All Tables

Table 1: The name, the HD number, the equatorial coordinates $\alpha$ and $\delta$ (J2000), the Galactic coordinates l and b, the formal period P, the amplitude in the V-magnitude $\Delta V$ , the photometric classification, the effective temperature $T_{{\rm eff}}$ , the surface gravity $\log g$ and the metallicity [ Fe/ H] of the seven classical RV Tauri stars from our sample.
Table 2: Observations with SCUBA: $850~\mu$ m fluxes.
Table 3: The five parameters of the dust model: 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 4: The estimated total colour excess E(B-V) and the optical depth estimates in the V-band. $\tau _{V,E(B-V)}$ is determined from the SED minimalization and gives the total line-of-sight extinction. The contribution from the ISM is given in Col. 3 assuming the distance range given in Table 5. $\tau_{V,{\rm dust~model}}$ was determined by integrating the spherically symmetric dust model and in the last column the mean optical depth is given, determined by the energy ratio from the dust excess over the optical fluxes.
Table 5: The bolometric corrections BC_V (from Bessell et al. 1998), the luminosity L (in $10^3~L_{\odot}$ ), the distance D (in kpc) and the dust mass ( $10^{-5}~M_{\odot}$ ) are given, together with the estimated errors.
Table A.1: Geneva data were acquired with the Flemish Mercator Telescope at La Palma, Spain. 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. For AC Her, our observational monitoring data are divided in two major blocks of 8 and 446 days with 4612 days inbetween. Additional data were found in the Geneva database (http://obswww.unige.ch/gcpd/gcpd.html).
Table A.2: Ground-based optical data, acquired over a long period, found in the literature.
Table A.3: Ground-based near-IR photometry found in the literature. If there was more than one measurement we used both the maximum and minimum data points. 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 A.4: IRAS photometry points at 12, 25, 60 and $850~\mu$ m. Note however that in some cases the $100~\mu$ m is an upper limit (L); these observations are probably contaminated by interstellar cirrus clouds. For RV Tau the $100~\mu$ m data point is a lower limit (:).
Table A.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.