The Supernova Legacy Survey: measurement of Ωm, Ω∧ and w from the first year data set. Commentary
The Supernova Legacy Survey: measurement of Ωm, Ω∧ and w from the first year data set. Commentary
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发表时间：
2006
影响因子：
6.5
通讯作者：
P. Astier;J. Guy;N. Regnault;R. Pain;E. Aubourg;D. Balam;S. Basa;R. Carlberg;S. Fabbro;D. Fouchez;I. Hook;D. Howell;H. Lafoux;J. Neill;N. Palanque-Delabrouille;K. Perrett;C. Pritchet;J. Rich;M. Sullivan;R. Taillet;G. Aldering;P. Antilogus;V. Arsenijević;C. Balland;S. Baumont;J. Bronder;H. Courtois;R. Ellis;M. Filiol;A. Gonçalves;A. Goobar;D. Guide;D. Hardin;V. Lusset;C. Lidman;R. McMahon;M. Mouchet;A. Mourão;S. Perlmutter;P. Ripoche;C. Tao;N. Walton;B. Leibundgut
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作者：
P. Astier;J. Guy;N. Regnault;R. Pain;E. Aubourg;D. Balam;S. Basa;R. Carlberg;S. Fabbro;D. Fouchez;I. Hook;D. Howell;H. Lafoux;J. Neill;N. Palanque-Delabrouille;K. Perrett;C. Pritchet;J. Rich;M. Sullivan;R. Taillet;G. Aldering;P. Antilogus;V. Arsenijević;C. Balland;S. Baumont;J. Bronder;H. Courtois;R. Ellis;M. Filiol;A. Gonçalves;A. Goobar;D. Guide;D. Hardin;V. Lusset;C. Lidman;R. McMahon;M. Mouchet;A. Mourão;S. Perlmutter;P. Ripoche;C. Tao;N. Walton;B. Leibundgut
我们目前的距离测量71高红移Ia型超新星发现在第一年的5年超新星遗产调查（SNLS）。这些事件被探测到，并使用加拿大-法国-夏威夷望远镜（CFHT）的MegaPrime/MegaCam仪器测量了它们的多色光变曲线，作为CFHT遗产巡天（CFHTLS）的一部分，通过在四个波段重复成像四个一平方度的场。后续的光谱学是在VLT、双子座和凯克望远镜上进行的，以确认超新星的性质并测量它们的红移。有了这个数据集，我们已经建立了一个扩展到z = 1的哈勃图，所有的距离测量都涉及至少两个波段。利用CFHT获得的多波段光度法评估系统不确定度。宇宙学拟合结果表明：对于平坦的ACDM模型，Ω M = 0.263 ± 0.042（stat）± 0.032（sys）; w =-1.023 ± 0.090（stat）± 0.054（sys）对于具有常数状态方程w的平坦宇宙学，当结合最近Sloan数字巡天测量重子的约束时，声振荡
We present distance measurements to 71 high redshift type Ia supernovae discovered during the first year of the 5-year Supernova Legacy Survey (SNLS). These events were detected and their multi-color light-curves measured using the MegaPrime/MegaCam instrument at the Canada-France-Hawaii Telescope (CFHT), by repeatedly imaging four one-square degree fields in four bands, as part of the CFHT Legacy Survey (CFHTLS). Follow-up spectroscopy was performed at the VLT, Gemini and Keck telescopes to confirm the nature of the supernovae and to measure their redshift. With this data set, we have built a Hubble diagram extending to z = 1, with all distance measurements involving at least two bands. Systematic uncertainties are evaluated making use of the multi-band photometry obtained at CFHT. Cosmological fits to this first year SNLS Hubble diagram give the following results: Ω M = 0.263 ± 0.042 (stat) ± 0.032 (sys) for a flat ACDM model; and w = ―1.023 ± 0.090 (stat) ± 0.054 (sys) for a flat cosmology with constant equation of state w when combined with the constraint from the recent Sloan Digital Sky Survey measurement of baryon acoustic oscillations.