The BigBoss Experiment

The BigBoss Experiment
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DOI：
10.2172/1027233
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发表时间：
2011-06
期刊：
--
影响因子：
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通讯作者：
D. Schlegel;F. Abdalla;T. Abraham;Chong H. Ahn;C. Prieto;J. Annis;É. Aubourg;M. Azzaro;S. Bailey;C. Baltay;C. Baugh;C. Bebek;S. Becerril;M. Blanton;A. Bolton;B. C. Bromley;R. Cahn;P. Carton;J. Cervantes-Cota;Y. Chu;Marina Cortês;K. Dawson;A. Dey;Mark Dickinson;H. Diehl;P. Doel;A. Ealet;J. Edelstein;D. Eppelle;S. Escoffier;A. Evrard;L. Faccioli;C. Frenk;M. Geha;D. Gerdes;P. Gondolo;A. González-Arroyo;B. Grossan;T. Heckman;H. Heetderks;Shirley Ho;K. Honscheid;D. Huterer;O. Ilbert;I. Ivans;P. Jelinsky;Y. Jing;D. Joyce;R. Kennedy;S. Kent;D. Kieda;A. Kim;C. Kim;J. Kneib;X. Kong;A. Kosowsky;K. Krishnan;O. Lahav;M. Lampton;S. LeBohec;V. Brun;M. Levi;C. Li;M. Liang;H. Lim;W. Lin;Eric V. Linder;W. Lorenzon;A. Macorra;C. Magneville;R. Malina;C. Marinoni;V. Martínez;S. Majewski;T. Matheson;R. Mccloskey;P. McDonald;T. McKay;J. McMahon;Brice Ménard;Jordi Miralda-Escudé;M. Modjaz;A. Montero-Dorta;I. Morales;N. Mostek;J. Newman;R. Nichol;P. Nugent;Knut Olsen;N. Padmanabhan;N. Palanque-Delabrouille;I. Park;J. A. Peacock;W. Percival;S. Perlmutter;C. Péroux;P. Petitjean;F. Prada;É. Prieto;J. Prochaska;K. Reil;C. Rockosi;N. Roe;E. Rollinde;A. Roodman;N. Ross;G. Rudnick;V. Ruhlmann-Kleider;Javier Sánchez;D. Sawyer;C. Schimd;M. Schubnell;R. Scoccimaro;U. Seljak;H. Seo;E. Sheldon;M. Sholl;R. Shulte-Ladbeck;A. Slosar;D. Smith;G. Smoot;W. Springer;A. Stril;A. Szalay;C. Tao;G. Tarlé;E. Taylor;A. Tilquin;J. Tinker;Francisco Valdes;J. Wang;T. Wang;B. Weaver;D. Weinberg;M. White;M. Wood-Vasey;J. Yang;X. Yang.;N. Zakamska;A. Zentner;C. Zhai;Pengjie Zhang;C. Yèche
D. Schlegel;F. Abdalla;T. Abraham;Chong H. Ahn;C. Prieto;J. Annis;É. Aubourg;M. Azzaro;S. Bailey;C. Baltay;C. Baugh;C. Bebek;S. Becerril;M. Blanton;A. Bolton;B. C. Bromley;R. Cahn;P. Carton;J. Cervantes-Cota;Y. Chu;Marina Cortês;K. Dawson;A. Dey;Mark Dickinson;H. Diehl;P. Doel;A. Ealet;J. Edelstein;D. Eppelle;S. Escoffier;A. Evrard;L. Faccioli;C. Frenk;M. Geha;D. Gerdes;P. Gondolo;A. González-Arroyo;B. Grossan;T. Heckman;H. Heetderks;Shirley Ho;K. Honscheid;D. Huterer;O. Ilbert;I. Ivans;P. Jelinsky;Y. Jing;D. Joyce;R. Kennedy;S. Kent;D. Kieda;A. Kim;C. Kim;J. Kneib;X. Kong;A. Kosowsky;K. Krishnan;O. Lahav;M. Lampton;S. LeBohec;V. Brun;M. Levi;C. Li;M. Liang;H. Lim;W. Lin;Eric V. Linder;W. Lorenzon;A. Macorra;C. Magneville;R. Malina;C. Marinoni;V. Martínez;S. Majewski;T. Matheson;R. Mccloskey;P. McDonald;T. McKay;J. McMahon;Brice Ménard;Jordi Miralda-Escudé;M. Modjaz;A. Montero-Dorta;I. Morales;N. Mostek;J. Newman;R. Nichol;P. Nugent;Knut Olsen;N. Padmanabhan;N. Palanque-Delabrouille;I. Park;J. A. Peacock;W. Percival;S. Perlmutter;C. Péroux;P. Petitjean;F. Prada;É. Prieto;J. Prochaska;K. Reil;C. Rockosi;N. Roe;E. Rollinde;A. Roodman;N. Ross;G. Rudnick;V. Ruhlmann-Kleider;Javier Sánchez;D. Sawyer;C. Schimd;M. Schubnell;R. Scoccimaro;U. Seljak;H. Seo;E. Sheldon;M. Sholl;R. Shulte-Ladbeck;A. Slosar;D. Smith;G. Smoot;W. Springer;A. Stril;A. Szalay;C. Tao;G. Tarlé;E. Taylor;A. Tilquin;J. Tinker;Francisco Valdes;J. Wang;T. Wang;B. Weaver;D. Weinberg;M. White;M. Wood-Vasey;J. Yang;X. Yang.;N. Zakamska;A. Zentner;C. Zhai;Pengjie Zhang;C. Yèche
中科院分区：
其他
文献类型：
--
作者：
D. Schlegel;F. Abdalla;T. Abraham;Chong H. Ahn;C. Prieto;J. Annis;É. Aubourg;M. Azzaro;S. Bailey;C. Baltay;C. Baugh;C. Bebek;S. Becerril;M. Blanton;A. Bolton;B. C. Bromley;R. Cahn;P. Carton;J. Cervantes-Cota;Y. Chu;Marina Cortês;K. Dawson;A. Dey;Mark Dickinson;H. Diehl;P. Doel;A. Ealet;J. Edelstein;D. Eppelle;S. Escoffier;A. Evrard;L. Faccioli;C. Frenk;M. Geha;D. Gerdes;P. Gondolo;A. González-Arroyo;B. Grossan;T. Heckman;H. Heetderks;Shirley Ho;K. Honscheid;D. Huterer;O. Ilbert;I. Ivans;P. Jelinsky;Y. Jing;D. Joyce;R. Kennedy;S. Kent;D. Kieda;A. Kim;C. Kim;J. Kneib;X. Kong;A. Kosowsky;K. Krishnan;O. Lahav;M. Lampton;S. LeBohec;V. Brun;M. Levi;C. Li;M. Liang;H. Lim;W. Lin;Eric V. Linder;W. Lorenzon;A. Macorra;C. Magneville;R. Malina;C. Marinoni;V. Martínez;S. Majewski;T. Matheson;R. Mccloskey;P. McDonald;T. McKay;J. McMahon;Brice Ménard;Jordi Miralda-Escudé;M. Modjaz;A. Montero-Dorta;I. Morales;N. Mostek;J. Newman;R. Nichol;P. Nugent;Knut Olsen;N. Padmanabhan;N. Palanque-Delabrouille;I. Park;J. A. Peacock;W. Percival;S. Perlmutter;C. Péroux;P. Petitjean;F. Prada;É. Prieto;J. Prochaska;K. Reil;C. Rockosi;N. Roe;E. Rollinde;A. Roodman;N. Ross;G. Rudnick;V. Ruhlmann-Kleider;Javier Sánchez;D. Sawyer;C. Schimd;M. Schubnell;R. Scoccimaro;U. Seljak;H. Seo;E. Sheldon;M. Sholl;R. Shulte-Ladbeck;A. Slosar;D. Smith;G. Smoot;W. Springer;A. Stril;A. Szalay;C. Tao;G. Tarlé;E. Taylor;A. Tilquin;J. Tinker;Francisco Valdes;J. Wang;T. Wang;B. Weaver;D. Weinberg;M. White;M. Wood-Vasey;J. Yang;X. Yang.;N. Zakamska;A. Zentner;C. Zhai;Pengjie Zhang;C. Yèche

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BigBOSS 是第四阶段的地面暗能量实验，旨在通过超过 14,000 平方度的广域星系和类星体红移调查来研究重子声振荡 (BAO) 和结构的生长。为了响应基特峰 4 米 Mayall 望远镜的重大新仪器和高影响力科学计划的号召，该项目已被 NOAO 有条件接受。 BigBOSS 仪器是一款机器人驱动、光纤馈送的光谱仪，能够在 340 nm 至 1060 nm 的波长范围内同时采集 5000 个光谱，分辨率 R = 3000-4800。利用已经进行的成像调查的数据，选择光谱目标来追踪潜在的暗物质分布。特别是，目标包括 z = 1.0 以内的发光红色星系 (LRG)，从而扩展了 BOSS LRG 勘测的红移和勘测区域。为了探测宇宙更高的红移，BigBOSS 将瞄准 z = 1.7 以内的明亮 [OII] 发射线星系 (ELG)。总共获得了 2000 万个星系红移来测量 BAO 特征，追踪较小尺度的物质功率谱，并检测红移空间扭曲。 BigBOSS 将通过测量超过 600,000 个 2.2 < z < 3.5 类星体光谱中的 Ly-alpha 森林，对早期暗能量和宇宙曲率提供额外的约束。 BigBOSS 星系 BAO 测量与宽带功率分析（包括 BigBOSS 类星体光谱中的 Ly-alpha 森林）相结合，利用普朗克加上第三阶段先验实现了 395 的 FOM。该 FOM 基于宽带功率分析的保守假设 (kmax = 0.15)，如果当前工作允许我们将分析推向更高的波数 (kmax = 0.3)，则可能会增长到 600 以上。 BigBOSS 还将对修改后的重力和膨胀理论进行限制，并将测量中微子质量总和至 0.024 eV 的精度。
BigBOSS is a Stage IV ground-based dark energy experiment to study baryon acoustic oscillations (BAO) and the growth of structure with a wide-area galaxy and quasar redshift survey over 14,000 square degrees. It has been conditionally accepted by NOAO in response to a call for major new instrumentation and a high-impact science program for the 4-m Mayall telescope at Kitt Peak. The BigBOSS instrument is a robotically-actuated, fiber-fed spectrograph capable of taking 5000 simultaneous spectra over a wavelength range from 340 nm to 1060 nm, with a resolution R = 3000-4800. Using data from imaging surveys that are already underway, spectroscopic targets are selected that trace the underlying dark matter distribution. In particular, targets include luminous red galaxies (LRGs) up to z = 1.0, extending the BOSS LRG survey in both redshift and survey area. To probe the universe out to even higher redshift, BigBOSS will target bright [OII] emission line galaxies (ELGs) up to z = 1.7. In total, 20 million galaxy redshifts are obtained to measure the BAO feature, trace the matter power spectrum at smaller scales, and detect redshift space distortions. BigBOSS will provide additional constraints on early dark energy and on the curvature of the universe by measuring the Ly-alpha forest in the spectra of over 600,000 2.2 < z < 3.5 quasars. BigBOSS galaxy BAO measurements combined with an analysis of the broadband power, including the Ly-alpha forest in BigBOSS quasar spectra, achieves a FOM of 395 with Planck plus Stage III priors. This FOM is based on conservative assumptions for the analysis of broad band power (kmax = 0.15), and could grow to over 600 if current work allows us to push the analysis to higher wave numbers (kmax = 0.3). BigBOSS will also place constraints on theories of modified gravity and inflation, and will measure the sum of neutrino masses to 0.024 eV accuracy.