THE DISTANCE TO NOVA V959 MON FROM VLA IMAGING
THE DISTANCE TO NOVA V959 MON FROM VLA IMAGING
复制标题
DOI：
10.1088/0004-637x/805/2/136
复制
发表时间：
2015-03
期刊：
影响因子：
--
通讯作者：
J. Linford;Valério A. R. M. Ribeiro;Valério A. R. M. Ribeiro;L. Chomiuk;T. Nelson;J. Sokoloski;M. Rupen;K. Mukai;K. Mukai;Tim O'Brien;A. Mioduszewski;J. Weston
中科院分区：
文献类型：
--
作者：
J. Linford;Valério A. R. M. Ribeiro;Valério A. R. M. Ribeiro;L. Chomiuk;T. Nelson;J. Sokoloski;M. Rupen;K. Mukai;K. Mukai;Tim O'Brien;A. Mioduszewski;J. Weston
确定经典新星的可靠距离是推导其喷射质量和爆炸能量的一个具有挑战性但关键的步骤。在这里，我们结合联合收割机无线电膨胀测量从卡尔G。Jansky甚大天线阵的速度来自光谱，以估计新星V959 Mon的膨胀视差，这是通过其γ射线发射发现的第一颗新星。我们在空间上解决了新星在4.5-36.5 GHz的频率在9个不同的成像时期。前五个时期涵盖了从2012年10月到2013年1月的喷出物扩张，而最后四个时期跨越2014年2月至5月。这些观测对应于第一次探测到新星后的第126天至199天和第615天至703天。这些图像清楚地显示了非球形喷出物的几何形状。利用从光谱学的三维模型中导出的喷出物速度，射电膨胀意味着距离在0.9 ± 0.2和2.2 ± 0.4 kpc之间，最可能的距离为1.4 ± 0.4 kpc。这个距离意味着γ射线的亮度为0.6 × 1035？> erg s−1，比原型的γ射线探测新星V407 Cyg小得多，可能是因为V959 Mon系统中缺乏红巨星伴星。V959 Mon的γ射线光度也比迄今为止在γ射线中检测到的其他经典新星低得多，表明这些爆炸的γ射线光度范围至少为10倍。
Determining reliable distances to classical novae is a challenging but crucial step in deriving their ejected masses and explosion energetics. Here we combine radio expansion measurements from the Karl G. Jansky Very Large Array with velocities derived from optical spectra to estimate an expansion parallax for nova V959 Mon, the first nova discovered through its γ-ray emission. We spatially resolve the nova at frequencies of 4.5–36.5 GHz in nine different imaging epochs. The first five epochs cover the expansion of the ejecta from 2012 October to 2013 January, while the final four epochs span 2014 February–May. These observations correspond to days 126 through 199 and days 615 through 703 after the first detection of the nova. The images clearly show a non-spherical ejecta geometry. Utilizing ejecta velocities derived from three-dimensional modeling of optical spectroscopy, the radio expansion implies a distance between 0.9 ± 0.2 and 2.2 ± 0.4 kpc, with a most probable distance of 1.4 ± 0.4 kpc. This distance implies a γ-ray luminosity of 0.6 × 10 35 ?> erg s−1, which is much less than the prototype γ-ray-detected nova, V407 Cyg, possibly due to the lack of a red giant companion in the V959 Mon system. V959 Mon also has a much lower γ-ray luminosity than other classical novae detected in γ-rays to date, indicating a range of at least a factor of 10 in the γ-ray luminosities for these explosions.