A Hubble Space Telescope survey of the host galaxies of Superluminous Supernovae
A Hubble Space Telescope survey of the host galaxies of Superluminous Supernovae
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DOI：
10.1093/mnras/stw063
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发表时间：
2016-01
影响因子：
4.8
通讯作者：
C. Angus;A. Levan;D. Perley;N. Tanvir;J. Lyman;E. Stanway;A. Fruchter
中科院分区：
文献类型：
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作者：
C. Angus;A. Levan;D. Perley;N. Tanvir;J. Lyman;E. Stanway;A. Fruchter
我们展示了哈勃太空望远镜 (HST) 宽视场相机 3 对 21 个超光度超新星 (SLSNe) 宿主星系进行紫外和近红外 (nIR) 成像，为宿主内的恒星形成和恒星质量提供了灵敏的探测。将这些宿主星系的光度和形态特性与核心塌缩超新星（CCSNe）和长持续时间伽马射线暴（LGRB）进行比较，我们发现SLSN宿主在紫外和近红外波长下都更暗且更紧凑，在某些情况下，我们几乎无法恢复绝对星等在M_V ≈ -14左右的宿主。通过添加地面光学观测和档案结果，我们产生了适合这些宿主的光谱能量分布，并表明 SLSN 宿主具有较低的恒星质量和恒星形成率。这对于缺乏氢的 I 型 SLSN 宿主来说最为明显，尽管富含 H 的 II 型 SLSN 宿主星系仍然与大部分 CCSNe 不同，跨越了非常广泛的绝对星等范围，约 30% 的 SLSNe-II 源自比 M_(nIR) ∼ -14 更暗的星系。对我们最微弱的 SLSN 宿主的检测增加了 SLSNe-I 宿主在恒星形成率和恒星质量方面与 LGRB 不同的置信度，并表明金属丰度的明显相似性可能是由于发射线金属丰度测量可行的宿主比例有限。 SLSN-II 主体的广泛光度范围很难通过金属丰度削减来描述，并且与任何合理的紫外线加权光度函数的预期不符，这表明可能需要额外的环境限制来产生富氢的 SLSNe。
We present Hubble Space Telescope (HST) Wide Field Camera 3 UV and near-IR (nIR) imaging of 21 Superluminous Supernovae (SLSNe) host galaxies, providing a sensitive probe of star formation and stellar mass within the hosts. Comparing the photometric and morphological properties of these host galaxies with those of core-collapse supernovae (CCSNe) and long-duration gamma-ray bursts (LGRBs), we find SLSN hosts are fainter and more compact at both UV and nIR wavelengths, in some cases we barely recover hosts with absolute magnitude around M_V ≈ −14. With the addition of ground based optical observations and archival results, we produce spectral energy distribution fits to these hosts, and show that SLSN hosts possess lower stellar mass and star formation rates. This is most pronounced for the hydrogen deficient Type-I SLSN hosts, although Type-II H-rich SLSN host galaxies remain distinct from the bulk of CCSNe, spanning a remarkably broad range of absolute magnitudes, with ∼30 per cent of SLSNe-II arising from galaxies fainter than M_(nIR) ∼ −14. The detection of our faintest SLSN hosts increases the confidence that SLSNe-I hosts are distinct from those of LGRBs in star formation rate and stellar mass, and suggests that apparent similarities in metallicity may be due to the limited fraction of hosts for which emission line metallicity measurements are feasible. The broad range of luminosities of SLSN-II hosts is difficult to describe by metallicity cuts, and does not match the expectations of any reasonable UV-weighted luminosity function, suggesting additional environmental constraints are likely necessary to yield hydrogen rich SLSNe.