FIGGS：微弱不规则星系GMRT调查-概述、观测和初步结果
FIGGS: Faint Irregular Galaxies GMRT Survey - Overview, observations and first results
摘要：
微弱不规则星系GMRT巡天（FIGGS）是一个基于巨米波射电望远镜（GMRT）的HI成像巡天，系统地选择了附近极微弱的矮不规则星系样本。FIGGS的主要目标是提供一个全面的和统计上的强大的中性星际介质的微弱，富含气体的矮星系的属性的表征。FIGGS星系代表矮不规则星系群中质量极低的一端，中值M ${\rm{_B\sim-13.0}}$和中值HI质量为$\sim 3 \times 10^7$ M $_\odot$，扩展了质量和光度空间的基线，用于星系特性的比较研究。HI数据还得到了其他波长的观测数据的补充。此外，大多数样本星系的距离精确到10%。本文介绍了FIGGS，描述了GMRT观测，并给出了HI观测的第一批结果。从FIGGS数据，我们证实了随着光学光度降低，HI与光学直径比增加的趋势; FIGGS样品的D $_{\rm HI}$ /D $_{\rm Ho}$的中值比为2.4。此外，在比较我们的数据与孔径合成调查的明亮的螺旋，我们发现在最好的边缘证据，减少HI质量的平均表面密度的下降。一个很好的近似的气体丰富的星系盘，范围超过3个数量级的HI质量，可以被描述为从一个家庭与恒定HI面密度。
英文摘要：
The Faint Irregular Galaxies GMRT Survey (FIGGS) is a Giant Metrewave Radio Telescope (GMRT) based HI imaging survey of a systematically selected sample of extremely faint nearby dwarf irregular galaxies. The primary goal of FIGGS is to provide a comprehensive and statistically robust characterization of the neutral inter-stellar medium properties of faint, gas rich dwarf galaxies. The FIGGS galaxies represent the extremely low-mass end of the dwarf irregular galaxies population, with a median M${\rm{_B\sim-13.0}}$ and median HI mass of $\sim 3 \times 10^7$ M$_\odot$, extending the baseline in mass and luminosity space for a comparative study of galaxy properties. The HI data is supplemented with observations at other wavelengths. In addition, distances accurate to ~ 10% are available for most of the sample galaxies. This paper gives an introduction to FIGGS, describe the GMRT observations and presents the first results from the HI observations. From the FIGGS data we confirm the trend of increasing HI to optical diameter ratio with decreasing optical luminosity; the median ratio of D$_{\rm HI}$/D$_{\rm Ho}$ for the FIGGS sample is 2.4. Further, on comparing our data with aperture synthesis surveys of bright spirals, we find at best marginal evidence for a decrease in average surface density with decreasing HI mass. To a good approximation the disks of gas rich galaxies, ranging over 3 orders of magnitude in HI mass, can be described as being drawn from a family with constant HI surface density.
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