\begin{table}%t7
\par
\caption {\label{tab:inclinations}Rotation periods of stars with known inclinations.}
%\centerline
 {
\begin{tabular}{lcccccc}
\hline
\hline
\multicolumn{1}{c}{Object} &
\multicolumn{1}{c}{Inclination} &
\multicolumn{1}{c}{Adopted} &
\multicolumn{1}{c}{$v$~sin~$i$} &
\multicolumn{1}{c}{$v_{\rm eq}$} &
\multicolumn{1}{c}{$R$} &
\multicolumn{1}{c}{$P$} \\
\multicolumn{1}{c}{name} &
\multicolumn{1}{c}{Measurements} &
\multicolumn{1}{c}{Inclination} &
\multicolumn{1}{c}{[km s$^{-1}$]} &
\multicolumn{1}{c}{[km s$^{-1}$]} &
\multicolumn{1}{c}{[$R_{\odot}$]} &
\multicolumn{1}{c}{[d]} \\
 &
\multicolumn{1}{c}{[$^\circ{}$]} &
\multicolumn{1}{c}{[$^\circ{}$]} &
 &
 &
 &
 \\
\hline
%HD 53179          & 60                   & 60          & 100            & 115         & 14.4 & 6.3 \\
HD~95881         & 40$-$55$^1$          & 40$-$55     & 50$^q$         & 61$-$78     & 3.1$^{dd}$ & 2.0$-$2.6 \\
HD~97048         & 30$-$40$^a$          & 30$-$40     & 140$^r$        & 218$-$280   & 2.5$^{ee}$ & 0.5$-$0.6 \\
                  & 42.8$^b$             &             &                &             &     & \\
HD~100453        & $>$55$^2$            & $>$55       & 39$^s$         & $<$48       & 1.7$^{ff}$ & $>$1.8 \\
HD~100546        & 42$^c$               & $47\pm5$    & 65$^t$         & 82$-$97     & 1.7$^{ff}$ & 0.9$-$1.0 \\
                  & 51$^d$               &             &                &             &     & \\
HD~101412        & $>$55$^3$            & $>$55       & 5$^u$          & $<$6.1      & 2.1$^{gg}$ & $>$17.4 \\
HD~135344B       & 11$^e$               & 11          & 69$^v$         & 362         & 2.4$^{gg}$ & 0.3 \\
                  & 14$^f$               &             &                &             &     & \\
HD~139614        & $<$40$^g$            & $<$40       & 15$^{w}$        & $>$23       & 1.6$^{dd}$ & $<$3.5 \\
HD~144432        & 48~$\pm$~10$^e$        & 48~$\pm$~10   & 70$^{w}$        & 83$-$114    & 3.0$^{ff}$ & 1.3$-$1.8 \\
HD~144668        & 58$^h$               & 58          & 100$^{w}$       & 118         & 3.9$^{ee}$ & 1.7 \\
HD~150193        & $\sim$38$^i$         & 30$^5$      & 100$^t$        & 200         & 2.1$^{ee}$ & 0.5 \\
HD~152404        & 65$-$70$^j$          & 65$-$70     & $18.5\pm1$$^j$ & 18.5$-$21.5 & 2.6$^{dd}$ & 6.1$-$7.1 \\
HD~158643        & $\sim$90$^k$         & 90          & $267\pm5$$^v$  & 267~$\pm$~5   & 5.3$^{hh}$ & 1.0 \\
                  &                      &             & 228$^{x}$     & 228         &     & \\
HD~163296        & 51$^{+11,}_{-9}$$^l$ & 51          & 130$^{w}$     & 167         & 2.8$^{ee}$ & 0.8 \\
HD~169142        & 13~$\pm$~2$^e$         & $13\pm2$    & $66\pm2$$^v$   & 247$-$356   & 1.6$^{dd}$ & 0.2$-$0.3 \\
VV~Ser           & 72~$\pm$~5$^f$         & 72          & 142$^{y}$     & 149         & 2.4$^{ee}$ & 0.8 \\
                  &                      &             & 229$^{z}$     & 241         &     & \\
HD~179218        & $40\pm10$$^e$        & $40\pm10$   & 60$^{aa}$      & 78$-$120    & 4.8$^{gg}$ & 2.0$-$3.1\\
HD~190073        & $<$40$^4$            & $<$40       & 12$^{bb}$      & $>$18.7     & 3.3$^{ff}$ & $<$8.9 \\
\hline 
HD~9672          & 90$^m$               & 90          & 196$^{x}$     & 196         & 1.7$^{ii}$ & 0.4 \\
HD~39060         & 87$^n$               & 87          & 130$^k$        & 130         & 1.8$^{jj}$ & 0.7 \\
HD~109573        & 73$^o$               & 73          & 152$^{x}$     & 159         & 1.8$^{gg}$ & 0.6 \\
HD~181327        & 31.7$^p$             & 31.7        & 16$^{cc}$      & 30          & 1.2$^{gg}$ & 2.0 \\
%\hline 
%HD~31648         & 38$^q$               & 38          & 90$^{hh}$      & 146         & 2.5$^{ccc}$ & 0.9 \\
%                  & 36$\pm$1$^r$         &             &                &             &     & \\
%HD~104237        & 18$^s$               & 18          & 10$^v$         & 32          & 2.7$^{ccc}$ & 4.3 \\
\hline
\end{tabular}}
\par
\smallskip
\par
Notes:
Inclination angles derived for resolved disk detections from the literature and
from the study of \ion{Mg}{ii} spectral line profiles in UV spectra
or the study of H$\alpha$ line profiles in optical spectra and
the inclination values we finally adopt for further use are listed in Cols.~2 and 3.
$v$~sin~$i$ values and radii presented in Cols.~4
and 6, respectively, are for the most part gathered from the literature.
In Col.~7 we present the equatorial velocity values which are obtained from the inclination angles 
and the $v$~sin~$i$ values. $v_{\rm eq}$ and radii are used to estimate the rotation periods 
listed in the last column.
Radii marked as {\it this study} were calculated using \teff{} and bolometric luminosity, both taken from the literature.\\
References:
$^a$ Doering et~al.\ (\cite{Doering2007}),
$^b$ Doucet et~al.\ (\cite{Doucet2007}),
$^c$ Ardila et~al.\ (\cite{Ardila2007}),
$^d$ Augereau et~al.\ (\cite{Augereau2001}),
$^e$ Dent et~al.\ (\cite{Dent2005}),
$^f$ Pontoppidan et~al.\ (\cite{Pontoppidan2008}),
$^{g}$ Meeus et~al.\ \cite{Meeus1998},
$^h$ Preibisch et~al.\ (\cite{Preibisch2006}),
$^i$ Fukagawa et~al.\ (\cite{Fukagawa2003}),
$^j$ Alencar et~al.\ (\cite{Alencar2003}),
$^k$ Slettebak (\cite{Slettebak1982}),
$^l$ Wassell et~al.\ (\cite{Wassell2006}),
$^m$ Hughes et~al.\ (\cite{Hughes2008}),
$^n$ Heap et~al.\ (\cite{Heap2000}),
$^o$ Schneider et~al.\ (\cite{Schneider1999}),
$^p$ Schneider et~al.\ (\cite{Schneider2006}),
$^q$ Grady et~al.\ (\cite{Grady1996}),
$^r$ van den Ancker (\cite{vandenAncker1998}),
$^s$ Acke \& Waelkens (\cite{AckeWaelkens2004}),
$^t$ Hamidouche et~al.\ (\cite{Hamidouche2008}),
$^{u}$ this study (see Sect.~\ref{subsect:discussion_withfield}),
$^v$ Dunkin et~al.\ (\cite{Dunkin1997}),
$^{w}$ Hubrig et~al.\ (\cite{Hubrig2007b}),
$^{x}$ Royer et~al.\ (\cite{Royer2007}),
$^{y}$ Vieira et~al.\ (\cite{Vieira2003}),
$^{z}$ Mora et~al.\ (\cite{Mora2001}),
$^{aa}$ Bernacca \& Perinotto (\cite{BernaccaPerinotto1970}),
$^{bb}$ Pogodin et~al.\ (\cite{Pogodin2005}),
$^{cc}$ de la Reza \& Pinz\'on (\cite{delaRezaPinzon2004}),
$^{dd}$~Blondel \& Tjin (\cite{Blondel2006}),
$^{ee}$ Hillenbrand et~al.\ (\cite{Hillenbrand1992}),
$^{ff}$ Wade et~al.\ (\cite{Wade2007}), 
$^{gg}$ this study (see table caption),
$^{hh}$ Tatulli et~al.\ (\cite{Tatulli2008}), 
$^{ii}$ Hughes et~al.\ (\cite{Hughes2008}), and 
$^{jj}$ di Folco et~al.\ (\cite{diFolco2004}).\\ 
%$^q$Simon et~al.\ (\cite{Simon2000}),
%$^r$Pi\`etu et~al.\ (\cite{Pietu2006}),
%$^s$Grady et~al.\ (\cite{Grady2004}),
%$^z$Th\'e et~al.\ (\cite{The1985}),
%$^{hh}$Beskrovnaya et~al.\ (\cite{Beskrovnaya2004}),
%$^a$Meeus et~al.\ \cite{Meeus2002},
%$^x$this work,
%$^x$Guimar\~aes et~al.\ (\cite{Guimaraes2006}),
%Bernasconi \& Maeder (\cite{BernasconiMaeder1996}),
Comments on the inclination angles deduced in this study, mainly from IUE (LWR and LWP cameras) through analysis of line profile types.
Profile shapes are classified according to Beals (\cite{Beals1951}).
See also the discussion in Sect.~\ref{subsect:discussion_withfield}.
$^1$ \ion{Mg}{ii} alternates between P~Cygni type I (red emission, with blue-shifted absorption, IUE LWP 30~772)  and type III (double emission, IUE  LWP 13~082),
$^2$ the H$\alpha$ profile shown by Meeus et~al.\ (\cite{Meeus2002}) shows characteristic double-peaked H$\alpha$~emission,
$^3$ see the discussion in Sect.~\ref{subsect:discussion_withfield},
$^4$ \ion{Mg}{ii} has a type~I P~Cygni profile (IUE LWP 25~762, LWR 11~977, LWR 08~996),
$^5$ \ion{Mg}{ii} has a type~I  profile (IUE LWP 13~083).
%
%Comments on used IUE (LWR and LWP cameras) and HST spectra and deduced types of line profiles.
%Profile shapes are classified according to Beals (\cite{Beals1951}). Representative observations are indicated for each star. 
%$^1$\ion{Mg}{ii} alternates between P~Cygni type I (red emission, with blue-shifted absorption, IUE LWP 30772)  and type III (double emission, IUE  LWP 13082) type III,
%$^2$\ion{Mg}{ii} absorption (IUE LWR 11429, LWP 09517) with some filling in to the continuum (IUE LWP 21212, LWP 18869),
%$^3$\ion{Mg}{ii} is highly variable, ranging from type I P~Cygni (HST/STIS O5C902040), to inverse
%P~Cygni (IUE LWP 30172)  to type III (double emission, IUE LWP 30771), 
%$^4$\ion{Mg}{ii} has a type III profile (double emission, IUE LWP 30393),
%$^5$\ion{Mg}{ii} has a type III profile (double emission, IUE LWP 05470, LWP 06365, LWP 18717, LWR 10426, LWR 16729 LWP 21268, LWP 22612, LWP 32570, and LWP 32568),
%$^6$\ion{Mg}{ii} has a type I  profile (IUE LWP 13083),
%$^7$\ion{Mg}{ii} has a type III profile (IUE LWP 13006, LWP 08847),
%$^8$\ion{Mg}{ii} is in absorption (IUE LWP 22816, LWP 05834, LWP 30241, LWP 15172; HST/STIS O6LT01060),
%$^9$\ion{Mg}{ii} has alternated between type III (IUE LWR 06965) and type I (IUE LWP 11848, LWP 30190, LWP 8766; HST/STIS O66Q01020),
%$^{10}$\ion{Mg}{ii} has single emission partially filling in photospheric absorption (IUE LWP 30558),
%$^{11}$\ion{Mg}{ii} has emission which appears to be type I P~Cygni partially filling in the 
%photospheric absorption (IUE LWP 12989),
%$^{12}$\ion{Mg}{ii} has a type I P~Cygni profile (IUE LWP 25762, LWR 11977, LWR 08996).
%
%Comments on used IUE and HST spectra and deduced types of line profiles:\\
%$^1$LWP 30772 type I, LWP 13082 type III,
%$^2$LWR 11429, LWP 09517 abs; LWP 21212 and 18869 filled in to continuum level; possible type III but no net emission,
%$^3$LWP 30172 inv.\ P Cygni I with high vel.\ abs.\ LWP 30771 type III; variable absorption (Grady et~al.\ \cite{Grady1997}) ; type I for  STIS O5C902040,
%$^4$type III LWP 30393,
%$^5$type III LWP 05470, LWP 06365, LWP 18717, LWR 10426, LWR 16729 LWP 21268, LWP 22612, LWP 32570, LWP 32568,
%$^6$type I LWP 13083,
%$^7$type III LWP 13006, LWP 08847,
%$^8$abs; LWP 22816, LWP 05834, LWP 30241, LWP 15172 ; abs STIS O6LT01060,
%$^9$type III LWR06965, type I LWP 11848, LWP 30190; LWP 8766 ; I for STIS O66Q01020,
%$^{10}$single emission partially filling in photospheric absorption with ISM abs superposed,
%$^{11}$blueshifted absorption (wind) LWP 12989,
%$^{12}$type I LWP 25762, LWR 11977, LWR 08996,
%$^{13}$LWP 18883, and
%$^{14}$LWP 20324, LWP 25942, LWP 16072; LWP 27481 all type I P~Cygni profiles.
\end{table}