An investigation into the radial velocity variations of CoRoT7^{}
A. P. Hatzes^{1}  R. Dvorak^{2}  G. Wuchterl^{1}  P. Guterman^{3}  M. Hartmann^{1}  M. Fridlund^{4}  D. Gandolfi^{1,4}  E. Guenther^{1}  M. Pätzold^{5}
1  Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany
2 
Institute for Astronomy, University of Vienna, Türkenschanzstrasse 17, 1180 Vienna, Austria
3 
Laboratoire d'Astrophysique de Marseille, UMR 6110, Technopole de
MarseilleÉtoile, 13388 Marseille Cedex 13, France
4 
Research and Scientific Support Department, European Space Agency, ESTEC, 2200 Noordwijk, The Netherlands
5 
Rheinisches Institut für Umweltforschung, Universität zu Köln, Abt. Planetenforschung, Aachener Str. 209, 50931 Köln, Germany
Received 15 April 2010 / Accepted 22 June 2010
Abstract
Context. CoRoT7b, the first transiting ``superearth'' exoplanet, has a radius of 1.7
and a mass of 4.8
.
The HARPS radial velocity (RV) measurements used for deriving this mass
also detected an additional companion with a period of 3.7 days
and a mass of 8.4
.
The mass of CoRoT7b is a crucial parameter for planet structure
models, but is difficult to determine because CoRoT7 is a modestly
active star and there is at least one additional companion.
Aims. The aims of this paper are to assess the statistical
significance of the RV variations of CoRoT7b and CoRoT7c, to
obtain a better measurement of the planet mass for CoRoT7b, and to
search for additional companions in the RV data.
Methods. A Fourier analysis is performed on the HARPS spectral
data of CoRoT7. These data include RV measurements, spectral line
bisectors, the full width at half maximum of the crosscorrelation
function, and Ca II emission. The latter 3 quantities vary
due to stellar activity and were used to assess the nature of the
observed RV variations. An analysis of a subset of the
RV measurements where multiple observations were made per night
was also used to estimate the RV amplitude from CoRoT7b that was
less sensitive to activity variations.
Results. Our analysis indicates that the 0.85d and 3.7d
RV signals of CoRoT7b and CoRoT7c are present in the spectral
data with a high degree of statistical significance. We also find
evidence for another significant RV signal at 9 days. An analysis
of the activity indicator data reveals that this 9d signal most likely
does not arise from activity, but possibly from an additional
companion. If due to a planetary companion the mass is
,
assuming coplanarity with CoRoT7b. A dynamical study of the three
planet system shows that it is stable over several hundred millions of
years. Our analysis yields a RV amplitude of
m s^{1} for CoRoT7b which corresponds to a planet mass of
.
This increased mass would make the planet CoRoT7b more Earthlike in its internal structure.
Conclusions. CoRoT7 is confirmed to be a planet system with at least 2 and possibly 3 exoplanets having masses in the range 720
.
If the third companion can be confirmed then CoRoT7 may represent a case of an ultracompact planetary system.
Key words: star: individual: CoRoT7  techniques: radial velocities  planetary systems  stars: activity  starspots
1 Introduction
The 27cm space telescope CoRoT is devoted to obtaining ultrahigh precision light curves over a wide field for the dual purpose of asteroseismology and the detection of transiting exoplanets (Baglin 2006; Auvergne et al. 2009). This mission resulted in the milestone discovery of CoRoT7b, the first transiting superearth whose radius and mass have been accurately characterized. Photometric measurements of CoRoT7 made with the CoRoT Space Telescope from October 2007 to March 2008 revealed a transit like event with a period of 0.85 days and a depth of a mere 0.03%. A detailed analysis of the CoRoT light curve and ancillary measurements provided by ground based observations excluded all sources of false positives and established with high probability that the transit event was due to a planet with a radius of 1.7 (Leger et al. 2009).
CoRoT7 is a G9 main sequence star with an estimated age of 1.22.3 Gyr. From the analysis of the three best spectra obtained with HARPS, and using several methods, Bruntt et al. (2010) find K, , [M/H , and km s^{1}. They also find slightly different values for the mass and radius of CoRoT7: and . The revised stellar radius results in a slightly smaller radius for the planet of .
Queloz et al. (2009; hereafter Q09) presented over 100 precise stellar radial velocity (RV) measurements of CoRoT7 taken between November 2008 and February 2009 with the High Accuracy Radial velocity Planet Searcher (HARPS) spectrograph mounted on ESO's 3.6 m telescope at La Silla. The RV analysis presented in Q09 was complicated by the relatively high activity of the host star. The CoRoT7 light curve shows photometric variations of up to 2% with a rotation period of 23 days. The implied spot filling factor suggests an RV ``jitter'' due to stellar activity of more than 10 m s^{1}(Saar & Donahue 1997) which was confirmed by the RV measurements.
Two approaches were used in Q09 for the analysis of the RV data. Fourier prewhitening resulted in an RV amplitude of m s^{1}for CoRoT7b, while filtering using rotational harmonics resulted in an amplitude of 1.90 0.4 m s^{1}. By applying correction terms to these amplitudes due to the effects of the filtering process a consistent amplitude of 3.5 0.6 m s^{1} was obtained. This corresponded to a planet mass of 4.8 0.8 . Their analysis also revealed the presence of a 3.7d period with an amplitude of 4.0 0.5 m s^{1} that was not associated with the stellar activity. This signal is most likely due to a second companion with a mass of 8.4 0.9 .
One of the most important parameters we can determine for an exoplanet is its mass. For transiting exoplanets we also know the radius and the average density of the planet and this is a unique parameter that will allow us to estimate the planet's composition, e.g. the fraction of metals and/or water. For transiting exoplanets we also know the radius and average density of the planet, . A high value of , as seem to be the case for CoRoT7b (Q09, this work), indicates a high metal content and a low water abundance. Interestingly, another lowmass planet with a similar radius (2.7 ) has recently been found by the MEarth project (Charbonneau et al. 2009), but with a much lower than CoRoT7b. Valencia et al. (2010) using the mass of CoRoT7b from Q09 concluded that the internal structure was consistent with a significantly depleted iron core. However, a mere increase of only 1 in the mass and a slightly smaller radius would make the planet more Earthlike. Clearly, a careful determination of the mass, to go with the radius provided by the exquisite CoRoT photometric data is absolutely imperative. This mass must rely on how accurately we can determine the RV amplitude of CoRoT7b and unfortunately the activity signal makes this difficult. The details in which the activity signal is removed may affect the final RV amplitude of CoRoT7b.
Figure 1: Scargle periodograms of the RV ( top), bisector ( upper middle), Ca II Sindex ( lower middle), and FWHM ( bottom) measurements for the frequency range 00.3 c d^{1} ( left panels) and 1.01.3 c d^{1} ( right panels). The vertical blue lines mark frequencies seen only in the RV (the one in the right panel is the transit frequency). Vertical red lines mark the rotational frequency and its first 3 harmonics. 

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 to assess the statistical significance of CoRoT7b seen in the RV data;
 to look for possible additional planet signals in the HARPS data;
 to understand the nature of all detected signals in the HARPS RV data;
 to obtain the best possible determination of the mass, and thus density of CoRoT7b.
2 Observations
The HARPS spectrograph obtained 106 RV measurements for CoRoT7 over a time span of 4 months. We refer the reader to Q09 for a detailed description of the RV measurements. Besides RV information, the HARPS data also provided information on the activity of the star via the bisector span of the cross correlation function (CCF), the Ca II Sindex, and the fullwidth at half maximum (FWHM) of the CCF. In particular, the line bisector has become a common tool for confirming exoplanet discoveries (e.g. Hatzes et al. 1988; Queloz et al. 2001). Figure 1 of Q09 shows the RV measurements for CoRoT7 as well as the activity indicators.
3 Scargle periodograms of measured quantities
A periodogram analysis can give us a quick overview as to possible periods that may be present in the data. Scargle periodograms were calculated for the four quantities measured from the HARPS spectra: RV, bisector span, Ca II Sindex, and the FWHM of the CCF. These are shown in Fig. 1. The RV measurements contain information about possible planetary companions and activity while the other quantities should only contain information on stellar activity. A comparison of the periodograms gives a first indication as to which peaks in the RV periodogram arise from activity and those which may be due to companions. Two frequency ranges are shown. The left panels are for c d^{1} and the right panels are for c d^{1}. The vertical blue lines indicate RV frequencies not seen in the activity indicators. The one in the right panel is the CoRoT7b transit frequency. Because of 1day aliases all frequencies in the left panel also appear as peaks at in the right panel. (Note: we have not marked the 1day alias of the CoRoT transit frequency at 0.17 c d^{1}, although one can see a peak at this frequency location.) The vertical red lines mark the rotational frequency, , and its first 3 harmonics (2 , 3 , and 4 ).
There are several important features to note in these periodograms. First, the dominant peak in all 3 quantities occurs at c d^{1}, the rotational frequency as determined from the CoRoT light curve. Clearly, RV variations are dominated by the activity RV jitter from rotational modulation which will complicate the extraction of RV variations due to bona fide companions. Second, the periodograms of the bisectors and Ca II look remarkably similar with the same peaks identifiable in both periodograms. Third, although the FWHM periodogram shows similar peaks near the rotational frequency, its shape looks more like the RV periodogram but without the peaks shown by the vertical dashed lines. The strong peaks at and 0.13 c d^{1}, which are the first and second harmonics of , are not as strong in the FWHM as in the bisector and Ca II periodogram. The most important point is that the 3 peaks seen in the RV data at , 0.27, and 1.17 c d^{1} (and their 1day aliases) are not found in any of the other quantities. This is our first hint for the presence of RV variability not associated with stellar activity.
Figure 2 shows the spectral window for the data. As expected it is rather complex with strong sidelobes at +0.013 and 0.04 c d^{1}. Note that the same spectral window applies for all data (RV, bisectors, Ca II, and FWHM).
4 Frequency analysis of the data sets
It is evident from the periodograms that all spectral quantities have multiperiodic variations. As such they are well suited to the classic technique of prewhitening often employed in the study of stellar oscillations. In this process a Fourier transform (FT) finds the highest peak in the power spectrum. A least squares fit to the frequency, amplitude, and phase to the found signal is made and then subtracted from the time series. Note that by subtracting this signal we also remove all aliases of the dominant frequency. A subsequent FT on the residuals yields the next dominant frequency in the time series. This sequential subtraction of dominant components is continued until the level of the noise is obtained using the criterion that peaks more than 4 times the Fourier noise level are regarded as real (Kuschnig et al. 1997). This frequency analysis was performed on the HARPS data using the program Period04 (Lenz & Breger 2004).
4.1 Radial velocity data
A prewhitening analysis of the RV measurements was already presented in Q09. In that analysis a 12component sine fit was made to the data which resulted in an rms to the fit of 1.81 m s^{1}. Table 1 lists frequencies using a more conservative solution. In this case the stopping criterion for the prewhitening (last significant peak) was assessed using a bootstrap randomization procedure (e.g. Kürster et al. 1997). Frequencies above the horizontal line have a false alarm probability less than or equal to about 1%. The rms scatter of the fit to the RV is 2.96 m s^{1} which is significantly higher than the mean RV error of 1.89 m s^{1}. Including the two frequencies below the space break results in an rms scatter of 2.18 m s^{1}, only slightly worse than the 12component fit from Q09. Figure 5 in Q09 shows the fit to the RV data provided by the 12component fit. The 9component fit listed in Table 1 is of comparable quality so is not shown here.
Most of the frequencies from the FT analysis arise from stellar activity with the most dominant one being the rotational frequency, c d^{1} and its harmonics. This is noted in the comment column. The rotational period derived from the RV data is 22.32 0.08 days, hence larger than the value of 21.65 0.03 days obtained from the CoRoT light curve. It is not known whether this difference merely reflects the difficulty in measuring the rotational period from such complex RV and light curves, or if this is a real difference due to possibly differential rotation. There are 3 frequencies denoted f_{1}, f_{2}, and f_{3} that are not readily associated with stellar activity. The frequency f_{1} is the CoRoT7b transit frequency of 1.17165 c d^{1}, f_{2} is the 3.7day planet reported by Q09, and f_{3} corresponds to a period of 9.02 days and will discussed at length below. In Table 1 there are three additional frequencies above the space break and two below that could not be readily associated with rotational harmonics, but as we show below these are most likely related to the activity signal. For convenience in referencing we denote sequentially the additional frequencies f_{4}  f_{8}, although for the following discussion f_{1}, f_{2}, and f_{3} are the most important.
Figure 2: Spectral window function for the HARPS measurements. 

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Table 1: Frequencies and amplitudes found by a prewhitening procedure on the HARPS RV data.
The CoRoT light curve for CoRoT7 is complex and shows evidence for spot evolution on time scales of less than 150 days, or comparable to the time span of our RV measurements. Although the fit to the data using the full RV data set is excellent, the Fourier sine components may not accurately represent the activity variations over such a long time span. An analysis of the data in subsets of shorter time interval may minimize the uncertainties in the activity signal due to spot evolution.
To minimize possible effects of spot evolution, a frequency analysis was also performed on subsections of the HARPS data. The RV data were divided into 3 sets each roughly spanning one rotation period. The time span of these data sets are listed in the first 3 lines of Table 2. When analyzing data containing periods comparable to the time span of the data string there can be risks to using the prewhitening procedure. This is certainly true for the rotational period and to some extent to the 9d period since it only undergoes 2 cycles over the time span of the subset observations. Likewise the 0.85d suffers from being severely undersampled for some of the data subsets. In short, alias effects and spectral leakage may result in a spurious period being identified and removed from the data and thus resulting in an erroneous solution.
Indeed, when performing a straight prewhitening procedure to Subset 1 the dominant frequency is f = 0.13 c d^{1} and the rotational frequency appears at 0.05 c d^{1}. Only f_{2} is recovered. However, when one first fits the data using the CoRoT7b frequency first, the procedure recovers both f_{2} and f_{3}. A prewhitening analysis on Subset 2 recovers , f_{1}, and f_{2}, but the nearest frequency to f_{3} was at 0.08 c d^{1}. Subset 3 also yields different results. The dominant frequency occurs at 0.03 c d^{1}, significantly different from . Both f_{2} and f_{3} are recovered, but the nearest frequency to f_{1}, the transit frequency, is at 1.18 c d^{1}.
Therefore, in fitting the subset data we assumed that f_{1}, f_{2}, and f_{3} were present in the data asked the question ``Can the subset data be fit using these frequencies?'' To answer this we first fit and removed the frequencies that were found in the full data set, namely , f_{1}, f_{2}, and f_{3}. In this fitting only the frequencies were held fixed, but the amplitudes and phases were allowed to vary. The prewhitening procedure was continued until the rms fit to the data was comparable to the HARPS measurement error (better than 2 m s^{1}).
Tables 35 lists the frequencies and amplitudes from the Fourier analysis. In all cases the rms fit of the data is comparable to the mean error of the HARPS measurements. The amplitude of the , 0.27, and 1.17 c d^{1} signals remain relatively constant. The largest amplitude variations are found for the frequency associated with rotation, but it is not clear how significant these are given the data subinterval spans only one rotation period. The amplitude is thus probably not well determined. In summary, this has established that the RV variations in the subset data are consistent with the presence of f_{1}, f_{2}, and f_{3}, and with amplitudes comparable to those found in the full data set. Note that the additional frequencies found in the prewhitening procedure can be identified with frequencies found in the full data set analysis.
The referee suggested an analysis of the longest data string between JD = 2 454 847.62 454 884.7 as this has few gaps (Subset 4). A Fourier prewhitening procedure found f_{1} and f_{2}, but was unable to find f_{3}. This was also the case when we generated a fake data set using the periods listed in Table 1, sampled in the same manner as Subset 4, and with random noise with m s^{1}. The prewhitening procedure was also unable to detect f_{3}even though it was present in the data. Table 6 lists the results of the Fourier analysis by first fitting , f_{1}, f_{2}, and f_{3} similar to the procedure used for generating Tables 35. Note that the amplitude of f_{3} is considerably lower than was found for Subsets 13. This may be an indication that it is an artifact of the activity signal. However, when performing the same analysis on the fake data generated using the frequencies and amplitudes in Table 1 (again with the appropriate sampling and noise), the fitted amplitude for f_{3} is a factor of 3 less. The fitted amplitudes for the fake data are listed in the third column of Table 6. So, any evidence for amplitude variations for f_{3} is inconclusive.
Table 2: The data subsets.
Table 3: Frequencies found in data Subset 1.
Table 4: Frequencies found in data Subset 2.
Table 5: Frequencies found in data Subset 3.
Table 6: Frequencies found in data Subset 4 using the same analysis as Tables 35, i.e. first removing the contribution of , f_{1}, f_{2}, f_{3}. Column 3 shows the amplitude derived using fake data (see text).
4.2 Frequency analysis of activity indicators
A Fourier analysis with prewhitening was performed on the bisector, Ca II Sindex, and FWHM measurements. These are listed in Tables 79. The prewhitening procedure was continued beyond the last frequency we considered significant to see if at any point a frequency was detected that coincided with either f_{1}, f_{2}, and f_{3}. Both the bisector and FWHM measurements show frequencies near f_{2}: c d^{1} (P = 3.6 d), but only after prewhitening the data well past our stopping criterion (7th frequency found in the bisector and the 6th frequency in the FWHM). These amplitude frequencies are essentially at or below the noise level. Furthermore, when we phase the bisector and FWHM data after removing all components except those near the 3.7d period, no obvious sinusoidal variations are present. We therefore do not consider these frequencies to be significant.
Table 7: Frequencies found in the bisector data using a prewhitening procedure.
Table 8: Frequencies found in the Ca II data using a prewhitening procedure.
Table 9: Frequencies found in the FWHM data using a prewhitening procedure.
5 Statistical significance of the RV frequencies
A common way of assessing the statistical significance of a period found in time series data is via the Scargle periodogram (Scargle 1982). In this formulation of the Fourier transform the power of a peak is related to a statistical significance rather than the amplitude of the periodic signal. If a peak in the Scargle periodogram has power, z, then the false alarm probability (FAP, probability that it is due to noise) can be calculated under two cases. The first is if one is searching for an unknown signal over a wide frequency range, and the second is for a period known to be present in the data. In the former, the FAP is given by FAP ) , where N is the number of independent frequencies. For the latter, the FAP is given by FAP , where now there is only one independent frequency (N=1).
5.1 Statistical significance of 0.85d RV period
Because we know that a 1.1716 c d^{1} signal is present in the CoRoT light curves we should ask: what is the FAP for a signal at the known frequency of the CoRoT transit? Table 10 lists the Scargle power, z, and the false alarm probability, FAP = for the peak at 1.17 c d^{1} in each of the data sets. Clearly, the 0.85d period in the RV data is significant, whereas the false alarm probability of the corresponding peak at the same frequency in any of the activity indicators is over a factor of 20 higher.
Of course, the Scargle prescription uses the rms scatter of the full data set to set the noise level in assessing the FAP. If there is real variablity in the data this increases the rms scatter and results in an overestimate of the FAP. For weaker signals in time series that are dominated by a stronger one, you should subtract the contribution of the dominant signal to get a better estimate of the FAP for the weaker signal.
Table 10: Scargle power and False Alarm Probability for the Peak at 1.17 c d^{1}, for RV, bisector, and Ca II data.
Figure 3: Scargle periodograms resulting from sequential adding of data subsets. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. 

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Figure 3 shows the Scargle periodogram of the RV residuals after subtracting all sine components except that due to the CoRoT planet at 0.85 days. The red line shows the Scargle periodogram using Subset 1, the green is after adding Subset 2, and the blue is the periodogram of the full data set. The fact that the Scargle power increases with the addition of each new data set (i.e. increasing statistical significance) gives us some reassurance that the signal is indeed present in all data sets. The final Scargle power of the 1.171 c d^{1} signal is z = 39, which results in an FAP of 10^{17} for a known signal in the data. The FAP that noise would create a peak with power higher anywhere in the full spectral range (first equation from above) is 10^{15}. Thus this signal would be highly significant even if we were unaware of the CoRoT transit period.
5.2 Statistical significance of 3.7d RV period
The 3.7d period ( f_{2} = 0.11 c d^{1}) has Scargle power of 5.67. Based on this power level we would normally not be considered the signal to be significant. An FAP was assessed by using a bootstrap randomization method. The RV values of the data (with all signals present) were shuffled randomly keeping the observation times fixed and a periodogram calculated for this random data. After 10^{5} such ``shuffles'' the number of random periodograms having power greater than 5.67 over the frequency range 00.5 d^{1} gave an estimate of the FAP. This value was 0.3.
However, as stated earlier, this FAP may be overestimated due to the presence of the other signals in the RV data. To get a more realistic assessment of the false alarm probability the contributions from all sine components except that due to the 3.7day period were subtracted from the three subsets (the 3.7d residuals). Figure 4 shows the Scargle periodogram after sequentially adding the residual RVs from each of the data subsets. The Scargle power increases with the addition of each subset and the final value is 40 which corresponds to an FAP 10^{16}.
5.3 Statistical significance of 9.0d RV period
The peak at 9 days in the RV periodogram has Scargle power of 12.13. A bootstrap randomization with 10^{5} shuffles yields an FAP . We can be confident that this signal is statistically significant even without subtraction of the other signals. Figure 5 shows the Scargle periodograms for the 9d RV residuals, i.e. the RV measurements with all signals except the 9d period subtracted, and as each subset is added. The increase in the statistical significance with the addition of more RV measurements is an indication of a longlived and coherent signal. The FAP of the final peak after including all RV measurements is 10^{16}.
Figure 4: Scargle periodograms resulting from sequential adding of residual RV data for the 3.7day period. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. All sine components except the that associated with the 9.02day period. 

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Figure 5: Scargle periodograms resulting from sequential adding of residual RV subsets for the 9day period. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. 

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6 Is the 0.85d period an alias of a rotation harmonic?
The Scargle periodograms in Fig. 1 are dominated by the rotational frequency, . However, there is also power at the first two harmonics of the rotational frequency, namely 2 and . Indeed, Q09 applied harmonic filtering using the rotational frequency and its first two harmonics to remove the signature of activity. Because of this there is some concern that the 1.1715 transit frequency is close to the oneday alias of the 3rd harmonic of the rotational frequency (i.e. c d^{1}). In the best case, the activity signal can thus contribute some power at the orbital frequency of CoRoT7b. In the worse case all the RV signal at this frequency could arise from activity.
Q09 argued that because repeated measurements were taken on the same nights, that this alias effect was minimized and that the 0.85d RV period was the one actually present in the data. To investigate whether alias effects of a rotational harmonic can account for the observed 0.85d period in the RV data we performed an analysis on a subset of the RV consisting only of those nights for which at least 3 RV measurements were made during the night. In the following analysis it is assumed that the activity signal contributes a constant value to the measured RV on a given night. This is a reasonable assumption. The maximum time separation between the first and last measurement on a given night is less than 4 h. This corresponds to a change in rotation phase of only 0.007. The contribution of stellar activity to the measured RV should thus be a constant over that time. This also assumes that spot evolution over 4 h is negligible. Meanwhile, the change in orbital phase of CoRoT7b is 0.2 and should cause the dominant variations observed in the RV during the course of the night.
It is not strictly true that the nonCoRoT7b RV variations are constant during the night. The orbital motion due to the CoRoT7c should produce an appreciable variation over 4 hours. However, this contribution is also relatively small. Over 4 hour time span the orbital phase of CoRoT7c only changes by 0.05 which corresponds to a maximum RV variation of only 1.5 m s^{1} well below the measurement error.
There were 7 nights where at least 3 RV measurements of CoRoT7 were made resulting in a total of 21 measurements. The data from these nights were treated as 7 independent data sets with each one have a different a zeropoint velocity which could vary from night to night. A least squares sinefit the 7 data sets was made keeping the period fixed to the transit period of 0.8535 days, but allowing phase and the zeropoint value for each night to vary. The advantage of such an approach is that it is a ``minimal impact'', low pass filter that makes no assumptions about the underlying time variability due to stellar activity, only that it is constant on a given night.
The top panel of Fig. 6 shows the Scargle periodogram of these 21 RV measurements after subtracting the individual zeropoint offsets determined by the least squares fitting. The strongest peak is at the transit frequency of 1.1715 c d^{1} and with a smaller peak at the alias frequency of 0.1715 c d^{1}. Figure 7 shows the RV measurements phased to the period of CoRoT7b and the alias period (5.7 days). The ``cleaner'' phase diagram of the 0.85 d period supports that this is the true period in the data, and not the alias of .
The false alarm probablity of the peak at 1.1715 c d^{1} was assessed using a bootstrap randomization procedure. The RV values were shuffled times keeping the observed times fixed and periodograms calculated for this random data. Over the frequency range c d^{1}there was only four instances where the periodogram of the random exceeded the power of the real data. The FAP for this signal is thus . We should note that this bootstrap was evaluated over the full frequency range 02 c d^{1}. Since we are interested in the known frequency of CoRoT7c it is more appropriate to evaluate the bootstrap over a much narrower range centered on c d^{1}. The FAP of this signal is almost certainly much less.
Figure 6: (Top) Scargle periodogram of the data set consisting of 7 nights where at least 3 RV measurements were made. The measurements from each night were considered an independent data set and a fit was made using the period of CoRoT7b and allowing zero point offset from each night to vary. The periodogram is of the data with the offset to each night subtracted. (Bottom) Same as in the top panel but with the addition of 16 nights for which two RV measurements were made per night. 

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There were an additional 16 nights where 2 RV measurements were taken of CoRoT7. The time separation of these points are large enough to provide some good sampling of the 0.85d sine wave presumed to be in the data. These nights were added to the data subset of 3 points per night to give a total of 53 data points spread over 23 nights. A new fit was performed, again allowing the nightly zeropoint values to vary, but keeping the period fixed to the transit period. The lower panel of Fig. 6 shows the periodogram of these data with the zero point offsets applied. Note that the Scargle power has significantly increased indicating a more signficant detection (FAP 10^{16}). Also, the frequency at 1.1716 c d^{1} is still higher than the alias frequency. A phase diagram of these data will be shown below when we present orbital solutions.
Figure 7: (Top) RV measurments of the 7night data set (zeropoint offsets applied) phased to the period of CoRoT7b. (Bottom) same measurements phased to the alias period of 5.82 days. 

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We also investigated whether the period of CoRoT7b could be extracted from the data without a priori knowledge of the transit period. To do this a range of periods were fit to the 53 RV measurements of the data set with multiple observations per night. At each trial fit the period was fixed, but the phase and zeropoint offset were allowed to vary. Figure 8 shows the reduced fit to the data as a function of the fitting period. Good fits occur at periods where is minimized. This procedure could be considered as a variant of the phase dispersion minimization technique of Stellingwerf (1978), but which allows the mean value of individual data sets to float (i.e. a ``floating mean'' phase dispersion minimization). The deepest minimum is near the period of CoRoT7b (vertical line). Other minima are clearly alias periods and phasing of the data to these periods does not produce as clean a phase diagram as for the CoRoT7b period.
6.1 Fourier analysis of nightly offsets
As a sanity check we performed a Fourier analysis on the nightly offsets produced by our least squares fitting. If these derived nightly offsets have some relationship to the activity we should see evidence of the rotational period. The top panel of Fig. 9 shows the Fourier transform of the nighty offsets (23 values). The highest peak corresponds to the rotational frequency of CoRoT7 (indicated by the vertical dashed line). This indicates that the nightly zeropoint offset indeed follows the RV rotational modulation due to activity.
Of interest is when we prewhiten the nightly offsets to search for additional periods. The second panel shows the offset data after removing the contribution of the rotational frequency. The highest peak corresponds to a frequency of 0.27 c d^{1} (indicated by the vertical line). The bottom panel shows the amplitude spectrum of the residuals after removing the contribution of the 0.27 c d^{1} frequency. The highest peak corresponds to 0.112 c d^{1}, close to the 0.11 c d^{1} frequency found in the RV (indicated by the vertical line). It is reassuring that the nightly offsets show evidence for the rotation period of the star, but also the 3.7d and 9d period found in the RV analysis.
Figure 8: The reduced as a function of period for the data set consisiting of nights with multiple RV measurements. The zeropoint offset from each night was allowed to vary. The vertical line indicates the period of CoRoT7b. 

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Figure 9: A prewhitening on the zeropoint offsets of the multimeasurement nights found by the least squares fitting. ( Top) Amplitude spectrum of the zeropoint values. The dashed line indicates the rotation period of CoRoT7b. ( Middle) The amplitude spectrum after removing the rotational frequency. The vertical line corresponds the frequency of the 3.7d period of CoRoT7c. ( Bottom) The amplitude spectrum after also removing 3.7d period signal. The vertical line corresponds to the frequency f_{3}. 

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7 On the nature of the 9d period
Figure 10: (Top) Scargle periodogram for the fit to RV first data subset (truncated JD = 47754807) sampled in the same manner as the data and with noise at a level of m s^{1}. (bottom) The Scargle periodogram of the real data. The vertical lines mark the frequencies of the 9d and 3.7d signals that are in the fake data. 

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In Q09 the two approaches to the RV data analysis (harmonic filtering and Fourier prewhitening) agree on the presence of a 0.85d and 3.7d period in the data. The main difference to the two approaches was that the prewhitening procedure yielded a significant period at 9d, whereas this signal was absent in the harmonic filtering of activity signal. The obvious interpretation is that the 9d period arises from the activity signal. However, the harmonic filtering worked on subsets of the data that were roughly the length of the rotation period, whereas the prewhitening procedure was performed on the full dataset. The 9d period is very close to , i.e. the first harmonic of the rotation period. There is a danger that when applying harmonic filtering one may remove real signals not associated with a rotational harmonic.
To test this hypothesis the frequency solution of the Subset 1 (Table 3) was used to generate a fake data set. This fake data included the signals f_{1}, f_{2}, and f_{3}. The fits were sampled in exactly the same way as the real data and noise at a level of m s^{1} was also added. The Scargle periodogram of the fake data (top panel) is compared to the periodograms of the real data (lower panel) in Fig. 10. The frequency of the input 3.7d and 9d period signals are shown as vertical lines.
There are two things to note about this figure. The periodogram of the fake data looks exactly like the real data, as it should. After all, the rms scatter about the fit is under 2 m s^{1}. If you fit the data you fit the periodogram. Note, however, because of the short data window the true frequency in the data, f_{3}, appears at a slightly different frequency of 0.12 c d^{1}.
This fake Subset 1 data set was analyzed using harmonic analysis and prewhitening. The data was first fit using the rotational frequency and its first two harmonics ( , 2 , and 3 ) as well as 0.5 (there was evidence for the presence of this frequency, see Table 1). The frequencies were kept fixed, but the amplitude and phase were made to vary. The prewhitening procedure was then carried out to find additional frequencies. The results are listed in Table 11. The prewhitening procedure found only 2 additional frequencies, f_{1} and f_{2}, but not f_{3} even though it was present in this fake data. The same result was found when applying this procedure to the other data sets.
Harmonic filtering was also performed on the full RV (real) data set by first fitting , 2 , and 3 to the data and then continuing the prewhitening procedure to find additional frequencies. After all frequencies were found the solution optimized by fitting all components simultaneously. The results are shown in Table 12. The frequencies f_{1}, f_{2}, and f_{3} were recovered in spite of the harmonic prefiltering.
This investigation has demonstrated that one should be careful in filtering the time series data using harmonics of the rotational frequency of CoRoT7 on a limited time span data set. In this case, using rotational harmonics essentially filtered out the real period that was in the simulated data. When applying rotational harmonic filtering to the full real data set the 9d period was still recovered. The reason for this is that over a 23d time span there is little difference between c d^{1} and the first harmonic of the rotational frequency, c d^{1}. Harmonic filtering will essentially remove this signal. However, over the 100 days that the RV data were acquired the subtle frequency difference between f_{3} and 2 can be resolved and harmonic filtering cannot fully remove the signal due to f_{3}. When performing an analysis on data subsets it is instructive to look also at the full data covering the longest time span.
7.1 Bisector  RV correlations
Table 11: Frequencies found in the simulated data set of Subset 1 (Fig. 10) using a prewhitening procedure and harmonic analysis.
Table 12: Prewhitened frequencies found in the RV data after first fitting the rotational frequency and its first 2 harmonics.
The HARPS data also contain three indicators of activity: the FWHM of the CCF, the bisector of the CCF, and the Ca II emission measure. Of these 3 activity indicators only the line bisectors have a direct relationship to the RV variations due to activity. Ca II emission originates in plage and these regions do not necessarily have the same surface distribution as spots. For cool spots the FWHM is outofphase with the RV variations. The FWHM is a minimum when the spot distortions are the wings of the spectral line (i.e. limb of star) and a maximum when the spots are at disk center (zero RV). Thus there is a phase shift of between the maximum of the RV and FWHM. During this time spot evolution may be significant. On the other hand, surface spots produce a distortion in the spectral line which results in a shift in the line centroid. Thus any RV variations due to activity must be correlated directly with variations in the spectral line bisector without the need to apply any phase shift. For this reason we will focus on the RV  bisector variations in CoRoT7 to assess the nature of the 9d period.RV variations caused by cool spots should show an anticorrelation (negative slope) with the bisector variations (see Queloz et al. 2001). The RV variations of CoRoT7 do show a slight anticorrelation with the bisectors (left panel of Fig. 11). If an RV signal is not due to activity, then removing this from the observed RV measurements should result in a stronger correlation between the bisectors and RV variations. Indeed, when one removes that signal of the 0.85d, 3.7d, and 9d period from the RV data the bisector span  RV variations become more correlated (r = 0.42, right panel). This suggests that the 0.85d, 3.7d, and 9d periods (i.e. f_{1}, f_{2}, and f_{3}) found in the RV data are not associated with activity.
Figure 11: (Left) Bisctor span of the CCF versus the RV measurements. The correlation coefficient is 0.28. (Right) The BisectorRV correlation after f_{1}, f_{2}, f_{3} (planet signals) have been removed from the data. The correlation coefficient is 0.42. 

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Figure 12 shows the correlation coefficient between the bisector and RV measurements as a function of data sets with the contributions of various frequencies removed (denoted ``Model Number'') Model 1 is to the original RV data set. Model 2 is this data set with the 0.85d period removed. Model 3 is the previous model, but with the 3.7 d period also removed. Model 4 is the data set with the 0.85d, 3.7d, and 9d periods removed. Note that the correlation coefficient becomes more negative with the removal of each data set suggesting that these 3 periods are not associated with stellar activity.
Model 5 represents Model 4  . Each subsequent model is the previous model with successive frequencies listed in Table 1 removed (and skipping of course f_{1}, f_{2}, and f_{3} already subtracted in Model 4). The fact that the RVBisector variations become more uncorrelated with the removal of additional frequencies suggests that all frequencies in Table 1 except f_{1}, f_{2}, and f_{3} are most likely due to activity.
Figure 12: The correlation coefficient of the CCF bisector span with RV as a function of different versions of the RV data with the frequencies in Table 1 removed. Model 1: raw data, Model 2: f_{1} removed, Model 3: f_{1} and f_{2} removed, Model 4: f_{1}, f_{2}, and f_{3} removed. Model 5: Model 4 and removed. Others: subsequent removal of all other frequencies in Table 1. 

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Because the RV variations are directly related to the bisector variability we can use the temporal variations of the RV to produce a predicted bisector variability. Saar & Donahue (1997) gave relationships relating both the bisector span and RV amplitude as a function of spot filling factor and rotational velocity of the star. The RVtoBisector amplitudes ratio from their expressions is predicted to be about a factor of 10. However, the exact ratio depends on several factors, primarily how one measures the bisector span and which spectral lines are used. Their result cannot be directly compared to the bisector measurements of the CCF from the HARPS data. A better way is to use the RVtoBisector amplitude ratio estimated by comparing the amplitudes of frequencies found in both the RV and bisector amplitude spectra and using data where these quantities (bisector and RV) were measured in a consistent way. The RV frequencies c d^{1} and 0.094 c d^{1} in Table 1 have amplitudes of 7.5 m s^{1} and 5.69 m s^{1}. The corresponding frequencies in the bisector amplitude spectrum have amplitudes of 4.21 m s^{1} and 2.81 m s^{1}, respectively. This implies that the RVtoBisector amplitude is 2.
We created a model of the bisector variations based on the amplitude spectrum of the RV measurements. Two fake data sets of bisector variations were generated. The first used all the frequencies in Table 1, excluding f_{1}, f_{2}, and f_{3}. All amplitudes in Table 1 were reduced by a factor 0.5 corresponding to the bisectortoRV amplitude ratio. The sampling of this time series was the same as the actual data. The bisector variations have an rms scatter of 4.5 m s^{1} after removal of the dominant frequencies. This was taken as the mean bisector error and random noise at this level was added to the fake bisector data. The second data set was similar to the first one, but the frequency f_{3} was present with the appropriately scaled amplitude (i.e. only f_{1} and f_{2} were removed).
The top panel of Fig. 13 shows the Scargle periodogram of the actual bisector measurements. The middle panel shows the periodogram of the fake data, but without the presence of the 9d period. The bottom panel shows the periodogram of the fake bisector data with the 9d period present. Vertical red lines show the rotation frequency and its first 3 harmonics. The vertical blue line shows the frequency corresponding to the 9d period.
There are two interesting features about this figure. First, the periodogram of the fake bisector data without the 9d period looks qualitatively like the real data. Many of the same peaks are seen in both periodograms. The ratio of the amplitudes are not quite correct probably due to the bisector data having more complicated noise characteristics than the Gaussian noise in our simple model. Furthermore, for high frequency components that the RVtoBisector amplitude ratio may be different. The second important feature to note is that in the periodogram of the fake data with the 9d period present there is a signficant peak at c d^{1} that is not seen in the data periodogram. If the 9d period was due to activity we should have seen a corresponding peak in the periodogram of the bisectors and most likely in the Ca II and FWHM. This also argues in favor of the 9d period not being related to activity.
Figure 13: (Top) Scargle periodogram of the CCF bisector variations. (Middle) Scargle periodogram of a fit generated using the RV frequencies of Table 1, but without f_{1}, f_{2}, and f_{3}present. Amplitudes were adjusted according to the measured RVtoBisector amplitudes. Random noise at the level observed for the bisector measurements were also added. (Bottom) Same as for the middle panel but with f_{3} (9d period) present. 

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8 A search for transits from CoRoT7d
The CoRoT7 light curve was analyzed to see if a 9d transit signal could be found in the data. A similar investigation was already performed to search for transits from CoRoT7c, but none was found (Q09). If the orbits of all planets are coplanar we do not expect to see transits from CoRoT7d. However, if substantial differences of the orbital inclination between the planets exist, CoRoT7d may well transit in spite of having a larger orbital radius than CoRoT7c.
The CoRoT7 light curve first had to be filtered for the large variations due to the stellar activity. This was done by: 1) normalizing the light curve by the maximum value; 2) performing outlier rejection; 3) reducing residual orbital effects by using a running median of length one orbit; and 4) tracking slow variations using a sliding polynomial of 12 hours and subtracting these. Finally, we fit the transit curve of CoRoT7b and subtracted that from the light curve.
This processed light curve was then phasefolded to the 9.02 d period. No transit signal above the noise was detected. We derive an upper limit of for the depth of any transit at a period of 9.02 d.
9 Orbital solutions
9.1 The 0.85d period
Models of the internal structure of CoRoT7b rely on the mass determination which in turn hinges on the amplitude of the RV variations. In Q09 the amplitude of CoRoT7b was estimated to be 3.5 m s^{1}using two different approaches and this corresponds to a planet mass of 4.8 . However, this value was obtained after applying a correction term for the effects of the filtering process to both techniques using simulated data. The uncorrected prewhitening procedure amplitude was slightly higher at 4.2 m s^{1} and the harmonic filtering amplitude lower at 1.9 m s^{1}. Clearly, the amplitude of CoRoT7b depends on how one removes the activity signal.
As an alternative approach to determining the RV amplitude of CoRoT7b we took the results from Sect. 6. In this analysis we used only the RV data for which multiple measurements were made each night. A least squares sine fit to this data was made keeping the period fixed and allowing the nightly offset to vary. The final offsets were then subtracted from the individual nights and the data combined. This may be the best way to account for the RV variations of activity without any assumptions about its temporal behavior. An orbital solution was performed on all the residual RVs keeping the ephemeris, T_{0}, fixed to the CoRoT transit time of 2 454 446.7311.
Table 13: Orbital parameters for the 0.85d period.
Table 13 lists the orbital elements. At first the nightly data were fit keeping the CoRoT transit period of 0.8535 days. If we allow this parameter to vary we get a best fit to the data with a period of 0.85359 days which is listed in the table. Allowing the T_{0} to vary, but keeping the period fixed results in T_{0} = 2 454 446.7330 a value very close to the CoRoT ephemeris. Allowing the eccentricity to vary results in a best fit value of 0.08, but with large error, 3. We cannot exclude a slight eccentricity in the orbit, but given the large variations due to activity and the additional companions, this may be difficult to extract reliably from the RV data. Figure 14 shows the zeropoint corrected data phased to the CoRoT transit ephemeris and a period of 0.85359. The solid line represents the orbital solution.
The derived Kamplitude is 5.04 1.09 m s^{1} which results in a companion mass of 6.9 1.4 . This is slightly larger than the Kamplitude of 4.16 0.27 m s^{1}(m = 5.75 0.37 ) by prewhitening the full data set (Q09). The Kamplitude from prewhitening of the full data set and the analysis of the subset RV data with multiple measurements each night both suggest a slightly higher planet mass than the 4.8 0.8 of Q09, although all determinations are consistent to within the errors.
Figure 14: (Top) Orbital solution for the 0.85d period using the data with repeated nightly measurements and the appropriate zeropoint offset applied. 

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9.2 The 3.7d period
RV residuals were produced by subtracting all sine components except for f_{2} from the full RV data set and an orbital solution calculated. In removing the contribution of f_{1} the amplitude in Table 13 was used rather than the slightly higher amplitude found in Table 1. The derived amplitude is slightly lower than the one presented in Q09 (5.5 m s^{1}) that removed f_{1} using the amplitude found in the prewhitening procedure. In order to estimate the range of velocity amplitudes for f_{2} a least squares fit to the original RV data was first made using this frequency and the subsequent frequencies found in the prewhitening process sequentially subtracted. The range of amplitudes for f_{2} during this process ranged from 4.75 to 5.4 m s^{1}. An error of m s^{1} was adopted which is slightly more than the formal error of m s^{1} from the orbit fitting. Note that this formal error is much lower than for the amplitude CoRoT7b which was calculated using only a subset of the data.
Figure 15 shows the orbital solution the 3.7day period. The orbital elements are listed in Table 14. A slight eccentricity is found, but this may well be an artifact due to the filtering process.
Figure 15: The RV residuals of CoRoT7 after removing all components in Table 1 except for f_{2} and phased to the 3.7 d period (points). The orbital fit is shown as a line 

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9.3 The 9d period
The RV residuals were calculated after subtracting all sine components in Table 1 except for f_{3} and again using the amplitude for f_{1} from Table 13. The range of possible amplitudes for f_{3} during the prewhitening procedure was 5.57.15 m s^{1}. We thus adopted an error in the ampitude of m s^{1}, larger than the formal error of m s^{1}, but probably a more realistic estimate. A best fit orbit allowing the eccentricity to vary resulted in a slightly negative value. We therefore took a solution with the eccentricity fixed to zero with an error of .
Figure 16 shows the orbital solution to the RV residuals using the 9day period. The orbital elements are listed in Table 15. Note the gaplike structures in the phase curve. This is undoubtedly due to the period being nearly an integer value of one day, i.e. our typical sampling rate.
Table 14: Orbital parameters for the 3.7d period.
10 On the dynamical stablity of the 3planet system.
We also investigated whether the 3planet system would be dynamically stable. Although a stable system is no proof that all 3 planets exist, an unstable system would indicate that the additional planetary signals found in the HARPS data may arise from activity.
10.1 An ultracompact planet system?
The stability of planetary systems involves multiple interactions of planets by mutual perturbations often involving interactions of resonances between more than two planets and various components of their motions. It is a stability for some time. As Lecar et al. (2001) summarize it: The solar system is not stable, it is just old!. Given the snapshot provided by discovery orbital elements we first briefly overview the gross/overall properties of the CoRoT7 system by a simple stability indicator based on Hillexclusion volumes. It requires nonoverlapping cylindrical volumes of halfwidth , around each planet orbit. The Hillradius to lowest order is , with m_{i},a_{i} denoting the mass and semimajoraxis of the ith planet, respectively, and k is a factor of 415 depending on the number of planets, the dynamical structure of the system (masses, orbital elements), and the timescale for stability under consideration, cf. e.g. Chambers et al. (1996) including a discussion on system stability with longterm orbital calculations. Funk et al. (2010) show that for closein systems, there are surprisingly large volumes of phase space for stable and planetrich systems at periods of less than 10 days around solar mass stars. These ultra compact systems can easily harbor 8 Super Neptunes for and up to . Funk et al. (2010) determine a factor of that is necessary for stability in the present context  3 planets, masses below Neptune's and few Ga timescales  and give examples for it being sufficient including closein systems with an additional Jupitermass planet at (i.e. 50 days).
An application of this Hillstability estimator to the CoRoT7 system is shown in Fig. 17. The Hillexclusion regions are outlined in a mass versus semimajor axis diagram for the system parameters determined here. Forbidden regions for other planets in a stable system are shown by shaded areas around every orbit. The dark reddish shaded area is for k=7, a secure upper bound to the Funk et al. (2010) results. The larger, lightblueish areas are for k=10 in order to approximately account for and securely bound uncertainties in the mass and semimajor axis determinations (6 and 3% resp. at ) and 15% for a possible orbital inclination^{}, of c and d. The width of the stability exclusion regions is emphasized by two horizontal bars in the resp. color at the top. The stellar radius (yellow) and the Rochelimit (green) are plotted as vertical bars on the left.
Figure 16: The RV residuals of CoRoT7 after removing all components in Table 1 except for f_{3} and phased to the 9.02 d period (points). The orbital fit is shown as a line 

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Table 15: Orbital parameters for the 9.02d period.
Figure 17: Synopsis and simple stability for the CoRoT7 system. Planetary mass in Earthunits is plotted against the distance from the star in AU. Mass and semimajor axis determinations of this work (blue dots) and the discovery paper (green dots) are shown for the CoRoT7system, together with their 1 and error ellipses (reddish and greenish, resp). Errors are due to the measurements and analysis of the RV signals for CoRoT7 and the high resolution spectroscopic analysis of its photosphere. Semimajor axis ranges excluded by the Hillexclusion stability criteria are shaded. Dark, reddish and light, blueish areas corresponding to kvalues of 7 and 10 respectively. Uncertainties in stability analysis, orbital inclinations and measurement errors are included approximately by the latter value, see text. The stellar radius (yellow) and the Rochelimit (green) are indicated on the left for orientation. The nonoverlap of the shaded areas required by Hillexclusionstability indicates the stability of the CoRoT7system as outlined here. Note: error ellipses are partially covered by the dotsymbols for CoRoT7b,c. 

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For comparison the massestimates of the discovery paper, Q09 are shown with their 1 and errorellipses to demonstrate that they clearly provide less stringent stability constraints due to smaller mass values.
The CoRoT7 system as presented here, is clearly found stable as demonstrated by the nonoverlap of the appropriate Hillexclusion zones. Not much space for stable planet orbits is left between components c and d. Thus the system is dynamically full  as the solar system, cf. Lecar et al. (2001). However, according to this simple approach a small planet might fit in between b and c if orbits are and remain circular.
This merits a detailed dynamical analysis that fully accounts for orbital inclinations (with only loose observational constraints for c,d), the eccentricities and the interactions of all components on the various timescales.
10.2 A short dynamical study of the CoRoT7 system
Figure 18: Time evolution of the three planets' eccentricities for different inclinations of CoRoT7c: 1 (top), 16 (middle) and (lower). 

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We performed a more detailed dynamical study of the stability of CoRoT7 using different initial parameters that took into account the errors in the orbital elements:
 the orbital periods of all three planets have only errors in the order of 0.1 and consequently for our numerical study these were not varied;
 because of the large errors in the perihelia we just set them to 0;
 for the planet masses we have taken the nominal values (8.3, 12.8 and 17.1 for CoRoT7b, CoRoT7c and CoRoT7d, respectively);
 the eccentricities of all planets are relatively small and especially the innermost one may suffer from tides which may keep its eccentricity very small^{};
 there is no information available about the mutual inclination; therefore in a first attempt we just set their orbital inclination to small values (1, 2 and ).
 1.
 R1: the inclination of CoRoT7c was initially set to , whereas the other two planets initially moved in the same plane;
 2.
 R2: the inclination of CoRoT7d was initially set to , whereas the other two planets initially moved in the same plane.
The results of R2 are shown in Fig. 19, where it is again seen that a different inclination for one of the planets' orbits (in this case of CoRoT7d) may change the other orbits significantly. This is not the case when the inclination of the outermost planet is set to only ; we do not show this graph since it is quite similar to the one with CoRoT7c set to an inclined orbit of . In the two upper panels we depict the results of the time evolution of the eccentricities of all three planets using an inclination for CoRoT7d of (upper panel) and (middle panel). In the upper panel it is visible that the innermost planet has a quite different period in its eccentricity behavior compared to Fig. 18 (middle panel). For the picture is very different from the lower panel in Fig. 18. It is evident that the CoRoT7b (eccentricity 0 < e < 0.45) is not on a regular orbit but shows signs of chaoticity in eccentricity and in inclination (Fig. 19 lower panel). This can be understood in terms of the larger mass of CoRoT7d strongly perturbing CoRoT7c and thus indirectly perturbing CoRot7b and making the orbit of this innermost planet chaotic, but not yet unstable. A larger inclination of either CoRoT7c or CoRoT7d may put CoRoT7b into a Kozai resonance (Kozai 1962) which is known to enlarge the eccentricity significantly and can lead to unstability of the whole system.
Figure 19: Time evolution of the three planets' eccentricities for different inclinations of CoRoT7d: (upper graph) and (middle graph). On the lower panel we plot the inclination and the eccentricity (times 100) of CoRoT7b, where the nonregular behaviour is clearly visible. 

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10.2.1 Consequences of different inclinations for the transit
With the quite reasonable assumption that the three planets move on mutually inclined orbits we now test how that would influence the transit of the innermost planet CoRoT7b. We cannot expect a large influence in its orbit on the short time scales CoRoT7 was observed by CoRoT or HARPS. However, the big advantage of the planetary system which we are studying is that CoRoT7b has an orbital period of less than one day and the other two presumed planets are also in very closein orbits around the star. This accelerates the dynamics of the system, which means that any mutual gravitational influence (perturbations on the Keplerian orbits) is visible on short time scales. We checked the change in the inclination of the orbit of CoRoT7b depending on the mutual inclinations with the aim of possibly measuring the influence on the inclination of CoRoT7b which could be larger than the given errors bars derived from the light curve analysis ( ).
In fact, Fig. 20 (upper panel) shows how the dynamics of the system could influence the inclination of CoRoT7b. The lower line shows the difference in inclination with respect to the actual assumed orbit after 1 year, the middle line after 3 years, and the upper line after 10 years when the inclination of CoRoT7c has different inclinations between 1 and . Figure 20 (lower panel) shows the same for a change in the inclination of CoRoT7d.
After these results we can conclude the following: after one year of observation (lowest line with ``+'') in none of the cases is the effect larger than the errors on i. This is shown by the thick horizontal line which indicates the error in the determined inclination of CoRoT7b. The change in i is well within the measurement error. After three years could be in the order when CoRoT7c would be on an inclined orbit of ( with respect to CoRoT7b). This is visible from the crossing of the line (with stars) and the thick line; it would be undetectable when CoRoT7d would move on an inclined orbit. Only after ten years of observation a significant effect ( ) would be detectable for inclinations and for runs R1 and R2, respectively.
We can conclude that
 1.
 the system of three planets of the star CoRoT7 with the parameters determined via RV and the transits observed by CoRoT is in a very stable state even for hundreds millions of years when their orbital planes are almost the same. They would even be stable for mutually inclined orbits ;
 2.
 mutually inclined orbits show quite interesting effects on the duration of the transit of CoRoT7b. If CoRoT7c were inclined by with respect to CoRoT7b, a detectable effect could be observed in the change in the inclination of CoRoT7b via the duration of the transit within the lifetime of the satellite CoRoT.
11 Discussion
Our Fourier analysis of the HARPS time series of RV measurements for CoRoT7 reveals up to 9 frequencies. Most of these are associated with the activity signal. However, this analysis also found 3 frequencies not associated with activity: f_{1} = 1.1715 c d^{1} ( P = 0.8535 d), f_{2} = 0.270 c d^{1}, and f_{3} = 0.1101 c d^{1}). The first coincides with the transit frequency found in the CoRoT7 light curve and f_{2} coincides with the second planet, CoRoT7c, also reported by Q09 using the same data set. The final frequency f_{3} may be due to an additional companion.
The analysis of the RV data presented in Sects. 5 and 6 reveals that the CoRoT transit period is present in the RV data with a very high degree of statistical significance. There can be no doubt the transitlike events seen in the CoRoT7 light curves are caused by a 2 radius planet in a 0.85d orbit.
The mass of CoRoT7b which is important for planet structure models depends on the amplitude of the 0.85d period in the RV data. Unfortunately, due to the relatively high activity of CoRoT7 this amplitude depends on the details of how the stellar signal is removed. In Q09 the mass of CoRoT7b can thus be as low as 2.6 and as high as 5.5 .
Figure 20: The difference in inclination of CoRoT7b (yaxis) compared to an initial plane orbit of CoRoT7b (xaxis) versus the inclination of CoRoT7c (upper graph) after 1 (lower line), 3 and 10 years (upper line). The same plot for different inclinations of CoRoT7d; the thick line is the assumed error ( in the determination of the orbit of (lower graph). 

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The analysis of the RV measurements from individual nights where at least 2 measurements were made may yield the best estimate of the RV amplitude of CoRoT7b. By fitting the CoRoT7b period to the data and allowing the zeropoint velocity offset to vary each night in a least squares sense we can account for the influence of stellar activity in a simple and model independent way. The fact that the calculated zeropoint offsets from each night recovers both the rotational period of the star and the signal due to CoRoT7c suggests that this approach is valid. This approach yields an RV amplitude of 5.04 1.09 m s^{1} which results in a mass of 6.9 1.4 .
Recently, Bruntt et al. (2010) performed a detailed spectral analysis of CoRoT7 and determined a stellar radius of R_{*} = 0.82 0.04 . This results in a revised planet radius of .58 0.1 . This along with our slightly higher planet mass results in a density of 9.6 2.7 gm cm^{3} which puts it squarely on the Valencia et al. (2009) curve for Earthlike planets (33% iron and 67% silicates). In terms of structure CoRoT7c may indeed be an Earthlike planet.
Although this work and Q09 conclude that the 3.7d period in the RV is due to an additional companion, the nature of the 9day period is still not fully resolved. Other approaches to the analysis of the RV time series attributes this signal to the activity signal (Melo, in prep.). Lanza et al. (2010) investigated the effects of photospheric spots on the RV variations of CoRoT7, but could not confirm whether a 9d period was in fact due to activity. However, our analysis presented here gives strong evidence in support of a third companion:
 When the data is divided into subsets the Scargle power in the periodogram at 0.11 c d^{1} increases with the addition of each data set (Sect. 5). In other words the signal becomes more significant with additional data  a behavior consistent with a periodic signal that is coherent and longlived.
 This signal is not found in the periodograms of any of the three activity indicators: bisector span, Ca II Sindex, and the FWHM of the CCF in spite of all three having the exact same sampling as the RV data. Any activity signal found in the RV should be seen in at least one of these indicators.
 We have demonstrated that an analysis of subsets of the data using filtering with rotational harmonics may remove a 9d period to the data even if one is known to be present. Just because harmonic filtering removes a 9d signal from the Fourier power spectrum is not an indication that this signal is due to rotation modulation.
 The highest degree of correlation between the RV and bisector data occurs after removing the RV signal of the 0.85d, 3.7d, and 9.02d periods. This suggests that these 3 periods do not arise from stellar activity.
 A model of the bisector variations using scaled version of the RV variations, but without the presence of f_{1}, f_{2}, and f_{3} and with the appropriate level of noise produces a periodogram that is in good agreement with the periodogram of the observed bisector variations. It is difficult to understand why the 9d period appears so strongly in the RV power spectrum,but not at all in the bisector power spectrum if it is due to activity.
The hypothesis that CoRoT7 has a third planetary companion is one that is easily verified. All that is required are additional RV measurements of quality and quantity that are comparable to the HARPS measurements used in this study. If the RV signal for CoRoT7d remains constant in phase and amplitude it would be difficult to attribute it to activity. (This also holds for CoRoT7c). However, given that the 9d period is close to the first harmonic of the rotational frequency, data with a rather long time base, like the ones used in this study, may be required. Verification of the third planet is important as this would make the CoRoT7 system an excellent example of an ultrapacked planetary system.
Additional RV measurements are also important for reducing the errors on the planet mass needed for comparing to planetary structure models. The complexity of the RV variations for CoRoT7 and the high level of activity also means that it would be difficult to obtain a value of the planet mass of CoRoT7b to better than about 20% without signficantly more RV measurements. However, CoRoT7 is such an interesting system further measurements may be worthwhile. Given that 80 h of HARPS time have already been devoted to CoRoT7 only stresses the need for considerable telescope resources for precise RV studies of exoplanets.
AcknowledgementsThe authors thank DLR and the German BMBF for support under grants 50 OW 0205, 50 OW 0501, 50 OW 0603. Günther Wuchterl thanks the MPE for computationresources on DEC/VMS machines. A.P.H. would like to thank the CoRoT Exoplanet Science Team for useful discussions, helpful comments, and critical remarks which resulted in a much improved analysis of the RV data. We also thank the referee, Gordon Walker, for useful comments which resulted in an improved paper. We also thank him for his rapid refereeing of the paper.
References
 Auvergne, M., Bodin, L., Boisnard, L., et al. 2009, A&A, 506, 411 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Baglin, A., Auvergne, M., Boisnard, L., et al. 2006, in COSPAR, Plenary Meeting, 36th COSPAR Scientic Assembly, 36, 3749 [Google Scholar]
 Bruntt, H., Deleuil, M., Fridlund, M., et al. 2010, A&A, 519, A51 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Chambers, J. E., Wetherill, G. W., & Boss, A. P. 1996, Icarus, 119, 261 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Charbonneau, D., Berta, Z. K., Irwin, J., et al. 2009, Nature, 462, 891 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Funk, B., Wuchterl, G., Schwarz, R., PilatLohinger, E., & Eggl, S. 2010, accepted [Google Scholar]
 Hatzes, A. P., Cochran, W. J., & Bakker, E. J. 1998, ApJ, 508, 380. [NASA ADS] [CrossRef] [Google Scholar]
 Kozai, Y. 1962, AJ, 67, 591 [NASA ADS] [CrossRef] [MathSciNet] [Google Scholar]
 Kürster, M., Schmitt, J. H. M. M., Cutispoto, G., & Dennerl, K. 1997, A&A, 320, 831 [NASA ADS] [Google Scholar]
 Kuschnig, R., Weiss, W. W., Gruber, R., Bely, P. Y., & Jenkner, H. 1997, A&A, 328, 544 [NASA ADS] [Google Scholar]
 Lanza, A. F., Bonomo, A. S., Moutou, C., et al. 2010, A&A, 520, A53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Lecar, M., Franklin, F. A., Holman, M. J., & Murray, N. J. 2001, ARA&A, 39, 581 [NASA ADS] [CrossRef] [Google Scholar]
 Leger, A., Rouan, D., Schneider, J., et al. 2009, A&A, 506, 287 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [Google Scholar]
 Lenz, P., & Breger, M. 2004, The AStar Puzzle (Cambridge, UJ: Cambridge University Press), IAU Symp., 224, 786 [Google Scholar]
 Queloz, D., Henry, G., Sivan, J. P., et al. 2001, A&A, 379, 279 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Queloz, D., Bouchy, F., Moutou, C., et al. 2009, A&A, 506, 303 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Saar, S. H., & Donahue, R. A. 1997, ApJ, 485, 319 [NASA ADS] [CrossRef] [Google Scholar]
 Scargle, J. D. 1982, ApJ, 263, 835 [NASA ADS] [CrossRef] [Google Scholar]
 Stellingwerf, R. F. 1978, ApJ, 224, 953 [NASA ADS] [CrossRef] [Google Scholar]
 Valencia, D., Ikoma, M., Guillot, T., & Nettelmann, N. 2010, A&A, 516, A20 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
Footnotes
 ...CoRoT7^{}
 Based on observations made with HARPS spectrograph on the 3.6m ESO telescope under programs 082.C0120, 082.C0308(A), and DDT program 282.C5036(A).
 ... inclination^{}
 That corresponds to an inclination of the orbital plane with respect to the sky, .
 ... small^{}
 The computations have been undertaken in the Newtonian framework with assumed point masses of the planets. Internal tests have shown that the tides may not significantly change all orbits even when the parameter Q_{0} was varied within orders of magnitudes
 ... tested^{}
 Note that an assumed inclination in the signal of the RV means that the masses of CoRoT7c and 7d are minimum masses; we therefore in our test computations took care of this fact.
All Tables
Table 1: Frequencies and amplitudes found by a prewhitening procedure on the HARPS RV data.
Table 2: The data subsets.
Table 3: Frequencies found in data Subset 1.
Table 4: Frequencies found in data Subset 2.
Table 5: Frequencies found in data Subset 3.
Table 6: Frequencies found in data Subset 4 using the same analysis as Tables 35, i.e. first removing the contribution of , f_{1}, f_{2}, f_{3}. Column 3 shows the amplitude derived using fake data (see text).
Table 7: Frequencies found in the bisector data using a prewhitening procedure.
Table 8: Frequencies found in the Ca II data using a prewhitening procedure.
Table 9: Frequencies found in the FWHM data using a prewhitening procedure.
Table 10: Scargle power and False Alarm Probability for the Peak at 1.17 c d^{1}, for RV, bisector, and Ca II data.
Table 11: Frequencies found in the simulated data set of Subset 1 (Fig. 10) using a prewhitening procedure and harmonic analysis.
Table 12: Prewhitened frequencies found in the RV data after first fitting the rotational frequency and its first 2 harmonics.
Table 13: Orbital parameters for the 0.85d period.
Table 14: Orbital parameters for the 3.7d period.
Table 15: Orbital parameters for the 9.02d period.
All Figures
Figure 1: Scargle periodograms of the RV ( top), bisector ( upper middle), Ca II Sindex ( lower middle), and FWHM ( bottom) measurements for the frequency range 00.3 c d^{1} ( left panels) and 1.01.3 c d^{1} ( right panels). The vertical blue lines mark frequencies seen only in the RV (the one in the right panel is the transit frequency). Vertical red lines mark the rotational frequency and its first 3 harmonics. 

Open with DEXTER  
In the text 
Figure 2: Spectral window function for the HARPS measurements. 

Open with DEXTER  
In the text 
Figure 3: Scargle periodograms resulting from sequential adding of data subsets. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. 

Open with DEXTER  
In the text 
Figure 4: Scargle periodograms resulting from sequential adding of residual RV data for the 3.7day period. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. All sine components except the that associated with the 9.02day period. 

Open with DEXTER  
In the text 
Figure 5: Scargle periodograms resulting from sequential adding of residual RV subsets for the 9day period. Red line: subset 1, green line: subset 1 plus subset 2, blue: all data sets. 

Open with DEXTER  
In the text 
Figure 6: (Top) Scargle periodogram of the data set consisting of 7 nights where at least 3 RV measurements were made. The measurements from each night were considered an independent data set and a fit was made using the period of CoRoT7b and allowing zero point offset from each night to vary. The periodogram is of the data with the offset to each night subtracted. (Bottom) Same as in the top panel but with the addition of 16 nights for which two RV measurements were made per night. 

Open with DEXTER  
In the text 
Figure 7: (Top) RV measurments of the 7night data set (zeropoint offsets applied) phased to the period of CoRoT7b. (Bottom) same measurements phased to the alias period of 5.82 days. 

Open with DEXTER  
In the text 
Figure 8: The reduced as a function of period for the data set consisiting of nights with multiple RV measurements. The zeropoint offset from each night was allowed to vary. The vertical line indicates the period of CoRoT7b. 

Open with DEXTER  
In the text 
Figure 9: A prewhitening on the zeropoint offsets of the multimeasurement nights found by the least squares fitting. ( Top) Amplitude spectrum of the zeropoint values. The dashed line indicates the rotation period of CoRoT7b. ( Middle) The amplitude spectrum after removing the rotational frequency. The vertical line corresponds the frequency of the 3.7d period of CoRoT7c. ( Bottom) The amplitude spectrum after also removing 3.7d period signal. The vertical line corresponds to the frequency f_{3}. 

Open with DEXTER  
In the text 
Figure 10: (Top) Scargle periodogram for the fit to RV first data subset (truncated JD = 47754807) sampled in the same manner as the data and with noise at a level of m s^{1}. (bottom) The Scargle periodogram of the real data. The vertical lines mark the frequencies of the 9d and 3.7d signals that are in the fake data. 

Open with DEXTER  
In the text 
Figure 11: (Left) Bisctor span of the CCF versus the RV measurements. The correlation coefficient is 0.28. (Right) The BisectorRV correlation after f_{1}, f_{2}, f_{3} (planet signals) have been removed from the data. The correlation coefficient is 0.42. 

Open with DEXTER  
In the text 
Figure 12: The correlation coefficient of the CCF bisector span with RV as a function of different versions of the RV data with the frequencies in Table 1 removed. Model 1: raw data, Model 2: f_{1} removed, Model 3: f_{1} and f_{2} removed, Model 4: f_{1}, f_{2}, and f_{3} removed. Model 5: Model 4 and removed. Others: subsequent removal of all other frequencies in Table 1. 

Open with DEXTER  
In the text 
Figure 13: (Top) Scargle periodogram of the CCF bisector variations. (Middle) Scargle periodogram of a fit generated using the RV frequencies of Table 1, but without f_{1}, f_{2}, and f_{3}present. Amplitudes were adjusted according to the measured RVtoBisector amplitudes. Random noise at the level observed for the bisector measurements were also added. (Bottom) Same as for the middle panel but with f_{3} (9d period) present. 

Open with DEXTER  
In the text 
Figure 14: (Top) Orbital solution for the 0.85d period using the data with repeated nightly measurements and the appropriate zeropoint offset applied. 

Open with DEXTER  
In the text 
Figure 15: The RV residuals of CoRoT7 after removing all components in Table 1 except for f_{2} and phased to the 3.7 d period (points). The orbital fit is shown as a line 

Open with DEXTER  
In the text 
Figure 16: The RV residuals of CoRoT7 after removing all components in Table 1 except for f_{3} and phased to the 9.02 d period (points). The orbital fit is shown as a line 

Open with DEXTER  
In the text 
Figure 17: Synopsis and simple stability for the CoRoT7 system. Planetary mass in Earthunits is plotted against the distance from the star in AU. Mass and semimajor axis determinations of this work (blue dots) and the discovery paper (green dots) are shown for the CoRoT7system, together with their 1 and error ellipses (reddish and greenish, resp). Errors are due to the measurements and analysis of the RV signals for CoRoT7 and the high resolution spectroscopic analysis of its photosphere. Semimajor axis ranges excluded by the Hillexclusion stability criteria are shaded. Dark, reddish and light, blueish areas corresponding to kvalues of 7 and 10 respectively. Uncertainties in stability analysis, orbital inclinations and measurement errors are included approximately by the latter value, see text. The stellar radius (yellow) and the Rochelimit (green) are indicated on the left for orientation. The nonoverlap of the shaded areas required by Hillexclusionstability indicates the stability of the CoRoT7system as outlined here. Note: error ellipses are partially covered by the dotsymbols for CoRoT7b,c. 

Open with DEXTER  
In the text 
Figure 18: Time evolution of the three planets' eccentricities for different inclinations of CoRoT7c: 1 (top), 16 (middle) and (lower). 

Open with DEXTER  
In the text 
Figure 19: Time evolution of the three planets' eccentricities for different inclinations of CoRoT7d: (upper graph) and (middle graph). On the lower panel we plot the inclination and the eccentricity (times 100) of CoRoT7b, where the nonregular behaviour is clearly visible. 

Open with DEXTER  
In the text 
Figure 20: The difference in inclination of CoRoT7b (yaxis) compared to an initial plane orbit of CoRoT7b (xaxis) versus the inclination of CoRoT7c (upper graph) after 1 (lower line), 3 and 10 years (upper line). The same plot for different inclinations of CoRoT7d; the thick line is the assumed error ( in the determination of the orbit of (lower graph). 

Open with DEXTER  
In the text 
Copyright ESO 2010