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J/MNRAS/403/2157    Main-sequence star chromospheres         (Houdebine+, 2010)

Observation and modelling of main-sequence star chromospheres. X. Radiative budgets on Gl 867A and AU Mic (dM1e), and a two-component model chromosphere for Gl 205 (dM1). Houdebine E.R. <Mon. Not. R. Astron. Soc., 403, 2157-2166 (2010)> =2010MNRAS.403.2157H
ADC_Keywords: Stars, late-type ; Magnetic fields ; Spectroscopy Keywords: stars: chromospheres - stars: late-type - stars: magnetic fields Abstract: We report on high-resolution observations of two dM1 stars: Gl 867A, an active dM1e star, and Gl 205, a less active dM1 star. The wavelength coverage is from 3890 to 6820Å with a resolving power of about 45000. The difference spectrum of these two stars allows us to make a survey of spectral lines sensitive to magnetic activity. Description: The observations presented here were acquired using the 1.93-m telescope at the Observatoire de Haute Provence, equipped with the ELODIE spectrograph. ELODIE is a cross-dispersed echelle spectrograph with an original optical design that yields evenly spaced orders. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 22 38 45.6 -20 37 16 Gl 867A = HD 214479 05 31 27.4 -03 40 38 Gl 205 = HD 36395 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1a.dat 26 32 Total results for each Flux sets table1.dat 63 602 List of the spectral lines sensitive to chromospheric activity
Byte-by-byte Description of file: table1a.dat
Bytes Format Units Label Explanations
1- 4 I4 0.1pm dEW ? Difference equivalent widths between Gl867A and Gl 205 6- 9 F4.2 hW/m2 Flux Continuum flux from Allard et al. (1997ARA&A..35..137A) (in 105erg/cm2/s) 10 A1 --- --- [@] 11- 14 I4 0.1nm lam.F Flux wavelength (Å) 15 A1 --- --- [A] 17- 23 F7.2 10W/m2 dFlux Difference radiative losses in the lines (1) 25- 26 I2 --- No ?=- Order number of the corresponding spectral order
Note (1): The total difference radiative losses in the line is 1020.73x10W/m2. (103erg/s/cm2 = 1W/m2)
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 F7.2 0.1nm lambda0 ?=- Vacuum wavelength 9- 15 F7.2 0.1nm lambda ?=- Gl 205 wavelength 17- 20 I4 0.1pm dEW Difference equivalent widths between Gl867A and Gl 205 22- 25 F4.2 hW/m2 Flux Continuum flux from Allard et al. (1997ARA&A..35..137A) (in 105erg/cm2/s) 26 A1 --- --- [@] 27- 30 I4 0.1nm lam.F Flux wavelength 31 A1 --- --- [A] 33- 38 F6.2 10W/m2 dFlux Difference radiative losses in the lines 40- 52 A13 --- Ident Line identification 54- 55 I2 --- No ?=- Order number of the corresponding spectral order 57- 63 A7 --- Rem Original catalog from which we identified each line
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 18-Oct-2010
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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