论文标题
用詹姆斯·韦伯太空望远镜在z <5处检测稳定的超新星
Detecting Pair-Instability Supernovae at z<5 with the James Webb Space Telescope
论文作者
论文摘要
配对超新星（Pisne）是最终的宇宙灯塔，能够在z <25处观察到，并揭示了宇宙黎明处原始恒星的特性。但是现在可以理解，这些事件的光谱和光曲线随红移而演变，因为宇宙被重元素污染，因为在这种质量范围内化学丰富的恒星通常会丢失大部分氢信封并爆炸为裸氦芯。如今，此类瞬态的光曲线在近红外（NIR）中可能比相等能量和祖细胞质量的原始Pisne的光曲线要昏暗。在这里，我们计算了PISNE的检测率，其祖细胞的外层将其外层损失到Z <10的线驱动风或旋转，这是詹姆斯·韦伯太空望远镜（JWST）的红移的检测极限。我们发现JWST可能只能在Z <4的红移范围内检测到POP II（金属贫困）Pisne，但不能检测其POP III（无金属）对应物。
Pair-instability supernovae (PISNe) are the ultimate cosmic lighthouses, capable of being observed at z<25 and revealing the properties of primordial stars at cosmic dawn. But it is now understood that the spectra and light curves of these events evolved with redshift as the universe became polluted with heavy elements because chemically enriched stars in this mass range typically lose most of their hydrogen envelopes and explode as bare helium cores. The light curves of such transients can be considerably dimmer in the near infrared (NIR) today than those of primordial PISNe of equal energy and progenitor mass. Here, we calculate detection rates for PISNe whose progenitors lost their outer layers to either line-driven winds or rotation at z<10, their detection limit in redshift for the James Webb Space Telescope (JWST). We find that JWST may be able to detect only Pop II (metal-poor) PISNe over the redshift range of z<4, but not their Pop III (metal-free) counterparts.
