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The classification of frequencies in the {\gamma} Doradus / {\delta} Scuti hybrid star HD 49434

Hybrid stars of the {\gamma} Doradus and {\delta} Scuti pulsation types have great potential for asteroseismic analysis to explore their interior structure. To achieve this, mode identi- fications of pulsational frequencies observed in the stars must be made, a task which is far from simple. In this work we begin the analysis by scrutinizing the frequencies found in the CoRoT photometric satellite measurements and ground-based high-resolution spectroscopy of the hybrid star HD 49434. The results show almost no consistency between the frequencies found using the two techniques and no characteristic period spacings or couplings were identified in either dataset. The spectroscopic data additionally show no evidence for any long term (5 year) variation in the dominant frequency. The 31 spectroscopic frequencies identified have standard deviation profiles suggesting multiple modes sharing (l, m) in the {\delta} Scuti frequency region and several skewed modes sharing the same (l, m) in the {\gamma} Doradus frequency region. In addition, there is a clear frequency in the {\gamma} Doradus frequency region that appears to be unrelated to the others. We conclude HD 49434 remains a {\delta} Scuti/ {\gamma} Doradus candidate hybrid star but more sophisticated models dealing with rotation are sought to obtain a clear picture of the pulsational behaviour of this star.


INTRODUCTION
The discovery of numerous candidate hybrid γ Doradus/ δ Scuti stars by space telescopes, is proving to be a real problem for asteroseismology. Several γ Doradus/δ Scuti hybrid stars have now been detected and studied from ground-based observations and further candidates are still being discovered with data from the MOST, CoRoT and Kepler space telescopes. These stars all show frequencies, attributed to pulsation, in both the δ Scuti and γ Doradus frequency ranges. Despite the impressive quality of the data, no mode identification has yet been published of such a hybrid star to confirm their nature. The detailed spectroscopic study of the candidate hybrid star HD 49434 presents an opportunity to confirm the existence of hybrid stars and draw conclusions on their nature.
Early Kepler results show that γ Doradus/δ Scuti hybrid stars may challenge current understanding of the classical instability strip and the definitions of δ Scuti and γ Doradus stars (Grigahcène et al. 2010a, Grigahcène et al. 2010b. Whilst many of the first hybrid stars studied from space show hundreds of excited modes, other detailed investigations of the frequencies show many of these hundreds are aliases, combinations or couplings of one another Chapellier et al. 2011Chapellier et al. , 2012Breger et al. 2012). Other studies have shown that granulation could be responsible for many of these frequencies, especially those previously attributed to high degree l modes which suffer cancellation effects in photometry, even for high-precision space telescopes (Kallinger & Matthews 2010).
Examination of the statistics of the class identifications is also proving to be problematic. The large numbers of hybrid stars found all over the δ Scuti and γ Doradus regions of the Hertzsprung-Russell diagram are as yet unexplained Uytterhoeven et al. 2011;Balona 2011) and are particularly difficult to explain in the hotter spectral-type A stars. These stars are beyond the theoretical limit for driving of γ Doradus-type pulsation and, indeed, any type of low-frequency pulsation. The alternate explanation, starspots, is also problematic as the lack of a sizeable convective shell for these hot stars inhibits starspot formation (Balona 2011). To shed light on all these questions arising from space photometry, more ground-based observations of stars, such as HD 49434, are required to characterise the frequency spectra of hybrid stars.
Historically, HD 49434 (HR 2514, HIP 32617) was a remarkably understudied star given it has a visual magnitude of 5.74 (Bruntt et al. 2004). Since its identification as a γ Doradus star by Bruntt et al. (2002) however, much more effort has been put into several photometric and spectroscopic studies. The significant recent studies of Uytterhoeven et al. (2008) and Chapellier et al. (2011) have demonstrated that this star has frequencies in the γ Doradus region (0.3−3 d −1 ) and in the δ Scuti region (3 − 80 d −1 ) and this star thus offers the first detailed view of a hybrid γ Doradus/ δ Scuti star.
HD 49434 has a spectral type of F1V and effective temperature of 7632 ± 126 K (Gillon & Magain 2006). This places the star squarely in the expected overlap region of the p-mode δ Scuti pulsations and the g-mode γ Doradus pulsations. Rotational velocity measurements show this star is a rapid rotator; the most precise value is from Gillon & Magain (2006) giving v sin i = 85.4 ± 6.6 km s −1 . The same paper also contains a detailed abundance analysis, generally finding metallicities slightly higher than solar values. The abundances, in general, agree with previous spectroscopic work by Bruntt et al. (2002). The spectroscopic parameters from these works and those from two further photometric studies by Lastennet et al. (2001) and Poretti et al. (2005) are given in Table 1. The radius of the star is estimated from 2mass infra-red photometry to be 1.601 ± 0.052 R⊙ (Masana et al. 2006) and an estimate of the stellar mass of 1.55 ± 0.14 M⊙ is given in Bruntt et al. (2002).
Analysis of pulsations in HD 49434 began using groundbased spectroscopy in 1998 (Bruntt et al. 2002) when lowamplitude variations were observed in the spectral-line profiles. Strömgren photometry, taken in 2001, confirmed the variability with excess power in the 1 d −1 to 5 d −1 region, but yielded no identifiable frequencies (Bruntt et al. 2002). Further spectroscopy by Mathias et al. (2004) showed, again, low-amplitude variations in the blue wing of the line profile.
This star has been observed at Mt John University Observatory (mjuo) since February 2007 when a two-week observing run as part of a multi-site campaign was undertaken. The purpose of the campaign was to gather spectroscopic data simultaneous with observations from the CoRoT photometric satellite. The results were published in Uytterhoeven et al. (2008). From the spectroscopic data, three γ Doradus and five δ Scuti frequencies were identified, leading to the classification of HD 49434 as a hybrid pulsator. Only one of the γ Doradus and none of the δ Scuti frequencies were detected in the accompanying ground-based photometry from Sierra Nevada Observatory, Spain and San Pedro Mártir Observatory, Mexico. The frequencies from the CoRoT data analysis are presented in Chapellier et al. (2011). The high-precision photometry revealed a staggering 1686 significant frequencies in the five-month observing run with 840 of these identified as pulsation frequencies.
The vast number of frequencies found have led to further questions regarding the origins and stability of the stellar pulsations. This work expands on the analysis of the 689 spectra in Uytterhoeven et al. (2008) with the analysis of a further 1058 multi-site spectra making a total of 1747 observations.

OBSERVATIONS AND DATA TREATMENT
Observations of HD 49434 have continued at mjuo from the initial run in 2007 until January 2012, contributing to a large, long-term dataset to confirm and refine these frequencies. These data were combined with line profiles computed in Uytterhoeven et al. (2008) with additional spectra from feros and sophie taken in 2008. A summary of the times and dates of observations of the individual sites is presented in Table 2. These observations are plotted in Figure 1 to show the temporal distribution of the data.
Spectra from mjuo in New Zealand were collected using the 1 m McLellan telescope with the fibre-fed High Efficiency and Resolution Canterbury University LargeÉchelle Spectrograph (hercules) with a resolving power of R = 50000 operating over a range of 3800Å to 8000Å (Hearnshaw et al. 2002). The data collected from mjuo was divided into two time periods. The oldest dataset, which contained observations taken in 2007 and 2008, was analysed as part of the multi-site analysis of Uytterhoeven et al. (2008). Since then, observations have been taken from 2009 to 2012 which were analysed as a single-site dataset. This dataset had a total of 381 observations. Spectra were reduced using a matlab pipeline written by Dr. Duncan Wright. This pipeline performs the basic steps of flat fielding from whitelamp observations, calculating a dispersion solution from thorium-lamp observations and outputting the data into a two dimensional format.
feros is now installed on the Max-Planck-Gesellschaft / eso 2.2 m telescope and has a resolving power of R = 48000 (Kaufer et al. 1999). The spectral range covered is 3500Å Figure 1. Timing of spectra obtained from the four data sites; hercules data in blue diamonds and blue crosses, foces data in green squares, feros data in red circles and sophie data in black stars. The clusters of observations loosely match 2007 to 2012 observation seasons. The two hercules datasets were reduced using different image processing software and are regarded as independent sites. The prior-published data in Uytterhoeven et al. (2008) corresponds to the first cluster of observations in all datasets from the 2007 observing season around JD 245 4100.
to 9200Å. Reductions were done using a pipeline written for feros in midas (Rainer 2003).
The 1.93 m telescope at the Observatoire de Haute Provence, France, can observe with sophie (Spectrographe pour l'Observation des Phénomènes des Intérieurs stellaires et des Exoplanètes) (Perruchot et al. 2008). The wavelength range is 3870Å to 6940Å with a resolving power of R = 70000 (high-resolution mode). A software package adapted from the High Accuracy Radial velocity Planet Searcher (harps) spectrograph was used to reduce the spectra.
Each spectrum was cross-correlated using the deltafunction method (Wright, 2008, building on Wright et al., 2007 to create a single representative line-profile from approximately 4000 lines in the full spectrum. To check the consistency of methods between this paper and that of Uytterhoeven et al. (2008), a selection of the data taken as part of the 2007 multi-site spectroscopic campaign was analysed in famias. These data were provided as line profiles (as discussed in Uytterhoeven et al., 2008) which were computed using a Least-Squares Deconvolution (lsd) method (Donati et al. 1997(Donati et al. , 1999. This method differs slightly to the δ-function cross-correlation method used for the more recent hercules data, but produces very similar line profiles. Time-series analysis was performed using famias (Zima 2008), applied as in Zima et al. (2006). This entailed an analysis of the variations in the representative line profiles which identified the frequencies present. For examples of γ Doradus stars analysed using these techniques see a, b or Davie et al. (2014). A periodogram of the amplitude of the variation at each pixel in the line profile (in velocity measurements) for each frequency is shown in Figure 2 as an example of the pixel-by-pixel (pbp) technique. Frequency analysis of the moments (radial velocity, width and skewness) relies on the average symmetry of the line profile over a pulsation period. This is not the case for HD 49434 and the strong asymmetry of the variation of the line profile (see Figure 5 and Figure 6) results in non-sinusoidal be- haviour of these measurements, limiting the detection of the frequencies. Further comments on the origins and repercussions of the skew line profile is included in the discussion (Section 5.1).
A comparison between the results of the two data sets showed the pixel-by-pixel analysis to be nearly identical to the results of the line profile variations in Uytterhoeven et al. (2008). These results show excellent consistency between the Discrete Fourier Transform method employed in famias compared with the Intensity Period Search (Telting & Schrijvers 1997) method used in Uytterhoeven et al. (2008). The consistency between the results means we can merge the line profiles into a single extensive observational dataset and indicates no significant change to the results from the calculation of the line profile using the δ-function cross-correlation or an lsd technique.
For γ Doradus and δ Scuti stars, the standard deviation and phase profiles show the motion of the pulsation though the spectral line. These profiles vary depending on the mode, frequency and stellar parameters which can be determined using the mode identification tools in famias. In general, different modes have distinctive shapes in the line profiles and smooth phase profiles across the line with jumps linked to stationary points of the line profile. Examples of typical γ Doradus and δ Scuti line, standard deviation and phase profiles can be seen in  and Schmid et al. (2014), respectively.
Spectroscopic mode identification relies on the rotational broadening of the line profile to return a use number of pixels in the line profile. To date stars from v sin i = 9 km s −1 (Aerts & Kaye 2001) to v sin i = 101 km s −1 (Davie 2013) have been analysed successfully although it is noted that famias does have a mode-dependent rotation limit as deviations of the star from spherical symmetry due to rotation are ignored.  Table 3. Frequencies found in the pbp analysis of the full HD 49434 dataset. A † represents frequencies discarded as aliases as described in the text. Values in column 2 in bold type were also identified in the first 100 detected frequencies of CoRoT. Frequencies underlined indicate those in common with the identification of Uytterhoeven et al. (2008), with (*) being found only using the moment method. The pbp amplitudes are measured in normalised intensity units. Column 5 indicates group members of dsl, gdl, irr and spc as described in the text.

FREQUENCY ANALYSIS
The frequencies were analysed solely using the pixel-by-pixel method due to the severe asymmetry of the line profile. In total 31 frequencies (f1 to f31) were identified from the peaks in the Fourier spectra that were above the detection limit as defined in famias. A full list is shown in Table 3 and the Fourier spectra at selected prewhitening stages are shown in Figure 3. Formal uncertainties on the frequencies range from ± 0.00003 d −1 for f4 to ± 0.0002 d −1 for f31, but due to the low amplitude of the pulsations and the numerous observa- tional uncertainties inherent in the data, the frequencies are reported with a conservative error of ±0.001 d −1 . Upon inspection, six of these frequencies (f4, f13, f19, f23, f26 and f29) were flagged as possible aliases due to their proximity to 0 d −1 or 1 d −1 , but were kept for the subsequent analysis of the aliases standard deviation profiles. Artificially increased amplitudes in the Fourier spectrum are possible due to higher noise levels particularly in the 0 to 1 d −1 region, which can push a noise peak higher than a real frequency peak.

Frequency Aliases and Combinations
The large number of frequencies found in the multi-site spectroscopic data warranted the computation and comparison of frequency aliases and combinations in an automated way. For aliasing this focused the search for fa ± p = f b ± 0.002 for integer values of p up to p = 12. Only the match f3 ≈ f28 was identified.
Combinations of frequencies were tested for p * fa ± q = r * f b ± 0.002 d −1 for integer values of p, q and r up to 12 including q = 0. Several identifications were discovered but on closer examination these had high values of two or more of p, q and r (e.g. 3f1 ≈ 5f11) and are unlikely to arise without the additional presence of simpler combinations. As such they are regarded as purely coincidental. It is also unlikely that combinations not involving the highest amplitude frequencies would arise without seeing higher amplitude combinations from f1 to f3.

Comparison with CoRoT Results
The results of the dedicated CoRoT study of more than 331 000 single-passband photometric observations, taken over nearly 140 days from October 2007 to March 2008, are presented in Chapellier et al. (2011). They find a staggering 1686 significant frequency peaks and propose 840 frequencies intrinsic to HD 49434. The frequencies and their properties are available in electronic format as supplementary information to the paper. The uninterrupted high quality of the dataset allows for high precision of the detected frequencies and these can be compared with the spectroscopic results to understand the variability of this star. In the following analyses, the full 1686 frequencies are considered. The ten frequencies with the highest amplitude from the CoRoT analysis were first compared with the spectroscopic results to see if any frequencies matched. The frequencies are given in Table 4. Only the frequencies fc2, fc3, fc6 and fc7 were found in the spectroscopic analysis. The frequencies fc1 to fc10 were then imposed on the spectroscopic data to observe any potential signal and characterise the standard deviation and phase profiles. None of the ten frequencies have clear line profile and phase variations easily attributable to pulsations.
When the first 100 frequencies of the CoRoT findings were compared to the pbp frequencies, 12 of the 31 pbp frequencies were found to match to within ±0.003 d −1 . These matches are listed in Table 5. It is surprising how poorly the frequencies detected in each method align, especially the high-amplitude frequencies.

Classification of Frequencies
A least-squares fit was performed on the representative line profiles of the 1747 observations using the profiles of the 31 frequencies identified. The standard deviation profiles of each frequency fit were compared. Upon inspection, the profiles could be seen to fit into one of four classes. The mean profiles of the first two classes are plotted together in Figure  4 for direct comparison.
The first group, with the majority of the frequencies, has a two-bump structure with peaks terminating at the edges of the profile. The centres of the standard deviation and phase profiles are shifted to the right and are centred  near 18 km s −1 , an effect not seen in other γ-Doradus and δ-Scuti stars. Nineteen of the frequencies fitted this description and they are plotted in Figure 5. Noting the frequencies were all in the δ Scuti range, this group was named "δ-Scuti like" (dsl). The second-identified group contained five of the frequencies and since these were found to be exclusively in the γ Doradus range this set was labelled "γ-Doradus like" (gdl). The standard deviations and phases are plotted in Figure 6. Note the normalised phases of two of the frequencies can be inverted to match those of the other three frequencies.
The third group of misshapen standard deviation profiles was named " Irregular " (irr) and individual profiles are plotted in Figure 7 with nine frequencies of this type found. Most show only small changes in phase. Many of these profiles have frequencies at zero or one cycle-per-day as described above and most are likely to be artefacts of the data sampling. The two exceptions are f16 and f28. The latter is almost certainly a residual from the removal of the strong f3 frequency and the former could be an alias or combination frequency, or a real frequency undistinguished from the noise. This may also be the case for some others in this group.
The final group contained just one interesting frequency. The profile of f31 had a shape similar to other identified profiles in fast-rotating γ Doradus stars with narrow variation peaks in the wings and no variation in the line centre. This variation is matched by the changes in the phase profile. This frequency is plotted in Figure 8 and is labelled as a "special case" (spc).
To further investigate these groups, the residuals from the subtraction of the mean line profiles were phased over each of the 31 identified frequencies in Table 3. The results of the four groups are represented by the plots in Figure 9. These plots provide information on the stability of the frequency. Stellar frequencies are expected to show a smooth 'braided rope' structure as the pulsation moves through the line profile. Different modes will also show different inclinations and structure through the pulsation phase. As with the standard deviation profiles, the plots fall into one of three categories. The first group includes those plots with a clear structure with narrow 'braids', mostly in two regions of the line profile. These plots generally correspond to the δ-Scuti like (dsl) frequencies. Most of the γ-Doradus like (gdl) frequencies show a similar 'braided rope' shape with fewer braids with a more gentle phase slope. Frequencies with no clear pulsation spreading across the entire phase were classed as irregular (irr) and one frequency does not fit the above classifications, the special case (spc).
Based on the standard deviation profiles, phased residual profiles and the proximity of many to integer values, the frequencies in the irr group were classified as non-stellar frequencies, likely arising from data sampling aliases. The frequency f28 was also put in this group as it is the same as f3 within the detection limit. The remaining frequencies are regarded as candidate stellar frequencies which, together with the non-stellar frequencies, are further scrutinised in the following section.
The shape of the standard deviation profiles of the dsl group could be fitted by a mode identification, but the central shift and uneven amplitude of the standard deviation profiles are not easily accounted for. The homogeneity of the shapes of all the frequencies suggests that they are all representations of the same excited mode (couplings or splittings), or that there are many excitations of modes with the same (l, m) and different (n) . The shape of the gdl standard deviation profiles is not typical of a pulsation and suggests that they may be artefact frequencies, possibly of some rotational effect. This topic is discussed further in Section 4. The special case frequency, f31, on the other hand appears to be a real mode typical of a γ Doradus pulsation. It is not clear why this mode shows such clean variation with low amplitude. The shape of the standard deviation and phase profiles are recognisable in an individual least-squares fit, with only mild distortions, which rules out the frequency being a random residual from the interaction of other frequencies. tational velocity would shift frequencies from the co-moving frame according to rotational perturbation theory, and current perturbative methods (such as those used in famias) are not directly applicable to stars with such high rotational velocities to allow for an estimation of this (Ballot et al. 2010). If this were the case, it is not clear why kic 8054146, with a very high rotation rate, does not show the same phenomenon.

Radial Modes
Further results from the Chapellier et al. (2012) study of CoRoT 105733033 showed the majority (187 of 246) of the δ Scuti frequencies were couplings of the γ Doradus frequencies and the dominant frequency, identified as the fundamental radial mode (F ). The coupling followed the pattern p * F ±fγDor for p = 1, 2, 3 with amplitudes four times smaller than the original γ Doradus frequencies (fγDor). This was also seen in Breger et al. (2011), and further analysed in Guzik & Breger (2011), for the δ Scuti star kic 9700322.
Here the low frequency was identified as the difference between two dominant radial modes. The physical explanation offered by Chapellier et al. (2012) for this effect is the trapping of g-modes in the interior of the star which may induce thermodynamic perturbations in the convective envelope where the p-modes originate. Many δ Scuti stars follow this model of a dominant radial mode, so it could be expected for a hybrid star to display the same behaviour.
The dominant mode in the spectroscopic analysis of this star (f1 = 9.307 d −1 ) is a δ Scuti frequency which could potentially be the radial fundamental mode (usually A to F spectral-type stars have fundamental radial mode frequencies between 8 d −1 and 24 d −1 ). The standard deviation profile of the frequency is a two-bump shape typical of the radial modes (see for example Zima et al. 2006Zima et al. , 2007. The phase changes of HD 49434, however, are much smoother than the sharp "jumps" observed in the above examples. If f1 was found to be the fundamental radial mode then the other dsl frequencies would be also interpreted as radial modes. This cannot be the case as the low-frequency modes such as f5 could not also be radial modes. Better mode-identification of the primary frequency is required for a conclusive result. The spacings between this candidate radial mode and the other δ Scuti frequencies were tested for a correlation with the γ Doradus frequencies for p * F ± q * fa = f b ± 0.002 d −1 for integer vales of p and q from one to five. No matches were found other than for 3F ≈ 5f11 as found in Section 3.1.

Characteristic Spacings
In the asymptotic regime, frequencies with the same g-mode identification are predicted to be related by characteristic period spacings between frequencies of consecutive degree (Tassoul 1980). The study of Chapellier et al. (2012) found 24 of the 180 identified γ Doradus frequencies to have an asymptotic period spacing. Similarly, p-mode oscillations have a characteristic frequency spacing for modes with sequential n. Given the possibility of both p-and g-modes being present in HD 49434, both frequency and period spacings were tested for sequencing. This search also could identify any equidistant frequencies arising from rotational splitting of the frequencies.
As with the aliases and combinations, this was tested using an automated procedure by computing all possible spacings for the frequencies and corresponding periods identified in Table 3 and binning them using a resolution of 0.002 d −1 . The resulting histogram is shown as Figure 10(a) for the frequency spacing and Figure 10(b) for the spectroscopic results. This was repeated for the CoRoT full frequency identification and selected frequency subset in Figure 10(c) and Figure 10(d).
A possible repeated frequency spacing at 4.585 d −1 and a possible repeated period spacing at 0.0235 d were observed in the spectroscopic data. The CoRoT data do not show any single frequency or period spacing that is favoured, so it is likely the spectroscopic identification is coincidental, particularly as it does not involve the strongest δ Scuti or γ Doradus frequencies. If the δ-Scuti range frequencies arise from one or more radial modes then it is not expected any rotational splitting will be seen, unlike CoRoT 102918586 (Maceroni et al. 2010). Additionally, the very high value of v sin i for this star may mean it is a very rapid rotator and splits may become asymmetric (splitting values vary by up to 0.008 d −1 in the above CoRoT star) and indistinguishable from other frequency peaks.
The above computation of the frequency spacings also allowed a comparison with the results of Chapellier et al. (2012) and Breger et al. (2012), where frequency spacings from the dominant δ Scuti frequencies were found to match those of the high-amplitude γ Doradus frequencies. A search for frequency combinations in the spectroscopic data revealed only a possible link between f7, f8 and f35. Extended searches showed no other links between the strong frequencies. A general search for combinations in the CoRoT data reveals many candidate groups of frequencies due to the large number of inputs. A more constrained search of the first 100 identified frequencies for spacings, including one or more frequencies above 4 d −1 with links to one of the 10 highest-amplitude frequencies, found 10 frequency groups with limits of ±0.002 d −1 . None of these combinations included any other of the 30 highest-amplitude frequencies, so it is unlikely that the frequencies in HD 49434 are showing the same effects as the above hybrid stars.

Frequency and Amplitude Variations
Recent high-precision studies of γ Doradus/δ Scuti hybrid stars (e.g. Chapellier et al. 2012;Breger et al. 2012) have identified variations in the photometric amplitudes of observed frequencies over time, on a scale of months to years. The same phenomenon was tested using the spectroscopy of HD 49434. The data were broken into observing year blocks, generally comprising of the southern-hemisphere summer observing season. The blocks correspond to the groups depicted in Figure 1. The years 2007 to 2012, excepting 2009, were tested as there were insufficient observations in the 2009 season for an independent analysis. The Fourier spectrum for each dataset was calculated and the highest amplitude frequency extracted. This was the equivalent of fp1 for all but the 2010 dataset. The full results are given in Table 6. It is not clear why fp1 is not recovered in the 2010 dataset, but it may be due to unfortunate data sampling or lower quality data. Despite this, the four distinct time periods are sufficient for an indication of any amplitude variabil-    ity. The table shows the variation of the best fit amplitude over the five years of data to be a maximum of 0.00037 or 25%. The frequencies themselves show no variation within the detection limits (±0.001 d −1 ). The amplitudes do appear to vary by up to 25%, but it is not clear that this is not an effect of the different size and data quality encompassed in each set. All but the most extreme amplitude variation would be extremely difficult to detect in the best groundbased spectroscopic campaigns and Blazhko-like variability (non-symmetric changes in the maximum and minimum amplitudes), as seen in Breger et al. (2012), is beyond the precision of current spectroscopic methods. It is thus still possible that HD 49434 has variations in the amplitudes of its pulsations, but this cannot be confirmed in this study.

DISCUSSION
The analysis of some of the best-available spectroscopic and photometric datasets on a γ Doradus, or γ Doradus hybrid star, has clearly highlighted the complexities and gaps in current understanding of these pulsators. This discussion focuses on three areas where ground has been broken in this study, yet a full explanation is still lacking.

Standard Deviation Profile
Skewed line profiles and slight asymmetries in the standard deviation profile have been observed in several other γ Doradus stars, e.g. hd 40745 (Maisonneuve et al. 2011) and hd 189631 (Davie 2013). This has usually been observed in the blue wing of the line profiles. It is not yet clear whether this effect is intrinsic to the star or if it is an artefact of the line profile creation. Currently, two further refinements to line profile generation are being developed to form part of the reduction package. These including the inclusion of a least-squares deconvolution to the cross-correlation technique and improvements to the weighting of the δ-function amplitudes for individual lines. These may improve the signal in the line profiles in future. This is the first γ Doradus star that exhibits a severe shift in velocity space between the mean line profile and the standard deviation profile. The cause of this relative shift is not known, yet it hampers significantly the mode identification. Both rotation and non-adiabatic surface effects could be proposed as the mechanism for the shift but more examples are required for a solid analysis. It follows that future modelling routines should be capable of fitting this shift, and therefore shedding light on its physical origin.
Any rapidly-rotating star must be carefully analysed with the knowledge that there are not yet available pulsation models which include a full description of stellar rotation. It is therefore likely that the inclination and rotation could skew line profiles by confining pulsations to an equatorial wave-guide (Townsend 2003), which is not entirely visible to the observer. With the next generation of mode identification models promising the inclusion of more of these effects, it is hoped that this will lead to an explanation of some, or all, of the observed asymmetric phenomena.

Spectroscopic and Photometric Frequencies
Previous photometric and spectroscopic studies have identified frequencies and estimated the degree, l, of the corresponding modes. Analysis of the 2007 subset of the spectroscopic line profile variations in Uytterhoeven et al. (2008) found six frequencies, for which all but one was recovered in this extended analysis. No evidence for the rotational frequency of 2.666 d −1 proposed by the above was found. Two photometric frequencies in the same work were recovered but did not match those of the spectroscopy. The acquisition of high-temporal-resolution photometric data from the CoRoT satellite allowed for the detection of 840 significant photometric frequencies. The photometry and spectroscopy of this star show very self-consistent results, even over a fiveyear time period, yet the two methods do not show the expected consistency between the observed frequencies. Highamplitude δ Scuti frequencies are weak or non-existent in the photometry and conversely, high-amplitude γ Doradus frequencies are absent or have low-amplitudes in the spectroscopic data. The particular absence of the strongest frequency from the photometry (1.735 d −1 ) in the spectroscopic results is quite surprising. Furthermore, three of the twelve frequencies that match between the photometry and spectroscopy were discarded as they had irregular phased residual profiles. Although they are unlikely to be pulsational frequencies, their true origin is unknown.
There are some physical explanations for suppression of frequencies in photometric studies. The most obvious is the decreased sensitivity of photometric methods to modes with high l, as the surface integrated flux changes weaken with each additional nodal line. This is also expected to affect spectroscopic results, with smaller amplitude velocity variations across the star and increased noise in the standard deviation profiles. The low amplitude of the mode could be responsible for the lack of signal in the photometric data, but this is still a puzzling result.
Even more perplexing is the absence of the clearly dominant fc1 in the spectroscopic results. There are no particular modes expected to be suppressed in spectroscopic data but clear in photometry. There is the possibility that this frequency has another stellar origin, such as from a starspot. With an effective temperature close to 7300 K this star is close to the theoretical limit of convective blocking (T > 7400 K) above which spots are not predicted to occur. The time range of the CoRoT run (140 days) does not exclude the possibility of spot frequencies arising in the data, but it would be coincidental to also detect spots in the ground-based photometry from Uytterhoeven et al. (2008) spanning four years. It is not possible to exclude the possibility of fc1 being a rotational or a pulsational frequency, but, for either possibility, it is difficult to explain why it is not present in the spectroscopy.

The Unresolved Hybrid Phenomenon
The hybrid classification of HD 49434 was proposed based on the two types of frequencies observed in the star. Inspection of the standard deviation profiles and phased residual profiles of the γ Doradus group questions the independence of all but one of these frequencies. The remaining frequency, f31, is of an extremely low amplitude. Other recent studies of hybrid stars have suggested most of the δ Scuti frequencies to be non-intrinsic to the star, arising from interactions of the γ Doradus frequencies with the strong δ Scuti or radial fundamental modes (Chapellier et al. 2012;Breger et al. 2012). A summary of the properties of the two hybrids compared with those of HD 49434 is presented in Table 7.
The comparisons show that, although there is some suggestion that the CoRoT and Kepler stars share some similar properties, HD 49434 does not appear to be similar to either. The high rotational velocity of kic 8054146 may explain why no characteristic spacings are observed, yet the clarity of the triplet and "picket fence" patterns show other regular behaviours. A low inclination, and thus a very fast rotation of HD 49434, would explain some of the effects, such as finding no gap between the frequency domains (Handler 2012) and could even explain some of the difference between the photometric and spectroscopic frequency spectra.
The hybrid status of HD 49434 is questioned in Bouabid et al. (2009) since low, γ Doradus range frequencies could be a result of rotational splitting of the numerous high-degree p-modes. However, theoretical studies have shown that hundreds of frequencies are possible from an energy viewpoint (Moya & Rodríguez-López 2010). Attempts to explain the origins of the modes through stochastic excitation have thus far been inconclusive (Campante et al. 2010).
From the frequency analysis it appears that HD 49434 is a pulsating star with multiple modes sharing (l, m) in the traditional δ Scuti frequency region and several skewed but possibly related modes sharing the same (l, m) in the γ Doradus frequency region. In addition, there is a clear frequency in the γ Doradus frequency region that appears to be unrelated to the others. This means HD 49434 remains a candidate hybrid star. However this classification requires more evidence and understanding of properties of the line profile, rotational effects and hybrid nature before it can be confirmed.

Summary
Overall, the more data that are collected on HD 49434, the more questions seem to be raised. The spectroscopic frequency results are surprising and show several unexplained phenomena, yet the clear distinction in the shape of the standard deviation and phase profiles of the higher and lower frequencies that are found suggests an interesting physical origin. With the recent studies of hybrids in the Kepler field as a whole Balona et al. 2011;) and individual CoRoT and Kepler Table 7. Summary of the comparison of HD 49434 to CoRoT 105733033 (Chapellier et al. 2012) and kic 8054146 (Breger et al. 2012 hybrid stars (Chapellier et al. 2012;Breger et al. 2012) more questions are raised about these stars. The existence of the hybrid phenomenon is already in question and the spectroscopic results for HD 49434 so far add weight to both sides of the debate. On the one hand most of the γ Doradus frequencies appear to be manifestations of the dominant δ Scuti mode. Yet the existence of just one γ Doradus frequency that is visually distinct prevents the classification of this star as a pure δ Scuti.
To determine the true nature of hybrids, it is clear that classification cannot be made based on frequencies alone until more is understood about the physical origins of all the detected frequencies. Unfortunately, the alternative, collecting large numbers of high-resolution spectra, is telescopeintensive and is limited to relatively bright stars. Observations at mjuo are limited to about seventh magnitude stars, beyond which, exposure times smear out the temporal resolution required to study γ Doradus-type pulsations. This renders follow-up spectroscopy on most of the hybrid stars discovered with CoRoT and Kepler impossible at this time.
More observational data are always useful in the study of pulsations, but it is not evident that more data alone will answer the numerous questions arising from HD 49434. It appears to be a lack of understanding and modelling of the rotational aspects of the star that is hindering the mode identification the most. More sophisticated models, and perhaps a new approach to the rotation problem, are required before further significant advances in the understanding of this star can be made.