GASP. XX. From the loose spatially-resolved to the tight global SFR-Mass relation in local spiral galaxies. (arXiv:1907.00976v1 [astro-ph.GA])

GASP. XX. From the loose spatially-resolved to the tight global SFR-Mass relation in local spiral galaxies. (arXiv:1907.00976v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Vulcani_B/0/1/0/all/0/1">Benedetta Vulcani</a> (INAF-OAPD), <a href="http://arxiv.org/find/astro-ph/1/au:+Poggianti_B/0/1/0/all/0/1">Bianca M. Poggianti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moretti_A/0/1/0/all/0/1">Alessia Moretti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Franchetto_A/0/1/0/all/0/1">Andrea Franchetto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gullieuszik_M/0/1/0/all/0/1">Marco Gullieuszik</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fritz_J/0/1/0/all/0/1">Jacopo Fritz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bettoni_D/0/1/0/all/0/1">Daniela Bettoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tonnesen_S/0/1/0/all/0/1">Stephanie Tonnesen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Radovich_M/0/1/0/all/0/1">Mario Radovich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jaffe_Y/0/1/0/all/0/1">Yara L. Jaffe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGee_S/0/1/0/all/0/1">Sean McGee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bellhouse_C/0/1/0/all/0/1">Callum Bellhouse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fasano_G/0/1/0/all/0/1">Giovanni Fasano</a>

Exploiting the sample of 30 local star-forming, undisturbed late-type
galaxies in different environments drawn from the GAs Stripping Phenomena in
galaxies with MUSE (GASP), we investigate the spatially resolved Star Formation
Rate-Mass ({Sigma}SFR-{Sigma}_star) relation. Our analysis includes also the
galaxy outskirts (up to >4 effective radii, re), a regime poorly explored by
other Integral Field Spectrograph surveys. Our observational strategy allows us
to detect H{alpha} out to more than 2.7re for 75% of the sample. Considering
all galaxies together, the correlation between the {Sigma}SFR and
{Sigma}_star is quite broad, with a scatter of 0.3 dex. It gets steeper and
shifts to higher {Sigma}_star values when external spaxels are excluded and
moving from less to more massive galaxies. The broadness of the overall
relation suggests galaxy-by-galaxy variations. Indeed, each object is
characterized by a distinct {Sigma}SFR-{Sigma}_star relation and in some
cases the correlation is very loose. The scatter of the relation mainly arises
from the existence of bright off-center star-forming knots whose
{Sigma}SFR-{Sigma}_star relation is systematically broader than that of the
diffuse component. The {Sigma}SFR-{Sigma}tot gas (total gas surface density)
relation is as broad as the {Sigma}SFR-{Sigma}_star relation, indicating that
the surface gas density is not a primary driver of the relation. Even though a
large galaxy-by-galaxy variation exists, mean {Sigma}SFR and {Sigma}_star
values vary of at most 0.7 dex across galaxies. We investigate the relationship
between the local and global SFR-M_star relation, finding that the latter is
driven by the existence of the size-mass relation.

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