Detailed study of B037 based on HST images
Detailed study of B037 based on HST images
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基于HST图像的B037详细研究
DOI：
10.1088/1674-4527/11/5/003
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发表时间：
2011-03
影响因子：
1.8
通讯作者：
Ma, Jun
中科院分区：
文献类型：
--
作者：
Ma, Jun
B 037是M31中最亮和最红的星团，因此它很有意义。利用哈勃太空望远镜（HST）上的高级巡天相机进行的深度观测和高空间分辨率图像首次显示，这个星团被一条尘埃带穿过。F606 W和F814 W滤光片的测光数据表明，尘埃带中（F606 W-F814 W）的颜色比B 037其它区域的颜色偏红约0.4等。哈勃望远镜的图像显示，这条尘埃带似乎包含在B 037中，而不是在M31盘或银河系中。据我们所知，尘埃的形成需要金属丰度相当高的气体。然而，B 037的金属丰度较低，[Fe/H] = −1.07 ± 0.20。因此，观察到的尘埃带似乎不太可能与B 037有物理联系。很明显，这条沙尘带的起源值得进一步研究。此外，基于这些图像，我们给出了B 037的椭圆率和位置角以及表面亮度分布的精确变化，并通过拟合单质量各向同性King模型确定了B 037的结构参数。在F606 W滤波器中，我们得到最佳拟合尺度半径r 0 = 0.56 ± 0.02“（= 2.16 ± 0.08 pc），潮汐半径rt = 8.6 ± 0.4”（= 33.1 ± 1.5 pc），浓度指数c = log（rt/r 0）= 1.19±0.02。在F814 W滤波器中，我们推导出r 0 = 0.56 ± 0.01“（= 2.16 ± 0.04 pc），rt = 8.9 ± 0.3”（= 34.3 ± 1.2 pc），c = log（rt/r 0）= 1.20 ± 0.01。在F606 W滤光片中，经折射校正的中心表面亮度为μ0 = 13.53 ± 0.03 mag arcsec−2，在F814 W滤光片中为12.85 ± 0.03 mag arcsec−2。我们还计算了在F606 W滤光片中rh = 1.05 ± 0.03“（= 4.04 ± 0.12 pc）和在F814 W滤光片中rh = 1.07 ± 0.01”（= 4.12 ± 0.04 pc）处的半光半径。此外，通过将ACS星等转换为标准星等，得到了B 037在V波段和I波段的完整星等，与以往的地基宽带测光结果吻合较好。
B037 is of interest because it is both the most luminous and the most highly reddened cluster known in M31. Deep observations and high spatial resolution images with the Advanced Camera for Surveys on the Hubble Space Telescope (HST) first showed that this cluster is crossed by a dust lane. Photometric data in the F606W and F814W filters obtained in this paper indicate that colors of (F606W — F814W) in the dust lane are redder ~ 0.4 mag than ones in the other regions of B037. The HST images show that this dust lane seems to be contained in B037, instead of in the M31 disk or the Milky Way. As far as we know, the formation of dust requires gas with a rather high metallicity. However, B037 has a low metallicity of [Fe/H] = −1.07 ± 0.20. So, it seems improbable that the observed dust lane is physically associated with B037. It is clear that the origin of this dust lane is worthy of future study. In addition, based on these images, we present the precise variation of ellipticity and position angle, and of surface brightness profile, and determine the structural parameters of B037 by fitting a single-mass isotropic King model. In the F606W filter, we derive the best-fitting scale radius r0 = 0.56 ± 0.02'' (= 2.16 ± 0.08 pc), a tidal radius rt = 8.6 ± 0.4'' (= 33.1 ± 1.5 pc), and a concentration index c = log(rt/r0) = 1.19±0.02. In the F814W filter, we derive r0 = 0.56 ± 0.01'' (= 2.16 ± 0.04 pc), rt = 8.9 ± 0.3'' (= 34.3 ± 1.2 pc), and c = log(rt/r0) = 1.20 ± 0.01. The extinction-corrected central surface brightness is μ0 = 13.53 ± 0.03 mag arcsec−2 in the F606W filter, and 12.85 ± 0.03 mag arcsec−2 in the F814W filter. We also calculate the half-light radius at rh = 1.05 ± 0.03'' (= 4.04 ± 0.12 pc) in the F606W filter and rh = 1.07 ± 0.01'' (= 4.12 ± 0.04 pc) in the F814W filter. In addition, we derived the complete magnitudes of B037 in the V and I bands by transforming the magnitudes from the ACS system to the standard system, which are in good agreement with previous ground-based broadband photometry studies.
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DOI：
10.1086/500257
发表时间：
2005-12
期刊：
The Astrophysical Journal Letters
影响因子：
--
作者：
Jun Ma;S. van den Bergh;Hong Wu;Yanbin Yang;Xu Zhou;Jian-sheng Chen;Zhenyu Wu;Zhao-ji Jiang;Jianghua Wu
通讯作者：
Jun Ma;S. van den Bergh;Hong Wu;Yanbin Yang;Xu Zhou;Jian-sheng Chen;Zhenyu Wu;Zhao-ji Jiang;Jianghua Wu
DOI：
10.1086/339667
发表时间：
2002-01
期刊：
The Astronomical Journal
影响因子：
--
作者：
P. Barmby;Stephen Holland;J. Huchra
通讯作者：
P. Barmby;Stephen Holland;J. Huchra
影响因子：
6.5
作者：
S. Galleti;S. Galleti;L. Federici;M. Bellazzini;F. F. Pecci-F.;S. Macrina
通讯作者：
S. Galleti;S. Galleti;L. Federici;M. Bellazzini;F. F. Pecci-F.;S. Macrina
DOI：
--
发表时间：
2000-12
期刊：
--
影响因子：
--
作者：
H. Ford
通讯作者：
H. Ford
DOI：
10.1086/162815
发表时间：
1985
期刊：
The Astrophysical Journal
影响因子：
--
作者：
D. Crampton;A. Cowley;D. Schade;P. Chayer
通讯作者：
D. Crampton;A. Cowley;D. Schade;P. Chayer