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GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?

Moretti, Alessia; Paladino, Rosita; Poggianti, Bianca M.; Poggianti, Bianca M; Serra, Paolo; Roediger, Elke; Gullieuszik, Marco; Tomiči´c, Neven Tomiči´; Tomičić, Neven; Radovich, Mario; Vulcani, Benedetta; Jaffé, Yara L; Jaffé, Yara L.; Fritz, Jacopo; Bettoni, Daniela; Ramatsoku, Mpati; Wolter, Anna

Authors

Alessia Moretti

Rosita Paladino

Bianca M. Poggianti

Bianca M Poggianti

Paolo Serra

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Dr Elke Roediger E.Roediger@hull.ac.uk
Senior Lecturer/ Director of Studies for Physics

Marco Gullieuszik

Neven Tomiči´ Tomiči´c

Neven Tomičić

Mario Radovich

Benedetta Vulcani

Yara L Jaffé

Yara L. Jaffé

Jacopo Fritz

Daniela Bettoni

Mpati Ramatsoku

Anna Wolter



Abstract

Within the GASP survey, aimed at studying the effect of the ram-pressure stripping on the star formation quenching in cluster galaxies, we analyze here ALMA observations of the jellyfish galaxy JW100. We find an unexpected large amount of molecular gas (∼ 2.5 × 10 10 M), 30% of which is located in the stripped gas tail out to ∼35 kpc from the galaxy center. The overall kinematics of molecular gas is similar to the one shown by the ionized gas, but for clear signatures of double components along the stripping direction detected only out to 2 kpc from the disk. The line ratio r 21 has a clumpy distribution and in the tail can reach large values (≥ 1), while its average value is low (0.58 with a 0.15 dispersion). All these evidence strongly suggest that the molecular gas in the tail is newly born from stripped HI gas or newly condensed from stripped diffuse molecular gas. The analysis of interferometric data at different scales reveals that a significant fraction (∼ 40%) of the molecular gas is extended over large scales (≥ 8 kpc) in the disk, and this fraction becomes predominant in the tail (∼ 70%). By comparing the molecular gas surface density with the star formation rate surface density derived from the Hα emission from MUSE data, we find that the depletion time on 1 kpc scale is particularly large (5 − 10 Gyr) both within the ram-pressure disturbed region in the stellar disk, and in the complexes along the tail.

Citation

Moretti, A., Paladino, R., Poggianti, B. M., Serra, P., Roediger, E., Gullieuszik, M., …Wolter, A. (2019). GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?. The Astrophysical journal, 889(1), . https://doi.org/10.3847/1538-4357/ab616a

Journal Article Type Article
Acceptance Date Dec 11, 2019
Online Publication Date Jan 20, 2020
Publication Date Dec 16, 2019
Deposit Date Jan 22, 2020
Publicly Available Date Jan 27, 2020
Journal The Astrophysical Journal
Print ISSN 0004-637X
Publisher American Astronomical Society
Peer Reviewed Peer Reviewed
Volume 889
Issue 1
Pages
DOI https://doi.org/10.3847/1538-4357/ab616a
Keywords Space and Planetary Science; Astronomy and Astrophysics; D galaxies (346); Galaxy clusters (584); Molecular gas (1073); Galaxy evolution (594)
Public URL https://hull-repository.worktribe.com/output/3352218
Additional Information Journal title: The Astrophysical Journal; Article type: paper; Article title: GASP. XXII. The Molecular Gas Content of the JW100 Jellyfish Galaxy at z ∼ 0.05: Does Ram Pressure Promote Molecular Gas Formation?; Copyright information: © 2020. The American Astronomical Society. All rights reserved.; Date received: 2019-09-17; Date accepted: 2019-12-11; Online publication date: 2020-01-20

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