The 1.87- and 2.07-μm observations of three Galactic Centre clusters with miniTAO at Atacama: classification of stellar components in massive star clusters

2018 ◽  
Vol 480 (2) ◽  
pp. 1507-1521
Author(s):  
Masuo Tanaka ◽  
Shin-ichiro Okumura ◽  
Hidenori Takahashi ◽  
Kentaro Osawa ◽  
Kentaro Motohara ◽  
...  
Keyword(s):  
Massive Star ◽  
Star Clusters ◽  
Galactic Centre

scholarly journals Proper-motion measurements in the Quintuplet cluster

2009 ◽  
Vol 5 (S266) ◽  
pp. 422-422
Author(s):  
Benjamin Hußmann ◽  
Andrea Stolte ◽  
Wolfgang Brandner
Keyword(s):  
Proper Motion ◽  
Massive Star ◽  
Star Clusters ◽  
Mass Function ◽  
Spatial Density ◽  
Galactic Centre ◽  
Data Sets ◽  
Centre Region ◽  
Low Mass ◽  
The Individual

AbstractThe three young, massive star clusters found in the Galactic Centre region (Young Nuclear Cluster, the Arches and Quintuplet clusters) are among the six most massive star clusters in our Galaxy, with masses similar to low-mass, extragalactic starburst clusters. The conditions for star formation in this region are extreme and likely comparable to those found in the Hii regions in starburst galaxies and tidal-interaction zones of mergers. As the inner Galactic star clusters can be resolved, they can serve as templates for extragalactic starburst clusters. With knowledge of the spectral types, masses and ages of the individual stars, their stellar population can be studied in detail, allowing derivation of their present-day mass function (PDMF). The Quintuplet cluster, with an age of about 4 Myr, is the most extended of the three clusters and also displays a lower spatial density. To determine its mass function correctly, the distinction between cluster and field stars is therefore of particular importance. We present the first determination of a proper-motion-membership sample for the Quintuplet cluster. By comparing two high-precision astrometric VLT/NACO data sets with a time baseline of 5 years, the displacement of the Quintuplet cluster relative to the field population was measured and a selection of the proper-motion cluster members could be established, from which the PDMF can be derived.

scholarly journals On the Origin of Hyperfast Neutron Stars

2007 ◽  
Vol 3 (S246) ◽  
pp. 365-366
Author(s):  
V.V. Gvaramadze ◽  
A. Gualandris ◽  
S. Portegies Zwart
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Massive Star ◽  
Galactic Disk ◽  
Star Clusters ◽  
Supernova Explosion ◽  
Star Cluster ◽  
Galactic Centre ◽  
The Core ◽  
Dense Cores

AbstractWe propose an explanation for the origin of hyperfast neutron stars (e.g. PSR B1508+55, PSR B2224+65, RX J0822–4300) based on the hypothesis that they could be the remnants of a symmetric supernova explosion of a high-velocity massive star (or its helium core) which attained its peculiar velocity (similar to that of the neutron star) in the course of a strong three- or four-body dynamical encounter in the core of a young massive star cluster. This hypothesis implies that the dense cores of star clusters (located either in the Galactic disk or near the Galactic centre) could also produce the so-called hypervelocity stars – ordinary stars moving with a speed of ~ 1 000 km s−1.

scholarly journals From young massive star clusters to old globulars: long-term survival chances

2006 ◽  
Vol 2 (S237) ◽  
pp. 408-408
Author(s):  
Richard de Grijs
Keyword(s):  
Galaxy Formation ◽  
Massive Star ◽  
Cluster Formation ◽  
Star Clusters ◽  
Term Survival ◽  
Star Forming ◽  
Distant Galaxies ◽  
Wide Range ◽  
Galaxy Collisions

Young, massive star clusters (YMCs) are the most notable and significant end products of violent star-forming episodes triggered by galaxy collisions and close encounters. The question remains, however, whether or not at least a fraction of the compact YMCs seen in abundance in extragalactic starbursts, are potentially the progenitors of (≳10 Gyr) old globular cluster (GC)-type objects. If we could settle this issue convincingly, one way or the other, the implications of such a result would have far-reaching implications for a wide range of astrophysical questions, including our understanding of the process of galaxy formation and assembly, and the process and conditions required for star (cluster) formation. Because of the lack of a statistically significant sample of YMCs in the Local Group, however, we need to resort to either statistical arguments or to the painstaking approach of case-by-case studies of individual objects in more distant galaxies.

scholarly journals Red Supergiants as Cosmic Abundance Probes: Massive Star Clusters in M83 and the Mass–Metallicity Relation of Nearby Galaxies

2017 ◽  
Vol 847 (2) ◽  
pp. 112 ◽  
Author(s):  
Ben Davies ◽  
Rolf-Peter Kudritzki ◽  
Carmela Lardo ◽  
Maria Bergemann ◽  
Emma Beasor ◽  
...  
Keyword(s):  
Massive Star ◽  
Star Clusters ◽  
Cosmic Abundance ◽  
Red Supergiants ◽  
Nearby Galaxies

scholarly journals Using young massive star clusters to understand star formation and feedback in high-redshift-like environments

2015 ◽  
Vol 75-76 ◽  
pp. 43-48
Author(s):  
S. Longmore ◽  
A. Barnes ◽  
C. Battersby ◽  
J. Bally ◽  
J.M. Diederik Kruijssen ◽  
...  
Keyword(s):  
Star Formation ◽  
Massive Star ◽  
High Redshift ◽  
Star Clusters

scholarly journals THE EVOLUTIONARY TRACKS OF YOUNG MASSIVE STAR CLUSTERS

2014 ◽  
Vol 794 (2) ◽  
pp. 147 ◽  
Author(s):  
S. Pfalzner ◽  
G. Parmentier ◽  
M. Steinhausen ◽  
K. Vincke ◽  
K. Menten
Keyword(s):  
Massive Star ◽  
Star Clusters

scholarly journals Stellar wind retention and expulsion in massive star clusters

2018 ◽  
Vol 478 (2) ◽  
pp. 2794-2811 ◽  
Author(s):  
J P Naiman ◽  
E Ramirez-Ruiz ◽  
D N C Lin
Keyword(s):  
Stellar Wind ◽  
Massive Star ◽  
Star Clusters

scholarly journals THE PREVALENCE AND IMPACT OF WOLF–RAYET STARS IN EMERGING MASSIVE STAR CLUSTERS

2016 ◽  
Vol 826 (2) ◽  
pp. 194 ◽  
Author(s):  
Kimberly R. Sokal ◽  
Kelsey E. Johnson ◽  
Rémy Indebetouw ◽  
Philip Massey
Keyword(s):  
Massive Star ◽  
Star Clusters

scholarly journals The search for multiple populations in Magellanic Clouds clusters – V. Correlation between cluster age and abundance spreads

2019 ◽  
Vol 487 (4) ◽  
pp. 5324-5334 ◽  
Author(s):  
S Martocchia ◽  
E Dalessandro ◽  
C Lardo ◽  
I Cabrera-Ziri ◽  
N Bastian ◽  
...  
Keyword(s):  
Significant Role ◽  
Massive Star ◽  
Milky Way ◽  
Star Clusters ◽  
Magellanic Clouds ◽  
Key Factors ◽  
Strong Function ◽  
Combining Data ◽  
Chemical Anomalies ◽  
Cluster Age

ABSTRACT In our HST photometric survey, we have been searching for multiple stellar populations (MPs) in Magellanic Clouds (MCs) massive star clusters which span a significant range of ages (∼1.5–11 Gyr). In the previous papers of the series, we have shown that the age of the cluster represents one of the key factors in shaping the origin of the chemical anomalies. Here, we present the analysis of four additional clusters in the MCs, namely Lindsay 38, Lindsay 113, NGC 2121, and NGC 2155, for which we recently obtained new UV HST observations. These clusters are more massive than ∼104 M⊙ and have ages between ∼2.5 and ∼6 Gyr, i.e. located in a previously unexplored region of the cluster age/mass diagram. We found chemical anomalies, in the form of N spreads, in three out of four clusters in the sample, namely in NGC 2121, NGC 2155, and Lindsay 113. By combining data from our survey and HST photometry for three additional clusters in the Milky Way (namely 47 Tuc, M15, and NGC 2419), we show that the extent of the MPs in the form of N spread is a strong function of age, with older clusters having larger N spreads with respect to the younger ones. Hence, we confirm that cluster age plays a significant role in the onset of MPs.

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