2010年极高能gamma-ray耀斑& M 87多波长观测的10年
The 2010 very high energy gamma-ray flare & 10 years of multi-wavelength observations of M 87
摘要：
摘要：巨大的射电星系M 87及其邻近的著名喷流和超大质量黑洞提供了一个独特的机会来研究相对论外流和超大质量黑洞周围产生的极高能量（VHE; E>100 GeV）伽马射线辐射的起源。M 87自2006年以来一直是VHE伽马射线发射器。VHE伽马射线发射在短至一天的时间尺度上显示出强烈的可变性。本文报道了2010年MAGIC和VERITAS仪器对M87进行的VHE联合监测活动的结果。在活动期间，在VHE检测到耀斑，触发了在VHE（H.E.S.S.）的进一步观测，X射线（Chandra）和无线电（43 GHz VLBA）。VHE伽马射线光变曲线的出色采样使人们能够获得耀斑的精确时间特性：单个孤立的耀斑可以很好地描述为具有显著不同通量上升和衰减时间的双侧指数函数。虽然2010年耀斑的总体变率模式似乎与2005年和2008年的VHE耀斑有些不同，但它们具有非常相似的时间尺度（~天）、峰值通量（Φ（>0.35 TeV）~=（1-3）x 10^-11 ph cm^-2 s^-1）和VHE光谱。43 GHz VLBA射电观测的内喷流区域表明，在2010年没有增强的流量在2008年的观测，其中增加的无线电通量的最内核区域的VHE耀斑相吻合。另一方面，在VHE伽马射线发射峰值后约3天进行的钱德拉X射线观测显示，来自核心的通量增强。M 87的长期（2001-2010）多波长光变曲线，从无线电到VHE，包括来自HST，LT，VLA和EVN的数据，用于进一步研究VHE伽马射线发射的起源。三个VHE耀斑没有独特的，共同的MWL签名已被确定。
英文摘要：
Abridged: The giant radio galaxy M 87 with its proximity, famous jet, and very massive black hole provides a unique opportunity to investigate the origin of very high energy (VHE; E>100 GeV) gamma-ray emission generated in relativistic outflows and the surroundings of super-massive black holes. M 87 has been established as a VHE gamma-ray emitter since 2006. The VHE gamma-ray emission displays strong variability on timescales as short as a day. In this paper, results from a joint VHE monitoring campaign on M 87 by the MAGIC and VERITAS instruments in 2010 are reported. During the campaign, a flare at VHE was detected triggering further observations at VHE (H.E.S.S.), X-rays (Chandra), and radio (43 GHz VLBA). The excellent sampling of the VHE gamma-ray light curve enables one to derive a precise temporal characterization of the flare: the single, isolated flare is well described by a two-sided exponential function with significantly different flux rise and decay times. While the overall variability pattern of the 2010 flare appears somewhat different from that of previous VHE flares in 2005 and 2008, they share very similar timescales (~day), peak fluxes (Phi(>0.35 TeV) ~= (1-3) x 10^-11 ph cm^-2 s^-1), and VHE spectra. 43 GHz VLBA radio observations of the inner jet regions indicate no enhanced flux in 2010 in contrast to observations in 2008, where an increase of the radio flux of the innermost core regions coincided with a VHE flare. On the other hand, Chandra X-ray observations taken ~3 days after the peak of the VHE gamma-ray emission reveal an enhanced flux from the core. The long-term (2001-2010) multi-wavelength light curve of M 87, spanning from radio to VHE and including data from HST, LT, VLA and EVN, is used to further investigate the origin of the VHE gamma-ray emission. No unique, common MWL signature of the three VHE flares has been identified.
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