text:
\section{Introduction}
The booming study of exoplanets allow us to assess the diversity of the planetary
systems of the Milky Way and to put our own solar system in perspective. Notably,
ground-based  transit surveys targeting relatively bright ($V<13$) stars are detecting
at an increasing rate  short-period giant planets amenable for a thorough characterization
(orbit, structure, atmosphere), thanks to the brightness of their host star, the favorable
planet-star size ratio and their high stellar irradiation (e.g. Winn 2010).  With its very high detection
efficiency, the WASP transit survey (Pollacco et al. 2006) is one of the most productive
projects in that domain.

In this context, we report here the detection by WASP of two new giant planets,
 WASP-64\,b and WASP-72\,b, transiting relatively bright Southern stars.
 Section~2 presents the WASP discovery photometry, and  high-precision
 follow-up observations  obtained from La Silla ESO Observatory (Chile) by the TRAPPIST and
 {\it Euler} telescopes to confirm the transits and planetary nature of both objects and to
 determine precisely the systems parameters. In Sect.~3, we present the spectroscopic
 determination of the stellar properties and the derivation of the systems parameters  through
 a combined analysis of the follow-up photometric and spectroscopic time-series.
Finally, we discuss our results in Sect.~4.

\section{Observations}

\subsection{WASP transit detection photometry}

The stars 1SWASPJ064427.63-325130.4 (WASP-64; $V$=12.3, $K$=11.0)
and 1SWASPJ024409.60-301008.5 (WASP-72; $V$=10.1, $K$=9.6)
 were observed by the Southern station of the WASP survey (Hellier et al. 2011)
 between 2006 Oct 11 and 2010 Mar 12 and between 2006 Aug 11 and 2007
 Dec 31, respectively. The 17981 and 6500 pipeline-processed photometric
 measurements were detrended and  searched for transits using the  methods
  described by Collier-Cameron et al. (2006). The selection process
  (Collier-Cameron et al. 2007) identified WASP-72 as a  high priority
  candidate  showing periodic low-amplitude (2-3 mmag) transit-like signatures
   with period of  2.217~days. For WASP-64, similar transit-like signals with a period of
   1.573~days were also detected,  not only on the target itself but also on a brighter star at 28'',
   1SWASPJ064429.53--325129.5 (TYC7091-1288-1, $V$=12.3, $K$=11.0).   Fig.~1 presents for
TYC7091-1288-1 and WASP-64  the WASP photometry folded on the deduced transit ephemeris.
Fig.~2 does the same for WASP-72.

A search for periodic modulation was  applied to the photometry of
WASP-72, using for this purpose the method described in
 Maxted et al. (2011). No periodic signal was found down to the mmag amplitude.
  We did not perform such a  search for TYC7091-1288-1 and WASP-64, as these two
 stars  are blended together at the spatial resolution of the WASP instrument (see below).
 Still, a Lomb-Scargle periodogram analysis of their photometric time-series did
 not reveal any significant power excess.

\subsection{Follow-up photometry}

\subsubsection{WASP-64}

WASP-64 is at 28'' West from TYC7091-1288-1, close
 enough to have most of its point-spread function (PSF) enclosed in the smallest
 of the WASP photometry extraction apertures (radius=34'', see Fig.~3).
Both objects have an entry in the WASP database,  because it is based
 on an input catalogue of star positions. Still, the WASP light curve obtained with an
 aperture centered on WASP-64 is of poorer quality (see Fig.~1), because the centering algorithm
 does not work optimally  when there is a bright object off-centre in the aperture or
  just outside of it,  while significant levels of red noise are brought by PSF variations. This
  explains why the transit was first detected from the photometry centered on TYC7091-1288-1.
Having both stars nearly totally enclosed in the smallest apertures for both centerings prevented us to decide
from the WASP photometry alone  if the eclipse signal detected by WASP was originating  from
 one or the other star, so our first follow-up action was to measure on 2011 Jan 20 a transit at a
 better spatial resolution with the robotic 60cm telescope TRAPPIST ({\it TRA}nsiting
{\it P}lanets and {\it P}lanetes{\it I}mals {\it S}mall {\it T}elescope; Gillon et al. 2011,
Jehin et al. 2011) located at ESO La Silla Observatory in the Atacama Desert, Chile.
TRAPPIST is equipped with a thermoelectrically-cooled 2K\,$\times$\,2K CCD having
 a pixel scale of 0.65'' that translates into a 22'\,$\times$\,22'  field of view. Differential
 photometry was obtained with TRAPPIST for both stars on the night of 2011 Jan 20,
 corresponding to a transit window as derived from WASP data. These observations
 were obtained with the telescope focused and through a special `$I+z$' filter that has a
transmittance $>$90\% from 750 nm to beyond
1100 nm\footnote{http://www.astrodon.com/products/filters/near-infrared/}.
The positions of the stars on the chip were maintained to within a few pixels over the course of the run,
thanks to a `software guiding' system deriving
regularly  an astrometric solution for the most recently acquired image and sending
 pointing corrections to the mount if needed.  After a standard pre-reduction (bias, dark,
 flatfield correction), the stellar fluxes were extracted from the images using the {\tt IRAF/DAOPHOT}\footnote{{\tt IRAF} is
 distributed by the National Optical Astronomy Observatory, which is
 operated by the Association of Universities for Research in Astronomy, Inc., under cooperative agreement
  with the National Science Foundation.} aperture photometry software (Stetson,
 1987). Several sets of reduction parameters were tested, and we kept the one giving the
 most precise photometry for the stars of similar brightness as the target. After a careful
  selection of a set of 22 reference stars, differential photometry was then obtained.  This reduction
  procedure was also applied for the subsequent TRAPPIST runs.

 This first TRAPPIST run resulted in a flat light curve for TYC7091-1288-1,
 while the light curve for WASP-64 showed a clear  transit-like structure (Fig.~3), identifying thus
WASP-64 as the source of the transit signal. A second (partial) transit was observed in the
 $I+z$ filter on 2011 Feb 22 to better constrain  the shape of the eclipse (Fig.~4, second light
  curve from the top). As for the following WASP-64 transits, the telescope was defocused
  to $\sim$3'' to improve the duty cycle and average the pixel-to-pixel effects. A global analysis
  of the two first TRAPPIST  transit light curves led to an eclipse depth and shape compatible
 with the transit of a giant planet in front of a solar-type star.  Our next action was to observe
 a third transit with TRAPPIST, this time in the $V$ filter to assess the chromaticity of the
 transit depth (Fig.~4, third light curve from the top). The analysis of the resulting light curve
 led to a transit depth consistent with the one measured in the $I+z$ filter, as expected for a
 transiting planet. We then observed an $occultation$ window in the $z'$-band on 2011 Apr 30.
 We could not detect any eclipse in the resulting photometric time-series (Fig.~5), which was again
  consistent with the transiting planet scenario. At this stage, we began our spectroscopic
 follow-up of WASP-64 that confirmed the solar-type nature of WASP-64 and the planetary nature
  of its eclipsing companion (see Sec. 2.3).

Once the planetary nature of WASP-64\,b was confirmed, we observed seven more of its transits with
TRAPPIST, using then a blue-blocking filter\footnote{http://www.astrodon.com/products/filters/exoplanet/}
that has a transmittance  $>$90\% from 500 nm to beyond 1000 nm.  The goal of using this very
wide red filter is to maximize the signal-to-noise ratio (S/N) while minimizing the influence of
 moonlight pollution, differential extinction and stellar limb-darkening on the transit light curves.
 The resulting light curves are shown in Fig.~4.
The transit of 2011 Oct 19 was also observed in the Gunn-$r$ filter with the EulerCam CCD camera
at the 1.2-m {\it Euler} Telescope at La Silla Observatory. This nitrogen-cooled camera has a
4k\,$\times$\,4k E2V CCD with a 15'\,$\times$\,15'  field of view  (scale=0.23"/pixel). Here too,
a defocus was applied to the telescope to optimize the observation efficiency and minimize
pixel-to-pixel effects, while flat-field effects were further reduced by keeping the stars on the same
pixels, thanks to a `software guiding' system similar to the one of TRAPPIST (Lendl et al. 2012).
The reduction was similar to that performed on TRAPPIST data. The resulting light curve is also
shown in Fig.~4.

\subsubsection{WASP-72}

We monitored for WASP-72 five transits with TRAPPIST (see Table 1 and Fig.~6),  two partial and
 two full transits in the $I+z$ filter and one full transit in the blue-blocking filter. For the three transits
  observed in 2011, the telescope was defocused to $\sim$3''.  A first partial transit was observed in
  2011 Jan 21 in the $I+z$ filter at high airmass, confirming the low-amplitude eclipse detected by
  WASP (Fig.~6, first light curve from the top). The next season, a full transit was observed on 2011
  Oct 25 in the blue-blocking filter. A technical problem damaged these data: a shutter  problem led to
  a scatter twice higher than expected.  In 2011,  a partial transit was also observed in the  $I+z$ filter on
  Dec 4.  In 2012, two new full transits were observed with TRAPPIST in the $I+z$ filter. For these two last
  runs, the telescope was kept focused to minimize the effects of a  focus drift problem with an amplitude
  stronger for out-of-focus observations. We are still investigating the origin of this technical problem.
  Two transits of WASP-72 were also observed with {\it Euler} on 2011 Nov 26 and 2012 Nov 16,  with the
  same strategy than for WASP-64. For the second {\it Euler} transit, a crash of the tracking system led to significant
  shifts of the stars on the detectors (up to 50 pixels), giving rise to significant systematic effects in the differential
  photometry (see Fig.~6)
\\
\\
Table 1 presents a summary of the follow-up photometric time-series obtained for WASP-64 and WASP-72.

\begin{figure}
\label{fig:wasp64+TYC}
\centering
\includegraphics[width=9cm]{f1.eps}
\caption{WASP photometry for TYC7091-1288-1 ($top$) and  WASP-64 ($bottom$)
folded on the best-fitting transit ephemeris from the transit search algorithm presented in Collier Cameron et al. (2006),
and binned per 0.01d intervals.}
\end{figure}

\begin{figure}
\label{fig:wasp72}
\centering
\includegraphics[width=9cm]{f2.eps}
\caption{WASP photometry for WASP-72
folded on the best-fitting transit ephemeris from the transit search algorithm presented in Collier Cameron et al. (2006),
and binned per 0.01d intervals.}
\end{figure}

\begin{figure*}
\label{fig:w64ima}
\centering
\includegraphics[width=18cm]{f3.eps}
\caption{280''$\times$280'' TRAPPIST $I+z$ image centered on TYC7091-1288-1. North is up and East is left.
The three concentric circles indicate the three photometry extraction apertures used in the WASP pipeline.
WASP-64 is  the closest star to the right of TYC7091-1288-1. For both stars, the light curve
obtained by TRAPPIST on 2011 Jan 20 is shown (cyan=unbinned, black=binned per intervals of
0.005d).
}
\end{figure*}

\begin{figure}
\label{fig:w64phot}
\centering
\includegraphics[width=9cm]{f4.eps}
\caption{Follow-up transit photometry for WASP-64\,b.  For
each light curve, the best-fit transit+baseline model deduced from the global analysis is superimposed
(see Sec. 3.2). The light curves are shifted along the $y$-axis for clarity.  BB = Blue-blocking filter.}
\end{figure}

\begin{figure}
\label{fig:w64occ}
\centering
\includegraphics[width=8.5cm]{f5.ps}
\caption{TRAPPIST $z'$ time-series photometry obtained during an occultation window of WASP-64\,b, unbinned and
binned per intervals of 0.005d. An occultation model assuming a circular orbit and a depth of 0.5\% is superimposed
for comparison.  }
\end{figure}

\begin{figure}
\label{fig:w72phot}
\centering
\includegraphics[width=9cm]{f6.eps}
\caption{Follow-up transit photometry for WASP-72\,b. For each light curve, the best-fit
 transit+baseline model deduced from the global analysis is superimposed (see Sec. 3.2). The light curves
 are shifted along the $y$-axis for clarity.}
\end{figure}

\begin{table*}
\begin{center}
\begin{tabular}{cccccccc}
\hline
Target &      Night    & Telescope & Filter & $N$         & $T_{exp}$ &  Baseline function  & Eclipse\\
             &                   &                    &            &                 &       (s)           &                                  &  nature              \\ \hline \noalign {\smallskip}
WASP-64  &  2011 Jan 20-21 & TRAPPIST &  $I+z$ & 792   & 8  &  $p(t^2)+o$  & transit               \\ \noalign {\smallskip}
WASP-64  &  2011 Feb 22-23  & TRAPPIST &  $I+z$ & 296  & 20 &  $p(t^2)$   & transit                \\ \noalign {\smallskip}
WASP-64   &  2011 Apr 4-5    &  TRAPPIST   &  $V$ & 364   & 30   &  $p(t^2)$    &  transit   \\ \noalign {\smallskip}
WASP-64   &  2011 Apr 30 - May 1& TRAPPIST &     $z'$ & 202    &  40 & $p(t^2)$ &   occultation              \\ \noalign {\smallskip}
WASP-64  & 2011 Oct 19-20   & TRAPPIST & BB &   578 &  15  &  $p(t^2)$  &   transit                \\ \noalign {\smallskip}
WASP-64  & 2011 Oct 19-20   & {\it Euler} & Gunn-$r$ &   159 &  60  &  $p(t^2)$    &  transit                \\ \noalign {\smallskip}
WASP-64  & 2011 Oct 30-31   & TRAPPIST & BB  &    533    &     15     &        $p(t^2)$     &  transit        \\ \noalign {\smallskip}
WASP-64  & 2011 Nov 21-22   & TRAPPIST & BB  &   512     &   15   &  $p(t^2)+o$     & transit                  \\ \noalign {\smallskip}
WASP-64  & 2011 Nov 29-30   & TRAPPIST & BB  &    611    &    15          &        $p(t^2)$ &  transit        \\ \noalign {\smallskip}
WASP-64  & 2011 Dec 10-11   & TRAPPIST & BB  &  642    &   15    &    $p(t^2)+o$   & transit       \\ \noalign {\smallskip}
WASP-64 & 2011 Dec 21-22   & TRAPPIST & BB  &   566     & 15    &    $p(t^2)+o$ & transit   \\ \noalign {\smallskip}
WASP-64 & 2012 Jan 12-13   & TRAPPIST & BB  & 578       &     15    &        $p(t^2)$ &  transit        \\[0.33cm]
WASP-72 & 2011 Jan 21-22   & TRAPPIST & $I+z$  &  707      &        8          &     $p(t^2)$         & transit   \\ \noalign {\smallskip}
WASP-72 & 2011 Oct 25-26   & TRAPPIST & BB  &  2042      &   4     &  $p(t^2)+o$   & transit   \\ \noalign {\smallskip}
WASP-72 & 2011 Nov 25-26 & {\it Euler} & Gunn-$r$ & 294 & 40 & $p(t^2)+p(a^2)$ & transit \\ \noalign {\smallskip}
WASP-72 & 2011 Dec 4-5   & TRAPPIST & $I+z$ &  892      &       10           &   $p(t^2)+o$         & transit    \\ \noalign {\smallskip}
WASP-72 & 2012 Nov 16-17   & TRAPPIST & $I+z$ &  1344      &       6          &   $p(t^2)+o$         & transit    \\ \noalign {\smallskip}
WASP-72 & 2012 Nov 16-17   & {\it Euler} & Gunn-$r$ &  217     &       70          &   $p(t^2+xy^1)+o$      & transit    \\ \noalign {\smallskip}
WASP-72 & 2012 Dec 6-7   & TRAPPIST & $I+z$ &  1197     &       6           &   $p(t^2)+o$         & transit    \\ \noalign {\smallskip}
\hline
\end{tabular}
\caption{Summary of follow-up photometry obtained for WASP-64 and WASP-72. $N$=
number of measurements. $T_{exp}$ = exposure time. BB = blue-blocking
filter. The baseline functions are the analytical functions used to model the photometric baseline of each
light curve (see Sec. 3.2). $p(t^2)$ denotes a quadratic time polynomial, $p(a^2)$ a quadratic
airmass polynomial, $p(xy^1)$ a linear function of the stellar position on the detector, and $o$ an offset fixed at the time of
the meridian flip.}
\end{center}
\label{wasp64+72_trappist}
\end{table*}

\subsection{Spectroscopy and radial velocities}

Once WASP-64 and WASP-72 were identified as  high priority candidates, we gathered spectroscopic measurements
with the {\tt CORALIE} spectrograph mounted on {\it Euler} to confirm the planetary nature of the eclipsing bodies and
obtain mass measurements. 16 usable spectra were obtained for WASP-64 from 2011 May 2 to 2011 November 7
with an exposure time of 30 minutes. For WASP-72, 18 spectra were gathered from 2011 January 9 to 2011 December 29,
here too with an exposure time of 30 minutes.  For both stars, radial velocities  (RVs)  were computed by weighted cross-correlation
 (Baranne et al. 1996) with a numerical G2-spectral template giving close to optimal precisions for late-F to early-K dwarfs, from our
 experience.  The resulting RVs are shown in Table~2.

The RV time-series show variations that are  consistent with planetary-mass companions. Preliminary orbital analyses
of the RVs resulted in periods and phases in excellent agreement with those deduced from the WASP transit detections (Fig.~7 \& 8,
upper panels).  For WASP-64, assuming a stellar mass $M_{\ast} = 0.98 \pm 0.09$ $M_{\sun}$  (Sect.~3.1), the fitted semi-amplitude
$K = 212 \pm 17$ m\,s$^{-1}$ translates into a secondary mass slightly higher than Jupiter's, $M_p = 1.19 \pm 0.12$ $M_{\rm Jup}$.
The resulting orbital eccentricity is consistent with zero, $e = 0.05_{-0.03}^{+0.06}$. For WASP-72, assuming a stellar mass $M_{\ast} =
1.23 \pm 0.10$ $M_{\sun}$  (Sect.~3.1), the fitted semi-amplitude $K = 179 \pm 6$ m\,s$^{-1}$ translates into a secondary mass
$M_p = 1.31 \pm 0.08$ $M_{\rm Jup}$, while the deduced orbital eccentricity is also consistent with zero, $e = 0.05_{-0.03}^{+0.03}$.

A model with a slope is slightly favored in the case of WASP-72, its value being -82 $\pm$ 22 \mbox{m\,s$^{-1}$ }~per year. Indeed,
 the respective values for the Bayesian Information Criterion (BIC; Schwarz 1978)  led to likelihood ratios
 (Bayes factors) between 10 and 55 in favor of
 the slope model, depending if the orbit was assumed to be circular or not. Such  values for the
 Bayes factor are not high enough to be decisive,
 and more RVs will be needed to confirm this possible trend.

To confirm that  the RV signal originates well from planet-mass objects orbiting the stars,
we analyzed the {\tt CORALIE} cross-correlation functions (CCF) using the line-bisector technique described in Queloz et al (2001).
The bisector spans revealed to be stable, their standard deviation being close to their average error (57 $vs$ 47 \mbox{m\,s$^{-1}$ } for WASP-64 and
28 $vs$ 24 \mbox{m\,s$^{-1}$ } for WASP-72). No evidence for a correlation between the RVs and the bisector spans was found (Fig.~7 \& 8, lower panels),
 the slopes deduced from linear regression being $-0.02 \pm 0.08$ (WASP-64) and $-0.01 \pm 0.04$ (WASP-72). These values and errors
 makes any blend scenario very unlikely. Indeed, if the orbital signal of a putative blended eclipsing binary  (EB) is able to create a clear periodic
 wobble of the sum of both CCFs,  it should also create a significant periodic distortion of its shape, resulting  in correlated variations of
 RVs and bisector spans having the same order of magnitude (Torres et al. 2004). The power of this effect to identify blended EBs among transit
 candidates was first demonstrated by the classical case of  CSC 01944-02289 (Mandushev et al. 2005), for which the bisector spans
 varied in phase with the RVs and with an amplitude about twice lower.  Another famous case
 is the HD\,41004 system (Santos et al. 2002), with a K-dwarf blended with a M-dwarf companion
(separation $\sim$0.5'') which  is itself orbited by a short-period brown dwarf. For this extreme system, the RVs show a clear signal at the period
of the brown dwarf orbit (1.3 days) and with an amplitude $\sim 50$ \mbox{m\,s$^{-1}$ } that could be taken for the signal of a sub-Saturn mass planet
orbiting the K-dwarf, except that the slope of the bisector-RV relation is $0.67 \pm 0.03$, clearly revealing that the main spectral component
of the CCF is  not responsible for the observed signal. In the case of WASP-64 and 72, the 3-$\sigma$ upper limits of 0.23 and 0.09 that we derived
from Monte-Carlo simulations for the bisector-RV slopes combined with the much higher amplitude of the measured RV signals allow
us to confidently infer that  the RV signal is actually originating from the target stars.  This conclusion is strengthened by the consistency
of the solutions derived from the global analysis of our spectroscopic and photometric data (see next Section).
We conclude thus that the stars WASP-64 and
WASP-72 are transited by a giant planet  every $\sim$1.573 and $\sim$2.217 days, respectively. Of course,
 we cannot exclude that the light of those stars is not diluted by a well-aligned object able to bias our inferences about the planets.
 Still, our multicolor transit photometry showing no dependance of the transit depths on the wavelength, and  the absence of any
 detectable second spectra in the {\tt CORALIE}  data strongly disfavors any significant pollution of the light of the host stars.

\begin{figure}
\label{fig:rv}
\centering
\includegraphics[width=8.5cm]{f7.ps}
\includegraphics[width=8.5cm]{f8.ps}
\caption{$Top$: {\tt CORALIE} RVs for WASP-64 phase-folded on the best-fit orbital period, and with the best-fit
Keplerian model over-imposed. $Bottom$: correlation diagram CCF bisector spans $vs$ RV. The colors indicate the
measurement timings. }
\end{figure}

\begin{figure}
\label{fig:rv}
\centering
\includegraphics[width=8.5cm]{f9.ps}
\includegraphics[width=8.5cm]{f10.ps}
\caption{$Top$: {\tt CORALIE} RVs for WASP-72 phase-folded on the best-fit orbital period, and with the best-fit
Keplerian model over-imposed. $Bottom$: correlation diagram CCF bisector spans $vs$ RV. The colors indicate the
measurement timings. }
\end{figure}

\begin{table}
\begin{center}
\begin{tabular}{ccccc}
\hline
Target & $HJD_{TDB}$-2450000 & RV & $\sigma_{RV}$ & BS\\
 &  & (km~s$^{-1}$) & (m~s$^{-1}$) & (km~s$^{-1}$) \\ \hline \noalign {\smallskip}
WASP-64 & 5622.652685 & 33.1075 &  21.5 & 0.1171  \\ \noalign {\smallskip}
WASP-64 & 5629.582507 & 33.3234 & 19.8 & --0.0900  \\ \noalign {\smallskip}
WASP-64 & 5681.541466 & 33.3368 & 23.9 & --0.0601  \\ \noalign {\smallskip}
WASP-64 & 5696.488635 & 33.0326 & 24.3 & --0.0057   \\ \noalign {\smallskip}
WASP-64 & 5706.460152 & 33.4079 & 24.3 & --0.0156    \\ \noalign {\smallskip}
WASP-64 & 5707.460947 & 33.0038 & 28.0 & --0.0075  \\ \noalign {\smallskip}
WASP-64 & 5708.461813 & 33.2129 &  25.1 & --0.0169   \\ \noalign {\smallskip}
WASP-64 & 5711.463695 & 33.3160 & 26.3 & 0.0040  \\ \noalign {\smallskip}
WASP-64 & 5715.458133 & 33.1019 & 27.2 & --0.0645  \\ \noalign {\smallskip}
WASP-64 & 5716.463634 & 33.0977 & 26.1 & --0.0121  \\ \noalign {\smallskip}
WASP-64 & 5842.867334 & 33.0986 & 24.0 &  --0.0453  \\ \noalign {\smallskip}
WASP-64 & 5861.847564 & 33.1559 & 25.4  & 0.0061  \\ \noalign {\smallskip}
WASP-64 &  5864.795499 & 33.0230 & 18.1 &  --0.0346   \\ \noalign {\smallskip}
WASP-64 &  5869.724123 & 33.1725 & 20.6 & --0.0504  \\ \noalign {\smallskip}
WASP-64 & 5871.734734 & 33.4248 & 21.1 &  0.0752   \\ \noalign {\smallskip}
WASP-64 & 5872.762875 & 33.1044 & 20.1 &  0.0877   \\[0.33cm]
WASP-72 & 5570.618144 & 35.7945 & 13.3 &	0.0176    \\ \noalign {\smallskip}
WASP-72 & 5828.890931	 & 36.0233 & 11.3 & 0.0566     \\ \noalign {\smallskip}
WASP-72 & 5829.865219	 & 35.8029 & 9.8  &  0.0466      \\ \noalign {\smallskip}
WASP-72 & 5830.866138	 & 35.9320 & 11.5 & 0.0623      \\ \noalign {\smallskip}
WASP-72 & 5832.894502	 & 35.8391 & 14.6 & 0.0396	 \\ \noalign {\smallskip}
WASP-72 & 5852.780149	 & 35.7640 & 15.5 & 0.0092	\\ \noalign {\smallskip}
WASP-72 & 5856.757447	 & 35.7288 & 11.5 & 	0.0390	\\ \noalign {\smallskip}
WASP-72 & 5858.689011	 & 35.8146 & 15.2 &	--0.0198	\\ \noalign {\smallskip}
WASP-72 & 5863.800340	 & 35.7664 & 10.4 & 	0.0462	\\ \noalign {\smallskip}
WASP-72 & 5864.750293	 & 36.0695 & 10.0 & 0.0292	\\ \noalign {\smallskip}
WASP-72 & 5865.812141	 & 35.7283 & 11.9 & 0.0968	\\ \noalign {\smallskip}
WASP-72 & 5866.605265	 & 36.0331 & 10.6 & 	0.0734	\\ \noalign {\smallskip}
WASP-72 & 5867.628720	 & 35.7586 & 10.3 &	0.0605	\\ \noalign {\smallskip}
WASP-72 & 5868.759336	 & 35.9966 & 10.4 & --0.0019	\\ \noalign {\smallskip}
WASP-72 & 5873.808914	 & 35.9928 & 10.9 &	0.0368	\\ \noalign {\smallskip}
WASP-72 & 5886.748911	 & 36.0460 & 16.3 &  0.0624 \\ \noalign {\smallskip}
WASP-72 & 5914.700813	 & 35.7261  & 9.5 & 	0.0504	\\ \noalign {\smallskip}
WASP-72 & 5924.584434	 & 36.0624 & 10.0 &	0.0562	\\ \noalign {\smallskip}
\hline
\end{tabular}
\caption{{\tt CORALIE} radial-velocity measurements for WASP-64 and WASP-72 (BS = bisector spans).}
\end{center}
\label{wasp64+72-rvs}
\end{table}

\section{Analysis}

\subsection{Spectroscopic analysis - stellar properties}

The {\tt CORALIE} spectra of WASP-64 and WASP-72 were co-added to produce
single spectra with average S/N of 60 and 80, respectively. The standard pipeline
reduction products were used in the analysis.

The spectral analysis was performed using the methods given by
Gillon et al. (2009a). The \mbox{$H_\alpha$}\ line was used to determine the
effective temperature (\mbox{$T_{\rm eff}$}). For WASP-64,  the Na\,{\sc i}\,D and Mg\,{\sc i}\,b lines
were used as surface gravity ($\log g$) diagnostics.  For WASP-72,
getting an measurement of $\log g$ was more critical, as
the transit photometry does not constrain strongly the stellar density (see Sec. 3.2), so
we used the improved method recently described by Doyle et al. (2013) and based on the ionization balance
of selected Fe~{\sc i}/Fe~{\sc ii} lines in addition to the pressure-broadened Ca~{\sc i} lines at 6162{\AA} and 6439{\AA}
 (Bruntt et al. 2010a), along with the Na~{\sc i} D lines.
 The parameters
obtained from the analysis are listed in Table~3.
The elemental abundances were determined from equivalent width measurements
of several clean and unblended lines. A value for microturbulence (\mbox{$\xi_{\rm t}$})
was determined from Fe~{\sc i} lines using the method of Magain (1984). The
quoted error estimates include those given by the uncertainties in \mbox{$T_{\rm eff}$}, \mbox{$\log g$ }\
and \mbox{$\xi_{\rm t}$}, as well as the scatter due to measurement and atomic data uncertainties.

The projected stellar rotation velocities (\mbox{$v \sin{i_\ast}$ }) were determined by fitting the
profiles of several unblended Fe~{\sc i} lines. Values for macroturbulence
(\mbox{$v_{\rm mac}$}) of 1.8 $\pm$ 0.3 and 4.0 $\pm$ 0.3 {\mbox{km\,s$^{-1}$ }} were assumed for
WASP-64 and WASP-72, respectively, based on the calibration by
Bruntt at al. (2010b). An instrumental FWHM of 0.11 $\pm$ 0.01~{\AA} was
determined for both stars from the telluric lines around 6300\AA.
Best-fitting values of \mbox{$v \sin{i_\ast}$ }\ = 3.4 $\pm$ 0.8 \mbox{km\,s$^{-1}$ }\ (WASP-64) and
\mbox{$v \sin{i_\ast}$ }\ = 6.0 $\pm$ 0.7 \mbox{km\,s$^{-1}$ }\ (WASP-72) were obtained.

\begin{table}[h]
\begin{center}
\begin{tabular}{ccc} \hline
Parameter  & WASP-64 & WASP-72 \\ \hline
RA (J2000)  & 06 44 27.61 & 02 44 09.60 \\
DEC (J2000) & -32 51 30.25 & -30 10 08.5 \\
$V$ & 12.29 & 10.88 \\
$K$ &10.98  & 9.62 \\
\mbox{$T_{\rm eff}$}      &   5550 $\pm$ 150 K  & 6250 $\pm$ 100 K \\
\mbox{$\log g$ }      &   4.4 $\pm$ 0.15  &  $4.08 \pm 0.13$ \\
\mbox{$\xi_{\rm t}$}    &   0.9 $\pm$ 0.1 \mbox{km\,s$^{-1}$ }  &   1.6 $\pm$ 0.1 \mbox{km\,s$^{-1}$ } \\
\mbox{$v \sin{i_\ast}$ }     &   3.4 $\pm$ 0.8 \mbox{km\,s$^{-1}$ } &   6.0 $\pm$ 0.7 \mbox{km\,s$^{-1}$ } \\
{[Fe/H]}   &$-$0.08 $\pm$ 0.11 &$-$0.06 $\pm$ 0.09 \\
{[Na/H]}   &   0.14 $\pm$ 0.08 &$-$0.03 $\pm$ 0.04 \\
{[Mg/H]}   &   0.12 $\pm$ 0.12    &  \\
{[Al/H]}   &    0.00 $\pm$ 0.08 &     \\
{[Si/H]}   &    0.10 $\pm$ 0.10 &   0.02 $\pm$ 0.07 \\
{[Ca/H]}   &   0.05 $\pm$ 0.16 &  0.07 $\pm$ 0.14 \\
{[Sc/H]}   &    0.07 $\pm$ 0.10 & 0.14 $\pm$ 0.07 \\
{[Ti/H]}   &   $-$0.02 $\pm$ 0.11 & 0.07 $\pm$ 0.11 \\
{[V/H]}    &   0.03 $\pm$ 0.16 &$-$0.01 $\pm$ 0.08 \\
{[Cr/H]}   &   0.01 $\pm$ 0.08 &   0.02 $\pm$ 0.10 \\
{[Mn/H]}   &   0.09 $\pm$ 0.10 &$-$0.11 $\pm$ 0.06 \\
{[Co/H]}   &   0.06 $\pm$ 0.09 &$-$0.06 $\pm$ 0.18 \\
{[Ni/H]}   &$-$0.04 $\pm$ 0.11 &$-$0.04 $\pm$ 0.06 \\
log A(Li)  &   $<$ 0.61 $\pm$ 0.15  & $<$1.21 $\pm$ 0.17 \\
Mass       &   0.98 $\pm$ 0.09 $M_{\sun}$ &   $1.31 \pm 0.11 M_{\sun}$ \\
Radius     &   1.03 $\pm$ 0.20 $R_{\sun}$ &  $1.72 \pm 0.31 R_{\sun}$ \\
Sp. Type   &   G7 & F7 \\
Distance   &   350 $\pm$ 90 pc  &   $340 \pm 60$ pc \\ \hline
\end{tabular}
\end{center}
\label{wasp64+72-params}
\caption{Basic and spectroscopic parameters of WASP-64 and WASP-72
from spectroscopic analysis. \newline
{\bf Notes:} The values for the stellar mass, radius and
surface gravity are given here for information purpose only. The values that
we finally adopted for these parameters are the ones derived
from the global analysis of our data (Sec. 3.2) and are presented in Table 5 and 6.
Mass and radius estimate using the
calibration of Torres et al. (2010). Spectral type estimated from \mbox{$T_{\rm eff}$}\
using the table in Gray (2008). }
\end{table}

There is no significant detection of lithium in the spectra, with equivalent
width upper limits of 2m\AA  ~for both stars, corresponding to abundance
upper limits of log~A(Li) $<$ 0.61 $\pm$ 0.15 (WASP-64) and log~A(Li)
$<$ 1.21 $\pm$ 0.17 (WASP-72). These imply ages of at least a few Gyr
(Sestito \& Randich, 2005).

The rotation rate for WASP-64 ($P_{\rm rot} = 15.3 \pm 4.7$~d)
and WASP-72 ($P_{\rm rot} = 14.5 \pm 3.1$~d) implied by the {\mbox{$v \sin{i_\ast}$ }}
give gyrochronological ages of $\sim$$1.2_{-0.7}^{+1.2}$ Gyr (WASP-64) and
$\sim 3.7_{-1.9}^{+4.0}$ Gyr (WASP-72) under the Barnes (2007) relation.

We obtained with {\tt CORALIE} two spectra of TYC7091-1288-1, the brighter star
lying at 28'' East from WASP-64 (Sec. 2.2.1, Fig.~3).  The co-added spectrum has a S/N
 of only $\sim$30. A spectral analysis led to \mbox{$T_{\rm eff}$} $\sim$5700K and \mbox{$\log g$ } $\sim$4.5,
 with no sign of any significant lithium absorption, and a low {\mbox{$v \sin{i_\ast}$ }} $\sim$4~\mbox{km\,s$^{-1}$ }. The RV is $\sim$35 {\mbox{km\,s$^{-1}$ }},
compared to 33.2~{\mbox{km\,s$^{-1}$ }} for WASP-64. The cross-correlation function reveals that
TYC 7091-1288-1 is an SB2 system (Fig.~8). The PPMXL catalogue
(Roeser et al. 2010) shows that proper motions of both stars are consistent to within their quoted
uncertainties. If these stars are physically associate, as suggested by their similar proper motions
and  radial velocities, their angular separation corresponds to a projected distance of 9800 $\pm$ 2500 AU,
which is possible for a very wide triple system. Of course, the spectra of TYC7091-1288-1 and
WASP-64 are totally separated at the spatial resolution of  {\tt CORALIE} (typical seeing $\sim$1'',
fiber diameter of 2''), considering the 28'' separation between both objects.

\begin{figure}
\label{fig:rv}
\centering
\includegraphics[width=9cm,angle=0]{f11.eps}
\caption{The cross-correlation functions  for the two {\tt CORALIE} spectra of TYC7091-1288-1.
Their clear asymmetry indicates  the SB2 nature of the star.}
\end{figure}

\subsection{Global analysis}

For both systems, we performed a global analysis of the follow-up photometry and the
 {\tt CORALIE} RV measurements.  The analysis was performed using the adaptive
Markov Chain Monte-Carlo (MCMC) algorithm described by Gillon et al. (2012, and references therein).
To summarize, we simultaneously fitted the data, using for the photometry the transit
model of Mandel \& Agol (2002) multiplied  by a baseline model consisting of a different
second-order polynomial in time for each of the light curves. We motivate the choice of this
`minimal' baseline model by its better ability to represent properly any smooth variation due to a combination of
differential extinction and low-frequency stellar variability, compared to other possible simple functions
 (scalar, linear function of time or airmass). We outline that using a simple scalar as baseline model
relies on the strong assumptions that the ensemble of comparison stars used to derive the differential
photometry has exactly the same color than the target, that the target is perfectly stable, and that no low-frequency
noise could have modified the transit shape.
For  eight TRAPPIST light curves
(see Table 1), a normalization offset was also part of the model to represent the effect of
 the meridian flip. TRAPPIST's mount is a german equatorial type, which means
  that the telescope has to undergo a 180$^{\circ}$ rotation when the meridian is reached,
  resulting in different locations of the stellar images on the detector before and after the flip,
  and thus in a possible jump of the differential flux at the time of the flip.  For the first WASP-72 {\it Euler}
  transit, a quadratic function of airmass had to be added to the minimal baseline model to account
  for the strong extinction effect caused by the high airmass ($>$2.5) at the end of the run.
For the second WASP-72 transit observed by {\it Euler}, a normalization offset and a linear term in $x$- and
$y$-position were added to model the effects on the photometry of the telescope tracking problem.
 On their side, the RVs were  represented by a classical model assuming Keplerian orbits
 (e.g. Murray \& Correia 2010, eq. 65), plus a linear trend for WASP-72  (see Sec.~2.3).

The jump parameters\footnote{Jump parameters are the parameters that are randomly
perturbed at each step of the MCMC.} in our MCMC analysis were: the planet/star area
ratio $(R_p /R_\ast )^2$, the transit width (from first to last contact) $W$,  the parameter $b' =
a \cos{i_p}/R_\ast$ (which is the transit impact parameter in case of a circular orbit) where
$a$ is the planet's semi-major axis and $i_p$ its orbital inclination,  the orbital
period $P$ and time of minimum light $T_0$,  the parameter $K_2 = K  \sqrt{1-e^2}
 \textrm{ } P^{1/3}$, where $K$ is the RV orbital semi-amplitude,  and the two parameters $\sqrt{e} \cos{\omega}$
and $\sqrt{e} \sin{\omega}$, where $e$ is the orbital eccentricity and $\omega$ is the argument
of periastron. The choice of these two latter parameters is motivated by our will to avoid biasing
the derived posterior distribution of $e$,  as their use corresponds to a uniform prior for $e$ (Anderson
et al. 2011).

We assumed a uniform prior distribution for all these jump parameters.
The photometric baseline model parameters and the systemic radial velocity of the star $\gamma$ (and the
 slope of the trend for WASP-72) were not actual jump parameters; they were determined by
 least-square minimization at each step of the MCMC.

We assumed a quadratic limb-darkening law, and we allowed  the quadratic coefficients $u_1$
and $u_2$ to float in our MCMC analysis, using as jump parameters not these coefficients
themselves but the combinations $c_1 = 2 \times u_1 + u_2$  and $c_2 = u_1 - 2 \times u_2$
to minimize the correlation of the uncertainties (Holman et al. 2006).  To obtain a
limb-darkening solution consistent with theory, we used normal prior distributions
for $u_1$ and $u_2$ based on theoretical values and 1-$\sigma$ errors interpolated in the
tables by Claret (2000; 2004) and shown in Table 4. For our two non-standard filters ($I+z$ and
blue-blocking), we estimated the effective wavelength basing on the transmission curves
of the filters, the quantum efficiency curve of the camera and the spectral energy distributions
of the stars (assumed to emit as blackbodies), and we interpolated the corresponding
limb-darkening coefficient values in Claret's tables and estimated their errors by using the values for the
two nearest standard filters.  We tested the insensitivity of our results to the details of this
interpolation by performing short MCMC analyses with different prior distributions for the limb-darkening
coefficients of the non-standard filters (e.g. assuming $I+z$ = $I$-Cousins, blue-blocking = $R$-Cousins, etc.)
which led to results fully consistent with those of our nominal analysis. Such tests had also been performed in
the past for other WASP planets, with similar results (e.g. Smith et al. 2012).

\begin{table}
\begin{center}
\begin{tabular}{ccc}
\hline \noalign {\smallskip}
{\it Limb-darkening coefficient} &  WASP-64 & WASP-72 \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
$u1_{V}$            &  $0.50 \pm 0.035$   &    -                                \\ \noalign {\smallskip}
$u2_{V}$            &  $0.23 \pm 0.025$   &     -                                 \\ \noalign {\smallskip}
$u1_{Gunn-r}$   &  $0.43 \pm 0.03$ &   $0.31 \pm 0.015$    \\ \noalign {\smallskip}
$u2_{Gunn-r}$     &  $0.26 \pm 0.02$ &   $0.315 \pm 0.005$  \\ \noalign {\smallskip}
$u1_{BB}$          &  $0.36 \pm 0.05$   &   $0.255 \pm 0.04$   \\ \noalign {\smallskip}
$u2_{BB}$          &  $0.255 \pm 0.02$   &   $0.305 \pm 0.01$   \\ \noalign {\smallskip}
$u1_{I+z}$          &  $0.29 \pm 0.03$   &   $0.205 \pm 0.02$   \\ \noalign {\smallskip}
$u2_{I+z}$          &  $0.255 \pm 0.015$ &   $0.295 \pm 0.01$  \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
\end{tabular}
\caption{Expectation and standard deviation of the normal distributions used
as prior distributions for the quadratic limb-darkening coefficients $u1$ and $u2$ in our
MCMC analysis. }
\end{center}
\end{table}

Our analysis was composed of five Markov chains of $10^5$ steps, the first 20\% of each
chain being considered as its burn-in phase and discarded. For each run the convergence of the
five Markov chains was checked using the statistical test presented by Gelman and Rubin (1992).
The correlated noise present in the light curves was taken into account as described by  Gillon et al. (2009b),
by comparing the scatters of the residuals in the original and in
time-binned versions of the data, and by rescaling the errors accordingly.
For the WASP-72 RVs, a  `jitter' noise of 5.1 \mbox{m\,s$^{-1}$ }\  was added quadratically to the error bars,
to equalize the mean error with the $rms$ of the best-fitting model residuals.

At each step of the Markov chains the dynamical stellar density $\rho_\ast$ deduced from the
jump parameters (b', W, $(R_p /R_\ast )^2$, $\sqrt{e} \cos{\omega}$, $\sqrt{e} \sin{\omega}$, $P$;
see, e.g., Winn 2010)
and values for  $T_{\rm eff}$ and  [Fe/H] drawn from the normal distributions deduced from our
spectroscopic analysis (Sect.~3.1), were used to determine a value for the stellar mass $M_\ast$
 through an empirical law $M_\ast$($\rho_\ast$, $T_{\rm eff}$, [Fe/H]) (Enoch et al. 2010;
 Gillon et al. 2011) calibrated using the parameters of the extensive list of stars belonging to
 detached eclipsing binary systems presented by Southworth (2011). For WASP-64, the list
 was restricted to the 113 stars with a mass between 0.5 and 1.5 $M_\odot$, while the
 212 stars with a mass between 0.7 to 1.7 $M_\odot$ were used for WASP-72, the goal
 of this selection being to benefit from our preliminary estimation of the stellar mass  (Sec. 3.1, Table 3)
 to improve the determination of the physical parameters while using a number
 of calibration stars large enough to avoid small number statistical effects. To propagate properly the
 errors on the calibration law, the parameters of the selected subset of eclipsing binary stars
 were normally perturbed within their observational error bars and the coefficients of the law were
 redetermined at each MCMC step. Using the resulting stellar mass, the physical parameters
 of the system were then deduced from the jump parameters.  In this procedure to derive
 the physical parameters of the system, the  spectroscopic stellar gravity is thus not used,
 the stellar density deduced from the dynamical + transit parameters constraining by itself
 the evolutionary state of the star (Sozzetti et al. 2007). Still, for WASP-72 we assumed a normal
 prior distribution for  \mbox{$\log g$ }  based on the spectroscopic value and error bar (Table 3), because
 the low transit depth combined with the significant level of correlated noise of our data led to
 relatively poor constraint on the stellar density from the photometry alone (error of 50\%).

 For both systems, two analyses were performed, one assuming a circular orbit and the other
 an eccentric orbit. For the sake of completeness, the derived parameters for both models are shown
 in Table 5 (WASP-64) and Table 6 (WASP-72), while the best-fit transit models
 are shown in Fig.~10 and 11 for the circular model. Using the BIC as proxy for the
 model marginal likelihood, the resulting Bayes factors are $\sim$3000 (WASP-64)
 and $\sim$5000 (WASP-72) in favor of the circular models.  A circular orbit is
 thus favored for both systems, and we adopt the corresponding results
 as our nominal solutions (right columns of Table 5 and 6). This choice is strengthened by the modeling
 of the tidal evolution of both planets, as discussed in Sec. 4.

\subsubsection{Stellar evolution modeling}

After the completion of the MCMC analyses described above, we performed for both systems a stellar evolution
modeling based on the code CLES (Scuflaire et al. 2008) and on the Levenberg-Marquardt optimization algorithm (Press et al. 1992),
using as input the stellar densities deduced from the
 MCMC, and the effective temperatures and metallicities deduced from our
spectroscopic analyses, with the aim  to assess the reliability of the deduced physical parameters and to estimate
the age of the systems. The resulting  stellar masses were  $0.95 \pm 0.05$ $M_\odot$
(WASP-64) and $1.34 \pm 0.11$ $M_\odot$ (WASP-72), consistent with the
MCMC results, while the resulting ages were $7.0 \pm 3.5$ (WASP-64) and $3.2 \pm 0.6$
Gy (WASP-72).

Unlike WASP-64, WASP-72 appears to be significantly evolved. To check further
the reliability of our inferences for the system, we derived its parameters using the solar calibrated value of
the mixing length parameter and a value 20\% lower, and we also investigated the effects of convective
 core overshooting and microscopic diffusion of helium.  All the results are within 1sigma
 for the mean density and surface metallicity, and within 1.5 sigma for the effective temperature,
 however the best fits of mean density and $T_{eff}$  are found for models including convective
 core overshooting.  Solutions with standard physics tend to produce mean density higher than
 0.2 and $T_{eff}$ higher than 6300K.

\subsubsection{Global analysis of the transits with free timings}

 As a complement to our global analysis, we performed for both systems
 another global analysis with the timing of each transit being free parameters in the MCMC.
The goal here was to benefit from the strong constraint brought on the transit shape provided by the total
data set to derive accurate transit timings  and to assess the transit periodicity.  In this analysis,
the parameters $T_0$ and $P$ were kept under the control of  normal prior distributions based on
the values shown for a circular orbit in Table 5 (WASP-64) and Table 6 (WASP-72), and we added
a timing offset as jump parameter for each transit. The orbits were assumed to be circular. The
resulting transit timings and their errors are shown in Table 7. This table also shows (last column) the resulting
 transit timing variations (TTV = observed minus computed timing, O-C). These TTVs are shown as a function of the transit  epochs in Fig.~12.
 They are all compatible with zero, i.e. there is no sign of transit aperiodicity.

\begin{figure}
\label{fig:cw64}
\centering
\includegraphics[width=8.5cm]{f12.ps}
\caption{Combined follow-up transit photometry for WASP-64\,b, detrended, period-folded and binned per
intervals of 2 min.  For each
filter, the best-fit transit model from the global MCMC analysis is superimposed. The $V$, Gunn-$r$ and
blue-blocking light curves are shifted along the $y$-axis for the sake of clarity.}
\end{figure}

\begin{figure}
\label{fig:cw72}
\centering
\includegraphics[width=8.5cm]{f13.ps}
\caption{Combined follow-up transit photometry for WASP-72\,b, detrended, period-folded and binned per
intervals of 2 min.  For each
filter, the best-fit transit model from the global MCMC analysis is superimposed. The Gunn-$r$ and
blue-blocking light curves are shifted along the $y$-axis for the sake of clarity.}
\end{figure}

\begin{figure}
\label{fig:ttv}
\centering
\includegraphics[width=8.5cm]{f14.ps}
\includegraphics[width=8.5cm]{f15.ps}
\caption{TTVs ($O-C$ = observed minus computed timing) derived from the global MCMC analyzes of
the WASP-64\,b (top) and WASP-72\,b (bottom) transits (see Sec. 3.2.1).}
\end{figure}

\begin{table*}[h]
\begin{center}
\begin{tabular}{ccc}
& {\bf WASP-64}  & \\
\hline \noalign {\smallskip}
$Free$ $parameters$ &  $e \geq 0 $ & $e = 0$ {\bf (adopted)} \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
Planet/star area ratio  $ (R_p/R_\ast)^2 $  [\%]         &  $1.524 \pm 0.025$                       & $1.522 \pm 0.025$ \\ \noalign {\smallskip}
$b'=a\cos{i_p}/R_\ast$ [$R_*$]                                    &  $0.321_{-0.065}^{+0.046}$        &   $0.322_{-0.068}^{+0.048}$                    \\ \noalign {\smallskip}
Transit width  $W$ [d]                                                     &   $0.10005 \pm 0.00047$            & $0.09999 \pm 0.00046$                 \\ \noalign {\smallskip}
$T_0-2450000$ [$HJD_{TDB}$]                                  &  $5582.60171 \pm 0.00026$      &$5582.60169 \pm 0.00027$ \\ \noalign {\smallskip}
Orbital period  $ P$ [d]                                                    &  $1.5732918 \pm 0.0000015$   &  $1.5732918 \pm 0.0000015$                 \\ \noalign {\smallskip}
RV $K_2$  [m\,s$^{-1}$\,d$^{1/3}$]                              & $248 \pm 14$                                &    $257 \pm 11$                     \\ \noalign {\smallskip}
RV $\gamma$ [km\,s$^{-1}$]                                         & $33.191 \pm 0.010$                    &  $33.1854 \pm 0.0057$   \\ \noalign {\smallskip}
$\sqrt{e}\cos{\omega}$                                                   &  $0.083_{-0.088}^{+0.081}$       &    0 (fixed)             \\ \noalign {\smallskip}
$\sqrt{e}\sin{\omega}$                                                    &  $-0.10 \pm 0.15$                         &      0 (fixed)            \\ \noalign {\smallskip}
$c1_{V}$                                                               & $1.167 \pm 0.058$                    &   $1.168 \pm 0.058$                         \\ \noalign {\smallskip}
$c2_{V}$                                                               & $0.017 \pm 0.056$                    & $0.016 \pm 0.061$              \\ \noalign {\smallskip}
$c1_{Gunn-r}$                                                    & $0.983 \pm 0.050$                     &  $0.985 \pm 0.050$                          \\ \noalign {\smallskip}
$c2_{Gunn-r}$                                                    & $-0.121 \pm 0.044$                    &  $-0.122 \pm 0.045$                        \\ \noalign {\smallskip}
$c1_{BB}$                                                            & $1.040 \pm 0.045$                     &  $1.041 \pm 0.045$  \\ \noalign {\smallskip}
$c2_{BB}$                                                            & $-0.129 \pm 0.053$                    &  $-0.125 \pm 0.051$                           \\ \noalign {\smallskip}
$c1_{I+z}$                                                            & $0.859 \pm 0.053$                     &   $0.856 \pm 0.053$                            \\ \noalign {\smallskip}
$c2_{I+z}$                                                            & $-0.206 \pm 0.041$                    &   $-0.208 \pm 0.0241$                              \\ \noalign {\smallskip}
$T_{eff}$ [K] $^a$                                                        & $5400 \pm 100$              &   $5400 \pm 100$       \\ \noalign {\smallskip}
{[Fe/H]} $^a$                                                                 &$-$0.08 $\pm$ 0.11            &         $-$0.08 $\pm$ 0.11 \\\noalign {\smallskip}
\hline \noalign {\smallskip}
$Deduced$ $stellar$ $parameters$   &  &  \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
Density $\rho_* $  [$\rho_\odot $]                       & $0.90_{-0.09}^{+0.16}$ &  $0.849_{-0.044}^{+0.053}$       \\ \noalign {\smallskip}
Surface gravity $\log g_*$ [cgs]                          & $4.406_{-0.029}^{+0.044}$      &  $4.392 \pm 0.016$   \\ \noalign {\smallskip}
Mass $M_\ast $    [$M_\odot$]                            & $0.993_{-0.037}^{+0.034}$       &  $1.004 \pm 0.028$ \\ \noalign {\smallskip}
Radius  $ R_\ast $   [$R_\odot$]                         & $1.036_{-0.065}^{+0.046}$       &  $1.058 \pm 0.025 $       \\ \noalign {\smallskip}
Luminosity $L_\ast$ [$L_\odot$]                        & $0.90 \pm 0.15$             &    $0.95 \pm 0.13$          \\ \noalign {\smallskip}
$u1_{V}$                                                              & $0.470 \pm 0.033$           &   $0.470 \pm 0.035$      \\ \noalign {\smallskip}
$u2_{V}$                                                              & $0.226 \pm 0.027$           &    $0.227 \pm 0.028$      \\ \noalign {\smallskip}
$u1_{Gunn-r}$                                                    & $0.369 \pm 0.027$           &    $0.370 \pm 0.027$        \\ \noalign {\smallskip}
$u2_{Gunn-r}$                                                    & $0.245 \pm 0.020$           &   $0.246 \pm 0.020$      \\ \noalign {\smallskip}
$u1_{BB}$                                                          & $0.391 \pm 0.025$            &  $0.392 \pm 0.025$        \\ \noalign {\smallskip}
$u2_{BB}$                                                          & $0.259 \pm 0.023$            &  $0.259 \pm 0.022$      \\ \noalign {\smallskip}
$u1_{I+z}$                                                          & $0.302 \pm 0.028$            &   $0.301 \pm 0.028$      \\ \noalign {\smallskip}
$u2_{I+z}$                                                          & $0.255 \pm 0.017$            &   $0.255 \pm 0.018$   \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
$Deduced$ $planet$ $parameters$   & &   \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
RV $K$ [\mbox{m\,s$^{-1}$ }]                                                         & $214 \pm 13$           &   $221 \pm 11$                \\ \noalign {\smallskip}
$R_p/R_\ast$                                                       & $0.1234 \pm 0.0011$    & $0.1234 \pm 0.0011$                 \\ \noalign {\smallskip}
$b_{tr}$ [$R_\ast$]                                               & $0.313_{-0.064}^{+0.049}$ &  $0.322_{-0.068}^{+0.048}$          \\ \noalign {\smallskip}
$b_{oc}$ [$R_\ast$]                                             & $0.296_{-0.070}^{+0.059}$    & $0.322_{-0.068}^{+0.048}$ \\ \noalign {\smallskip}
$T_{oc}-2450000$ [$HJD_{TDB}$]                  &  $5583.403_{-0.024}^{+0.026}$            &   $5583.38834 \pm 0.00029$     \\ \noalign {\smallskip}
Orbital semi-major axis $ a $ [AU]                    &  $0.02640_{-0.00033}^{+0.00030}$        &   $0.02648 \pm 0.00024$       \\ \noalign {\smallskip}
$a / R_\ast$                                                            & $5.49_{-0.19}^{+0.31}$                & $5.39_{-0.09}^{+0.11}$  \\ \noalign {\smallskip}
Orbital inclination $i_p$ [deg]                               & $86.69_{-0.66}^{+0.79}$              &  $86.57_{-0.60}^{+0.80}$ \\ \noalign {\smallskip}
Orbital eccentricity $ e $                                       & $0.035_{-0.025}^{+0.039}$, $<0.132$ (95\%)           &     0 (fixed) \\ \noalign {\smallskip}
 Argument of periastron  $ \omega $ [deg]          & $308_{-36}^{+80}$                         & -   \\ \noalign {\smallskip}
Equilibrium temperature $T_{eq}$ [K]$ $$^b$    & $1672_{-63}^{+59}$                     & $1689 \pm 49$  \\ \noalign  {\smallskip}
Density  $ \rho_p$ [$\rho_{\rm Jup}$]                    &  $0.64_{-0.08}^{+0.12}$             &   $0.619_{-0.052}^{+0.064}$    \\ \noalign {\smallskip}
Surface gravity $\log g_p$ [cgs]                             &  $3.294_{-0.043}^{+0.049}$                         &  $3.292 \pm 0.030$ \\ \noalign  {\smallskip}
Mass  $ M_p$ [$M_{\rm Jup}$]                               & $1.217 \pm 0.083$                                        &    $1.271 \pm 0.068$  \\ \noalign {\smallskip}
Radius  $ R_p $ [$R_{\rm Jup}$]                            & $1.244_{-0.080}^{+0.062}$                        & $1.271 \pm 0.039$  \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
\end{tabular}
\caption{Median and 1-$\sigma$ limits of the marginalized posterior distributions obtained for the WASP-64
system parameters as derived from our MCMC analysis. $^a$Using as priors the spectroscopic values given in Table 3. $^b$Assuming a null Bond albedo ($A_B$=0) and isotropic reradiation ($f$=1/4). }
\end{center}
\end{table*}

\begin{table*}[h]
\begin{center}
\begin{tabular}{ccc}
& {\bf WASP-72}  & \\
\hline \noalign {\smallskip}
$Free$ $parameters$ &  $e \geq 0 $ & $e = 0$ {\bf (adopted)} \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
Planet/star area ratio  $ (R_p/R_\ast)^2 $  [\%]         &  $0.423_{-0.037}^{+0.039}$               & $0.430_{-0.039}^{+0.043}$ \\ \noalign {\smallskip}
$b'=a\cos{i_p}/R_\ast$ [$R_*$]                                    &  $0.58_{-0.20}^{+0.10}$                      &  $0.59_{-0.18}^{+0.10}$       \\ \noalign {\smallskip}
Transit width  $W$ [d]                                                     &   $0.1552 \pm 0.0029$                  & $0.1558_{-0.0029}^{+0.0035}$  \\ \noalign {\smallskip}
$T_0-2450000$ [$HJD_{TDB}$]                                 &  $5583.6525 \pm 0.0021$                   & $5583.6529 \pm 0.0021$       \\ \noalign {\smallskip}
Orbital period  $ P$ [d]                                       &  $2.2167434_{-0.0000077}^{+0.0000084}$    & $2.2167421 \pm 0.0000081$    \\ \noalign {\smallskip}
RV $K_2$  [m\,s$^{-1}$\,d$^{1/3}$]                             & $236.6 \pm 5.6$                                    &  $236.1 \pm 5.5$                          \\ \noalign {\smallskip}
RV $\gamma$ [km\,s$^{-1}$]                                        & $35.923 \pm 0.015$                             &  $35.919 \pm 0.014$   \\ \noalign {\smallskip}
RV slope [m\,s$^{-1}$\,y$^{-1}$]                         &  $-44 \pm 19$                                                 &   $-39 \pm 17$                \\ \noalign {\smallskip}
$\sqrt{e}\cos{\omega}$                                         &  $-0.022 \pm 0.071$                                      &  0 (fixed)                         \\ \noalign {\smallskip}
$\sqrt{e}\sin{\omega}$                                          &  $-0.06 \pm 0.11$                                          &   0 (fixed)                        \\ \noalign {\smallskip}
$c1_{Gunn-r}$                                                       & $0.938 \pm 0.026$                                        &  $0.936 \pm 0.026$          \\ \noalign {\smallskip}
$c2_{Gunn-r}$                                                       & $-0.318 \pm 0.016$                                       & $-0.319 \pm 0.017$      \\ \noalign {\smallskip}
$c1_{BB}$                                                            & $0.820 \pm 0.082$                                          &  $0.818 \pm 0.078$  \\ \noalign {\smallskip}
$c2_{BB}$                                                            & $-0.352 \pm 0.046$                                         & $-0.352 \pm 0.042$   \\ \noalign {\smallskip}
$c1_{I+z}$                                                            & $0.713 \pm 0.041$                                          &  $0.710 \pm 0.042$   \\ \noalign {\smallskip}
$c2_{I+z}$                                                            & $-0.382 \pm 0.028$                                         &  $-0.383 \pm 0.027$  \\ \noalign {\smallskip}
$T_{eff}$ [K] $^a$                                                   & $6250 \pm 100$                                              &  $6250 \pm 100$                         \\ \noalign {\smallskip}
[Fe/H] $^a$                                                                  &$-$0.06 $\pm$ 0.09                                        &  $-$0.06 $\pm$ 0.09                    \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
$Deduced$ $stellar$ $parameters$   &  &  \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
Surface gravity $\log g_*$ [cgs] $^a$                      & $3.99 \pm 0.10$                      &  $3.99_{-0.11}^{+0.10}$              \\ \noalign {\smallskip}
Density $\rho_* $  [$\rho_\odot $]                       & $0.181_{-0.046}^{+0.074}$                      &  $0.177_{-0.048}^{+0.073}$       \\ \noalign {\smallskip}
Mass $M_\ast $    [$M_\odot$]                            & $1.382 \pm 0.053$                       & $1.386 \pm 0.055$        \\ \noalign {\smallskip}
Radius  $ R_\ast $   [$R_\odot$]                         & $1.97 \pm 0.23$                             & $1.98 \pm 0.24$                \\ \noalign {\smallskip}
Luminosity $L_\ast$ [$L_\odot$]                        & $5.3_{-1.2}^{+1.4}$                                    &  $5.3_{-1.3}^{+1.5}$                      \\ \noalign {\smallskip}
$u1_{Gunn-r}$                                                       & $0.311 \pm 0.013$                                     &  $0.311 \pm 0.013$                        \\ \noalign {\smallskip}
$u2_{Gunn-r}$                                                    & $0.3148 \pm 0.0063$                                   &   $0.3147 \pm 0.0060$                  \\ \noalign {\smallskip}
$u1_{BB}$                                                          & $0.257 \pm 0.043$                                         &  $0.256 \pm 0.041$                        \\ \noalign {\smallskip}
$u2_{BB}$                                                          & $0.305 \pm 0.013$                                         &  $0.305 \pm 0.014$                        \\ \noalign {\smallskip}
$u1_{I+z}$                                                          & $0.209 \pm 0.022$                                         &   $0.208 \pm 0.022$                        \\ \noalign {\smallskip}
$u2_{I+z}$                                                          & $0.295 \pm 0.012$                                          &   $0.295 \pm 0.013$                       \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
$Deduced$ $planet$ $parameters$   & &   \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
RV $K$ [\mbox{m\,s$^{-1}$ }]                                                        & $181.3 \pm 4.2$                                               & $181.0 \pm 4.2$                \\ \noalign {\smallskip}
$R_p/R_\ast$                                                       & $0.0650 \pm 0.0029$                    &  $0.0656 \pm 0.0031$  \\ \noalign {\smallskip}
$b_{tr}$ [$R_\ast$]                                               & $0.57_{-0.20}^{+0.10}$                                &  $0.59_{-0.18}^{+0.10}$                \\ \noalign {\smallskip}
$b_{oc}$ [$R_\ast$]                                             & $0.58_{-0.21}^{+0.11}$                                & $0.59_{-0.18}^{+0.10}$                 \\ \noalign {\smallskip}
$T_{oc}-2450000$ [$HJD_{TDB}$]                &   $5584.758 \pm 0.042$                   & $5584.7612 \pm 0.0021$             \\ \noalign {\smallskip}
Orbital semi-major axis $ a $ [AU]                       &  $0.03705 \pm 0.00047$    & $0.03708 \pm 0.00050$  \\\noalign{\smallskip}
$a / R_\ast$                                                          & $4.05_{-0.38}^{+0.49}$                                   & $4.02_{-0.40}^{+0.49}$  \\ \noalign {\smallskip}
Orbital inclination $i_p$ [deg]                               & $81.8_{-2.5}^{+3.5}$                                   &  $81.6_{-2.6}^{+3.2}$ \\ \noalign {\smallskip}
Orbital eccentricity $ e $                                       & $0.014_{-0.010}^{+0.018}$, $<0.079$ (95\%) &   0 (fixed) \\ \noalign {\smallskip}
Argument of periastron  $ \omega $ [deg]            & $115_{-47}^{+111}$                                     &  -   \\ \noalign {\smallskip}
Equilibrium temperature $T_{eq}$ [K]$ $$^b$      & $2200_{-120}^{+110}$                            &$2210_{-130}^{+120}$  \\ \noalign  {\smallskip}
Density  $ \rho_p$ [$\rho_{\rm Jup}$]                         &  $0.75_{-0.25}^{+0.45}$                       & $0.72_{-0.25}^{+0.43}$    \\ \noalign {\smallskip}
Surface gravity $\log g_p$ [cgs]                           &  $3.37_{-0.11}^{+0.13}$                              & $3.36 \pm 0.12$ \\ \noalign  {\smallskip}
Mass  $ M_p$ [$M_{\rm Jup}$]                                   & $1.459 \pm 0.056$                  &  $1.5461_{-0.056}^{+0.059}$    \\ \noalign {\smallskip}
Radius  $ R_p $ [$R_{\rm Jup}$]                                &    $1.25 \pm 0.19$                     &  $1.27 \pm 0.20$   \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
\end{tabular}
\caption{ Median and 1-$\sigma$ limits of the marginalized posterior distributions obtained for the WASP-72
system parameters as derived from our MCMC analysis. $^a$Using as priors the spectroscopic values given in Table 3. $^b$Assuming a null Bond albedo ($A_B$=0) and isotropic reradiation ($f$=1/4). }
\end{center}
\end{table*}

\begin{table}
\begin{center}
\begin{tabular}{cccc}
\hline \noalign {\smallskip}
Planet & Epoch &  Transit timing - 2450000 & $O-C$  \\ \noalign {\smallskip}
& & [$HJD_{TDB}$] & [$s$] \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
WASP-64\,b & 0   &  $5582.60070 \pm 0.00051$     & $-85 \pm 50$  \\ \noalign {\smallskip}
& 21  & $5615.64057 \pm 0.00057$     & $-19 \pm 55$  \\ \noalign {\smallskip}
& 47  & $5656.54655  \pm 0.00035$    & $+15 \pm 39$ \\ \noalign {\smallskip}
& 173 &  $5854.78224 \pm 0.00027$   & $+97 \pm 40$ \\ \noalign {\smallskip}
& 173 &  $5854.78091 \pm 0.00032$   & $-19 \pm 41$  \\ \noalign {\smallskip}
& 180  &  $5865.79456 \pm 0.00025$  & $+35 \pm 39$ \\ \noalign {\smallskip}
& 194  &  $5887.82045 \pm 0.00035$   & $+18 \pm 44$ \\ \noalign {\smallskip}
& 199  &  $5895.68667 \pm 0.00029$   & $-5 \pm 42$    \\ \noalign {\smallskip}
& 206 &  $5906.69953 \pm 0.00041$    & $-19 \pm 50$  \\ \noalign {\smallskip}
& 213  &  $5917.71279 \pm 0.00019$   & $-1 \pm 38$    \\ \noalign {\smallskip}
& 229  &  $5939.73781 \pm 0.00030$  & $-92 \pm 45$   \\[0.33cm]
WASP-72\,b & 0   &  $5583.6542 \pm 0.0024$     & $+3.3 \pm 5.0$  \\ \noalign {\smallskip}
& 125  & $5860.7441 \pm 0.0048$     & $-0.7\pm 7.7$  \\ \noalign {\smallskip}
& 139  & $5891.7797  \pm 0.0017$    & $+0.9 \pm 4.6$ \\ \noalign {\smallskip}
& 143 &  $5900.6475 \pm 0.0043$   & $+3.4 \pm 8.5$ \\ \noalign {\smallskip}
& 300 &  $6248.6710 \pm 0.0029$   & $-5.0 \pm 6.4$ \\ \noalign {\smallskip}
& 300 &  $6248.6758 \pm 0.0012$   & $+1.8 \pm 5.3$ \\ \noalign {\smallskip}
& 309 &  $6268.6292 \pm 0.0024$   & $+5.7 \pm 6.3$ \\ \noalign {\smallskip}
\hline \noalign {\smallskip}
\end{tabular}
\caption{Transit timings and TTVs  ($O-C$ = observed minus computed timing)
derived from the MCMC global analyzes of the WASP-64\,b and  WASP-72\,b transits. }
\end{center}
\end{table}

\section{Discussion}

WASP-64\,b and WASP-72\,b are thus two new very short-period (1.57d and 2.22d)
planets slightly more massive than Jupiter orbiting moderately bright ($V$=12.3 and 10.1)
Southern stars. Their detection demonstrates nicely  the high photometric potential
 of the WASP transit survey  (Pollacco et al. 2006), as both planets show transits of very low-amplitude
($<$ 0.5\%) in the WASP data. For WASP-64, the reason is not the intrinsic size contrast with the
 host star but the dilution of the signal by a close-by spectroscopic binary that could be dynamically
 bound to WASP-64 (Sec. 3.1).

Fig.~13 shows the position of both planets in mass-radius  and irradiation-radius diagrams
for a mass range from 1 to 2 $M_{Jup}$. WASP-64\,b  lies in a well-populated
area of  the irradiation-radius diagram. Its physical dimensions can be considered as rather standard.
Its measured radius of  $1.27 \pm 0.04$ $R_{\rm Jup}$ agrees well with the value of $1.22 \pm
0.11$ $R_{Jup}$ predicted by the equation derived by Enoch et al. (2012) from a sample of 71
transiting planets with a mass between 0.5 and 2  $M_{\rm Jup}$ and relating planets' sizes to
their equilibrium temperatures and semi-major axes. On the contrary, WASP-72\,b
 appears to be a possible outlier,  its measured radius of $1.27 \pm 0.20$ $R_{\rm Jup}$
 being marginally lower than the value predicted by Enoch et al's empirical relation,
 $1.70 \pm 0.11$ $R_{Jup}$. Its density of $0.732_{-0.25}^{+0.43}$ $\rho_{\rm Jup}$
 could indeed be considered as  surprisingly high given its  extreme irradiation
 ($\sim5.5\times10^9$ erg\,s$^{-1}$\,cm$^{-2}$), suggesting a  possible enrichment of heavy elements.
 Nevertheless, Fig.~13 clearly shows that the errors
on its physical parameters  are still too high to draw any strong inference on
its internal structure or its possible peculiarity.  Indeed, the transit parameters are still loosely determined,
especially the impact parameter, resulting in a high relative error on the  stellar density that propagates to the
 stellar and planetary radii. Planets with similar irradiation and mass being still rare, it will thus be especially interesting
  to improve these parameters with new follow-up observations.

 As described in Sec. 3.2, we have adopted the circular orbital models for both
 planets, basing on their higher marginal likelihoods. To assess the validity of this choice
 on a theoretical basis, we integrated the future orbital  evolution of both systems through
 the low-eccentricity tidal model presented by Jackson et al. (2008), assuming as starting eccentricity
 the 95\% upper limits derived in our MCMC analysis (0.132 for WASP-64\,b and 0.052 for WASP-72\,b)
 and assuming mean values of $10^{7}$ and $10^{5}$ for, respectively, the stellar and planetary tidal
  dissipation parameters $Q'_\ast$ and  $Q'_p$ (Goldreich \& Soter, 1966). These integrations resulted
  in circularization times (defined as the time needed to reach $e<0.001$) of 4 and  24 Myr for, respectively,
  WASP-64\,b and WASP-72\,b. These times are much shorter than the estimated age of the systems, strengthening
our selection of the circular orbital solutions. It is worth mentioning that both systems are tidally unstable,
as most of the hot Jupiter systems (Levrard et al. 2009),  the times remaining for the planets to reach their Roche limits
being respectively 0.9 Gy (WASP-64\,b) and  0.35 Gy (WASP-72\,b) under the assumed tidal dissipation parameters.

The new transiting systems reported here represent both two interesting targets for follow-up
observations. Thanks to its extreme irradiation and its moderately high planet-to-star size ratio,
WASP-64\,b is a good target for near-infrared occultation (spectro-)photometry programs able
to probe its day-side  spectral energy distribution. Assuming a null albedo for the planet
and blackbody spectra for both the planet and the host star, we computed occultation depths
of 650-1550 ppm in $K$-band, 1500-2750 ppm at 3.6 $\mu$m and 2050-3350 ppm at 4.5 $\mu$m, the
lower and upper limits corresponding, respectively, to a uniform redistribution of the stellar radiation
 to both planetary hemispheres and to a direct reemission of the dayside hemisphere. Precise
measurement of such occultation depths is definitely within the reach of several ground-based and
 space-based facilities (e.g. Gillon et al. 2012). For ground-based programs, the situation is made easier
  by the presence of a bright ($K=9.8$) comparison star at only 28'' from the target (Fig.~3). For
  WASP-72, atmospheric measurements are certainly more challenging considering the lower
  planet-to-star size ratio. Here, the first follow-up actions should certainly be to  confirm and improve
  our measurement of the planet's size through high-precision transit photometry, and to gather more RVs
  to confirm the trend marginally detected in our analysis.
\begin{figure*}
\label{fig:mr}
\centering
\includegraphics[width=8.5cm]{f16.ps}
\includegraphics[width=8.5cm]{f17.ps}
\caption{$Left$: mass--radius diagram for the transiting planets with masses
ranging from 1 to 2 $M_{\rm Jup}$ (data from exoplanet.eu, Schneider et al. 2011).
WASP-64\,b and WASP-72\,b are shown as red square symbols, while the other planets are
shown as open circles without their error bars for the sake of clarity. Different iso-density lines are also
shown. $Right$: position of WASP-64\,b and WASP-72\,b in a
irradiation--radius diagram for the same exoplanets sample.}
\end{figure*}

\begin{acknowledgements}
WASP-South is hosted by the South African Astronomical Observatory and we are grateful for their ongoing support and assistance. Funding for WASP comes from consortium universities and from UK's Science and Technology Facilities Council. TRAPPIST is a project funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, F.R.S-FNRS) under grant FRFC 2.5.594.09.F, with the participation of the Swiss National Science Fundation (SNF).  M. Gillon and E. Jehin are FNRS Research Associates.
We thank the anonymous referee for his useful criticisms and suggestions that helped us to improve the
quality of the present paper.
\end{acknowledgements}

\bibliographystyle{aa}

redpajama_set_name: RedPajamaArXiv


text:
Hanesbrands' Revenue Breakdown by Segment (2016-2022)
This statistic highlights Hanesbrands' Revenue Breakdown by Segment, split between Innerwear, International, Activewear and Others, reported on a quarterly basis from Q1 2016 onwards.
By Hiket Shah
Hanesbrands' Revenue Breakdown by Segment
The following table highlights Hanesbrands' Revenue by Segment, in some of the recent quarters.
Segment Q3 2020 Q2 2021 Q3 2021 Contribution in Q3 2021
Innerwear $792.60 $780.65 $702.62 39.26%
International $506.20 $478.92 $536.48 29.99%
Activewear $324.92 $404.19 $462.50 25.84%
Others $68.14 $87.55 $87.95 4.91%
Total $1691.86 $1751.31 $1789.55 100.00%
(All figures in millions, except percentages)
These segments are organized mainly by product category and geographic location. Every segment has its management team that is responsible for the operations of the segment's businesses. However, the segments share a common supply chain and media and marketing platforms.
The Innerwear segment includes core apparel products, such as men's underwear, women's panties, children's underwear, socks, and intimate apparel like bras and shapewear, sold in the United States. It also includes sales of personal protective equipment products such as cloth face coverings and gowns.
In the United States, Hanesbrands is the intimate apparel category leader. Some of their well-known brands are Hanes, Bali, Maidenform, Playtex, Champion, Just My Size (JMS), etc.
On a QoQ basis, there is a 10% decrease in the total revenue of this segment from $780.65 million in Q2 2021 to $702.62 million in Q3 2021, as compared to an 11.35% fall on a YoY basis. There is a clear seasonality effect in this segment, having a spike in Q2 each year, followed by a decrease in the subsequent quarters. Moreover, in Q2 2020, this segment's revenue had a huge growth, which was due to the sales of PPE kits. The company exited the PPE business in 2021, resulting in falling revenue.
The International segment includes innerwear, activewear, hosiery, and home goods products, sold outside the United States. All of the Hanesbrands' categories are sold outside the United States, primarily in Australasia, Europe, Asia, Canada, and Latin America. Some of their brands are also market leaders across various countries. In 2020, this segment also included the sales of PPE.
There was a growth of 12% in the revenue in this segment on a QoQ basis. There was a growth of 5.98% on a YoY basis attributable to strong consumer demand in the Americas, Europe, and some markets of Asia. The company had discontinued its operations of the European Innerwear business in Q1 2021 and plans to sell it to an affiliate of Regent L.P. by Q1 2022.
The Activewear segment consists of products such as T-shirts, fleece, performance apparel, sport shirts, and thermals, sold in the United States. The company makes these products available in department stores like Walmart (the company's largest customer), its own e-commerce website, and through pure-play commerce websites like Amazon. This segment also includes the sale of licensed sports and logo apparel in collegiate bookstores, and through mass retailers.
On a QoQ basis, there was a 14.4% increase in the total revenue from this segment as compared to a 42.3% YoY increase. This increase was driven by lower sales in 2020 due to COVID-19 pandemic-related shutdowns and incremental sales partially as a result of higher U.S. government stimulus spending.
This segment consists of Hanesbrands' U.S.-based outlet stores, U.S. hosiery business, and certain sales from the European Innerwear business. The net sales in this segment increased as a result of increased sales at their retail outlets during Q2 2021 since the stores reopened after temporary closures during the COVID-19 pandemic.
On a QoQ basis, there has been a growth of only $0.4 million, however, there was a 29% increase on a YoY basis. This segment has seen a huge downfall in revenue during FY 2020.
Hanesbrands Inc. is a leading marketer of everyday basic innerwear and activewear apparel in the Americas, Australia, Europe, and Asia/Pacific. The company is headquartered in North Carolina and was founded in 1901. Their business strategy integrates brand superiority, industry-leading innovation, and a low-cost global supply chain to provide higher value products while lowering production costs. They sell their products under some of the world's strongest apparel brands, including Hanes, Champion, Bonds, Bali, Maidenform, Playtex, Bras N Things, JMS/Just My Size, Wonderbra, Alternative, Berlei, L'eggs, and Gear for Sports.
These products are marketed to consumers shopping in mass merchants, mid-tier and department stores, specialty stores, and the consumer-directed channel, which includes the company's owned retail locations, as well as e-commerce sites. The brands hold either the number one or number two market position by units sold in many of the product categories and geographies in which they compete.
Did you like Hanesbrands' Revenue Breakdown by Segment statistic?
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redpajama_set_name: RedPajamaCommonCrawl


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text:
« From Homeless to a Huge Hit: The Ray Howard Band Lights Up Our Labor Day Again
I'm a Mutant, Too! »
Uncategorized | September 6, 2019
The AMP Trio: Hot and Ready!
Adrianne Murchison, Staff Editor
The Velvet Note Acoustic Living Room
The musicians of AMP Trio have a global reach similar to that of The Velvet Note: Friends around the world with a love and appreciation for jazz artistry. In fact, the title of AMP Trio's upcoming album, "Go-Naïve"is inspired by a friend who invited them to perform in Japan back in 2012.
AMP Trio, featuring vocalist Tahira Clayton, takes The Velvet Note stage on Saturday, September 7, performing tunes from four albums, as well as their soon-to-be-released fifth record.
"We are going to be coming pretty hot," drummer Matt Young says. "We will all be in Atlanta and with our new music."
AMP Trio, featuring Tahira Clayton
Matt Young, Perrin Grace and Addison Frei met about seven years ago while attending the University of Texas and discovered they have a few important things in common. They're fans of acoustic bands, and similarly influenced by the likes of Phineas Newborn Jr., Blue Mitchell and Oscar Peterson.
"We were probably sophomores in college and had been playing in a fusion band that was pretty much opposite of what we do in this band," Matt says. "It was a loud, crazy intense energy and we missed playing acoustic music."
So the drummer, pianist and bassist formed AMP Trio. Matt lives in Atlanta and the other band members reside in the New York City area. Before coming together each had received international acclaim.
First prize in the 2017 Parmigiani Montreau Jazz Piano Solo Competition is one of Addison's numerous honors.
Germany, South Korea and The Netherlands are only a few countries where Perrin has performed.
And in addition to Matt's globe travels, in 2015 he took part in the Betty Carter Jazz Ahead program, a two-week international residency project at The Kennedy Center in Washington D.C.,
Tahira Clayton
AMP Trio's many collaborations with Tahira – whose rich harmonic voice captivates audiences – include top honors at the 2017 DCJazzPrix international band competition in Washington D. C.
"We push each other and share the same music morals," Matt says. "We know that we can rely on each other, and represent each other in a way that we trust."
The Velvet Note sets a high bar that the trio takes pride in reaching, Matt adds. For the upcoming show, the crowd can expect the band's new music to be a little more groove driven than their previous albums, he says. "Perry's [compositions] are definitely darker songs, tonally and texturally."
Not too long after AMP Trio came together, the band received their first invitation to Ofunato, Japan, a port city shattered by the tsunami of 2011.
"We go back to Japan every summer," Matt says. "Eiko Konno, the host, brought us over one time after finding us on the Internet and listening to our music. She's a big classical music buff, and an incredible classical pianist."
Eiko's invitation was on behalf of a cultural program and government grant that would introduce AMP Trio's jazz music to citizens of Ofunato.
"They had a newly built performance hall," Matt recalls. "The tsunami was tough on them. It's crazy because you go there now and everything is brand spanking new, '[with the exception of some structures] and artifacts that were on higher ground."
It's Eiko, who is the muse behind AMP Trio's new album title.
"She and Perry had become pen pals, and when we visited she asked, 'What did you think of me when I emailed you out of nowhere,'" Matt explained. "Perry said, 'If that's what it takes to come to Japan, let's go naïve.'"
This entry was posted on Friday, September 6th, 2019 at 3:39 pm and is filed under Uncategorized. You can follow any responses to this entry through the RSS 2.0 feed. Both comments and pings are currently closed.


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Q: how i can create multi image with different Location in javascript? how i can create 14 image with different Location ( Random Location ) in html using javascript ?
this is my code
function createAliens() {

        $('body').append('<img class="alien" src="alien.ico" width="70" height="70">');

}

A: I would say that you need to use html canvas and access the coordinates properties of it, and then properly add your objects to that layout

redpajama_set_name: RedPajamaStackExchange


PTT will focus on regional growth, having reached the limit in domestic expansion, with the aim of becoming the second-largest petrochemicals player behind national brands in some countries within five years.
The company will also increase the sales ratio of non-oil businesses such as Amazon coffee houses, 7-Eleven convenience stores and quick-service restaurants from 20-30 per cent to 50 per cent in the next two to three years. The move will offset lower profit margins from oil sales.
Saran Rangkasiri, executive vice president of PTT, said the company would maintain the number of PTT petrol stations in Thailand at about 1,300.
"We will focus on strategic expansion, especially in neighbouring markets where we have a geographic advantage in terms of logistics and distribution of our finished oil," said Saran.
He said PTT's overseas expansion would be one of the company's major strategies in the next three to five years.
The company has 30 petrol stations in Laos, 46 in the Philippines and six in Cambodia.
He said PTT would spend between Bt300 million and Bt500 million on expanding its network of petrol stations overseas over the next two years.
"We will not focus on the number of petrol stations to be opened abroad, but on oil volume traded per station, as well as their sales values and profit margins," said Saran.
He added that potential markets included Cambodia, the Philippines, Laos and southern China, as well as Myanmar and Vietnam, once local regulations preventing foreign investment in petrol businesses were relaxed.
"We want to be one of the leading brands in particular countries with the highest market share in the next five years," said Saran.
PTT yesterday celebrated the opening of 555 Amazon coffee houses in Thailand, of which most are located in PTT petrol stations. The company launched Amazon nine years ago. It expects to sell about 30 million cups of fresh coffee this year, up 25 per cent over last year.
"We plan to open another 120 Amazon coffee houses this year, including 10 pilot outlets that will be opened outside the petrol stations. Potential locations will be large and small shopping malls and office buildings," said Saran.
He said the company expected the number of Amazon branches to reach 2,000 in two to three years.
He added that the company would open its first overseas Amazon outlet in Laos this year.
Saran said PTT earned Bt1.08 per litre on diesel sales. Dealers earned about 78 satang per litre.
He said the government's price control policy had cost PTT about Bt1.4 billion and urged the new elected government not to interfere in oil prices.
"We believe in the market mechanism and free trade. Full market competition will benefit both business entrepreneurs and consumers. Any form of government subsidy on energy products such as oil will discourage consumers from energy saving," he said.
~ by FSVSF Admin on 6 June, 2011.


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L'Oratoire Saint-Joseph - Congrégation de Sainte-Croix au Canada
L'Oratoire Saint-Joseph
Saint Joseph's Oratory – A dream come true
A story that began in 1904
Door keeper at college Notre-Dame, Brother Andre has a dream. From the narrow window of his office he saw this small hill that people of Montreal proudly called "the mountain". In fact it was a quiet hill were wealthy people had built cottages a little away from the city. Brother Andre hoped and prayed that one day it would be possible to build on this hill a small Oratory where people could come and pray Saint Joseph. In 1896 the community bought this land and the hope of Brother Andre revived. In 1904 the superior of the college allowed Brother Andre to build his Oratory. The community was poor at the time and Brother Andre with his friends and collaborators has to find the money to build this small Oratory.
At the beginning Brother Andre was surrounded by a small group of faithful friends but soon people started coming in great numbers to meet Brother Andre and pray with him. With the help of the pilgrims the project started to grow. Twenty years after the foundation, a rectory for the religious had been built, a crypt church big enough to accommodate thousand persons was completed and already plans are made to complete the large Church that would later be declared Basilica.
Brother Andre wanted an Oratory, a small prayer place but the faith of millions of people coming to this sanctuary transform this early plan into the marvelous shrine we find today on the Mont-Royal. On January 6, 1937, when Brother Andre died, the construction was on its way and Brother Andre rejoiced to see the marvels that were realized. He knew well that this is God's way of using the most humble servant to realize great things.
After the death of Brother Andre, the interest of pilgrims for this sanctuary continued and millions of pilgrims and visitors continued to come to the shrine. The beatification of Brother Andre in 1982 and his canonization in 2010 were important moments in the life of to the shrine. Today tow millions of pilgrims and visitors visit the place every year.
A beacon of faith and peace at the hearth of a modern city
Every week thousands of people come to the Oratory to pray and celebrate their faith. Beautiful liturgies in French, in English and occasionally in Spanish allow catholic to participate in the prayers and worship of the Church. Those who wish to meet a priest for the sacrament of penance and reconciliation find pries available every day from morning to evening.
Nowadays, Christians and non-Christians come to the Oratory to find a place of peace and personal prayer. Some will spend time praying in the crypt church, others in the votive chapel, or near the tomb of Saint Andre Bessette. Some prefer the majestic Basilica others will rather spend time in the small original chapel or in the beautiful garden of the way of the cross. Some prefer to play in silence others prefer to join in common prayer and worship.
A place of beauty for all
Visitors are impressed by the beauty of this place, The art work the impressive architecture the lovely gardens, the melodious music create a climate of peace and invite even non-believers to stop and open their heaths to the beauty of this world, a beauty that invited to Go beyond what the eyes can see and the ear hear. The beauty of the place invites to discover the mystery that lies beyond. For some visitors the experience of the beauty of the place lights a spark in their hearth and slowly awaken a quest for God. Tourists come curious to discover this famous shrine but they often find much more, they find their way to meet God.
A place to meet people filled with compassion
In the early days people came to meet an exceptional man, a humble brother who met every one with compassion and spoke to them about the love of God for us, about the Virgin Mary and Saint Joseph. The religious who pursue the work of Brother Andre continue to receive visitor, listen to their hopes and their sufferings. They welcome each one and invite them to discover the power of God's love.
Holy Cross religious are proud to continue the mission of the Oratory
Saint Andre Bessette was a Holy-Cross brother and the congregation of Holy Cross has discovered in his life and work an important part of its tradition. Today it has become clear that the mission of the Oratory is part and parcel of the mission of Holy-Cross. In the past this mission was almost exclusively done by Canadian members of Holy-Cross. Holy Cross has changed and today we find Holy Cross of five different nationalities working together at the service of the pilgrims and visitors. We can foresee in the coming years a rich diversity of members of Holy-Cross working together at the service of the more than 2 millions of visitors coming to the sanctuary every year. Blessed Basil Anthony Moreau encouraged the members of Holy Cross to work together with zeal, bringing to people the message of Jesus. It is with the same zeal for the mission that Holy-Cross from different parts of the world, come together today to pursue the mission of Holy-Cross, inspired by Saint Andre Bessette.
And the dream goes on
The dream of Brother Andre was not an ordinary dream; it was an act of faith. Brother Andre new that God it was God's work and he knew that God will continue this work. Since the very beginning men and women have come together to pursue with the same faith the work so well begun. Thousands of pilgrims come to the Oratory every year; they come with the hope to see a world transformed by compassion, love, solidarity and justice. They come with their sufferings and their hope. They come to place their lives in the hands of God and entrust their worries to saint Brother Andre their brother and their friend.
Working in this Shrine is a privilege. Our faith is constantly revived by the faith of pilgrims, our love of Saint Joseph and brother Andre is strengthened by their love, our hope is nourished by their unfailing hope. We are touched by the courage and spiritual depth of so many pilgrims and visitors. Their response to the Lord strengthens us in our own vocation as religious of Holy Cross. We walk along with them as men of hope and we know that this dream will always go on.
Crédit: Père Claude Grou, c.s.c.


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Q: Window.localstorage throws script error in MAC OS safari browser I have tried window.localStorage and window.sessionStorage. both of them return below error

Security Error: DOM Exception 18: An attempt was made to break through the security policy of the user agent

It works properly in windows OS. .The issue in MAC only.
How to resolve it?

A: Quick search returns this page where Nolan Lawson states:

DOM Exception 18 usually means you exceeded the quota allowed on the device (50MB), although in some environments it's because Apple removed WebSQL support (e.g. WKWebView).

How much data are you attempting to store?


OKAHAO, 28 JUN (NAMPA) – Namibian women are proud of the peace and stability that is prevailing in the country for the past 25 years of national freedom and independence.
Gender Equality and Child Welfare Deputy Minister, Lucia Witbooi said this whilst addressing a belated celebration of International Women's Day by members of the Omusati Region's Swapo-Party Women's Council (SPWC) at Okahao on Saturday.
"We need peace in Africa and peace in the world. Without peace, there will be no development; obviously there will be no empowerment of women," Witbooi told her audience.
She indicated that Namibian women, if not all women in Africa, have a serious concern about their fellow women who are suffering in countries such as the Democratic Republic of Congo, Burundi, Nigeria, Central Africa Republic and Palestine.
"We support Aspiration 4 of the Africa Agenda 2063 for a peaceful and secure Africa, that by 2020 guns will be silent," the new deputy minister stated.
Africa Agenda 2063 is a visionary statement and action plan by the African Union to have African societies utilise the sources of their rich continent in ways that benefit its people.
She then called on Namibian women to rededicate their efforts in whatever they are doing to shape the future of Namibian children, and to be their role models at all cost.
Witbooi wants to see women's empowerment starting within the women themselves. She used the same platform to urge all political parties in Namibia to adopt a zebra listing, which aims at achieving 50/50 (equal) men and women representation in decision-making organs.
"Namibia held a very successful election in 2014 and we are very proud to say the number of women in politics, especially in the National Assembly (NA), has increased tremendously from 24 to 46 per cent," she noted.
Namibia's achievement of 46 per cent women's representation in the NA, Witbooi said, is a big step towards the achievement of the Southern African Development Community (SADC) Protocol on Gender target of 50 per cent women's representation by 2015.
She expressed hope that the remaining 4 per cent of women's representation in the NA will be achieved in the Regional and Local Authorities elections expected to take place later this year, as well as the next general elections in four years' time.
Speaking at the same event, Coordinator of the SPWC in the Omusati Region, Rachel Shoopala encouraged the women of her region to avail themselves for election as councillors during the upcoming Regional and Local Authorities elections.
"The Omusati Regional Council has only one woman councillor all these years, but I want to see seven women councillors to five men councillors in our regional council after the forthcoming elections," Shoopala urged.
The International Women's Day aims that all nations worldwide eliminate all forms of discrimination against women, focussing on helping women gain full and equal participation in the socio-economic and political development. The Day is celebrated on 08 March each year.


7 billion people share this planet. 145,000 people share this city. Who are we? What do we look like? What can we learn from others?
Understanding Barrie's diversity helps ensure our community considers the needs of all residents. It allows for a better understanding of different perspectives that residents bring from across Canada and the world, to help our community grow economically and socially. It is important to understand who we are to better plan for residents who have been here for generations and for those who are new to Barrie.
Using statistics from 2014, we have reduced Barrie to a village of 100 people so it's easier to understand and appreciate our diversity. This is our village, and it includes you.
Source: Environics Analytics. DemoStats 2014, Environics Analytics acquires and distributes Statistics Canada files in accordance with the Government of Canada's Open Data Policy. No confidential information was provided by Statistics Canada.
Source: Statistics Canada, 2011 National Household Survey, Statistics Canada Catalogue no. 99-012-X2011032.
Source: Statistics Canada. 2013. Barrie, CY, Ontario (Code 3543042) (table). National Household Survey (NHS) Profile. 2011 National Household Survey. Statistics Canada Catalogue no. 99-004-XWE. Ottawa. Released September 11, 2013. (accessed May 26, 2015).
Lesbian, Gay, Bisexual and Transgender (LGBT) individuals, people with disabilities (including physical, visual, hearing, developmental disability, learning disability, brain injury and mental health issues) and individuals who live below the poverty line all live in our village.
Reliable ways to quantify or categorize demographics about sexual orientation and gender identity, people with special needs and those who live below the poverty line have not been established so far so we are unable to report how many villagers identify in these categories.
• representatives from Barrie and Area Chinese Community Association, Adams Law Office, CFB Borden, Barrie Chamber of Commerce, and The Barrie Examiner.


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Home Nona "Nick's Of North Adelaide"
Nona "Nick's Of North Adelaide"
Home > Australia > SA > North Adelaide > Nona "Nick's Of North Adelaide"
Italian Restaurant, Cafe
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41 O'Connell Street North Adelaide, SA, Australia
Hawaiian Restaurant
47 O'Connell Street, North Adelaide, SA, Australia
Burger Restaurant, Fast Food Restaurant, Fish & Chips Restaurant
Blue and White Cafe
43 O'Connell Street North Adelaide, Adelaide, SA, Australia
Hours: Tue-Thu: 11:00 - 01:00; Fri,Sat: 11:00 - 03:00; Sun: 13:00 - 00:00
Fast Food Restaurant, Fish & Chips Restaurant, Cafe
Blue & White Cafe
Discover restaurants in North Adelaide
Most Popular Restaurants in North Adelaide
Asian Fusion Restaurant, Thai Restaurant
Gin Long Canteen
Cuisines: Asian Fusion, Thai, Vietnamese
Hours: Tue-Fri: 12:00 - 14:30; Sat: 17:30 - 22:30
Zaep Tastes Of Thailand
Cuisines: Thai
Hours: Open Now Mon: 17:00 - 22:00; Wed-Sun: 11:30 - 15:00
Barbecue Restaurant, Wine Bar
Pink Pig Wine Bar
50 O'Connell St, North Adelaide, SA, Australia
Cuisines: Barbeque