Unlocking the secrets of stellar haloes using combined star counts and surface photometry

Unlocking the secrets of stellar haloes using combined star counts and surface photometry
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利用恒星计数和表面光度测量相结合解开恒星晕的秘密

DOI:
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发表时间:
2011
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影响因子:
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通讯作者:
G. Micheva
G. Micheva
中科院分区:
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文献类型:
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作者:
E. Zackrisson;R. D. Jong;G. Micheva

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星系的恒星晕目前可以通过观测分辨的晕星或通过表面光度学来研究。奇怪的是,这两种方法似乎给出了相互矛盾的结果,因为一些表面测光测量显示,综合颜色太红,无法与从解析恒星研究中推断出的晕属性相协调。对于这种异常现象有几种解释,包括尘埃的光致发光、河外背景光的消光和底部重的恒星初始质量函数。然而,仍然缺乏决定性的考验。在这里,我们解释如何观察附近星系的晕,涉及到表面光度和明亮的星星计数的组合,可以用来区分所提出的解释。我们得出的观测要求,这项工作,并发现,星星计数过滤器VI和表面测光过滤器VIJ似乎是最佳的策略。由于所需的晕星星计数已经可以用于许多附近的星系,这项测试中最具挑战性的部分可能是光学表面测光,这需要在4-8米望远镜上曝光几个晚上,以及近红外表面测光,这是最容易使用即将到来的詹姆斯韦伯太空望远镜进行的。
The stellar haloes of galaxies can currently be studied either through observations of resolved halo stars or through surface photometry. Curiously, the two methods appear to give conflicting results, as a number of surface photometry measurements have revealed integrated colours that are too red to be reconciled with the halo properties inferred from the study of resolved stars. Several explanations for this anomaly have been proposed – including dust photoluminescence, extinction of extragalactic background light and a bottom-heavy stellar initial mass function. A decisive test is, however, still lacking. Here, we explain how observations of the halo of a nearby galaxy, involving a combination of both surface photometry and bright star counts, can be used to distinguish between the proposed explanations. We derive the observational requirements for this endeavour and find that star counts in filters VI and surface photometry in filters VIJ appear to be the optimal strategy. Since the required halo star counts are already available for many nearby galaxies, the most challenging part of this test is likely to be the optical surface photometry, which requires several nights of exposure time on a 4–8 m telescope, and the near-infrared surface photometry, which is most readily carried out using the upcoming James Webb Space Telescope.
DOI: 10.1088/0067-0049/192/2/18
发表时间: 2011-02-01
影响因子: 8.7
作者:
Komatsu, E.;Smith, K. M.;Wright, E. L.
通讯作者: Wright, E. L.
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DOI: 10.1088/0067-0049/195/2/18
发表时间: 2011
期刊: The Astrophysical Journal Supplement Series
影响因子: --
作者:
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通讯作者: Vlajić