论文标题
伽玛射线爆发无线电余星量如何？
How are gamma-ray burst radio afterglows populated?
论文作者
论文摘要
我们系统地分析了三个GRB样品，分别为无线电，无线电和无余气。结果表明，无需无需进行无线电的二分法。有趣的是，我们发现及时的持续时间（$ t_ {int} $），迅速的伽马射线（$ e_ {γ，ISO} $）的各向同性能量以及其主机星系的红移（$ z $）都是针对无线电和无线电的广播样本进行的逻辑 - 正态分布。基于$ t_ {int} $，$ e_ {γ，iso} $的独特分布，圆周中等密度（$ n $）和无线电量的各向异性等效能量（$ l_ {c {ν，p} $），我们确认GRB无线电的效果是更好地分配给GRB Afterglows to nos dim dim dim dim dim dim dim night and the Bright类型。但是，值得注意的是，从两类无线电倒数类的主机星系中，通量密度（$ f_ {host} $）的分布在本质上非常相似。同时，我们指出，根据$ t_ {int} $的累积频率分布和$ e_ {γ，ISO} $，与上述两个样本显然与上述两个样本不同，以及$ t_ {int} $和$ z $。此外，$ e_ {γ，ISO} $与$ l_ {ν，p} $之间的正相关性是在无线电大通样品中找到的，尤其是对于超新星相关的GRB。此外，我们还发现在放射测量样品中这种正相关。 $ t_ {int} $和$ z $之间的负相关也可以确认为放射定价样品。其余框架中短grb之间的分界线为$ t_ {int} \ simeq $ 1 s。因此，我们建议无线电，无线电定价和无线电GRB可以起源于不同的祖细胞。
We systematically analyze three GRB samples named as radio-loud, radio-quiet and radio-none afterglows, respectively. It is shown that dichotomy of the radio-loud afterglows is not necessary. Interestingly, we find that the intrinsic durations ($T_{int}$), isotropic energies of prompt gamma-rays ($E_{γ, iso}$) and redshifts ($z$) of their host galaxies are log-normally distributed for both the radio-loud and radio-quiet samples except those GRBs without any radio detections. Based on the distinct distributions of $T_{int}$, $E_{γ, iso}$, the circum-burst medium density ($n$) and the isotropic equivalent energy of radio afterglows ($L_{ν,p}$), we confirm that the GRB radio afterglows are really better to be divided into the dim and the bright types. However, it is noticeable that the distributions of flux densities ($F_{host}$) from host galaxies of both classes of radio afterglows are intrinsically quite similar. Meanwhile, we point out that the radio-none sample is also obviously different from the above two samples with radio afterglows observed, according to the cumulative frequency distributions of the $T_{int}$ and the $E_{γ, iso}$, together with correlations between $T_{int}$ and $z$. In addition, a positive correlation between $E_{γ, iso}$ and $L_{ν,p}$ is found in the radio-loud samples especially for the supernova-associated GRBs. Besides, we also find this positive correlation in the radio-quiet sample. A negative correlation between $T_{int}$ and $z$ is confirmed to hold for the radio-quiet sample too. The dividing line between short and long GRBs in the rest frame is at $T_{int}\simeq$1 s. Consequently, we propose that the radio-loud, the radio-quiet and the radio-none GRBs could be originated from different progenitors.
