The newborn planet population emerging from ring-like structures in discs. (arXiv:1903.05117v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Lodato_G/0/1/0/all/0/1">G. Lodato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dipierro_G/0/1/0/all/0/1">G. Dipierro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ragusa_E/0/1/0/all/0/1">E. Ragusa</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Long_F/0/1/0/all/0/1">F. Long</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herczeg_G/0/1/0/all/0/1">G.J. Herczeg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pascucci_I/0/1/0/all/0/1">I. Pascucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pinilla_P/0/1/0/all/0/1">P. Pinilla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Manara_C/0/1/0/all/0/1">C. F. Manara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tazzari_M/0/1/0/all/0/1">M. Tazzari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Liu_Y/0/1/0/all/0/1">Y. Liu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mulders_G/0/1/0/all/0/1">G. D. Mulders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harsono_D/0/1/0/all/0/1">D. Harsono</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boehler_Y/0/1/0/all/0/1">Y. Boehler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Menard_F/0/1/0/all/0/1">F. Menard</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Johnstone_D/0/1/0/all/0/1">D. Johnstone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Salyk_C/0/1/0/all/0/1">C. Salyk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Plas_G/0/1/0/all/0/1">G. van der Plas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrit_S/0/1/0/all/0/1">S. Cabrit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Edwards_S/0/1/0/all/0/1">S. Edwards</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_W/0/1/0/all/0/1">W. J. Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hendler_N/0/1/0/all/0/1">N. Hendler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nisini_B/0/1/0/all/0/1">B. Nisini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rigliaco_E/0/1/0/all/0/1">E. Rigliaco</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Avenhaus_H/0/1/0/all/0/1">H. Avenhaus</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banzatti_A/0/1/0/all/0/1">A. Banzatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gully_Santiago_M/0/1/0/all/0/1">M. Gully-Santiago</a>
ALMA has observed a plethora of ring-like structures in planet forming discs
at distances of 10-100 au from their host star. Although several mechanisms
have been invoked to explain the origin of such rings, a common explanation is
that they trace new-born planets. Under the planetary hypothesis, a natural
question is how to reconcile the apparently high frequency of gap-carving
planets at 10-100 au with the paucity of Jupiter mass planets observed around
main sequence stars at those separations. Here, we provide an analysis of the
new-born planet population emerging from observations of gaps in discs, under
the assumption that the observed gaps are due to planets. We use a simple
estimate of the planet mass based on the gap morphology, and apply it to a
sample of gaps recently obtained by us in a survey of Taurus with ALMA. We also
include additional data from recent published surveys, thus analysing the
largest gap sample to date, for a total of 48 gaps. The properties of the
purported planets occupy a distinctively different region of parameter space
with respect to the known exo-planet population, currently not accessible
through planet finding methods. Thus, no discrepancy in the mass and radius
distribution of the two populations can be claimed at this stage. We show that
the mass of the inferred planets conforms to the theoretically expected trend
for the minimum planet mass needed to carve a dust gap. Finally, we estimate
the separation and mass of the putative planets after accounting for migration
and accretion, for a range of evolutionary times, finding a good match with the
distribution of cold Jupiters.
ALMA has observed a plethora of ring-like structures in planet forming discs
at distances of 10-100 au from their host star. Although several mechanisms
have been invoked to explain the origin of such rings, a common explanation is
that they trace new-born planets. Under the planetary hypothesis, a natural
question is how to reconcile the apparently high frequency of gap-carving
planets at 10-100 au with the paucity of Jupiter mass planets observed around
main sequence stars at those separations. Here, we provide an analysis of the
new-born planet population emerging from observations of gaps in discs, under
the assumption that the observed gaps are due to planets. We use a simple
estimate of the planet mass based on the gap morphology, and apply it to a
sample of gaps recently obtained by us in a survey of Taurus with ALMA. We also
include additional data from recent published surveys, thus analysing the
largest gap sample to date, for a total of 48 gaps. The properties of the
purported planets occupy a distinctively different region of parameter space
with respect to the known exo-planet population, currently not accessible
through planet finding methods. Thus, no discrepancy in the mass and radius
distribution of the two populations can be claimed at this stage. We show that
the mass of the inferred planets conforms to the theoretically expected trend
for the minimum planet mass needed to carve a dust gap. Finally, we estimate
the separation and mass of the putative planets after accounting for migration
and accretion, for a range of evolutionary times, finding a good match with the
distribution of cold Jupiters.
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