296 research outputs found
Extragalactic Globular Cluster Systems
Das Ziel dieser Dissertation ist die spektroskopische Studie von extragalaktischen Kugelsternhaufensystemen. Ihre Motivation ist das bessere Verstaendnis der Bildung und Entwicklung dieser Kugelsternhaufensysteme und ihrer Wirtsgalaxien. Zu diesem Zweck werden spektroskopische Linienindices des integrierten Lichts einzelner extragalaktischer Kugelsternhaufen gemessen, aus denen das Alter, die Metallizitaet und das Haeufigkeitsverhaeltnis von alpha-Elementen zu Eisen (im folgenden [alpha/Fe]) abgeleitet werden kann. Dies erlaubt detaillierte Rueckschluesse auf ihre Entstehungsepochen und -mechanismen
Extragalactic Globular Cluster Systems
Das Ziel dieser Dissertation ist die spektroskopische Studie von extragalaktischen Kugelsternhaufensystemen. Ihre Motivation ist das bessere Verstaendnis der Bildung und Entwicklung dieser Kugelsternhaufensysteme und ihrer Wirtsgalaxien. Zu diesem Zweck werden spektroskopische Linienindices des integrierten Lichts einzelner extragalaktischer Kugelsternhaufen gemessen, aus denen das Alter, die Metallizitaet und das Haeufigkeitsverhaeltnis von alpha-Elementen zu Eisen (im folgenden [alpha/Fe]) abgeleitet werden kann. Dies erlaubt detaillierte Rueckschluesse auf ihre Entstehungsepochen und -mechanismen
Old Metal-rich Globular Cluster Populations: Peak Color and Peak Metallicity Trends with Mass of Host Spheroids
We address the problem of the factors contributing to a peak color trend of
old metal-rich globular cluster (MRGC) populations with mass of their hosts,
early-type galaxies and spheroidal subsystems of spiral ones (spheroids). The
color-mass trend is often converted to a metallicity-mass trend under the
assumption that age effects are small or negligible. While direct estimates of
the ages of MRGC populations neither can rule out nor reliably support the
populations' age trend, key data on timing of the formation of spheroids and
other indirect evidence imply it in the sense: the more massive spheroid the
older on average its MRGC population. We show that the contribution of an
allowable age trend of the MRGC populations to their peak color trend can
achieve up to ~50 % or so. In this event the comparable value of the color
trend, ~30 %, is due to alpha-element ratio systematic variations of the order
of Delta[alpha/Fe] ~ 0.1 to 0.2 dex because of a correlation between the
[alpha/Fe] ratios and age. Hence a systematic variation of exactly [Fe/H]
ratios may turn out to be less significant among the contributors, and its
range many times lower, i.e. of the order of Delta[Fe/H] ~ 0.1 or even none,
than the corresponding range deduced by assuming no age trend.Comment: 5 pages, 1 figure, accepted for publication in Astronomische
Nachrichte
On Collision Course: The Nature of the Binary Star Cluster NGC 2006 / SL 538
The LMC hosts a rich variety of star clusters seen in close projected
proximity. Ages have been derived for few of them showing differences up to few
million years, hinting at being binary star clusters. However, final
confirmation needs to be done through spectroscopic analysis. Here we focus on
the LMC cluster pair NGC2006-SL538 and aim to determine whether the star
cluster pair is a bound entity (binary star cluster) or a chance alignment.
Using the MIKE echelle spectrograph at LCO we have acquired integrated-light
spectra for each cluster. We have measured radial velocities by two methods: a)
direct line profile measurement yields v km/s for NGC2006 and
km/s for SL538. b) By comparing observed spectra with
synthetic bootstrapped spectra yielding km/s for NGC2006 and
km/s for SL538. Finally when spectra are directly compared,
we find a km/s. Full-spectrum SED fits reveal that the
stellar population ages lie in the range 13-21 Myr with a metallicity of
Z=0.008. We find indications for differences in the chemical abundance patterns
as revealed by the helium absorption lines between the two clusters. The
dynamical analysis shows that the two clusters are likely to merge within the
next 150 Myr. The NGC2006-SL538 cluster pair shows radial velocities,
stellar population and dynamical parameters consistent with a gravitational
bound entity. We conclude that this is a genuine binary cluster pair, and we
propose that their differences in ages and stellar population chemistry is most
likely due to variances in their chemical enrichment history within their
environment. We suggest that their formation may have taken place in a loosely
bound star-formation complex which saw initial fragmentation but then had its
clusters become a gravitationally bound pair by tidal capture.Comment: Accepted for publication in Astronomy & Astrophysics. 15 pages, 10
figures in low resolutio
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