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J/A+A/445/673       X-ray spectrum of SV Cam               (Sanz-Forcada+, 2006)

A compact flare eclipsed in the corona of SV Camelopardalis. Sanz-Forcada J., Favata F., Micela G. <Astron. Astrophys. 445, 673 (2006)> =2006A&A...445..673S
ADC_Keywords: Stars, variable ; Spectroscopy ; X-ray sources Keywords: stars: coronae - stars: abundances - stars: individual: SV Cam - stars: late-type - X-rays: stars - binaries: eclipsing Abstract: The eclipsing active binary SV Cam (G0V/K6V, Porb=0.593071d) was observed with XMM-Newton during two campaigns in 2001 and 2003. Description: This table includes the observed fluxes of the lines identified in the X-ray spectrum (XMM/RGS) of SV Cam. The table 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) ------------------------------------------- 06 41 19.07 +82 16 02 SV Cam = HD 44982 ------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table4.dat 116 53 XMM/RGS line fluxes of SV Cam (October 2003)
See also: J/A+A/406/193 : SV Cam BVR light curves in Feb/2001-Mar/2002 (Zboril, 2003) J/A+A/376/158 : SV Cam BVR light curves (Albayrak+, 2001) Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 8 A8 --- Ion Ion 10- 16 F7.4 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 EMD) 22- 29 E8.3 mW/m2 Fobs Observed line flux measured in XMM/RGS SV Cam spectra 31- 34 F4.1 --- S/N Signal-to-noise ratio 36- 40 F5.2 --- log(Fobs/Fpred) ?=- Observed to predicted flux ratio (1) 42-116 A75 --- Blends Blends to the main line amounting more than a 5% of the total flux (2)
Note (1): Predicted flux includes correction by interstellar medium absorption. Note (2): For a line not identified in APED, a tentative identification is suggested in this column based on Kelly (, 1897, Atomic and ionic spectrum lines below 2000 Angstroms. Hydrogen through Krypton, New York: American Institute of Physics (AIP), American Chemical Society and the National Bureau of Standards).
Acknowledgements: Jorge Sanz-Forcada, jsanz(at)
(End) Jorge Sanz-Forcada [RSSD, ESA], Patricia Vannier [CDS] 05-Nov-2005
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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