TY - JOUR
T1 - GASP XXXVII
T2 - The Most Extreme Jellyfish Galaxies Compared with Other Disk Galaxies in Clusters, an H i Study
AU - Luber, N.
AU - Müller, A.
AU - Van Gorkom, J. H.
AU - Poggianti, B. M.
AU - Vulcani, B.
AU - Franchetto, A.
AU - Bacchini, C.
AU - Bettoni, D.
AU - Deb, T.
AU - Fritz, J.
AU - Gullieuszik, M.
AU - Ignesti, A.
AU - Jaffe, Y.
AU - Moretti, A.
AU - Paladino, R.
AU - Ramatsoku, M.
AU - Serra, P.
AU - Smith, R.
AU - Tomicic, N.
AU - Tonnesen, S.
AU - Verheijen, M.
AU - Wolter, A.
N1 - Funding Information:
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under a cooperative agreement by Associated Universities, Inc. J.F. acknowledges financial support from the UNAM-DGAPA-PAPIIT IN111620 grant, Mexico. A.I., D.B., M.G., R.P., and B.V. acknowledge the Italian PRIN-Miur 2017 (PI: A. Cimatti). Y.J. acknowledges financial support from CONICYT PAI (Concurso Nacional de Inserción en la Academia 2017) No. 79170132 and FONDECYT Iniciación 2018 No. 11180558. M.V. acknowledges support by the Netherlands Foundation for Scientific Research (NWO) through VICI grant 016.130.338. Based on observations collected at the European Organization for Astronomical Research in the Southern Hemisphere under ESO program 196.B-0578. This project has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (grant agreement No. 833824). This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement No. 679627). We acknowledge funding from the INAF mainstream funding program (PI: B. Vulcani).
Publisher Copyright:
© 2022. The Author(s). Published by the American Astronomical Society.
PY - 2022/3/1
Y1 - 2022/3/1
N2 - We present the results of a Very Large Array H i imaging survey aimed at understanding why some galaxies develop long extraplanar Hα 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 Hα 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′ × 40′) and observed bandwidth (6500 km s-1). We detect 13 of these 88 spirals, plus one uncataloged spiral, with H i masses ranging from 1 to 7 × 109 M ⊙. Many of these detections have extended H i disks, two show direct evidence for ram pressure stripping, and others are possibly affected by tidal forces and/or ram pressure stripping. We stack the 75 nondetected spiral galaxies and find an average H i mass of 1.9 × 108 M ⊙, which, given their average stellar mass, implies that they are very H i deficient. Comparing the extreme jellyfish galaxies to the other disk galaxies, we find that they are at smaller projected distance from the cluster center, and have a higher stellar mass and higher relative velocity than all other H i detections and most nondetections. 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.
AB - We present the results of a Very Large Array H i imaging survey aimed at understanding why some galaxies develop long extraplanar Hα 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 Hα 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′ × 40′) and observed bandwidth (6500 km s-1). We detect 13 of these 88 spirals, plus one uncataloged spiral, with H i masses ranging from 1 to 7 × 109 M ⊙. Many of these detections have extended H i disks, two show direct evidence for ram pressure stripping, and others are possibly affected by tidal forces and/or ram pressure stripping. We stack the 75 nondetected spiral galaxies and find an average H i mass of 1.9 × 108 M ⊙, which, given their average stellar mass, implies that they are very H i deficient. Comparing the extreme jellyfish galaxies to the other disk galaxies, we find that they are at smaller projected distance from the cluster center, and have a higher stellar mass and higher relative velocity than all other H i detections and most nondetections. 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.
UR - http://www.scopus.com/inward/record.url?scp=85126581693&partnerID=8YFLogxK
U2 - 10.3847/1538-4357/ac469a
DO - 10.3847/1538-4357/ac469a
M3 - Article
AN - SCOPUS:85126581693
SN - 0004-637X
VL - 927
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 39
ER -