arXiv 2207.047802022-07-11astro-ph.CO

在近红外线中检验Ia型超新星的均匀性以进行精确的距离估算

Testing the Homogeneity of Type Ia Supernovae in the Near-Infrared for Accurate Distance Estimations

T. E. Müller-Bravo, L. Galbany, E. Karamehmetoglu, M. Stritzinger, C. Burns, K. Phan, A. Iáñez Ferres, J. P. Anderson, C. Ashall, E. Baron, P. Hoeflich, E. Y. H… 展开作者

T. E. Müller-Bravo, L. Galbany, E. Karamehmetoglu, M. Stritzinger, C. Burns, K. Phan, A. Iáñez Ferres, J. P. Anderson, C. Ashall, E. Baron, P. Hoeflich, E. Y. Hsiao, T. de Jaeger, S. Kumar, J. Lu, M. M. Phillips, M. Shahbandeh, N. Suntzeff, S. A. Uddin

备注：: Accepted in A&A
发表信息：: A&A 665, A123 (2022)
DOI：: 10.1051/0004-6361/202243845

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摘要：

Ia型超新星（SNe Ia）已经被广泛地用作光学标准化烛光几十年了。然而，超新星Ia在近红外（NIR）中表现出更均匀的特性，其中尘埃消光的影响也被减弱。在这项工作中，我们探讨了使用少量的近红外观测准确的距离估计的可能性，在这些波长的均匀性。我们发现，$J$和/或$H$频带中的一个历元，加上良好的$gr$频带覆盖，给出了$J$（$J_{max}$）和$H$（$H_{max}$）频带中峰值幅度的准确估计。单个NIR历元的使用仅在$B$ -频带峰值幅度（$T_{max}$）的时间附近的历元中引入$\sim0.05$ mag的额外散射。我们还测试了光学节奏和信噪比（S/N）的影响，估计$T_{max}$和其不确定性传播的近红外峰值幅度。节奏和S/N具有类似的贡献，其中我们将每个的引入散射约束为$J_{max}$中的$<0.02$ mag和$H_{max}$中的$<0.01$。然而，如果数据质量与附近SNe（$z\lesssim0.1$）的观测结果相当，这些影响预计可以忽略不计。同时还对近红外光谱中信噪比的影响进行了测试。对于位于$0.08<z\lesssim0.1$的Ia超新星，必须进行信噪比比CSP样品更好的近红外观测，以将引入的散射限制在最小值（$\lesssim0.05$等）。这些结果为我们的FLOWS项目提供了信心，该项目旨在使用具有公共ZTF光学光变曲线和少数NIR历元的SNe Ia来绘制局部宇宙的奇特速度场。这将使我们能够确定暗物质在我们自己的超星系团Laniakea中的分布，并通过测量结构的增长率来测试标准宇宙学模型，参数为$fD$和哈勃-勒梅特常数$H_0$。

英文摘要：

Type Ia Supernovae (SNe Ia) have been extensively used as standardisable candles in the optical for several decades. However, SNe Ia have shown to be more homogeneous in the near-infrared (NIR), where the effect of dust extinction is also attenuated. In this work, we explore the possibility of using a low number of NIR observations for accurate distance estimations, given the homogeneity at these wavelengths. We found that one epoch in $J$ and/or $H$ band, plus good $gr$-band coverage, gives an accurate estimation of peak magnitudes in $J$ ($J_{max}$) and $H$ ($H_{max}$) bands. The use of a single NIR epoch only introduces an additional scatter of $\sim0.05$ mag for epochs around the time of $B$-band peak magnitude ($T_{max}$). We also tested the effect of optical cadence and signal-to-noise ratio (S/N) in the estimation of $T_{max}$ and its uncertainty propagation to the NIR peak magnitudes. Both cadence and S/N have a similar contribution, where we constrained the introduced scatter of each to $<0.02$ mag in $J_{max}$ and $<0.01$ in $H_{max}$. However, these effects are expected to be negligible, provided the data quality is comparable to that obtained for observations of nearby SNe ($z\lesssim0.1$). The effect of S/N in the NIR was tested as well. For SNe Ia at $0.08<z\lesssim0.1$, NIR observations with better S/N than that found in the CSP sample is necessary to constrain the introduced scatter to a minimum ($\lesssim0.05$ mag). These results provide confidence for our FLOWS project that aims in using SNe Ia with public ZTF optical light curves and few NIR epochs to map out the peculiar velocity field of the local Universe. This will allow us to determine the distribution of dark matter in our own supercluster, Laniakea, and test the standard cosmological model by measuring the growth rate of structures, parameterised by $fD$, and the Hubble-Lemaître constant, $H_0$.

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