Deep MUSE observations in the HDFS - Morpho-kinematics of distant star-forming galaxies down to 108M⊙
Deep MUSE observations in the HDFS - Morpho-kinematics of distant star-forming galaxies down to 108M⊙
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HDFS 中的深度 MUSE 观测 - 低至 108M 的遥远恒星形成星系的形态运动学⊙
DOI：
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
G. Soucail
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作者：
T. Contini;B. Épinat;N. Bouch'e;J. Brinchmann;L. Boogaard;E. Ventou;R. Bacon;J. Richard;P. Weilbacher;L. Wisotzki;D. Krajnovi'c;J. Vielfaure;E. Emsellem;H. Finley;H. Inami;J. Schaye;M. Swinbank;A. Gu'erou;T. Martinsson;L. Michel;I. Schroetter;M. Shirazi;G. Soucail
目标。虽然大质量星系的气体运动学演化现在相对较好地建立了红移z类似于3，但对较低质量（M-* \textless= 10（10）M-circle dot）星系的运动学知之甚少。我们使用MUSE，一个功能强大的宽视场，光学积分场摄谱仪（IFS）最近安装在VLT，在中等红移的星系人口的特点。方法.我们利用了迄今为止在哈勃深场南方（HDFS）上进行的最深的MUSE观测。该数据立方体由27小时的积分时间产生，覆盖了前所未有的深度处的1弧分（2）视场（1 σ发射线表面亮度极限为1 × 10（19）erg s（-1）cm（-2）arcsec（-2）），最终空间分辨率约为0.7 μ m。我们确定了一个28个分辨发射线星系的样本，延伸的区域至少是视星盘的两倍，分布在0.2 \textless z \textless 1.4的红移间隔上。超过一半的星系的z近似于0.3近似于0.7，这是一个迄今为止用IFS运动学研究得很少的红移范围。我们使用的公共HST图像和多波段测光的HDFS约束恒星质量和星星形成率（SFR）的星系，并使用GALFIT进行形态分析，提供估计的磁盘倾角，磁盘规模的长度，和主轴的位置角。我们从MUSE数据中导出了这些星系的电离气体特性，并对盘进行了建模（在2D和3D中使用GALPAK（3D）），以检索其固有气体运动学，包括最大旋转速度和速度色散。结果我们建立了一个样本的解决发射线星系的恒星质量低得多，SFR（由类似的1-2个数量级）比以前的IFS调查。大多数空间分辨的MUSE-HDFS星系的气体运动学与盘状旋转一致，但大约20%的速度色散大于旋转速度，30%是一个紧密的对的一部分和/或显示出最近引力相互作用的明显迹象。这些分数与之前IFS对更大质量星系的调查中发现的相似，表明电离气体的动力学状态和恒星形成星系的引力相互作用水平不是恒星质量的强函数。在高质量的制度，MUSE-HDFS星系遵循塔利-费舍尔关系定义从以前的IFS调查在一个类似的红移范围。这种比例关系也延伸到较低的质量/速度，但具有较高的分散。我们发现，90%的恒星质量低于10（9.5）M圆点的MUSE-HDFS星系都有沉降的气体盘。MUSE-HDFS星系遵循在局部宇宙中定义的特定角动量和恒星质量之间的标度关系。然而，我们发现，中等红移，恒星形成星系填补了从螺旋到椭圆局部标度关系的连续过渡，根据动力学状态（即，旋转或色散为主）。这表明一些星系可能会失去它们的角动量，并在变得被动之前变得弥散主导。
Aims. Whereas the evolution of gas kinematics of massive galaxies is now relatively well established up to redshift z similar to 3, little is known about the kinematics of lower mass (M-* \textless= 10(10) M-circle dot) galaxies. We use MUSE, a powerful wide-field, optical integral-field spectrograph (IFS) recently mounted on the VLT, to characterize this galaxy population at intermediate redshift. Methods. We made use of the deepest MUSE observations performed so far on the Hubble Deep Field South (HDFS). This data cube, resulting from 27 h of integration time, covers a one arcmin(2) field of view at an unprecedented depth (with a 1 sigma emission-line surface brightness limit of 1 x 10(19) erg s(-1) cm(-2) arcsec(-2)) and a final spatial resolution of approximate to 0.7 `'. We identified a sample of 28 resolved emission-line galaxies, extending over an area that is at least twice the seeing disk, spread over a redshift interval of 0.2 \textless z \textless 1.4. More than half of the galaxies are at z similar to 0.3 similar to 0.7, which is a redshift range poorly studied so far with IFS kinematics. We used the public HST images and multiband photometry over the HDFS to constrain the stellar mass and star formation rate (SFR) of the galaxies and to perform a morphological analysis using GALFIT, providing estimates of the disk inclination, disk scale length, and position angle of the major axis. We derived the resolved ionized gas properties of these galaxies from the MUSE data and model the disk (both in 2D and in 3D with GALPAK(3D)) to retrieve their intrinsic gas kinematics, including the maximum rotation velocity and velocity dispersion. Results. We build a sample of resolved emission-line galaxies of much lower stellar mass and SFR (by similar to 1-2 orders of magnitude) than previous IFS surveys. The gas kinematics of most of the spatially resolved MUSE-HDFS galaxies is consistent with disk-like rotation, but about 20% have velocity dispersions that are larger than the rotation velocities and 30% are part of a close pair and/or show clear signs of recent gravitational interactions. These fractions are similar to what has been found in previous IFS surveys of more massive galaxies, indicating that the dynamical state of the ionized gas and the level of gravitational interactions of star-forming galaxies is not a strong function of their stellar mass. In the high-mass regime, the MUSE-HDFS galaxies follow the Tully-Fisher relation defined from previous IFS surveys in a similar redshift range. This scaling relation also extends to lower masses/velocities but with a higher dispersion. We find that 90% of the MUSE-HDFS galaxies with stellar masses below 10(9.5) M-circle dot have settled gas disks. The MUSE-HDFS galaxies follow the scaling relations defined in the local Universe between the specific angular momentum and stellar mass. However, we find that intermediate-redshift, star-forming galaxies fill a continuum transition from the spiral to elliptical local scaling relations, according to the dynamical state (i.e., rotation-or dispersion-dominated) of the gas. This indicates that some galaxies may lose their angular momentum and become dispersion-dominated prior to becoming passive.
DOI：
10.1088/0004-637x/799/2/209
发表时间：
2014-09
期刊：
The Astrophysical Journal
影响因子：
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作者：
E. Wisnioski;N. F. Schreiber;S. Wuyts;E. Wuyts;K. Bandara;D. Wilman;R. Genzel;R. Bender;R. Da
通讯作者：
E. Wisnioski;N. F. Schreiber;S. Wuyts;E. Wuyts;K. Bandara;D. Wilman;R. Genzel;R. Bender;R. Da
低z发光恒星形成星系的电离气体流出和整体运动学
DOI：
10.1017/s174392131400934x
发表时间：
2015
期刊：
Proceedings of the International Astronomical Union
影响因子：
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作者：
Arribas S
通讯作者：
Arribas S