim
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作者：
T. Goto;T. Takagi;H. Matsuhara;T. Takeuchi;C. Pearson;C. Pearson;C. Pearson;T. Wada;T. Nakagawa;O. Ilbert;E. Floc’h;S. Oyabu;Y. Ohyama;M. Malkan;Ho-Gyu Lee;M. Lee;H. Inami;H. Inami;H. Inami;N. Hwang;H. Hanami;M. Im;K. Imai;T. Ishigaki;S. Serjeant;H. Shim
目标。尘埃遮蔽的恒星形成随着强度和红移的增加而增加。我们的目标是使用AKARI的深红外观测来揭示被尘埃掩盖的宇宙恒星形成历史。方法.我们使用AKARI NEP深场中的4128个红外源构建了0.15 < z < 2.2处的restframe 8 μm、12 μm和全红外（TIR）光度函数（LF）。AKARI卫星在中红外波长（2.4、3.2、4.1、7、9、11、15、18和24 μm）的连续滤光片覆盖范围使我们能够估计restframe 8 μm和12 μm的光度，而无需使用基于SED拟合的大外推，这是以前工作中最大的不确定性。结果我们发现所有8 μm（0.38 < z < 2.2）、12 μm（0.15 < z < 1.16）和TIR LF（0.2 < z < 1.6）都表现出向更高红移的连续和强烈的演化。我们对8 μm LF的直接估计是有用的，因为以前的工作通常必须使用从Spitzer 24 μm到8 μm的大的外推，其中由于PAH排放，SED建模更加困难。在z < 1.2时，我们用解析拟合积分得到的宇宙红外光度密度（Ω_（IR））与前人的工作符合得很好。我们发现ΩIR的演化为<$（1 + z）^（4.4±1.0）。当我们分开LIRGs和ULIRG对Ω_（IR）的贡献时，我们发现在更高的红移下，更多的红外光源越来越重要。我们发现，ULIRG（LIRG）的贡献增加了10（1.8）倍，从z = 0.35到z = 1.4。
Aims. Dust-obscured star-formation increases with increasing intensity and increasing redshift. We aim to reveal the cosmic starformation history obscured by dust using deep infrared observation with AKARI. Methods. We constructed restframe 8 μm, 12 μm, and total infrared (TIR) luminosity functions (LFs) at 0.15 < z < 2.2 using 4128 infrared sources in the AKARI NEP-deep field. A continuous filter coverage in the mid-IR wavelength (2.4, 3.2, 4.1, 7, 9, 11, 15, 18, and 24 μm) by the AKARI satellite allowed us to estimate restframe 8 μm and 12 μm luminosities without using a large extrapolation based on an SED fit, which was the largest uncertainty in previous work. Results. We find that all 8 μm (0.38 < z < 2.2), 12 μm (0.15 < z < 1.16), and TIR LFs (0.2 < z < 1.6) show continuous and strong evolution toward higher redshift. Our direct estimate of 8 μm LFs is useful since previous work often had to use a large extrapolation from the Spitzer 24 μm to 8 μm, where SED modeling is more difficult because of the PAH emissions. In terms of cosmic infrared luminosity density (Ω_(IR)), which was obtained by integrating analytic fits to the LFs, we find good agreement with previous work at z < 1.2. We find the ΩIR evolves as ∝(1 + z)^(4.4±1.0). When we separate contributions to Ω_(IR) by LIRGs and ULIRGs, we found more IR luminous sources are increasingly more important at higher redshift. We find that the ULIRG (LIRG) contribution increases by a factor of 10 (1.8) from z = 0.35 to z = 1.4.