Abstract

We study the mid-infrared photometric properties of a sample of compact star-forming galaxies from the SDSS Data Release 14. The sample includes about 30 000 galaxies. The H_β emission lines with equivalent widths EW(H_β) > 1 nm are observed in the spectra of all selected galaxies. The selected galaxies are compact objects with angular diameters less than 6 arcsec. About 10 000 galaxies were detected by the WISE space telescope at wavelengths of 3.4 and 4.6 μm. A considerable number of galaxies was also detected at wavelengths of 12 and 22 μm. Using these data and the results of observations obtained in the ultraviolet range with the GALEX space telescope, it was shown that the heating of dust in the sample of galaxies is caused by the ultraviolet radiation of massive stars in the star-forming regions. The stellar and ionized-gas emission dominates at wavelengths of 3.4 and 4.6 μm in a majority of galaxies, whereas the dust emission dominates at wavelengths of 12 and 22 μm. In some galaxies with high H_β luminosity, dust emission is observed even at the short wavelength of 3.4 μm, and it has a steep increase in the intensity toward the wavelength of 4.6 μm. This emission is characterized by “red” color (W1 – W2 > 2^m), where W1 and W2 are magnitudes at wavelengths of 3.4 and 4.6 μm, respectively. The probable cause of this emission is the presence of hot dust with a temperature of hundreds of Kelvins. A list of 39 galaxies with such an extremely high W1 – W2 color index is presented.

中文翻译：

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从WISE太空望远镜获得的数据来看，中红外范围内的恒星形成星系的性质

摘要

我们研究了来自SDSS数据发布14的紧凑型恒星形成星系样本的中红外光度学特性。该样本包含约3万个星系。为H _β发射谱线具有同等宽度EW（H _β在所有选定星系的光谱中观察到> 1 nm。所选星系是角直径小于6 arcsec的紧凑物体。WISE太空望远镜在3.4和4.6μm的波长处检测到约10,000个星系。在12和22μm的波长处也检测到相当数量的星系。利用这些数据和用GALEX太空望远镜在紫外线范围内获得的观测结果，表明星系样品中尘埃的加热是由恒星形成区域中大质量恒星的紫外线辐射引起的。在大多数星系中，恒星和离子化气体的辐射占主导地位，波长分别为3.4和4.6μm，而粉尘的辐射占主导地位，波长分别为12和22μm。在一些星系与高^ h _β发光度，甚至在短波长为3.4μm时也观察到粉尘发射，并且在4.6μm波长处强度急剧增加。这种发射的特征是“红色”（W 1 – W 2> 2 ^m），其中W 1和W 2分别是波长为3.4和4.6μm时的幅度。这种排放的可能原因是存在温度为数百开氏温度的热尘。列出了39个具有如此高的W 1 – W 2颜色指数的星系。