Volume 574, February 2015
|Number of page(s)||24|
|Section||Interstellar and circumstellar matter|
|Published online||28 January 2015|
To compare our observations with the emission expected from an isothermal slab model with a given Tex and N(CO), we minimize the sum over all detections within one ro-vibrational transition following in the parameter space between
100 K ≤Tex ≤ 2500 K and 1016 cm-2≤N(CO) ≤ 1020 cm-2 for 12CO emission (Fig. A.1), and 100 K ≤Tex ≤ 1200 K and 1017 cm-2≤N(CO) ≤ 1021 cm-2 for 13CO emission (Fig. A.2), in steps of ΔTex = 25 K and Δ10log(N(CO)) = 0.1. We define our fitting error as to all solutions within a 1 σ confidence interval of the best fit value. The best fit values are listed in Table 3.
Best fit contours for associated 12CO Boltzmann plots. Color contours denote deviations of 1σ (green), 2σ (yellow), 3σ (orange) and >3σ (red) confidence intervals.
|Open with DEXTER|
Best fit contours for associated 13CO Boltzmann plots. Color contours denote deviations of 1σ (green), 2σ (yellow), 3σ (orange) and >3σ (red) confidence intervals.
|Open with DEXTER|
We list the fluxes and upper limits of the CO v = 2−0 R03 lines in Table B.2 and those of the Pfund β hydrogen recombination line in Table B.3. We were unable to identify this line in the spectrum of HD 101412 due to the many strong and overlapping ro-vibrational CO lines in the line region (c.g. Fig. 1).
We flux-calibrate the CO overtone spectra using the Ks magnitudes at 2.17 μm as published in the 2MASS catalog (Skrutskie et al. 2006), and the Pfund β and CO fundamental spectra with the 4.77 μm flux, as determined with a spline interpolation to the M band data points, from (e.g. Kilkenny et al. 1985; Hillenbrand et al. 1992; de Winter et al. 2001).
Line fluxes and upper limits of the CO v = 2−0 R03 line at 2337.4128 nm.
Pfund β line fluxes and FWHM values for the programme stars.
Line flux and error values used in this manuscript.
© ESO, 2015
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