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GASP XXIII: a jellyfish galaxy as an astrophysical laboratory of the baryonic cycle

Poggianti, Bianca M.; Ignesti, Alessandro; Gitti, Myriam; Wolter, Anna; Brighenti, Fabrizio; Biviano, Andrea; George, Koshy; Vulcani, Benedetta; Gullieuszik, Marco; Moretti, Alessia; Paladino, Rosita; Bettoni, Daniela; Franchetto, Andrea; Jaffé, Yara L.; Radovich, Mario; Roediger, Elke; Tomičić, Neven; Tonnesen, Stephanie; Bellhouse, Callum; Fritz, Jacopo; Omizzolo, Alessandro


Bianca M. Poggianti

Alessandro Ignesti

Myriam Gitti

Anna Wolter

Fabrizio Brighenti

Andrea Biviano

Koshy George

Benedetta Vulcani

Marco Gullieuszik

Alessia Moretti

Rosita Paladino

Daniela Bettoni

Andrea Franchetto

Yara L. Jaffé

Mario Radovich

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Dr Elke Roediger
Reader in Astrophysics/ Director of Studies for Physics

Neven Tomičić

Stephanie Tonnesen

Callum Bellhouse

Jacopo Fritz

Alessandro Omizzolo


© 2019. The American Astronomical Society. All rights reserved. With MUSE, Chandra, VLA, ALMA, and UVIT data from the GASP program, we study the multiphase baryonic components in a jellyfish galaxy (JW100) with a stellar mass 3.2 × 1011 M o hosting an active galactic nucleus (AGN). We present its spectacular extraplanar tails of ionized and molecular gas, UV stellar light, and X-ray and radio continuum emission. This galaxy represents an excellent laboratory to study the interplay between different gas phases and star formation and the influence of gas stripping, gas heating, and AGNs. We analyze the physical origin of the emission at different wavelengths in the tail, in particular in situ star formation (related to Hα, CO, and UV emission), synchrotron emission from relativistic electrons (producing the radio continuum), and heating of the stripped interstellar medium (ISM; responsible for the X-ray emission). We show the similarities and differences of the spatial distributions of ionized gas, molecular gas, and UV light and argue that the mismatch on small scales (1 kpc) is due to different stages of the star formation process. We present the relation Hα-X-ray surface brightness, which is steeper for star-forming regions than for diffuse ionized gas regions with a high [O i]/Hα ratio. We propose that ISM heating due to interaction with the intracluster medium (either for mixing, thermal conduction, or shocks) is responsible for the X-ray tail, observed [O i] excess, and lack of star formation in the northern part of the tail. We also report the tentative discovery in the tail of the most distant (and among the brightest) currently known ULX, a pointlike ultraluminous X-ray source commonly originating in a binary stellar system powered by either an intermediate-mass black hole or a magnetized neutron star.


Poggianti, B. M., Ignesti, A., Gitti, M., Wolter, A., Brighenti, F., Biviano, A., …Omizzolo, A. (2019). GASP XXIII: a jellyfish galaxy as an astrophysical laboratory of the baryonic cycle. The Astrophysical journal, 887(2),

Journal Article Type Article
Acceptance Date Oct 25, 2019
Online Publication Date Dec 17, 2019
Publication Date Dec 20, 2019
Deposit Date Jan 15, 2020
Journal Astrophysical Journal
Print ISSN 0004-637X
Electronic ISSN 1538-4357
Publisher American Astronomical Society
Peer Reviewed Peer Reviewed
Volume 887
Issue 2
Article Number 155
Keywords Galaxy evolution; Galaxy clusters; Galaxy processes
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Copyright Statement
© 2019. The American Astronomical Society. All rights reserved.

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