Clump formation in ram-pressure stripped galaxies: evidence from mass function

Eric Giunchi; Claudia Scarlata; Ariel Werle; Bianca M. Poggianti; Alessia Moretti; Marco Gullieuszik; Bendetta Vulcani; Alessandro Ignesti; Antonino Marasco; Anita Zanella; Anna Wolter

doi:10.1051/0004-6361/202452983

paper

Clump formation in ram-pressure stripped galaxies: evidence from mass function

arXiv:2502.15554 · doi:10.1051/0004-6361/202452983

Abstract

The mass function (MF) of young ( $age ≲ 200$ Myr) stellar clumps is an indicator of the mechanism driving the collapse of the interstellar medium (ISM) into giant molecular clouds. Typically, the clump MF in main-sequence galaxies is described by a power law ( $d N / d M_{*} \propto M_{*}^{- α}$ ) with slope $α = 2$ , hinting a turbulence-driven collapse. To understand whether the local environment affects star formation, we have modelled the clump MF of six cluster galaxies from the GASP survey, undergoing strong ram-pressure stripping. This process, exerted by the hot and high-pressure intra-cluster medium (ICM), has produced long tails of stripped ISM where clumps form far away from the galactic disk and surrounded by the ICM itself. Clumps were selected from HST-UVIS/WFC3 images, covering from near-UV to red-optical bands and including H $α$ -line maps. The catalogue comprises 398 H $α$ (188 in tails, 210 in disk outskirts, the so-called extraplanar region) and 1270 UV clumps (593 tail, 677 extraplanar). Using mock images, we quantified the mass completeness and bias of our sample. Accounting for these two effects, we adopted a Bayesian approach to fit the clump mass catalogue to a chosen function. The resulting MFs are steeper than expected. In the tails, the H $α$ clumps have slope $α = 2.31 \pm 0.12$ , while the UV slope is larger ( $2.60 \pm 0.09$ ), in agreement with ageing effects. Similar results are found in the extraplanar region, with H $α$ slope $α = 2.4 5_{- 0.16}^{+ 0.20}$ and UV slope $α = 2.6 3_{- 0.18}^{+ 0.20}$ , even if they are consistent within uncertainties. We suggest that the steepening results from the higher-than-usual turbulent environment, arising from the interaction between ISM and ICM. As shown by recent works, this process can favour the fragmentation of the largest ISM clouds, inhibiting the formation of very massive clumps.

Clump formation in ram-pressure stripped galaxies: evidence from mass function

Abstract

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