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arXiv 1409.7526astro-ph.GA
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NGC 3310 - II星盘中的电离恒星星族。沃尔夫-拉叶人口

Ionizing stellar population in the disc of NGC 3310 - II. The Wolf-Rayet population

D. Miralles-Caballero, F. F. Rosales-Ortega, A. I. Díaz, H. Otí-Floranes, E. Pérez-Montero, S. F. Sánchez

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Accepted for publication in MNRAS; 23 pages, 11 figures, 4 tables
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摘要：

我们使用积分场光谱详细研究了NGC 3310中的Wolf-Rayet（WR）人口，在空间上分辨出18个典型大小为200-300 pc的星系盘中的恒星形成结，这些星系盘中有大量的WR人口。在所谓的蓝色隆起中检测到的发射主要归因于晚型氮WR（WNL），每个区域的恒星数量从几十到几百颗不等。我们估计的WNL/（WNL+O）的比率是可比的经验关系，一旦反射校正的发射进一步校正星云内的尘埃颗粒的存在下，吸收不可忽略的一部分紫外光子。观测值与恒星星族模型的比较显示出大于2-3倍的差异。然而，如果考虑到相互作用的双星和/或光子泄漏的影响，观测和预测往往会收敛。我们估计托管WR的\hii区域的二进制部分是显着的，以恢复所观察到的X射线通量，从而证明，二进制通道可以是关键时，预测可观的。我们还探讨了环境与目前的假设，即WR可以祖长期伽马射线暴（GRB）的连接。星系的相互作用，这可能会引发强烈的事件，在中心区域的恒星形成，可能是一个合理的环境，WR可能会作为伽玛暴的祖先。最后，即使化学丰度一般是均匀的，我们也发现了微弱的证据，快速N污染的WR恒星风的尺度约为200 pc。

英文摘要：

We use integral field spectroscopy to study in detail the Wolf-Rayet (WR) population in NGC 3310, spatially resolving 18 star-forming knots with typical sizes of 200-300 pc in the disc of the galaxy hosting a substantial population of WRs. The detected emission in the so-called blue bump is attributed mainly to late-type nitrogen WRs (WNL), ranging from a few dozens to several hundreds of stars per region. Our estimated WNL/(WNL+O) ratio is comparable to reported empirical relations once the extinction-corrected emission is further corrected by the presence of dust grains inside the nebula that absorb a non-negligible fraction of UV photons. Comparisons of observables with stellar population models show disagreement by factors larger than 2-3. However, if the effects of interacting binaries and/or photon leakage are taken into account, observations and predictions tend to converge. We estimate the binary fraction of the \hii regions hosting WRs to be significant in order to recover the observed X-ray flux, hence proving that the binary channel can be critical when predicting observables. We also explore the connection of the environment with the current hypothesis that WRs can be progenitors to long-duration gamma-ray bursts (GRBs). Galaxy interactions, which can trigger strong episodes of star formation in the central regions, may be a plausible environment where WRs may act as progenitors of GRBs. Finally, even though the chemical abundance is generally homogeneous, we also find weak evidence for rapid N pollution by WR stellar winds at scales of ~ 200 pc.

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