Table 7
Variation of the Ca II average absorption depth and average flux around Ca II K and H circumstellar lines.
| Periods | Average absorption depth | Average flux (arb. unit) | |||||
|---|---|---|---|---|---|---|---|
| CS-line | D-family | S-family | Tip of CS-line | Blue wing | |||
| K only | H only | K and H co-added | K only | H only | K only | ||
| ±5 km s−1 | ±5 km s−1 | 5–25 km s−1 | 50–100 km s−1 | 0 ± 2 km s−1 | 0 ± 2 km s−1 | –150 ± 5 km s−1 | |
| 2003–2004 | 0.704 ± 0.014 | 0.61597 ± 0.010 | 0.276 ± 0.028 | 0.0495 ± 0.0045 | 0.01118 ± 0.00063 | 0.01843 ± 0.00062 | 0.3881 ± 0.0010 |
| 2004–2007 | 0.753 ± 0.029 | 0.68788 ± 0.027 | 0.152 ± 0.024 | 0.0580 ± 0.0088 | 0.0105 ± 0.0016 | 0.0162 ± 0.0024 | 0.3864 ± 0.0024 |
| 2007–2008 | 0.701 ± 0.013 | 0.61683 ± 0.013 | 0.283 ± 0.064 | 0.134 ± 0.027 | 0.01146 ± 0.00074 | 0.01679 ± 0.00080 | 0.3768 ± 0.0038 |
| 2008–2009 | 0.828 ± 0.020 | 0.75697 ± 0.026 | 0.336 ± 0.040 | 0.061 ± 0.011 | 0.00437 ± 0.00059 | 0.00801 ± 0.00091 | 0.3810 ± 0.0017 |
| 2009–2010a | 0.72174 | 0.64518 | 0.135 | 0.081 | 0.0079 | 0.0204 | 0.3869 |
| 2010–2011 | 0.610 ± 0.036 | 0.54054 ± 0.037 | 0.114 ± 0.022 | 0.0265 ± 0.0069 | 0.0124 ± 0.0022 | 0.0198 ± 0.0029 | 0.39563 ± 0.00057 |
| 2013–2014 | 0.531 ± 0.012 | 0.48492 ± 0.012 | 0.234 ± 0.020 | 0.104 ± 0.014 | 0.02185 ± 0.00060 | 0.02788 ± 0.00065 | 0.3820 ± 0.0024 |
| 2014–2015 | 0.634 ± 0.016 | 0.52135 ± 0.015 | 0.242 ± 0.045 | 0.0170 ± 0.0041 | 0.01436 ± 0.00060 | 0.0233 ± 0.0011 | 0.3949 ± 0.0014 |
| 2015–2016 | 0.46 ± 0.11 | 0.34875 ± 0.12 | 0.099 ± 0.035 | 0.0294 ± 0.0048 | 0.0241 ± 0.0060 | 0.049 ± 0.012 | 0.3950 ± 0.0021 |
| 2016–2017 | 0.602 ± 0.034 | 0.4145 ± 0.026 | 0.200 ± 0.024 | 0.0450 ± 0.0054 | 0.0182 ± 0.0012 | 0.04530 ± 0.00092 | 0.3858 ± 0.0013 |
Notes. Average absorption depths are calculated from the normalized spectra, either separating K and H spectra, either co-adding the K and H absorption lines. Average fluxes are calculated from the raw spectra. Their continuum is scaled to an arbitrary level that is common to all spectra. (a) With only one night observed it is not possible to evaluate uncertainties.
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