Exploring cosmic origins with CORE: Extragalactic sources in cosmic microwave background maps
Exploring cosmic origins with CORE: Extragalactic sources in cosmic microwave background maps
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DOI：
10.1088/1475-7516/2018/04/020
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发表时间：
2016-09
影响因子：
6.4
通讯作者：
G. Zotti;J. González-Nuevo;M. López-Caniego;M. Negrello;J. Greenslade;C. Hernandez-Monteagudo;J. Delabrouille;Z. Cai;M. Bonato;A. Achúcarro;P. Ade;R. Allison;M. Ashdown;M. Ballardini;A. Banday;R. Banerji;J. Bartlett;N. Bartolo;S. Basak;M. Bersanelli;M. Biesiada;Maciej Bilicki;A. Bonaldi;J. Borrill;F. Bouchet;F. Boulanger;T. Brinckmann;M. Bucher;C. Burigana;A. Buzzelli;M. Calvo;C. Carvalho;M. Castellano;A. Challinor;J. Chluba;D. Clements;S. Clesse;S. Colafrancesco;I. Colantoni;A. Coppolecchia;M. Crook;G. D’Alessandro;P. Bernardis;G. Gasperis;J. Diego;E. D. Valentino;J. Errard;S. Feeney;R. Fernández-Cobos;S. Ferraro;F. Finelli;F. Forastieri;S. Galli;R. Génova-Santos;M. Gerbino;S. Grandis;S. Hagstotz;S. Hanany;Will Handley;C. Hervías-Caimapo;M. Hills;E. Hivon;K. Kiiveri;T. Kisner;T. Kitching;M. Kunz;H.Kurki-Suonio;G. Lagache;L. Lamagna;A. Lasenby;M. Lattanzi;A. Brun;J. Lesgourgues;A. Lewis;M. Liguori;V. Lindholm;G. Luzzi;B. Maffei;N. Mandolesi;E. Martínez-González;C. Martins;S. Masi;M. Massardi;D. McCarthy;A. Melchiorri;J. Melin;D. Molinari;A. Monfardini;P. Natoli;A. Notari;A. Paiella;D. Paoletti;R. B. Partridge;G. Patanchon;M. Piat;G. Pisano;L. Polastri;G. Polenta;A. Pollo;V. Poulin;M. Quartin;M. Remazeilles;M. Roman;G. Rossi;B. Roukema;J. Rubiño-Martín;L. Salvati;D. Scott;S. Serjeant;A. Tartari;L. Toffolatti;M. Tomasi;N. Trappe;S. Triqueneaux;T. Trombetti;M. Tucci;C. Tucker;J. Valiviita;R. Weygaert;B. Tent;V. Vennin;P. Vielva;N. Vittorio;K. Young;F. T. B. collaboration
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作者：
G. Zotti;J. González-Nuevo;M. López-Caniego;M. Negrello;J. Greenslade;C. Hernandez-Monteagudo;J. Delabrouille;Z. Cai;M. Bonato;A. Achúcarro;P. Ade;R. Allison;M. Ashdown;M. Ballardini;A. Banday;R. Banerji;J. Bartlett;N. Bartolo;S. Basak;M. Bersanelli;M. Biesiada;Maciej Bilicki;A. Bonaldi;J. Borrill;F. Bouchet;F. Boulanger;T. Brinckmann;M. Bucher;C. Burigana;A. Buzzelli;M. Calvo;C. Carvalho;M. Castellano;A. Challinor;J. Chluba;D. Clements;S. Clesse;S. Colafrancesco;I. Colantoni;A. Coppolecchia;M. Crook;G. D’Alessandro;P. Bernardis;G. Gasperis;J. Diego;E. D. Valentino;J. Errard;S. Feeney;R. Fernández-Cobos;S. Ferraro;F. Finelli;F. Forastieri;S. Galli;R. Génova-Santos;M. Gerbino;S. Grandis;S. Hagstotz;S. Hanany;Will Handley;C. Hervías-Caimapo;M. Hills;E. Hivon;K. Kiiveri;T. Kisner;T. Kitching;M. Kunz;H.Kurki-Suonio;G. Lagache;L. Lamagna;A. Lasenby;M. Lattanzi;A. Brun;J. Lesgourgues;A. Lewis;M. Liguori;V. Lindholm;G. Luzzi;B. Maffei;N. Mandolesi;E. Martínez-González;C. Martins;S. Masi;M. Massardi;D. McCarthy;A. Melchiorri;J. Melin;D. Molinari;A. Monfardini;P. Natoli;A. Notari;A. Paiella;D. Paoletti;R. B. Partridge;G. Patanchon;M. Piat;G. Pisano;L. Polastri;G. Polenta;A. Pollo;V. Poulin;M. Quartin;M. Remazeilles;M. Roman;G. Rossi;B. Roukema;J. Rubiño-Martín;L. Salvati;D. Scott;S. Serjeant;A. Tartari;L. Toffolatti;M. Tomasi;N. Trappe;S. Triqueneaux;T. Trombetti;M. Tucci;C. Tucker;J. Valiviita;R. Weygaert;B. Tent;V. Vennin;P. Vielva;N. Vittorio;K. Young;F. T. B. collaboration
我们讨论了下一代星载宇宙微波背景（CMB）实验对河外源研究的潜力。我们的分析对未来太空项目CORE的定义有特别的影响，该项目已提交，以响应欧空局的号召，作为普朗克卫星的继任者，需要一个中型任务机会。尽管有效望远镜的尺寸会比普朗克的小一些，但CORE在其最高频率上的角分辨率会好得多，因为与普朗克相比，CORE在所有频率上都有衍射限制。改进的分辨率意味着源混淆的显著减少，即大大降低了检测限。特别是，CORE将探测到分布在整个天空中的数千个强透镜高z星系。这些星系的极端亮度将使通过后续观测对它们进行非常详细的研究成为可能。此外，CORE分辨率比普朗克分辨率更符合高z星系原星团的典型尺寸，从而提高了探测效率；这些天体将处于演化阶段，超出了其他波段的测量范围。此外，核心将提供独特的信息，恒星形成的演变，在活跃的群体和星系团，直到最高可能的红移。最后，由于其非常高的灵敏度，CORE将探测到数千个射电源的偏振发射，并首次探测到尘埃星系的偏振发射，分别是毫米和亚毫米波长。
We discuss the potential of a next generation space-borne Cosmic Microwave Background (CMB) experiment for studies of extragalactic sources. Our analysis has particular bearing on the definition of the future space project, CORE, that has been submitted in response to ESA's call for a Medium-size mission opportunity as the successor of the Planck satellite. Even though the effective telescope size will be somewhat smaller than that of Planck, CORE will have a considerably better angular resolution at its highest frequencies, since, in contrast with Planck, it will be diffraction limited at all frequencies. The improved resolution implies a considerable decrease of the source confusion, i.e. substantially fainter detection limits. In particular, CORE will detect thousands of strongly lensed high-z galaxies distributed over the full sky. The extreme brightness of these galaxies will make it possible to study them, via follow-up observations, in extraordinary detail. Also, the CORE resolution matches the typical sizes of high-z galaxy proto-clusters much better than the Planck resolution, resulting in a much higher detection efficiency; these objects will be caught in an evolutionary phase beyond the reach of surveys in other wavebands. Furthermore, CORE will provide unique information on the evolution of the star formation in virialized groups and clusters of galaxies up to the highest possible redshifts. Finally, thanks to its very high sensitivity, CORE will detect the polarized emission of thousands of radio sources and, for the first time, of dusty galaxies, at mm and sub-mm wavelengths, respectively.