We collected the information of 304 gamma-ray bursts (GRBs) from the literature, and analyzed the correlations among the host galaxy offsets (the distance from the site of the GRB to the center of its host galaxy), $T_{\mathrm{90},\mathrm{i}}$ (the duration $T_{\mathrm{90}}$ in rest-frame), $T_{\mathrm{R45},\mathrm{i}}$ (the duration $T_{\mathrm{R45}}$ in rest-frame), $E_{\mathit{\gamma },\mathrm{iso}}$ (the isotropic equivalent energy), $L_{\mathit{\gamma },\mathrm{iso}}$ ($=E_{\mathit{\gamma },\mathrm{iso}}/T_{\mathrm{90},\mathrm{i}}$, the isotropic equivalent luminosity) and $L_{\mathrm{pk}}$ (peak luminosity). We found that $T_{\mathrm{90},\mathrm{i}}$, $T_{\mathrm{R45},\mathrm{i}}$, $E_{\mathit{\gamma },\mathrm{iso}}$, $L_{\mathrm{pk}}$ have negative correlation with offset, which is consistent with origin of short GRBs (SGRBs) and long GRBs (LGRBs). On separate analysis, we found similar results for $\log E_{\mathit{\gamma },\mathrm{iso}}-\log (\mathrm{offset})$ and $\log L_{\mathrm{pk}}-\log (\mathrm{offset})$ relations in case of SGRBs only, while no obvious relation for LGRBs. There is no correlations between offset and $L_{\mathit{\gamma },\mathrm{iso}}$. We also put the special GRB 170817A and GRB 060218A on the plots. The two GRBs both have low luminosity and small offset. In the $\log (\mathrm{offset})-\log T_{\mathrm{90},\mathrm{i}}$ plot, we found GRB 170817A locates in between the two regions of SGRBs and LGRBs and it is the outlier in the $\mathrm{offset}-E_{\mathit{\gamma },\mathrm{iso}}$, $\mathrm{offset}-L_{\mathit{\gamma },\mathrm{iso}}$ and $\mathrm{offset}-L_{\mathrm{pk}}$ plots. Together with GRB 060218A being an outlier in all plots, it indicates the speciality of GRBs 170817A and 060218A, and might imply more subgroups of the GRB samples.

我们从文献中收集了304个伽马射线暴（GRB）的信息，并分析了宿主星系偏移量（从GRB的位置到其宿主星系中心的距离）之间的相关性， ${Ť}_{\mathrm{90}，\mathrm{一世}}$ （持续时间 ${Ť}_{\mathrm{90}}$ 在其余帧中）， ${Ť}_{\mathrm{R45}，\mathrm{一世}}$ （持续时间 ${Ť}_{\mathrm{R45}}$ 在其余帧中）， ${Ë}_{\mathit{\gamma }，\mathrm{iso}}$ （各向同性等效能量）， ${\mathrm{大号}}_{\mathit{\gamma }，\mathrm{iso}}$ （$={Ë}_{\mathit{\gamma }，\mathrm{iso}}/{Ť}_{\mathrm{90}，\mathrm{一世}}$，各向同性等效光度）和 ${\mathrm{大号}}_{\mathrm{pk}}$（峰值亮度）。我们发现${Ť}_{\mathrm{90}，\mathrm{一世}}$， ${Ť}_{\mathrm{R45}，\mathrm{一世}}$， ${Ë}_{\mathit{\gamma }，\mathrm{iso}}$， ${\mathrm{大号}}_{\mathrm{pk}}$与偏移量呈负相关，这与短GRB（SGRB）和长GRB（LGRB）的起源一致。在单独的分析中，我们发现$\mathrm{日志}{Ë}_{\mathit{\gamma }，\mathrm{iso}}-\mathrm{日志}（\mathrm{抵消}）$ 和 $\mathrm{日志}{\mathrm{大号}}_{\mathrm{pk}}-\mathrm{日志}（\mathrm{抵消}）$仅在SGRB的情况下存在关系，而与LGRB的关系则不明显。偏移量和${\mathrm{大号}}_{\mathit{\gamma }，\mathrm{iso}}$。我们还将特殊GRB 170817A和GRB 060218A放在地块上。两个GRB均具有较低的亮度和较小的偏移。在里面$\mathrm{日志}（\mathrm{抵消}）-\mathrm{日志}{Ť}_{\mathrm{90}，\mathrm{一世}}$ 图中，我们发现GRB 170817A位于SGRB和LGRB的两个区域之间，它是 $\mathrm{抵消}-{Ë}_{\mathit{\gamma }，\mathrm{iso}}$， $\mathrm{抵消}-{\mathrm{大号}}_{\mathit{\gamma }，\mathrm{iso}}$ 和 $\mathrm{抵消}-{\mathrm{大号}}_{\mathrm{pk}}$情节。与GRB 060218A在所有图中都是一个异常值一起，它表明GRB 170817A和060218A的特长，并且可能意味着GRB样本的更多子组。