GASP XXXVII: The Most Extreme Jellyfish Galaxies Compared to Other Disk Galaxies in Clusters, an HI Study
N. Luber, A. Müller, J. H. van Gorkom, B. M. Poggianti, B. Vulcani, A. Franchetto, C. Bacchini, D. Bettoni, T. Deb, J. Fritz, M. Gullieuszik, A. Ignesti, Y. Jaf… 展开作者
N. Luber, A. Müller, J. H. van Gorkom, B. M. Poggianti, B. Vulcani, A. Franchetto, C. Bacchini, D. Bettoni, T. Deb, J. Fritz, M. Gullieuszik, A. Ignesti, Y. Jaffe, A. Moretti, R. Paladino, M. Ramatsoku, P. Serra, R. Smith, N. Tomicic, S. Tonnesen, M. Verheijen, A. Wolter
我们提出的VLA HI成像调查的结果，旨在了解为什么一些星系开发长的面外H $α$尾巴，成为极端的水母星系。观测集中在五个极端的水母星系，光学选择的WINGS和OmegaWINGS调查，并确认有长H $α$尾巴通过MUSE观测。每个星系都位于不同的星系团中。在观测中，在视场（40'x40'）和观测带宽（6500 km/s $^{-1}$）内共有88个其他螺旋星系。我们检测到这88个螺旋中的13个，加上一个未编目的螺旋，HI质量范围从1到7 $\times$ 10 ${^9}$ M $_{\odot}$。许多这些检测扩展HI磁盘，两个显示冲压压力剥离的直接证据，而其他可能受潮汐力和/或冲压压力剥离。我们将75个未探测到的螺旋星系叠加起来，发现它们的平均HI质量为1.9 $\times$ 10 $^{8}$ M $_{\odot}$，这意味着它们的平均恒星质量非常缺乏HI。比较极端水母星系和其他盘状星系，我们发现它们比几乎所有盘状星系都有更大的恒星质量，比所有HI探测到的星系都有更小的离星系团中心的投影距离，比所有HI探测到的星系和大多数未探测到的星系都有更高的相对速度。我们的结论是，高恒星质量允许极端的水母星系在被剥离之前深深地落入星系团，周围的ICM压力产生了它们壮观的恒星形成尾巴。
英文摘要：
We present the results of a VLA HI imaging survey aimed at understanding why some galaxies develop long extraplanar H$α$ tails, becoming extreme jellyfish galaxies. The observations are centered on five extreme jellyfish galaxies, optically selected from the WINGS and OmegaWINGS surveys and confirmed to have long H$α$ tails through MUSE observations. Each galaxy is located in a different cluster. In the observations there are in total 88 other spiral galaxies within the field of view (40'x40') and observed bandwidth (6500 km s$^{-1}$). We detect 13 of these 88 spirals, plus one uncatalogued spiral, with HI masses ranging from 1 to 7 $\times$ 10${^9}$ M$_{\odot}$. Many of these detections have extended HI disks, two show direct evidence for ram pressure stripping, while others are possibly affected by tidal forces and/or ram-pressure stripping. We stack the 75 non-detected spiral galaxies and find an average HI mass of 1.9 $\times$ 10$^{8}$ M$_{\odot}$, which given their average stellar mass, implies they are very HI deficient. Comparing the extreme jellyfish galaxies to the other disk galaxies, we find that they have a larger stellar mass than almost all disk galaxies and than all HI detected galaxies, they are at smaller projected distance from the cluster center and at higher relative velocity to the cluster mean than all HI detections and most non-detections. We conclude that the high stellar mass allows extreme jellyfish galaxies to fall deeply into the cluster before being stripped and the surrounding ICM pressure gives rise to their spectacular star-forming tails.
Ultra-Violet Imaging Telescope view of ram-pressure stripping in action: Star formation in the stripped gas of the GASP jellyfish galaxy JO201 in Abell 85
Molecular gas and star formation in GASP jellyfish galaxies
INAF - Padova Astronomical Observatory（意大利国家天体物理研究所帕多瓦天文台）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文研究所）；European Southern Observatory（欧洲南方天文台）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯玻尔研究所DARK中心）；Dipartimento di Fisica e Astronomia, Università di Bologna（博洛尼亚大学物理与天文学系）；INAF - Osservatorio Astrofisico di Arcetri（意大利国家天体物理研究所阿切尔奇天文台）；Center for Astrophysics - Harvard & Smithsonian（哈佛-史密森天体物理中心）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）
INAF - Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；INAF - Osservatorio Astronomico di Cagliari（意大利国家天体物理研究所卡利亚里天文台）；Leibniz Institute for Astrophysics Potsdam (AIP)（波茨坦莱布尼茨天体物理研究所）；Center for Computational Astrophysics, Flatiron Institute（平托研究所计算天体物理学中心）；Departamento de Física, Universidad Técnica Federico Santa María（弗雷德里科·圣塔玛利亚技术大学物理系）；Millennium Nucleus for Galaxies (MINGAL)（星系千年核心）；DARK, Niels Bohr Institute, University of Copenhagen（哥本哈根大学尼尔斯·玻尔研究所DARK研究中心）；Kapteyn Astronomical Institute, University of Groningen（格罗宁根大学卡普坦天文研究所）；Department of Physics and Astronomy "Augusto Righi", University of Bologna（博洛尼亚大学奥古斯托·里吉物理与天文学系）；INAF - Osservatorio Astronomico di Brera（意大利国家天体物理研究所布雷拉天文台）；University Observatory, LMU Faculty of Physics（慕尼黑大学物理学院天文台）；INAF - Istituto di Radioastronomia（意大利国家天体物理研究所射电天文学研究所）
