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Near-infrared [iron II] emission in starburst galaxies.

机译：星暴星系中的近红外[铁II]发射。

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摘要

We used the near-infrared [Fe II] emission line signature to detect supernova remnants (SNRs) in the nearby starburst galaxies NGC 1569, NGC 3738 and NGC 5253. The near-infrared narrow-band imaging program has led to the detection of 10 SNR candidates in NGC 1569, 7 in NGC 5253, and none in NGC 3738. A spatially extended component to the [Fe II] line emission is observed in NGC 1569 and NGC 5253. This component dominates the integrated [Fe II] luminosity in both galaxies, the compact sources accounting for 14% and 7% of the total [Fe II] luminosity of NGC 1569 and NGC 5253, respectively.; Despite the starburst environment, the [Fe II] luminosity of the individual SNRs is two orders of magnitude lower than the luminosities observed for SNRs in M82. We find that the density and the structure of the interstellar medium is a more important factor than the starburst nature of a galaxy in determining the average [Fe II] luminosity of a SNR. We caution against the blind usage of supernova rate vs. [Fe II] luminosity relations, which are most often calibrated with the average luminosity of the remnants in M82.; We suggest that a significant fraction of the ISM in NGC 1569 and NGC 5253 is under the influence of SNRs. This does not appear to be the case in M82, where the impact of the SNRs is limited to high density knots. Also, we find evidence for an [Fe II]-emitting lifetime as long as 105 yrs, which contrasts with the 104 yrs derived from SNRs in M82-like galaxies.; We find that the [Fe II] morphology, and the integrated luminosity observed in our sample galaxies, can be reproduced from a [Fe II]-emitting SNR population, as long as the pre-shock density is kept as low as 1 cm −3. Higher pre-shock density models are strongly rejected. We find a supernova rate of 0.006 SN/yr for NGC 1569 and 0.005 SN/yr for NGC 5253.
机译：我们使用近红外[Fe II]发射线签名来检测附近的星爆星系NGC 1569，NGC 3738和NGC 5253中的超新星残余（SNR）。近红外窄带成像程序已导致检测到10 NGC 1569中的SNR候选值，NGC 5253中的SNR候选值，NGC 3738中的SNR候选值都不存在。在NGC 1569和NGC 5253中观察到[Fe II]线发射的空间扩展分量。该分量支配了两者中集成的[Fe II]发光度星系中，致密源分别占NGC 1569和NGC 5253总[Fe II]光度的14％和7％。尽管有星爆环境，单个SNR的[Fe II]发光度比在M82中观察到的SNR的发光度低两个数量级。我们发现，在确定SNR的平均[Fe II]光度时，星际介质的密度和结构比星系的星暴特性更重要。我们告诫不要盲目使用超新星速率与[Fe II]的光度关系，该关系最经常用M82中残余物的平均光度进行校准。我们建议，NGC 1569和NGC 5253中的ISM很大一部分受SNR的影响。在M82中似乎并非如此，其中SNR的影响仅限于高密度结。此外，我们发现[Fe II]发射寿命长达10 5 年的证据，这与10 4 yrs 。我们发现，[Fe II]形态和在我们的样本星系中观察到的综合光度，可以从发射[Fe II]的SNR种群中复制，只要将震前密度保持在低至1 <斜体即可> cm -3 。较高的震前密度模型被强烈拒绝。我们发现NGC 1569的超新星率是0.006 SN / ，而NGC 5253的超新星率是0.005 SN / yr 。

著录项

  • 作者

    Labrie, Kathleen.;

  • 作者单位

    University of Victoria (Canada).;

  • 授予单位 University of Victoria (Canada).;
  • 学科 Physics Astronomy and Astrophysics.
  • 学位 Ph.D.
  • 年度 2003
  • 页码 219 p.
  • 总页数 219
  • 原文格式 PDF
  • 正文语种 eng
  • 中图分类 天文学;
  • 关键词

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