GASP XXXIV: Unfolding the thermal side of ram pressure stripping in the jellyfish galaxy JO201

Abstract

X-ray studies of jellyfish galaxies play a crucial role in understanding the interactions between the interstellar medium (ISM) and the intracluster medium (ICM). In this paper, we focused on the jellyfish galaxy JO201. By combining archival Chandra observations, MUSE H$\alpha$ cubes, and maps of the emission fraction of the diffuse ionised gas, we investigated both its high energy spectral properties and the spatial correlation between its X-ray and optical emissions. The X-ray emission of JO201 is provided by both the Compton thick AGN (L${}_{\text{X}}^{0.5-10\text{keV}}$=2.7$\cdot$10${}^{41}$ erg s${}^{-1}$, not corrected for intrinsic absorption) and an extended component (L${}_{\text{X}}^{0.5-10\text{keV}}\approx$1.9-4.5$\cdot$10${}^{41}$ erg s${}^{-1}$) produced by a warm plasma (kT$\approx$1 keV), whose luminosity is higher than expected from the observed star formation (L${}_{\text{X}}\sim$3.8$\cdot 10^{40}$ erg s${}^{-1}$). The spectral analysis showed that the X-ray emission is consistent with the thermal cooling of hot plasma. These properties are similar to the ones found in other jellyfish galaxies showing extended X-ray emission. A point-to-point analysis revealed that this X-ray emission closely follows the ISM distribution, whereas CLOUDY simulations proved that the ionisation triggered by this warm plasma would be able to reproduce the [OI]/H$\alpha$ excess observed in JO201. We conclude that the galactic X-ray emitting plasma is originated on the surface of the ISM as a result of the ICM-ISM interplay. This process would entail the cooling and accretion of the ICM onto the galaxy, which could additionally fuel the star formation, and the emergence of [OI]/H$\alpha$ excess in the optical spectrum.

21 pages, 6 figures, 5 tables. Manuscript in press in Apj

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Cited by in corpus (28)

• Ram Pressure Stripping in High-Density Environments
• Simulating Groups and the IntraGroup Medium: The Surprisingly Complex and Rich Middle Ground Between Clusters and Galaxies
• A universal correlation between warm and hot gas in the stripped tails of cluster galaxies
• GASP XXXVIII: The LOFAR-MeerKAT-VLA view on the non-thermal side of a jellyfish galaxy
• Observing ram pressure at work in intermediate redshift clusters with MUSE: the case of Abell 2744and Abell 370
• How Ram Pressure Drives Radial Gas Motions in the Surviving Disk
• A New Method to Constrain the Appearance and Disappearance of Observed Jellyfish Galaxy Tails
• GASP XXXV: Characteristics of the diffuse ionised gas in gas-stripped galaxies
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• UV and H$\alpha$ HST observations of 6 GASP jellyfish galaxies
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• GASP XXXVII: The Most Extreme Jellyfish Galaxies Compared to Other Disk Galaxies in Clusters, an HI Study
• Ram pressure stripping in clusters: Gravity can bind the ISM but not the CGM
• The CO emission in the Taffy Galaxies (UGC 12914/5) at 60pc resolution-I: The battle for star formation in the turbulent Taffy Bridge
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• Clump formation in ram-pressure stripped galaxies: evidence from mass function
• Fading in the Flow: Suppression of cold gas growth in expanding galactic outflows
• Evidence for mixing between ICM and stripped ISM by the analysis of the gas metallicity in the tails of jellyfish galaxies