Universität zu Köln

Dinnbier, Frantisek ORCID: 0000-0001-5532-4211 and Kroupa, Pavel ORCID: 0000-0002-7301-3377 (2020). Tidal tails of open star clusters as probes to early gas expulsion: II. Predictions for Gaia. Astron. Astrophys., 640. LES ULIS CEDEX A: EDP SCIENCES S A. ISSN 1432-0746

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Abstract

Aims. We study the formation and evolution of the tidal tail released from a young star Pleiades-like cluster, due to expulsion of primordial gas in a realistic gravitational field of the Galaxy. The tidal tails (as well as clusters) are integrated from their embedded phase for 300 Myr. We vary star formation efficiencies (SFEs) from 33% to 100% and the timescales of gas expulsion as free parameters, and provide predictions for the morphology and kinematics of the evolved tail for each of the models. The resulting tail properties are intended for comparison with anticipated Gaia observations in order to constrain the poorly understood early conditions during the gas phase and gas expulsion.Methods. The simulations are performed with the code NBODY6 including a realistic external gravitational potential of the Galaxy, and an analytical approximation for the natal gaseous potential.Results. Assuming that the Pleiades formed with rapid gas expulsion and an SFE of approximate to 30%, the current Pleiades are surrounded by a rich tail extending from approximate to 150 to approximate to 350 pc from the cluster and containing 0.7x to 2.7x the number of stars in the present-day cluster. If the Pleiades formed with an SFE close to 100%, then the tail is shorter (less than or similar to 90 pc) and substantially poorer with only approximate to 0.02x the number of present-day cluster stars. If the Pleiades formed with an SFE of approximate to 30%, but the gas expulsion was adiabatic, the tail signatures are indistinguishable from the case of the model with 100% SFE. The mass function of the tail stars is close to that of the canonical mass function for the clusters including primordial gas, but it is slightly depleted of stars more massive than approximate to 1 M-circle dot for the cluster with 100% SFE, a difference that is not likely to be observed. The model takes into account the estimated contamination due to the field stars and the Hyades-Pleiades stream, which constitutes a more limiting factor than the accuracy of the Gaia measurements.

Item Type:	Journal Article
Creators:	Creators Email ORCID ORCID Put Code Dinnbier, Frantisek UNSPECIFIED orcid.org/0000-0001-5532-4211 UNSPECIFIED Kroupa, Pavel UNSPECIFIED orcid.org/0000-0002-7301-3377 UNSPECIFIED
URN:	urn:nbn:de:hbz:38-323100
DOI:	10.1051/0004-6361/201936572
Journal or Publication Title:	Astron. Astrophys.
Volume:	640
Date:	2020
Publisher:	EDP SCIENCES S A
Place of Publication:	LES ULIS CEDEX A
ISSN:	1432-0746
Language:	English
Faculty:	Unspecified
Divisions:	Unspecified
Subjects:	no entry
Uncontrolled Keywords:	Keywords Language BROWN DWARF CANDIDATES; ORION-NEBULA CLUSTER; DYNAMICAL EVOLUTION; IONIZING FEEDBACK; MASSIVE CLUSTERS; NEARBY STARS; PLEIADES; HIPPARCOS; ORIGIN; PHASE Multiple languages Astronomy & Astrophysics Multiple languages
URI:	http://kups.ub.uni-koeln.de/id/eprint/32310