All Tables

Table 1: The IRAS number, the HD number or the name from the GCVS, the spectral type, the equatorial coordinates $\alpha$ and $\delta$ (J2000), the effective temperature $T_{{\rm eff}}$ , the surface gravity $\log g$ , the metallicity [ Fe/ H], the reference for the model parameters, the type of object (post-AGB, RV Tauri or New Sample) and a reference where the orbital motion of the object can be found, are given. Note that IRAS 11472-0800 is a strongly depleted object added to our sample stars.
Table 2: New observational data at $850~\mu$ m from SCUBA.
Table A.1: First the estimated total colour excess E(B-V) is given. Then the five parameters of the dust model are shown: the normalization temperature T₀, the inner radius of the dust shell $r_{{\rm in}}$ , the outer radius of the dust shell $r_{{\rm out}}$ , the spectral index p and the density parameter m. The last column lists the energy ratio $L_{{\rm IR}}/L_\ast$ .
Table A.2: For those stars for which we have a parallax obtained by Hipparcos, we derive the distance D (pc) and the luminosity L( $10^3~L_{\odot}$ ) based on that parallax. In the second part of the table, distance and luminosity estimates are given based on the P-L relation of Alcock et al. (1998). Periods P (days) are from SIMBAD and bolometric corrections ${\it BC}_V$ from Bessell et al. (1998). The luminosity L (in $10^3~L_{\odot}$ ) and the distance D (in kpc) are given together with the estimated errors. Where we don't have a pulsation period, distances are estimated based on a luminosity of $L = 5000\pm2000~L_\odot$ .
Table B.1: The orbital period is given. Note that we included further refinements of our own based on longer time series. The original reference is given.
Table C.1: Geneva data were acquired with the 70 cm Swiss Telescope at La Silla (Chile) and with the Flemish Mercator Telescope at La Palma (Spain), using the refurbished Geneva photometer P7 (Raskin et al. 2004). Our total dataset was scanned for the maximum and minimum magnitudes. Observation dates, number of measurements and total timebases of these maxima and minima are given as well. Additional data were found in the Geneva database: the General Catalogue of Photometric Data (GCPD, http://obswww.unige.ch/gcpd/gcpd.html).
Table C.2: Ground-based optical ( ${\it UBVRI}$ ) data, acquired over a long period, found in the literature. If possible the maximum and minimum magnitudes of a dataset are taken into account.
Table C.3: Ground-based near-infrared ( ${\it JHKLM}$ ) photometry found in the literature. If there was more than one measurement we used both the maximum and minimum datapoints. For the data from 2 MASS and DENIS we made use of the catalogues found in VIZIER (http://vizier.u-strasbg.fr/viz-bin/VizieR).
Table C.4: IRAS photometry points at 12, 25, 60 and $100~\mu$ m. Note however that in some cases the data points are upper limits (L); these observations are probably contaminated by interstellar cirrus clouds. Other data are lower limits (:). Remark also that for BD+39 $^{\circ }$ 4926 we don't have IRAS datapoints.
Table C.5: Data of the Midcourse Space eXperiment (MSX). The instrument on board MSX is the SPIRIT III (Spatial Infrared Imaging Telescope III). The approximate effective wavelengths of the 6 MSX filters are in $\mu$ m.
Table C.6: $850~\mu$ m fluxes from observations with the Submillimetre Common-User Bolometer Array (SCUBA) at the James Clerk Maxwell Telescope (JCMT), Mauna Kea, Hawaii.