6,383 research outputs found
Library of medium-resolution fiber optic echelle spectra of F, G, K, and M field dwarfs to giants stars
We present a library of Penn State Fiber Optic Echelle (FOE) observations of
a sample of field stars with spectral types F to M and luminosity classes V to
I. The spectral coverage is from 3800 AA to 10000 AA with nominal a resolving
power 12000. These spectra include many of the spectral lines most widely used
as optical and near-infrared indicators of chromospheric activity such as the
Balmer lines (H_alpha, H_beta), Ca II H & K, Mg I b triplet, Na I D_{1} and
D_{2}, He I D_{3}, and Ca II IRT lines. There are also a large number of
photospheric lines, which can also be affected by chromospheric activity, and
temperature sensitive photospheric features such as TiO bands. The spectra have
been compiled with the goal of providing a set of standards observed at medium
resolution. We have extensively used such data for the study of active
chromosphere stars by applying a spectral subtraction technique. However, the
data set presented here can also be utilized in a wide variety of ways ranging
from radial velocity templates to study of variable stars and stellar
population synthesis. This library can also be used for spectral classification
purposes and determination of atmospheric parameters (T_eff, log{g}, [Fe/H]). A
digital version of all the fully reduced spectra is available via ftp and the
World Wide Web (WWW) in FITS format.Comment: Latex file with 17 pages, 4 figures. Full postscript (text and
figures) available at http://www.ucm.es/info/Astrof/fgkmsl/FOEfgkmsl.html To
be published in ApJ
Library of high-resolution UES echelle spectra of F, G, K and M field dwarf stars
We present a library of Utrecht echelle spectrograph (UES) observations of a
sample of F, G, K and M field dwarf stars covering the spectral range from 4800
AA to 10600 AA with a resolution of 55000. These spectra include some of the
spectral lines most widely used as optical and near-infrared indicators of
chromospheric activity such as H_beta, Mg I b triplet, Na I D_1, D_2, He I D_3,
H_alpha, and Ca II IRT lines, as well as a large number of photospheric lines
which can also be affected by chromospheric activity. The spectra have been
compiled with the aim of providing a set of standards observed at
high-resolution to be used in the application of the spectral subtraction
technique to obtain the active-chromosphere contribution to these lines in
chromospherically active single and binary stars. This library can also be used
for spectral classification purposes. A digital version with all the spectra is
available via ftp and the World Wide Web (WWW) in both ASCII and FITS formats.Comment: Latex file with 5 figures using l-aa.sty and psfig.sty. Full
postscript (text and figures) available at
http://www.ucm.es/OTROS/Astrof/fgkmsl/UESfgkmsl.html Accepted for publication
in: Astronomy and Astrophysics Supplement
Argentina's default and the lack of dire consequences
We analyze the 2001 Argentine default on its foreign debt and its consequences in terms of the existing literature on sovereign debt default. It is our purpose to evaluate this experience and to see to what extent the Argentine case requires a re-thinking on the nature and consequences of defaults. We show that the Argentine case contradicts many of their standard predictions, in particular its posterior lack of access to international credit, restriction to international trade and negative economic growth. Moreover, it corroborates the historical fact that many defaulters “get away with it.
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