光学无偏GRB主机（TOUGH）调查。VI。z<1时的射电观测和与典型恒星形成星系的一致性
The optically unbiased GRB host (TOUGH) survey. VI. Radio observations at z<1 and consistency with typical star-forming galaxies
摘要：
本文的目的是确定在一个样本的伽马射线暴（GRB）主机的模糊恒星形成活动和尘埃衰减的水平，并测试的假设，即GRB主机具有与一般恒星形成星系人口的属性一致。我们提出了一个无线电连续调查的所有z<1伽玛暴主机的光学无偏伽玛暴主机（TOUGH）样本补充无线电数据的所有（主要是前斯威夫特）GRB-SN主机发现2006年10月之前。我们提出了新的无线电数据的22个对象，并已获得检测其中三个（GRB 980425，021211，031203;没有在TOUGH样本），增加了无线电检测到的GRB主机的数量从两个到五个。GRB 021211宿主星系的恒星形成率（SFR）为~825 Mo yr^-1，是迄今为止所报道的GRB宿主星系的最高值，因此将其归入超亮红外星系的范畴。我们发现，至少有63%的伽玛暴宿主的SFR < 100 Mo yr^-1，最多有8%的宿主的SFR > 500 Mo yr^-1。对于未被探测到的宿主，平均射电通量（<35 μ Jy 3 σ）对应于平均SFR < 15 Mo yr^-1。此外，约88%的z<1的GRB宿主的紫外尘埃衰减A_UV < 6.7 mag（可见衰减A_V < 3 mag）。因此，我们没有发现大部分伽玛射线暴宿主中存在大尘埃遮蔽的证据。最后，我们发现GRB宿主星系的SFR和AUV分布与Lyman break星系、具有相似红移的H α发射体以及宇宙学模拟的星系的分布一致。伽马射线暴与其他恒星形成星系的相似性与伽马射线暴的假设是一致的，至少在z<1时，伽马射线暴追踪了所有恒星形成的很大一部分，因此比以前认为的偏差更小。
英文摘要：
The objective of this paper is to determine the level of obscured star formation activity and dust attenuation in a sample of gamma-ray burst (GRB) hosts; and to test the hypothesis that GRB hosts have properties consistent with those of the general star-forming galaxy populations. We present a radio continuum survey of all z<1 GRB hosts in The Optically Unbiased GRB Host (TOUGH) sample supplemented with radio data for all (mostly pre-Swift) GRB-SN hosts discovered before October 2006. We present new radio data for 22 objects and have obtained a detection for three of them (GRB 980425, 021211, 031203; none in the TOUGH sample), increasing the number of radio-detected GRB hosts from two to five. The star formation rate (SFR) for the GRB 021211 host of ~825 Mo yr^-1, the highest ever reported for a GRB host, places it in the category of ultraluminous infrared galaxies. We found that at least 63% of GRB hosts have SFR < 100 Mo yr^-1 and at most 8% can have SFR > 500 Mo yr^-1. For the undetected hosts the mean radio flux (<35 uJy 3sigma) corresponds to an average SFR < 15 Mo yr^-1. Moreover, ~88% of the z<1 GRB hosts have ultraviolet dust attenuation A_UV < 6.7 mag (visual attenuation A_V < 3 mag). Hence we did not find evidence for large dust obscuration in a majority of GRB hosts. Finally, we found that the distributions of SFRs and A_UV of GRB hosts are consistent with those of Lyman break galaxies, Halpha emitters at similar redshifts and of galaxies from cosmological simulations. The similarity of the GRB population with other star-forming galaxies is consistent with the hypothesis that GRBs, a least at z<1, trace a large fraction of all star formation, and are therefore less biased indicators than once thought.
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