GHASP：螺旋星系的H $α$运动学巡天- XII。用R $_c$波段光度学研究螺旋星系和不规则邻近星系中的亮物质和暗物质分布
GHASP: an H$α$ kinematics survey of spiral galaxies - XII. Distribution of luminous and dark matter in spiral and irregular nearby galaxies using R$_c$-band photometry
摘要：
利用H-$α$旋转曲线和R-$_c$ -波段表面亮度剖面，计算了100个邻近旋涡星系和不规则星系的质量模型，涵盖了从Sa到Irr的形态类型。使用扫描法布里-珀罗干涉仪获得的运动学。其中一个目的是将我们的结果与Korsaga等人（2018）的结果进行比较，后者使用中红外（MIR）WISE W1（3.4 $μ$ m）光度数据。对于分析，两个条带使用相同的工具。伪等温（ISO）核心和Navarro-Frenk-White（NFW）尖瓣模型已被使用。我们使用B-V颜色测试最佳拟合模型（BFM）、最大圆盘模型（MDM）和M/L固定的模型。与在MIR 3.4 $μ$ m波段中发现的情况类似，当使用光学R $_c$波段时，大多数观察到的旋转曲线更好地由中心核密度分布（ISO）描述，而不是由尖形分布（NFW）描述。在两个波段中，对于固定M/L拟合，（M/L）值的离散度较小。对于W_1测光法，导出的DM晕参数与形态类型有关。我们发现类似的关系比文献中的那些，只有当我们比较我们的结果的膨胀穷人的子样本，因为大多数以前的结果主要是基于晚型螺旋。由于模型参数的色散较小，而且恒星质量在该波段中定义得更好，因此，在可能的情况下，应优先采用和平号红外测光，而不是光学波段。结果表明，对于高z星系，没有完全的剖面分解，仍然可以得到合理的结果。
英文摘要：
Mass models of 100 nearby spiral and irregular galaxies, covering morphological types from Sa to Irr, are computed using H$α$ rotation curves and R$_c$-band surface brightness profiles. The kinematics was obtained using a scanning Fabry-Perot interferometer. One of the aims is to compare our results with those from Korsaga et al. (2018), which used mid-infrared (MIR) WISE W1 (3.4 $μ$m) photometric data. For the analysis, the same tools were used for both bands. Pseudo-Isothermal (ISO) core and Navarro-Frenk-White (NFW) cuspy models have been used. We test Best Fit Models (BFM), Maximum Disc Models (MDM) and models for which M/L is fixed using the B - V colors. Similarly to what was found in the MIR 3.4 $μ$m band, most of the observed rotation curves are better described by a central core density profile (ISO) than a cuspy one (NFW) when using the optical R$_c$-band. In both bands, the dispersion in the (M/L) values is smaller for the fixed M/L fits. As for the W1 photometry, the derived DM halos' parameters depend on the morphological types. We find similar relations than those in the literature, only when we compare our results for the bulge-poor sub-sample because most of previous results were mainly based on late-type spirals. Because the dispersion in the model parameters is smaller and because stellar masses are better defined in that band, MIR photometry should be preferred, when possible, to the optical bands. It is shown that for high-z galaxies, sensible results can still be obtained without full profile decomposition.
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