Title: Near-IR dust and line emission from the central region of Mrk1066: Constraints from Gemini NIFS Show Chinese title

Title: 近红外尘埃和线发射来自Mrk1066中心区域：来自Gemini NIFS的约束

Abstract: 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. Show Chinese abstract

Abstract: 我们展示了使用Gemini NIFS获得的Mrk1066内部350 pc的积分场光谱，在空间分辨率为35 pc的情况下。这种高空间分辨率使我们首次在这个星系中观察到一个未解析的尘埃集中区域，其质量为0.014 M_Sun，可能是尘埃环的一部分。发射线流量在PA=135/315度方向上拉长，与[OIII]和射电图像一致，除了H线外，北西方向比南东方向更明亮。H发射在南东方向更强，我们在那里发现了一个大的恒星形成区域。射电辐射与最高发射线流量之间的强相关性表明，射电喷流在这些强度水平上起着基本作用。H2流量分布更均匀，激发温度为2100 K。其起源似乎是被AGN的X射线加热的核周围气体。[FeII]发射也与X射线加热一致，但还有由于射电喷流中的冲击波激发产生的额外发射。[CaVIII]和[SIX]的冕线发射在我们的观测中未解析，表明它们分布在距离核18 pc以内。消光范围从E(B-V) ~ 0到E(B-V) ~ 1.7，最高值沿着PA ~ 135/315度定义了一个S形结构。在电离锥内的发射线比率类似塞弗特，表明这些位置的线发射由中心活动核驱动。在电离锥之外观察到低电离区域，可能由通过电离锥壁过滤的弥漫辐射场驱动。在核南东方向0.5角秒和北西方向1角秒处的两个区域显示出类似星暴的线比率，这归因于恒星形成区域的额外发射。