Seyfert星系NGC 1068中多环芳烃和暖尘排放的示踪
Tracing PAHs and Warm Dust Emission in the Seyfert Galaxy NGC 1068
摘要：
我们利用斯皮策太空望远镜上的IRAC、IRS和MIPS仪器获得的中红外和远红外数据对附近的塞弗特星系NGC 1068进行了研究。这些图像显示了广泛的8 μ m和24 μ m的辐射，与距离核心约15”（1 kpc）的内螺旋中的恒星形成相一致，以及距离核心西南47”（3 kpc）的明亮的恒星形成复合体。最亮的8 μ m PAH发射区域与在Halpha图像中观察到的结非常吻合。强PAH功能在6.2，7.7，8.6，和11.3微米检测IRS光谱测量在许多位置内，内，外的内螺旋。这些地区的IRAC颜色和IRS光谱排除了由活动星系核加热的尘埃作为主要发射源; SED主要由星光和PAH发射。PAH功能的内螺旋的等效宽度和流量比一般是一致的条件下，在一个典型的螺旋星系ISM。内部的内螺旋，活动星系核的影响，ISM是显而易见的，通过PAH通量比表示一个较高的电离参数和一个显着较小的平均等效宽度比观察到的内螺旋。最明亮的8和24微米的发射峰在星系盘，即使在距离以外的内螺旋，位于电离锥跟踪的[O III]/H β，他们也是非常好的无线电喷流的轴对齐。虽然活动星系核的辐射有可能直接增强PAH的激发，或者触发OB星的形成，OB星随后在内螺旋的这些位置激发PAH的发射，但活动星系核的准直辐射和内螺旋中的恒星形成结的方向可能是一致的。（节略）
英文摘要：
We present a study of the nearby Seyfert galaxy NGC 1068 using mid- and far- infrared data acquired with the IRAC, IRS, and MIPS instruments aboard the Spitzer Space Telescope. The images show extensive 8 um and 24 um emission coinciding with star formation in the inner spiral approximately 15" (1 kpc) from the nucleus, and a bright complex of star formation 47" (3 kpc) SW of the nucleus. The brightest 8 um PAH emission regions coincide remarkably well with knots observed in an Halpha image. Strong PAH features at 6.2, 7.7, 8.6, and 11.3 um are detected in IRS spectra measured at numerous locations inside, within, and outside the inner spiral. The IRAC colors and IRS spectra of these regions rule out dust heated by the AGN as the primary emission source; the SEDs are dominated by starlight and PAH emission. The equivalent widths and flux ratios of the PAH features in the inner spiral are generally consistent with conditions in a typical spiral galaxy ISM. Interior to the inner spiral, the influence of the AGN on the ISM is evident via PAH flux ratios indicative of a higher ionization parameter and a significantly smaller mean equivalent width than observed in the inner spiral. The brightest 8 and 24 um emission peaks in the disk of the galaxy, even at distances beyond the inner spiral, are located within the ionization cones traced by [O III]/Hbeta, and they are also remarkably well aligned with the axis of the radio jets. Although it is possible that radiation from the AGN may directly enhance PAH excitation or trigger the formation of OB stars that subsequently excite PAH emission at these locations in the inner spiral, the orientation of collimated radiation from the AGN and star formation knots in the inner spiral could be coincidental. (abridged)
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