A&A 488, L47-L50 (2008)
DOI: 10.1051/0004-6361:200810273


Transiting exoplanets from the CoRoT space mission

V. CoRoT-Exo-4b: stellar and planetary parameters[*],[*]

C. Moutou1 - H. Bruntt2 - T. Guillot3 - A. Shporer4 - E. Guenther5 - S. Aigrain6 - J. M. Almenara7 - R. Alonso1 - M. Auvergne8 - A. Baglin8 - M. Barbieri1 - P. Barge1 - W. Benz9 - P. Bordé10 - F. Bouchy11 - H. J. Deeg7 - R. De la Reza12 - M. Deleuil1 - R. Dvorak13 - A. Erikson14 - M. Fridlund15 - M. Gillon16 - P. Gondoin15 - A. Hatzes5 - G. Hébrard11 - L. Jorda1 - P. Kabath14 - H. Lammer17 - A. Léger10 - A. Llebaria1 - B. Loeillet1,11 - P. Magain18 - M. Mayor16 - T. Mazeh4 - M. Ollivier10 - M. Pätzold19 - F. Pepe16 - F. Pont6 - D. Queloz16 - M. Rabus7 - H. Rauer14,21 - D. Rouan8 - J. Schneider20 - S. Udry16 - G. Wuchterl5

1 - LAM, UMR 6110, CNRS/Univ. de Provence, 38 rue F. Joliot-Curie, 13388 Marseille, France
2 - School of Physics A28, University of Sydney, Australia
3 - OCA, CNRS UMR 6202, BP 4229, 06304 Nice Cedex 4, France
4 - Wise Observatory, Tel Aviv University, Tel Aviv 69978, Israel
5 - Thüringer Landessternwarte, 07778 Tautenburg, Germany
6 - School of Physics, Univ. of Exeter, Exeter EX4 4QL, UK
7 - Instituto de Astrofísica de Canarias, 38205 La Laguna, Spain
8 - LESIA, CNRS UMR 8109, Obs. de Paris, 92195 Meudon, France
9 - Physikalische Institut Univ. Bern, 3012 Bern, Switzerland
10 - IAS, Université Paris XI, 91405 Orsay, France
11 - IAP, CNRS, Univ. Pierre & Marie Curie, Paris, France
12 - Observatório Nacional, Rio de Janeiro, RJ, Brazil
13 - IfA University of Vienna, 1180 Vienna, Austria
14 - Institute of Planetary Research, DLR, 12489 Berlin, Germany
15 - RSSD, ESA/ESTEC, 2200 Noordwijk, The Netherlands
16 - Obs. de Genève, Univ. de Genève, 1290 Sauverny, Switzerland
17 - IWF, Austrian Academy of Sciences, 8042 Graz, Austria
18 - IAG, Université de Liège, Allée du 6 août 17, Liège 1, Belgium
19 - RIU, Universität zu Köln, 50931 Köln, Germany
20 - LUTH, Obs. de Paris, 5 place J. Janssen, 92195 Meudon, France
21 - ZAA, Technical University Berlin, 10623 Berlin, Germany

Received 27 May 2008 / Accepted 14 July 2008

Aims. The CoRoT satellite has announced its fourth transiting planet (Aigrain et al. 2008, A&A, 488, L43) with space photometry. We describe and analyse complementary observations of this system performed to establish the planetary nature of the transiting body and to estimate the fundamental parameters of the planet and its parent star.
Methods. We have analysed high precision radial-velocity data, ground-based photometry, and high signal-to-noise ratio spectroscopy.
Results. The parent star CoRoT-Exo-4 (2MASS 06484671-0040219) is a late F-type star of mass of 1.16 $M_{\odot}$ and radius of 1.17 $R_{\odot}$. The planet has a circular orbit with a period of 9.20205 d. The planet radius is 1.19  $R_{\rm Jup}$ and the mass is 0.72  $M_{\rm Jup}$. It is a gas-giant planet with a ``normal'' internal structure of mainly H and He. CoRoT-Exo-4b has the second longest period of the known transiting planets. It is an important discovery since it occupies an empty area in the mass-period diagram of transiting exoplanets.

Key words: planetary systems - techniques: photometric - techniques: radial velocities - stars: fundamental parameters

1 Introduction

The masses and radii of extrasolar planets are fundamental parameters for constraining the physics at play in their interiors. A combination of photometric and Doppler techniques is presently the only way to indirectly derive these parameters. However, this possibility is limited to planets that transit in front of their stars, hence a sample of objects that is highly biased towards close-in orbits.

The planet search programme conducted from space by CoRoT (Baglin et al. 2006) is currently monitoring tens of thousands of stars and is regularly discovering new transiting planets (Barge et al. 2008; Deleuil et al. 2008a; Alonso et al. 2008). CoRoT has the ability to discover planets with smaller radii and/or longer periods than what is routinely achieved by ground-based transit surveys. The evolution of fundamental parameters of extrasolar planets will thus be explored as a function of the distance to the star and as related characteristics like irradiation. This has important implications for our understanding of these planets. For example, it is a way to test whether tidal damping (highly dependent on orbital distance), increased opacities, or alternative theories are the explanation for the anomalously large sizes of some extrasolar planets (e.g. Guillot et al. 2006; Burrows et al. 2007; Chabrier & Baraffe 2007).

With the current detection threshold of the first CoRoT run (45 day duration), 26 transiting events were detected. Two of them turned out to be planets (CoRoT-Exo-1b and 4b, Barge et al. (2008); Aigrain et al. (2008), 2 are grazing eclipsing binaries, 7 are low-mass binaries, and 10 are background eclipsing binaries. Four events remain unsolved cases, either because they are fast rotators (no possible radial velocity follow-up, the cross-correlation function is too wide or undetected with HARPS) or because they showed no radial-velocity variations. These cases are still in the list of systems to be observed at the next visibility season with higher accuracy. The statistics achieved on this run is compatible with expectations and the simulations on CoRoT detection, with its current threshold and follow-up performances.

The present paper focuses on the fourth planet discovered by CoRoT. The detection and light curve analysis is described in a companion paper (Aigrain et al. 2008, hereafter Paper IV). With its 9.20205 d period, the planet CoRoT-Exo-4b has the second longest period known so far in the family of transiting planets, after HD 17156b (Barbieri et al. 2007). We conducted a series of complementary observations from the ground to establish the planetary nature of CoRoT-Exo-4b and to derive the fundamental parameters of both the star and the planet.

2 Observations

2.1 Photometric observations

The photometric measurement was performed on-board CoRoT in an aperture that is adapted to each star and is trapeze shaped, with a solid angle close to that of a 14 arcsec diameter circle. It means that a faint eclipsing binary in the vicinity of the main target can produce a transiting event diluted enough to mimic a planetary signal (Brown 2003). The contamination factor of CoRoT-Exo-4 is estimated from the CoRoT entry catalogue EXODAT (Deleuil et al. 2008b) to be extremely low, i.e. only 0.3% of the light comes from neighbouring stars. The first step in establishing the nature of the transiting body is to check the photometric behaviour of the stars in the vicinity of the target, and especially those that fall inside the photometric aperture mask. This is easily done with ground-based telescopes.

CoRoT-Exo-4 was first observed from the Wise Observatory 18-inch telescope (Brosch et al. 2008) on November 12, 2007. Only a partial transit was recorded, thus preventing a precise estimate of the transit depth (of about 1.4%, which should be compared to the out-of-transit scatter of 0.16% in 5-min bins), but it is important that no significant variation was observed in nearby stars. Another transit event was observed with the Euler Camera (120-cm Swiss Telescope at La Silla Observatory) on November 30th, 2007. Two time series of about 40-min were collected in the star field, with a reference series taken at a similar elevation but one night prior to the transit. The transit depth was estimated to be $1.2\pm0.15$%, in agreement with the CoRoT measurements (1.1%). Finally, the ingress of another transit was observed at the Canada-France-Hawaii Telescope with MegaCam on December 10, 2007. Again, only a partial transit was observed, and the transit depth was not fully reliable.

The three sets of photometric follow up confirm that 1) the transit observed by CoRoT occurs on the central target at the predicted epochs; 2) no star encompasses a deep eclipse, or even a short-term variation, in the vicinity of the target; 3) the transit depth is compatible with the depth measured by CoRoT (i.e. no strong dilution by background objects). A detailed analysis of these data will be given in Deeg et al. (in preparation).

2.2 Radial velocity observations

Seven radial velocity measurements of CoRoT-Exo-4 were obtained with SOPHIE on the 1.93 m telescope at Observatoire de Haute Provence (France), from October 31, 2007 to February 2, 2008. These first data points established the planetary nature of the companion, showing a detectable and low-amplitude, radial-velocity variation in phase with the CoRoT ephemeris. Thirteen additional measurements were also obtained with HARPS (3.6 m telescope at La Silla, ESO, Chile), from November 19, 2007 to January 21, 2008.

Both instruments are cross-dispersed, fiber-fed échelle spectrographs on which precise radial-velocity measurements were performed with regular Th-Ar calibration observations and the reduction involves cross-correlation techniques (Pepe et al. 2002; Baranne et al. 1996). With SOPHIE, the high-efficiency mode was used with a resolving power of 40 000, and the sky background was simultaneously recorded to correct for contamination (Bouchy 2006). The radial velocities were obtained with a weighted cross correlation of the extracted spectra with a numerical mask corresponding to a G2 star.

The data are listed in Table 2 (available in the on-line version) and shown in Fig. 1. The orbital solution was derived using the combined HARPS and SOPHIE datasets. In the fit we included a constant offset between the two sets of measurements. The ephemeris of the CoRoT light curve was used to constrain the solution. The data were best-fitted with a circular Keplerian orbit of semi-amplitude of $63\pm6$  m/s. When using the 13 HARPS data points alone, the residual rms is 17.6  m/s. With the combined SOPHIE and HARPS datasets (20 measurements), the residual rms is 19.4  m/s. The offset between SOPHIE and HARPS data is only 5  m/s. Figures 1 and 2 show the data and the best fit as a function of time and orbital phase. The O-C time series does not show any variations that would indicate a second massive body in the system with a baseline of 100 days (Fig. 1).

The bisector analysis is shown in Fig. 3. The errors on the span of the bisector slopes are twice as large as for the peak position of the cross-correlation function. The behaviour of the bisector span (BIS) with respect to the radial velocity shows a dispersed relation with little or no trend. Given that short-term variations are seen in the CoRoT light curve (see with Fig. 2 in Paper IV), we tentatively interpret these variations as possibly stemming from a residual of stellar activity.

\par\includegraphics[width=7.5cm,clip]{}\end{figure} Figure 1: Radial-velocity measurements of CoRoT-Exo-4 as a function of time, showing the best-fit solution and O-C residuals. Black filled circles are HARPS data, and red open diamonds are SOPHIE data.

2.3 Determination of spectroscopic parameters

From radial velocity observations we estimated the projected velocity of the parent star. The result is $v \sin i = 6.4\pm1$  km s-1, based on the width of the cross-correlation functions from SOPHIE and HARPS. This agrees with a direct comparison of the observed spectrum with a rotationally broadened synthetic spectrum. With our determination of the stellar radius $R_\star=1.15$ $R_{\odot}$ (see below), this translates into a rotational period of the star ranging between $P_{\rm rot}=8.5$ and 10.0 days. This value for the rotation period is compatible with the analysis in Paper IV, and is consistent with a synchronicity of the stellar rotation and the planet orbit.

\par\includegraphics[angle=90,width=7.5cm,clip]{}\end{figure} Figure 2: Radial-velocity measurements of CoRoT-Exo-4 with respect to the orbital phase as estimated from the CoRoT ephemeris and the best-fit solution. Black filled circles are HARPS data, and red open diamonds are SOPHIE data.

\par\includegraphics[width=7.5cm,clip]{}\end{figure} Figure 3: Bisector variations (span of the bisector slope) as a function of orbital phase ( top panel) and radial velocity value ( bottom panel). Black filled circles are HARPS data, and red open diamonds are SOPHIE data.

We determined the fundamental parameters of the host star by analysing a HARPS spectrum. The signal-to-noise (S/N) level in the continuum is around 60 per pixel in the range 5000-6000 Å and it decreases to 40 in the red and blue parts. The spectrum was carefully normalized by identifying continuum windows in a synthetic spectrum calculated with the parameters of the target star. A spline function was fitted to the continuum windows and divided into the observed spectrum to obtain the normalized spectrum. We made sure that the shapes and depths of lines in adjacent spectral orders were in good agreement. In the final spectrum, the orders were merged and the overlapping parts added using weights based on the measured S/N.

We analysed the normalized spectrum using the semi-automatic software package VWA (Bruntt et al. 2004,2008). More than 600 mostly non-blended lines were selected for analysis in the wavelength range 3980-6830 Å. The VWA uses atmosphere models interpolated in the grid by Heiter et al. (2002) and atomic parameters from the VALD database (Kupka et al. 1999). Abundances were calculated relative to the solar spectrum from Hinkle et al. (2000) following the approach by Bruntt et al. (2008). The VWA automatically adjusts the parameters ( $T_{\rm eff}$, $\log g$, microturbulence) of the applied atmospheric model to get consistent results for all iron lines. The program iteratively minimizes the correlation between the abundance and equivalent width found from weak Fe  I lines (equivalent widths <80 mÅ), the correlation of abundance and excitation potential of Fe  I lines (equivalent widths <140 mÅ), and the mean abundance of neutral and ionized Fe lines must yield the same result. To estimate the uncertainty on the derived parameters and abundances of individual elements, we measured the sensitivity of the results when changing the parameters of the atmospheric model (see Bruntt et al. 2008).

The result is $T_{\rm eff}=6190\pm60$ K, $\log g=4.41\pm0.05$, and a microturbulence $\xi_t=0.94\pm0.07$ km s-1. The determined spectroscopic parameters do not depend on the adopted value of $v \sin i$. The overall metallicity is found as the mean abundance of the elements with at least 20 lines (Si, Ca, Ti, Cr, Mn, Fe, Ni) yielding [M/H $] =+0.05\pm0.07$. Details on individual abundances of CoRoT host stars will be given in a later paper.

3 Estimation of the stellar and planetary parameters

3.1 Stellar mass, radius, and age

Using evolutionary tracks (Morel & Lebreton 2007; Siess et al. 2000), the spectroscopic determination of $T_{\rm eff}$ and the ratio  $M_{\rm s}^{1/3}/R_{\rm s}$ estimated from the CoRoT photometry (Paper IV), we derived the following estimates for the mass and radius of the star: $M_{\rm s} = 1.16_{-0.02}^{+0.03}$ $M_{\odot}$ and $R_{\rm s} = 1.17_{-0.03}^{+0.01}$ $R_{\odot}$. This corresponds to a surface gravity of $\log g= 4.37\pm0.02$, which agrees with the spectroscopic value of $4.41\pm0.05$.

While the details of the process of how lithium is depleted in F-stars is not yet fully understood, it is now well-established that lithium is depleted for stars with a temperature below 6200 K (Steinhauer & Deliyannis 2004). However, lithium depletion in F-stars is expected to be slow, and data taken for stars with the same age and spectral type show a huge scatter in the equivalent width. By comparing the equivalent width of the Li  I line at $\lambda$6708 ( $35.2\pm4.8$ mÅ) of CoRoT-Exo-4b with the data for the Hyades (Thorburn et al. 1993; Boesgaard & Tripicco 1986), the UMa moving group (Soderblom et al. 1993), and NGC 3960 (Prisinzano & Randich 2007), an age of about 1 -0.3+1.0  Gyr is the most likely estimate for CoRoT-Exo-4b.

3.2 Planetary mass and radius

\par\includegraphics[width=7.5cm,clip]{10273fg4.eps}\end{figure} Figure 4: Theoretical models for the contraction of CoRoT-Exo-4b with time compared to the observations. The models (Guillot et al. 2006) assume either solar composition ( left panel) or the presence of a central dense core of $20~M_\oplus$ ( right panel). In each case, three possible evolution models are shown: (1) a standard model; (2) a model assuming that 1% of the incoming stellar luminosity is transformed into kinetic energy and dissipated in the deep interior by tides; (3) a model in which interior opacities have been arbitrarily increased by a factor 30.

Using the values obtained from the transit fit to the CoRoT light curve (Paper IV), the characteristics of the radial-velocity fit, and the stellar parameters from the previous section, we get a planetary mass of $M_{\rm p} = 0.72 \pm 0.08$  $M_{\rm Jup}$ and a planetary radius $R_{\rm p} =
1.19_{-0.05}^{+0.06}$  $R_{\rm Jup}$. The semi-major axis of the orbit is $a=0.090\pm0.001$ AU. The mean density of the planet is $0.525\pm0.15$  g cm-3. This new planet is found in the expected location of the mass-radius diagram (Fressin et al. 2007). In terms of composition, Fig. 4 shows that it contains a relatively small amount of heavy elements (0 to up to $\sim$ $30~M_\oplus$, depending on the model chosen), as expected from the empirical correlation between stellar metallicity and mass of heavy elements in the planet (Guillot et al. 2006; Burrows et al. 2007; Guillot 2007). The agreement with different models of planetary evolution implies that we cannot rule out any specific scenario used to explain anomalously large planets at this point. However, the discovery of other transiting planets on long-period orbits will be extremely valuable.


Table 1: The orbit parameters and the fundamental parameters of CoRoT-Exo-4b and its host star.

V0 [ km s-1]
$32.301 \pm 0.005 $ K [ m/s] $63\pm6$
e $0.0 \pm 0.1 $ a [AU] $0.090 \pm 0.001 $
P [d] 9.20205 $\pm$ 0.00037    
$M_{\rm p}$ [ $M_{\rm Jup}$] $0.72 \pm 0.08 $ $R_{\rm p}$ [ $R_{\rm Jup}$] $\rm 1.190_{-0.05}^{+0.06}$
$\rho_{\rm p}$ [g/cm3] $0.525\pm0.15$ $T_{\rm eq}$ [K] $1.074 \pm 19 $
$M_{\rm s}$ [$M_{\odot}$] $\rm 1.16_{-0.02}^{+0.03} $ $R_{\rm s}$ [$R_{\odot}$] $\rm 1.17_{-0.03}^{+0.01} $
$v \sin i$ [ km s-1] $6.4 \pm 1.0 $ $T_{\rm eff}$ [K] $6190 \pm 60 $
$\log g$ $4.41\pm0.05$ Age [Gy] $\rm 1_{-0.3}^{1.0}$

4 Discussion

The planet CoRoT-Exo-4b has the second longest period of the transiting systems known today and is found in a region of the mass-period parameter space that was previously empty (see Fig. 5 available on-line).

The mean density of 0.525  g cm-3 makes CoRoT-Exo-4b a gas-giant with a ``normal'' internal structure dominated by H and He. It is located in the bulk of Hot Jupiters in the mass-radius diagram. We estimate the age of the parent star to be about 1 Gyr; thus, the star is likely to be fairly active and its age and rotation rate (Paper IV) are compatible.

New discoveries made with CoRoT will likely populate the mass-period diagram in the period range 5-50 days and allow further investigations of the importance of star-to-planet distance on the internal structure of giant planets. This will complement the output from current radial-velocity surveys, allow us to better understand the mechanisms that govern the contraction of these planets, and provide constraints for planet formation models.

We thank the OHP and ESO staff for help provided during the SOPHIE/HARPS observations. The German CoRoT team acknowledges support through DLR grants 50OW0204, 50OW0603 and 50QP0701. H.J.D. and J.M.A. acknowledge support by grants ESP2004-03855-C03-03, and ESP2007-65480-C02-02 of the Spanish Education and Science ministry.



5 Online Material

\par\includegraphics[width=12.5cm,clip]{}\end{figure} Figure 5: Mass-period diagram of the 35 known transiting planets showing the location of CoRoT-Exo-4b (diamond).


Table 2: Radial-velocity measurements of CoRoT-Exo-4 with SOPHIE (lines 1 to 7) and with HARPS (lines 8 to 20). ``BIS'' is the slope of the bisector span, measured in the cross-correlation function.
BJD RV Uncertainty BIS err(BIS)
-2 400 000 [km s-1] [km s-1] [km s-1] [km s-1]
54 405.6545 32.370 0.024 -0.021 0.048
54 408.6667 32.278 0.018 -0.004 0.036
54 410.6344 32.258 0.027 -0.025 0.054
54 413.6784 32.343 0.034 -0.113 0.068
54 416.6908 32.294 0.027 -0.097 0.054
54 494.3741 32.259 0.019 +0.020 0.036
54 507.3778 32.320 0.020 +0.067 0.040
54 423.8430 32.352 0.022 +0.020 0.044
54 424.8273 32.344 0.019 +0.012 0.040
54 428.8091 32.234 0.014 -0.017 0.028
54 442.7618 32.381 0.012 +0.032 0.024
54 443.7161 32.361 0.021 -0.050 0.042
54 445.7748 32.270 0.012 -0.012 0.024
54 447.7813 32.239 0.013 +0.015 0.026
54 448.7990 32.268 0.014 -0.005 0.028
54 449.7871 32.272 0.017 +0.002 0.034
54 450.7729 32.373 0.013 -0.072 0.026
54 481.6668 32.287 0.016 +0.040 0.032
54 482.6719 32.287 0.015 +0.040 0.030
54 486.6509 32.290 0.015 -0.002 0.030

Copyright ESO 2008