HAT-P-6b: A Hot Jupiter transiting a bright F star

0.27 MB·

by  R. W. Noyes

Draftversion February2,2008– VERSION14
PreprinttypesetusingLATEXstyleemulateapjv.12/14/05
HAT-P-6b: A HOT JUPITER TRANSITING A BRIGHT F STAR †
R. W. Noyes1, G. A´. Bakos1,2, G. Torres1, A. Pa´l1,3, G´eza Kova´cs4, D. W. Latham1, J. M. Ferna´ndez1,
D. A. Fischer5, R. P. Butler6, G. W. Marcy7, B. Sipo˝cz3,1, G. A. Esquerdo1, Ga´bor Kova´cs1, D. D. Sasselov1,
B. Sato8, R. Stefanik1, M. Holman1, J. La´za´r9, I. Papp9 & P. Sa´ri9
Draft versionFebruary 2, 2008 – VERSION 14
ABSTRACT
IntheongoingHATNetsurveywehavedetectedagiantplanet,withradius1.33 0.06R andmass
Jup
±
1.06 0.12M , transiting the bright (V =10.5) star GSC 03239-00992. The planet is in a circular
8 ± Jup
orbit with period 3.852985 0.000005days and mid-transit epoch 2,454,035.67575 0.00028(HJD).
0 ± ±
The parent star is a late F star with mass 1.29 0.06M , radius 1.46 0.06R , T 6570 80K,
0 ⊙ ⊙ eff
2 [Fe/H] = 0.13 0.08 and age 2.3+0.5Gy. W±ith this radius and m±ass, HAT-P-6b∼has som±ewhat
− ± ∼ −0.7
largerradiusthantheoreticallyexpected. Wedescribetheobservationsandtheiranalysistodetermine
n
physical properties of the HAT-P-6 system, and briefly discuss some implications of this finding.
a
J Subject headings: stars: individual (GSC 03239-00992,HAT-P-6) – planetary systems

3
1
1. INTRODUCTION better than 2% light curve rms. The field was observed

in network mode, whereby at the end of its nightly ob-
] The detection of transiting exoplanets is very impor-
h servingsequencetheHAT-6telescopeinArizonahanded
tant to exoplanet research because of the information
p offto the HAT-9telescopeinHawaii,thus extending the
about both planetary radius and mass that comes from
- durationofcontinuous observations. Following standard
o photometric transit light curves combined with follow-
frame calibrationprocedures,astrometry was performed
r up radial velocity observations. The transiting exoplan-
t as described in Pa´l & Bakos (2006), and aperture pho-
s ets known as of this writing span a wide range in the
a physical parameter space of planetary mass, radius, or- tometry results were subjected to External Parameter
[ bital period, semi-major axis, eccentricity; and parent Decorrelation (EPD, described briefly in Bakos et al.
star parameters, including mass, radius, effective tem- 2007a),andtheTrendFilteringAlgorithm(TFA;Kov´acs
3
etal.2005). Wesearchedthelightcurvesforbox-shaped
v perature, metallicity, and age. Filling out their distri-
transit signals using the BLS algorithm of Kov´acs et al.
4 bution in this multidimensional space is certain to give
(2002). A very significant periodic dip in intensity was
9 us important information on the origin and evolution of
detected in the I 10.6 magnitude star GSC 03239-
8 exoplanetary systems. Here we report on the discovery
≈
00992 (also known as 2MASS 23390581+4227575, with
2 by HATNet of its sixth transiting planet, HAT-P-6b, an
. inflated Jupiter-mass gas giant in an essentially circu- a depth of 9 mmag, a period of P = 3.8529days, and a
0
duration of 3.1 hours.
1 lar orbit about an F dwarf star with slightly sub-solar
7 metallicity.
0
: 2. PHOTOMETRICDETECTION 9.73 a)
v mag 9.74
i The HATNet telescopes HAT-6 and HAT-9 (HATNet; I 9.75
X
Bakos et al. 2002, 2004) observed HATNet field G161,
-0.4 -0.2 Phase 0.2 0.4
r centered at α=00h32m, δ =+37◦30′, on a near-nightly 9.92
a
bhaavsies gfraotmher2e0d05alAtouggeutshter1295t5o02050-m5iDneecxempobseurre1s6,.eaWche g (inst) 99..9934 b)
yielding photometric measurements for approximately ma
35,000 stars with I < 14 and about 10,000 stars with z 9.95
9.96
1Harvard-Smithsonian Center for Astrophysics, Cambridge, -0.15 -0.1 -0.05 T - TC (days) 0.05 0.1 0.15
MA,[email protected] Fig. 1.— (a) Unbinned instrumental I-band discovery light
2HubbleFellow curve of HAT-P-6 obtained with HATNet, folded with the pe-
3Department of Astronomy, Eo¨tvo¨s Lora´nd University, Bu- riod of P = 3.852985 days. Superimposed (larger dots) is the
dapest,Hungary. same data binned to 1/200 in phase. (b) Unbinned instrumen-
4KonkolyObservatory,Budapest, Hungary talSloanz-bandphotometrycollectedwiththeKeplerCamatthe
5Department of Physics and Astronomy, San Francisco State FLWO1.2m telescope on2006 October 26(top curve) andagain
University,SanFrancisco,CA on UT 2007 September 4 (next curve); superimposed on both is
6Department of Terrestrial Magnetism, Carnegie Institute of ourbest-fittransitmodelcurve(seetext).
Washington, DC
7Department of Astronomy, University of California, Berkeley,
CA
8TokyoInstituteofTechnology, Tokyo,Japan TheHATNet discoverylightcurveis showninFig.1a.
9HungarianAstronomicalAssociation,Budapest, Hungary As is shownin the following sections we deduce that the
† Based in part on observations obtained at the W. M. Keck signal is due to the transit of a Jovian planet across the
Observatory,whichisoperatedbytheUniversityofCaliforniaand face of the star. Hereafter we refer to the star as HAT-
theCaliforniaInstituteofTechnology. Kecktimehasbeeninpart
P-6, and to the planetary companion as HAT-P-6b.
grantedbyNASA(runN162Hr)andNOAO(runA285Hr).
2 Noyes et al.
coverage is 3800 8000 ˚A. An iodine gas absorption
TABLE 1 cell was use∼d to su−perimpose a dense forest of I lines
2
Relativeradial velocity measurementsof HAT-P-6
on the stellar spectrum and establish a highly accurate
wavelength fiducial (see Marcy & Butler 1992). In to-
(2,40B0J,0D00+) (mRsV−1) (mσRs−V1) tal15exposureswereobtainedbetween2006October14
and 2007 August 25 with the iodine cell, along with one
54022.70228........ +74.01 4.85 without I for use as a template. Relative radial veloci-
54023.78901........ +47.70 4.85 2
54085.81512........ −3.70 5.72 ties in the Solar System barycentric frame were derived
54130.72257........ +62.40 6.93 as described by Butler et al. (1996), incorporating full
54247.11201........ +67.25 4.55 modeling of the spatial and temporal variations of the
54248.08955........ −110.02 4.91
instrumental profile. Data and their internal errors are
54249.08558........ −94.78 4.23
listed in Table 1.
54250.12528........ +66.22 4.61
54251.08766........ +56.10 4.21
54258.11601........ +103.71 4.09 4. ANALYSIS
54279.09485........ −127.75 6.05
54286.12699........ −18.23 6.84 We determined the parameters of the star, and of the
54319.11890........ +32.41 4.30 transiting planet, from the combined photometric and
54336.87654........ −112.33 4.13 spectroscopic data by the following procedure.
54337.86117........ −59.68 4.41 First,theiodine-freetemplatespectrumfromKeckwas
used for an initial determination of the atmospheric pa-
3. FOLLOW-UPOBSERVATIONS rameters of the star. Spectral synthesis modeling was
HAT-P-6wasobservedspectroscopicallywiththe CfA carriedoutusing the SME software(Valenti &Piskunov
DigitalSpeedometer (Latham1992)atthe FLWO 1.5 m 1996), with wavelength ranges and atomic line data as
Tillinghastreflectorofthe FredL.Whipple Observatory described by Valenti & Fischer (2005). We obtained
(FLWO) in order to rule out the possibility that the ob- initial values as follows: effective temperature T =
eff
served drop in brightness is caused by a transiting low- 6353 88K, surface gravity logg = 3.84 0.12, iron
⋆
± ±
massstellarcompanionratherthanaplanet,aswellasto abundance [Fe/H] = 0.23 0.08, and projected rota-
characterizethe rotation and surface gravity of the star. tional velocity vsini =− 8.7 ±1.0kms−1. The tempera-
±
Seven spectra were obtained over an interval of 92 days. tureandsurfacegravitycorrespondtoanF8dwarf. The
Radial velocities were obtained by cross-correlationand uncertainties in SME-derived parameters quoted here
have a typical precision of 0.4kms−1. They showed no andinthe remainderofthis discussionaretwicethe sta-
variation within the uncertainties, ruling out a compan- tistical uncertainties; this reflects our attempt, based on
ionofstellarmass. Themeanheliocentricradialvelocity prior experience, to incorporate systematic errors.
is 22.7 0.5kms−1. Next, an initial modeling of the 2006KeplerCamlight
− ±
Photometric follow-up of HAT-P-6 was then carried curve was carried out using the formalism based on
out in the Sloan z-band with KeplerCam (see e.g. Hol- Mandel & Agol (2002), using the quadratic model for
man et al. 2007)on the FLWO 1.2 m telescope, on 2006 limb darkening without the assumption that the planet
October 26. An astrometric solution between the indi- issmall. Theinitialquadraticlimb-darkeningcoefficients
vidual frames and the 2MASS catalog was carried out (namely, γ = 0.1452 and γ = 0.3488) were taken from
1 2
using first order polynomials based on 400 stars per thetablesofClaret(2004)byinterpolationtotheabove-
∼
frame. Aperture photometry was performed using a se- mentionedSMEvalues. Theperiodwasinitially fixedat
ries of apertures in fixed positions around the 2MASS- thevaluegivenearlierfromtheHATNetphotometry,and
based(x,y)pixelcoordinates. Weselectedaframetaken theorbitwasassumedtobecircular,basedontheresults
near the meridian and used 260stars and their magni- from the radial velocity fit to be discussed below. The
∼
tudes as measured on this reference frame to transform four adjustable parameters are the planet-to-star ratio
all other frames to a common instrumental magnitude of the radii (R /R ), the normalized separation (a/R )
p ⋆ ⋆
system. The apertureyielding the lowestscatter outside where a is the semi-major axis of the relative orbit, the
oftransitwasusedin the subsequentanalysis. The light normalized impact parameter (b acosi/R ), and the
⋆
≡
curve was then de-correlated against trends using the time of the center of the transit (T ). Both for the ini-
c
out-of-transit sections and a dependence on hour angle tiallightcurvefitandthefurtherfits(seebelow)weused
(see Fig. 1b, upper curve). theMarkovChainMonte-Carlo(MCMC)methodtofind
A follow-up KeplerCam observation was recently ob- the best fit parameters (see, e.g. Ford 2004, for a com-
tained (2007 Sep 4), for the purpose of improving the prehensive description). To estimate errors we used the
photometric accuracy of the transit curve model, and method of refitting to synthetic data sets to determine
alsotodeterminetheorbitalperiodandmid-transittime their uncertainties and correlations. The synthetic data
with maximum accuracy. The data were treated identi- sets consist of the analytic (fitted) model plus Gaussian
callytothoseforthe2006October26transit;resultsare and red-noise, based on both white-noise and red-noise
shown in the lower curve of Fig. 1b. estimates of the residuals. The characteristicsof the red
Following the first KeplerCam observation, high res- noise component of the residuals were preserved by per-
olution spectroscopy was initiated with the HIRES in- turbing only the phase of their Fourier spectrum. We
strument (Vogt et al. 1994) on the Keck I telescope, in found that this method of error estimation is preferable
orderbothtodeterminethestellarparametersmorepre- to direct estimation using the MCMC method, since it
cisely and to characterize the radial velocity signal due is not sensitive to the number of out-of-transit points
to the companion. With a spectrometer slit of 0′.′86 the used. We also note that instead of a/R and b, we used
⋆
resolving power is λ/∆λ 55,000, and the wavelength the parameters ζ/R and b2 for the fit, where ζ is an
⋆
≈
HAT-P-6b: Transiting Hot Jupiter around a bright F star 3
TABLE 2 TABLE 3
StellarparametersforHAT-P-6. Spectroscopic andlightcurvesolutions forHAT-P-6, and
inferredplanetparameters
Parameter Value Source
Parameter Value
T[Feeff/H(K].)........................ −605.7103±±800.08 SSMMEEa Lightcurveparameters
vlosging⋆i((kcgms)s−..1.)......... 48.2.27±±01..003 YSM2+ELC+SMEb TPc((dHayJDs)−.2.,.4.0.0.,.0.0.0.).................. 543,.083552.9687557±50±.000.000000528
MLR⋆⋆⋆(((LRM⊙⊙⊙)))................................ 113..42.5697±±+−0000..5..4002366 YYY222+++LLLCCC+++SSSMMMEEE RTaT/11p42R/R⋆=(d⋆.aT.y..3s..4)..a.(.d....a....y...s...)...a............................................... 000.0..9107341.36868189±±±±0000....020002000115713
MV (mag)......... 3.36±0.16 Y2+LC+SME b≡acosi/R⋆................ 0.602±0.030
Age(Gyr)......... 2.3+0.5 Y2+LC+SME i(deg)....................... 85◦.51±0◦.35
Distance(pc)...... 260−±0.270 Y2+LC+SME ζ (R⋆/day).................. 15.696±0.086
aSME = Package for analysis of high-resolution spectra Valenti Spectroscopic parameters
&Piskunov(1996). K (ms−1)................... 115.5±4.2
bY2+LC+SME = Yale-Yonsei isochrones (Yi et al. 2001), light γ (kms−1).................. −22.7±0.5
curveparameters,andSMEresults. e............................ 0(adopted)
auxiliaryvariablewithdimensionsofvelocity,definedby Planetparameters
ζ 2πa/(cid:0)P√1 b2(cid:1). These parameters have been cho- Mp (MJ).................... 1.057±0.119
se≡ntoeliminate−thecorrelationbetweena/R⋆andb2(see ρRpp((gRcJm)−..3.)................................... 10..535380±±00..004671
also Bakos et al. 2007b). a(AU)...................... 0.05235±0.00087
Next, we used the values of Teff and [Fe/H] from the gp (ms−2) .................. 14.8±1.0
initial SME analysis, together with the initial value of a T14: total transit duration, time between first to last contact;
a/R⋆ from the Mandel-Agol fit, to estimate the stellar T12 =T34: ingress/egress time, timebetween first and second, or
properties from comparison with the Yonsei-Yale (Y2) thirdandfourthcontact.
stellarevolutionmodelsbyYietal.(2001). Thevalueof
as the one in the previous iteration to within uncertain-
a/R iscloselyrelatedtothestellardensity,andisthusa
⋆
ties, so we stopped the iteration at this point.
proxyforluminosity(L ). AsdescribedbySozzettietal.
⋆
¿From the value of vsini and the stellar radius R ,
(2007), a/R is typically a better constraint on L than ⋆
⋆ ⋆
and assuming an inclination of the rotational equator of
the spectroscopic value of logg , which has a relatively
⋆
approximately 90 deg (that is, similar to the inclination
subtle effect on the line profiles and whose determina-
of the planetary orbital plane), we estimate the stellar
tion is therefore more susceptible to systematic errors.
rotation period to be about 9 days. We have searched
FollowingSozzettiet al.(2007)we determined the range
theHATNetlightcurve(aftereliminationofdataduring
of stellar masses and radii that are consistent with the
transits)forperiodicitiesbetween6and12days,suchas
SME-determinedvaluesofT ,[Fe/H],anda/R derived
eff ⋆ might be produced by significant spots or other stellar
from the light curve. We obtained M = 1.19+0.12M
⋆ −0.10 ⊙ activity, and found no evidence for this.
and R⋆ = 1.45+−00..2117R⊙. The resultant surface gravity, Anindependentestimateoftheagewasobtainedfrom
logg = 4.19+0.08, was significantly larger than the ini- the Ca+ H and K line emissionstrength, measuredfrom
⋆ −0.10
tial SME-derived value discussed above. We fixed logg the mean of 14 Keck spectra: logR = 4.81, lead-
⋆ HK
−
atthis new, moreaccuratevalue, andrepeatedthe SME ing to an age of 2.8Gy (based on Noyes et al. 1984),
analysis. Fixing surface gravity slightly affects the so- consistent with the evolutionary track age. The lu-
lution for other parameters such as [Fe/H] and other minosity and T , imply an absolute visual magnitude
eff
individual element abundances as well as vsini. The M =3.36 0.16mag. Combined with the apparentvi-
V
±
correlationsbetween these free parametersin turn affect sual magnitude (V =10.440 0.036;Droege et al. 2006;
±
the final solution for effective temperature, causing it to Hoget al.2000),this yields a distance of260 20pc, ig-
±
change by about twice its original uncertainty. The re- noring extinction. For reference, the final values for the
sulting values from this iteration are T =6570 80K, stellar parameters listed above are given in Table 2.
eff
[Fe/H]= 0.13 0.08, and vsini=8.2 1.0km±s−1. Setting the difference between the transit centers of
− ± ±
We then performed a second iteration of the above the two KeplerCam light curves, T T , to 81 or-
c2 c1
−
steps using the new values of T ,logg , and [Fe/H], as bital periods, we obtain a more accurate value for the
eff ⋆
well as correspondingly changed limb darkening coeffi- period: P = 3.852985 0.000005 days. This value,
±
cents: γ = 0.1211 and γ = 0.3646. This iteration also and the reference epoch of mid-transit, T T =
1 2 c c1
≡
incorporated both the 2006 and 2007 KeplerCam light 2,454,035.67575 0.00028, are given in Table 3. Also
±
curves(Fig.1b)into a single fit, whichyieldedthe times giveninTable3arethefinalfittedlightcurveparameters
of each transit center T and T , as well as the shape a/R ,R /R ,b,i(orbitalinclination),andthe radiusof
c1 c2 ⋆ p ⋆
parameters a/R , R /R , and b, which we assumed to the planet, R = 1.330 0.061R , as determined from
⋆ p ⋆ p J
±
be the same for both of the transit events. R and R /R . The modeled z-band transit light curve
⋆ p ⋆
Finally, usingthe new values ofa/R , T , and[Fe/H] is shownas a solid line superimposed on the data points
⋆ eff
together with the Y2 evolutionary models discussed in Fig. 1b.
above, we re-determined the stellar parameters. Table 2 The Keck radial velocity data were initially fit with a
summarizes these, which include a further refined deter- Keplerian model with period and epoch constrained to
mination of logg =4.217+0.029. This value is the same the value determined from the photometry ( 2) and no
⋆ −0.027 §
4 Noyes et al.
150 et al. (2007) (i.e. WASP-1b, HAT-P-4b, HD 209458b,
a) TrES-4, and HAT-P-1b). However, its mass of 1.06M
m/s) 100 isgreaterthanthemassofanyofthese,andhenceithaJs
adial velocity ( - 55 000 aopflalaintresgtemgriamvsesen,abnaygdFeepnos=fit2yL.3⋆a/nG(d4yπs,uaar2fn)a,dcmesotgderleallavsriotyffl.BuFxuorFrropawasptleattnahelet.
R -100 (2007) predict a radius of about 1.21 R , assuming that
J
-150 theplanethasnoheavy-elementcore. The metallicityof
O-C (m/s) -22055 b) HkbnuAolkTw-cnPot-mr6a,pn[oFssieit/tiinHogn]p=olaf−nH0eAt.1Th3o-±Pst0-.6s0tb8a,rtsirs.aacIkmfswotenhgaestshmuemestmealtlahilclaiettsytthooeff
S (m/s) -22055 c) istmsahlol,stbusttanr,otthveansiizsehionfgiltysshoe.avTyh-uesletmheenptrceodriectsehdouralddibues
B 0 0.2 0.4Phase 0.6 0.8 1 fromBurrowsetal.(2007)iscomparableto,butperhaps
slightly higher, than one might expect for HAT-P-6b.
Fig. 2.—(a)Radial-velocitymeasurementsfromKeckforHAT-
However, the actual radius found here, R = 1.330
P-6,alongwithanorbitalfit,shownasafunctionoforbitalphase. p
±
Thecenter-of-massvelocityhasbeensubtracted. (b)Phasedresid- 0.061, lies above the predicted value by about 2σ, so it
uals after subtracting off the orbital fit. The rms variation of the appears to be somewhat inflated relative to that model.
residuals is about 8.6ms−1. (c) Bisector spans (BS) for the 16 Hansen & Barman (2007) proposed that hot jupiters
Keck spectra plus the singletemplate spectrum, computed as de-
can be placed into two classes based on their equilib-
scribedinthetext. Themeanvaluehasbeensubtracted. Vertical
scaleforallthreepanelsisthesame. rium temperature and Safronov number Θ, where Θ
≡
(a/R ) (M /M ) is the ratio of the escape velocity
constraint on eccentricity. We found an eccentricity of p × p ⋆
from the surface of the planet to the orbital velocity.
e = 0.046 0.031, not significantly different from zero.
± When Safronov number is plotted versus equilibrium
Therefore the data were re-fit with a circular orbit, in
temperature,transitinghotjupitersseemtofallintotwo
which both the period P and the mid-transit time T
c groups, with an absence of objects between. However,
were held fixed at their values from the light curve anal-
theSafronovnumberforHAT-P-6bis0.064 0.004;along
ysis(Table3). Thesolutionfitsthedatawell;seeFig.2a. ±
withHAT-P-5b(Bakosetal.2007b)withSafronovnum-
No long-term trends are seen in the residuals.
ber 0.059 0.005, these two planets appear to fall be-
In order to get a reduced chi-square value near unity ±
tween the two groups in such a plot. Hansen & Barman
for the fit, it was necessaryto addanadditionalrandom
also noted a difference in the relation between planet
noisecomponentwithamplitude8.6ms−1inquadrature
massandequilibriumtemperatureforplanets ofthe two
to the internal errors. This is essentially identical to the
classes, but HAT-P-6b and HAT-P-5b appear to fall be-
8.7 ms−1 radial velocity “jitter” expected to arise from
tween the two classes in this respect as well. It would
stellar surface activity, based on the above-mentioned
seemthatdiscoveryandcharacterizationofalargenum-
strengthof the emissioncoresof the Ca+ H and K lines,
ber of additional transiting exoplanets may be neces-
logR′ = 4.81 (Wright 2005). The parameters of
HK − sary to establish unambiguously whether there is a bi-
theresultingfinalfitarenotsignificantlychangedbythe
modal distribution of hot jupiter planets according to
inclusion of this jitter, and are listed in Table 3.
their Safronov number.
Following Torres et al. (2007), we explored the pos-
sibility that the measured radial velocities are not real,
butinsteadduetodistortionsinthespectrallineprofiles
duetocontaminationfromanearbyunresolvedeclipsing
binary. In that case the “bisector span” of the aver-
agespectrallineshouldvaryperiodicallywithamplitude
and phase similar to the measured velocities themselves
(Quelozetal.2001;Mandushevetal.2005). Instead,we Operation of the HATNet project is funded in part
detect no variation in excess of the measurement uncer- byNASAgrantNNG04GN74G.Weacknowledgepartial
tainties(seeFig.2,bottompanel). Weconcludethatthe support also from the Kepler Mission under NASA Co-
velocity variations are real and that the star is orbited operativeAgreementNCC2-1390(D.W.L., PI).G.T.ac-
by a Jovian planet. knowledges partial support from NASA under grant
Combined with the results from the light curve and NNG04LG89G, and work by G.A´.B. was supported by
radial velocity modeling, the above stellar parameters
NASA through HST-HF-01170.01-A Hubble Fellowship
yieldaplanetmass ofM =1.06 0.12M . The surface
p J Grant. G.K. and A.P. thank the Hungarian Scientific
±
gravity, gp = 14.8 1.0ms−1, was obtained from the ResearchFoundation(OTKA)forsupportthroughgrant
±
light curve and radial velocity fits (see Southworth et K-60750. A.P. would like to thank the hospitality of the
al. 2007). The mean density and its uncertainty, ρp = CfA,wherethisworkhasbeenpartiallycarriedout,and
0.558 0.047gcm−3, follow from the absolute radius of acknowledge support from the Doctoral Scholarship of
±
the planet. All planet parameters are listed in Table 3. Eo¨tv¨os University. This research has made use of Keck
telescope time granted through NASA and NOAO, of
5. DISCUSSION the VizieR service (Ochsenbein et al. 2000) operated at
HAT-P-6b, with radius 1.33R , is similar in size to CDS, Strasbourg, France, of NASA’s Astrophysics Data
J
five low density “inflated” planets tabulated by Kov´acs System Abstract Service, and of the 2MASS Catalog.
HAT-P-6b: Transiting Hot Jupiter around a bright F star 5
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