Abstract—We present the Hα images of ultra-flat (UF) spiral galaxies seen practically edgeon. The galaxies have the angular diameter in the B band \(a > 1.9' \) and the apparent axial ratio (a/b) > 10. We found that their Hα images look, on average, almost two times thinner than those in the red continuum. The star-formation rate in the studied objects, determined from the Hα flux, is in good agreement with that calculated from the FUV flux from the GALEX survey if we use the modified Verheijen and Sancisi formula taking into account the internal extinction in the UF galaxies. The logarithm of the specific star-formation rate in the UF galaxies shows a small scatter, 0.19, with a smooth decrease from –10.4 for dwarf spirals to –10.7 for massive ones. The relative amount of the hydrogen mass in UF disks varies from about 50% in dwarf disks to about 8% in massive ones. Structural distortions are less common in the UF galaxies (about 16%) than those in thick (less isolated) disks of edge-on spiral galaxies. On the cosmic time scale, 13.7 Gyr, large spiral disks are more efficient “engines” for gas processing into stars than dwarf spirals.

中文翻译：

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超平边缘螺旋星系的Ha图像

摘要—我们提出了实际上在埃顿上看到的超扁平（UF）旋涡星系的Hα图像。这些星系在B波段的角直径为（a> 1.9'\），视在轴向比率（a / b）> 10。我们发现，它们的Hα图像平均比其Hα图像的厚度薄几乎两倍。红色连续体。如果我们使用修正的Verheijen和Sancisi公式并考虑到UF星系的内部消光，则由Hα通量确定的被研究物体的恒星形成率与GALEX调查的FUV通量计算的恒星形成率非常吻合。。UF星系中特定恒星形成率的对数显示出较小的散射，0。19，并从–10平滑减少。4矮级螺旋到–10 。7对于大规模的。UF盘中氢质量的相对量从矮盘中的约50％到大块中的约8％不等。在超滤星系中，结构畸变的发生率不高（约16％），而在边缘螺旋星系的厚（较少分离）的圆盘中，结构畸变的发生率较低。在宇宙时间尺度13.7 Gyr上，大型螺旋盘比矮螺旋形更有效地将气体加工成恒星的“引擎”。