Planck 中期结果. XXXIX. Planck 高红移源候选体列表
星系天体物理
2016-12-14 v2
摘要
Planck 任务凭借其大频率范围和全天空覆盖，具有系统探测天空中最亮、最稀有的亚毫米波源的独特潜力，包括由尘埃发射示踪的高红移宇宙中的遥远天体。一种基于使用 Planck 和 IRAS 数据组合的成分分离过程的新方法，已被应用于挑选最明亮的冷亚毫米波源，其光谱能量分布在 5' 分辨率下在 353 和 857 GHz 之间达到峰值。在天空最干净的 26% 区域中，已探测到 2151 个 Planck 高红移源候选体（PHZ），其在 545 GHz 的通量密度高于 500 mJy。这些高红移候选体嵌入接近混淆极限的宇宙红外背景中，表现出比周围环境更冷的颜色，假设尘埃温度为 35 K、光谱指数为 1.5，则与红移 z>2 一致。从光学到亚毫米波获得的首次后续观测证实，该列表由两个不同的群体组成。一小部分（约 3%）的源被证认为强引力透镜星暴星系，它们是红移 2 到 4 之间最亮的亚毫米波透镜天体（在 545 GHz 的通量密度从 350 mJy 到 1 Jy）。然而，绝大多数 PHZ 源表现为尘埃星暴星系的过密度，其颜色与 z>2 一致，可被视为原团候选体。PHZ 提供了一个原始样本，补充了 Planck Sunyaev-Zeldovich 星表；通过将维里化大质量星系团群体扩展到 z>1.5 的源群体，PHZ 可能包含当今星系团的祖体。因此，PHZ 为研究结构形成的早期时代以及理解高红移下剧烈星暴阶段打开了新窗口。
引用
@article{arxiv.1508.04171,
title = {Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates},
author = {Planck Collaboration and P. A. R. Ade and N. Aghanim and M. Arnaud and J. Aumont and C. Baccigalupi and A. J. Banday and R. B. Barreiro and N. Bartolo and E. Battaner and K. Benabed and A. Benoit-Lévy and J. -P. Bernard and M. Bersanelli and P. Bielewicz and A. Bonaldi and L. Bonavera and J. R. Bond and J. Borrill and F. R. Bouchet and F. Boulanger and C. Burigana and R. C. Butler and E. Calabrese and A. Catalano and H. C. Chiang and P. R. Christensen and D. L. Clements and L. P. L. Colombo and F. Couchot and A. Coulais and B. P. Crill and A. Curto and F. Cuttaia and L. Danese and R. D. Davies and R. J. Davis and P. de Bernardis and A. de Rosa and G. de Zotti and J. Delabrouille and C. Dickinson and J. M. Diego and H. Dole and O. Doré and M. Douspis and A. Ducout and X. Dupac and F. Elsner and T. A. Enßlin and H. K. Eriksen and E. Falgarone and F. Finelli and I. Flores-Cacho and M. Frailis and A. A. Fraisse and E. Franceschi and S. Galeotta and S. Galli and K. Ganga and M. Giard and Y. Giraud-Héraud and E. Gjerløw and J. González-Nuevo and K. M. Górski and A. Gregorio and A. Gruppuso and J. E. Gudmundsson and F. K. Hansen and D. L. Harrison and G. Helou and C. Hernández-Monteagudo and D. Herranz and S. R. Hildebrandt and E. Hivon and M. Hobson and A. Hornstrup and W. Hovest and K. M. Huffenberger and G. Hurier and A. H. Jaffe and T. R. Jaffe and E. Keihänen and R. Keskitalo and T. S. Kisner and J. Knoche and M. Kunz and H. Kurki-Suonio and G. Lagache and J. -M. Lamarre and A. Lasenby and M. Lattanzi and C. R. Lawrence and R. Leonardi and F. Levrier and P. B. Lilje and M. Linden-Vørnle and M. López-Caniego and P. M. Lubin and J. F. Macías-Pérez and B. Maffei and G. Maggio and D. Maino and N. Mandolesi and A. Mangilli and M. Maris and P. G. Martin and E. Martínez-González and S. Masi and S. Matarrese and A. Melchiorri and A. Mennella and M. Migliaccio and S. Mitra and M. -A. Miville-Deschênes and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and J. A. Murphy and F. Nati and P. Natoli and N. P. H. Nesvadba and F. Noviello and D. Novikov and I. Novikov and C. A. Oxborrow and L. Pagano and F. Pajot and D. Paoletti and B. Partridge and F. Pasian and T. J. Pearson and O. Perdereau and L. Perotto and V. Pettorino and F. Piacentini and M. Piat and S. Plaszczynski and E. Pointecouteau and G. Polenta and G. W. Pratt and S. Prunet and J. -L. Puget and J. P. Rachen and M. Reinecke and M. Remazeilles and C. Renault and A. Renzi and I. Ristorcelli and G. Rocha and C. Rosset and M. Rossetti and G. Roudier and J. A. Rubiño-Martín and B. Rusholme and M. Sandri and D. Santos and M. Savelainen and G. Savini and D. Scott and L. D. Spencer and V. Stolyarov and R. Stompor and R. Sudiwala and R. Sunyaev and A. -S. Suur-Uski and J. -F. Sygnet and J. A. Tauber and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and M. Tucci and M. Türler and G. Umana and L. Valenziano and J. Valiviita and B. Van Tent and P. Vielva and F. Villa and L. A. Wade and B. D. Wandelt and I. K. Wehus and N. Welikala and D. Yvon and A. Zacchei and A. Zonca},
journal= {arXiv preprint arXiv:1508.04171},
year = {2016}
}