J/A+A/416/281 X-ray spectra of 4 cool stars (Sanz-forcada+, 2004)
Coronal versus photospheric abundances of stars with different activity levels.
Sanz-forcada J., Favata F., Micela G.
<Astron. Astrophys., 416, 281-290 (2004)>
=2004A&A...416..281S 2004A&A...416..281S
ADC_Keywords: Stars, late-type ; X-ray sources ; Spectroscopy
Keywords: stars: coronae - stars: abundances - stars: late-type -
X-rays: stars - line: identification
Description:
These tables include the observed fluxes of the lines identified in
the X-ray spectra of four cool stars (Procyon, epsilon Eri, lambda And
and V851 Cen). The spectra were taken using different configurations
(Chandra/LETG, Chandra/HETG and XMM/RGS). The tables list the observed
fluxes at Earth, and a comparison with the fluxes predicted for a
given thermal coronal structure (the Emission Measure Distribution,
EMD), the emissivities provided by the Astrophysical Plasma Emission
Model (APED) and column density of absorbing material in the
interstellar medium towards the star. A list of the most important (at
least a 5% of the flux predicted for the line) blends that have been
considered for each line is included.
Objects:
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RA (2000) DE Designation(s) (File)
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03 32 55.8442 -09 27 29.744 epsilon Eri = HD 22049 (table5.dat)
07 39 18.1183 +05 13 29.975 Procyon = HD 61421 (table4.dat)
13 44 00.9239 -61 21 59.148 V851 Cen = HD 119285 (table7.dat)
23 37 33.8425 +46 27 29.347 lambda And = HD 222107 (table6.dat)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 98 146 Chandra/LETG line fluxes of Procyon (6/7-Nov-1999)
table5.dat 94 119 Chandra/LETG line fluxes of epsilon Eri (7-Nov-1999)
table6.dat 122 148 Chandra/HETG line fluxes of lambda And (21-Mar-2001)
table7.dat 135 51 XMM/RGS line fluxes of V851 Cen (7-Mar-2003)
tables.tex 178 628 LaTeX version of the tables
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Byte-by-byte Description of file: table?.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Ion Ion
9- 16 F8.4 0.1nm lambda Wavelength of the line as identified in the
model.
18- 20 F3.1 [K] logTmax ? Maximum temperature of formation of the line
(unweighted by the Emission Measure
Distribution)
22- 29 E8.3 mW/m2 Fobs Observed line flux
31- 34 F4.1 --- S/N Signal-to-noise ratio
36- 40 F5.2 --- Ratio ? log(observed flux/predicted flux) (1)
42-135 A94 --- Blends Blends to the main line amounting more than a
5% of the total flux (2)
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Note (1): The fluxes are in ergs units. Predicted flux includes
correction by interstellar medium absorption.
Note (2): For some lines not identified in Astrophysical Plasma
Emission Model, a tentative identification is suggested in this column
based on Kelly (1987, Atomic and ionic spectrum lines below 2000
Angstroms. Hydrogen through Krypton (New York: American Institute of
Physics, Amer. Chem. Soc. and the Nat. Bureau of Standards)).
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Acknowledgements:
Jorge Sanz-Forcada
(End) Patricia Bauer [CDS] 01-Mar-2004