Infrared luminosity functions of AKARI Sloan Digital Sky Survey galaxies
Infrared luminosity functions of AKARI Sloan Digital Sky Survey galaxies
复制标题
DOI：
10.1111/j.1365-2966.2011.18499.x
复制
发表时间：
2011-02
影响因子：
4.8
通讯作者：
T. Goto;S. Arnouts;Matthew Malkan Toshinobu Takagi;H. Inami;C. Pearson;T. Wada;H. Matsuhara;C. Yamauchi;T. Takeuchi;T. Nakagawa;S. Oyabu;D. Ishihara;D. Sanders;E. Floc’h;Hyung-Mok Lee;W. Jeong;S. Serjeant;C. Sedgwick
中科院分区：
文献类型：
--
作者：
T. Goto;S. Arnouts;Matthew Malkan Toshinobu Takagi;H. Inami;C. Pearson;T. Wada;H. Matsuhara;C. Yamauchi;T. Takeuchi;T. Nakagawa;S. Oyabu;D. Ishihara;D. Sanders;E. Floc’h;Hyung-Mok Lee;W. Jeong;S. Serjeant;C. Sedgwick
通过将阿卡里全天巡天在6个红外(IR)波段(9，18，65，90,140和160μm)与斯隆数字巡天星系进行交叉关联，我们识别了2,357个具有光谱红移的IR星系。这不仅是最大的本地IR星系样本之一，而且AKARI提供了重要的远红外(FIR)波段，用于精确测量星系在>；100μm尘埃发射峰值上的光谱能量分布。通过将现代IR光谱能量分布模型与AKARI光度法相匹配，我们测量了单个星系的总红外光度(L IR)。利用这个L红外，我们构造了红移中值为z=0.031的红外星系的光度函数(LF)。Lf与z=0.0082(修正后的亮星系样本)时的结果吻合得很好，显示出在阿卡里北黄道极(NEP)深场测量到的向更高红移LFS平滑和持续的演化。通过对L加权的红外低频积分，我们测量了Ω_(IR_=(3.8^(+5.8)_(−1.2))×10^8 L_⊙Mpc^(−3)的局域宇宙红外光度密度。我们使用[N II]/Hα与[O III]/Hβ线比将星系分为活动星系核、恒星形成星系和复合星系。在9×10^(11)L_⊙，随着L的IR从25%增加到90%，活动星系核的比例持续增加，与SFG和AGN IR LFS的断裂相一致。在L_(IR)≤10^(11)L_⊙中，SFG占据主导地位。在局部宇宙中，只有1.1±0.1%的Ω_(IR)由发光红外星系(L_(IR)>；10^(11)L_⊙)产生，而由超亮红外星系(L_(IR)>；10^(12)L_⊙)产生的仅为0.03%±0.01%。与Akari NEP深部探测的高红移结果相比，我们观察到Ω^(SFG)IR、∝(1+z)^(4.1±0.4)和Ω^(AGN)IR、∝(1+z)^(4.1±0.5)的强烈演化。我们的结果表明，我们的所有测量量(IR，LFS，L^*，Ω^(AGN)IR，Ω^(SFG)IR)都显示出从低红移(修正后的明亮星系样本)到高红移(Akari NEP深度探测)平稳而稳定的增加。
By cross-correlating the AKARI all-sky survey in six infrared (IR) bands (9, 18, 65, 90, 140 and 160 μm) with the Sloan Digital Sky Survey (SDSS) galaxies, we identified 2357 IR galaxies with a spectroscopic redshift. This is not just one of the largest samples of local IR galaxies, but AKARI provides crucial far-IR (FIR) bands for accurately measuring the galaxy spectral energy distribution (SED) across the peak of the dust emission at > 100 μ m. By fitting modern IR SED models to the AKARI photometry, we measured the total infrared luminosity (L_(IR)) of individual galaxies. Using this L_(IR), we constructed the luminosity functions (LF) of IR galaxies at a median redshift of z= 0.031. The LF agrees well with that at z= 0.0082 (the Revised Bright Galaxy Sample), showing smooth and continuous evolution towards higher redshift LFs measured in the AKARI North Ecliptic Pole (NEP) deep field. By integrating the IR LF weighted by L_(IR), we measured the local cosmic IR luminosity density of Ω_(IR_= (3.8^(+5.8)_(−1.2)) × 10^8 L_⊙ Mpc^(−3). We separate galaxies into active galactic nuclei (AGN), star-forming galaxies (SFG) and composite by using the [N ii]/Hα versus [O iii]/Hβ line ratios. The fraction of AGN shows a continuous increase with increasing L_(IR) from 25 to 90 per cent at 9 10^(11) L_⊙, coinciding with the break of both the SFG and AGN IR LFs. At L_(IR)≤ 10^(11) L_⊙, SFG dominates IR LFs. Only 1.1 ± 0.1 per cent of Ω_(IR) is produced by luminous infrared galaxies (L_(IR) > 10^(11) L_⊙), and only 0.03 ± 0.01 per cent by ultraluminous infrared galaxies (L_(IR) > 10^(12) L_⊙) in the local Universe. Compared with high-redshift results from the AKARI NEP deep survey, we observed a strong evolution of Ω^(SFG)IR^∝ (1 +z)^(4.1±0.4) and Ω^(AGN)IR^∝ (1+z)^(4.1±0.5). Our results show that all of our measured quantities (IR LFs, L^*, Ω^(AGN)IR, Ω^(SFG)IR) show smooth and steady increase from lower redshift (the Revised Bright Galaxy Sample) to higher redshift (the AKARI NEP deep survey).