Issue 
A&A
Volume 593, September 2016



Article Number  A120  
Number of page(s)  13  
Section  Stellar structure and evolution  
DOI  https://doi.org/10.1051/00046361/201628616  
Published online  04 October 2016 
Interior rotation of a sample of γ Doradus stars from ensemble modelling of their gravitymode period spacings^{⋆}
^{1} Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D 3001 Leuven Belgium
email:
timothy.vanreeth@ster.kuleuven.be
^{2} Department of Astrophysics, IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands
Received: 31 March 2016
Accepted: 3 July 2016
Context. Gamma Doradus stars (hereafter γ Dor stars) are known to exhibit gravity and/or gravitointertial modes that probe the inner stellar region near the convective core boundary. The nonequidistant spacing of the pulsation periods is an observational signature of the stellar evolutions and current internal structure and is heavily influenced by rotation.
Aims. We aim to constrain the nearcore rotation rates for a sample of γ Dor stars for which we have detected period spacing patterns.
Methods. We combined the asymptotic period spacing with the traditional approximation of stellar pulsation to fit the observed period spacing patterns using χ^{2}optimisation. The method was applied to the observed period spacing patterns of a sample of stars and used for ensemble modelling.
Results. For the majority of stars with an observed period spacing pattern we successfully determined the rotation rates and the asymptotic period spacing values, although the uncertainty margins on the latter were typically large. This also resulted directly in the identification of the modes that correspond to the detected pulsation frequencies, which for most stars were prograde dipole gravity and gravitoinertial modes. The majority of the observed retrograde modes were found to be Rossby modes. We also discuss the limitations of the method that are due to the neglect of the centrifugal force and the incomplete treatment of the Coriolis force.
Conclusions. Despite its current limitations, the proposed method was successful to derive the rotation rates and to identify the modes from the observed period spacing patterns. It forms the first step towards detailed seismic modelling based on observed period spacing patterns of moderately to rapidly rotating γDor stars.
Key words: asteroseismology / methods: data analysis / stars: fundamental parameters / stars: variables: general / stars: oscillations
Based on data gathered with the NASA Discovery mission Kepler and the HERMES spectrograph, which is installed at the Mercator Telescope, operated on the island of La Palma by the Flemish Community at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, and supported by the Fund for Scientific Research of Flanders (FWO), Belgium, the Research Council of KU Leuven, Belgium, the Fonds National de la Recherche Scientifique (F.R.S.FNRS), Belgium, the Royal Observatory of Belgium, the Observatoire de Genève, Switzerland, and the Thüringer Landessternwarte Tautenburg, Germany.
© ESO, 2016
1. Introduction
Gamma Doradus stars are early F to late Atype stars (with 1.4 M_{⊙} ≲ M ≲ 2.0 M_{⊙}) that exhibit nonradial gravity and/or gravitoinertial mode pulsations (e.g. Kaye et al. 1999). This places them directly within the transition region between lowmass stars with a convective envelope and intermediatemass stars with a convective core, where the CNOcycle becomes increasingly important relative to the ppchain as the dominant hydrogen burning mechanism (e.g. Silva Aguirre et al. 2011). The pulsations in γ Dor stars are excited by the flux blocking mechanism at the bottom of the convective envelope (Guzik et al. 2000; Dupret et al. 2005), although the κ mechanism has been linked to γ Dor type pulsations as well (Xiong et al. 2016). The oscillations predominantly trace the radiative region near the convective core boundary. As a result, these pulsators are ideally suited to characterise the structure of the deep stellar interior.
As shown by Tassoul (1980), highorder (n ≫ l) gravity modes are asymptotically equidistant in period for nonrotating chemically homogeneous stars with a convective core and a radiative envelope. This study was further expanded upon by Miglio et al. (2008). The authors found characteristic dips to be present in the period spacing series when the influence of a chemical gradient is included in the analysis. The periodicity of the deviations is related to the location of the chemical gradient, while the amplitude of the dips was found to be indicative of the steepness of the gradient. Bouabid et al. (2013) further improved upon the study by including the effects of diffusive mixing and rotation, which they introduced using the traditional approximation. The authors concluded that the mixing processes partially wash out the chemical gradients inside the star, resulting in a reduced amplitude for the dips in the spacing pattern. Stellar rotation introduces a shift in the pulsation frequencies, leading to a slope in the period spacing pattern. Zonal and prograde modes, as seen by an observer in an inertial frame of reference, were found to have a downward slope, while the pattern for the retrograde highorder modes has an upward slope.
Over the past decade the observational study of pulsating stars has benefitted tremendously from several spacebased photometric missions, such as MOST (Walker et al. 2003), CoRoT (Auvergne et al. 2009) and Kepler (Koch et al. 2010). While typically only a handful of modes could be resolved using groundbased data, the space missions have provided nearcontinuous high S/N observations of thousands of stars on a long time base, resulting in the accurate determination of dozens to hundreds of pulsation frequencies for many targets. In particular, this has proven to be invaluable for γ Dor stars, as their gravity and/or gravitoinertial mode frequencies form a very dense spectrum in the range of 0.3 to 3 d^{1}. Period spacing patterns have now been detected for dozens of γ Dor stars (e.g. Chapellier et al. 2012; Kurtz et al. 2014; Bedding et al. 2015; Saio et al. 2015; Keen et al. 2015; Van Reeth et al. 2015; Murphy et al. 2016).
In this study we focus on the period spacing patterns detected by Van Reeth et al. (2015) in a sample of 68 γ Dor stars with spectroscopic characterisation and aim to derive the stellar internal rotation rates and the asymptotic period spacing value of the series. This serves as a first step for future detailed analyses of differential rotation, similar to the studies that have previously been carried out in slow rotators among gmode pulsators that have recently been interpreted in terms of angular momentum transport by internal gravity waves (e.g. Triana et al. 2015; Rogers 2015). In this paper we present a grid of theoretical models, which we use as a starting point (Sect. 2), and explain our method to derive the rotation frequency (Sect. 3). The method is illustrated with applications on synthetic data (Sect. 4.1), a slowly rotating star with rotational splitting, KIC 9751996, and a fast rotator with a prograde and a retrograde period spacing series, KIC 12066947 (Sect. 4.2). We then analyse the sample as a whole (Sect. 4.3) before moving on to the discussion and plans for future indepth modelling of individual targets (Sect. 5).
2. Grid of stellar models and pulsation frequencies
We first computed a rough grid of theoretical stellar models to gain further insight into the internal structure and properties of γ Dor stars. To allow for a complete understanding, the models were purposely kept relatively simple. We did not include any rotational effects into the equilibrium models, allowing us to assume spherical symmetry and compute onedimensional models with the onedimensional MESA stellar evolution code (v7385; Paxton et al. 2011, 2013, 2015). The convection was treated using the mixing length theory with α_{MLT} = 1.8 and the Ledoux criterion with α_{sc} = 0.01. A single diffusive mixing coefficient was defined in the radiative region and fixed at a value of 1 cm^{2} s^{1}. We used the solar metallicity values given by Asplund et al. (2009) and OPAL type I opacity tables (Rogers & Nayfonov 2002). The varying parameter values of the models in the grid are given in Table 1.
For each of the models in our grid we also computed the asymptotic period spacing (1)with (2)as derived by Tassoul (1980) for highorder gravity modes. Here l is the spherical degree of the pulsation mode, r is the distance from the stellar centre, N is the BruntVäisälä frequency, and the boundaries of the mode trapping region are marked by r_{1} and r_{2} (Aerts et al. 2010). While ΔΠ_{l} is smaller for higher values of l (Eq. (1)), ΔΠ_{l} also changes as the star evolves. We therefore calculated the probability of observing different spacing values using the stellar ages in our grid models. As shown in Fig. 1, we typically expect ΔΠ_{l} values of about 3100 s and 1800 s for l = 1 and l = 2, respectively, which in turn implies that Π_{0} is of the order of 4400 s. In addition, there are strong linear correlations for ΔΠ_{l} between models with different values of M, Z, X, f_{ov}, and α_{ov}, assuming a fixed hydrogen abundance X_{c} in the convective core.
As shown by Bouabid et al. (2013) and as observed by Van Reeth et al. (2015), gravitymode period spacing patterns are heavily influenced by rotation. We therefore introduced the influence of rotation on the pulsation periods using the traditional approximation (Eckart 1960; Lee & Saio 1987; Townsend 2005). In this framework the θcomponent of the rotation vector is ignored (Lee & Saio 1997) and it is assumed that the star is sufficiently slowly rotating, so that the effects of the centrifugal force can be neglected. While this particular assumption may not always be applicable, gravity modes and gravitoinertial modes are mostly sensitive to the stellar properties near the convective core, where the rotational deformation of the star remains limited. This is illustrated in Fig. 2, which shows the BruntVäisälä frequency N and the rotational kernel K_{nl} for the lowest and highestorder mode of the stellar model discussed in Sect. 4.1. Both functions correlate with the sensitivity of the pulsations to the different regions in the star and peak near the convective core boundary. The rotational kernel K_{nl} specifically indicates the sensitivity of the pulsations to the local stellar rotation profile. Thus, the rotational frequencies deduced from pulsational properties throughout this paper correspond with the nearcore interior rotation rates.
Fig. 1 Distributions of the asymptotic period spacing values ΔΠ_{l} for spherical degree l = 1 and 2 computed for the MESA evolution tracks with the input parameters provided in Table 1. The ages and evolution rates of the stellar models were taken into account in computing the distributions. 

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Parameter values of the computed grid of 1170 MESA evolutionary tracks, consisting of some 900 000 models.
Ballot et al. (2012) showed that the traditional approximation continues to perform adequately if the spin parameter  s  ≤ 2 (see Ballot et al. 2012, Fig. 2), with (3)where f_{rot} (= Ω / 2π) and f_{co} are the stellar rotation frequency and the pulsation frequency in the corotating frame, respectively. Thanks to the assumptions made in the traditional approximation, the computational requirements for the effects of rotation are dramatically reduced. In this work, we used the traditional approximation module from the onedimensional pulsation code GYRE v4.3 (Townsend & Teitler 2013) and followed the approach described by Ballot et al. (2012) and Bouabid et al. (2013). These authors showed that within the traditional approximation, an asymptotic pulsation period series can be rewritten for a rotating star as (4)where P_{nlm,co} is the pulsation period of radial order n, spherical degree l, and azimuthal order m in the corotating frame. In this paper, we adopt the convention that m> 0 corresponds with prograde modes and m< 0 with retrograde modes, respectively. In this equation, λ_{l,m,s} is the eigenvalue of the Laplace tidal equation depending on l, m, and the spin parameter s, while the phase term α_{g} depends on the internal stellar properties at the boundaries of the pulsation mode cavity and can be taken to be 0.5 for stars with a convective core and a convective envelope, such as γ Dor stars. In the limit of a nonrotating star, where s = 0, this expression reduces to (5)in agreement with Eq. (1) and as derived by Tassoul (1980). For each of the models in our grid, we computed the l = 1 and l = 2 mode frequencies for radial orders ranging from 5 to 120.
Fig. 2 BruntVäisälä frequency N (top) and the rotational kernel K_{nl} (bottom) for the lowest and highestorder mode of the stellar model discussed in Sect. 4.1. The inset shows a zoom of K_{nl}. Both functions correlate with the sensitivity of the gravitymode pulsations to the different regions inside the star. 

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3. Method
As we have discussed in the previous section, the influence of rotation on the pulsation frequencies depends on the values of l and m, while the asymptotic spacing ΔΠ_{l} is dependent on the value of l (Eq. (1)). It is therefore necessary to have a pulsation mode identification if we wish to constrain the rotation profile of the observed star properly.
To derive a reliable estimate of the rotation rate of a γ Dor star with one or more observed period spacing patterns, we considered all the possible combinations of l and m values for the mode identification of the GYRE pulsation frequencies computed for the MESA models in our grid. For each combination of l and m, we computed the asymptotic spacing value ΔΠ_{l}, as expressed in Eq. (1) and subsequently corrected it in the framework of the traditional approximation according to Eq. (5). This is illustrated graphically in Fig. 3. Because the application of a rotational frequency shift does not introduce dips into the period spacing patterns, we did not need to take them into account at this point. A uniform period spacing series is sufficient for our needs.
The pulsation frequencies in this series were then rotationally shifted using the traditional approximation, as described by Eq. 4 and assuming the star is rigidly rotating. The values of the pulsation periods in the inertial reference frame are then obtained by (6)This introduced a slope into the model spacing series, as shown in Fig. 3. The resulting pattern was subsequently fitted to the observed period spacing series using χ^{2}minimisation, optimising for the variables ΔΠ_{l} and f_{rot}. Finally, we selected the best solution for all studied l and m values, taking into account the theoretical expectations for the asymptotic spacing ΔΠ_{l}, as shown in Fig. 1 and derived from our model grid in Sect. 2. From this fit, we then obtained estimates for the rotation rate f_{rot} and the asymptotic spacing ΔΠ_{l}, as well as a mode identification.
Fig. 3 Illustration of our method to derive the rotation rate f_{rot} and asymptotic spacing ΔΠ_{l} from an observed period spacing pattern (black dots). An equidistant spacing series (grey squares) is defined, rotationally shifted (white squares), and fitted to the observed pattern using χ^{2}minimisation, optimising for the variables l, m, ΔΠ_{l} , and f_{rot}. 

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4. Applications
4.1. Synthetic data
To illustrate our method, we first analyse a simulated period spacing pattern. The simulated data were computed using the MESA and GYRE codes with the input values provided in Table 2, further taking (l, m) = (1, 1). For the computation of the evolution track itself the influence of rotation was not taken into account. The rotation was only included in the GYRE computations using the traditional approximation module. The computed pattern is shown in Fig. 4 and the values of the pulsation periods are listed in Table A.1.
The results of our analysis are shown in Figs. 4 to 6. In Fig. 4 we fitted the simulated data nicely when we excluded the dips in the pattern from the analysis and assumed (l, m) = (1, 1). However, similarly good results were obtained when we treated the pulsations as (2, 1) modes or (2, 2) modes during our analysis, as illustrated in Fig. 5. In other words, we cannot obtain a clear mode identification based solely on the obtained χ^{2}values. This problem is solved when we recall the expected values of the asymptotic spacing ΔΠ_{l} for different values of l, which we previously showed in Fig. 1. The values for ΔΠ_{l} we found are clearly far too high for l = 2. We can therefore safely identify the simulated data as (1, 1) modes, and obtain f_{rot} = 0.664 ± 0.013 d^{1} and ΔΠ_{l = 1} = 3020 ± 190 s.
It is important to exclude any significant dips in the period spacing structure from this analysis. In our technique, we do not take the influence of chemical gradients in the stellar interior into account. As shown by Miglio et al. (2008), these gradients result in nonuniform deviations from the asymptotic spacing series. Because we can only observe a small part of a period spacing pattern, any nonuniform variations in the pattern will change the measured mean spacing and/or the measured slope of the pattern. This, in turn, will influence our analysis. By ignoring significant nonuniform variations in the period spacing structure, we limit their influence on the analysis, so that we obtain results that are correct within or on the order of 1σ. For our simulated data set this is illustrated with the 2dimensional χ^{2}distribution shown in Fig. 6. While we ignored the large dip in the period spacing structure (as seen in Fig. 4), the remaining nonuniform variations still affected the analysis. As a result, there is a small offset between the input values of the data set and the 1σconfidence interval for the obtained solution.
Parameter values of the simulated period spacing pattern.
Fig. 4 Top: the input period spacing pattern (black dots and grey triangles) with the bestfitting pattern (white squares) as obtained from the χ^{2}minimisation in Fig. 6 assuming (l, m) = (1, 1). The black part of the input patterns was used to determine f_{rot} and ΔΠ_{l}, while the grey section was excluded. Bottom: the residuals of the fit. 

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Fig. 5 Best χ^{2}values for the synthetic data shown in Fig. 2 for each (l,m) combination, as a function of the asymptotic spacing ΔΠ_{l}. The black and light grey lines correspond to l = 1 and l = 2, respectively, while the modes with m = 0 are indicated with dashed lines, m = 1 with full lines, and m = 2 with the dashdotted line. 

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Fig. 6 for the simulated period spacing series assuming l = 1 as a function of the asymptotic period spacing ΔΠ_{l} and the rotation rate f_{rot}. The white dot indicates the input values, while the white cross and the red boundary indicate the solution and its 1σuncertainty margins, respectively. 

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4.2. Slow and fast rotator
In our sample we have one slowly rotating star, KIC 9751996, for which we detected period spacing series with rotational splitting, delivering immediately the mvalues of the modes. To additionally validate our proposed method, we have applied it to KIC 9751996. In a first step, we only analysed the prograde period spacing pattern to test the reliability of our method. Assuming (l, m) = (1, 1), this led us to find f_{rot} = 0.07 ± 0.02 d^{1}, which is shown in the top panel of Fig. 7. However, assuming l = 1,m = 0 for the treated series, we found f_{rot} = 0.19 ± 0.03 d^{1} for a similar χ^{2} value. The challenge in this case is that the shift and slope in the period spacing pattern are almost negligibly small compared to the nonuniform period spacing variations as a result of a chemical gradient. This was resolved when we fit the prograde, zonal, and retrograde dipole modes simultaneously, as shown in Fig. 8. Not only did this allow us to formally identify the (l,m,n) values of the modes, it also resulted in a much higher precision for the rotation rate f_{rot} = 0.0696 ± 0.0008 d^{1} and the spacing ΔΠ_{l = 1} = 3086 ± 6 s (see Fig. 7). Interestingly, we have another independent indication for this derived rotation rate. In the series of the prograde and retrograde modes, we have a pulsation period that does not seem to follow the pattern at values of 0.8 days and 0.9 days, respectively. These modes are likely trapped, which has influenced their pulsation period. When the periods of these retrograde and prograde modes are converted into their values in the corotating reference frame using the derived rotation rate, we find that the pulsation periods are almost equal, which is consistent with the interpretation of trapped pulsation modes.
Fig. 7 for the observed period spacing series of KIC 9751996, assuming l = 1, as a function of the asymptotic period spacing ΔΠ_{l} and the rotation rate f_{rot}. The white crosses indicate the bestfit solutions. Top: the χ^{2}distribution that we find by only analysing the detected prograde series. Bottom: the χ^{2}distribution obtained by fitting the prograde, zonal, and retrograde spacing series simultaneously. 

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Fig. 8 Observed period spacing patterns (black dots and grey triangles) for the retrograde (top), zonal (middle), and prograde (bottom) modes of KIC 9751996. The black parts of the input patterns were used to determine f_{rot} and ΔΠ_{l}, while the grey sections were excluded. The white squares indicate the modes of the optimal model in the grid when all three series are fitted simultaneously. 

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Next we also analysed the period spacing patterns of KIC 12066947, a fastrotating star for which both a prograde and a retrograde period spacing series were detected. While we were able to fit the pattern of prograde modes to derive a rotation rate f_{rot}, the observed retrograde series presented us with a challenge. We found these to correspond with Rossby modes rather than “classical” gravity or gravitoinertial modes. Rossby modes can only occur in rotating stars and originate from the interaction between the stellar rotation and toroidal modes (e.g. Papaloizou & Pringle 1978; Townsend 2003b). Our identification of the retrograde modes as Rossby modes is illustrated in the top panel of Fig. 9, where we show the observed period spacing patterns for the detected prograde and retrograde series, as well as the spacings predicted by the most suitable model in the grid, by assuming the values for f_{rot} and ΔΠ_{l} obtained by modelling the prograde series. To calculate the period series for the Rossby modes, Π_{0} was derived from ΔΠ_{l} using Eq. (1), and this value was subsequently filled into Eq. (4). The appropriate eigenvalues λ were computed using the asymptotic approximation derived by Townsend (2003b), that is, Eq. (37) in that study. This equation is valid when λ ≠ m^{2}, as is the case here. The expected values of λ for Rossby modes are three to four orders of magnitude smaller than for retrograde gravitoinertial modes, which allowed us to identify the observed pulsations. However, as Townsend (2003b) pointed out, the asymptotic approximation does not converge well to the numerical solution for these modes. The possibility of computing Rossby modes has not yet been included in the publicly available version of GYRE. As a consequence, we were unable to perform a reliable quantitative analysis of the retrograde series at this point and focused on the analysis of the prograde series to derive f_{rot}. However, several qualitative arguments can be made in favour of Rossby modes as a correct identification. From the upward slope and the small average period spacing of the observed pattern, we derive that these modes are retrograde in the corotating frame with  f_{co}  <f_{rot}, which is completely in line with theoretical expectations. Furthermore, the observed spin parameter values are higher for the retrograde than for the prograde modes: the values of the dominant modes of the two series are 15.8 ± 0.4 and 7.7 ± 0.1, respectively. This indicates that in the corotating frame the pulsation frequencies of the retrograde modes are smaller than those of the prograde modes, which in turn can be explained by the low values of the eigenvalues λ. Finally, Townsend (2003b) also noted that compared to the retrograde gravitoinertial modes, Rossby modes are less equatorially confined as the stellar rotation rate increases. As a result, the latter can be expected to be less influenced by the geometrical cancellation effects, although the effect is still present. For KIC 12066947, we find that the dominant prograde and Rossby modes are confined within equatorial bands with a width of 77.2° and 53.5°, respectively.
For a fastrotating star such as KIC 12066947, we also have to take into acccount rotational deformation. The centrifugal force leads to a lower effective gravity at the equator than at the pole. This influences the BruntVäisälä frequency, which affects the pulsations. For KIC 12066947, we were able to roughly estimate the deformation of the star, using Eq. A.6 from Maeder & Meynet (2000). In this analysis we evaluated the observed spectroscopic parameter values and asymptotic spacing ΔΠ_{l} using the models in our MESA grid and took the bestmatching model (M = 1.5 M_{⊙}, Z = 0.014, X_{i} = 0.69, X_{c} = 0.452, α_{ov} = 0.01) as a guess for the stellar structure. We found that f_{rot}/f_{rot,crit} = 0.78 and R_{pole}/R_{eq} = 0.88. A twodimensional treatment of the rotation is clearly needed to quantify the effect of the rotation on the modes, which will allow us to improve our constraints on f_{rot} and ΔΠ_{l}.
Fig. 9 Top: observed period spacing patterns (black dots and grey triangles) for the prograde (left) and retrograde (right) modes of KIC 12066947. The black part of the pattern was used to determine f_{rot} and ΔΠ_{l}, while the grey section was excluded. The white squares indicate the model fit, assuming these are gravitoinertial modes and using the f_{rot} and ΔΠ_{l} values obtained from the analysis of the marked prograde series. The white diamonds indicate the model computed for Rossby waves using the same f_{rot} and ΔΠ_{l} values, assuming m = −1 and k = −2 in the kbased indexing scheme by Lee & Saio (1997). Bottom: the residuals of the fit to the prograde period spacing series. 

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4.3. Sample study
Subsequently, we also applied our method to the other stars in our sample. This led to the mode identification and determination of the rotation rate f_{rot} for the period spacing series of 40 stars in our sample. Six additional sample stars only exhibit retrograde modes and fast rotation, and cannot be quantitatively analysed with our current methodology. The difference of the best χ^{2}value for different (l, m) combinations is too small for the remaining stars, therefore no unique solution could be determined.
For the 40 stars that were successfully analysed, the results are listed in Table B.1. The vast majority of these stars were found to exhibit prograde dipole modes. For fourteen targets in the sample we detected multiple series. In principle, these are prime targets to look for differential rotation. However, for ten of them the second detected period spacing pattern corresponds to Rossby modes, for which we still need to develop a suitable computational tool to arrive at appropriate numerical values, as discussed in Sect. 4.2. For the remainder of this study, we assign the values of f_{rot} and ΔΠ_{l} that we obtained from the prograde series to the retrograde series of the same star. Because formal mode identification of these retrograde pulsations is currently not possible, they are marked as “R” in Table B.1. For two other stars we have both a zonal and prograde dipole series, while for a third we have prograde dipole and quadrupole modes. Finally, KIC 9751996, the slowly rotating star we discussed in Sect. 4.2 is the only target for which we have a series of rotationally split multiplets. For each of these last four stars, we were able to use the multiple detected period spacing patterns to refine the obtained f_{rot} and ΔΠ_{l}.
Fig. 10 Part of the frequency spectrum of KIC 7365537. The light grey area shows the location of the pulsation modes that form the detected period spacing pattern of this star. The dashed line shows the value of the derived rotation frequency f_{rot}, while the dotted line indicates the solitary highamplitude mode we found. 

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There are several stars for which a single highamplitude mode was detected that does not belong to a period spacing series and that differs from the rotation frequency. In Fig. 10 we show the frequency spectrum of KIC 7365537 as an example. For these modes the identification in Table B.1 is marked “S”. Because our method cannot be applied to these single modes, we again used the values of f_{rot} and ΔΠ_{l} that were derived from the prograde series in the same star in the subsequent analysis. The selection of series of modes in some stars versus the presence of single modes in others also provides much information about their respective stellar structure. It has been suggested by Dziembowski & Pamyatnykh (1991) that such single highamplitude modes might be caused by mode trapping effects. However, detailed theoretical modelling of each of these individual stars is required to confirm this.
Fig. 11 Dominant pulsation frequency f_{dom,corot} in the corotating frame as a function of the rotation frequency f_{rot} for the identified gmode pulsations of 40 stars in the sample. The thick vertical lines indicate the full extent of the detected spacing series. The dashed red line shows where the pulsations pass from the superinertial regime (above the line) into the subinertial regime (below the line). 

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Fig. 12 Absolute value of the spin parameter s for the detected period spacing series of the stars in our sample as a function of the rotation frequency f_{rot}. The dashed red line shows where the pulsations pass from the superinertial regime (below the line) into the subinertial regime (above the line). The symbols are the same as in Fig. 11. 

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Figure 11 illustrates the frequency f_{dom,corot} of the dominant mode of each detected series in the corotating frame with respect to the computed rotation frequency. An alternative version of Fig. 11 in the inertial reference frame is included in Fig. C.1. For the majority of the stars, we obtain similar values of f_{dom,corot} between 0.15 and 0.75 d^{1}. This can be linked to the convective flux blocking excitation mechanism. Dupret et al. (2005) and Bouabid et al. (2013) remarked that for the mode excitation mechanism to be efficient, the thermal timescale τ_{th} at the bottom of the convective envelope has to be similar to the pulsation periods in the corotating frame. From this information and the content of Fig. 11, we can also derive that the detected retrograde spacing series and single modes most likely have azimuthal order m = −1 because only  m  = 1 led to similar f_{dom,corot} values for the series of different stars. While these results are consistent, we note that the observed pulsation periods in the corotating frame are typically longer than the theoretical values computed by Bouabid et al. (2013). For the retrograde Rossby modes this can be linked to the correspondingly low eigenvalues λ of the Laplace tidal equation. However, the same discrepancy is observed for the prograde modes as well, although to a lesser degree. This discrepancy may point towards limitations of the current theory of mode excitation in γ Dor stars for moderate to fast rotators or may be caused by the limited applicability of the traditional approximation for these rotation rates. Further research on this topic is required.
Results of the linear regression analysis.
In Fig. 12 we show the spin parameter s, as defined in Eq. (3) and listed in the last column of Table B.1, as a function of the measured rotation frequency f_{rot}. The spin parameter s is a measure of the effect of rotation on the pulsation frequency and is inversely proportional to the pulsation frequency f_{co} in the corotating frame. Once again, the Rossby modes (shown as dark blue dots) have low values for the eigenvalue λ. In addition, although both prograde sectoral modes and Rossby modes are less easily confined in a band around the equator, the effect is still significant for these high values of s (Townsend 2003b). This implies that many of the stars in our sample are seen at moderate to high inclination angles. We furthermore note that our observed values of s are on average much higher than the values quoted in theoretical papers in the literature (e.g. Townsend 2003a; Ballot et al. 2012).
Figure 13 shows the three slowest rotating stars in our sample in greater detail, one of which is KIC 9751996, which has been discussed in Sect. 4.2. These three stars have comparable properties. They are slow rotators, placing them in the superinertial regime, and they are hybrid γ Dor/δ Sct pulsators. Each of them exhibits variability in the frequency range between 5 d^{1} and 8 d^{1}. These striking similarities suggest that there is a link between the low stellar rotation rates and their hybrid properties, marking them as interesting targets for followup research.
Fig. 13 Section of the Fourier spectra of the three slowest rotating stars in our sample. These are our only stars in the superinertial regime, and all three are hybrid γ Dor/δ Sct pulsators with variabilities of between 5 d^{1} and 8 d^{1}. 

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Fig. 14 Correlation between the spectroscopic vsini values and the values of the rotation rate f_{rot}. The black line indicates the corresponding linear fit, for which the coefficients are listed in Table 3. The symbols are the same as in Fig. 11. For all of the stars a series of prograde dipole modes was detected. If another series was detected as well, the symbol of the corresponding mode identification was used. 

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4.3.1. Statistical analysis
Finally, we also searched for correlations between the parameter values of our stars, similar to the multivariate statistical analysis that was carried out by Van Reeth et al. (2015). In this work, we again used the spectroscopic fundamental parameter values obtained by Van Reeth et al. (2015) in our analysis. We also included the detected values of the variables f_{rot}, ΔΠ_{l}, Rsin i = vsin i/f_{rot} and the dominant pulsation frequency f_{dom} (in the corotating and the inertial reference frame). For consistency, we focused on the parameter values derived from the identified prograde dipole mode series of 40 stars in the sample. The results of our multivariate statistical study are summarised in Table 3.
Most of the correlations presented previously by Van Reeth et al. (2015) were indicative of the strong relation between the observed gravitymode pulsations and the stellar rotation. In retrospect, these can now be linked to the identification of most pulsations as prograde dipole gravity, gravitoinertial, or retrograde Rossby modes with  m  = 1. In particular, those previous results are echoed in our current work by the detected correlations between f_{rot} and vsini, and f_{rot} and f_{dom,inert}. The strong correlation between f_{rot} and vsini is illustrated in Fig. 14. The previously detected correlations between vsini and the mean period spacing ⟨ ΔP ⟩, the mean pulsation period ⟨ P ⟩ and the mean slope of the observed series discussed in Van Reeth et al. (2015) are now also reflected in similar correlations with f_{rot}. We do find a level of scatter in the relationship between these parameters and the rotation rate f_{rot}, originating from the broad variety of radial orders of the detected modes, the limited lengths of some of the observed series, and from nonuniform variations in the period spacing patterns covered by our sample. Moreover, we assumed a constant rotation rate throughout the stars to deduce f_{rot}, which is simplistic compared to predictions based on numerical simulations (Rogers 2015). Allowing for a variety of nonuniform interior rotation profiles will likely complicate the correlations.
Van Reeth et al. (2015) also found a smaller contribution of T_{eff} to the multivariate correlation with f_{dom,inert} and vsini. While this contribution drops when we replace vsini with f_{rot}, there is a weak correlation between T_{eff} and Rsini. As a star ages, its temperature T_{eff} drops and its radius increases. A similarly weak correlation was found between f_{rot} and log g, indicating that as the star evolves and its radius increases, the surface gravity and the rotation rate both decrease. The correlation between Rsini and log g was not significant, probably because of the relatively large uncertainties.
In contrast, we did not find correlations between the asymptotic spacing ΔΠ_{l} and any of the other parameters. The uncertainty margins on the value of ΔΠ_{l} are likely too large for a proper correlation to be unravelled. Multivariate correlations were not detected either.
5. Discussion and conclusions
We have presented a method to derive the nearcore interior rotation rate f_{rot} from an observed period spacing pattern and to perform mode identification for the pulsations in the series. In a first step, we considered all combinations of l and m values for mode identification. For each pair of landm, we considered the asymptotic spacing ΔΠ_{l} and computed the corresponding equidistant model period spacing pattern as described by Tassoul (1980). Using the traditional approximation, the frequencies of the model pattern were then shifted for an assumed rotation rate f_{rot} and the chosen l and m. The bestfit values of ΔΠ_{l}, f_{rot}, l, and m were then determined by fitting the model pattern to the observed period spacing series using leastsquares optimisation and taking into account that different values of ΔΠ_{l} are expected for different values of l.
In most cases this method was reasonably successful. For slow rotators it may be difficult to find the correct value for the azimuthal order m, although this problem is solved when multiple series with different l and m values are considered. By fitting these series simultaneously, not only did we obtain the mode identification, but the values for ΔΠ_{l} and f_{rot} were also much more precise than when we did not detect multiplets. When we considered a moderate to fast rotator, the retrograde modes were found to be Rossby modes, which arise from the interaction between the stellar rotation and toroidal modes. We used the asymptotic approximation derived by Townsend (2003b) to compute their eigenvalues λ of the Laplace tidal equation. A complete numerical treatment of these modes is required to exploit them quantitatively. A complete and detailed analysis of such stars with multiple gravitymode period spacings will allow us to study possible differential rotation in γ Dor stars, ultimately leading to proper observational constraints on rotational chemical mixing and angular momentum transport mechanisms.
From the ensemble modelling of the gravitymode period spacings of the stars in our sample, we found that there is a wide range in the stellar rotation rates. Interestingly, only three out of forty targets were found to be in the superinertial regime. These three stars, KIC 8645874, KIC 9751996, and KIC 11754232, are hybrid γ Dor/δ Sct stars that exhibit variability in the frequency range from 5 d^{1} to 8 d^{1}. This indicates that these low stellar rotation rates are most likely linked to their hybrid character, making them prime targets for further asteroseismological analysis. The other stars were found to be in the subinertial regime. Their pulsation frequencies in the corotating frame are typically confined in the narrow range between 0.15 and 0.75 d^{1}. This is in agreement with the theoretical expectation that γ Dor pulsation frequencies in the corotating frame are approximately on the thermal timescale τ_{th} at the bottom of the convective envelope (Bouabid et al. 2013). However, this frequency range does not agree with the predicted values by Bouabid et al. (2013). With the exception of the three stars in the superinertial regime, we found that on average the observed modes have longer pulsation periods in the corotating frame than theory predicts. This is also reflected in the high spin parameter values we derived for many of the stars. The high spin parameters detected for the retrograde Rossby modes are linked to the low eigenvalues λ of these modes, as already found on theoretical grounds by Townsend (2003b).
The global results for the mode identification are consistent with existing spectroscopic studies. The majority of the modes were found to be prograde dipole modes. This is in line with the results obtained by Townsend (2003a) for heatdriven gravity modes in slowly pulsating B stars. In addition, we found single highamplitude modes, as opposed to a series, to be present in several stars. They are consistent with retrograde Rossby modes with m = −1. They are most likely heavily influenced by mode trapping, and as a result contain valuable information about the internal structure of these stars.
We conducted a linear regression analysis on the combined spectroscopic and photometric parameter values for the sample. The strong correlation between vsini and f_{rot} independently confirmed the reliability of the obtained rotation rates. We also detected weak correlations between Rsini = vsini/f_{rot} and T_{eff} and between log g and f_{rot}. As a star with a convective core evolves on the main sequence, its radius increases, and its temperature and rotation rate decrease.
Despite the limitations of the traditional approximation, the results we obtained in this work are consistent and offer the first estimates of the interior rotation frequencies for a large sample of γDor stars. The high observed spin parameter values indicate that the pulsations are constrained in a waveguide around the equator (Townsend 2003a,b). This in turn implies that the vast majority of the stars should be seen at moderate to high inclination angles, which is also what we can indirectly derive from the relation between the observed vsini and f_{rot} in Fig. 14. From the grid of theoretical models in Sect. 2, we find radii between 1.3 R_{⊙} and 3 R_{⊙}. For many stars in our sample, this results in inclination angle estimates of or above 50°. Two of the stars for which lower inclination angle estimates were found, KIC 4846809 and KIC 9595743, are also the stars for which we detected zonal dipole modes. This is consistent with expectations for the geometrical cancellation effects of the pulsations.
These ensemble analyses now form an ideal starting point for detailed asteroseismological modelling of individual targets in the sample. This, in turn, will allow us to place constraints on the shape and extent of the convective core overshooting and the diffusive mixing processes in the radiative nearcore regions, and by extension on the evolution of the convective core itself as it was recently achieved for a hybrid δSct – γDor binary (Schmid & Aerts 2016) and also for a slowly (Moravveji et al. 2015) and a moderately (Moravveji et al. 2016) rotating gravitymode pulsator of ~3.3 M_{⊙}.
Acknowledgments
The research leading to these results was based on funding from the Fund for Scientific Research of Flanders (FWO), Belgium, under grant agreement G.0B69.13, and on funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement N 670519: MAMSIE). T.V.R. thanks Ehsan Moravveji for the extensive discussions on the use of the MESA and GYRE codes and Santiago A. Triana for the enlightening conversations about the influence of rotation on stellar pulsations. T.V.R. also thanks François Lignières and the other participants of the Toulouse 2016 SpaceInn workshop on Stellar Rotation for the useful discussions. We furthermore thank the anonymous referee for helpful remarks that helped us to improve the interpretations and presentation of the research. We are grateful to Bill Paxton and Richard Townsend for their valuable work on the stellar evolution code MESA and stellar pulsation code GYRE. We gratefully acknowledge the Thüringer Landessternwarte in Tautenburg, Germany, for the computation time on their computer cluster. Funding for the Kepler mission is provided by NASA’s Science Mission Directorate. We thank the whole team for the development and operations of the mission. This research made use of the SIMBAD database, operated at CDS, Strasbourg, France, and the SAO/NASA Astrophysics Data System. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.
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Appendix A: Simulated period spacing pattern
Appendix B: Stellar rotation rates and mode identification
Rotation rates f_{rot} and asymptotic period spacings ΔΠ_{l} computed from the observed period spacing patterns, as well as the mode identification and the dominant pulsation frequency for each series.
Appendix C: Sample analysis
Fig. C.1 Dominant pulsation frequency f_{dom,inert} in the inertial frame as a function of the rotation frequency f_{rot} for the identified gmode pulsations of 40 stars in the sample. The thick vertical lines indicate the full extent of the detected spacing series. The full black line indicates where f_{inert} is equal to f_{rot}. 

Open with DEXTER 
All Tables
Parameter values of the computed grid of 1170 MESA evolutionary tracks, consisting of some 900 000 models.
Rotation rates f_{rot} and asymptotic period spacings ΔΠ_{l} computed from the observed period spacing patterns, as well as the mode identification and the dominant pulsation frequency for each series.
All Figures
Fig. 1 Distributions of the asymptotic period spacing values ΔΠ_{l} for spherical degree l = 1 and 2 computed for the MESA evolution tracks with the input parameters provided in Table 1. The ages and evolution rates of the stellar models were taken into account in computing the distributions. 

Open with DEXTER  
In the text 
Fig. 2 BruntVäisälä frequency N (top) and the rotational kernel K_{nl} (bottom) for the lowest and highestorder mode of the stellar model discussed in Sect. 4.1. The inset shows a zoom of K_{nl}. Both functions correlate with the sensitivity of the gravitymode pulsations to the different regions inside the star. 

Open with DEXTER  
In the text 
Fig. 3 Illustration of our method to derive the rotation rate f_{rot} and asymptotic spacing ΔΠ_{l} from an observed period spacing pattern (black dots). An equidistant spacing series (grey squares) is defined, rotationally shifted (white squares), and fitted to the observed pattern using χ^{2}minimisation, optimising for the variables l, m, ΔΠ_{l} , and f_{rot}. 

Open with DEXTER  
In the text 
Fig. 4 Top: the input period spacing pattern (black dots and grey triangles) with the bestfitting pattern (white squares) as obtained from the χ^{2}minimisation in Fig. 6 assuming (l, m) = (1, 1). The black part of the input patterns was used to determine f_{rot} and ΔΠ_{l}, while the grey section was excluded. Bottom: the residuals of the fit. 

Open with DEXTER  
In the text 
Fig. 5 Best χ^{2}values for the synthetic data shown in Fig. 2 for each (l,m) combination, as a function of the asymptotic spacing ΔΠ_{l}. The black and light grey lines correspond to l = 1 and l = 2, respectively, while the modes with m = 0 are indicated with dashed lines, m = 1 with full lines, and m = 2 with the dashdotted line. 

Open with DEXTER  
In the text 
Fig. 6 for the simulated period spacing series assuming l = 1 as a function of the asymptotic period spacing ΔΠ_{l} and the rotation rate f_{rot}. The white dot indicates the input values, while the white cross and the red boundary indicate the solution and its 1σuncertainty margins, respectively. 

Open with DEXTER  
In the text 
Fig. 7 for the observed period spacing series of KIC 9751996, assuming l = 1, as a function of the asymptotic period spacing ΔΠ_{l} and the rotation rate f_{rot}. The white crosses indicate the bestfit solutions. Top: the χ^{2}distribution that we find by only analysing the detected prograde series. Bottom: the χ^{2}distribution obtained by fitting the prograde, zonal, and retrograde spacing series simultaneously. 

Open with DEXTER  
In the text 
Fig. 8 Observed period spacing patterns (black dots and grey triangles) for the retrograde (top), zonal (middle), and prograde (bottom) modes of KIC 9751996. The black parts of the input patterns were used to determine f_{rot} and ΔΠ_{l}, while the grey sections were excluded. The white squares indicate the modes of the optimal model in the grid when all three series are fitted simultaneously. 

Open with DEXTER  
In the text 
Fig. 9 Top: observed period spacing patterns (black dots and grey triangles) for the prograde (left) and retrograde (right) modes of KIC 12066947. The black part of the pattern was used to determine f_{rot} and ΔΠ_{l}, while the grey section was excluded. The white squares indicate the model fit, assuming these are gravitoinertial modes and using the f_{rot} and ΔΠ_{l} values obtained from the analysis of the marked prograde series. The white diamonds indicate the model computed for Rossby waves using the same f_{rot} and ΔΠ_{l} values, assuming m = −1 and k = −2 in the kbased indexing scheme by Lee & Saio (1997). Bottom: the residuals of the fit to the prograde period spacing series. 

Open with DEXTER  
In the text 
Fig. 10 Part of the frequency spectrum of KIC 7365537. The light grey area shows the location of the pulsation modes that form the detected period spacing pattern of this star. The dashed line shows the value of the derived rotation frequency f_{rot}, while the dotted line indicates the solitary highamplitude mode we found. 

Open with DEXTER  
In the text 
Fig. 11 Dominant pulsation frequency f_{dom,corot} in the corotating frame as a function of the rotation frequency f_{rot} for the identified gmode pulsations of 40 stars in the sample. The thick vertical lines indicate the full extent of the detected spacing series. The dashed red line shows where the pulsations pass from the superinertial regime (above the line) into the subinertial regime (below the line). 

Open with DEXTER  
In the text 
Fig. 12 Absolute value of the spin parameter s for the detected period spacing series of the stars in our sample as a function of the rotation frequency f_{rot}. The dashed red line shows where the pulsations pass from the superinertial regime (below the line) into the subinertial regime (above the line). The symbols are the same as in Fig. 11. 

Open with DEXTER  
In the text 
Fig. 13 Section of the Fourier spectra of the three slowest rotating stars in our sample. These are our only stars in the superinertial regime, and all three are hybrid γ Dor/δ Sct pulsators with variabilities of between 5 d^{1} and 8 d^{1}. 

Open with DEXTER  
In the text 
Fig. 14 Correlation between the spectroscopic vsini values and the values of the rotation rate f_{rot}. The black line indicates the corresponding linear fit, for which the coefficients are listed in Table 3. The symbols are the same as in Fig. 11. For all of the stars a series of prograde dipole modes was detected. If another series was detected as well, the symbol of the corresponding mode identification was used. 

Open with DEXTER  
In the text 
Fig. C.1 Dominant pulsation frequency f_{dom,inert} in the inertial frame as a function of the rotation frequency f_{rot} for the identified gmode pulsations of 40 stars in the sample. The thick vertical lines indicate the full extent of the detected spacing series. The full black line indicates where f_{inert} is equal to f_{rot}. 

Open with DEXTER  
In the text 
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