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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
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: --------------------------------------------------------------------- RA (2000) DE Designation(s) (File) --------------------------------------------------------------------- 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) --------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 135 146 Chandra/LETG line fluxes of Procyon (6/7-Nov-1999) table5.dat 135 119 Chandra/LETG line fluxes of epsilon Eri (7-Nov-1999) table6.dat 135 148 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
Byte-by-byte Description of file: table?.dat
Bytes Format Units Label Explanations
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)
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)).
Acknowledgements: Jorge Sanz-Forcada
(End) Patricia Bauer [CDS] 01-Mar-2004
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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