Mid-Infrared Identification of Faint Submillimeter Sources
Mid-Infrared Identification of Faint Submillimeter Sources
复制标题
微弱亚毫米源的中红外识别
DOI：
10.1086/344561
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发表时间：
2002
期刊：
影响因子：
--
通讯作者：
H. Okuda
中科院分区：
文献类型：
--
作者：
Y. Sato;L. Cowie;K. Kawara;Y. Taniguchi;Y. Sofue;H. Matsuhara;H. Okuda
詹姆斯·克拉克麦克斯韦望远镜上的亚毫米波普通用户测辐射热计阵列探测到的微弱亚毫米波源由于望远镜的宽光束轮廓而面临识别问题。在这里，我们提出了一种新的方法来识别这样的亚毫米波源与中红外图像具有更精细的点扩散函数。红外空间天文台提供了夏威夷深场SSA 13的一幅非常深的6.7 μm图像。这三个微弱的850 μm源都有6.7 μm的对应源。它们在光学图像中被确认为相互作用的星系对。这些对也在无线电中检测到。其中两颗在光学上是暗淡的，非常红（I > 24，I-K > 4），其中一颗被钱德拉卫星探测到了硬X射线。由于这些观测性质与本地超亮红外星系相似，它们的光度红移是基于亚毫米到中红外的流量比推导出来的，假设光谱能量分布（SED）为阿普220。其他的光度学红移是通过可用的光度学数据和模板SED之间的χ2最小化获得的。这两个估计都在z = 1-2的范围内，与光谱红移和毫米红移非常一致。重建的阿普220 SED与这些红移的估计是一致的所有测光数据，除了钱德拉的硬X射线探测。光源的亮度将比阿普220高出几倍。假设活动星系核的贡献可以忽略不计，那么在高红移的星系中，已经存在大量恒星物质的星系中，星星的形成率似乎非常高。
Faint submillimeter sources detected with the Submillimeter Common-User Bolometer Array on the James Clerk Maxwell Telescope have faced an identification problem due to the telescope's broad beam profile. Here we propose a new method to identify such submillimeter sources with a mid-infrared image having a finer point-spread function. The Infrared Space Observatory has provided a very deep 6.7 μm image of the Hawaii Deep Field SSA13. All three faint 850 μm sources in this field have their 6.7 μm counterparts. They have been identified with interacting galaxy pairs in optical images. These pairs are also detected in the radio. Two of them are optically faint and very red (I > 24, I-K > 4), one of which has a hard X-ray detection with the Chandra satellite. As these observing properties are similar to those of local ultraluminous infrared galaxies, their photometric redshifts are derived based on submillimeter-to-mid-infrared flux ratios assuming a spectral energy distribution (SED) of Arp 220. Other photometric redshifts are obtained via χ2-minimization between the available photometry data and template SEDs. Both estimates are in the range z = 1-2, in good agreement with a spectroscopic redshift and a millimetric one. The reconstructed Arp 220 SEDs with these redshift estimates are consistent with all the photometry data except Chandra's hard X-ray detection. The sources would be a few times more luminous than Arp 220. With an assumption that contributions from active galactic nuclei are negligible, it appears that extremely high star formation rates are occurring in galaxies at high redshifts with massive stellar contents already in place.
加拿大本地债券 (2)
DOI：
--
发表时间：
2006
期刊：
Chihosai Geppo 329
影响因子：
--
作者：
IKEGAMI;Takehiko
通讯作者：
Takehiko