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首页> 外文期刊>The Astrophysical journal >10-30 MICRON MAPS OF THE CENTRAL 5 PARSECS OF THE GALAXY: HEATING OF THE CAVITY AND NEUTRAL GAS DISK
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10-30 MICRON MAPS OF THE CENTRAL 5 PARSECS OF THE GALAXY: HEATING OF THE CAVITY AND NEUTRAL GAS DISK

机译：银河系中部5个裂口的10-30微米制图：腔体和中性气体盘的加热

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We present 10, 20, and 30 μm maps of the central 60″ x 90″ (R.A. x decl.) of the Galaxy made at approximately 4″ resolution with the NASA/Marshall Space Flight Center bolometer array. The maps span 2.5 x 3.8 pc centered near Sgr A IRS 1 and are the first to show the thermal emission from dust particles in both the ionized cavity and the neutral-gas ring with high sensitivity and an angular resolution as good as several arcseconds. In addition to warm dust associated with previously identified filaments in the central 40″, these maps show the detailed distribution of dust along the entire Western Arc of ionized gas at the inner edge of the neutral-gas ring. A prominent tongue of high 30 μm optical depth extends from the northern part of the ring into the cavity near IRS 1, nearly bisecting the cavity; since we detect warm dust in this 30 μm-emitting feature, which we call the Northern Intruder, it must be heated by radiation emitted in the cavity, thus confirming previous speculations based on far-infrared and O° observations that substantial neutral material protrudes into the cavity and may constitute infalling matter that fuels the central activity. We show that all the major ionized filaments (the Western Arc, the Bar, the Northern Arm, and the Eastern Arm) are ionization fronts at the interfaces between low- and high-density regions, as had been previously demonstrated convincingly only for the Western Arc. The locations of these ionization fronts are consistent with the dominant UV heating and ionizing sources being centrally located in the cavity. The derived dust temperatures strongly support this picture: they decrease away from the region of IRS 1 and Sgr A~*, and they drop abruptly where the gas density increases at the ring. We determine that the total ultraviolet luminosity emitted by the central cluster and required to heat the dust to the inferred temperatures is 1.7 ± 0.5 x 10~7 solar luminosity, which agrees with our derived infrared luminosity. Half of this ultraviolet luminosity is absorbed by dust in the cavity, and more than 40% of the ultraviolet radiation that propagates to the edge of the cavity is absorbed by dust in the neutral-gas ring.
机译：我们用美国国家航空航天局（NASA）/马歇尔太空飞行中心（Marshall Space Flight Center）辐射热测量仪阵列绘制了约60英寸x 90英寸（R.A. x偏角）的银河系中心的10、20和30μm图，分辨率约为4英寸。这些图跨度为2.5 x 3.8 pc，位于Sgr A IRS 1附近，并且是第一个以高灵敏度和高达几弧秒的角分辨率显示电离腔和中性气体环中灰尘颗粒的热辐射的图。这些图除了与先前确定的中央40''细丝相关的暖尘外，还显示了中性气体环内边缘沿电离气体整个Western Arc的详细分布。光学深度高的突出舌片从环的北部延伸到IRS 1附近的空腔中，几乎将空腔一分为二;由于我们在发出30μm辐射的特征中检测到暖尘，我们将其称为“北方入侵者”，因此必须通过腔体中发出的辐射对其进行加热，从而证实了基于远红外和O°观测的先前的推测，即大量中性物质会突入空腔，可能构成刺激中心活动的物质。我们显示，所有主要的离子化灯丝（西方弧线，巴尔，北臂和东臂）在低密度区域和高密度区域之间的界面处都是电离前沿，如先前仅针对西域的论证弧。这些电离前沿的位置与位于腔体中央的主要UV加热和电离源一致。得出的粉尘温度有力地支持了这一情况：它们远离IRS 1和Sgr A〜*的区域而降低，并且在环的气体密度增加的地方突然下降。我们确定，中央星团发出的，将粉尘加热到推定温度所需的总紫外线光度为1.7±0.5 x 10〜7太阳光度，这与我们得出的红外光度一致。这种紫外光度的一半被空腔中的灰尘吸收，而传播到空腔边缘的紫外线辐射的40％以上被中性气体环中的灰尘吸收。

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