We present new 37.7 μm far-infrared imaging of the infrared luminous (LIR ~ 5.16 × 1011 L☉) interacting galaxy Arp 299 (= IC 694 + NGC 3690). We show that the 38 μm flux, like the 60 and 100 μm emission, traces the luminosity of star forming galaxies but at considerably higher spatial resolution. Our data establish that the major star formation activity of the galaxy originates from a point source in its eastern component, IC 694, which is inconspicuous in the optical, becoming visible only at the near- and mid-infrared. We find that IC 694 is 2 times more luminous than NGC 3690, contributing to more than 46% of the total energy output of the system at this wavelength. The spectral energy distribution of the different components of the system clearly shows that IC 694 has 6 times the infrared luminosity of M82, and it is the primary source responsible for the bolometric luminosity of Arp 299.
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机译：我们提出了相互作用的星系Arp 299（= IC 694 + NGC 3690）的红外发光（LIR〜5.16×1011L☉）的新37.7μm远红外成像。我们显示出38μm的光通量，像60和100μm的发射光一样，可以追踪形成恒星的星系的光度，但其空间分辨率要高得多。我们的数据表明，星系的主要恒星形成活动源自其东部分量IC 694中的一个点源，该点在光学上不明显，仅在近红外和中红外可见。我们发现，IC 694的发光度是NGC 3690的2倍，在该波长下贡献了系统总能量输出的46％以上。该系统不同组件的光谱能量分布清楚地表明，IC 694的红外发光度是M82的6倍，它是负责Arp 299辐射热测定的主要来源。
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