论文标题
$ z \ sim 0.8 $的短GRB 161104a的遥远的星系集群环境，与短GRB宿主人群进行了比较
The distant, galaxy cluster environment of the short GRB 161104A at $z\sim 0.8$ and a comparison to the short GRB host population
论文作者
论文摘要
我们介绍了Swift短期伽马射线爆发（GRB）GRB 161104A及其主机银河系的光学观察结果，$ z = 0.793 \ pm 0.003 $。我们用恒星群体推理代码前瞻性对多播的光度法和光谱进行了建模，并使用嵌套采样探索后验。我们发现，大规模加权年龄$ t_m = 2.12^{+0.23} _ { - 0.21} $ 〜gyr，stellar Mass $ \ log {（m/m_ \ odot）} = 10.21 = 10.21 \ pm 0.04 $，Metalicity $ \ log \ log \ log \ log {z/z _ \ odot）}} 0.08^{+0.05} _ { - 0.06} $，灰尘灭绝$ a_v = 0.08^{+0.08} _ { - 0.05} $ mag和恒星形成率$ \ text {sfrate {sfr} = 9.9 = 9.9 \ times 10^times 10^{ - 2} m_ \ odot $ $ $ $ $ $ y〜y〜这些特性，以及突出的4000 Angstrom断裂和光吸收线将该宿主分类为早期类型的静态星系。使用黑暗能源调查的银河系目录，我们证明了GRB 161104A的宿主位于银河集群的郊区，$ z \约0.8 $，位于可能最亮的集群星系中$ \ 1 $ MPC。我们还提出了20个额外的20个短GRB主机（$ \ of $ \％$ $的新建模），其中是早期类型星系），找到了$ \ log（m/m_ \ odot）= 9.94^{+0.88} _ { - 0.88} _ { - 0.98} $ and { - 0.88} $ { - 0.98} $ and $ t_m = 1.07^$ 1.98} $ 1.98} （$ 68 \％$置信度）。我们进一步发现，GRB 161104a的宿主比其他四个与星系簇相关的Short GRB宿主更遥远，更大和年轻。簇短grb具有淡淡的余波，在下$ \ \ \％$（$ \ 30 \％$）中，观察到的X射线（光学）发光度。我们对星系簇中短GRB的比例限制了$ \ \ \ \％$ 5-13 \％$的那些，这与Redshifts $ 0.1 \ leq Z \ leq leq leq leq 0.8 $的星系群中的恒星质量$ \％$ \％$ \％$ \％一致。
We present optical observations of the Swift short-duration gamma-ray burst (GRB) GRB 161104A and its host galaxy at $z=0.793 \pm 0.003$. We model the multiband photometry and spectroscopy with the stellar population inference code Prospector, and explore the posterior using nested sampling. We find that the mass-weighted age $t_m = 2.12^{+0.23}_{-0.21}$~Gyr, stellar mass $\log{(M/M_\odot)} = 10.21 \pm 0.04$, metallicity $\log{(Z/Z_\odot)} = 0.08^{+0.05}_{-0.06}$, dust extinction $A_V = 0.08^{+0.08}_{-0.05}$ mag, and the star formation rate $\text{SFR} = 9.9 \times 10^{-2} M_\odot$~yr$^{-1}$. These properties, along with a prominent 4000 Angstrom break and optical absorption lines classify this host as an early-type, quiescent galaxy. Using Dark Energy Survey galaxy catalogues, we demonstrate that the host of GRB 161104A resides on the outskirts of a galaxy cluster at $z\approx 0.8$, situated $\approx 1$ Mpc from the likely brightest cluster galaxy. We also present new modeling for 20 additional short GRB hosts ($\approx33\%$ of which are early-type galaxies), finding population medians of $\log(M/M_\odot) = 9.94^{+0.88}_{-0.98}$ and $t_m = 1.07^{+1.98}_{-0.67}$~Gyr ($68\%$ confidence). We further find that the host of GRB 161104A is more distant, less massive, and younger than the four other short GRB hosts known to be associated with galaxy clusters. Cluster short GRBs have faint afterglows, in the lower $\approx 11\%$ ($\approx 30\%$) of observed X-ray (optical) luminosities. We place a lower limit on the fraction of short GRBs in galaxy clusters versus those in the field of $\approx 5-13\%$, consistent with the fraction of stellar mass $\approx 10-20\%$ in galaxy clusters at redshifts $0.1 \leq z \leq 0.8$.
