A Distinct Structure inside the Galactic Bar
A Distinct Structure inside the Galactic Bar
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DOI：
10.1086/429291
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发表时间：
2005-02
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通讯作者：
S. Nishiyama;T. Nagata;D. Baba;Y. Haba;R. Kadowaki;D. Kato;M. Kurita;C. Nagashima;T. Nagayama;Yuka Murai;Y. Nakajima;M. Tamura;H. Nakaya;K. Sugitani;T. Naoi;N. Matsunaga;T. Tanabé;N. Kusakabe;S. Sato
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作者：
S. Nishiyama;T. Nagata;D. Baba;Y. Haba;R. Kadowaki;D. Kato;M. Kurita;C. Nagashima;T. Nagayama;Yuka Murai;Y. Nakajima;M. Tamura;H. Nakaya;K. Sugitani;T. Naoi;N. Matsunaga;T. Tanabé;N. Kusakabe;S. Sato
本文介绍了用IRSF 1.4 m望远镜和SIRIUS相机沿银道面沿着进行的近红外巡天观测结果，观测条件为-10. ° 5 ≤ l ≤ 10.°5，B = +1°。Ks与H-Ks色星等图显示了一个定义明确的红团星群体，其视星等峰值沿银道面连续沿着变化，从l = -10°时的Ks = 13.4到去红后l = 10°时的Ks = 12.2。这种变化可以用以前研究中发现的棒状结构来解释，但我们发现了一个额外的内部结构，在101 °至104 °之间，视星等-视星等关系与外部棒状结构不同，视星等峰值在中心8°上仅变化10.1等。这种内部结构的确切性质还不确定。
We present the result of a near-infrared (JHKs) survey along the Galactic plane, -10.°5 ≤ l ≤ 10.°5 and b = +1°, with the IRSF 1.4 m telescope and the SIRIUS camera. Ks versus H - Ks color-magnitude diagrams reveal a well-defined population of red clump stars whose apparent magnitude peak changes continuously along the Galactic plane, from Ks = 13.4 at l = -10° to Ks = 12.2 at l = 10° after dereddening. This variation can be explained by the barlike structure found in previous studies, but we find an additional inner structure at ∣ l ∣ ≲ 4°, where the longitude-apparent magnitude relation is distinct from the outer bar and where the apparent magnitude peak changes by only ≈0.1 mag over the central 8°. The exact nature of this inner structure is as yet uncertain.