A DEEP CHANDRA ACIS SURVEY OF M83
A DEEP CHANDRA ACIS SURVEY OF M83
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DOI：
10.1088/0067-0049/212/2/21
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发表时间：
2014-04
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影响因子：
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通讯作者：
K. Long;K. Kuntz;W. Blair;L. Godfrey;L. Godfrey;P. Plucinsky;R. Soria;C. Stockdale;P. Winkler
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作者：
K. Long;K. Kuntz;W. Blair;L. Godfrey;L. Godfrey;P. Plucinsky;R. Soria;C. Stockdale;P. Winkler
我们利用钱德拉获得了附近星系 M83 的一系列深度 X 射线图像，总曝光量为 729 ks。将新数据与总计 61 ks 的早期档案观测相结合，我们在星系的 D25 轮廓内发现了 378 个点源。我们在 D25 等值线之外发现了另外 80 个源，其中大部分是背景活动星系核 (AGN)。使用澳大利亚望远镜紧凑阵列对 M83 进行的新射电勘测中发现了 47 个 X 射线源。根据 X 射线和其他波长的特性组合，在 X 射线源中，至少 87 个似乎可能是超新星遗迹 (SNR)。我们尝试通过光谱和时间分析的结合对 M83 的点源种群进行分类。作为这项工作的一部分，我们对 29 个最亮的 X 射线源进行了初步光谱分析。圆盘中的软 X 射线源（其中许多是 SNR）与旋臂相关，而较硬的 X 射线源（主要是 X 射线双星 (XRB)）似乎与旋臂无关。在消除 AGN、前景恒星并从样本中识别出 SNR 后，我们构建了亮于 8 × 1035 erg s−1 的 XRB 的累积光度函数 (CLF)。尽管 M83 的恒星形成率相对较高，但 CLF 表明盘中的大多数 XRB 都是低质量 XRB。
We have obtained a series of deep X-ray images of the nearby galaxy M83 using Chandra, with a total exposure of 729 ks. Combining the new data with earlier archival observations totaling 61 ks, we find 378 point sources within the D25 contour of the galaxy. We find 80 more sources, mostly background active galactic nuclei (AGNs), outside of the D25 contour. Of the X-ray sources, 47 have been detected in a new radio survey of M83 obtained using the Australia Telescope Compact Array. Of the X-ray sources, at least 87 seem likely to be supernova remnants (SNRs), based on a combination of their properties in X-rays and at other wavelengths. We attempt to classify the point source population of M83 through a combination of spectral and temporal analysis. As part of this effort, we carry out an initial spectral analysis of the 29 brightest X-ray sources. The soft X-ray sources in the disk, many of which are SNRs, are associated with the spiral arms, while the harder X-ray sources, mostly X-ray binaries (XRBs), do not appear to be. After eliminating AGNs, foreground stars, and identified SNRs from the sample, we construct the cumulative luminosity function (CLF) of XRBs brighter than 8 × 1035 erg s−1. Despite M83's relatively high star formation rate, the CLF indicates that most of the XRBs in the disk are low mass XRBs.