\documentclass{esoform} 
\begin{document}

%---- BOX 1 ------------------------------------------------------------

\Cycle{74A}

\Title{Mapping the Realm of Hot Jupiters}

\SubCategoryCode{C7}

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\Abstract{As part of an international consortium aimed at identifying
new hot Jupiters, we propose to measure precise radial velocities for a
subsample of several hundred stars out of a bigger sample of 2000~stars 
not currently surveyed by ongoing Doppler searches.
The sample stars have been selected based on Stroemgren photometry to
have at least solar metallicity, in order to 
enhance the chances of finding new planets.
The samples of currently on-going Doppler Surveys have already been culled
from virtually all short-period gas giant planets, leading to a stagnant
pool of about 20 hot Jupiters. In order to advance our understanding
of planet structure, atmospheres, and orbital migration, additional
short-period, multi-planet systems with observable non-Keplerian interactions
or planetary transits have to be detected.
Our observing strategy is exactly designed to fulfill this task, dropping any
star from the list that does not show significant radial velocity variations
during three consecutive nights.}

%---- BOX 3 ------------------------------------------------------------

\ObservingRun{A}{74}{HARPS}{6n}{any}{n}{n}{THN}{v}
\ObservingRun{B}{74}{UVES}{3n}{any}{n}{n}{THN}{v}

%---- BOX 4 ------------------------------------------------------------

\FutureNights{3.6m/UT2}{6n/3n}

%---- BOX 5 ------------------------------------------------------------

\SpecialRemarks{Minimum useful time allocation would be 3 half nights
on either telescope.}

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\PI{A.}{Quirrenbach}{Sterrewacht Leiden}{NL}{quirrenbach@strw.leidenuniv.nl}

\CoI{S.}{Frink}{Sterrewacht Leiden}{NL}
\CoI{D.}{Fischer}{San Francisco State University}{USA}

%---- BOX 7 ------------------------------------------------------------

%\Thesis{}{}

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\ScientificRationale{Extrasolar Planet Searches and their implications are one
of the hot topics in astronomy right now, gaining attention not only from
scientists, but also from the wider public. One of the most surprising results
of the early Doppler surveys
was the discovery of hot Jupiters, gas giant planets of several Jupiter masses
that orbit very closely to the parent stars, with orbital periods of only a few
days (see e.g.\ the discovery paper of 51~Peg, Mayor \& Queloz 1995, 
Nature~378, 355).
These discoveries have spawned a whole new research field, including the
development of theoretical arguments for the existence of such planets
as well as new observational methods to detect and characterize such
objects, including a number of space missions to be carried out in the coming
decade. The planetary transit observed for HD~209458 has confirmed the gas
giant hypothesis for this object (along with the astrometrically observed
system GJ~876 the only two ones for which we have reasonably accurate
planet masses), and lead to the first discovery of a planetary atmosphere
by HST (Charbonneau et al.\ 2002, ApJ~568, 377).
\smallskip

Hot Jupiters provide:
\medskip

%\hspace*{-3cm}
\begin{minipage}{16.5cm}
\begin{itemize}
\item {\bf High probability transit candidates:}\\
The detection of a planet transiting HD~209458 (Charbonneau et al.\ 2000,
ApJ~529, L45; Henry et al.\ 2000, ApJ~529, L41) 
has garnered about 200 citations in the literature
and spawned 22 transit search projects (Horne 2003, ASP Conf.\ Ser.~294, 
361). The quality of physical information about
HD~209458b, made possible by the transit observation, far
exceeds that of any other known exoplanet. The scientific yield from this
transit was only possible because the intrinsic brightness of the host star
enabled high temporal resolution HST photometry. The detection of 60 new hot
Jupiters will statistically yield {\bf three new transiting planets around 
bright, nearby stars}. These transits will provide high quality information 
about planet radii, densities, atmospheres, interior structure and heating.
\item {\bf Tracers of multiple planet systems with orbital periods short enough
to exhibit non-Keplerian interactions:}\\
Of the planet-bearing stars which have been detected with the Lick RV survey,
over half appear to have at least one additional planet in the system
(Fischer et al.\ 2001). Among these, the $\Upsilon$~And and 55~Cnc systems 
(which both have hot Jupiters) have greatly deepened and constrained our
understanding of chaotic orbital evolution, disk migration, and the dynamics of
resonances. A resonant configuration with an inner planet period of about three
to ten days would show strong non-Keplerian interactions on easily observed 
timescales.
\item {\bf Constraints on tidal dissipation indicating the presence or absence 
of a core:}\\
As more planets are discovered with periods between three and ten days, the
free parameters in the tidal circularization theory will become
over-constrained and reveal internal structure in hot Jupiters.
\item {\bf Statistical anomalies such as a pile-up in orbital periods at three
days, systematically lower planet masses and higher stellar masses:}\\
All of these statistical anomalies are in need of confirmation, which can only
be provided by finding more short-period planets.
\end{itemize}
\end{minipage}
\medskip

These fundamental discoveries confirmed the gas-giant nature of the first
Doppler-detected planets, revealed and deepened our understanding of orbital
migration, allowed the detection of orbital resonances and demonstrated
non-Keplerian interactions. However, a stagnant sample of about 20 hot Jupiters
now serves as the test cases for theory. Significant advances in our
understanding of planet formation, migration and evolution require many new hot
Jupiters. The only way to find these planets is to survey a fresh sample of stars.
}

\ImmediateObjective{Here we propose to measure precise radial velocities of a 
sample of about 200~FGK~stars, pre-selected to exclude stars of low metallicity
as well those stars already routinely observed by ongoing Doppler surveys,
with an observing strategy designed to efficiently identify the hot Jupiters
in such a sample.
Monte Carlo simulations (see {\bf Fig.~1}) show that RV measurements obtained on
three consecutive nights with a precision of 7~m/s will identify $>3\sigma$
RV velocity scatter in virtually all stars hosting planets more massive than
0.5~$M_{\mbox{\tiny Jup}}$  with orbital periods between 1.25 and 14~days. 
Velocity trends
for more massive planets with orbital periods up to one year and double- and
single-lined spectroscopic binaries will also be identified.

The rate of occurrence of extrasolar planets with periods less than
14~days is about {\bf 1.5\%}. Note that this rate is higher than the 
usual 0.75\%
(e.g.\ Butler et al.\ 2001, ApJ~555, 377) because the orbital period range 
to which we
are sensitive here extends beyond three to five day orbits. These numbers hold
for a parent sample of stars which is not selected according to metallicity.
Our detection rate of hot Jupiters should even be somewhat {\bf higher} 
than those
numbers because we preferentially selected stars of approximately solar or higher
metallicity, based on a photometric $uvby$ calibration (Martell \& Laughlin
2002, ApJ~577, L45). This calibration is accurate to 0.1~dex, more than
sufficient for our purpose of rejecting the more metal-poor stars.
Reddening is not taken into account, since our stars are typically closer
than 100~pc where any reddening is only a small correction. Since we
are not interested in the highest possible accuracy metallicities here,
it is completely negligible.

{\bf Figure~2} quantifies the planet-metallicity correlation: stars with
solar or higher metallicity are far more likely to host Doppler-detectable
planets than metal-poor stars.

Thus, if our detection rate of hot Jupiters was around 3\%, we would be able
to identify of the order of {\bf 60~fresh hot Jupiters} in a parent sample of 
2000~stars pre-selected for metallicity, observed by our consortium. 
The same detection rate would yield about six new hot Jupiters for the sample
of about 200~stars we propose to observe in the framework of this proposal.

We would like to stress again that we do not propose to perform a full radial
velocity monitoring campaign for those stars, but rather a fast test as to
whether those systems might harbor hot Jupiters or not. If any given star
observed during three consecutive nights does not show radial velocity jitter
at a level larger than 3~$\sigma$, we will drop this star from our lists and
never observe it again.

The success of the current proposal as well as that the whole
consortium critically depends on whether we manage to observe a large enough
sample in order detect a statistically significant number of new hot Jupiters.
The consortium members consists of observers from the US (Keck), 
Chile (Magellan) and Japan (Subaru). While our first ESO proposal for this
project was rejected, the proposals of all other consortium partners 
were accepted, resulting in four nights of Keck time, three nights of
Magellan time, and four nights of Subaru time (all of what was requested).
So this project is definitely going ahead, with or without ESO participation.
While the majority of the observing time is still to come, the first
five hot Jupiter candidates have already been identified (see {\bf Fig.3}
for one example), and follow-up radial velocity observations as well as
photometry is now underway. 

As mentioned earlier, our goal as a consortium is to
observe a sample of about 2000~stars within a few years. Our list for the
current proposal contains about 300~targets. Most of them are suitable for
HARPS, but since fast troughput is essential for our program, it is not
efficient to observe stars with HARPS for which integration times would
be larger than about 5~minutes (which occurs at about 8~mag for a target
S/N of larger than 100, which should give us radial velocities with 7~m/s
precision). However, since we pre-selected according to metallicity, some of
our stars lie in the magnitude range between 8 and 10~mag, and those can
only be efficiently observed with UVES.
}

\TelescopeJustification{We require a high resolution spectrograph which is
capable of producing radial velocities with a precision of 7~m/s.
The only available choices are therefore HARPS at the 3.6m and UVES at the UT2.
We decided to divide the observing program between those two spectrographs, using
HARPS whenever possible to reduce the observing load at the VLT. However, 
many of our stars are too faint to be efficiently observed with HARPS, so that
we also require UVES time for a successful execution of this program.}

\ModeJustification{We propose to perform these observations in visitor mode,
since our target list is very large and might require ad-hoc decisions about 
which stars to observe. Furthermore, we definitely want to use the output
of the pipeline reduction mode for HARPS, which is currently only
accessible in visitor mode. Similarly, iodine cell observations with UVES
are also best performed in visitor mode.}

\Strategy{Data reduction is straightforward. For HARPS, the pipeline directly
outputs science grade radial velocities, which we plan to use for this 
project. For UVES, we will follow a different measurement and data reduction
philosophy. In order to be able to measure precise radial velocities with
UVES, we plan to use the iodine cell technique. After standard flatfielding
and extraction of the spectrum, which is done by the ESO pipeline, the 
reduced data will be fed into the radial velocity pipeline developed by
Marcy \& Butler, which is available to us for the purpose of this project.
A synthetic template will be used, eliminating the need for an additional
template observation of each star and thus reducing the observing load
by 25\%. The resulting velocity precision is sufficient for our project 
flagging hot Jupiters,
which can then be followed up with a traditional template yielding
higher precision radial velocities.

An additional pipeline for spectral synthesis was developed by Fischer \&
Valenti and will also be used for this project. In addition to T$_{\mbox{eff}}$, 
[Fe/H] and $v\cdot \sin i$, problematic double-lined spectroscopic binaries
as well as chromospherically active stars will be readily identified.

All investigators have experience with high precision radial velocity work,
and facilities and computers to conduct the data reduction are available at
all participating institutes.}


\MakePicture{detectability.pdf}{\vspace*{-1cm}}{angle=90,width=8cm}
\MakeCaption{{\bf Fig.1:} The mean number of sigma (in RMS velocity
scatter) is plotted as a function of the orbital period. Different phases
of theoretical Keplerians for a 0.5~M$_{\mbox{Jup}}$ companion were
tested with a Monte Carlo simulation of observational data, assuming
7~m/s Doppler precision. Chromospherically quiet stars with more
than 3$\sigma$ RV scatter are strong candidates for harboring hot Jupiters.}


\MakePicture{fe_bargraph.pdf}{\vspace*{-1cm}}{angle=90,width=8cm}
\MakeCaption{{\bf Fig.2:} Abundance analysis of FGK stars on the Keck,
Lick and AAT planet search projects, quantifying the planet-metallicity
correlation (Fischer \& Valenti 2003, ASP Conf.\ Ser.\ 294, 117). The
subset of 767~stars represented here have sufficient observations to
rule in (or out) the presence of a gas giant planet with an orbital
period less than 2~years.}


\MakePicture{hotjup.pdf}{\vspace*{-1cm}}{angle=90,width=8cm}
\MakeCaption{{\bf Fig.3:} One out of five new hot Jupiter 
candidates that have been identified with Keck time to this project
so far. Follow-up radial velocities as well as photometry to search
for possible transits are underway.}


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\WhyLunarPhase{For radial velocity observations there are no 
restrictions regarding lunar phase.}

\WhyNights{In order to detect a significant number of new hot Jupiters,
a large parent sample of stars has to be observed. Our parent sample
to be observed by the international consortium as a whole thus consists 
of about 2000~stars, out of 
which we expect to detect around 60~new hot Jupiters. We propose here
to observe a subsample of 200~stars out of those 2000~stars in total,
so that we can expect to detect about 6~new hot Jupiters. Smaller numbers 
of nights would be possible, for example half-nights instead of
full nights, but the main aim of the proposal - detecting a {\bf statistically
significant} sample of new hot Jupiters - would be somewhat compromised.
Note that is critical to our scientific goals to obtain measurements at
3 different epochs (3 continuous nights are preferred).
We expect to observe between 50 and 100 stars per full night at each telescope.
Once integration times become larger than 5 minutes in order to reach a S/N
of at least 100 (for a radial velocity precision of 7~m/s), we will observe
it with UVES instead HARPS; that implies that stars which are fainter than
$V\approx8$~mag will have to be observed with UVES.
}

\StandardCalibrations

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\LastObservationRemark{
}

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\Publications{
Fischer, D.A., Marcy, G.W., Butler, R.P., Vogt, S.S., Walp, B., Apps, K.,
2002, PASP, 114, 529: Planetary Companions to HD~136118, HD~50554, and
HD~106252
\smallskip\\
Fischer, D.A., Marcy, G.W., Butler, R.P., Laughlin, G., Vogt, S.S.,
2002, ApJ, 564, 1028: A Second Planet Orbiting 47~Ursae Majoris
\smallskip\\
Fischer, D.A., Marcy, G.W., Butler, R.P., Vogt, S.S., Henry, G.W.,
Pourbaix, D., Walp, B., Misch, A.A., Wright, J.T., 2003, ApJ, 586, 1394:
A Planetary Companion to HD~40979 and Additional Planets Orbiting
HD~12661 and HD~38529
\smallskip \\
Fischer, D.A., Butler, R.P., Marcy, G.W., Vogt, S.S., Henry, G.W.,
2003, ApJ, 590, 1081: A Sub-Saturn Mass Planet Orbiting HD~3651
\smallskip \\
Fischer, D.A., Valenti, J.A., 2003, ASP Conference Series, 294, 117:
Metallicities of Stars with Extrasolar Planets
\smallskip \\
Frink, S., Mitchell, D.S., Quirrenbach, A., Fischer, D.A., Marcy, G.W.,
Butler, R.P., 2002, ApJ, 576, 478: Discovery of a Substellar Companion 
to the K2~III Giant $\iota$~Draconis
\smallskip \\
Mitchell, D.S., Frink, S., Quirrenbach, A., Fischer, D.A., Marcy, G.W.,
Butler, R.P., 2004, submitted to ApJ: Sub-Stellar Companions to K~Giant
Stars $\tau$~Gem, HD~59686, $\nu$~Oph, and 91~Aqr
}

%---- BOX 12 -----------------------------------------------------------

\Target{A}{HIP 58579}{12 00 48}{--12 09 27}{0.2}{7.96}{}{[Fe/H]=0.19, G0}{}
\Target{B}{HIP 59077}{12 06 55}{--38 06 23}{0.2}{9.35}{}{[Fe/H]=--0.01, G8/K0}{}

\TargetNotes{Our target list for this proposal consists of about 300~stars
and did not fit entirely onto the one page limit. We therefore provide the
first few stars of each of the lists for HARPS (run~A) and UVES (run~B)
as an example. The stars span the whole range right ascension range
accessible during the months from October to March, and have all southern
declinations. For HARPS, the stars are brighter than 8.5~mag in V, 
and brighter than about 10~mag for UVES. The last column gives our
derived {\bf metallicity} as well as the spectral type.}

%---- BOX 12b -- ESO Archive ------------------------------------------

\RequestedDataRemark{}

%---- BOX 13 -----------------------------------------------------------

\RunSplitting{A}{3,100w,3}
\RunSplitting{B}{3}

%\TimeCritical{A}{12-may-04}{14-may-04}{parallel observation with HST} 

%\UnsuitableTimes{A}{12-may-04}{14-may-04}{International Conference}

%\Link{B}{after}{A}{10 days}
%\Link{B}{after}{A}{any}
%\Link{B}{simultaneous}{C}{}

%\SpecialRequirements{}{}

%\MovingTargets{A}{large proper motion, still to be estimated}

%---- BOX 14 -----------------------------------------------------------

%-----------------------------------------------------------------------
%---- HARPS at the 3.6 -------------------------------------------------
%-----------------------------------------------------------------------
%
\INSconfig{A}{HARPS}{spectro-Thosimult}{}
%\INSconfig{}{HARPS}{spectro-I2cell}{}
%\INSconfig{}{HARPS}{spectro-ObjA(B)}{}

%-----------------------------------------------------------------------
%---- UVES at the VLT-UT2 (KUEYEN) -------------------------------------
%-----------------------------------------------------------------------

%\INSconfig{}{UVES}{BLUE}{Standard setting: 346}
%\INSconfig{}{UVES}{BLUE}{Standard setting: 437}
%\INSconfig{}{UVES}{BLUE}{Non-std setting: provide HERE central wavelength}
%\INSconfig{}{UVES}{RED}{Standard setting: 520}
%\INSconfig{B}{UVES}{RED}{Standard setting: 580}
\INSconfig{B}{UVES}{RED}{Iodine cell standard setting: 600}
%\INSconfig{}{UVES}{RED}{Standard setting: 860}
%\INSconfig{}{UVES}{RED}{Non-std setting: provide HERE central wavelength}
%\INSconfig{}{UVES}{DIC-1}{Standard setting: 346+580}
%\INSconfig{}{UVES}{DIC-1}{Standard setting: 390+564}
%\INSconfig{}{UVES}{DIC-1}{Standard setting: 346+564}
%\INSconfig{}{UVES}{DIC-1}{Standard setting: 390+580}
%\INSconfig{}{UVES}{DIC-1}{Non-std setting: provide HERE central wavel.}
%
%\INSconfig{}{UVES}{DIC-2}{Standard setting: 437+860}
%\INSconfig{}{UVES}{DIC-2}{Standard setting: 346+860}
%\INSconfig{}{UVES}{DIC-2}{Standard setting: 390+860}
%\INSconfig{}{UVES}{DIC-2}{Non-std setting: provide HERE central wavel.}
%
%\INSconfig{}{UVES}{Field Derotation}{yes}
%\INSconfig{}{UVES}{Image slicer-1}{yes}
%\INSconfig{}{UVES}{Image slicer-2}{yes}
%\INSconfig{}{UVES}{Image slicer-3}{yes}
\INSconfig{B}{UVES}{Iodine cell}{yes}

\MakeProposal
\end{document}
