# GASP XVII. HI imaging of the jellyfish galaxy JO206: gas stripping and enhanced star formation

## TL;DR

This study uses VLA HI observations to analyze gas stripping and star formation in the jellyfish galaxy JO206, revealing a long HI tail, enhanced star formation, and rapid gas depletion caused by ram-pressure stripping.

## Contribution

First detailed HI imaging of JO206 showing gas stripping effects and star formation enhancement due to ram-pressure in a jellyfish galaxy.

## Key findings

- HI tail length matches ionised gas tail (≥90 kpc)
- HI depletion time is ~0.5 Gyr, four times shorter than normal spirals
- Star formation rate is higher than in similar galaxies

## Abstract

We present VLA HI observations of JO206, a prototypical ram-pressure stripped galaxy in the GASP sample. This massive galaxy (M$_{\ast} =$ 8.5 $\times$ 10$^{10}$ M$_{\odot}$) is located at a redshift of $z =$ 0.0513, near the centre of the low-mass galaxy cluster, IIZw108 ($\sigma \sim575$ km/s). JO206 is characterised by a long tail ($\geq$90 kpc) of ionised gas stripped away by ram-pressure. We find a similarly long HI tail in the same direction as the ionised gas tail and measure a total HI mass of $3.2 \times 10^{9}$ M$_{\odot}$. This is about half the expected HI mass given the stellar mass and surface density of JO206. A total of $1.8 \times 10^{9}$ M$_{\odot}$ (60%) of the detected HI is in the gas stripped tail. An analysis of the star formation rate shows that the galaxy is forming more stars compared to galaxies with the same stellar and HI mass. On average we find a HI gas depletion time of $\sim$0.5 Gyr which is about four times shorter than that of "normal" spiral galaxies. We performed a spatially resolved analysis of the relation between star formation rate density and gas density in the disc and tail of the galaxy at the resolution of our HI data. The star formation efficiency of the disc is about 10 times higher than that of the tail at fixed HI surface densities. Both the inner and outer parts of JO206 show an enhanced star formation compared to regions of similar HI surface density in field galaxies. The enhanced star formation is due to ram-pressure stripping during the galaxy's first infall into the cluster.