207 research outputs found
Ages and metallicities of faint red galaxies in the Shapley Supercluster
We present results on the stellar populations of 232 quiescent galaxies in
the Shapley Supercluster, based on spectroscopy from the AAOmega spectrograph
at the AAT. The key characteristic of this survey is its coverage of many
low-luminosity objects (sigma ~ 50 km/s), with high signal-to-noise (~45 per
Angstrom). Balmer-line age estimates are recovered with ~25% precision even for
the faintest sample members. We summarize the observations and absorption line
data, and present correlations of derived ages and metallicities with mass and
luminosity. We highlight the strong correlation between age and alpha-element
abundance ratio, and the anti-correlation of age and metallicity at fixed mass,
which is shown to extend into the low-luminosity regime.Comment: Four pages, three figures; To appear in Proceedings of IAU Symp. 245
"Formation and Evolution of Galaxy Bulges", (Oxford, July 16-20 2007), Eds.
Martin Bureau, Lia Athanassoula, and Beatriz Barbu
ELEVATED Α-FETOPROTEIN IN ASSOCIATION WITH LOSS OF SERUM HBeAg
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/73663/1/j.1572-0241.1993.tb07621.x.pd
Severe Cholestasis Associated with Methyltestosterone: A Case Report
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/75504/1/j.1572-0241.1987.tb01706.x.pd
Hepatitis B infection and liver transplantation: The art of the possible
No Abstract.Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/38405/1/1840190134_ftp.pd
Are Recent Peculiar Velocity Surveys Consistent?
We compare the bulk flow of the SMAC sample to the predictions of popular
cosmological models and to other recent large-scale peculiar velocity surveys.
Both analyses account for aliasing of small-scale power due to the sparse and
non-uniform sampling of the surveys. We conclude that the SMAC bulk flow is in
marginal conflict with flat COBE-normalized Lambda-CDM models which fit the
cluster abundance constraint. However, power spectra which are steeper
shortward of the peak are consistent with all of the above constraints. When
recent large-scale peculiar velocity surveys are compared, we conclude that all
measured bulk flows (with the possible exception of that of Lauer & Postman)
are consistent with each other given the errors, provided the latter allow for
`cosmic covariance'. A rough estimate of the mean bulk flow of all surveys
(except Lauer & Postman) is ~400 km/s towards l=270, b=0.Comment: 8 pages, 3 figures. To appear in Proceedings of the Cosmic Flows
Workshop, Victoria, B. C., Canada, July 1999, eds. S. Courteau, M. Strauss,
and J. Willic
Near-Infrared Imaging of Early-Type Galaxies IV. The Physical Origins of the Fundamental Plane Scaling Relations
The physical origins of the Fundamental Plane (FP) scaling relations are
investigated for early-type galaxies observed at optical and near-infrared
wavelengths. The slope for the FP is shown to increase systematically with
wavelength from the U-band through the K-band. A distance-independent
construction of the observables is described which provides an accurate
measurement of the change in the FP slope between any pair of bandpasses. The
variation of the FP slope with wavelength is strong evidence of systematic
variations in stellar content along the elliptical galaxy sequence. The
intercept of the diagnostic relationship between log(D_K/D_V) and log(sigma_0)
shows no significant dependence on environment within the uncertainties of the
Galactic extinction corrections, demonstrating the universality of the stellar
populations contributions at the level of Delta(V-K)=0.03 mag to the zero-point
of the global scaling relations.
Several other constraints on the properties of early-type galaxies --- the
slope of the Mg_2-sigma_0 relation, the effects of stellar populations
gradients, and deviations of early-type galaxies from a dynamically homologous
family --- are included to construct an empirical, self-consistent model which
provides a complete picture of the underlying physical properties which are
varying along the early-type galaxy sequence. This empirical approach
demonstrates that there are significant systematic variations in both age and
metallicity along the elliptical galaxy sequence, and that a small, but
systematic, breaking of dynamical homology (or a similar, wavelength
independent effect) is required. Predictions for the evolution of the slope of
the FP with redshift are described. [abriged]Comment: to appear in The Astronomical Journal; 40 pages, including 10
Postscript figures and 3 tables; uses AAS LaTeX style file
Beyond Sérsic + exponential disc morphologies in the Coma Cluster
Galaxies are not limited to simple spheroid or bulge + disc morphologies. We explore the diversity of internal galaxy structures in the Coma Cluster across a wide range of luminosities (−17 > Mg > −22) and cluster-centric radii (0 10 kpc). 11 per cent of galaxies (N = 52) feature a break in their outer profiles, indicating ‘truncated’ or ‘antitruncated’ discs. Beyond the break radius, truncated galaxies are structurally consistent with exponential discs, disfavouring physical truncation as their formation mechanism. Bulge luminosity in antitruncated galaxies correlates strongly with galaxy luminosity, indicating a bulge-enhancing origin for these systems. Both types of broken disc are found overwhelmingly (>70 per cent) in ‘barred’ galaxies, despite a low measured bar fraction for Coma (20 ± 2 per cent). Thus, galaxy bars play an important role in formation of broken disc structures. No strong variation in galaxy structure is detected with projected cluster-centric radius
The Near-Infrared Fundamental Plane of Elliptical Galaxies
We present results from a near-infrared -band imaging survey of 59
elliptical galaxies in five nearby clusters. We measure photometric parameters
for each galaxy using surface photometry and draw velocity dispersions from the
literature. Three observables define a near-infrared Fundamental Plane (FP) of
elliptical galaxies with . The scatter in the near-infrared relation is small at
\% in distance, which is equivalent to, or less than, the scatter of the
optical FP. We suggest that the small deviation of the near-infrared FP
relation from the optical FP is due to the reduction of metallicity effects in
the near-infrared bandpass. While the small scatter of the optical FP could be
consistent with compensating effects of age and metallicity, the similarly
small scatter of the near-infrared FP is nearly independent of metallicity and
hence places a strong constraint on possible age spreads among elliptical
galaxies at every point along the FP. We suggest that the departure of the
near-infrared FP from the pure virial form , and the corresponding observed relation , may be explained by slight systematic departures of
the structure and dynamics of elliptical galaxies from a homology.Comment: to appear in The Astrophysical Journal (Letters); 12 pages, including
2 Postscript figures and 1 table; uuencoded, compressed format; the paper is
also available in various formats from
http://astro.caltech.edu/~map/map.bibliography.refereed.htm
CAGE
Peer Reviewedhttp://deepblue.lib.umich.edu/bitstream/2027.42/28986/1/0000013.pd
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