论文标题
I型超浮肿超新星SN 2017EGM的宿主星系的空间分辨分子气体特性
Spatially Resolved Molecular Gas Properties of Host Galaxy of Type I Superluminous Supernova SN 2017egm
论文作者
论文摘要
我们通过使用Atacama大毫米/外数阵列，介绍了I型超浮肿超新星（SLSN-I）的CO（1-0）观察结果，SN2017EGM，SN2017EGM，SN2017EGM，Z = 0.03063的最接近SLSNE-I之一。主机星系的分子气体为$ M _ {\ rm GAS} =（4.8 \ pm 0.3）\ times 10^9 $ $ M _ {\ odot} $，将其放在$ M _ {\ rm rm-rm gas} $ - star-forment速率（s s Star-formation fare）中。 SN2017EGM位置的分子氢柱密度高于同一宿主星系中的II型SN PTF10BGL的分子密度，以及位于不同星系中的其他II型和IA SNE的分子氢密度，这表明SLSNE-i具有浓厚的分子气体环境。另一方面，SN2017EGM位置的柱密度与IBC SNE型的柱密度相当。 SN2017EGM位置的分子气体和SFR的表面密度与空间分辨的局部恒星形成星系一致，并遵循Schmidt-Kennicutt的关系。这些事实表明，SLSNE-I可以发生在具有与正常星形星系相同的星形形成机理的环境中。
We present the results of CO(1-0) observations of the host galaxy of a Type I superluminous supernova (SLSN-I), SN2017egm, one of the closest SLSNe-I at z = 0.03063, by using the Atacama Large Millimeter/submillimeter Array. The molecular gas mass of the host galaxy is $M_{\rm gas} = (4.8 \pm 0.3) \times 10^9$ $M_{\odot}$, placing it on the sequence of normal star-forming galaxies in an $M_{\rm gas}$-star-formation rate (SFR) plane. The molecular hydrogen column density at the location of SN2017egm is higher than that of the Type II SN PTF10bgl, which is also located in the same host galaxy, and those of other Type II and Ia SNe located in different galaxies, suggesting that SLSNe-I have a preference for a dense molecular gas environment. On the other hand, the column density at the location of SN2017egm is comparable to those of Type Ibc SNe. The surface densities of molecular gas and the SFR at the location of SN2017egm are consistent with those of spatially resolved local star-forming galaxies and follow the Schmidt-Kennicutt relation. These facts suggest that SLSNe-I can occur in environments with the same star-formation mechanism as in normal star-forming galaxies.
