Reconstructing Nearby Young Clusters with Gaia EDR3. (arXiv:2110.04296v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Heyl_J/0/1/0/all/0/1">Jeremy Heyl</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caiazzo_I/0/1/0/all/0/1">Ilaria Caiazzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Richer_H/0/1/0/all/0/1">Harvey Richer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Miller_D/0/1/0/all/0/1">David R. Miller</a>
We searched through a seven-million cubic-parsec volume surrounding each of
the four nearest young open clusters with ages from 40 to 80 Myr to identify
both the current and past members of the clusters within the Gaia EDR3 dataset.
We find over 1,700 current cluster members and over 1,200 candidate escapees.
Many of these candidates lie well in front and behind the cluster from our
point of view, so formerly they were considered cluster members, but their
parallaxes put them more than 10 pc from the centre of the cluster today. We
found two candidate high-mass white dwarfs that may have escaped from the alpha
Persei cluster and several candidate main-sequence-white-dwarf binaries
associated with the younger clusters, NGC 2451A, IC 2391 and IC 2602. All of
these objects require spectroscopic confirmation. Using these samples of
escapee candidates, we develop and implement a novel technique to determine the
ages of these clusters and the Pleiades using kinematics with typical
uncertainties of $5-7$ Myr. For all five clusters, this kinematic age is
younger than the age estimated with isochrones but within the uncertainties of
the isochrone fitting. We find for the clusters that travel far from the
Galactic plane (the Pleiades, NGC 2451A and IC 2602), the formation of the
cluster coincides with when the cluster was in the Galactic plane within a few
Myr, supporting these age determinations.
We searched through a seven-million cubic-parsec volume surrounding each of
the four nearest young open clusters with ages from 40 to 80 Myr to identify
both the current and past members of the clusters within the Gaia EDR3 dataset.
We find over 1,700 current cluster members and over 1,200 candidate escapees.
Many of these candidates lie well in front and behind the cluster from our
point of view, so formerly they were considered cluster members, but their
parallaxes put them more than 10 pc from the centre of the cluster today. We
found two candidate high-mass white dwarfs that may have escaped from the alpha
Persei cluster and several candidate main-sequence-white-dwarf binaries
associated with the younger clusters, NGC 2451A, IC 2391 and IC 2602. All of
these objects require spectroscopic confirmation. Using these samples of
escapee candidates, we develop and implement a novel technique to determine the
ages of these clusters and the Pleiades using kinematics with typical
uncertainties of $5-7$ Myr. For all five clusters, this kinematic age is
younger than the age estimated with isochrones but within the uncertainties of
the isochrone fitting. We find for the clusters that travel far from the
Galactic plane (the Pleiades, NGC 2451A and IC 2602), the formation of the
cluster coincides with when the cluster was in the Galactic plane within a few
Myr, supporting these age determinations.
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