Issue 
A&A
Volume 579, July 2015



Article Number  A83  
Number of page(s)  76  
Section  Catalogs and data  
DOI  https://doi.org/10.1051/00046361/201525895  
Published online  02 July 2015 
Bayesian peak bagging analysis of 19 lowmass lowluminosity red giants observed with Kepler
^{1}
Instituut voor Sterrenkunde, KU Leuven, Celestijnenlaan 200D, 3001
Leuven, Belgium
^{2}
Laboratoire AIM, CEA/DSM – CNRS – Univ. Paris Diderot –
IRFU/SAp, Centre de
Saclay, 91191
GifsurYvette Cedex,
France
email: enrico.corsaro@cea.fr
^{3}
Instituto de Astrofísica de Canarias, 38205, La
Laguna, Tenerife, Spain
^{4}
Universidad de La Laguna, Departamento de
Astrofísica, 38206, La Laguna,
Tenerife, Spain
Received:
13
February
2015
Accepted:
27
March
2015
Context. Nonradial oscillations, observed in thousands of red giants by the space missions CoRoT and Kepler, allow us to greatly improve our understanding of stellar structure and evolution in cool lowmass stars. The currently available Kepler light curves contain an outstanding amount of information, but a detailed analysis of the individual oscillation modes in the observed power spectra, also known as peak bagging, is computationally demanding and challenging to perform on a large number of targets.
Aims. Our intent is to perform for the first time a peak bagging analysis on a sample of 19 lowmass lowluminosity red giants observed by Kepler for more than four years. This allows us to provide highquality asteroseismic measurements that can be exploited for an intensive testing of the physics used in stellar structure models, stellar evolution, and pulsation codes, as well as for refining existing asteroseismic scaling relations in the red giant branch regime.
Methods. For this purpose, powerful and sophisticated analysis tools are needed. We exploit the Bayesian code Diamonds, using an efficient nested sampling Monte Carlo algorithm, to perform both a fast fitting of the individual oscillation modes and a peak detection test based on the Bayesian evidence.
Results. We find good agreement for the parameters estimated in the background fitting phase with those given in the literature. We extract and characterize a total of 1618 oscillation modes, providing the largest set of detailed asteroseismic mode measurements ever published. We report on the evidence of a change in regime observed in the relation between linewidths and effective temperatures of the stars occurring at the bottom of the red giant branch. We show the presence of a linewidth depression or plateau around ν_{max} for all the red giants of the sample. Lastly, we show a good agreement between our measurements of maximum mode amplitudes and existing maximum amplitudes from global analyses provided in the literature, proving that amplitude scaling relations can be used as empirical tools to improve and simplify the future peak bagging analysis on a larger sample of evolved stars.
Key words: stars: oscillations / stars: evolution / methods: statistical / methods: numerical / methods: data analysis / stars: latetype
© ESO, 2015
Since the first detection of nonradial oscillations in cool giant stars, the asteroseismology of field red giants (RGs) has encountered a substantial increase in output, especially thanks to the advent of the spacebased photometric missions CoRoT (e.g., De Ridder et al. 2009; Kallinger et al. 2010b; Mosser et al. 2011b,a) and Kepler (e.g., Borucki et al. 2010; Koch et al. 2010; Bedding et al. 2010; Huber et al. 2010; Kallinger et al. 2010a, 2012). Kepler also allowed the study of RGs in open clusters (e.g., Stello et al. 2011; Miglio et al. 2012; Corsaro et al. 2012), and in eccentric binary systems (Beck et al. 2014).
The discovery of socalled mixed modes (Beck et al. 2011; Mosser et al. 2011a), i.e., modes with pmode as well as gmode characteristics, only observed in stars that have passed the mainsequence phase, has led to a significant improvement in our understanding of the internal structure and evolution of RGs. The characteristic period spacing of mixedmode frequencies provides a direct way to disentangle Hshell and Hecore burning RGs (Bedding et al. 2011; Mosser et al. 2012b) and has already been used to classify about 13,000 targets observed in the Kepler field of view (Stello et al. 2013). Additional studies of the effect of rotation as seen from the splitting of mixed modes show us that the RG cores rotate faster than their convective envelope (Beck et al. 2012; Deheuvels et al. 2012; Mosser et al. 2012a), thus opening the possibility to probe their internal rotation rates with direct observations of the oscillations at their surface. Red giants are also being used as distance and age indicators to study stellar populations and trace the formation and evolution of the Galaxy (see, e.g., Miglio et al. 2009, 2013, 2015).
Nonetheless, several problems and challenges arise in the analysis and physical interpretation of the asteroseismic properties of the RGs. Among the most important topics currently under investigation, we mention the forward modeling and inversion of the mode frequencies aimed at probing the stellar structure, constraining the evolution, and examining the physical mechanisms responsible for the transport of angular momentum inside the star (e.g., Tayar & Pinsonneault 2013; Benomar et al. 2014; Deheuvels et al. 2014, and references therein); the excitation and damping mechanism of the mixed modes (e.g., Grosjean et al. 2014), and the asymptotic behavior of their oscillation frequencies (Jiang & ChristensenDalsgaard 2014); the underlying physics responsible for the damping rates of the p modes in a temperature range cooler than that of GF type mainsequence and subgiant stars (e.g., Chaplin et al. 2009; Baudin et al. 2011; Belkacem et al. 2012; Corsaro et al. 2012); and the analysis of regions of sharpstructure variation inside the convective zone aimed at refining existing stellar models and at retrieving reliable helium abundances (e.g., Miglio et al. 2010; Broomhall et al. 2014; Vrard et al. 2014; Corsaro et al. 2015). Therefore, RGs are among the most interesting and useful types of stars with which to test thoroughly the physics implemented in both stellar structure models and in evolution and pulsation codes, but highprecision asteroseismic measurements of individual oscillation modes are needed to accomplish each one of the steps listed above.
With the present fouryear datasets available from Kepler for many RGs, we have the possibility of obtaining detailed asteroseismic properties such as frequency, amplitude, and lifetime of each individual oscillation mode observed with an unprecedented level of accuracy and precision. The required analysis, usually known as peak bagging (e.g., Appourchaux 2003), is essential to exploiting the full potential of the highquality power spectra of the stars. However, owing to the large number of modes populating the power spectrum of a red giant (~100), the peak bagging usually turns into a computationally demanding analysis (see, e.g., Benomar et al. 2009a; Gruberbauer et al. 2009; Kallinger et al. 2010b; Handberg & Campante 2011; Corsaro & De Ridder 2014). For this purpose we exploit Diamonds (Corsaro & De Ridder 2014, hereafter CD14), a new code well suited for model comparison and inference of highdimensional problems in a Bayesian perspective.
In this paper we show how to adequately extend the method used by CD14 for mainsequence stars to the case of RGs, hence we perform the peak bagging analysis on a sample of lowmass lowluminosity red giant branch (RGB) stars observed by Kepler for more than four years. We thus provide and discuss our results for the background signal, the asteroseismic parameters, the mode damping, and the amplitude of all the stars in our sample, stressing their relevance in the light of the open questions related to the physics of the red giant stars.
1. Observations and data
To select the sample of stars investigated in this work we started from the original sample of RGs observed in long cadence (LC) by Kepler (Jenkins et al. 2010) and studied by Huber et al. (2011) and by Corsaro et al. (2013), consisting of a total of 1111 stars. In this work we focus on lowmass lowluminosity RGB stars (hereafter LRGs), a particular type of RG that represents a small population of stars (about 5% of the entire population of RGs observed by Kepler).
We decided to analyze LRGs, out of the variety of RGs observed, for the following reasons:

The clean oscillation pattern caused by the high values of the characteristic frequency separations provides a more reliable fitting and identification of most of the observed modes.

The large number of modes (both p modes and mixed modes) and radial orders observed, thanks to the high frequency of maximum oscillation power ν_{max} and hence broader power excess compared to more evolved RGs, allow for more stringent frequency inversions and studies of the seismic signatures of helium inside the star.

The clear presence of rotation in the oscillations with different mixture levels between pressure and gravity modes is essential to investigating the physics of angular momentum transport and its evolution in different layers inside the star.

The location in a shortlived phase at the bottom of the RGB makes these stars rare to observe and important in order to refine stellar evolution theory.

The covered range in stellar effective temperatures, lying just below that of the coolest lowmass subgiant and mainsequence stars, fills the existing observational gaps that are crucial for our comprehension of the damping mechanism in the transition between the subgiant and the RGB phase of the stellar evolution.
Figure 1 illustrates the asteroseismic HertzsprungRussel diagram (HRD), ν_{max} − T_{eff}, for the sample of the 19 LRGs. The stars span a temperature range of about 4800−5500 K, and a range in ν_{max} of ~75 μHz starting from ~110 μHz upwards, with amplitudes at maximum power from 30 to ~70 ppm.
Fig. 1
Asteroseismic HRD ν_{max} − T_{eff} for the sample of 19 LRGs investigated. Amplitudes of maximum oscillation power, A_{max}, as measured by Huber et al. (2011) are indicated in color scale. All ν_{max} values are provided by Huber et al. (2011), while temperatures are taken from Pinsonneault et al. (2012). 1σ error bars are indicated for both coordinates. 

Open with DEXTER 
2. Peak bagging analysis
2.1. Background fitting
The first step for the peak bagging analysis of the stars is to estimate the background signal in their PSD. We follow the statistical analysis done on a large sample of stars by Kallinger et al. (2014), who found that two separate granulation components with a characteristic frequency close to the region containing the oscillations, together with a third component related to longterm variations, represent best the background signal of the RGs analyzed in this work. In particular, the superLorentzian (or Harveylike) profiles associated with each background component have an exponent set to four, again according to the findings by Kallinger et al. (2014). Thus, the background model that we adopt can be expressed as (1)where we assume W to be a flat noise level since we only study RGs with high ν_{max}, and with the response function that considers the sampling rate of the observations for LC Kepler data, (2)with ν_{Nyq} = 283.212 μHz the Nyquist frequency. The superLorentzian components are given by (3)with a_{i} the amplitude in ppm, b_{i} the characteristic frequency in μHz, and the normalization constant for a superLorentzian profile with exponent set to four (see, e.g., Karoff et al. 2013; Kallinger et al. 2014). The power excess containing the oscillations is as usual described as (4)and is only considered when fitting the background model to the overall PSD of the star.
The results from the fit done by means of Diamonds for all the stars in our sample are presented in Appendix A, in which both the parameter values (Tables A.1 and A.2) and the plots with the background fit are given (Fig. A.1). To illustrate the results obtained with the method presented in this paper, we shall from now on refer to the star KIC 12008916, randomly chosen from our sample. The resulting background fit for KIC 12008916 is shown in Fig. 2.
We adopted uniform priors for all the free parameters of the background model by starting from the results obtained by Kallinger et al. (2014). Uniform priors ensure the fastest computation and are easy to set up (see CD14). The configuring parameters of Diamonds used for the computations of the background fits are given in Appendix A. Our estimated parameters describing the granulation signal of the stars in this sample agree on average within 4.6% for the amplitudes (a_{gran,1}, a_{gran,2}) and within 5.1% for the characteristic frequencies (b_{gran,1}, b_{gran,2}) with those measured by Kallinger et al. (2014), who used Kepler light curves about 360 days shorter than ours (up to Q13).
Fig. 2
Background fit of the star KIC 12008916, as derived by Diamonds. The original PSD is shown in gray, while a smoothed version with boxcar width set to Δν/ 5, with Δν taken from Mosser et al. (2012c; see also Table 1), is shown as a black line to guide the eye. The red thick line represents the background model without the Gaussian envelope and computed with the values listed in Table A.1. The green dotted line accounts for the additional Gaussian component using the values listed in Table A.2. The individual components of the background model as given by Eq. (1) are shown by blue dotdashed lines. 

Open with DEXTER 
2.2. Extraction of the oscillation mode parameters
The subsequent step in analyzing the stellar PSDs is to adopt an adequate fitting model for the oscillation pattern contained in the region of the power excess. In this work we adopt a method similar to that used by CD14 (see Sect. 6.3), who applied it to the case of an Ftype main sequence star. We restrict our frequency range of analysis to the region containing the oscillations, which we identify as ν_{max} ± 3.5σ_{env}, with ν_{max} and σ_{env} listed in Table A.2, empirically chosen to ensure all observable modes to be included. We thus take into account some important features characterizing the oscillation pattern in RGs, as explained in the following.
In the oscillation pattern of all the RGs, one can observe forests of modes between consecutive quadrupole and radial modes (also referred to as ℓ = 2 and ℓ = 0, respectively, ℓ being the angular degree), which are known as dipole (ℓ = 1) mixed modes (Beck et al. 2011; Bedding et al. 2011; Mosser et al. 2011a). Since g modes have the highest mode inertia because they propagate in highdensity regions, their lifetime τ is significantly longer than that of pure pressure modes (see, e.g., ChristensenDalsgaard 2004). As a consequence, even with an observing time T_{obs}> 4 years now made available from Kepler, mixed modes with a gdominated character may still appear unresolved, while others having a more p modelike character can be partially or sometimes even fully resolved.
Fig. 3
Unresolved dipole mixed mode for KIC 12008916. The FWHM of the oscillation peak spans less than three data bins, as indicated by the red segment having a threebin width. The red dotted line represents the half maximum level of the peak. 

Open with DEXTER 
In this work we distinguish between resolved or partially resolved peaks, for which T_{obs} ≳ τ, and those that are unresolved, for which T_{obs} ≪ τ (see also Baudin et al. 2011, who used a similar approach). In the former case, the oscillation peak profile that we adopt is that of a Lorentzian (see, e.g., Kumar et al. 1988; Anderson et al. 1990) and it is given by (5)where A_{0}, Γ_{0}, and ν_{0} are the amplitude in ppm, the linewidth in μHz, and the frequency in μHz, respectively, and represent the three free parameters to be estimated during the fitting process (see Baudin et al. 2005, for more details about the relation between amplitude and linewidth of the peak). According to the Fourier analysis, an oscillation peak that is not resolved has a profile represented as (ChristensenDalsgaard 2004) (6)where H_{0} and ν_{0} are the height in PSD units and the central frequency in μHz of the oscillation peak, respectively, and must be estimated during the fitting process, while δν_{bin} is fixed as the frequency resolution introduced in Sect. 1. Fitting the height of an unresolved mode is preferred since it is an observable and the linewidth of the peak is not a fitting parameter in this case. However, one can easily derive the corresponding amplitude for the unresolved peak as . An example of this type of oscillation peak is shown in Fig. 3 for the star KIC 12008916, where the peak width spans only a few data bins in frequency. In this case, a Lorentzian profile would be an inadequate model because fitting the linewidth is neither meaningful nor needed for an unresolved mode. Moreover, using a Lorentzian profile to fit unresolved modes considerably destabilizes the fitting process because the linewidth tends to assume values smaller than the frequency resolution itself. Whereas this problem could be partially solved by setting a lower limit to the linewidth free parameter by means of an adequate prior, using a Lorentzian profile for the unresolved modes slows down the computation in any case since each Lorentzian profile requires one more free parameter to be fit with respect to the case of a sinc^{2} profile.
According to the description given in this section and still following CD14, we now fix the background parameters corresponding to the white noise, , and the superLorentzian profiles, , to the values listed in Table A.1. Then, the final peak bagging model can be represented as (7)where the model representing the oscillation peaks is now given by a mixture of Lorentzian and sinc^{2} functions (8)with N_{res} and N_{unres} the number of resolved and unresolved peaks to be fit, respectively. In an empirical Bayesian approach such as that used by CD14, the prior distributions on each free parameter can easily be set by visual inspection of the PSD of the stars. Also done for the case of the background fitting, we adopt uniform prior distributions for all the free parameters of the peak bagging model (see CD14). An example of the resulting fit by using the peak bagging model given by Eq. (7) is depicted in Fig. 5 for a chunk of PSD of KIC 12008916, where all the oscillation modes for which a Lorentzian profile was used are marked by a shaded colored band (see the figure caption for details).
2.3. Peak significance test
Testing the significance of an oscillation peak in the PSD of a star is a crucial aspect that has to be considered in order to provide a reliable set of modes that can be used for the modeling of the oscillations, hence to investigate the stellar structure and the evolution of the star. For this purpose, following CD14 (Sect. 6.5) we consider a detection probability for a single peak, p_{B}, defined as (9)where ℰ_{A} and ℰ_{B} are the Bayesian evidences for the models excluding and including, respectively, the oscillation peak to be tested. The probability p_{A} is the complementary probability stating the nondetection of the oscillation peak. For clarity, we shall only refer to p_{B} for the remainder of the paper as it represents a direct measure of the reliability of the oscillation peak.
In the Bayesian mindset, one has to provide all the peaks tested with their corresponding p_{B} value even if their detection probability is low (e.g., below 50%, see also CD14, Sect. 6.5). However, we have performed a test using simulations to calibrate the method and gain a more reliable understanding of which threshold in p_{B} is the most suitable to follow to properly select the oscillation modes. In particular, we have simulated 1000 chunks of PSD of a possible RG in the range 20−40 μHz by means of the simulator provided by De Ridder et al. (2006), with either flat noise only or flat noise and a single oscillation peak. This was done by including a randomly generated flat noise component in each of the 1000 simulations and by adding an oscillation peak corresponding to a resolved p mode (having the typical Lorentzian shape) in 100 randomly chosen simulations out of the initial 1000. This gives us a 10% probability of selecting one simulation containing a peak.
In each simulation containing a peak, the amplitude, the linewidth, and the central frequency of the peak were varied across the different simulations. We then performed a blind exercise by fitting the entire set of 1000 simulations without knowing which of them contained a peak and in what order. To do the test we used two models: (i) ℳ_{A}, including only a flat noise component, represented by a single free parameter; and (ii) ℳ_{B}, including both the flat noise component and the Lorentzian profile, given by Eq. (5), for a total of four free parameters. The two models considered are therefore fit to all the individual chunks, whether or not they contain the oscillation peak. An example of the two fitting models is shown in Fig. 4 for two different simulations, with and without the oscillation peak.
We computed 2000 Bayesian evidences, ℰ_{A,i} and ℰ_{B,i} with i ranging from 1 to 1000, namely one for each of the two models in each simulation. By computing the detection probabilities p_{B,i} for each simulation according to Eq. (9), all the simulations containing the oscillation peak could be identified when adopting the threshold p_{B} ≳ 0.99, which means that the model containing the oscillation peak is significantly more likely than the one containing only the flat noise component. This probability threshold corresponds to the limit of a strong evidence condition in the Jeffreys’ scale of strength (Jeffreys 1961). This shows that, although ℳ_{B} is disfavored because it contains three more free parameters than ℳ_{A} – according to the Bayesian perspective of Occam’s razor –, ℳ_{B} provides a much better fit than that of a single noise component when the oscillation peak is present, thus resulting in a considerably larger Bayesian evidence (see also CD14, Sect. 2.1 for more discussion). We therefore now have a method for detecting peaks based on the Bayesian model comparison that works well and is straightforward to conduct.
We can easily extend this analysis to the case of an unresolved peak by changing the function that describes the peak profile in the model ℳ_{B} with that given by Eq. (6). Thus, following Approach 1 described in CD14, for each star in our sample we fit chunks of PSD with a frequency range containing one radial order per time, and apply the peak significance test as described before to all the ambiguous detections occurring in the selected chunk.
We note that while performing the peak significance test for the 19 LRGs, we found that a 8σ level, with σ representing the background level fit given in Sect. 2.1 and used in the peak bagging model, Eq. (7), is a raw indication of the 99% threshold in p_{B} for all the targets, and can thus be used as a guideline to select peaks to be tested with our method based on the Bayesian model comparison. Figure 5 illustrates an example of peak significance test performed for KIC 12008916, where p_{B}< 0.99 (the peak marked by the vertical dotted red line), with a 8σ background level overlaid (dashed blue line) to show that the peak height of the tested peak is well comparable.
Fig. 4
Simulations of a chunk of PSD for the peak significance test in a red giant. The top panel shows the case of a simulation containing only a flat noise component, while the bottom panel shows a simulation including an oscillation peak with its characteristic Lorentzian shape. The black thick line represents the resulting fit as computed by Diamonds (using ℳ_{A} in the top panel and ℳ_{B} in the bottom panel), with median values for each parameter. 

Open with DEXTER 
2.4. Mode identification
The last step of the peak bagging analysis involves the mode identification. In the case of pure acoustic ℓ = 1,2,3 modes this is accomplished by computing their position relative to that of the closest radial mode, which in turn can usually be easily identified in all the stars owing to its high amplitude and linewidth. We therefore adopt the asymptotic relation for p modes (Vandakurov 1968; Tassoul 1980), obtaining for each radial order nwhere Δν is the mean large frequency separation. The mean small frequency spacings δν_{01} and δν_{02} are derived through the relations provided by Corsaro et al. (2012), with massdependent slopes (15)and (16)valid for RGB stars like in our sample. The mean small frequency spacing δν_{03} is given by the relation (Huber et al. 2010) (17)For the ℓ = 1 mixed modes we instead adopt the asymptotic relation provided by Mosser et al. (2012b, their Eq. (9)). The mode identification for the rotationally split modes (m = + 1, − 1, with m the azimuthal order) is instead derived from the position of the central components since the modes are in general well separated in LRGs. All the values for Δν, mass, the period spacing of g modes ΔΠ_{1}, and the coupling factor q are taken from Mosser et al. (2012c) and are listed in Table 1 as a summary.
Whereas the asymptotic values for p modes proved to be quite accurate for all the stars, in the case of mixed modes a correction for ΔΠ_{1} and q from the values listed in Mosser et al. (2012c) was required for some targets (indicated in Table 1), especially those showing variations in ΔΠ_{1} with the radial order (see Sect. 3 for more details). The correction was made by an auxiliary fit to the mixedmode frequencies in a bidimensional grid (ΔΠ_{1},q) spanning ± 10 s and ± 0.05 units, respectively, from the literature values. The auxiliary fit has the only purpose of providing a more reliable proxy for the frequency position of the dipole mixed modes, hence used for the mode identification process.
In particular, the stars KIC 8475025, KIC 9267654, and KIC 11353313 were found to show mixed modes with a peculiar frequency position because the frequency splitting due to the rotation of the star is very similar to the frequency spacing between adjacent mixed modes. This generates a misleading mode identification at first glance. A cautious inspection of all the rotational split components for these stars was therefore needed in order to solve the ambiguity (see, e.g., Beck et al. 2014, for more discussion on mode identification in these difficult cases). For the remainder of the stars in the sample, the mode identification was straightforward even when rotational effects are present.
Literature values for Δν, mass, ΔΠ_{1}, and q used for the mode identification of the stars.
Fig. 5
Example of a fit chunk for KIC 12008916 derived by Diamonds. The PSD is shown in black, while the resulting fit using the parameters listed in Tables B.37 and B.38 is indicated by a green solid line. The level of eight times the background is shown with a blue dashed line as a reference for the peak significance. The colored vertical bands highlight the oscillation modes modeled by a Lorentzian profile, Eq. (5), with ℓ = 0 in blue, ℓ = 2 in green, ℓ = 3 in orange, and ℓ = 1 mixed modes in red. The vertical dotted lines mark the central frequency ν_{0} for each of the fit modes, with the corresponding mode identification (Peak #, ℓ, m) also labeled, according to the description given in Appendix B. The case of the unresolved mixed mode (26,1, −1) is shown in red because the peak has a detection probability (p_{B} = 0.002) below the threshold suggested in Sect. 2.3. 

Open with DEXTER 
3. Results
All the results for oscillation frequencies, amplitudes, linewidths for the resolved modes, and oscillation frequencies and heights for the unresolved ones are presented in Appendix B, with detection probabilities for the peaks that required a significance test as explained in Sect. 2.3, and with a mode identification as explained in Sect. 2.4. A total of 1618 oscillation modes was fit for the peak bagging analysis presented in this work, with an average of ~85 modes per star. We performed a peak significance test for a total of 612 peaks (~38% of the entire number of oscillation modes), of which 380 (~62% of tested peaks) gave a detection probability p_{B} ≥ 0.99. This results in ~14% of the total number of peaks that did not fulfil the suggested detection threshold. The configuring parameters of Diamonds used during the computations are specified in the corresponding appendix.
The 68% Bayesian credible intervals are provided for each measurement as computed from the individual marginal probability distributions of the model parameters, according to the description given by CD14. We note that for some oscillation modes, the quoted error bars of the corresponding frequencies can be smaller than the formal frequency resolution of the PSD. Although not intuitive at first glance, this may happen because the reported error bars only refer to the capability of the adopted model to reproduce the observations, an aspect that does not uniquely depend on the resolution of the dataset, in our case represented by the formal frequency resolution obtained from the Fourier analysis (see, e.g., Fröhlich et al. 2012, for more discussion on the presence of error bars smaller than the resolution given by the data, as obtained from another astrophysical application of the Bayesian inference). This effect is evident for those oscillation modes for which a sinc^{2} profile is used. Since this profile has a small FWHM (few data bins) and it is an appropriate profile shape for reproducing spikelike peaks (see Fig. 3), it leads to a more precise estimate of the frequency centroid than when the Lorentzian profile is used. This latter profile is instead fitted to resolved or partially resolved modes, and it averages for the stochastic nature of the oscillation peak over many data bins. As a result of our analysis, the error bar on the frequency of the unresolved modes is on average 10 times smaller than that of the resolved modes. Therefore, for clarity we stress that in general the precision level of the error bars reported in this work is not limited by the formal frequency resolution of the PSD because it represents the adequacy of the model presented in Sect. 2.2 to fit the data.
As reported in Table 1, 7 stars out of the 19 analyzed required a refitting of ΔΠ_{1} during the mode identification process, with deviations from the literature values found up to ~9 s for KIC 6144777, and ~4 s for KIC 7060732. In particular, the stars KIC 6144777 and KIC 12008916 show ΔΠ_{1} that varies on the order of seconds with varying radial order. This caused the mode identification process to be more complex than for other stars in the sample, although still feasible with an appropriate refitting of ΔΠ_{1} as explained in Sect. 2.4. For completeness, we note that in the newer catalogue provided by Mosser et al. (2014), the measurement of ΔΠ_{1} for the stars KIC 6144777 and KIC 8366239 was corrected, thus corresponding to the refitted value used in this work.
We confidently detect the signature of rotation through the presence of rotationally split modes in all the LRGs except KIC 9145955, KIC 9882316, KIC 10123207, and KIC 10200377. However, KIC 6117517 only shows the presence of two significant rotationally split modes in the highest S/N region of the PSD, which makes a detailed study of rotation for this star difficult. Instead, the stars KIC 7619745, KIC 8366239, KIC 8475025, KIC 9267654, KIC 10257278, KIC 11913545, and KIC 12008916 show very few or even no oscillation modes corresponding to the zonal component m = 0. The mode identification was possible in most of the cases, except for those low S/N oscillation peaks in the wings of the PSD for which no clear azimuthal order could be assigned, or for oscillation peaks with double mode identification. The latter case is observable in the stars KIC 8475025, KIC 9267654, and KIC 11353313 in which the confusion limit due to the large rotational splitting is present, as mentioned in Sect. 2.4. The double mode identification for some of the peaks in the stars mentioned before can be explained by the overlap of the split component m = + 1 with the adjacent m = −1 when the rotational splitting is the same as the frequency spacing between two adjacent mixed modes of different g mode.
The star KIC 7060732, despite the presence of the largest number of fit modes among the 19 LRGs (123 in total), shows the largest number of nonidentified peaks (40), all placed in the wings of the PSD, because of the confusion generated by the low S/N of the peaks coupled with the large rotational splitting observed. KIC 9882316 has instead the lowest number of fit modes (49) but with a clear and straightforward mode identification.
Fig. 6
Mode linewidths for KIC 12008916 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
3.1. Mode linewidths
The first result related to the asteroseismic measurements of individual oscillation modes is represented by the behavior of mode linewidths with increasing frequency in the PSD. The socalled linewidth depression has been observed in several CoRoT stars (Benomar et al. 2009b; Barban et al. 2009; Deheuvels et al. 2010; Ballot et al. 2011b) and more recently in a larger sample of mainsequence and subgiant stars observed with Kepler (Benomar et al. 2013; Appourchaux et al. 2014). Theoretical studies of solar data by Belkacem et al. (2011) have confirmed that ν_{max} is closely related to the frequency position of the linewidth depression, although a full interpretation of this result requires more investigation.
The top panel of Fig. 6 shows all the linewidth measurements of KIC 12008916 for the angular degrees ℓ = 0,2,3, and the resolved (or partially resolved) ℓ = 1 mixed modes, as a function of the corresponding oscillation frequencies in the PSD. As can be seen in the region marked by the vertical gray band, the linewidths either flatten or even decrease when the frequency of the oscillation peak is close to ν_{max}. This is clearer for ℓ = 0,2 modes, while for ℓ = 3 the number of modes is not sufficiently large to let us conclude on a possible trend. For the case of ℓ = 1 mixed modes we have included a lowdegree polynomial fit to visualize the global trend, which also shows a depression in linewidth close to ν_{max}. We note, however, that the measured linewidths of the ℓ = 2 modes are not the physical linewidths and are only used to show the presence of the linewidth depression in comparison to the other modes with different angular degree; by fitting a single Lorentzian profile to the region of the ℓ = 2 modes we are not taking into account the possible effects arising from both the rotational splitting and from the presence of quadrupole mixed modes, thus resulting in measured linewidths that are broader than the real ones.
To investigate more thoroughly the behavior of the mode linewidths in a star we computed the normalized fraction of resolved ℓ = 1 mixed modes with respect to unresolved ones, which can be expressed for each radial order as (18)where N_{res,n} and N_{unres,n} are the number of resolved and unresolved mixed modes, respectively, fit in each radial order n. The denominator of Eq. (18) allows us to normalize by the total number of mixed modes fit in the star, hence to compare the value among different stars in the sample. The resulting normalized fraction, hereafter f_{res} for simplicity, as a function of the average frequency position of the dipole mixed modes falling in each radial order, is shown in the bottom panel of Fig. 6 for KIC 12008916. The horizontal dotted line separates the regime of resolved mixed modes fitting (upper part, f_{res}> 0) from that of unresolved mixed modes fitting (lower part, f_{res}< 0). We do not compute f_{res} for radial orders in which no mixed modes are fit.
For radial orders where the mode linewidths encounter a depression, we therefore expect f_{res} to decrease as well, since the number of fit resolved mixed modes is likely to be lower than in the case of radial orders in which the modes have a larger linewidth. This is shown again in the bottom panel of Fig. 6, where the decrease in f_{res} is sited in the region close to ν_{max}. This behavior is evident for all the other stars in the sample as well (see the figures in Appendix B). To use f_{res} as an indicator of the resolving level of the mixed modes fit in the star, we can compute an average value as (19)where N_{radial} is simply the total number of radial orders where the mixed modes are fit. The value ⟨ f_{res} ⟩ for KIC 12008916 is indicated in the bottom panel of Fig. 6 by a horizontal dashed red line, and similarly for all the other stars in the corresponding figures provided in Appendix B. For KIC 12008916 we find that ⟨ f_{res} ⟩ = 0.003, namely the highest value in the entire sample and the only one falling in the resolveddominated regime: the number of resolved (or partially resolved) mixed modes per radial order in this star is on average larger than that of the unresolved ones. For KIC 3744043, instead, we find the minimum value of the sample, ⟨ f_{res} ⟩ = −0.057, lying in the unresolveddominated regime. The highest values of ⟨ f_{res} ⟩ correspond to stars in which no rotation is detected, or in most cases to stars for which the central component of dipole mixed modes, m = 0, is missing.
Fig. 7
Average mode linewidth at maximum mode height, ⟨ Γ_{H} ⟩, for the LRGs (red circles) and the sample of mainsequence and subgiant stars analyzed by Appourchaux et al. (2012) (blue triangles) as a function of the stellar effective temperature from Pinsonneault et al. (2012), in a linearlog scale. 1σ error bars are shown on both coordinates. The solid pink line shows a polynomial fit to the sample of RGs, while the solid teal line represents the law proposed by Appourchaux et al. (2012) for their sample of stars. The dashed yellow line is a polynomial fit to the total sample of stars. The 3σ regions coming from the polynomial fits are also shown for comparison. The inset shows a zoomin of our sample of red giant stars. 

Open with DEXTER 
An often investigated quantity related to the linewidth measurements, as already mentioned in Sects. 1 and 2, is their correlation with the stellar effective temperature (see, e.g., Hekker et al. 2010; Baudin et al. 2011; Appourchaux et al. 2012; Belkacem et al. 2012; Corsaro et al. 2012, for more results and details). A theoretical modeling of the damping rates of radial modes based on the existing observations from CoRoT and Kepler (Belkacem et al. 2012) has proposed a common physical description of the linewidthtemperature correlation from mainsequence to lowtemperature giant stars (down to ~4000 K), although it did not exploit linewidth measurements in the critical temperature range used in this paper.
Following Baudin et al. (2011) and Appourchaux et al. (2012), we have computed for each star in our sample an average linewidth at maximum mode height, ⟨ Γ_{H} ⟩, by taking the average linewidth of radial modes in three radial orders around the radial mode with maximum height, which is more immune to systematic effects as discussed by e.g., Appourchaux et al. (2012). The resulting ⟨ Γ_{H} ⟩ values are shown in Fig. 7 (red circles) as a function of T_{eff} from Pinsonneault et al. (2012), where the error bars on each ⟨ Γ_{H} ⟩ are the standard deviations from the three linewidths used in the calculation. This allows us to compare the result with the existing set of measurements for a sample of mainsequence and subgiant stars investigated by Appourchaux et al. (2012) (blue triangles). We observe a steeper temperature gradient of ⟨ Γ_{H} ⟩ for the hotter mainsequence stars with respect to the cooler RGs, in agreement with previous studies (Baudin et al. 2011; Belkacem et al. 2012). This change in the slope of the correlation between T_{eff} and linewidths appears more evident in the temperature range around T_{eff} ~ 5400 K, and is emphasized by the polynomial fits overlaid to our measurements and by the confidence regions marked with grayshaded bands, in comparison to the power law fit derived by Appourchaux et al. (2012).
Fig. 8
Mode amplitudes for KIC 12008916 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
3.2. Mode amplitudes
Mode amplitudes are the primary information used to study the detectability of the oscillations and the physical process responsible for their excitation mechanism, especially in the less known case of the mixed modes (e.g., Grosjean et al. 2014). Retrieving empirical relations that allow us to predict amplitudes in other RG stars (e.g., Corsaro et al. 2013, and references therein) is certainly useful to facilitate future detailed asteroseismic analyses on a larger sample of targets.
An example of the resulting mode amplitudes as a function of the corresponding oscillation frequencies for KIC 12008916 is given in Fig. 8 for the different angular degrees, including the resolved mixed modes for which a polynomial fit to enhance the trend was added. The plots for all the other stars can be found in Appendix B. By computing an average ratio (or visibility factor) of the amplitudes between ℓ = 0 modes, ⟨ A_{0} ⟩, and ℓ = 2, resolved ℓ = 1, and ℓ = 3 modes, ⟨ A_{2} ⟩, ⟨ A_{1} ⟩, ⟨ A_{3} ⟩, respectively, we find that ⟨ A_{0} ⟩ / ⟨ A_{2} ⟩ = 1.19 ± 0.10, ⟨ A_{0} ⟩ / ⟨ A_{1} ⟩ = 1.84 ± 0.26, and ⟨ A_{0} ⟩ / ⟨ A_{3} ⟩ = 2.77 ± 0.41. The error bars are computed from the dispersion in the ratios coming from the sample analyzed. These visibilities are useful for setting up prior distributions on mode amplitudes in other red giant stars (see Sect. 4 for more discussion), while individual mode amplitudes can also be used to compare visibilities of LRGs with stars in different evolutionary stages (e.g., Ballot et al. 2011a; Benomar et al. 2013).
Fig. 9
Maximum radial mode amplitudes for the LRGs (red circles) as a function of the corresponding radial mode frequency ν_{Amax} in a log–log scale, with 68% Bayesian credible intervals overlaid. Included, the amplitude measurements by Huber et al. (2011) for the same stars (filled green triangles), with their 1σ error bars, reported as a function of their ν_{max} values. The corresponding amplitude predictions for the measurements by Huber et al. (2011), computed from the best scaling relation model found by Corsaro et al. (2013), are also included for comparison (open green triangles). 

Open with DEXTER 
To show how the behavior of the mode amplitude varies from star to star, we plot the maximum radial mode amplitude of each star, here indicated as A_{max}, against the corresponding radial mode frequency ν_{Amax} in Fig. 9 (red circles). We note that the amplitude measurements from this work agree on average within 6% with those listed by Huber et al. (2011), despite the different datasets used and the method adopted, which in the latter case provides maximum amplitudes per radial mode from a global analysis of the power excess of the stellar oscillations (see Huber et al. 2011, and references therein for more details). The values A_{max} and ν_{Amax} from this work are all part of the results coming from a detailed peak bagging analysis (see the tables in Appendix B). The amplitude scaling relation used for computing the predictions for the measurements provided by Huber et al. (2011), indicated with open green triangles in Fig. 9, is given by the best model ℳ_{4,β} of Corsaro et al. (2013) for the case of LC data. When comparing our A_{max} measurements with the predictions, on average we find an agreement of around 19%. We point out, however, that the amplitude scaling relation adopted for the comparison is calibrated on a set of global parameters such as ν_{max}, Δν, and A_{max} from the power excess, and not on detailed measurements for an individual oscillation mode as those provided in this work.
4. Discussion and conclusions
Starting from the background fitting phase, we find a good agreement (~5%) between our estimated parameters of the granulation signal, Eq. (3), and those available from Kallinger et al. (2014), proving that even with an additional year of observation this background signature has remained nearly unchanged for this sample of stars. This shows that we can easily retrieve prior distributions for the background free parameters of the RGs even if new datasets are used. This aspect is helpful for improving our performance in extracting oscillations from a large number of stars since the background fitting is a necessary step in the peak bagging analysis.
As shown by Fig. 6 for KIC 12008916, and in all the other figures in Appendix B for the entire sample of LRGs investigated, every star manifests a clear linewidth depression in the frequency region close to ν_{max}, consistent with the expectations for less evolved stars. This behavior is clear for ℓ = 0,2 modes (although the measured linewidths of the quadrupole modes are not the real ones, as stated in Sect. 3.1) and is less pronounced for resolved (or partially resolved) ℓ = 1 mixed modes, although still evident (see, e.g., the polynomial fit shown in red in Fig. 6, top panel), whereas it is questionable for ℓ = 3 modes because the low number of fit peaks does not fully cover the observed frequency range of the oscillations. The presence of a depression in linewidth for all the stars is also supported by our computation of the normalized fraction of resolved to unresolved mixed modes, f_{res}, given by Eq. (18). The average normalized fraction ⟨ f_{res} ⟩ given by Eq. (19) instead tells us that even with four years of nearly continuous observations with Kepler, all the red giants in our sample are still dominated by the presence of unresolved mixed modes, except for KIC 12008916 where there is basically the same number of unresolved modes as resolved or partially resolved ones. This proves that the lifetime of the g modes, clearly not lower than that of the most gdominated mixed modes, is still not measurable. A detailed study involving the new individual linewidth measurements provided here would definitely help to tighten the constraints on the physical relation between the location of the linewidth depression, the cutoff frequency, and ν_{max} in red giants, thus shedding light on our understanding of the damping mechanism of the oscillations, especially in the case of the dipole mixed modes (Grosjean et al. 2014).
Another significant result involving linewidths is their correlation with the stellar effective temperatures. In the comparison given in Fig. 7, we observe a temperature gradient in the linewidths that is steeper for mainsequence and subgiant stars than for RGs, thus flattening toward lower temperatures, as already found by Baudin et al. (2011) and Belkacem et al. (2012). Unlike the large spread in linewidths found by Baudin et al. (2011) for the RGs observed with CoRoT, our linewidths appear to be much less dispersed, systematically lower, and quite correlated with T_{eff}, despite the small temperature range available, as also highlighted by the polynomial fit, and the corresponding confidence region, to our sample shown in Fig. 7. This is in agreement with the theoretical predictions by Belkacem et al. (2012). We find that the change in the slope of the correlation between linewidths and temperatures from our sample of RGs to that of the mainsequence and subgiant stars observed by Kepler and analyzed by Appourchaux et al. (2012) is more evident in the temperature range around T_{eff} ~ 5400 K and could be related to a change in the regime responsible for the mode damping mechanism at the beginning of the RGB. Importantly, the temperature range of the RGs analyzed in this work, 4800−5500 K, covers the gap in observations between red giants and subgiant and mainsequence stars from previous works that used CoRoT and Kepler data (e.g., Baudin et al. 2011; Belkacem et al. 2012; Corsaro et al. 2012). We therefore consider that the new results presented are important in order to perform a more realistic modeling of the underlying physics responsible for the observed change in gradient occurring at the bottom of the RGB.
We have noted that our measurements of maximum mode amplitude, available in Appendix B and plotted in Fig. 9, are in good agreement (~6%) with the amplitudes of maximum power derived by Huber et al. (2011) according to the method described by Kjeldsen et al. (2005, 2008). This shows that, at least for the range of ν_{max} investigated in this work, the existing amplitude scaling relations can in principle be used to retrieve raw predictions on maximum amplitudes of individual radial modes. By introducing the optimal amplitude scaling relation derived by Corsaro et al. (2013), we find that the amplitude predictions for our sample of stars agree within ~19%. By exploiting the average amplitude visibilities, ⟨ A_{0} ⟩ / ⟨ A_{ℓ} ⟩, amplitude estimates for the different angular degrees can be derived. These tools are very useful for the preparation of prior distributions on mode amplitudes in RGs having ν_{max} ∈ [110,200] μHz, hence they build the base for setting up the peak bagging analysis for a large number of stars. A wider range of ν_{max} will certainly allow more accurate testing of these simple relations and eventually obtaining and calibrating one or more specific scaling relations for individual mode amplitudes in a similar fashion to that investigated by Corsaro et al. (2013). Our physical comprehension and modeling of the stochastic excitation mechanism of the mixed modes in RGs (see, e.g., Grosjean et al. 2014) will certainly benefit from individual mode amplitudes and corresponding linewidth measurements of the dipole mixed modes provided in this paper.
In addition, the remarkable precision level obtained on the individual mode frequencies of the p modes of all the LRGs, ranging from 10^{2} to 10^{3} μHz, coupled with the large number of p modes extracted from each star (spanning from six to nine different radial orders), allow us to constrain the regions of sharp structure variation caused by the He ii zone inside the red giants with an unprecedented level of detail (see Corsaro et al. 2015, for more details). The new frequency measurements derived here will help to improve existing stellar structure models of evolved lowmass stars settling in the RGB phase of the stellar evolution.
Through the peak bagging analysis exploiting the highquality Kepler data used in this work, we could extract and characterize a total of more than 1600 different oscillation modes. Following the work proposed by CD14, we successfully extended the fitting procedure to the more complex case of the red giant stars, for which a large number of mixed modes is present. As shown by CD14, and now in this work, the Bayesian approach coupled with highefficiency sampling algorithms, offers a valuable and robust way of inferring asteroseismic parameters from power spectra. This approach allows us to perform the fitting of many oscillation modes, i.e., of several tens of free parameters, in a reasonably short time (of the order of minutes). In addition, the computation of the Bayesian evidence has allowed us to quickly and easily test the peak significance of more than 600 oscillation modes, as also discussed in Sects. 2.3 and 3.
By adopting the peak bagging model given by Eq. (8), the Diamonds code has performed well for all the computations done. This is in general explained by an easy setting up of the prior distributions for the free parameters of the model, by the absence of degeneracies in the sampling of the parameter space when adopting individual parameters for each mode and with the combination of amplitudelinewidth instead of heightlinewidth in the mode profile (see Eq. (5)), and by the avoided estimation of the linewidths for the narrowest (namely unresolved) oscillation peaks (see Sect. 2.2). The latter case in particular proves that by using a mixture of two different profiles, hence distinguishing between resolved (or partially resolved) modes and unresolved ones, considerably improves our performance for the fitting of the oscillations in RGs. The main drawbacks of this approach are related to the requirement of a visual inspection of the region of the PSD of the star containing the oscillations, thus involving the selection of the modes to be fit, the choice of the peak profile to be adopted, and the setting up of the corresponding prior distributions. However, these steps can all be improved and made easier by means of auxiliary tools based on existing asteroseismic scaling relations, as presented in Sect. 2.4. Since the number of mixed modes in RGs is largely dominant over that of p modes, and since among the mixed modes most are still unresolved, as seen in nearly all the stars analyzed here with more than four years of observations (Sect. 3.1), we therefore recommend the adoption of a peak bagging model along the same lines as those described in Sect. 2.2 for future fitting of the oscillations in evolved lowmass stars.
The mode identification process, presented in Sect. 2.4, may sometimes be problematic for the case of the dipole mixed modes since having a reliable estimate of the true period spacing ΔΠ_{1} is necessary. By starting from the literature values listed in Table 1, we find that a refitting of ΔΠ_{1} was required for 7 stars out of the 19 analyzed (~37% of the sample), meaning that the extraction process for the mixed modes may need an additional search for a proper solution of ΔΠ_{1}, always coupled with a visual inspection of the result. Based on the experience gained with the analysis done for the 19 LRGs, we consider the visual inspection for the mode identification of the mixed modes an important and often decisive step, especially for those stars where the confusion limit due to the rotational splitting is present (KIC 8475025, KIC 9267654, KIC 11353313) and for those with variations in ΔΠ_{1} with the radial order (KIC 6144777 and KIC 12008916). This aspect clearly represents a limitation to the full automatization of the peak bagging analysis in red giant stars, but it might be improved in the future by analyzing and comparing the results arising from a larger variety of targets, especially those having higher rotation rates. However, we stress that, provided that the used values of ΔΠ_{1} are accurate enough, the asymptotic relation for the mixed modes works remarkably well at reproducing their frequencies for all the peaks identified in our analysis. This is in agreement with the recent theoretical study by Jiang & ChristensenDalsgaard (2014), who investigated the asymptotic regime of the mixed modes and confirmed the reliability of their asymptotic relation.
Last but not least, the clear detection of rotation in 14 stars of the sample will greatly help to constrain the physical mechanisms responsible for the angular momentum transport in RGs (e.g., Tayar & Pinsonneault 2013, and references therein). In particular, by reconstructing the rotational profile of the star up to the core level by using the mixed modes with different mixture content between p and g modes, provided in this work, it will be possible to investigate the evolution of the angular momentum transport inside the star starting from the mainsequence phase of the stellar evolution. Thanks to the variety of masses of the stars in our sample, spanning the range 1−2 M_{⊙} (Table 1), the models involving the decoupling of the convective and radiative zones in lowmass RGs, expected after the first dredge up (Tayar & Pinsonneault 2013), can be intensively tested and refined.
To conclude, the full set of results presented in Sect. 3 and discussed in Sect. 4, representing the largest set of detailed asteroseismic mode measurements ever made available, with the high precision and accuracy level achieved from fouryear datasets, offers a great opportunity to perform thorough investigations and testing of the existing stellar models and stellar evolution theory, asteroseismic scaling relations, and of the underlying physics of both the damping and the excitation mechanisms of solarlike and mixedmode oscillations in red giant stars. Future works following the approach presented here to extend the peak bagging analysis to larger samples of red giants observed by Kepler, will definitely bring an outstanding improvement to our understanding level on the stellar physics of lowmass stars.
Acknowledgments
E.C. is funded by the European Community’s Seventh Framework Programme (FP7/2007−2013) under grant agreement N° 312844 (SPACEINN). The research leading to these results has received funding from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007–2013) ERC grant agreement N° 227224 (PROSPERITY), from the Fund for Scientific Research of Flanders (G.0728.11), and from the Belgian federal science policy office (C90291 GaiaDPAC). E.C. thanks F. Baudin, P. Beck, G. Davies, T. Kallinger and A. Miglio for useful discussions.
References
 Anderson, E. R., Duvall, Jr., T. L., & Jefferies, S. M. 1990, ApJ, 364, 699 [NASA ADS] [CrossRef] [Google Scholar]
 Appourchaux, T. 2003, Ap&SS, 284, 109 [NASA ADS] [CrossRef] [Google Scholar]
 Appourchaux, T., Benomar, O., Gruberbauer, M., et al. 2012, A&A, 537, A134 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Appourchaux, T., Antia, H. M., Benomar, O., et al. 2014, A&A, 566, A20 (A14) [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ballot, J., Barban, C., & van’t VeerMenneret, C. 2011a, A&A, 531, A124 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ballot, J., Gizon, L., Samadi, R., et al. 2011b, A&A, 530, A97 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Barban, C., Deheuvels, S., Baudin, F., et al. 2009, A&A, 506, 51 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Baudin, F., Samadi, R., Goupil, M.J., et al. 2005, A&A, 433, 349 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Baudin, F., Barban, C., Belkacem, K., et al. 2011, A&A, 529, A84 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Beck, P. G., Bedding, T. R., Mosser, B., et al. 2011, Science, 332, 205 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Beck, P. G., Montalban, J., Kallinger, T., et al. 2012, Nature, 481, 55 [NASA ADS] [CrossRef] [Google Scholar]
 Beck, P. G., Hambleton, K., Vos, J., et al. 2014, A&A, 564, A36 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Bedding, T. R., Huber, D., Stello, D., et al. 2010, ApJ, 713, L176 [NASA ADS] [CrossRef] [Google Scholar]
 Bedding, T. R., Mosser, B., Huber, D., et al. 2011, Nature, 471, 608 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Belkacem, K., Goupil, M. J., Dupret, M. A., et al. 2011, A&A, 530, A142 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Belkacem, K., Dupret, M. A., Baudin, F., et al. 2012, A&A, 540, L7 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Benomar, O., Appourchaux, T., & Baudin, F. 2009a, A&A, 506, 15 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Benomar, O., Baudin, F., Campante, T. L., et al. 2009b, A&A, 507, L13 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Benomar, O., Bedding, T. R., Mosser, B., et al. 2013, ApJ, 767, 158 [NASA ADS] [CrossRef] [Google Scholar]
 Benomar, O., Belkacem, K., Bedding, T. R., et al. 2014, ApJ, 781, L29 [NASA ADS] [CrossRef] [Google Scholar]
 Borucki, W. J., Koch, D., Basri, G., et al. 2010, Science, 327, 977 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Broomhall, A.M., Miglio, A., Montalbán, J., et al. 2014, MNRAS, 440, 1828 [NASA ADS] [CrossRef] [Google Scholar]
 Chaplin, W. J., Houdek, G., Karoff, C., Elsworth, Y., & New, R. 2009, A&A, 500, L21 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 ChristensenDalsgaard, J. 2004, Sol. Phys., 220, 137 [NASA ADS] [CrossRef] [Google Scholar]
 Corsaro, E., & De Ridder, J. 2014, A&A, 571, A71 (CD14) [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Corsaro, E., Stello, D., Huber, D., et al. 2012, ApJ, 757, 190 [NASA ADS] [CrossRef] [Google Scholar]
 Corsaro, E., Fröhlich, H.E., Bonanno, A., et al. 2013, MNRAS, 430, 2313 [NASA ADS] [CrossRef] [Google Scholar]
 Corsaro, E., De Ridder, J., & García, R. A. 2015, A&A, 578, A76 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Deheuvels, S., Bruntt, H., Michel, E., et al. 2010, A&A, 515, A87 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Deheuvels, S., García, R. A., Chaplin, W. J., et al. 2012, ApJ, 756, 19 [NASA ADS] [CrossRef] [Google Scholar]
 Deheuvels, S., Doğan, G., Goupil, M. J., et al. 2014, A&A, 564, A27 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 De Ridder, J., Arentoft, T., & Kjeldsen, H. 2006, MNRAS, 365, 595 [NASA ADS] [CrossRef] [Google Scholar]
 De Ridder, J., Barban, C., Baudin, F., et al. 2009, Nature, 459, 398 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Fröhlich, H.E., Frasca, A., Catanzaro, G., et al. 2012, A&A, 543, A146 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 García, R. A., Hekker, S., Stello, D., et al. 2011, MNRAS, 414, L6 [NASA ADS] [CrossRef] [Google Scholar]
 García, R. A., Mathur, S., Pires, S., et al. 2014, A&A, 568, A10 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Grosjean, M., Dupret, M.A., Belkacem, K., et al. 2014, A&A, 572, A11 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Gruberbauer, M., Kallinger, T., Weiss, W. W., & Guenther, D. B. 2009, A&A, 506, 1043 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Handberg, R., & Campante, T. L. 2011, A&A, 527, A56 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Hekker, S., Barban, C., Baudin, F., et al. 2010, A&A, 520, A60 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Huber, D., Bedding, T. R., Stello, D., et al. 2010, ApJ, 723, 1607 [NASA ADS] [CrossRef] [Google Scholar]
 Huber, D., Bedding, T. R., Stello, D., et al. 2011, ApJ, 743, 143 [NASA ADS] [CrossRef] [Google Scholar]
 Jeffreys, H. 1961, Theory of Probability, 3rd edn. (Oxford: OUP) [Google Scholar]
 Jenkins, J. M., Caldwell, D. A., Chandrasekaran, H., et al. 2010, ApJ, 713, L120 [NASA ADS] [CrossRef] [Google Scholar]
 Jiang, C., & ChristensenDalsgaard, J. 2014, MNRAS, 444, 3622 [NASA ADS] [CrossRef] [Google Scholar]
 Kallinger, T., Mosser, B., Hekker, S., et al. 2010a, A&A, 522, A1 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Kallinger, T., Weiss, W. W., Barban, C., et al. 2010b, A&A, 509, A77 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Kallinger, T., Hekker, S., Mosser, B., et al. 2012, A&A, 541, A51 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Kallinger, T., De Ridder, J., Hekker, S., et al. 2014, A&A, 570, A41 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Karoff, C., Campante, T. L., Ballot, J., et al. 2013, ApJ, 767, 34 [NASA ADS] [CrossRef] [Google Scholar]
 Kjeldsen, H., Bedding, T. R., Butler, R. P., et al. 2005, ApJ, 635, 1281 [NASA ADS] [CrossRef] [Google Scholar]
 Kjeldsen, H., Bedding, T. R., Arentoft, T., et al. 2008, ApJ, 682, 1370 [NASA ADS] [CrossRef] [Google Scholar]
 Koch, D. G., Borucki, W. J., Basri, G., et al. 2010, ApJ, 713, L79 [NASA ADS] [CrossRef] [Google Scholar]
 Kumar, P., Franklin, J., & Goldreich, P. 1988, ApJ, 328, 879 [NASA ADS] [CrossRef] [Google Scholar]
 Mathur, S., García, R. A., Catala, C., et al. 2010, A&A, 518, A53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Miglio, A., Montalbán, J., Baudin, F., et al. 2009, A&A, 503, L21 [NASA ADS] [CrossRef] [EDP Sciences] [MathSciNet] [Google Scholar]
 Miglio, A., Montalbán, J., Carrier, F., et al. 2010, A&A, 520, L6 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Miglio, A., Brogaard, K., Stello, D., et al. 2012, MNRAS, 419, 2077 [NASA ADS] [CrossRef] [Google Scholar]
 Miglio, A., Chiappini, C., Morel, T., et al. 2013, MNRAS, 429, 423 [NASA ADS] [CrossRef] [Google Scholar]
 Miglio, A., Girardi, L., Rodrigues, T. S., Stello, D., & Chaplin, W. J. 2015, Astrophys. Space Sci. Proc., 39, 11 [NASA ADS] [CrossRef] [Google Scholar]
 Mosser, B., Barban, C., Montalbán, J., et al. 2011a, A&A, 532, A86 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mosser, B., Belkacem, K., Goupil, M. J., et al. 2011b, A&A, 525, L9 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mosser, B., Goupil, M. J., Belkacem, K., et al. 2012a, A&A, 548, A10 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mosser, B., Goupil, M. J., Belkacem, K., et al. 2012b, A&A, 540, A143 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Mosser, B., Goupil, M. J., Belkacem, K., et al. 2012c, VizieR Online Data Catalog: J/A&A/540/A143 [Google Scholar]
 Mosser, B., Benomar, O., Belkacem, K., et al. 2014, A&A, 572, L5 [NASA ADS] [CrossRef] [EDP Sciences] [PubMed] [Google Scholar]
 Pinsonneault, M. H., An, D., MolendaŻakowicz, J., et al. 2012, ApJS, 199, 30 [NASA ADS] [CrossRef] [Google Scholar]
 Pires, S., Mathur, S., Garcia, R. A., et al. 2015, A&A, 574, A18 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Stello, D., Meibom, S., Gilliland, R. L., et al. 2011, ApJ, 739, 13 [NASA ADS] [CrossRef] [Google Scholar]
 Stello, D., Huber, D., Bedding, T. R., et al. 2013, ApJ, 765, L41 [NASA ADS] [CrossRef] [Google Scholar]
 Tassoul, M. 1980, ApJS, 43, 469 [NASA ADS] [CrossRef] [Google Scholar]
 Tayar, J., & Pinsonneault, M. H. 2013, ApJ, 775, L1 [NASA ADS] [CrossRef] [Google Scholar]
 Thompson, S. E., Christiansen, J. L., Jenkins, J. M., et al. 2013, Kepler Data Release 21 Notes (KSCI19061001), Kepler mission [Google Scholar]
 Vandakurov, Y. V. 1968, Sov. Ast., 11, 630 [NASA ADS] [Google Scholar]
 Vrard, M., Mosser, B., & Barban, C. 2014, in SF2A2014: Proc. Annual meeting of the French Society of Astronomy and Astrophysics, eds. J. Ballet, F. Martins, F. Bournaud, R. Monier, & C. Reylé, 531 [Google Scholar]
Appendix A: Results for the background fitting
The parameter values derived by means of Diamonds for the entire sample of 19 LRGs analyzed in this work are listed in Table A.1 for the Harveylike profiles B(ν), Eq. (3), and in Table A.2 for the Gaussian envelope G(ν), Eq. (4). The background fits are shown in Fig. A.1 for all the stars except KIC 12008916, which is instead shown in Fig. 2.
Referring to the definitions presented by CD14, the configuring parameters of Diamonds used for all the computations are initial enlargement fraction 1.5 ≤ f_{0} ≤ 2.1, shrinking rate 0.01 ≤ α ≤ 0.03, number of live points N_{live} = 500, number of clusters 1 ≤ N_{clust} ≤ 10, number of total drawing attempts M_{attempts} = 10^{4}, number of nested iterations before the first clustering M_{init} = 1500, and number of nested iterations with the same clustering M_{same} = 50.
Fig. A.1
Same as for Fig. 2 but for the remaining stars of the sample. 

Open with DEXTER 
Appendix B: Results for the oscillation modes
To list the results from the peak bagging analysis we adopt a nomenclature similar to that used by CD14 and present the oscillation modes in ascending frequency order, divided by angular degree. Each mode can be identified uniquely by the set of numbers (Peak #, ℓ, m). An example of this nomenclature for KIC 12008916 is given in Fig. 5. The missing values for amplitudes and linewidths correspond to the cases of unresolved mixed modes, were only the heights are fit. The missing values for the detection probability p_{B} represent peaks for which the significance test was not necessary owing to their large height and the clear position with respect to the asymptotic relations for p and mixed modes (Sect. 2.4).
This appendix also includes the figures for mode linewidths and mode amplitudes for all the stars of the sample, similarly to Figs. 6 and 8, respectively, shown for KIC 12008916.
Referring to the definitions presented by CD14, the configuring parameters of Diamonds used for all the computations are initial enlargement fraction 0.5 ≤ f_{0} ≤ 3.4, shrinking rate α = 0.01, number of live points N_{live} = 1000, number of clusters 1 ≤ N_{clust} ≤ 4, number of total drawing attempts M_{attempts} = 10^{4}, number of nested iterations before the first clustering M_{init} = 1000, and number of nested iterations with the same clustering M_{same} = 50.
Fig. B.1
Mode linewidths for KIC 3744043 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.2
Mode amplitudes for KIC 3744043 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.3
Mode linewidths for KIC 6117517 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.4
Mode amplitudes for KIC 6117517 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.5
Mode linewidths for KIC 6144777 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.6
Mode amplitudes for KIC 6144777 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.7
Mode linewidths for KIC 7060732 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.8
Mode amplitudes for KIC 7060732 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.9
Mode linewidths for KIC 7619745 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.10
Mode amplitudes for KIC 7619745 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.11
Mode linewidths for KIC 8366239 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.12
Mode amplitudes for KIC 8366239 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.13
Mode linewidths for KIC 8475025 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.14
Mode amplitudes for KIC 8475025 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.15
Mode linewidths for KIC 8718745 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.16
Mode amplitudes for KIC 8718745 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.17
Mode linewidths for KIC 9145955 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.18
Mode amplitudes for KIC 9145955 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.19
Mode linewidths for KIC 9267654 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.20
Mode amplitudes for KIC 9267654 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.21
Mode linewidths for KIC 9475697 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.22
Mode amplitudes for KIC 9475697 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.23
Mode linewidths for KIC 9882316 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.24
Mode amplitudes for KIC 9882316 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.25
Mode linewidths for KIC 10123207 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.26
Mode amplitudes for KIC 10123207 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.27
Mode linewidths for KIC 10200377 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.28
Mode amplitudes for KIC 10200377 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.29
Mode linewidths for KIC 10257278 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.30
Mode amplitudes for KIC 10257278 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.31
Mode linewidths for KIC 11353313 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.32
Mode amplitudes for KIC 11353313 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.33
Mode linewidths for KIC 11913545 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.34
Mode amplitudes for KIC 11913545 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Fig. B.35
Mode linewidths for KIC 11968334 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER 
Fig. B.36
Mode amplitudes for KIC 11968334 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER 
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 7619745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8366239, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8366239, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8475025, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8475025, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8718745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8718745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9145955, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9145955, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9267654, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9267654, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9475697, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9475697, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9882316, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9882316, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10123207, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10123207, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10200377, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10200377, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10257278, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10257278, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11353313, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11353313, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11913545, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11913545, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11968334, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11968334, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 12008916, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 12008916, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
All Tables
Literature values for Δν, mass, ΔΠ_{1}, and q used for the mode identification of the stars.
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 7619745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8366239, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8366239, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8475025, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8475025, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 8718745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 8718745, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9145955, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9145955, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9267654, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9267654, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9475697, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9475697, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 9882316, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 9882316, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10123207, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10123207, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10200377, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10200377, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 10257278, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 10257278, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11353313, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11353313, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11913545, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11913545, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 11968334, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 11968334, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, linewidths, and heights of the mixed modes of KIC 12008916, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
Median values with corresponding 68.3% shortest credible intervals for the oscillation frequencies, amplitudes, and linewidths of the p modes of KIC 12008916, as derived by Diamonds by using the peak bagging model defined by Eqs. (7) and (8).
All Figures
Fig. 1
Asteroseismic HRD ν_{max} − T_{eff} for the sample of 19 LRGs investigated. Amplitudes of maximum oscillation power, A_{max}, as measured by Huber et al. (2011) are indicated in color scale. All ν_{max} values are provided by Huber et al. (2011), while temperatures are taken from Pinsonneault et al. (2012). 1σ error bars are indicated for both coordinates. 

Open with DEXTER  
In the text 
Fig. 2
Background fit of the star KIC 12008916, as derived by Diamonds. The original PSD is shown in gray, while a smoothed version with boxcar width set to Δν/ 5, with Δν taken from Mosser et al. (2012c; see also Table 1), is shown as a black line to guide the eye. The red thick line represents the background model without the Gaussian envelope and computed with the values listed in Table A.1. The green dotted line accounts for the additional Gaussian component using the values listed in Table A.2. The individual components of the background model as given by Eq. (1) are shown by blue dotdashed lines. 

Open with DEXTER  
In the text 
Fig. 3
Unresolved dipole mixed mode for KIC 12008916. The FWHM of the oscillation peak spans less than three data bins, as indicated by the red segment having a threebin width. The red dotted line represents the half maximum level of the peak. 

Open with DEXTER  
In the text 
Fig. 4
Simulations of a chunk of PSD for the peak significance test in a red giant. The top panel shows the case of a simulation containing only a flat noise component, while the bottom panel shows a simulation including an oscillation peak with its characteristic Lorentzian shape. The black thick line represents the resulting fit as computed by Diamonds (using ℳ_{A} in the top panel and ℳ_{B} in the bottom panel), with median values for each parameter. 

Open with DEXTER  
In the text 
Fig. 5
Example of a fit chunk for KIC 12008916 derived by Diamonds. The PSD is shown in black, while the resulting fit using the parameters listed in Tables B.37 and B.38 is indicated by a green solid line. The level of eight times the background is shown with a blue dashed line as a reference for the peak significance. The colored vertical bands highlight the oscillation modes modeled by a Lorentzian profile, Eq. (5), with ℓ = 0 in blue, ℓ = 2 in green, ℓ = 3 in orange, and ℓ = 1 mixed modes in red. The vertical dotted lines mark the central frequency ν_{0} for each of the fit modes, with the corresponding mode identification (Peak #, ℓ, m) also labeled, according to the description given in Appendix B. The case of the unresolved mixed mode (26,1, −1) is shown in red because the peak has a detection probability (p_{B} = 0.002) below the threshold suggested in Sect. 2.3. 

Open with DEXTER  
In the text 
Fig. 6
Mode linewidths for KIC 12008916 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. 7
Average mode linewidth at maximum mode height, ⟨ Γ_{H} ⟩, for the LRGs (red circles) and the sample of mainsequence and subgiant stars analyzed by Appourchaux et al. (2012) (blue triangles) as a function of the stellar effective temperature from Pinsonneault et al. (2012), in a linearlog scale. 1σ error bars are shown on both coordinates. The solid pink line shows a polynomial fit to the sample of RGs, while the solid teal line represents the law proposed by Appourchaux et al. (2012) for their sample of stars. The dashed yellow line is a polynomial fit to the total sample of stars. The 3σ regions coming from the polynomial fits are also shown for comparison. The inset shows a zoomin of our sample of red giant stars. 

Open with DEXTER  
In the text 
Fig. 8
Mode amplitudes for KIC 12008916 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. 9
Maximum radial mode amplitudes for the LRGs (red circles) as a function of the corresponding radial mode frequency ν_{Amax} in a log–log scale, with 68% Bayesian credible intervals overlaid. Included, the amplitude measurements by Huber et al. (2011) for the same stars (filled green triangles), with their 1σ error bars, reported as a function of their ν_{max} values. The corresponding amplitude predictions for the measurements by Huber et al. (2011), computed from the best scaling relation model found by Corsaro et al. (2013), are also included for comparison (open green triangles). 

Open with DEXTER  
In the text 
Fig. A.1
Same as for Fig. 2 but for the remaining stars of the sample. 

Open with DEXTER  
In the text 
Fig. B.1
Mode linewidths for KIC 3744043 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.2
Mode amplitudes for KIC 3744043 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.3
Mode linewidths for KIC 6117517 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.4
Mode amplitudes for KIC 6117517 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.5
Mode linewidths for KIC 6144777 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.6
Mode amplitudes for KIC 6144777 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.7
Mode linewidths for KIC 7060732 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.8
Mode amplitudes for KIC 7060732 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.9
Mode linewidths for KIC 7619745 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.10
Mode amplitudes for KIC 7619745 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.11
Mode linewidths for KIC 8366239 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.12
Mode amplitudes for KIC 8366239 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.13
Mode linewidths for KIC 8475025 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.14
Mode amplitudes for KIC 8475025 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.15
Mode linewidths for KIC 8718745 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.16
Mode amplitudes for KIC 8718745 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.17
Mode linewidths for KIC 9145955 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.18
Mode amplitudes for KIC 9145955 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.19
Mode linewidths for KIC 9267654 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.20
Mode amplitudes for KIC 9267654 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.21
Mode linewidths for KIC 9475697 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.22
Mode amplitudes for KIC 9475697 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.23
Mode linewidths for KIC 9882316 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.24
Mode amplitudes for KIC 9882316 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.25
Mode linewidths for KIC 10123207 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.26
Mode amplitudes for KIC 10123207 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.27
Mode linewidths for KIC 10200377 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.28
Mode amplitudes for KIC 10200377 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.29
Mode linewidths for KIC 10257278 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.30
Mode amplitudes for KIC 10257278 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.31
Mode linewidths for KIC 11353313 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.32
Mode amplitudes for KIC 11353313 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.33
Mode linewidths for KIC 11913545 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.34
Mode amplitudes for KIC 11913545 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Fig. B.35
Mode linewidths for KIC 11968334 as a function of the corresponding oscillation frequencies. Top panel: linewidth measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the linewidths as derived by Diamonds are shown for each data point. The red solid line represents a polynomial fit to the linewidths of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The shaded region represents the range ν_{max} ± σ_{env}, with ν_{max} from Table A.2 indicated by the dashed vertical line. Bottom panel: the normalized fraction of resolved mixed modes with respect to unresolved ones, f_{res} (black dots), defined by Eq. (18). The frequency position of each point is the average frequency of the resolved dipole mixed modes falling in each radial order (or that of the unresolved mixed modes if no resolved mixed modes are present). The horizontal dotted line represents the limit of resolveddominated regime, as defined in Sect. 3.1, while the horizontal dashed red line marks the average f_{res} given by Eq. (19). 

Open with DEXTER  
In the text 
Fig. B.36
Mode amplitudes for KIC 11968334 as a function of the corresponding oscillation frequencies. Amplitude measurements as defined by Eq. (5) for each angular degree (ℓ = 0 blue squares, ℓ = 2 green triangles, ℓ = 3 yellow stars, and resolved ℓ = 1 mixed modes red circles). Open symbols represent modes with detection probability under the suggested threshold (see Sect. 2.3). The 68% credible intervals for the amplitudes as derived by Diamonds are shown for each data point. The solid red line represents a polynomial fit to the amplitudes of the ℓ = 1 mixed modes, included to emphasize the trend with frequency. The dashed vertical line indicates the ν_{max} value listed in Table A.2. 

Open with DEXTER  
In the text 
Current usage metrics show cumulative count of Article Views (fulltext article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 4896 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.