Spectra of High-Redshift Type Ia Supernovae and a Comparison with Their Low-Redshift Counterparts-猫眼课题宝

DOI：

10.1086/497635

发表时间：

2005-09

期刊：

The Astronomical Journal

影响因子：

通讯作者：

中科院分区：

其他

文献类型：

作者：

I. Hook;D. Howell;G. Aldering;R. Amanullah;M. S. Burns;A. Conley;A. Conley;S. Deustua;R. Ellis;S. Fabbro;V. Fadeyev;G. Folatelli;G. Garavini;G. Garavini;R. Gibbons;G. Goldhaber;G. Goldhaber;A. Goobar;D. Groom;A. Kim;R. Knop;M. Kowalski;C. Lidman;S. Nobili;S. Nobili;P. Nugent;R. Pain;C. Pennypacker;S. Perlmutter;S. Perlmutter;P. Ruíz-Lapuente;G. Sainton;B. E. Schaefer;E. Smith;A. Spadafora;V. Stanishev;R. Thomas;N. Walton;Lei Wang;W. M. Wood-Vasey;W. M. Wood-Vasey

我们给出了14颗高红移(0.17；z&lt；0.83)超新星的光谱，它们是由超新星宇宙学项目发现的，是测量宇宙学参数的活动的一部分。这些光谱被用来确定红移和分类超新星类型，如果超新星要用于宇宙学研究，这是必不可少的信息。红移要么来自宿主星系的光谱，要么来自超新星本身的光谱。我们通过与附近超新星的光谱进行匹配，提供了这些超新星属于Ia型(SNE Ia)的证据。我们发现，由这种拟合过程确定的光谱相对于最大光的日期与由光度学光曲线确定的日期是一致的，而且，SNE Ia在低红移和高红移时的光谱时间序列是不可区分的。我们还表明，从蓝移的Ca、H和K测量的膨胀速度与测量的低红移SNE Ia的膨胀速度是一致的。从这些第一级定量比较中，我们没有发现这些低红移和高红移样品之间SNIa性质的演变的证据。因此，即使我们的样品可能不是完全的，我们也可以得出结论，在高红移时有一群SneIa，它们的光谱性质与低红移时的一致。

We present spectra for 14 high-redshift (0.17 < z < 0.83) supernovae, which were discovered by the Supernova Cosmology Project as part of a campaign to measure cosmological parameters. The spectra are used to determine the redshift and classify the supernova type, essential information if the supernovae are to be used for cosmological studies. Redshifts were derived either from the spectrum of the host galaxy or from the spectrum of the supernova itself. We present evidence that these supernovae are of Type Ia (SNe Ia) by matching to spectra of nearby supernovae. We find that the dates of the spectra relative to maximum light determined from this fitting process are consistent with the dates determined from the photometric light curves, and, moreover, the spectral time sequences for SNe Ia at low and high redshift are indistinguishable. We also show that the expansion velocities measured from blueshifted Ca H and K are consistent with those measured for low-redshift SNe Ia. From these first-level quantitative comparisons we find no evidence for evolution in SN Ia properties between these low- and high-redshift samples. Thus, even though our samples may not be complete, we conclude that there is a population of SNe Ia at high redshift whose spectral properties match those at low redshift.

Spectra of High-Redshift Type Ia Supernovae and a Comparison with Their Low-Redshift Counterparts

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