超新星遗产巡天的ESO/VLT第三年Ia型超新星数据集
The ESO/VLT 3rd year Type Ia supernova data set from the Supernova Legacy Survey
摘要：
我们提出了139光谱的124 Ia型超新星（SNeIa），在欧洲南方天文台/VLT在前三年的加拿大-法国-夏威夷望远镜（CFHT）超新星遗产调查（SNLS）。这组均匀的数据被用来检验SNeIa光谱的红移演化，并将用于SNLS第三年的宇宙学分析。光谱已减少和提取的专用管道，使用深CFHT遗产调查（CFHT-LS）参考图像的光度信息，以跟踪，在亚像素精度，光谱图上的超新星位置作为波长的函数。在60%的情况下，它还将超新星和它的宿主光分开。超新星候选者的识别是使用分光光度SNIa模型进行的。在调查的前三年中，使用ESO/VLT共确定了124个SNeIa，约占整个SNLS光谱样本的50%。它们的红移范围从z=0.149到z=1.031。样品的平均红移为z=0.63+/-0.02。这是迄今为止在这个红移范围内最大的SNIa光谱集。光谱连同其最佳拟合光谱SNIa模型和主机模型在相关的。在后一种情况下，还呈现了主体减去的光谱。我们产生的平均光谱的前最大值，最大值和后最大的时代为两个z <0.5 and z>=0.5 SNeIa。我们发现z <0.5 spectra have deeper intermediate mass element absorptions than z>= 0.5的光谱。与红移的差异是一致的选择更明亮和更蓝的超新星在更高的红移。
英文摘要：
We present 139 spectra of 124 Type Ia supernovae (SNeIa) that were observed at the ESO/VLT during the first three years of the Canada-France-Hawai Telescope (CFHT) Supernova Legacy Survey (SNLS). This homogeneous data set is used to test for redshift evolution of SNeIa spectra, and will be used in the SNLS 3rd year cosmological analyses. Spectra have been reduced and extracted with a dedicated pipeline that uses photometric information from deep CFHT Legacy Survey (CFHT-LS) reference images to trace, at sub-pixel accuracy, the position of the supernova on the spectrogram as a function of wavelength. It also separates the supernova and its host light in 60% of cases. The identification of the supernova candidates is performed using a spectrophotometric SNIa model. A total of 124 SNeIa, roughly 50% of the overall SNLS spectroscopic sample, have been identified using the ESO/VLT during the first three years of the survey. Their redshifts range from z=0.149 to z=1.031. The average redshift of the sample is z=0.63+/-0.02. This constitutes the largest SNIa spectral set to date in this redshift range. The spectra are presented along with their best-fit spectral SNIa model and a host model where relevant. In the latter case, a host subtracted spectrum is also presented. We produce average spectra for pre-maximum, maximum and post-maximum epochs for both z<0.5 and z>=0.5 SNeIa. We find that z<0.5 spectra have deeper intermediate mass element absorptions than z>= 0.5 spectra. The differences with redshift are consistent with the selection of brighter and bluer supernovae at higher redshift.
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