GASP XXX. The spatially resolved SFR-Mass relation in stripping galaxies in the local universe. (arXiv:2007.04996v1 [astro-ph.GA])

GASP XXX. The spatially resolved SFR-Mass relation in stripping galaxies in the local universe. (arXiv:2007.04996v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">B. Vulcani</a> (INAF-OaPD), <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">B. M. Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tonnesen_S/0/1/0/all/0/1">S. Tonnesen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGee_S/0/1/0/all/0/1">S. L. McGee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">A. Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">J. Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullieuszik_M/0/1/0/all/0/1">M. Gullieuszik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Y. L. Jaffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franchetto_A/0/1/0/all/0/1">A. Franchetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tomicic_N/0/1/0/all/0/1">N. Tomicic</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mingozzi_M/0/1/0/all/0/1">M. Mingozzi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bettoni_D/0/1/0/all/0/1">D. Bettoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wolter_A/0/1/0/all/0/1">A. Wolter</a>

The study of the spatially resolved Star Formation Rate-Mass
(Sigma_SFR-Sigma_M) relation gives important insights on how galaxies assemble
at different spatial scales. Here we present the analysis of the
Sigma_SFR-Sigma_M of 40 local cluster galaxies undergoing ram pressure
stripping drawn from the GAs Stripping Phenomena in galaxies (GASP) sample.
Considering their integrated properties, these galaxies show a SFR enhancement
with respect to undisturbed galaxies of similar stellar mass; we now exploit
spatially resolved data to investigate the origin and location of the excess.
Even on ~1kpc scales, stripping galaxies present a systematic enhancement of
Sigma_SFR (~0.35 dex at Sigma_M =108^M_sun/kpc^2) at any given Sigma_M compared
to their undisturbed counterparts. The excess is independent on the degree of
stripping and of the amount of star formation in the tails and it is visible at
all galactocentric distances within the disks, suggesting that the star
formation is most likely induced by compression waves from ram pressure. Such
excess is larger for less massive galaxies and decreases with increasing mass.
As stripping galaxies are characterised by ionised gas beyond the stellar disk,
we also investigate the properties of 411 star forming clumps found in the
galaxy tails. At any given stellar mass density, these clumps are
systematically forming stars at a higher rate than in the disk, but differences
are reconciled when we just consider the mass formed in the last few 10^8yr
ago, suggesting that on these timescales the local mode of star formation is
similar in the tails and in the disks.

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