来自Mrk1066中心区域的近红外尘埃和谱线发射：来自Gemini NIFS的约束
Near-IR dust and line emission from the central region of Mrk1066: Constraints from Gemini NIFS
摘要：
我们目前的积分场光谱的内部350 pc的Mrk 1066与双子座NIFS获得的空间分辨率为35 pc。这种高空间分辨率使我们能够在这个星系中第一次观察到质量为0.014 M太阳的未解决的尘埃浓度，这可能是尘埃环的一部分。在PA=135/315度范围内，发射线通量被拉长，与[OIII]和射电图像一致，除H线外，西北方向比东南方向更亮。H辐射在东南方向更强，在那里我们发现了一个大的恒星形成区域。射电发射和最高发射线通量之间的强相关性表明，射电喷流在这些强度水平上起着根本性的作用。H2通量更均匀地分布，并且具有2100 K的激发温度。它的起源似乎是由来自活动星系核的X射线加热的环核气体。[Fe II]发射也与X射线加热一致，但由于无线电喷流中的冲击激发而产生额外的发射。[CaVIII]和[SIX]的冠状线发射未被我们的观测所分辨，表明其分布在离核18 pc以内。红化范围从E（B-V）~ 0到E（B-V）~ 1.7，最高值定义了沿PA ~ 135/315度的S形结构。在电离锥内的发射线比是类似于塞弗特的，表明线发射是由这些位置的中心活性核提供动力的。低电离区域远离电离锥被观察到，并且可以由通过电离锥壁过滤的扩散辐射场供电。两个区域在0.5角秒东南和1角秒西北的核心显示恒星爆发般的线比，归因于额外的排放从恒星形成的地区。
英文摘要：
We present integral field spectroscopy of the inner 350 pc of the Mrk1066 obtained with Gemini NIFS at a spatial resolution of 35 pc. This high spatial resolution allowed us to observe, for the first time in this galaxy, an unresolved dust concentration with mass 0.014 M_Sun, which may be part of the dusty torus. The emission-line fluxes are elongated in PA=135/315deg in agreement with the [OIII] and radio images and, except for the H lines, are brighter to the north-west than to the south-east. The H emission is stronger to the south-east, where we find a large region of star-formation. The strong correlation between the radio emission and the highest emission-line fluxes indicates that the radio jet plays a fundamental role at these intensity levels. The H2 flux is more uniformly distributed and has an excitation temperature of 2100 K. Its origin appears to be circumnuclear gas heated by X-rays from the AGN. The [FeII] emission also is consistent with X-ray heating, but with additional emission due to excitation by shocks in the radio jet. The coronal-line emission of [CaVIII] and [SIX] are unresolved by our observations indicating a distribution within 18pc from the nucleus. The reddening ranges from E(B-V) ~ 0 to E(B-V) ~ 1.7 with the highest values defining a S-shaped structure along PA ~ 135/315deg. The emission-line ratios are Seyfert-like within the ionization cone indicating that the line emission is powered by the central active nucleus in these locations. Low ionization regions are observed away from the ionization cone, and may be powered by the diffuse radiation field which filters through the ionization cone walls. Two regions at 0.5 arcsec south-east and at 1 arcsec north-west of the nucleus show starburst-like line ratios, attributed to additional emission from star forming regions.
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