The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4

The Herschel* PEP/HerMES luminosity function - I. Probing the evolution of PACS selected Galaxies to z ≃ 4
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DOI：
10.1093/mnras/stt308
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发表时间：
2013-02
期刊：
Monthly Notices of the Royal Astronomical Society
影响因子：
4.8
通讯作者：
C. Gruppioni;F. Pozzi;G. Rodighiero;I. Delvecchio;S. Berta;L. Pozzetti;G. Zamorani;P. Andreani;A. Cimatti;O. Ilbert;E. L. Floch;D. Lutz;B. Magnelli;L. Marchetti;L. Marchetti;P. Monaco;R. Nordon;S. Oliver;P. Popesso;L. Riguccini;I. Roseboom;I. Roseboom;D. Rosario;M. Sargent;Mattia Vaccari;Mattia Vaccari;B. Altieri;H. Aussel;Á. Bongiovanni;J. Cepa;E. Daddi;H. Domínguez-Sánchez;H. Domínguez-Sánchez;D. Elbaz;N. F. Schreiber;R. Genzel;A. Iribarrem;M. Magliocchetti;R. Maiolino;A. Poglitsch;A. P. Garćıa;M. Sánchez-Portal;E. Sturm;L. Tacconi;I. Valtchanov;A. Amblard;V. Arumugam;M. Béthermin;J. Bock;J. Bock;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;N. Castro-RodrÍguez;A. Cava;P. Chanial;D. Clements;A. Conley;A. Cooray;A. Cooray;C. Dowell;C. Dowell;E. Dwek;S. Eales;A. Franceschini;J. Glenn;M. Griffin;E. Hatziminaoglou;E. Ibar;K. Isaak;R. Ivison;R. Ivison;G. Lagache;L. Levenson;L. Levenson;N. Lu;S. Madden;B. Maffei;G. Mainetti;Hieu Nguyen;Hieu Nguyen;B. O’Halloran;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Pérez-Fournon;I. Pérez-Fournon;M. Pohlen;D. Rigopoulou;D. Rigopoulou;M. Rowan‐Robinson;B. Schulz;D. Scott;N. Seymour;N. Seymour;D. Shupe;A. Smith;J. Stevens;M. Symeonidis;M. Trichas;K. Tugwell;L. Vigroux;Lian-tao Wang;G. Wright;C. Xu;M. Zemcov;M. Zemcov;S. Bardelli;M. Carollo;T. Contini;O. Fèvre;S. Lilly;V. Mainieri;A. Renzini;M. Scodeggio;E. Zucca
C. Gruppioni;F. Pozzi;G. Rodighiero;I. Delvecchio;S. Berta;L. Pozzetti;G. Zamorani;P. Andreani;A. Cimatti;O. Ilbert;E. L. Floch;D. Lutz;B. Magnelli;L. Marchetti;L. Marchetti;P. Monaco;R. Nordon;S. Oliver;P. Popesso;L. Riguccini;I. Roseboom;I. Roseboom;D. Rosario;M. Sargent;Mattia Vaccari;Mattia Vaccari;B. Altieri;H. Aussel;Á. Bongiovanni;J. Cepa;E. Daddi;H. Domínguez-Sánchez;H. Domínguez-Sánchez;D. Elbaz;N. F. Schreiber;R. Genzel;A. Iribarrem;M. Magliocchetti;R. Maiolino;A. Poglitsch;A. P. Garćıa;M. Sánchez-Portal;E. Sturm;L. Tacconi;I. Valtchanov;A. Amblard;V. Arumugam;M. Béthermin;J. Bock;J. Bock;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;N. Castro-RodrÍguez;A. Cava;P. Chanial;D. Clements;A. Conley;A. Cooray;A. Cooray;C. Dowell;C. Dowell;E. Dwek;S. Eales;A. Franceschini;J. Glenn;M. Griffin;E. Hatziminaoglou;E. Ibar;K. Isaak;R. Ivison;R. Ivison;G. Lagache;L. Levenson;L. Levenson;N. Lu;S. Madden;B. Maffei;G. Mainetti;Hieu Nguyen;Hieu Nguyen;B. O’Halloran;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Pérez-Fournon;I. Pérez-Fournon;M. Pohlen;D. Rigopoulou;D. Rigopoulou;M. Rowan‐Robinson;B. Schulz;D. Scott;N. Seymour;N. Seymour;D. Shupe;A. Smith;J. Stevens;M. Symeonidis;M. Trichas;K. Tugwell;L. Vigroux;Lian-tao Wang;G. Wright;C. Xu;M. Zemcov;M. Zemcov;S. Bardelli;M. Carollo;T. Contini;O. Fèvre;S. Lilly;V. Mainieri;A. Renzini;M. Scodeggio;E. Zucca
中科院分区：
物理与天体物理2区
文献类型：
--
作者：
C. Gruppioni;F. Pozzi;G. Rodighiero;I. Delvecchio;S. Berta;L. Pozzetti;G. Zamorani;P. Andreani;A. Cimatti;O. Ilbert;E. L. Floch;D. Lutz;B. Magnelli;L. Marchetti;L. Marchetti;P. Monaco;R. Nordon;S. Oliver;P. Popesso;L. Riguccini;I. Roseboom;I. Roseboom;D. Rosario;M. Sargent;Mattia Vaccari;Mattia Vaccari;B. Altieri;H. Aussel;Á. Bongiovanni;J. Cepa;E. Daddi;H. Domínguez-Sánchez;H. Domínguez-Sánchez;D. Elbaz;N. F. Schreiber;R. Genzel;A. Iribarrem;M. Magliocchetti;R. Maiolino;A. Poglitsch;A. P. Garćıa;M. Sánchez-Portal;E. Sturm;L. Tacconi;I. Valtchanov;A. Amblard;V. Arumugam;M. Béthermin;J. Bock;J. Bock;A. Boselli;V. Buat;D. Burgarella;N. Castro-RodrÍguez;N. Castro-RodrÍguez;A. Cava;P. Chanial;D. Clements;A. Conley;A. Cooray;A. Cooray;C. Dowell;C. Dowell;E. Dwek;S. Eales;A. Franceschini;J. Glenn;M. Griffin;E. Hatziminaoglou;E. Ibar;K. Isaak;R. Ivison;R. Ivison;G. Lagache;L. Levenson;L. Levenson;N. Lu;S. Madden;B. Maffei;G. Mainetti;Hieu Nguyen;Hieu Nguyen;B. O’Halloran;M. Page;P. Panuzzo;A. Papageorgiou;C. Pearson;C. Pearson;I. Pérez-Fournon;I. Pérez-Fournon;M. Pohlen;D. Rigopoulou;D. Rigopoulou;M. Rowan‐Robinson;B. Schulz;D. Scott;N. Seymour;N. Seymour;D. Shupe;A. Smith;J. Stevens;M. Symeonidis;M. Trichas;K. Tugwell;L. Vigroux;Lian-tao Wang;G. Wright;C. Xu;M. Zemcov;M. Zemcov;S. Bardelli;M. Carollo;T. Contini;O. Fèvre;S. Lilly;V. Mainieri;A. Renzini;M. Scodeggio;E. Zucca

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我们利用赫歇尔保证时间观测 (GTO) PACS 演化探测器 (PEP) 巡天的深度和扩展远红外数据集（70、100 和 160 μm），结合赫歇尔多层河外巡天数据（250、350 和 500 μm），推导出静止帧 35、60、90 和总的演化红外线（IR） 光度函数 (LF) 高达 z 类似于 4。我们检测到总 IR LF (L-IR alpha (1 + z)(3.55 +/- 0.10) 高达 z 类似于 2，并且 (1 + z) 1.62 类似于 0.51 at 2 \textless z 小于或类似于 4）非常强的光度演化，以及密度演化 ((1 + z)-0.57 +/- 0.22 至 z 类似于 1 和。 (1 + z)-3.92 +/- 0.34 at 1 \textless z 小于或类似于 4)。与之前的发现一致，红外光度密度 (.IR) 急剧增加到类似于 1 的 z，然后在类似于 1 的 z 和类似于 3 的 z 之间变平，在类似于 3 的 z 处减小。具有不同光谱能量分布、质量和特定恒星形成率 (SFR) 的星系以非常不同的方式演化，这个大而深的统计样本是第一个使我们能够单独研究贡献的各个 IR 群体的不同演化行为的样本。 到.IR。发现占据完善的 SFR 恒星质量主序带 (MS) 的星系在所有红移中主导总 IR LF 和 IR，来自非 MS 源（= MS 以上 0.6 dex）的贡献几乎恒定（类似于总 IR 的 20%），并且在整个 0.8 \textless z \textless 2.2 范围内没有显示出随着 z 增加而增加的显着迹象。我们发现质量在 10 = log(M/M-圆点) = 11 范围内的源在总红外低频中占主导地位，在高 z（大于或类似于 2）低频的亮端普遍存在质量更大的星系。设想了红外星系的双重演化方案：一方面，一个以星暴为主的阶段，其中超大质量黑洞（SMBH）生长并被尘埃遮蔽（可能由重大合并事件触发），随后是一个以活动星系核为主的阶段，然后向局部椭圆演化。另一方面，含有低光度活动星系核的中等恒星形成星系具有多种特性，表明它们是稳定螺旋星系形成之前处于过渡阶段的系统的良好候选者。
We exploit the deep and extended far-IR data sets (at 70, 100 and 160 mu m) of the Herschel Guaranteed Time Observation (GTO) PACS Evolutionary Probe (PEP) Survey, in combination with the Herschel Multi-tiered Extragalactic Survey data at 250, 350 and 500 mu m, to derive the evolution of the rest-frame 35-, 60-, 90-and total infrared (IR) luminosity functions (LFs) up to z similar to 4. We detect very strong luminosity evolution for the total IR LF (L-IR alpha (1 + z)(3.55 +/- 0.10) up to z similar to 2, and. (1 + z) 1.62 similar to 0.51 at 2 \textless z less than or similar to 4) combined with a density evolution ( (1 + z)-0.57 +/- 0.22 up to z similar to 1 and. (1 + z)-3.92 +/- 0.34 at 1 \textless z less than or similar to 4). In agreement with previous findings, the IR luminosity density (.IR) increases steeply to z similar to 1, then flattens between z similar to 1 and z similar to 3 to decrease at z similar to 3. Galaxies with different spectral energy distributions, masses and specific star formation rates (SFRs) evolve in very different ways and this large and deep statistical sample is the first one allowing us to separately study the different evolutionary behaviours of the individual IR populations contributing to.IR. Galaxies occupying the well-established SFR-stellar mass main sequence (MS) are found to dominate both the total IR LF and.IR at all redshifts, with the contribution from off-MS sources (= 0.6 dex above MS) being nearly constant (similar to 20 per cent of the total IR) and showing no significant signs of increase with increasing z over the whole 0.8 \textless z \textless 2.2 range. Sources with mass in the range 10 = log(M/M-circle dot) = 11 are found to dominate the total IR LF, with more massive galaxies prevailing at the bright end of the high-z (greater than or similar to 2) LF. A two-fold evolutionary scheme for IR galaxies is envisaged: on the one hand, a starburst-dominated phase in which the Super Massive Black Holes (SMBH) grows and is obscured by dust (possibly triggered by a major merging event), is followed by an AGN-dominated phase, then evolving towards a local elliptical. On the other hand, moderately star-forming galaxies containing a low-luminosity AGN have various properties suggesting they are good candidates for systems in a transition phase preceding the formation of steady spiral galaxies.