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J/A+A/469/309    Chromospheric activity in late-type stars   (Cincunegui+, 2007)

Hα and the CaII H and K lines as activity proxies for late-type stars. Cincunegui C., Diaz R.F., Mauas P.J.D. <Astron. Astrophys., 469, 309-317 (2007)> =2007A&A...469..309C
ADC_Keywords: Stars, late-type ; Spectroscopy Keywords: stars: late-type - stars: activity - stars: chromospheres Abstract: The main chromospheric activity indicator is the S index, which is the ratio of the flux in the core of the CaII H and K lines to the continuum nearby, and is well studied for stars from F to K. Another chromospheric proxy is the Halpha line, which is believed to be tightly correlated with the CaII index. In this work we characterize both chromospheric activity indicators, the one associated with the H and K CaII lines and the other with Halpha, for the whole range of late type stars, from F to M. Description: We present periodic medium-resolution echelle observations covering the complete visual range, taken at the CASLEO Argentinean Observatory over 7 years. We use a total of 917 flux-calibrated spectra for 109 stars that range from F6 to M5. We statistically study these two indicators for stars of different activity levels and spectral types. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 127 109 Stars included in the sample
See also: J/A+A/331/581 : Rotation and activity in field M dwarfs (Delfosse+ 1998) J/A+AS/124/359 : CaII triplet lines in cool stars (Mallik 1997) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Name HD or GJ name 11- 16 A6 --- GJ GJ or Gliese designation 18- 32 A15 --- OName Other name 33- 36 A4 --- Note Notes (1) 38- 45 A8 --- SpType MK spectral type 47- 52 F6.3 mag Vmag V magnitude 54- 58 F5.3 mag B-V B-V colour index 60 A1 --- n_B-V [a] a: photometry from Simbad, else from HIP (Cat. I/239) 62- 67 F6.2 mas plx ?=- Parallax 69 A1 --- n_plx [b] b: parallax from Simbad, else from Jenkins (1952, UCTP, Cat. I/81) 70- 74 F5.2 --- logg ?=- Gravity surface 76 A1 --- l_[Fe/H] Limit flag on [Fe/H] 77- 81 F5.2 [Sun] [Fe/H] ?=- Metallicity 83 A1 --- n_[Fe/H] [c] c: logg and [Fe/H] from Cayrel de Strobel et al. (2001, Cat. III/221), else from Cayrel de Strobel et al. (1997, Cat. III/200) 85 A1 --- l_Prot Limit flag on Prot 86- 90 F5.2 d Prot ?=- Rotational period 92 A1 --- r_Prot [edfghiZz] Reference for Prot (2) 94- 95 I2 --- Nobs Number of observations 97-100 F4.2 --- <S> Mean activity index (in Mount Wilson units) 102-107 F6.2 hW/m2/nm <FHK> Average surface flux in CaII HK line (4) 109 A1 --- --- [(] FHa excluded from our analysis (3) 110-114 F5.2 kW/m2/nm <FHa> Average flux in Halpha line (4) 115 A1 --- --- [)] FHa excluded from our analysis (3) 117-121 F5.2 --- m ?=- Slope of the linear regression between F(Halpha) and F(HK) for the individual spectra of each star 123-127 F5.2 --- rho ?=- Correlation coefficient corresponding to m
Note (1): Notes as follows: * = stars with planets + = RS CVn type ++ = BY Dra type S = stars reported in CTIO as non-variable, which were used to calibrate the S indices t = dMe stars, or stars presumably active Note (2): Prot references as follows: e = Baliunas et al. (1996ApJ...457L..99B), d = Saar & Osten (1997MNRAS.284..803S), f = Noyes et al. (1984ApJ...279..763N), g = Saar et al. (1990A&A...235..291S), h = Hooten & Hall (1990ApJS...74..225H) i = Pettersen (1989AetA...209..279P). Z = periods estimated from vsini using Glebocki & Stawikowski (2000AcA....50..509G) z = periods estimated from vsini using Reiners & Schmitt (2003A&A...398..647R). Note (3): The Halpha fluxes between parentheses were excluded from our analysis in Section 4.1, since they might be subject to larger errors due to the use of B-V as a proxy for Teff for stars with B-V≤1.4. Note (4): CaII flux in 104erg/cm2/s/Å, and Hα flux in 105erg/cm2/s/Å.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 26-Oct-2007
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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