AKARI's infrared view on nearby stars : Using AKARI Infrared Camera All-Sky Survey, 2MASS, and Hipparcos catalog
AKARI's infrared view on nearby stars : Using AKARI Infrared Camera All-Sky Survey, 2MASS, and Hipparcos catalog
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DOI：
10.1051/0004-6361/200913695
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发表时间：
2010-03
期刊：
影响因子：
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通讯作者：
Y. Ita;M. Matsuura;D. Ishihara;S. Oyabu;S. Takita;H. Kataza;I. Yamamura;N. Matsunaga;T. Tanabé;Y. Nakada;H. Fujiwara;T. Wada;T. Onaka;H. Matsuhara;Naoj;Isasjaxa;Ucl;D. Physics;Astronomy;Mullard Space Science Laboratory;Nagoya University;Ioa;T. U. O. Tokyo;D. O. Astronomy
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文献类型：
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作者：
Y. Ita;M. Matsuura;D. Ishihara;S. Oyabu;S. Takita;H. Kataza;I. Yamamura;N. Matsunaga;T. Tanabé;Y. Nakada;H. Fujiwara;T. Wada;T. Onaka;H. Matsuhara;Naoj;Isasjaxa;Ucl;D. Physics;Astronomy;Mullard Space Science Laboratory;Nagoya University;Ioa;T. U. O. Tokyo;D. O. Astronomy
结果：我们发现（B-V） vs .s. （V-S9W）彩色图对识别星周包膜/盘中出现的红外过量恒星是有用的。在这张图中，红外过剩的恒星与其他类型的恒星是分开的。而（J-L18W） vs .s （S9W-L18W）图是对几种对象类型进行分类的强大工具。富碳渐近巨支（AGB）恒星和OH/IR恒星在这张彩色图中形成了不同的序列。年轻恒星天体（yso）、主序前恒星（PMS）、agb后恒星和行星状星云（PNe）的中红外颜色过剩最大，可以在红外表中识别出来。最后，我们利用AKARI数据和Hipparcos视差绘制了L18W vs .s （S9W-L18W）的彩色星等图。这张图可以用来识别低质量的yso和AGB恒星。我们发现这张图与使用斯皮策太空望远镜数据的大麦哲伦云源的[24]vs（[8.0]-[24]）图相当。我们对银河系天体的了解将用于解释斯皮策太空望远镜观测到的邻近星系恒星群的彩色星等图。结论：我们对AKARI颜色-颜色和颜色大小的研究将在未来用于探索未知物体的属性。此外，我们的分析强调了未来的一个关键项目，即一旦GAIA即将提供的天文数据可用，就可以通过星周包层了解恒星演化。
Results: We found that the (B-V) v.s. (V-S9W) color-color diagram is useful to identify the stars with infrared excess emerged from circumstellar envelopes/disks. Be stars with infrared excess are well separated from other types of stars in this diagram. Whereas (J-L18W) v.s. (S9W-L18W) diagram is a powerful tool to classify several object-types. Carbon-rich asymptotic giant branch (AGB) stars and OH/IR stars form distinct sequences in this color-color diagram. Young stellar objects (YSOs), pre-main sequence (PMS) stars, post-AGB stars and planetary nebulae (PNe) have largest mid-infrared color-excess, and can be identified in infrared catalog. Finally, we plot L18W v.s. (S9W-L18W) color-magnitude diagram, using the AKARI data together with Hipparcos parallaxes. This diagram can be used to identify low-mass YSOs, as well as AGB stars. We found that this diagram is comparable to the [24] vs ([8.0]-[24]) diagram of Large Magellanic Cloud sources using the Spitzer Space Telescope data. Our understanding of Galactic objects will be used to interpret color-magnitude diagram of stellar populations in nearby galaxies which Spitzer Space Telescope has observed. Conclusions: Our study of the AKARI color-color and color-magnitude will be used to explore properties of unknown objects in future. In addition, our analysis highlights a future key project to understand stellar evolution with circumstellar envelope, once the forthcoming astronometrical data with GAIA are available.