论文标题
在Stephan的五重奏中搜索与Sitelle：II的五重奏组中形成区域。物理特性和金属性
Searching for intergalactic star forming regions in Stephan's Quintet with SITELLE: II. Physical properties and metallicity
论文作者
论文摘要
基于Sitelle光谱法，我们研究了Stephan五重奏（SQ）中175 H $α$发射区域的离子气体发射。对SQ区域的恒星形成速率（SFR），氧丰度（O/H）和氮与氧的丰度比（N/O）进行了详细分析，以探索这种复杂结构的出处和演变。根据BPT图，我们发现了SQ中的91个HII，17个复合材料和7个活跃的银河系样区域。几个区域与没有太阳金属性和低密度的前体的快速冲击模型兼容（n = 0.1 cm $^{ - 3} $），速度在175-300 km S $^{ - 1} $之间。我们在SQ中得出了总SFR（log（sfr/m $ _ \ odot \，yr^{ - 1} $ = 0.496）; starburst a和b提供总SFR的28％和9％的SFR，45％来自区域，来自径向速度低于6160 km s $ s $^{-1} $的辐射速度，以下是c^{-1} $。 （Ni）没有显示高的SFR，因此在考虑整个SQ和NI的集成SFR时，SQ显然是淬火的，我们发现两个区域都与SDSS恒星形成的SDS中获得的SFR一致。 S $^{ - 1} $具有与径向速度较低的O/H和N/O的值（V $ \ LEQ $ 6160 km S $^{ - 1} $）。 O/H的内部变化和沿Ni链的某些发射线比最终，Young Tidal Tail链。
Based on SITELLE spectroscopy, we studied the ionised gas emission for the 175 H$α$ emission regions in the Stephan's Quintet (SQ). A detailed analysis is performed of the star formation rate (SFR), oxygen abundance (O/H), and nitrogen-to-oxygen abundance ratio (N/O) of the SQ regions, to explore the provenance and evolution of this complex structure. According to the BPT diagram, we found 91 HII, 17 composite, and 7 active galactic nucleus-like regions in SQ. Several regions are compatible with fast shocks models without a precursor for solar metallicity and low density (n=0.1 cm$^{-3}$), with velocities between 175 - 300 km s$^{-1}$. We derived the total SFR in SQ (log(SFR/M$_\odot\,yr^{-1}$=0.496); starburst A and B provide 28% and 9% of the total SFR, and 45% comes from the regions with a radial velocity lower than 6160 km s$^{-1}$. For this reason, we assume that the material prior to the collision with the new intruder (NI) does not show a high SFR, and therefore SQ was apparently quenched. When considering the integrated SFR for the whole SQ and the NI, we found that both zones have a SFR consistent with those obtained in the SDSS star-forming galaxies. At least two chemically different gas components cohabit in SQ where, on average, the regions with high radial velocities (v$>$6160 km s$^{-1}$) have lower values of O/H and N/O than those with low radial velocities (v$\leq$6160 km s$^{-1}$). The values found for the line ratios, O/H, and N/O for the southern debris region and the northernmost tidal tail, are compatible with regions belonging to the outer part of the galaxies. We highlight the presence of inner-outer variation for O/H and some emission line ratios along the NI strands and the young tidal tail south strand. Finally, the SQ H$α$ regions are outside the galaxies because the interactions have dispersed the gas to the peripheral zones.
