再论Arp299的核心坍缩超新星速率
The Core-Collapse Supernova Rate in Arp299 Revisited
摘要：
我们提出了一个研究的CCSN率在核A和B1的亮红外星系Arp 299，基于11年的甚大阵列监测其无线电发射在8.4 GHz的。在没有高分辨率甚长基线干涉测量观测的情况下，核射电通量密度的显著变化可用于确定CCSN的活动。在B1核的情况下，其测量到的弥散射电辐射的微小变化低于射电超新星的预期通量，因此非常适合通过通量密度变化来探测RSNe。事实上，我们找到了至少三个RSNe的强有力证据，这导致CCSN率的下限为每年0.28 +/- 0.16。在A核中，我们没有检测到任何显着的变异性，并发现SN检测阈值亮度仅允许检测已知最亮的RSNe。我们的方法基本上对A核内发生的正常CCSN爆炸是盲目的，这导致核通量密度的变化太小，仍然被核本身的强扩散辐射所稀释。此外，我们试图找到近红外对应的早期报道的RSNe在Arp 299核A，通过比较近红外自适应光学图像从Gemini-N望远镜与同期的欧洲VLBI网络的意见。然而，我们无法在核A的最内部区域内检测到报告的射电SNe的NIR对应物。虽然我们的近红外观测对距核A中心300 mas处的典型CCSNe敏感，但在A_v~15 mag处会发生消光，而对核最内侧区域的这种高度遮蔽的SNe不敏感，因为在那里大多数EVN源都被探测到。（节略）
英文摘要：
We present a study of the CCSN rate in nuclei A and B1 of the luminous infrared galaxy Arp299, based on 11 years of Very Large Array monitoring of their radio emission at 8.4 GHz. Significant variations in the nuclear radio flux density can be used to identify the CCSN activity in the absence of high-resolution very long baseline interferometry observations. In the case of the B1-nucleus, the small variations in its measured diffuse radio emission are below the fluxes expected from radio supernovae, thus making it well-suited to detect RSNe through flux density variability. In fact, we find strong evidence for at least three RSNe this way, which results in a lower limit for the CCSN rate of 0.28 +/- 0.16 per year. In the A-nucleus, we did not detect any significant variability and found a SN detection threshold luminosity which allows only the detection of the most luminous RSNe known. Our method is basically blind to normal CCSN explosions occurring within the A-nucleus, which result in too small variations in the nuclear flux density, remaining diluted by the strong diffuse emission of the nucleus itself. Additionally, we have attempted to find near-infrared counterparts for the earlier reported RSNe in the Arp299 nucleus A, by comparing NIR adaptive optics images from the Gemini-N telescope with contemporaneous observations from the European VLBI Network. However, we were not able to detect NIR counterparts for the reported radio SNe within the innermost regions of nucleus A. While our NIR observations were sensitive to typical CCSNe at 300 mas from the centre of the nucleus A, suffering from extinction up to A_v~15 mag, they were not sensitive to such highly obscured SNe within the innermost nuclear regions where most of the EVN sources were detected. (abridged)
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