SAMI-H i : The H i view of the Hα Tully–Fisher relation and data release
SAMI-H i : The H i view of the Hα Tully–Fisher relation and data release
复制标题
萨米-哈伊：哈伊对哈塔利费舍尔关系和数据发布的看法
DOI：
10.1093/mnras/stac3556
复制
发表时间：
2022
影响因子：
4.8
通讯作者：
Bland-Hawthorn, Joss
中科院分区：
文献类型：
--
作者：
Catinella, Barbara;Cortese, Luca;Tiley, Alfred L.;Janowiecki, Steven;Watts, Adam B.;Bryant, Julia J.;Croom, Scott M.;d’Eugenio, Francesco;van de Sande, Jesse;Bland-Hawthorn, Joss
我们目前SAMI-喜，296个星系的原子氢含量的调查与积分场光谱可从SAMI星系调查。样本跨越近4 dex的恒星质量（），红移< 0.06，并包括153个星系的新阿雷西博观测，我们发布了目录和Hispectra。我们使用这些数据来比较从光学和无线电观测获得的旋转速度，并显示系统的差异如何影响恒星质量和重子Tully-Fisher关系的斜率和散射。具体来说，我们表明，在星系内部测量的旋转速度（在这项工作中为1.3有效半径）系统地低估了Higlitazone测量，在低恒星质量下，Hi/速度比增加，旋转曲线通常仍在上升，测量没有达到其高原。结果表明，与Hiconterpart相比，恒星质量的Tully-Fisher关系更陡（当M φ为自变量时），并且具有更大的离散度。有趣的是，我们确认存在一小部分的低质量异常值的关系，不存在时，使用高速宽度，并没有解释的“孔径效应”。这些似乎是高度干扰的系统，其宽度不提供一个可靠的估计旋转速度。我们的分析重申了考虑到速度定义的差异，以及示踪剂时使用的解释从塔利-费舍尔关系，在低和高的红移和模拟比较偏移的重要性。
We present SAMI-Hi, a survey of the atomic hydrogen content of 296 galaxies with integral field spectroscopy available from the SAMI Galaxy Survey. The sample spans nearly 4 dex in stellar mass (), redshiftz< 0.06, and includes new Arecibo observations of 153 galaxies, for which we release catalogues and Hispectra. We use these data to compare the rotational velocities obtained from optical and radio observations and to show how systematic differences affect the slope and scatter of the stellar-mass and baryonic Tully–Fisher relations. Specifically, we show thatrotational velocities measured in the inner parts of galaxies (1.3 effective radii in this work) systematically underestimate Higlobal measurements, with Hi/velocity ratios that increase at low stellar masses, where rotation curves are typically still rising andmeasurements do not reach their plateau. As a result, thestellar mass Tully–Fisher relation is steeper (whenM⋆is the independent variable) and has larger scatter than its Hicounterpart. Interestingly, we confirm the presence of a small fraction of low-mass outliers of therelation that are not present when Hivelocity widths are used and are not explained by ‘aperture effects’. These appear to be highly disturbed systems for whichwidths do not provide a reliable estimate of the rotational velocity. Our analysis reaffirms the importance of taking into account differences in velocity definitions as well as tracers used when interpreting offsets from the Tully–Fisher relation, at both low and high redshifts and when comparing with simulations.