text:
\section{Introduction}

The existence of tight scaling relations between observable photometric
and kinematic galaxy parameters, in particular the Fundamental Plane (FP) of
elliptical galaxies (J\o rgensen et al. \cite{jorg}, Scodeggio
\cite{scodeggio}), and the Tully-Fisher relation for spirals (TF,
Tully \& Fisher \cite{tf}), finds
its most straightforward application in the evaluation of galaxy distances.
The small scatter observed in both relations implies a fine tuning
between parameters strictly related to the stellar component alone, such
as the optical luminosity,
and the kinematic properties of the galaxy, which are affected
by the overall mass distribution (both dark and visible).

In the case of spiral galaxies, it is therefore suggestive that a tight
scaling relation may also exist between photometric and kinematic properties
{\it of the disks alone}, with a scatter as low as, or even lower, than the
TF relation.
Karachentsev (\cite{kara}) found that, for a sample of 15 edge-on galaxy,
the disk scale length $R_d$ was connected to the 21~cm line velocity width
$W$ and the $I$--band central disk brightness $I(0)$ by the relation
$R_d \propto W^{1.4} I(0)^{-0.74}$,
with a scatter in $\log (R_d)$ of 0.048. The uncertainty
implied in the distance is around 12\%, smaller than the one usually
achieved by the TF relation ($15 \sim 20$\%).
More recently Chiba \& Yoshii (\cite{cy}, CY95 hereafter) tested on a sample
of 14 nearby spirals the relation
\begin{equation}
\protect\label{eq:cy}
\log R_d = a \log (V_2\; I(0)^{-0.5}) + b
\end{equation}
in the $B$ band,
where $V_2$ is the galaxy rotation velocity measured at 2.2 disk scalelengths.
Since the contribution from the disk to the overall rotation curve (RC)
has a maximum at this particular distance, the authors
argue that the contributions from bulge and dark
halo are likely to be less important, and therefore the
measured velocity should represent a good estimate for the rotation of the
disk alone.
For a set of exponential disks of fixed mass--to--light ratio ($M/L$) one
would expect $\log R_d \sim \log \, [V_2^2/I(0)]$, corresponding to $a=2$
in Eq.
(\ref{eq:cy}). Actually CY95 find $a=1.045$, again with a remarkably small
scatter.
On the other hand, recent work from Giovanelli (\cite{giovatf}) suggests
that the accuracy of Eq. (\ref{eq:cy}) as a distance indicator
is inferior to the one attained by the traditional TF relation
by at least a factor of 2.

Besides beeing a tool to provide redshift-independent distances,
scaling relations also contain information about
how galaxies -- and in particular their ``visible'' constituents -- have formed
and evolved (Gavazzi \cite{gava}, Ciotti \cite{ciotti}, Dalcanton et al.
\cite{dalca}, Burstein et al. \cite{burst} -- BBFN hereafter).
In this respect, spiral disks are a potentially ``easy'' class of systems,
since they are all characterized by well defined shape and
kinematics: if the effects of extinction on their surface
brightness distribution are accounted for, and a reliable estimate of their
mass is obtained, the subsequent scaling relations will be directly related
to systematic variations in the disks' stellar content.
Further information can be provided by the variation with wavelength
of such properties, in particular by scaling relations involving
colours (e.g., the colour magnitude relation; see Gavazzi \cite{gava1},
Tully et al. \cite{tully}, Peletier \& de Grijs \cite{pdg}).

In this work we investigate the existence and tightness of a general scaling
relation in the near infrared (NIR), similar to the one defining the FP, for
both structural components (disks and bulges) of a sample of 40 nearby spiral
galaxies.
Our aim is to test the power of these relations as tools to measure galaxy
distances, and use them to provide new information about the stellar content
and star formation history of spiral galaxies.
In the present paper we are going to deal mainly with the problem of the
distance measurements, leaving a thorough discussion of the second point
to future work.
The use of NIR photometry is well suited for a study of this kind,
since it minimizes the effect of internal extinction, and
provides a good tracing of the stellar mass.
In most cases, high resolution, optical RC's
allow us to trace the gravitational potential of the galaxies up to their
innermost regions.

The photometric parameters are obtained, in the NIR $H$ band, from a
bi-dimensional decomposition of the galaxy images, as described in
Sect.~\ref{phot}.
In Sect. \ref{kin} we show how the kinematical information are extracted
from the galaxy RC's, to which we fit a model composed by
bulge, disk, and a dark halo.
We subsequently derive the coefficients of the FP for bulges
and disks, and compare the potential accuracy in a distance determination
achieved by the disks' relation to the one we obtain using the TF relation
for the same sample.
We finally investigate the trends of $M/L$'s with luminosity and galaxy size.
Throughout the paper we adopt a Hubble constant
$H_{\circ} = 75$ km s$^{-1}$ Mpc$^{-1}$.

\section{The data}

The 40 spiral galaxies considered for this study are drawn from a larger
sample selected in the Pisces--Perseus supercluster region, for which
$H$ band images are available (see Moriondo et al. \cite{noi_2} and
\cite{noi_1} for a thorough description of the original sample).
This subset in particular contains the galaxies for
which a RC is also available both from the literature or the
private database of RG and MH, and includes morphological types ranging
from Sa to Scd.
In most cases, the RC's are derived from optical emission lines measurements
and are confined within two or three disk scale lengths.
For a few galaxies radio aperture--synthesis RC's (21~cm HI line)
are also available, extending well beyond the optical radius.
All the RC's were rescaled to our adopted values of distance
and inclination.
For all the galaxies (except UGC~2885) 21~cm line velocity widths are also
available from the database of RG and MH. We will use these values later on
to derive the $H$ band TF relation for the sample.
Table \ref{table:sample} contains the basic information on the galaxies
of the sample as well as the references for the RC's; many of these were
retrieved from the compilations by Corradi \& Capaccioli (\cite{corra})
and Prugniel et al. (\cite{prugni}).
We note that this sample is not appropriate to obtain an absolute
calibration of distances. It is however well suited to compare two
different scaling relations and their relative accuracy as distance
indicators.

\begin{table*}
\caption{The galaxy sample}
\begin{flushleft}
\protect\label{table:sample}
\begin{tabular}{lllllllll}
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\multicolumn{2}{c}{Names} & \multicolumn{2}{c}{R.A.~~~(J2000)~~~Dec.} & \multicolumn{1}{c}{RH Type} &
\multicolumn{1}{c}{$m_B$} & \multicolumn{1}{c}{$P.A.$} & \multicolumn{1}{c}{$D$ (Mpc)} &
\multicolumn{1}{c}{RC code} \\
\multicolumn{1}{c}{(1)} & \multicolumn{1}{c}{(2)} & \multicolumn{1}{c}{(3)} &
\multicolumn{1}{c}{(4)} & \multicolumn{1}{c}{(5)} & \multicolumn{1}{c}{(6)} &
\multicolumn{1}{c}{(7)} & \multicolumn{1}{c}{(8)} & \multicolumn{1}{c}{(9)} \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
UGC~00014   &          & 00 03 35.0 & 23 12 03 & Sc          & 13.8 &  41 & 92 & 1,2 \\
UGC~00026   & NGC~7819 & 00 04 24.5 & 31 28 19 & SB(s)b      & 14.2 &  99 & 61 & 3 \\
UGC~00089   & NGC~0023 & 00 09 53.4 & 25 55 25 & SB(s)a      & 12.8 & 171 & 56 & 4 \\
UGC~00673   &          & 01 06 09.7 & 31 24 24 & SAc?        & 15.7 &  45:& 79 & 1 \\
UGC~00725   &          & 01 10 11.0 & 43 06 35 & SBcd?       & 14.4 &  47 & 63 & 5 \\
UGC~00732   &          & 01 10 44.4 & 33 33 28 & SA(r)d      & 14.6 &  81 & 68 & 1 \\
UGC~00820   & NGC~0452 & 01 16 14.8 & 31 02 01 & SBab        & 13.6 &  35 & 62 & 6 \\
UGC~00927   & NGC~0496 & 01 23 11.5 & 33 31 46 & Sbc         & 14.1 &  38 & 76 & 1,7 \\
UGC~00940   &          & 01 23 37.9 & 34 34 11 & SA(s)c      & 15.1 &  68 & 89 & 7 \\
UGC~00975   &          & 01 25 15.6 & 34 21 34 & S           & 15.0 & 123 & 61 & 7 \\
UGC~01013   & NGC~0536 & 01 26 21.6 & 34 42 14 & SB(r)b      & 13.2 &  72 & 65 & 7 \\
UGC~01033   &          & 01 27 34.9 & 31 33 16 & Scd:        & 14.1 & 132 & 50 & 7 \\
UGC~01094   & NGC~0582 & 01 31 57.7 & 33 28 33 & SB?         & 14.1 &  60 & 54 & 7 \\
UGC~01238   & NGC~0668 & 01 46 22.6 & 36 27 39 & Sb          & 13.7 &  30 & 56 & 7,8 \\
UGC~01302   & NGC~0688 & 01 50 44.1 & 35 17 04 & (R')SAB(rs)b& 13.3 & 141 & 52 & 7,8 \\
UGC~01350   &          & 01 52 57.5 & 36 30 47 & SB(r)b      & 14.2 &  44 & 67 & 7 \\
UGC~01437   & NGC~0753 & 01 57 42.4 & 35 54 57 & SAB(rs)bc   & 13.0 & 131 & 62 & 7,8,9,10 \\
UGC~01633   & NGC~0818 & 02 08 44.4 & 38 46 36 & SABc:       & 13.2 & 114 & 53 & 9,11 \\
UGC~01835   & IC~0221  & 02 22 41.3 & 28 15 28 & Sc          & 13.7 &   5:& 65 & 1 \\
UGC~01935   & NGC~0931 & 02 28 14.5 & 31 18 42 & Sbc         & 14.5 &  82 & 64 & 1,12 \\
UGC~01937   & NGC~0935 & 02 28 10.9 & 19 35 59 & Scd:        & 13.6 & 153 & 52 & 13 \\
UGC~02134   &          & 02 38 51.8 & 27 50 50 & Sb          & 14.2 & 100 & 58 & 1 \\
UGC~02142   & NGC~1024 & 02 39 12.2 & 10 50 50 & (R')SA(r)ab & 13.1 & 158 & 44 & 14 \\
UGC~02185   &          & 02 43 11.4 & 40 25 34 & Scd:        & 13.5 & 141 & 55 & 1 \\
UGC~02223   &          & 02 45 14.4 & 35 11 21 & Scd:        & 14.8 &  46 & 63 & 1 \\
UGC~02241   & NGC~1085 & 02 46 25.3 & 03 36 26 & SA(s)bc:    & 13.1 &   2 & 88 & 15 \\
UGC~02617   &          & 03 16 00.7 & 40 53 08 & SAB(s)d     & 13.8 &  10 & 59 & 7 \\
UGC~02655   &          & 03 18 45.3 & 43 14 20 & SAB(s)d     & 13.5 & --  & 80 & 7 \\
UGC~02885   &          & 03 53 02.4 & 35 35 22 & SA(rs)c     & 13.5 &  45 & 76 & 10,16 \\
UGC~11973   &          & 22 16 50.4 & 41 30 13 & SAB(s)bc    & 12.9 &  42 & 52 & 17 \\
UGC~12173   &          & 22 43 52.0 & 38 22 37 & SAB(rs)c    & 13.5 & 101 & 59 & 1,7 \\
UGC~12230   & NGC~7407 & 22 53 21.2 & 32 07 44 & Sbc         & 13.9 & 160 & 81 & 1 \\
UGC~12378   & NGC~7489 & 23 07 32.5 & 22 59 50 & Sd          & 14.0 & 164 & 78 & 1 \\
UGC~12486   & NGC~7591 & 23 18 16.2 & 06 35 09 & SBbc        & 13.9 & 167:& 61 & 1,2,8,18 \\
UGC~12539   & NGC~7631 & 23 21 26.7 & 08 13 05 & SA(r)b:     & 13.9 &  77 & 45 & 18 \\
UGC~12598   & NGC~7664 & 23 26 39.9 & 25 04 50 & Sc:         & 13.4 &  88 & 42 & 1,10,19 \\
UGC~12618   & NGC~7679 & 23 28 46.8 & 03 30 41 & SB0         & 13.5 & --  & 64 & 20 \\
UGC~12666   &          & 23 33 41.0 & 32 23 02 & Scd:        & 14.4 & 124 & 62 & 1 \\
UGC~12667   &          & 23 33 49.5 & 30 03 37 & Scd:        & 13.5 & 127 & 46 & 1 \\
UGC~12780   & NGC~7753 & 23 47 04.7 & 29 29 01 & SAB(rs)bc   & 12.8 &  71 & 64 & 21 \\
\noalign{\smallskip}
\hline
            &          &            &          &             &      &     &    & \\
\end{tabular}
\end{flushleft}

{\small Notes to Table~1.\\
Cols. 5,6: from the Third Refernce Catalogue of Bright Galaxies (RC3), de Vaucouleurs et al.
1991. Col. 7: from Moriondo et al. 1999.
Col. 9: references for the rotation curves. 1: Courteau 1992; 2: Mathewson et al. 1992;
3: Szomoru et al. 1994; 4: Afanas'ev 1988a; 5: Van Moorsel 1983; 6: Oosterloo \& Shostak 1993;
7: Vogt 1995; 8: Amram et al. 1994; 9: Broeils \& Van Woerden 1994; 10: Rubin et al. 1980;
11: M\'arquez \& Moles 1996; 12: Amram et al. 1992; 13: Blackman 1977; 14: Rubin et al. 1985;
15: Rubin et al. 1982; 16: Roelfsema \& Allen 1985; 17: Afanas'ev 1988b; 18: Rubin et al. 1988;
19: Rhee \& Van Albada 1996; 20: Jore 1997; 21: Marcelin et al. 1987.
}

\end{table*}

\section{The fits to the brightness distributions \protect\label{phot}}

\begin{figure*}
\vspace{1.5cm}
\caption{Top panels: radial surface brightness profiles of the sample
galaxies, in a magnitude scale. For each plot, the triangles represent the
profile obtained by averaging the intensity over elliptical profiles (see
Moriondo et al. \cite{noi_1}); the dotted line is a cut along the major
axis of the galaxy; also shown are the best fit to the data (solid line) and
the contributions from bulge (dot--dash line) and disk (dashed line).
Bottom panels: the observed RC's (triangles) with the best fit to the data
(solid line). Again, the dot--dash and dashed lines represent the
contributions from bulge and disk respectively. The contribution from
the dark halo is shown as a dotted line.}
\label{fig:fit}\protect
\end{figure*}

\setcounter{figure}{0}
\begin{figure*}
\vspace{1.5cm}
\caption{Continued}
\end{figure*}

The photometric data reduction and analysis are described in detail in
Moriondo et al. (\cite{paper_1}, \cite{noi_1}). Briefly,
each galaxy image is fitted with a model consisting of an exponential disk
and a bulge, whose shape is described by a generalized exponential (S\`ersic
\cite{sersic}). Both brightness distributions are assumed to be elliptical
in the plane of the sky, and with a common centre and major axis. The
parameters of the fit are the two scalelengths, surface brightnesses and
apparent ellipticities (one for each component).
The results of these decompositions
were used in Moriondo et al. (\cite{noi_2}) to evaluate the effect
of internal extinction on the $H$-band structural parameters and derive
the corrections to the face-on aspect. The corrected
values for scalelengths, surface brightnesses and total luminosities
will be used in the following analysis.
In most cases an exponential bulge yields a satisfactory fit to the data.
For two galaxies in the subsample considered here (namely UGC~26 and UGC~820),
a value $n=2$ of the ``shape'' parameter in the exponent of the bulge
brightness distribution produces better results.
In two cases (UGC~673 and UGC~975) the disk alone is sufficient to fit
the galaxy, i.e. no trace of a bulge is found in the brightness
distribution.
Table \ref{tab:phot} contains the photometric parameters of the sample
galaxies, corrected to the face--on aspect and for the redshift;
the $H-$band total luminosity, in column 8, will be introduced in Sect. 5.
The resulting decompositions are plotted in the top
panels of Fig.~\ref{fig:fit}, together with the surface brightness profiles
averaged along elliptical contours (from Moriondo et al. 1999), and the
brightness profiles along the major axis. In the case of UGC 673 and UGC
12666, the discrepancy between these two profiles is due to the
ellipse--fitting routine, which in both cases has underestimated the galaxy
apparent ellipticity in the regions of lower signal--to--noise ratio.
Our fits, however, are in good agreement with the respective brightness
distributions, so that the estimated parameters
are reliable for these galaxies as well.

\begin{table*}
\caption{The photometric parameters}
\begin{flushleft}
\protect\label{tab:phot}
\begin{tabular}{cccccccc}
\noalign{\smallskip}
\hline
\noalign{\smallskip}
Name & $\mu_e$     & $R_e$ (kpc) & $\epsilon_b$ & $\mu(0)$    & $R_d$ (kpc) & $i$ (deg) & ${\cal M}_H$ \\
 (1) & (2)         & (3)   & (4)          & (5)         & (6)   & (7) & (8)   \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
 UGC~00014 & 16.45 (0.10) &  0.66 (0.04) &  0.27 (0.01) & 17.76 (0.08) &  4.08 (0.18) & 44.0 ( 1.9) & -24.03 (0.11) \\
 UGC~00026 & 17.93 (0.11) &  0.94 (0.05) &  0.16 (0.02) & 19.51 (0.11) &  5.69 (0.34) & 55.9 ( 1.2) & -23.14 (0.13) \\
 UGC~00089 & 14.99 (0.10) &  0.75 (0.03) &  0.31 (0.02) & 16.72 (0.10) &  2.79 (0.12) & 56.0 ( 0.5) & -24.63 (0.08) \\
 UGC~00673 &  ...         &   ...        &   ...        & 18.10 (0.64) &  1.92 (0.67) & 58.7 ( 4.3) & -22.27 (0.94) \\
 UGC~00725 & 18.55 (0.33) &  0.35 (0.09) &  0.01 (0.23) & 18.20 (0.24) &  3.40 (0.30) & 76.9 ( 0.3) & -23.00 (0.17) \\
 UGC~00732 & 17.91 (0.23) &  0.40 (0.06) &  0.41 (0.01) & 17.84 (0.10) &  2.85 (0.12) & 55.2 ( 0.6) & -23.02 (0.08) \\
 UGC~00820 & 16.00 (0.26) &  0.81 (0.05) &  0.22 (0.01) & 16.82 (0.25) &  2.85 (0.18) & 67.0 ( 0.5) & -24.50 (0.23) \\
 UGC~00927 & 16.92 (0.13) &  0.29 (0.03) &  0.12 (0.08) & 18.03 (0.09) &  3.83 (0.15) & 54.8 ( 0.5) & -23.44 (0.07) \\
 UGC~00940 & 19.14 (0.21) &  0.68 (0.12) &  0.15 (0.17) & 18.86 (0.10) &  4.16 (0.20) & 49.2 ( 1.7) & -22.86 (0.11) \\
 UGC~00975 &  ...         &   ...        &   ...        & 17.84 (0.09) &  1.73 (0.06) & 52.4 ( 0.7) & -21.96 (0.07) \\
 UGC~01013 & 15.84 (0.14) &  1.14 (0.06) &  0.43 (0.01) & 17.74 (0.13) &  4.74 (0.25) & 61.4 ( 0.5) & -24.69 (0.10) \\
 UGC~01033 & 17.56 (0.38) &  1.15 (0.17) &  0.75 (0.01) & 18.53 (0.36) &  2.87 (0.38) & 81.3 ( 0.4) & -22.82 (0.33) \\
 UGC~01094 & 17.03 (0.23) &  0.66 (0.07) &  0.23 (0.04) & 17.50 (0.21) &  3.40 (0.28) & 74.3 ( 0.3) & -24.21 (0.15) \\
 UGC~01238 & 16.53 (0.22) &  0.85 (0.02) &  0.14 (0.01) & 18.08 (0.22) &  3.02 (0.11) & 42.3 ( 1.4) & -23.38 (0.23) \\
 UGC~01302 & 15.19 (0.16) &  0.32 (0.04) &  0.29 (0.07) & 17.48 (0.14) &  2.41 (0.15) & 63.4 ( 0.9) & -23.39 (0.12) \\
 UGC~01350 & 17.35 (0.23) &  0.94 (0.03) &  0.35 (0.01) & 18.34 (0.23) &  6.15 (0.22) & 51.1 ( 0.6) & -24.25 (0.22) \\
 UGC~01437 & 15.92 (0.09) &  0.54 (0.02) &  0.28 (0.01) & 16.39 (0.07) &  2.64 (0.07) & 45.1 ( 0.7) & -24.37 (0.06) \\
 UGC~01633 & 16.26 (0.16) &  0.47 (0.03) &  0.42 (0.05) & 16.63 (0.13) &  2.76 (0.14) & 61.6 ( 0.3) & -24.22 (0.10) \\
 UGC~01835 & 17.19 (0.12) &  0.75 (0.06) &  0.06 (0.01) & 17.80 (0.09) &  4.32 (0.23) & 49.8 ( 1.6) & -23.95 (0.12) \\
 UGC~01935 & 14.97 (0.21) &  0.50 (0.04) &  0.43 (0.02) & 17.18 (0.19) &  4.33 (0.33) & 72.3 ( 0.3) & -24.88 (0.13) \\
 UGC~01937 & 16.54 (0.18) &  0.58 (0.05) &  0.32 (0.06) & 16.97 (0.17) &  3.13 (0.12) & 52.3 ( 0.8) & -24.20 (0.16) \\
 UGC~02134 & 17.51 (0.17) &  0.95 (0.08) &  0.15 (0.05) & 17.81 (0.16) &  4.15 (0.31) & 66.4 ( 0.9) & -23.89 (0.15) \\
 UGC~02142 & 15.57 (0.25) &  1.01 (0.05) &  0.42 (0.01) & 17.79 (0.24) &  4.64 (0.25) & 61.6 ( 0.5) & -24.58 (0.23) \\
 UGC~02185 & 17.17 (0.29) &  0.22 (0.04) &  0.16 (0.19) & 17.81 (0.21) &  3.64 (0.30) & 74.8 ( 0.3) & -23.56 (0.14) \\
 UGC~02223 & 19.67 (0.77) &  0.40 (0.34) &  0.00 (0.86) & 18.26 (0.30) &  2.76 (0.29) & 74.3 ( 0.9) & -22.51 (0.29) \\
 UGC~02241 & 17.75 (0.23) &  1.93 (0.15) &  0.20 (0.03) & 18.24 (0.36) &  4.20 (0.66) & 50.7 ( 2.8) & -23.93 (0.47) \\
 UGC~02617 & 17.69 (0.20) &  0.52 (0.09) &  0.38 (0.14) & 18.20 (0.13) &  3.16 (0.20) & 60.9 ( 1.1) & -22.88 (0.13) \\
 UGC~02655 & 18.65 (0.15) &  1.93 (0.27) &  0.15 (0.07) & 18.97 (0.26) &  6.26 (1.07) & 62.6 ( 2.7) & -23.64 (0.40) \\
 UGC~02885 & 15.80 (0.17) &  0.69 (0.05) &  0.00 (0.04) & 17.96 (0.15) &  9.42 (0.59) & 67.0 ( 0.4) & -25.58 (0.10) \\
 UGC~11973 & 16.90 (0.29) &  0.35 (0.05) &  0.27 (0.16) & 16.84 (0.20) &  3.61 (0.27) & 72.4 ( 0.3) & -24.57 (0.14) \\
 UGC~12173 & 17.36 (0.26) &  0.38 (0.09) &  0.13 (0.25) & 17.80 (0.08) &  4.59 (0.19) & 49.4 ( 1.4) & -24.02 (0.08) \\
 UGC~12230 & 17.34 (0.17) &  0.49 (0.09) &  0.00 (0.14) & 17.00 (0.11) &  3.10 (0.15) & 57.9 ( 0.7) & -24.01 (0.09) \\
 UGC~12378 & 17.14 (0.17) &  0.42 (0.07) &  0.19 (0.18) & 17.51 (0.10) &  3.40 (0.15) & 54.9 ( 1.0) & -23.77 (0.08) \\
 UGC~12486 & 15.74 (0.11) &  0.66 (0.03) &  0.00 (0.02) & 17.92 (0.11) &  4.04 (0.22) & 56.8 ( 1.1) & -24.12 (0.11) \\
 UGC~12539 & 16.71 (0.17) &  0.32 (0.02) &  0.23 (0.04) & 17.10 (0.16) &  2.12 (0.12) & 64.7 ( 0.3) & -23.17 (0.12) \\
 UGC~12598 & 16.24 (0.15) &  0.23 (0.03) &  0.16 (0.10) & 16.22 (0.11) &  1.43 (0.06) & 58.6 ( 0.4) & -23.18 (0.08) \\
 UGC~12618 & 15.49 (0.97) &  0.65 (0.03) &  0.03 (0.05) & 16.81 (0.98) &  2.01 (0.08) & 22.6 ( 3.8) & -23.83 (0.98) \\
 UGC~12666 & 19.32 (0.24) &  1.46 (0.25) &  0.33 (0.08) & 19.60 (0.27) &  6.97 (1.70) & 74.3 ( 2.4) & -23.14 (0.51) \\
 UGC~12667 & 17.73 (0.29) &  0.28 (0.06) &  0.38 (0.01) & 17.94 (0.09) &  2.84 (0.13) & 53.1 ( 1.2) & -22.82 (0.08) \\
 UGC~12780 & 16.14 (0.05) &  0.61 (0.03) &  0.06 (0.05) & 17.23 (0.05) &  4.75 (0.11) & 39.8 ( 0.7) & -24.81 (0.04) \\
\noalign{\smallskip}
\hline
        &              &              &              &              &              &             &         \\
\end{tabular}
\end{flushleft}

{\small Notes to Table~2.\\
Col 2.: bulge effective surface brigtness, in mag arcsec$^{-2}$. Col. 3:
bulge effective radius. Col. 4: bulge ellipticity. Col. 5: disk central
surface brightness in mag arcsec$^{-2}$. Col 6: disk scalelength. Col. 7:
disk inclination. Col. 8: Total absolute magnitude.
}

\end{table*}

\section{The fits to the rotation curves \protect\label{kin}}

To estimate the contribution of bulge and disk to a given RC we
use the information from the photometric data to predict the shape
of the RC's of the two components, and derive their $M/L$ ratios
from a best fit to the observed velocity profile. The accuracy of this
technique, which has been
used for a long time by many authors (van Albada et al. \cite{vanalb},
Kent \cite{kent1}, Martimbeau et al. \cite{mart}, Moriondo et al.
\cite{paper_2}), is actually impaired by the
scarce knowledge on the contribution of the dark component to
the overall RC.  This becomes certainly important beyond the disk rotation
peak, at around two disk scalelengths; however, it might also be
significant at smaller
radii, especially for low luminosity and low surface brightness galaxies --
as suggested by Persic et al. (\cite{persic}) and de Blok \& McGaugh
(\cite{dbmg}) -- but also
in the case of bright spirals (see Bosma, \cite{bosma}, for a recent
review on this topic). Courteau and Rix (\cite{cou_rix}) and Bottema
(\cite{botte}, \cite{botte2}), for
instance, estimate the disk contribution to be about 60\% of the overall
rotation at 2.2 scalelengths, whereas different authors (e.g. Verheijen
\& Tully \cite{verhe}, Dubinski et al. \cite{dubin}, Gerhard
\cite{gerhard}, Bosma \cite{bosma}) support a ``maximum disk'' scenario in
which such contribution is about 85\%, at least for bright galaxies.
The shape of the dark matter distribution is rather uncertain as well:
even the reliability of the distributions derived from numerical
simulations of structure formation (e.g. Navarro et al.
\cite{navarro}) is weakened by their apparent discrepancy with the observed
RC's of low surface brightness galaxies.
Since in this paper we are mainly interested in the properties of bulges
and disks, the choice of the dark halo distribution is not likely to be
important, at least
as long as the visible matter dominates the mass distribution in the inner
galaxy regions.

To have an idea of how the fit to the RC is influenced by the inclusion
in the model galaxy of a dark component, we perform two different fits
for each RC: one using only bulge and disk, and one including also the
contribution from a dark halo.
The expressions for the rotational velocity of an exponential disk and
a generic ellipsoidal bulge are reported in Moriondo et al. (\cite{paper_2}),
as well as two possible dark halo distributions, namely a constant
density sphere and a pseudo--isothermal one (Kent, \cite{kent1}).
The first halo distribution yields a linearly rising RC, and is
an approximation of the latter as $R$ tends to zero; the rotation velocity
associated to the pseudo--isothermal sphere, on the other hand, tends to a
constant value as $R$ goes to infinity.
This last distribution has been considered only for the 4 galaxies whose RC is
well sampled in the outer, flat part (if this is not the case, and the
asymptotic rotation velocity is not well defined, usually the two types
of dark matter halos yield the same result, in the sense that
only the linear part of the isothermal sphere is used by the minimization
routine that fits the data).

In general we find that if a dark component is included in the fit, it
never turns out to be dominant in the inner part of the RC, within two
disk scalelengths; this is also true when the dark matter distribution
is well constrained by a very extended RC.
In other words, the solutions we obtain are usually not very different
from the ``maximum disk'' ones, implying that,
in most cases, the visible part of the galaxy provides a good match
to the observed RC; we will therefore assume that the ``maximum disk''
hypothesis is basically correct for our galaxies.
An alternative scenario, however, will also be considered in
Sect.~\ref{sect:ml}.
In a few cases the available RC is not extended enough to constrain
even a constant density halo, and in these cases we use the results
from the ``bulge + disk'' fits.
We consider these values reliable, since in general the inclusion of
the dark halo in the fits does not produce major changes in the estimated
mass and $M/L$ of the visible components.

We also note that, in a few cases, at 2.2 $R_d$'s the contribution to the
overall rotation from the bulge is still significant, so that the
disk contribution is well below the measured circular velocity.
In these cases neglecting the presence of the bulge would
certainly lead to overestimate the disk mass and $M/L$.

Table \ref{tab:dyn} contains the parameters derived from the RC fits.
Also included in the table are the values
of the velocity width $W$ (corrected for instrumental smoothing,
redshift, turbulence, and inclination), and of the velocity at 2.2 $R_d$,
$V_2$ (corrected for redshift and inclination); both quantities will be
introduced in the
next section. In Fig.~\ref{fig:fit} (bottom panels) we show the best fits
to the RC's for all the galaxies in our sample.

\begin{table*}
\caption{The dynamical parameters}
\begin{flushleft}
\protect\label{tab:dyn}
\begin{tabular}{ccccccc}
\noalign{\smallskip}
\hline
\noalign{\smallskip}
Name & $M_b$            & $(M/L)_b$ & $M_d$            & $(M/L)_d$ & $W$ (km s$^{-1}$) & $v_2$ (km s$^{-1}$) \\
 (1) & (2)              & (3)       & (4)              & (5)       & (6)         & (7)         \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
 UGC~00014 &  12.2 ( 3.0) &  0.95 (0.25) &  97.5 ( 9.4) &  1.25 (0.16) & 456.7 (18.0)& 215.0 (18.2)  \\
 UGC~00026 &  ...         &  ...         &  22.5 ( 7.0) &  0.74 (0.25) & 271.6 ( 5.8)&  90.0 (27.6)  \\
 UGC~00089 &  21.7 ( 4.4) &  0.34 (0.08) &  29.2 ( 5.2) &  0.31 (0.06) & 445.2 ( 5.5)& 180.0 (31.2)  \\
 UGC~00673 &  ...         &  ...         &   8.9 ( 3.7) &  0.70 (0.53) & 299.2 (15.1)& 120.0 (26.0)  \\
 UGC~00725 &  ...         &  ...         &  24.5 ( 7.2) &  0.68 (0.26) & 293.1 ( 8.2)& 160.0 (44.9)  \\
 UGC~00732 &  ...         &  ...         &  17.4 ( 2.8) &  0.49 (0.09) & 289.7 (24.4)& 120.0 (18.7)  \\
 UGC~00820 &  ...         &  ...         &  55.1 ( 5.3) &  0.61 (0.16) & 462.7 ( 4.9)& 240.0 (17.4)  \\
 UGC~00927 &  ...         &  ...         &  34.7 ( 2.9) &  0.64 (0.08) & 314.3 (35.0)& 150.0 (11.2)  \\
 UGC~00940 &  ...         &  ...         &  65.7 ( 4.8) &  2.22 (0.27) & 328.8 (15.7)& 160.0 ( 8.9)  \\
 UGC~00975 &  ...         &  ...         &  13.1 ( 1.3) &  1.01 (0.13) & 275.0 ( 6.8)& 128.0 (12.0)  \\
 UGC~01013 & 181.1 (20.1) &  2.64 (0.46) &  81.1 (14.0) &  0.75 (0.16) & 550.9 ( 5.5)& 300.0 (49.5)  \\
 UGC~01033 &  10.2 ( 8.3) &  0.72 (0.64) &  12.7 ( 2.4) &  0.67 (0.28) & 323.1 ( 3.3)& 160.0 (22.0)  \\
 UGC~01094 &   3.9 ( 1.6) &  0.51 (0.25) &  49.2 ( 4.3) &  0.71 (0.16) & 435.2 ( 4.5)& 212.0 ( 5.6)  \\
 UGC~01238 &  23.8 ( 1.5) &  1.18 (0.27) &  28.7 ( 3.5) &  0.91 (0.23) & 397.9 (12.6)& 180.0 (21.1)  \\
 UGC~01302 &   9.0 ( 2.4) &  0.92 (0.29) &  23.1 ( 3.3) &  0.65 (0.13) & 353.9 ( 5.3)& 190.0 (24.8)  \\
 UGC~01350 &  ...         &  ...         & 169.2 (33.2) &  1.63 (0.49) & 731.3 (27.2)& 240.0 (46.2)  \\
 UGC~01437 &   6.6 ( 1.8) &  0.46 (0.13) &  49.6 ( 5.2) &  0.43 (0.05) & 420.1 ( 7.5)& 205.0 (20.6)  \\
 UGC~01633 &   4.5 ( 1.7) &  0.58 (0.24) &  56.9 ( 5.2) &  0.56 (0.09) & 479.4 ( 6.4)& 240.0 (18.3)  \\
 UGC~01835 &  10.2 ( 2.8) &  1.20 (0.36) &  65.4 (11.4) &  0.77 (0.15) & 423.2 (11.7)& 207.0 (34.2)  \\
 UGC~01935 &   1.4 ( 2.0) &  0.05 (0.07) &  46.8 ( 7.4) &  0.31 (0.08) & 447.0 ( 3.5)& 200.0 (27.8)  \\
 UGC~01937 &  ...         &  ...         &  56.5 ( 9.7) &  0.60 (0.14) & 437.8 ( 6.6)& 200.0 (33.5)  \\
 UGC~02134 &  15.5 ( 3.1) &  1.56 (0.41) &  34.8 ( 4.0) &  0.45 (0.09) & 335.6 ( 4.4)& 160.0 (13.9)  \\
 UGC~02142 &  65.1 (11.8) &  0.95 (0.29) & 109.2 ( 9.2) &  1.12 (0.29) & 520.1 ( 5.2)& 250.0 (16.3)  \\
 UGC~02185 &  ...         &  ...         &  37.6 ( 4.1) &  0.63 (0.15) & 437.1 (14.9)& 200.0 (14.2)  \\
 UGC~02223 &  ...         &  ...         &   7.2 ( 1.3) &  0.32 (0.11) & 244.9 (10.2)& 125.0 (19.5)  \\
 UGC~02241 &  82.3 (12.5) &  2.46 (0.68) &  44.6 (18.0) &  0.84 (0.45) & 461.9 (20.4)& 250.0 (93.0)  \\
 UGC~02617 &  ...         &  ...         &  22.4 ( 2.4) &  0.72 (0.12) & 535.4 (19.7)& 138.0 (12.0)  \\
 UGC~02655 &   9.1 ( 2.5) &  0.62 (0.20) &  39.1 ( 7.2) &  0.65 (0.20) & 307.0 (20.0)& 140.0 (10.2)  \\
 UGC~02885 &  53.8 ( 5.9) &  2.12 (0.43) & 185.7 (21.7) &  0.54 (0.10) &  ...        & 280.0 (27.6)  \\
 UGC~11973 &  ...         &  ...         & 104.1 (18.7) &  0.73 (0.20) & 503.2 ( 5.9)& 360.0 (59.1)  \\
 UGC~12173 &   5.2 ( 1.7) &  2.80 (1.16) & 104.2 ( 6.4) &  1.10 (0.11) & 465.3 (12.6)& 210.0 ( 9.7)  \\
 UGC~12230 &  ...         &  ...         &  83.1 ( 5.8) &  0.92 (0.12) & 517.0 ( 8.5)& 260.0 (12.9)  \\
 UGC~12378 &   1.3 ( 1.7) &  0.47 (0.60) &  52.3 ( 6.1) &  0.77 (0.12) & 407.4 ( 6.6)& 200.0 (21.5)  \\
 UGC~12486 &  33.1 ( 6.2) &  1.32 (0.29) &  61.9 ( 9.6) &  0.93 (0.18) & 432.6 ( 7.1)& 210.0 (30.5)  \\
 UGC~12539 &   2.2 ( 1.5) &  0.92 (0.62) &  21.5 ( 3.3) &  0.56 (0.12) & 375.2 ( 5.3)& 160.0 (22.5)  \\
 UGC~12598 &  ...         &  ...         &  18.8 ( 1.5) &  0.48 (0.06) & 360.2 ( 4.0)& 170.0 (11.0)  \\
 UGC~12618 &  14.1 ( 4.7) &  0.47 (0.48) &  36.2 (14.0) &  0.80 (0.84) & 630.9 (105.4)& 215.0 (82.6)  \\
 UGC~12666 &   3.8 ( 1.6) &  0.84 (0.41) &  47.0 (11.7) &  1.12 (0.41) & 271.9 ( 5.5)& 150.0 ( 7.1)  \\
 UGC~12667 &  ...         &  ...         &  21.5 ( 2.4) &  0.67 (0.09) & 253.7 ( 6.0)& 140.0 (14.2)  \\
 UGC~12780 &   1.3 ( 6.2) &  0.09 (0.42) & 161.0 (12.2) &  0.94 (0.08) & 515.8 (10.0)& 260.0 (18.9)  \\
\noalign{\smallskip}
\hline
           &              &              &              &              &              &              \\
\end{tabular}
\end{flushleft}

{\small Notes to Table~3.\\
Cols. 2,4: masses in units of 10$^9$ M$_{\odot}$. Cols. 3,5: M/L's in solar units.
}

\end{table*}

In 17 cases out of 40, the observed RC has either no data-points in the
innermost region (3 cases), or shows no evidence of contribution by
the bulge. For these galaxies the bulge mass and $M/L$ are either
unconstrained or likely to be underestimated.
Most of the 14 galaxies, for which the disk contribution alone is sufficient
to match the inner RC, are
characterized by the smallest bulge--to--disk ratios ($B/D$) of the sample
($B/D < 0.05$), or by the faintest bulge luminosities (${\cal M}_b > -21$).
It is not surprising, therefore, that in these cases the bulge contribution
to the overall RC cannot be adequately resolved.
A direct comparison between the $M/L$ of disks and bulges seems to
confirm these statements. In Fig.~\ref{fig:mllbd} mass
versus luminosity is plotted for the disks, and for the bulges with
$M_b > 10^9 M_{\odot}$. These are the 23 cases for which we obtain a
reliable fit to the RC for both components, and the two sets of objects seem
to form a smooth sequence, roughly delimited by $M/L = 0.25$ and
$M/L = 2.5$, in solar units.
The remaining ``low mass''
bulges are placed well below the sequence, out of the plot window, suggesting
that their mass is largely underestimated.
In the following analyisis, therefore, we will consider only the
bulges plotted in Fig.~\ref{fig:mllbd}.

\begin{figure}
\vspace{1.5cm}
\caption[]{Mass versus luminosity plotted for bulges and disks of our
sample galaxies. Open circles represent the bulges, whereas filled triangles
represent the disks.  Only bulges with mass $> 10^9 M_{\odot}$ are plotted.
The slope of the two dashed line is of constant $M/L$. The two $M/L$ values
plotted, 2.5 and 0.25, are in solar units ($H$ band).}
\label{fig:mllbd}\protect
\end{figure}

\section{The Tully Fisher relation for the sample \protect\label{sec:tf}}

To derive an $H$-band TF relation for our galaxies the 21~cm line velocity
widths from the RG and MH database (Table 3) have been corrected for instrumental
smoothing, redshift, turbulence, and inclination of the galaxy to the
line of sight, according to the prescriptions in Giovanelli et al.
(\cite{giova97}, \cite{giovanew}). The absolute galaxy magnitudes in the $H$
band (Table 2) are derived integrating the surface brightness profiles
extrapolated up to 8 disk scalelengths; a small correction to face-on aspect
is applied, using the results obtained for the disks alone in Moriondo et
al. (\cite{noi_2}).
Figure \ref{fig:tf} shows the plot we obtain, with the best fit to the
data after the exclusion of the three discrepant points to the right.
In the case of UGC~12618, our value for the inclination is probably
underestimated, leading to an exceedingly large correction for $W$; on
the other hand, due to its large errorbars, the contribution of this galaxy
to the fit is not very significant anyway. In the case of UGC~1350
and UGC~2617, the observed $W$ is likely to be overestimated, maybe for a
misidentification of the galaxy; we note that for these two objects
an estimate of the rotation derived from the RC is, respectively, about 75\%
and 50\% smaller than $W$.

The errors on both axes are of comparable magnitude, therefore the weight for
each data point is the RMS of the two contributions.
Since the relation we fit is $y = ax + b$, the i-th residual is weighted by
\begin{equation}
\protect\label{eq:wei}
 w(i) = \left [\sqrt{\epsilon_{y(i)}^2 + a^2 \epsilon_{x(i)}^2}\right ]^{-1} \;\;,
\end{equation}
where the $\epsilon$'s are the estimated errors.
The slope and zero offset, with respect to the average $\log W$, are
respectively $-7.7 \pm 1.0$ and $-23.67 \pm 0.08$.

\begin{figure}
\vspace{1.5cm}
\caption[]{The $H$-band Tully-Fisher relation for our sample, with the
best fit to the data after the exclusion of the three discrepant points
on the right side. Different symbols correspond to different morphological
types: filled circles for Sa-Sab, filled squares for Sb-Sbc, open squares
for Sc-Scd, crosses for Sd and dm.}
\label{fig:tf}\protect
\end{figure}

\section{Fundamental Planes}

We now fit separately to bulges and disks a relation
\begin{equation}
\protect\label{eq:fp}
\log R = a \log V + b \log I + c
\end{equation}
involving a scalelength, a velocity, and a surface brightness, analogous
to the FP of elliptical galaxies.
The designated parameters for the bulges are the effective
radius $R_e$, the surface brightness at $R_e$ ($I_e$),
and a velocity defined as
\begin{equation}
\protect\label{eq:v_b}
V_b = \sqrt{\frac{M_b}{R_e}}
\end{equation}
where $M_b$ is the bulge mass, in units of 10$^9 M_{\odot}$.
Since for all the bulges selected (the ones with $M_b > 1$) the
brightness distribution is fitted by a pure exponential -- i.e.
they all have the same shape -- this velocity scales as the rotation velocity,
measured at 2.2 bulge scalelengths $R_b$. Also, $R_e$ and $I_e$ are related
by constant factors respectively to $R_b$
and the central surface brightness $I(0)$ (the two parameters usually adopted
for the disks): $R_e = 1.67\; R_b$, and $I_e = 0.19\; I(0)$.
For the disks we choose the exponential scalelength $R_d$, the central surface
brightness $I(0)$, and a velocity $V_d$ defined via a relation analogous to Eq.
(\ref{eq:v_b}), with the disk mass and the disk scalelength. Again, this
velocity differs from the value at 2.2 $R_d$ by the same factor for
all the exponential distributions.
Following CY95, we also consider a relation involving $R_d$, $I(0)$, and the
{\it total galaxy rotation velocity} at 2.2 $R_d$, derived directly from the
RC, which we will indicate as $V_2$.

It turns out that the three parameters to be fitted have comparable
uncertainties, and each point needs to be weighted by a combination of them.
In the case of the structural parameters ($R$, $I$), besides the
formal error from the fit to the brightness distributions, a major
contribution
is added from the errors in the corrections to face-on aspect,
that is from the uncertainty in the amount of internal extinction.
These are evaluated according to the results in Moriondo et al. (\cite{noi_2}).
The uncertainty on the velocity depends in principle on the
errors associated both to the RC measurement and to the scale length.
However we expect this latter contribution to be less important,
especially for the disks, whose scalelength is always the best determined
parameter in the surface brightness decompositions. Therefore we assume
the uncertainty on the velocities to be well represented by the formal error
derived from the fitting routine.
The errors on all other quantities are derived from these
values: for example, the error on the disk mass is obtained combining the
uncertainties on the velocity and the scale length, since
$M \sim V^2\, R$.

The fit to the disk parameters yields
\begin{equation}
\protect\label{eq:fpd}
\begin{array}{lll}
\log R_d & =  & (1.31\, \pm\, 0.19) \, (\log V_d - <\log V_d >) + \\
         &    & (-0.62\, \pm\, 0.09) \, (\log I(0) - <\log I(0) >) + \\
         &    &  (1.29\, \pm\, 0.07) \;\;\; , \\
\end{array}
\end{equation}
where ``$<\; >$'' designates the average over the sample.
If $V_2$ is chosen, instead of the value defined in terms of the disk mass and
scalelength, we obtain
\begin{equation}
\protect\label{eq:fpd2}
\begin{array}{lll}
\log R_d & = & (1.47\, \pm\, 0.16) \, (\log V_2 - <\log V_2 >) + \\
         &   & (-0.61\, \pm\, 0.07) \, (\log I(0) - <\log I(0) >) + \\
         &   & (1.39\, \pm\, 0.06) \;\;\; . \\
\end{array}
\end{equation}
We note that these coefficients are close to the values implied
by the TF relation derived in Sect. \ref{sec:tf}:
in fact, from $L \sim W^{3.1}$, we derive $R \sim W^{1.5}I^{-0.5}$.
Therefore, the TF relation is a nearly edge-on
projection of the FP. Also, these values are not inconsistent with
the constraint implicit in the relation suggested by CY95
(Eq. (\ref{eq:cy}) ), i.e. $a = 2b$.

The best fit to the bulge parameters yields:
\begin{equation}
\protect\label{eq:fpb}
\begin{array}{lll}
\log R_e & = & (0.97\, \pm\, 0.13 ) \, (\log V_b - <\log V_b >) + \\
         &   & (-0.61\, \pm\, 0.08) \, (\log I_e - <\log I_e >) + \\
         &   & (-0.46\, \pm\, 0.10) \;\;\; . \\
\end{array}
\end{equation}
Again, a relation like Eq. (\ref{eq:cy}) is not ruled out, even
if with a slope $a$ slighlty different from the disks' value.

The errors associated to the various coefficients are estimated by performing
a large number of Monte Carlo simulations of the data sample and fitting
each simulation, to derive a distribution of values for each coefficient.
Figures \ref{fig:fpd} and \ref{fig:fpd2} show the relations we find for
the disks, whereas Fig. \ref{fig:fpb} shows the one for the bulges.

\begin{figure}
\vspace{1.5cm}
\caption[]{The scaling relation of Eq. (\ref{eq:fpd}) for the disks,
derived from the best fit to the RC. The data and the best fit
are shown.
The factorization of the $I(0)$ coefficient in the $x-$axis label
is chosen to make it easily comparable with Eq. (\ref{eq:cy}).
Symbols are as in Fig. \ref{fig:tf}.}
\label{fig:fpd}\protect
\end{figure}

\begin{figure}
\vspace{1.5cm}
\caption[]{The scaling relation of Eq. (\ref{eq:fpd2}) for the disks,
derived using the rotation velocities at 2.2 $R_d$. The data and the best
fit are shown. Symbols as in Fig. \ref{fig:tf}.}
\label{fig:fpd2}\protect
\end{figure}

\begin{figure}
\vspace{1.5cm}
\caption[]{The scaling relation of Eq. (\ref{eq:fpb}) for the bulges.
The data and the best fit are shown. Symbols as in Fig. \ref{fig:tf}.}
\label{fig:fpb}\protect
\end{figure}

\subsection{A comparison with published results}

The coefficients we derive for the disks are different
from the values found by CY95 ($a = 1.0$, $b = -0.5$), but closer to the
ones reported by Karachentsev (\cite{kara}), i.e. $a = 1.4$, $b = -0.7$;
we note however that, in the case of CY95, the photometric data
were in a very different passband ($B$).
Both our coefficients and the other quoted values are not consistent
with what would be expected on the basis of the virial theorem and a
universal mass--to--light ratio ($a=2$ and $b=-1$).

The various sets of coefficients can also be compared to the ones which
define the FP of elliptical galaxies, evaluated using
the central velocity dispersion as the kinematic parameter, and
the effective surface brightness.
For example, Bender et al. (\cite{bbf}) report for the Virgo cluster
$a = 1.4$ and $b = -0.85$, in the $B$ band; more recently J\o rgensen et al.
(\cite{jorg}) find $a = 1.24$ and $b = -0.82$ in the Gunn $r$ band, with a
scatter of
0.084 in $\log R_e$; Pahre et al. (\cite{pahre}) estimate the NIR
coefficients of the plane to be $a = 1.53$ and $b = -0.79$.
The various FP's are not very different, and actually the
existence of a ``cosmic metaplane'' has already been claimed by Bender et al.
(\cite{bendk}), and BBFN.
In particular they defined a set of three parameters (the $k$ parameters)
particularly suited to
represent the FP of elliptical galaxies in the $B$ band, and found
that basically all the self--gravitating systems show a similar behaviour
in the $k$-parameter space.
In the case of spiral galaxies, they considered their
global properties, without attempting a decomposition into structural
components, and for the bulges in their data sample they used the
central velocity dispersion as the kinematical parameter.
This work improves the approach by characterizing separately bulges
and disks from the photometric point of view; in addition, we are
able to determine the bulge mass independently of its kinematical status
(i.e., if it's more or less supported by rotation), and obtain an
independent estimate of the coefficients of the bulge FP.

Figure \ref{fig:ksp} shows our data in the $H-$band $k$--space, with
bulges denoted as open circles, and disks as triangles.
We have defined the three coordinates as
$k_1 = \log(M)$, $k_2 = log(M/L \;\cdot\; I_e^3)$, and $k_3 = \log(M/L)$,
where $M$ is the total mass in units of $M_{\odot}$, $M/L$ is the
stellar mass--to--ligth ratio in solar units, and $I_e$ is the effective
surface brightness in $L_{\odot}\, pc^{-2}$. These definitions, besides
being applied to a different passband, are slightly
different from the ones introduced by Bender et al. (\cite{bbf}).
We can calculate the transformations between the two sets of
coordinates from the relations reported in the Appendix A
to BBFN, and assuming that all our bulges and disks are adequately
described by exponentials. Using a typical $B-H = 3.5$ for both components,
we find

\vspace{0.2cm}
\begin{equation}
\protect\label{eq:trans}
\left\{ \begin{array}{lll}
		\; k^B_1 & = & \frac{1}{\sqrt{2}}\; (k_1 - 5.97) \\
		\; k^B_2 & = & \frac{1}{\sqrt{6}}\; (k_2 + 0.58) \\
		\; k^B_3 & = & \frac{1}{\sqrt{3}}\; (k_3 + 1.37) \\
	  \end{array} \right.
\end{equation}
\vspace{0.2cm}
\noindent
where $k^B_1$, $k^B_2$, and $k^B_3$ are the $B-$band BBFN parameters.

The dotted line in the upper right corner of the $k_1$ vs. $k_2$ plot
corresponds, in our set of coordinates, to the boundary of the so--called
Zone of Exclusion (ZOE), defined in the $B$ band by $k^B_1 + k^B_2 > 8$:
it is consistent with our data, in the sense that most bulges and all
the disks are placed to its left side.
The BBFN database for the bulges is here extended to lower
masses, with several data--points falling in the typical range of dwarf
ellipticals
($M < 10^{10} M_{\odot}$); the two classes of objects appear however
separated, with the bulges shifted towards higher values of $k_2$, and
therefore higher concentrations (note that, for a given mass,
$k_2$ is proportional to $\log (I_e^2/R_e^2)$, which is higher for compact,
bright objects).

For what concerns spiral galaxies, BBFN find that their
average distance from the ZOE increases steadily with morphological type,
from Sa's to Irregulars;
the data points of our disks, however, are all
placed in about the same region of the $k_1$--$k_2$ plane, quite distant
from the ZOE, and roughly coincident with the locus occupied by Scd's
galaxies in the BBFN's plots.
Most likely, this difference arises from the separation of the two structural
components, which has allowed us to plot the $k$ parameters of the {\it
disks alone}: if the values for the whole galaxies
are considered, one would expect the systems with higher
$B/D$ (namely, the early--type spirals) to lie closer to
the ZOE, due to the contamination of the bulge. The BBFN sequence, therefore,
would be mainly driven by the average $B/D$, which in turn is roughly
correlated with morphological type.
When considered separately, on the other hand, disks and bulges are
located in two distinct, contiguous regions of the $k-$space, as it
is also evident from the $k_2$--$k_3$ projection, with the disks shifted
towards higher masses and lower concentrations.
A different ZOE could in principle be defined for the disks, with about the
same slope but shifted by about two decades towards lower $k_2$ values.

In the top panel of Fig. \ref{fig:ksp}, we have plotted the slope of the
$B-$band FP for
the Virgo cluster, scaled to the centroid of the bulges (dashed line)
and of the disks (solid line).
It appears to be consistent with our data, as suggested by the similarity
of our coefficients in Eqs. (\ref{eq:fpd}) and (\ref{eq:fpd2}) to the ones
reported by Bender et al. (\cite{bbf}).
Also, using Eqs. (\ref{eq:trans}) and the definition in BBFN, we can
estimate the
quantity $\delta_{3:1}$ for bulges and disks, representing their average
vertical distance from the ellipticals' FP in the $k^B_1$--$k^B_3$ projection.
In the case of the bulges, we find $\delta_{3:1} = 0.03$ dex, in fair
agreement with the BBFN estimate (-0.03); for the disks
we find a shift of -0.19 dex, which is about the value found by BBFN for
spirals from type Sa to Sc.

\begin{figure}
\vspace{1.5cm}
\caption[]{Bulges (open circles) and disks (triangles) in the $k-$space
defined by Bender et. al (\cite{bbf}). In the top panel the slope of the
FP for elliptical galaxies is plotted for comparison. In the $k_1$ versus
$k_2$ panel the dotted line represents the Zone of Exclusion,
as defined by BBFN.}
\label{fig:ksp}\protect
\end{figure}

\section{The disk FP as a distance indicator}

In order to assess the goodness of Eqs. (\ref{eq:fpd}) and (\ref{eq:fpd2})
as tools to
measure galaxy distances, we compare the scatter of the data points, with
respect to the best fit, to the scatter associated to the TF relation.
The dispersion is defined as
\[ \sigma = \sqrt{\frac{\sum_i{(\Delta_i w_i)^2}}{\sum_i{w_i^2}}} \;\; ,\]
where $\Delta_i$ is the residual on the i-th data point and $w_i$ the
associated weight, defined by Eq. (\ref{eq:wei}).
We find a dispersion of 0.38 mag for the TF relation, implying an uncertainty
of 19\% on the distance of a single galaxy. We note that the galaxy
distances used in this context have been estimated purely from redshifts.
The peculiar velocity field thus adds scatter to the corresponding TF
relation in a measure which we estimate on the order of 0.15 to 0.20 mag,
at the typical distance of these objects. Had peculiar velocity--corrected
distances been used, the TF scatter would have been so that distance
estimates would have uncertainties of about 16\%, rather then 19\%.

In the case of the FP, we find a
dispersion of 0.11 in $\log r$ if we use velocities derived from the best
fits (Eq. (\ref{eq:fpd})), and of 0.09 if the velocities
are the actual rotation velocities (Eq. (\ref{eq:fpd2}) ).
The associated uncertainties in the
distance are respectively about 29\% and 23\%.
Even if these two values are less than 1/2 of the dispersion quoted by
Giovanelli for the relation proposed by CY95 and a sample of 153 spiral
galaxies (0.25 in $\log r$, not based on a detailed disk--bulge
decomposition analysis as we use here), they are still larger than the
uncertainty yielded by the TF relation for our sample.
Therefore, according to our data, the disk FP is not as accurate,
as a distance indicator, as the TF relation, even if it allows for one
more free parameter in the relation.
This result could be imputed to the scatter added to the relation by the
uncertainties introduced in the data analysis process (in particular,
the decomposition of the surface brightness distribution and the fit to the
RC). On the other hand, we find that a modified Tully-Fisher relation,
in which the velocity width is replaced by $V_2$, is characterized as well
by a larger dispersion of 0.45 mag. This value is equivalent to the
dispersion of 0.09 in $\log r$ associated to Eq. (\ref{eq:fpd2}).
In a similar way, if the total luminosity is replaced
by the luminosity within 2.2 $R_d$'s, we find a very large dispersion of
0.64 mag.
Since these alternative parameters are not strictly derived from the
surface brightness decompositions or by the fit to the RC's, as it is the
case for the FP ones, we argue that using parameters associated with the
inner part of the galaxy (rather than global quantities), is in itself a
major source of scatter in the scaling relation considered.
Thus, the fine tuning between photometric and kinematic
parameters that yield the TF relation would be more effective because
of their global character.
About the much reduced dispersion with respect to the Giovanelli data,
we attribute this difference to the use of a more refined
data-analysis technique for our sample.

\section{The relation between mass and luminosity \protect\label{sect:ml}}

Eqs.~(\ref{eq:fpd})--(\ref{eq:fpb}) show that for both disks and bulges
a systematic variation of $M/L$ exists,
if we assume that we have properly evaluated their
shape, photometric properties (including the effect of internal
extinction), and contribution to the RC.
In particular we can rewrite Eqs. (\ref{eq:fpd}) and (\ref{eq:fpb}) as
\begin{equation}
\protect\label{eq:lmd}
L_d \sim \frac{M_d^{1.0 \pm 0.2}}{R_d^{0.7 \pm 0.4}}
\end{equation}
and
\begin{equation}
\protect\label{eq:lmb}
L_b \sim \frac{M_b^{0.8 \pm 0.2}}{R_e^{0.5 \pm 0.3}} \;\; .
\end{equation}
Whereas for elliptical galaxies the $M-L$ plane shows an edge-on view of
the FP, this is not the case for disks and bulges, and a residual dependence
on the scalelength is left; this dependence is such that, if a given mass
settles into a larger size, the corresponding $M/L$ ratio is larger.
Actually, this result is already implicit in the work by CY95: a good match
to equation  \ref{eq:cy} with $a \neq 2$ is possible only if $M/L$ is a
function of $R_d$ alone.
Previous results, both observational (Persic et al. 1996), and
theoretical (Navarro et al. \cite{navarro}, Navarro \cite{nava}), have
suggested that the stellar
$M/L$ in the $B$ band increases with the galaxy luminosity, rather than
with its size. This conclusion is probably consistent with ours, since
the total galaxy luminosity, especially in the $B$ band, is mainly
determined by the disk scalelength.
Since the average stellar $M/L$ ratios are determined by the
star--formation history of the galaxy, a connection must necessarily
exist between the structural properties of the system, in
particular its size, and the characteristics of its average stellar
population. This is not surprising, since connections of this kind also
exist for ellipitical galaxies: for example the one at the base of the
well--known color--magnitude relation.
On the other hand, the parameters which characterize stellar populations
(age, metallicity, star--formation rate, etc.), whose systematic variation
could be responsible of the observed trend, are far too many to be
constrained by our $H-$band data alone.
Some additional information on this issue could be provided by a detailed
multiband
analysis -- possibly integrated by spectroscopic data -- as the one recently
carried out by Pahre et al. (\cite{pahre2}) for elliptical galaxies.

We note however that a different scenario can be outlined, in particular
if we forget Eqs. (\ref{eq:lmd}) and (\ref{eq:lmb}), and assume instead
that the stellar $M/L$ ratio is constant for all the galaxies.
In this hypothesis, Eq. (\ref{eq:fpd2}) can be used to
predict how the contribution of the disk to the RC should scale with
surface brightness and scalelength.
Since we have, for an exponential disk:
\begin{equation}
\protect\label{eq:vdisk}
V_d \sim [(M/L)\, I(0)\, R_d]^{0.5} \;\; ,
\end{equation}
and from Eq. (\ref{eq:fpd2}):
\[ V_{2} \sim I(0)^{0.41} R_d^{0.68} \;\; , \]
if $M/L$ is a constant, we derive

\begin{equation}
\protect\label{eq:vsc}
\frac{V_d}{V_{2}} \sim \frac{I(0)^{0.09 \pm 0.07}}{R_d^{0.18 \pm 0.07}} \;\; ,
\end{equation}

\noindent
implying that the relative disk contribution to the RC should be the smallest
for large galaxies and, although with less significance, for low surface
brightness ones\footnote{
From Eqs. (\ref{eq:fpd}) and (\ref{eq:fpd2}) we can see instead that, in
our RC fits, the ratio $V_d/V_2$ is about constant, i.e. independent of $R_d$
and $I(0)$: it amounts to about 85 \% on average, the typical ``maximum
disk'' value. As a consequence, the disk $M/L$ must increase with $R_d$.}.
For the bulges, using Eqs. (\ref{eq:fpb}) and (\ref{eq:vdisk}), we find
a trend with size similar to the one expressed by Eq. (\ref{eq:vsc}).
Considering the range of
parameters, rather uniformely covered by our sample (about three magnitudes
in $I(0)$ and a factor of 4 in $R_d$), and assuming that the brightest and
more compact disks contribute about 90\% to the overall RC at 2.2 $R_d$, then
Eq. (\ref{eq:vsc}) implies that,
for the galaxies with the largest radii and faintest surface brightness,
$V_d$ should be about 55\% of the observed rotation velocity.
In this hypothesis a ``maximum disk'' RC can be ruled out in most cases;
of course, to match the observed RC's, we have to postulate a conspicuous
increase with size of the relative amount of dark matter.
As already mentioned in Sect. \ref{kin}, the results by Bottema
(\cite{botte}, \cite{botte2}) and by Courteau \& Rix (\cite{cou_rix})
support a scenario of
this kind, with the disk contributing, on average, about 60\% of the
rotation at 2.2 $R_d$'s. Assuming that this rule holds for our sample
as well, then, Eq. (\ref{eq:vsc}) predicts that the ratio
$V_d/V_2$ should vary throughout the sample between about 0.45 and 0.75,
in a well defined way according to the size and surface brightness of
each disk. Neglecting the presence of the bulge, and assuming an infinitely
thin disk, the corresponding ratio of dark to visible mass
within $R_2$ can be expressed as
\[\frac{M_h}{M_d} \simeq 0.8\left[\left( \frac{V_2}{V_d} \right)^{2} - 1 \right] \;\; .\]
This quantity changes by more than a factor of 8 in our sample, from 0.4 to
3.3, whereas in the ``maximum disk'' hypothesis it stays roughly constant:
in principle, the predictions of a reliable model for galaxy formation could
help to distinguish between two such different behaviours.

Of course, any intermediate scenario between the two extremes discussed
here (``maximum disk'' solutions and constant stellar $M/L$) could be
considered as well.
From the observational point of view, again, more detailed spectrophotometric
data might better constrain
possible variations in the average stellar population of different
galaxies, and help to distinguish between the different possibilities.

\section{Summary}

Using near--infrared images and rotation curves of a sample of 40 spiral
galaxies, we have determined the scaling relations, between structural
and kinematic parameters of bulges and disks, analogous to the Fundamental
Plane of elliptical galaxies.
The accuracy of the  disk FP as a distance indicator, for this set of data and
our photometric decompositions, is comparable but slightly lower than the one
attained by the Tully--Fisher relation. This suggests that the fine tuning
between dark and visible components at the basis of the various scaling
relations is more effective for global parameters.
Also, we deduce that (a) either the stellar mass-to-light ratio of the disk
increases with $R_d$, or (b) the disk contribution to the observed RC
decreases according to Eq. (\ref{eq:vsc}) for galaxies of large size.
A similar behaviour is observed for the bulges.

\begin{acknowledgements}
We would like to thank the referee, A. Bosma, for his careful reading of
the manuscript, C. Giovanardi and L. Hunt for insightful comments and
suggestions, and Stephane Courteau for having provided his data
in electronic format.
This research was partially funded by ASI Grant ARS--98--116/22.
Partial support during residency of G.M. at Cornell University was obtained via
the NSF grant AST96-17069 to R. Giovanelli.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


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You've probably heard the expression, "It's the thought that counts." That is very much the case with Mother's Day gifts. I recently found myself scrambling among the mass of people shopping for something very unique and non-floral for my mother. However, I realized that there are many reasons why sending my mother a special flower arrangement is a unique Mother's Day gift.
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text:
Union Pacific begins to serve Missouri rail park
TTX promotes Savard, Deppisch
TTX Co. recently appointed Kathleen Savard vice president and chief financial officer to succeed Thomas Marion, who plans to retire after serving TTX for 30 years.
Savard, who will assume the post Jan. 1, joined TTX earlier this year as assistant VP of strategic financial planning. She previously served Bank of America Corp. in various financial capacities and Flowserve Corp. as VP and treasurer.
TTX also named Deborah Deppisch corporate secretary. Most recently assistant corporate secretary, she previously served Fort James Corp., Fortune Brands and Takada Pharmaceuticals in various capacities.
Owned by North America's nine largest railroads, TTX owns and operates a free-running pool of more than 207,500 freight cars.

redpajama_set_name: RedPajamaCommonCrawl


Courtesy of TransfixThis trucking company is in the middle of Manhattan.
Transfix, an app for truck drivers to connect with shippers, is based in New York City.
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Founded in 2013, Transfix CEO Drew McElroy said it was crucial for the company's success that they capture the engineering talent that's hard to find outside of New York or San Francisco.
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San Francisco, New York, and other coastal cities are the typical hubs we think of for major corporations and startups alike.
But the $US1.45 trillion logistics industry operates a little differently. The biggest companies in trucking, for instance, are headquartered in cities like Omaha, Nebraska, Green Bay, Wisconsin, and Lowell, Arkansas.
That created an interesting dynamic for logistics entrepreneurs like Drew McElroy and Jonathan Salama, when they were looking for a headquarters for their trucking startup Transfix.
Transfix, which was founded in 2013, is an app that connects truck drivers to shipping companies. McElroy said that, in order for the company to flourish, they needed the best people in both logistics and technology – people who know how the trucking industry works, as well as the best data scientists and engineers.
Many new companies in the logistics space, McElroy said, don't prioritise that blend.
McElroy said his decade in the logistics space combined with the engineering expertise of his co-founder Salama, a programmer who was previously at Gilt.com and Microsoft, sets Transfix apart from other startups.
Courtesy of TransfixTransfix co-founders Jonathan Salama and Drew McElroy.
In order to be somewhere where they could continue to attract the best in logistics and engineering, they would have to be strategic in where they located their offices. "What is absolutely critical is to get the best of everybody," McElroy said.
Locating in the Midwest or Southeast would be ideal for finding logistics talent. And, it's cheaper to operate there than in coastal hubs like New York or San Francisco. The median base salary for a software engineer in New York City is $US100,000, according to LinkedIn Salary. In Indianapolis, for comparison, the median pay is $US72,700.
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Other logistics startups have followed suit in keeping it coastal. Convoy, another freight brokerage app, is based in Seattle. Silicon Valley, meanwhile, is home to Trucker Path,Peloton Technology,Terminal 49, and Otto.


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text:
Maria Scheepers van Dommelen (17 November 1892 - 1989) was a Belgian pianist who arranged works and premiered several concerti for the Hans piano. She also performed with the Belgian Vocal Trio and arranged music for it. She used the pseudonym Mit Scapus.

Scheepers was born in Antwerp and lived there her entire life. She studied at the Royal Conservatory of Antwerp with August De Boeck. As a concert pianist, she presented many concerts with pianist Flore Levine-Cousyns. She performed with the Belgian Vocal Trio with Roitel and Tolkowsky, and arranged over 60 songs for the trio. She also served as president of the Concerts de Midi d'Anvers.

In 1926, Pierre Hans commissioned August De Boeck to compose a concerto for the Hans piano. Hans was an engineer with very thick fingers, who had asked the French firm Pleyel to build a piano he designed with an upper keyboard and a lower keyboard tuned a half tone apart.  Scheepers created the solo Hans piano part for De Boeck's concerto and premiered it. She also premiered Hans piano concerti composed by Ernest d'Agrèves, René Barbier, Pierre Hans,  and Carl Smulders. She taught Hans piano courses at conservatories in Belgium, France, Germany, Luxembourg and the Netherlands, and transcribed pieces for regular piano so they could be played on the Hans piano. Her manuscript for the De Boeck concerto is archived at the Letterenhuis in Belgium. The Hans piano was very expensive to build and fell out of use after World War II.

References

Belgian pianists
Belgian music educators
Music arrangers
1892 births
1989 deaths
Pseudonymous artists

redpajama_set_name: RedPajamaWikipedia


Donald Trump on Tuesday is scheduled to address the United Nations General Assembly. Climate change is expected to be high on the agenda at this year's gathering. Another major storm—Hurricane Maria—is gaining strength in the Caribbean and following a similar path as Hurricane Irma.
Donald Trump on Tuesday is scheduled to address the United Nations General Assembly. Climate change is expected to be high on the agenda at this year's gathering. As the world leaders meet, another major storm—Hurricane Maria—is gaining strength in the Caribbean and following a similar path as Hurricane Irma. The current forecast shows Maria could hit Puerto Rico as a Category 4 storm as early as Wednesday. The U.S. Virgin Islands, which were devastated by Irma, also appear to be in line to be hit by Maria. Meanwhile, The Wall Street Journal reported over the weekend that the Trump administration is considering staying in the Paris climate agreement, just months after the president vowed to pull out of it. The White House denied the report. Secretary of State Rex Tillerson on Sunday signaled Trump may back away from the Paris accord, but National Security Adviser H.R. McMaster gave a different message on Fox News Sunday.
Houston Mayor Sylvester Turner has tapped the former head of U.S. operations for oil giant Shell to lead Houston's post-Hurricane Harvey recovery effort. Marvin Odum was the chair of Shell for eight years. He retired in 2016. Hurricane Harvey killed at least 82 people, flooded thousands of homes and destroyed billions of dollars of property. It also caused widespread environmental contamination, triggering a half-million-gallon gasoline spill and the release of up to 5 million pounds of pollutants into the air.
Last week, Vermont independent Senator Bernie Sanders introduced a bill that would provide universal healthcare by expanding Medicare to include every American. Sanders introduced the bill flanked by doctors, nurses and some of the bill's 15 Democratic co-sponsors.


text:
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If you're looking for a quiet setting that has the comforts of a hotel at the prices of a hostel, then this is a great option.
Djordja Rajkovica 28 , Novi Sad Serbia
Reviews, Photos, & Prices
A good hostel for solo travellers, couples, and small groups.
Overall Rating: 87%
Hostel & Cafe Bar Rookies is another favorite hostel in Novi Sad. It's located in the middle of the city on Jevrejska Street and is within walking distance to several popular attractions. The surrounding area has many restaurants, bars, and shopping opportunities. There's also a lively nightlife scene nearby.
This is a charming and hospitable place to stay where you can relax after a busy day or night. There's an on-site bar that offers affordable drinks as well. The hostel also offers free parking, free wi-fi access, a welcome drink, and all kinds of travel information. They also organize tours to Fruska Gora Monasteries and Sremski Karlovci Wine Tasting.
The hostel has both private rooms and dorms available. Private rooms are either doubles or two bed apartments. Dorms sleep three, five, or six people.
Jevrejska 13 , Novi Sad Serbia
Dorm Bed: $12.72
Private Room: $15.27
City Hostel is located in the city center of Novi Sad. Despite its ideal location near the university and sports center, it's still in a quiet area. There are also many great restaurants and shops nearby. The hostel is modern, clean, and secure, and the staff are friendly and welcoming. You'll receive a free welcome drink on arrival and there is free wi-fi throughout the hostel. There is also public parking nearby.
The hostel has eight rooms that are spread across three floors. There are private doubles and ten bed dorms that make up a total of 51 beds. Each floor has its own bathrooms and there's a kitchen and dining are which guests can use. Many guests enjoy relaxing in the common areas that are found on each floor. There are televisions, movies, and video games that guests can use and there's also free wi-fi throughout the hostel.
This is a relaxing and fun place to stay where it's relatively easy to meet other guests. Whether you're traveling alone or as part of a group, you'll quickly feel right at home here.
Radnicka 21 , Novi Sad Serbia
Lazin Hostel is another popular place to stay for budget travelers. It's located in the heart of the city near the pedestrian zone and is near many restaurants and bars. Nearby you'll find the River Danube, the Cathedral, Danube Park, and many musuems and churches. The Petrovaradin Fortress is about a fifteen minute walk away.
The hostel has many great amenities including a free breakfast with filling food, wi-fi throughout the building, security lockers, luggage storage, and a full kitchen which guests can use. The hostel has twin and private rooms as well as apartments with four, six, and eight beds. There's common area in the hostel with a television where many guests like to hang out and listen to music. It's the perfect place to socialize or meet other travelers to head out on the town with.
Laze Teleckog 10 , Novi Sad Serbia
Check out other places to stay in amazing destinations around the world.
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text:
Curd Gustav Andreas Gottlieb Franz Jürgens (13 de diciembre de 1915 - 18 de junio de 1982) fue un actor alemán que tuvo cierta relación parental alemán-francés. En idioma inglés aparece generalmente el nombre sin diéresis como Curt Jurgens. En el año 1945 Jürgens tomo la ciudadanía austriaca.
Está enterrado en el Cementerio Central de Viena (Grupo 32 C, Nr. 54).

Obra
Curd Jürgens nació en Solln región de Baviera (Alemania). Comenzó su carrera trabajando como periodista antes de hacer de representante de la que sería su esposa, la actriz Lulu Basler.

Pasó la mayor parte de su carrera cinematográfica temprana en los estudios que había en la ciudad de Viena. Su carrera incluye varias películas europeas y americanas. Tuvo un papel en la saga James Bond, concretamente en la película The Spy Who Loved Me (La espía que me amó), y también en el polémico éxito Y Dios creó a la mujer, que supuso el lanzamiento de Brigitte Bardot como estrella internacional. Jürgens realizó después una gran cantidad de participaciones como actor secundario. En 1956, en la película "Miguel Strogoff el Correo del Zar" encarnó al protagonista de la novela de Julio Verne y en 1961 repitió papel protagonista en "El triunfo de Miguel Strogoff"

Curd Jürgens como actor de teatro

 1935	en el Metropoltheater de Dresde.
 1936–37 en el Berliner Theater cerca del Kurfürstendamm.
 1938–41 en el Volkstheater en Viena.
 1940–53 así como en el periodo 1965-68 en el Burgtheater de Viena; Hizo su debut el 30 de noviembre de 1940 como Benvolio en la obra de teatro de Shakespeare Romeo und Julia (Dirección Lothar Müthel, dirección artística Rochus Gliese); su última premier fue en 1966 como Galileo Galilei en Das Leben des Galilei de Bertolt Brecht (Dirección Kurt Meisel, Diseñod Lois Egg, Erni Kniepert).
 1973–77 actuó en el Salzburger Festspielen en el papel de Jedermann de Hugo von Hofmannsthal (Dirección Ernst Haeusserman).
 1979 en el vienés Theater in der Josefstadt como Sigmund Freud en Berggasse 19 de Henry Denker (Dirección Haeusserman, Diseño Gottfried Neumann-Spallart).
 1980 última actuación en una tournee en Japón con la Wiener Staatsoper haciendo el papel de Bassa Selim en Die Entführung aus dem Serail de Wolfgang Amadeus Mozart (Director Karl Böhm).

Curd Jürgens en televisión
Actuó en series de televisión alemanas y austriacas:
 1968 Serie "Babeck"
 1972 Serie "Der Kommissar: Der Traum eines Wahnsinnigen"
 1973 Serie "Der Kommissar: Ein Mädchen nachts auf der Straße"
 1973 TV-Film "Collin", con la introducción de Stefan Heym
 1975 Serie "Derrick: Madeira"
 1978 Serie "Tatort: Rot, rot, tot"
 1982 Serie "Smileys People - Dame, König, As, Spion"

Curd Jürgens como actor vocal
Puso en dos ocasiones su voz:
 Richard Basehart (Entscheidung vor Morgengrauen)
 George Sanders (Der schwarze Jack)

Literatura
 Curd Jürgens: "... und kein bißchen weise", 1976 (novela autobiográfica), ISBN 3-85886-054-9

Premios y distinciones

Festival Internacional de Cine de Venecia

Referencias

Enlaces externos

 Curd Jürgens at Find-A-Grave

 Breve biografía acerca del autor
 Prisma En línea - Descripción de películas del actor

Actores de cine de Austria
Actores de televisión de Austria
Actores de teatro de Austria
Actores de cine de Alemania
Actores de televisión de Alemania
Actores de teatro de Alemania
Actores de voz de Alemania
Fallecidos por infarto agudo de miocardio
Fallecidos en Viena


Canadian Imperial Bank has 44646 employees and is headquartered in Canada.
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TransCanada Corp is an energy infrastructure company. Its business segments include, Natural Gas Pipelines, Liquid Pipelines and Energy. The company has pipeline and power generation assets in Canada, the United States, and Mexico.
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Dollarama Inc operates dollar stores in Canada that sell all items for $4 or less. The Company maintains retail operations in every Canadian province.
Bank of Nova Scotia has 89755 employees and is headquartered in Canada.


text:
Bij cyclovoltammetrie wordt door middel van een potentiostaat het potentiaalverschil tussen twee elektroden in een oplossing gevarieerd van laag naar hoog en terug.Het potentiaalverschil wordt aangelegd tussen de meet-elektrode en een referentie-elektrode. De oplossing wordt niet geroerd en de potentiaal wordt met constante snelheid gevarieerd. Typisch ontstaat er een gesloten curve met twee pieken: een anodische piek voor de oxidatie-reactie en een kathodische piek voor de reductie-reactie.

Gedurende de eerste fase gaat de elektrodepotentiaal omhoog (het anodische traject).
In het begin is de stroom relatief laag. Deze stroom ontstaat door opladingseffecten aan het elektrode-oppervlak (zoals bij een condensator) en door reactie van onzuiverheden.
Vervolgens wordt de redoxpotentiaal van de opgeloste stof bereikt, waardoor deze gaat reageren. Hierdoor neemt de (anodische) stroom toe.
De opgeloste stof, die een reductor moet zijn (bijvoorbeeld Fe2+), wordt geoxideerd. Hierbij ontstaat de oxidator-vorm van deze stof (Fe3+).
De stroom neemt vervolgens af, want de reagerende stof raakt op. Omdat de oplossing namelijk niet geroerd wordt, kan enkel datgene reageren wat door diffusie (volgens de Wet van Fick) het elektrode-oppervlak bereikt. Er ontstaat een (anodische) piek Epa.

Gedurende de tweede fase, na het omkeerpunt, gaat de elektrodepotentiaal omlaag (het kathodische traject).
Indien de redoxpotentiaal wordt bereikt van de oxidator-vorm van de opgeloste stof (bijvoorbeeld Fe3+ dat in de eerste fase is ontstaan en waarvan de deeltjes zich nog dicht bij de elektrode bevinden omdat de oplossing niet geroerd wordt), gaat deze reageren en neemt de (kathodische) stroom toe.
De opgeloste stof wordt gereduceerd, waarbij de oorspronkelijke reductor-vorm van de stof weer wordt teruggevormd (Fe2+).
Ook nu neemt de stroom vervolgens weer af, omdat de reagerende stof op raakt. Er ontstaat een (kathodische) piek Epk.

Bij de volgende cyclus, dat wil zeggen indien het gehele proces wordt herhaald, ontstaan de twee bovengenoemde pieken opnieuw.

Toepassingen
Een cyclovoltammogram heeft een sterk diagnostisch karakter. Naast het bepalen van de evenwichtspotentiaal van een redoxkoppel, kan uit het potentiaalverschil (Epa - Epk) tussen de anodische en kathodische piek worden afgeleid, in hoeverre de opgeloste stof reversibel (omkeerbaar) reageert. Een volledig reversibel redoxkoppel met één elektron in de halfreactie geeft namelijk een theoretisch potentiaalverschil tussen de pieken van 59 mV.

Cyclovoltammetrie wordt in elektrochemisch wetenschappelijk onderzoek zeer veel gebruikt. Doordat het technisch mogelijk is om zeer kleine stromen te meten, is het een gevoelige techniek, die veel informatie kan opleveren. Zo heeft een zuivere platina-elektrode een karakteristiek cyclovoltammogram, waarin in het lage potentiaalgebied de pieken zijn te zien die worden toegeschreven aan de adsorptie en desorptie van waterstofatomen aan het platina-oppervlak.

Elektrochemie


Pentagram Partners Marina Willer and Naresh Ramchandani are challenging you to create a piece of compelling communication for the Dutch digital rights foundation Bits of Freedom. Using their backgrounds in graphic design and advertising, Marina and Naresh will guide this collaborative session, putting forward examples of compelling communication for the social good, exploring potential themes for Bits of Freedom and working with you to develop your ideas.
Bits of Freedom is the leading digital rights organization in the Netherlands, focusing on privacy and freedom of communication online. Working at the cutting edge of technology and law, Bits of Freedom strives to influence legislation and self-regulation, and empower citizens and users by advancing the awareness, use, and development of freedom-enhancing technologies.
You'll be asked to break into groups to develop communication ideas that will promote the importance of privacy and freedom of speech in the digital age. And, you'll be asked to present your work back to the group and to Bits of Freedom themselves, in a supportive and collaborative share.
Come away from this workshop with a greater knowledge of how to create compelling communication for causes that matter.


text:
Egypt is studying tests for Corona patients arriving from Saudi Arabia
The Egyptian Minister of Health, Hala Zayed, announced that the ministry is now analyzing infections with the Corona virus coming from Saudi Arabia, to discover what the new imported strain is.
With regard to the anti-Corona vaccine, she added that the Council of Ministers authorized the Ministers of Health and Finance to sign an agreement with the International Vaccine Alliance, and the agreement was signed on December 4, and that there are priorities in the shipments and quantities that each country will receive.
She emphasized that every shipment arriving in Egypt cannot be vaccinated the next day, because it undergoes 4 experiments before starting vaccination, and vaccination centers have been designed, and hospital workers will be chosen to register and administer doses to them, and follow them up during the period between the two vaccinations.
Source: Al Shorouk
A Gift from Adversity: Overcoming Sexual Abuse, Domestic Violence, Bullying, and Homelessness
A 90-year-old woman is the first to receive the Corona vaccination in Switzerland


Time marches towards the inevitable, and the side result is, I'm getting damn old.
Okay, okay, I am exaggerating.. slightly. I'm not ancient yet. I'm in that baby-boomer-shaking-a-fist-at group known as millennials. (Something something poor, something something avocado toast.) But I constantly look around and go "I don't get that. Why don't I get that?" and the answer is just that I'm now too old to get that. What things in particular make me feel that way?
– "On fleek." No matter how hard I try, I don't understand what that means. And I get a lot of the lingo, still. Fam, lit, thicc, etc. I'm pretty internet savvy and I've always had good reading comprehension so in general, I grok the meanings of slang. But on fleek? I still can't figure it out. What is fleek?? Why fleek? I don't know. Maybe I could google it and figure it out, but I think that would make me even older.
– All those hashtags. I get hashtags as a concept, obviously, and I use a handful of them in my instagram posts too. In general, they are basically a keyword organizing system. Useful. But why on earth do people use, like, 20 hashtags in one post? Why?? At some point you're not efficiently organizing stuff, you're just blasting words until 78.4% of your post is hashtags. Does nobody else find this weird? I mean, you do you, kids. I'll just be sticking to my modest, 2-4 encompassing hashtags.
– Burping in public. Last year, I worked with a group that included a lot of people in their early 20s. And while working with them, I heard more unrestrained, let-loose burps than in my entire previous existence. Nobody seemed particularly embarrassed to burp in front of all their coworkers, and nobody ever said "excuse me." They just let loose with burp after burp. You might think it was just that random group of 20-somethings with no sense of public decorum, but no. After I left that job, I still noticed young people in that age range around me burping, in public, with no apologies or attempts to restrain it. ?! Obviously burps are a natural body function, but you can usually keep it under control when in polite company, like at work. You don't normally just open your mouth wide and let it fly unimpeded, then keep going with your sentence as if nothing happened. I mean, unless you're a young person today, I guess.
I'm sure I could keep going. But it is a singularly weird feeling to look around and realize you're not a part of the young, trendsetting generation anymore. You're yesterday's news.
Well, I've depressed myself. I'm going to go eat some avocado toast.


text:
Q: Как разделить строку Python В переменной chess мы получаем какой-то любой фрагмент шахматной партии.
Например:
chess = '1. d2 e6 2. e4 d5 3. Кc3 c5 4. Кf3 Кc6 5. e:d5 e:d5 6. Сe2 Кf6 7. O-O Сe7 8. Сg5 O-O 9. d:c5 Сe6 10. Кd4 С:c5 11. Кb3 Сe7 12. Сf3 Кe5 13. Лe1 К:f3+ 14. Ф:f3 Лc8 15. h3 h6'

Как можно разделить строку чтобы распечатать ход первой партии? Мне нужно разделить все партии чтобы выглядело так:
['1. d2 e6', '2. e4 d5', '3. Кc3 c5', .... ]

A: попробуйте так:
def f(chess):
    chess = chess.split()
    return [" ".join(chess[i:i+3]) for i in range(0, len(chess), 3)]

chess = '1. d2 e6 2. e4 d5 3. Кc3 c5 4. Кf3 Кc6 5. e:d5 e:d5 6. Сe2 Кf6 7. O-O Сe7 8. Сg5 O-O 9. d:c5 Сe6 10. Кd4 С:c5 11. Кb3 Сe7 12. Сf3 Кe5 13. Лe1 К:f3+ 14. Ф:f3 Лc8 15. h3 h6'
print(f(chess))

A: import re
re.split(r'\s+?\b(?=\d+\.)', chess)

['1. d2 e6',
 '2. e4 d5',
 '3. Кc3 c5',
...

redpajama_set_name: RedPajamaStackExchange


What do you get for your $35 SCLA dues?
The Association needs every one of our residents' support to help maintain Sunset Canyon as a wonderful place to live. $35 per year is a bargain.
Owners can request a list of all unpaid-dues/fines/liens etc. here.
Homeowners behind in their dues can get help here.


text:
VOL. 37 | NO. 27 | Friday, July 5, 2013
House Republicans grapple with immigration
WASHINGTON (AP) — House Republicans on Wednesday confronted the politically volatile issue of immigration, their ranks divided and their way forward unclear even as national GOP leaders pressured them to act.
The latest prominent Republican to wade into the debate was former President George W. Bush, who urged Congress to reach a "positive resolution" on overhauling U.S. immigration laws, a goal that eluded him during his presidency. His comments suggested a need for Republicans to deal with immigration in a broad way, though he avoided specifics during brief remarks at a naturalization ceremony at his presidential library in Dallas, and he didn't directly endorse a comprehensive Senate-approved plan.
"We can uphold our tradition of assimilating immigrants and honoring our heritage of our nation built on the rule of law. But we have a problem. The laws governing the immigration system aren't working; the system is broken," Bush said.
At the White House, President Barack Obama met with members of the all-Democratic Congressional Hispanic Caucus, as the fate of one of his top second-term priorities rested in the hands of the restive House GOP.
Said presidential press secretary Jay Carney, "It's the moral thing to do. We'll keep at it."
Republican lawmakers were convening a special meeting Wednesday afternoon to try to work out a summer strategy following Senate passage late last month of a far-reaching bill. The Senate measure would spend tens of billions on border security, create new legal avenues for workers to come to the U.S., require employers to verify their workers' legal status and establish a path to possible eventual citizenship for the estimated 11 million already here illegally.
The calculus in the Republican-controlled House may be more complex and daunting.
Many of the conservatives who wield power in the House are in districts with few Hispanic voters and are thus insulated from much of the pressure to act on immigration. Speaker John Boehner, R-Ohio, already has rejected the idea of bringing the Senate bill to the House floor. He has pledged that no legislation will move without the support of a majority of his Republicans.
Like many in his conference, Boehner has said border security must come first. And many Republicans prefer a piecemeal, step-by-step approach rather than a single big bill like the one the Senate passed.
But for many, the most vexing issue is what to do about those who are already in the U.S. illegally.
The Senate bill offers a 13-year path for most, contingent on paying fines, learning English and meeting other qualifications. Agriculture workers and people brought to the United States as youths would have a faster route.
In the House, most Republicans are reluctant to endorse citizenship for 11 million unauthorized immigrants, but also shy away from suggestions of deportation.
Ahead of Wednesday's meeting, many lawmakers seemed to be gravitating toward supporting legal status of some kind for millions here illegally. But exactly what and how were far from clear.
For some, a guest worker status would be as far as it goes, while others left open the possibility that once they're in the country legally, immigrants eventually could attain citizenship through existing channels of family or employer sponsorship. Still others were focused on citizenship for people brought to the country as youths, military veterans and perhaps others who've lived in the country for years and proven their contributions to society.
"I wouldn't prohibit forever" people from getting citizenship, said Rep. James Lankford, R-Okla. "I'm a Christian, and restitution and reconciliation's a big deal. If you do something illegal or inappropriate you should be able to resolve that, face the penalty, clear it and be forgiven."
GOP presidential candidate Mitt Romney fared abysmally with Hispanic and Asian voters last year after suggesting that people in the country illegally could "self-deport." Such suggestions have been heard rarely among Republicans since Romney's loss. But there is a hardcore group in the House that opposes any legal status for people here illegally.
"I'm not going to support any kind of legalization because legalization is amnesty, is eventual citizenship if not instantaneous citizenship, and if we do that we get more law breakers," Rep. Steve King, R-Iowa, said.
If House Republicans do embrace something short of citizenship, it's not clear Democrats would go along. Republicans control 234 House seats and Democrats 201. Passing legislation requires a majority vote of 218 if all members are voting. Passing immigration legislation is likely to require some Democratic votes, and Democrats insisted Tuesday that nothing but a path to citizenship would suffice.
"America has stood for citizenship," Sen. Chuck Schumer, D-N.Y., said. "We have a Statue of Liberty here. It never has said you come here and you'll be second class. We will not stand for it. It will not happen."
Obama also has said he would not sign a bill without a path to citizenship.
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Want to have your cordwood cake and eat it too? Building a cordwood garage with living quarters is a excellent way to practice your cordwood technique & tuckpointing. In addition it provides a place to lay your weary head after a hard days work. The garage (aka Carriage House) has a room-in-the-attic truss. It allows for a 400 sq. ft. living space in the attic. Water was plumbed into the upstairs, as well as electricity. The roof pitch is 8/12. The stackwall corner posts are built at the same time as the post and beam framework. Then the roof is applied and braced. Finally, the cordwood is infilled. The stackwall corners are a old fashioned way to build with cordwood, but the owner learned a new way to make them so they functioned as a post and allowed the roof to be put on ahead of time. This is the lake home that was built next to the Carriage House in central Minnesota. The building inspector/code official requested that pressure treated lumber be used on the exterior framing. 150 year old barn timbers from Janesville, Wisconsin were used for the interior. An enamel Vermont Casting wood stove provides heat. (Below)Another look at the framing, the timbers and the stackwall corners. The lake is in the background.
This wood carving would have made a nice corner post, but it would have been very difficult to tuck point.
Below are some current photos of the Carriage House. (Below) Matt & Carrie built a similar room-in-the-attic two and a half car garage in Wisconsin. They are very pleased with the upstairs living space. Carrie is an architect, so she had a leg up with exterior and interior design.