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arXiv 0908.2535astro-ph.CO
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蓝色致密矮星系Markarian 59的近红外光谱

Near-infrared spectroscopy of the Blue Compact Dwarf galaxy Markarian 59

Y. I. Izotov, T. X. Thuan, J. C. Wilson

备注：
23 pages, 3 figures, accepted for publication in the Astrophysical Journal
发表信息：
ApJ, 2009, 703, 1984
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摘要：

我们提出了近红外（NIR）光谱观测的蓝色紧凑矮（BCD）星系Mrk 59，获得了与TripleSpec光谱仪安装在3.5米APO望远镜。Mrk 59的近红外光谱覆盖了0.90 - 2.40微米的波长范围，显示出原子氢、分子氢、氦、硫和铁的发射线。SDSS光谱补充了近红外数据。我们发现BCD中的消光很低[A（V）=0.24 mag]，并且在光学和NIR范围内是相同的。近红外光并不能揭示隐藏的恒星形成。H2发射来自致密的团块，并且H2振动发射线强度可以由光子激发来解释。不需要冲击激励。Mrk 59的云光化模式很好地再现了观测到的光学和近红外发射线通量。[Fe II] 1.257和1.643微米的发射谱线通常被用作低激发高金属量星暴星系中的超新星激波指示器，但在高激发低金属量的HII区（如Mrk 59）中不能起到这样的作用。

英文摘要：

We present near-infrared (NIR) spectroscopic observations of the blue compact dwarf (BCD) galaxy Mrk 59, obtained with the TripleSpec spectrograph mounted on the 3.5m APO telescope. The NIR spectrum of Mrk 59, which covers the 0.90 - 2.40 micron wavelength range, shows atomic hydrogen, molecular hydrogen, helium, sulfur and iron emission lines. The NIR data have been supplemented by a SDSS optical spectrum. We found extinction in the BCD to be low [A(V)=0.24 mag] and to be the same in both the optical and NIR ranges. The NIR light does not reveal hidden star formation. The H2 emission comes from dense clumps and the H2 vibrational emission line intensities can be accounted for by photon excitation. No shock excitation is needed. A CLOUDY photoinization model of Mrk 59 reproduces well the observed optical and NIR emission line fluxes. There is no need to invoke sources of ionization other than stellar radiation.The [FeII] 1.257 and 1.643 micron emission lines, often used as supernova shock indicators in low-excitation high-metallicity starburst galaxies, cannot play such a role in high-excitation low-metallicity HII regions such as Mrk 59.

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