New Beta Cephei stars with KELT
Jonathan Labadie-Bartz Gerald Handler Joshua Pepper Luis Balona Peter De Cat Daniel J. Stevens Michael B. Lund Keivan G. Stassun Joseph E. Rodriguez Robert J. Siverd David J. James Rudolf B. Kuhn
astro-ph.SR





Jonathan Labadie-Bartz
jbartz@usp.br

0000-0002-2919-6786]Jonathan Labadie-Bartz
Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, Rua do Matão 1226, Cidade Universitária, 05508-900 São Paulo, SP, Brazil
Department of Physics & Astronomy, University of Delaware, Newark, DE 19716, USA
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA

0000-0001-7756-1568]Gerald Handler
Nicolaus Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland

0000-0002-3827-8417]Joshua Pepper
Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA

0000-0003-1241-9792]Luis Balona
South African Astronomical Observatory, PO Box 9, Observatory, 7935, Cape Town, South Africa

0000-0001-5419-2042]Peter De Cat
Royal Observatory of Belgium, Av Circulaire 3-Ringlaan 3, B-1180 Brussels, Belgium

0000-0002-5951-8328]Daniel J. Stevens
Center for Exoplanets and Habitable Worlds, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA
Department of Astronomy & Astrophysics, The Pennsylvania State University, 525 Davey Lab, University Park, PA 16802, USA

0000-0003-2527-1598]Michael B. Lund
Caltech IPAC – NASA Exoplanet Science Institute 1200 E. California Ave, Pasadena, CA 91125, USA

0000-0002-3481-9052]Keivan G. Stassun
Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA
Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN 37208, USA

0000-0001-8812-0565]Joseph E. Rodriguez
Center for Astrophysics  Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138, USA

0000-0001-5016-3359]Robert J. Siverd
Department of Physics and Astronomy, Vanderbilt University, Nashville, TN 37235, USA

0000-0001-5160-4486]David J. James
Center for Astrophysics  Harvard & Smithsonian, 60 Garden St, Cambridge, MA 02138, USA
Black Hole Initiative at Harvard University, 20 Garden Street, Cambridge, MA 02138, USA


0000-0002-4236-9020]Rudolf B. Kuhn
South African Astronomical Observatory, PO Box 9, Observatory, 7935, Cape Town, South Africa
Southern African Large Telescope, PO Box 9, Observatory, 7935, Cape Town, South Africa



We present the results of a search for Galactic stars, which are massive pulsating stars with both pressure modes and mixed modes. Thus, these stars can serve as benchmarks for seismological studies of the interiors of massive stars. We conducted the search by performing a frequency analysis on the optical light curves of known O- and B-type stars with data from the KELT exoplanet survey. We identify 113 stars, of which 86 are new discoveries, which altogether represents a  70% increase in the number presently known. An additional 96 candidates are identified. Among our targets, we find five new eclipsing binaries and 22 stars with equal frequency spacings suggestive of rotational splitting of nonradial pulsation modes. Candidates for runaway stars among our targets and a number of interesting individual objects are discussed.  Most of the known and newly discovered stars will be observed by the TESS mission, providing by far the most comprehensive observational data set of massive main sequence pulsating stars of sufficient quality for detailed asteroseismic studies. Future analysis of these light curves has the potential to dramatically increase our understanding of the structure of stellar interiors and the physical processes taking place therein.









§ INTRODUCTION
 

Despite recent advances, there remain uncertainties regarding the evolution and structure of massive stars. 
Currently, the role of rotation, internal angular momentum distribution and transport, and internal mixing are not satisfactorily understood in the context of stellar evolution. Mixing of material into the hydrogen-burning stellar core (“convective overshooting”) considerably affects the main sequence lifetime of massive stars <cit.>, and causes surface abundances to change. Rotation influences this process, but the details remain poorly constrained <cit.>. Differential rotation is sometimes measured in massive stars, but there are significant uncertainties regarding the coupling between the stellar core and envelope, and the degree to which angular momentum is transported from the core outward <cit.>. To make further progress in understanding the nature of massive-star interiors, studies of massive stars that are amenable to seismology are needed.

As a class, stars are massive non-supergiant variable stars with spectral type O or B with photometric, radial velocity, and/or line profile variations caused by low-order pressure and gravity mode pulsations <cit.>. Most of them are early B-type stars (roughly spanning spectral types B0 – B2.5) with masses between 8 –17 M_⊙. They are characterized by their relatively high-frequency pulsations (with typical periods between 2 – 7 hours) driven by the κ mechanism <cit.>.


The pulsational properties of stars make them particularly well-suited for detailed asteroseismic studies. They tend to oscillate in several nonradial modes, and sometimes have both p- and g-mode pulsations <cit.>. Because the frequency of each oscillation mode is determined by the physical conditions in the region in which it propagates, measuring these frequencies (and knowing their geometries on the stellar surface and the interior) translates to constraints on the physical conditions in the stellar interior. Seismic modelling of a small number of stars has already yielded significant progress. Quantitative estimates of the core overshooting parameter have been derived for the star HD 129929 <cit.>, which is also found to undergo non-rigid internal rotation <cit.>. Similar analyses have been done for β CMa <cit.>, δ Ceti <cit.>, 12 Lac <cit.>, V2052 Oph <cit.>, and a few others. Asteroseismology can also be used to measure stellar mass and radius, the surface rotation rate, and the evolutionary stage. Given that these stars are fairly massive, they are correspondingly rare: only about 250 such pulsators are known in our Galaxy <cit.>.


The technique of asteroseismology relies on having a long enough time baseline and a high enough cadence and precision to identify the periodic signals of as many pulsation modes as possible. Space-based time-series photometry provides excellent data for these purposes. Although current and past space observatories have been successfully used for asteroseismology, only a small number of the high-mass type stars have been observed, and subsequently modeled, to date in this capacity (e.g. HD 180642 with CoRoT; , δ Ceti with MOST; , β Cen with BRITE; ) – there have been no comprehensive asteroseismic studies of this class of star. 

The recently launched NASA Transiting Exoplanet Survey Satellite (TESS) mission <cit.> is a nearly all-sky photometric survey with a photometric precision similar to that of the Kepler mission, but designed primarily to target stars some five magnitudes brighter. The photometric precision for a 10th magnitude star in one hour of TESS observations is estimated to be 200 ppm. While the primary science goal of the TESS mission is to discover transiting exoplanets, TESS light curves will be leveraged for a host of ancillary science efforts. Among these is the use of TESS data for an asteroseismic study of a large sample of stars. To maximize the scientific yield,  we are mining ground-based time-series photometric data to identify as many stars as possible, to then be targeted by TESS for the purpose of asteroseismology. The TESS light curves of these stars will allow for detailed modeling of an unprecedented number of massive stars across a wide range of parameter space, and will result in important constraints on theories regarding stellar structure and evolution. 


In Section <ref> we introduce the data used for our search, and the cuts used to narrow down the number of light curves to be analyzed. Section <ref> describes the methods by which the data are analyzed. Our results are presented in Section <ref>, and a summary of our main conclusions are given in Section <ref>. 






§ DATA
 
The source of data used for our analysis is the Kilodegree Extremely Little Telescope (KELT) survey <cit.>. KELT is a photometric survey designed to discover transiting exoplanets orbiting stars in the magnitude range of 7 ≲ V ≲ 12, with light curves for ∼4.9 million objects across ∼70% of the sky. The KELT survey employs two small-aperture (42 mm) wide-field (26^∘ x 26^∘) telescopes, with a northern location at Winer Observatory in Arizona in the United States, and a southern location at the South African Astronomical Observatory near Sutherland, South Africa. The effective passband is roughly equivalent to a broad R-band filter. With time baselines of up to 10 years, a typical cadence of 30 minutes, and the precision to detect periodic signals down to approximately one to a few mmag, KELT light curves are well-suited to the detection of the periodic variability exhibited by stars. The utility of KELT light curves to detect periodic oscillations in brightness was demonstrated by <cit.>, <cit.>, and <cit.>. 

The goal of this work is the identification of new and candidate stars. We begin with a star catalog that is used internally by the TESS target selection committees and maintained by one of us (LB, <http://redcliffcottage.co.za/tess/>), which contains stars brighter than 12th magnitude, and includes literature spectral types (when available), and photometric magnitudes in multiple passbands. All stars with a spectral type between O4 – B7 (determined either by literature spectral type, or by photometric color) were selected. These 16682 stars were then cross-matched to the KELT catalog of all fields reduced until February 2016, resulting in 5840 matches. The KELT light curves of these 5840 O4 – B7 stars are then analyzed for the signatures of pulsation. The range of stellar brightness covered by KELT coincides very well with that of a large fraction of TESS targets, which makes KELT an extremely valuable source to pre-select targets to be later observed from space.






§ ANALYSIS
 

For each of the 5840 light curves for stars with spectral types between O4 – B7, a Fourier periodogram was computed in the range of 0 – 20 . To perform a pre-selection of candidates, each periodogram that had the strongest peak in the range of known star pulsation frequencies (f ≳ 3 ) was visually inspected, as were the light curves phased to twice the recovered period. On the basis of these plots, and in doubtful cases based on additional frequency analyses, all stars that had either untrustworthy data, showed no significant variability, exhibited obvious binary or rotational light curves, and those whose periodograms could be explained solely by reduction imperfections (residual differential color extinction) were rejected. Those that were not rejected were scrutinized, and a few more obvious non-pulsators were removed. The remaining stars were preliminarily classified into stars and candidate stars.

Objects pre-classified as stars either showed periodic variability at a single frequency between 4 – 14 and have spectral types between B0 – B2, or showed periodic variability at multiple frequencies in the range 4 – 14 (suggesting they are multi-mode pulsators), but without further spectral type cuts. The choice of the low-frequency limit near 4 is justified by this being approximately the expected value of the radial fundamental mode frequency at the end of the main sequence in the mass range, but also as a reasonable cutoff to discriminate against close binaries, rotational variables or other pulsators.

The group pre-classified as candidates contains stars that do not fall in the previous category, but have primary frequencies in the range 3 – 22 (sometimes with multiple significant frequencies), and stars where only one frequency is detected (if their spectral type is outside the range of B0 – B2) and the light curve shape suggests a pulsational origin for the variability. This group likely contains genuine stars, but is certainly contaminated by other types of variable stars. 

Other types of variable objects are found near stars in the HR diagram. Slowly pulsating B (SPB) stars tend to have spectral types between approximately B2 – B9, and pulsate in relatively lower frequency g-modes compared to stars <cit.>. However, very rapid rotation can lead some of these g modes to attain frequencies in the domain <cit.>. There are also “hybrid” pulsators, oscillating in low-frequency g-modes and high-frequency p-modes simultaneously <cit.>. Classical Be stars span the entire spectral range of B-type stars (even extending into the O and A types), and can also be pulsators, often with multiple modes. They are very rapidly rotating as a class, on average rotating at about 80% of their critical (or breakup) velocity, and occasionally eject matter to form a circumstellar disk <cit.>. The rapid rotation of classical Be stars can complicate the observed frequency spectrum <cit.>, as can variability in the circumstellar environment <cit.>. Whereas some of the hotter Be stars can also be pulsators, some of their gravity modes may also attain sufficiently high frequency to constitute a source of confusion.


The pixel scale of KELT is large (23^''), and some stars in our sample lie in relatively crowded fields near the Galactic plane. As a result, light from other sources will sometimes be blended with the target star in the aperture used by KELT. If a neighboring star is blended with the target star and is variable, then this variability can appear in the light curve for the target. This contamination issue is addressed by first inspecting images of high spatial resolution (DSS and 2MASS images) that show a patch of sky in the vicinity of the target, and identifying any neighboring sources that are close enough to the target to be blended in KELT photometry. Then, difference images of the pixels in the KELT images are analyzed to determine precisely which pixels are the source of the detected variability. This blending analysis can robustly identify contaminating sources further than two KELT pixels away from the target, and is effective at determining which source is variable in somewhat crowded fields. Through this analysis, we reject 3 stars that would have otherwise been classified as candidates. Additionally, three stars that were pre-selected as were found to have their signal originating in a neighboring star that could possibly be of a spectral type consistent with pulsation, and this variable source is included in our list of candidates. Another consequence of blending is that the measured amplitude of variability will be diluted proportional to the amount of flux from neighboring sources that leaks into the aperture used to extract the target star light curve. Therefore, all photometric amplitudes quoted here should be understood as a lower limit, although this effect is small in practice for the majority of stars in our samples. Since it is primarily the frequency (and spectral type or number detected of modes) that was used to pre-classify the stars in this work, and not the photometric amplitude, the amplitude suppression is not a significant concern for the purposes of classification. Of course, there can be cases where the amplitude suppression is so severe that we would miss the stellar signal completely. Another important cause of amplitude suppression is CCD saturation for bright stars. In this case, only non-saturated pixels would carry the stellar signal, but the total flux would include the saturated ones, resulting in a net decrease in amplitude in units of magnitude.

Keeping in mind the considerations above, the stars that survived the pre-selection (148 objects preliminarily identified as stars, and an additional 90 candidates) were frequency-analyzed by hand. To this end we used the Period04 software <cit.>. This package applies single-frequency Fourier analysis and simultaneous multi-frequency sine-wave least-squares fitting. It also includes advanced options such as the calculation of optimal light-curve fits for multiperiodic signals including harmonic, combination, and equally spaced frequencies. 

It is important to discuss under which conditions the detection of a variability signal is considered significant. The classical approach is to evaluate the signal-to-noise ratio of a peak in the Fourier amplitude spectrum. We computed the noise level as the average amplitude in a 2interval centered on the frequency of interest, i.e. considering possible additional stellar signals as noise at each prewhitening step. For ground-based campaign observations, S/N>4 is usually considered a safe choice <cit.>. On the other hand, in their search for stars in ASAS data whose basic characteristics should be similar to that of our data sets, <cit.> adopted a more conservative criterion of S/N>5. After careful examination of all our “borderline” cases that have the strongest signal within 4<S/N<5 we decided to select S/N>5 as the threshold for a star to be classified as a pulsator, and a more relaxed S/N>4 for candidates. At this stage, two stars were rejected because they were found to have met the S/N criterion only because of uncorrected artifacts in the data. Two further stars were rejected because of heavy crowding in the center of a cluster and likely data artifacts. Two more stars separated by 89" showed the same variability frequencies, suggesting the same source of origin of the variations. Our blending analysis unambiguously shows this signal as coming from the brighter of this pair, and so this brighter source (ALS 7011) is selected as a candidate while the other is not. 

Following that, the astronomical literature was checked for each of the individual stars. The position of these stars in the HR Diagram was determined, or at least estimated. In most cases, a luminosity estimate from the Gaia DR2 parallax <cit.> and Galactic reddening determinations <cit.> could be obtained, but for some stars more information such as accurate multicolor photometry was available, mostly in the Strömgren system <cit.>; calibrations thereof <cit.> were applied to estimate T_ eff and log g. These criteria allowed us to identify stars with frequency spectra similar to pulsators but with different stellar properties (such as and sdB pulsators). Based on these examinations, a few stars were moved in between the two groups (stars and candidates), and 22 more were rejected. We finally classify 113 stars as and 96 as candidates; 27 and three of those, respectively, have been reported in the literature before.





§ RESULTS
 



 §.§ New and Candidate Systems
 

Basic information on the stars investigated is listed in Tables <ref>, <ref>, and <ref>, sorted by increasing TESS Input Catalog (TIC, ) identifier. In addition to a primary identifier, the primary frequency and its photometric amplitude, the number of independent modes in the domain detected, coordinates, the V-band magnitude, and the spectral type are listed. All reported amplitudes are the semi-amplitudes. The next column indicates if the star is previously known to belong to the class (showing the appropriate reference), followed by a column that indicates whether the star is a known cluster member. Remarks are listed next, which are especially useful if the target has close visual companions (which is important input for TESS target selection). The amplitudes listed in Tables  <ref> and  <ref> should be viewed as lower limits, since light from neighboring sources can blend with the target star, acting to dilute the signal, as discussed in <ref>. This dilution is strongest in crowded fields. The sky positions of the and candidate stars identified in this work are shown in Fig. <ref>. KELT does not uniformly observe the sky. Some regions have no data, and there can be a large range in the number of observations from field to field. The distributions in Fig. <ref> are some convolution of KELT sampling and the intrinsic distribution of and candidate stars across the sky.







In Fig. <ref> we show the distribution of the primary detected frequency and its photometric amplitude, separated by spectral type bins. The overall median primary frequency is 6.04 for the group and 5.53 for the candidates, and the median amplitudes are 6.5 mmag and 3.0 mmag, respectively. Fig. <ref> shows histograms of the frequency, amplitude, number of modes, and V-band brightness for the and candidate stars. 








In Fig. <ref> we show the detection level (S/N=4) for pulsations in the domain for the stars with detections. Despite a few outliers (mostly blended faint stars) it is satisfactory, with a median detection level of 1.15 mmag and mean value of 1.8 mmag. This is approximately a factor of 3 lower than that of <cit.>, largely due to higher photometric precision and greater number of observations. As can be expected, there is a dependence of detection level on stellar magnitude, with median levels of 0.7 mmag for 8 < V < 9, 1.0 mmag for 9 < V < 10, 1.3 mmag for 10 < V < 11, and 2.3 mmag for V>11. The brightest stars we could detect variability for are the known pulsators 12 and 16 Lac, the faint end lies at V=12.1, which is however more of a limitation in the availability of spectral classification (the major historical star catalogues have a magnitude limit of V≈ 10) than of the KELT time series data.

To demonstrate how this work can be applied in the context of new and upcoming data from the NASA TESS mission, Fig. <ref> shows the frequency spectrum of a typical and arbitrarily-chosen star from this work, with the upper panel displaying the spectrum computed from KELT data, and the lower panels showing the results from TESS 2-minute cadence data. The two significant frequencies identified in this work from the KELT data are indicated with red triangles. These are also the most significant frequencies in the TESS data. Additional significant frequencies found in the TESS data are indicated with red tick marks. The lower-most panel zooms in on these peaks. A comprehensive analysis of available TESS data for the stars in our sample is beyond the scope of this work.










 §.§ Interesting Systems
 
During the process of manual inspection for each new and candidate systems, a number of systems show interesting features in addition to the periodic photometric signals characteristic of stars. Here we identify and briefly discuss these cases. 



  §.§.§ Eclipsing Binaries
 

Approximately two thirds of all stars with spectral types that would put them into the domain are located in binary systems <cit.>. Therefore it can be expected that some of our targets show eclipses. Indeed, we found five objects that can confidently be classified as eclipsing binaries; others may also have binary-induced light variations and are mentioned in Appendix A. We show phase-folded light curves of the pulsation-removed light curves of the eclipsing binaries in Fig. <ref>. We give ephemerides for the times of primary minimum in Table <ref>, in the form

min_I=T_0+E*P_orb

It should be pointed out that we classified only the first three stars in Table <ref> as definite pulsators; V447 Cep is among the candidates and HD 254346 among the rejected stars (see discussion in Sect. A.3).







lcr
1
Ephemerides of the eclipsing binaries containing a or candidate star. Error estimates are given in parentheses after the last significant digit.
0pt

ID     P_ orb     T_0

      (d)     (HJD)

TIC 10891640 = HD 339003     6.1636(1)     2456003.90(1)

TIC 42365645 = HD 227977     1.50626(1)     2456001.131(6)

TIC 451932686 = HD 344880     54.494(2)     2456050.2(1)

TIC 335484090 = V447 Cep     7.4976(7)     2456006.06(2)

TIC 426520557 = HD 254346     5.4319(3)     2456002.15(4)




Inspecting Fig. <ref>, one notices a reflection effect in the light curve of HD 339003 in addition to the total eclipses. Given this light curve, the companion star must be of grossly different surface temperature and smaller than the pulsator. This means that it could either be an evolved star or belongs to the recently proposed class of binaries by <cit.>, containing a hotter main sequence star and a cooler pre-main sequence companion. HD 227977 is the shortest-period eclipsing system we have discovered. There is some evidence for geometrical (ellipsoidal) distortion of the primary. The star also has a rich pulsation spectrum which is discussed in Sect. <ref>. HD 344880, on the other hand, is the longest-period system detected. Its orbit is obviously eccentric; secondary eclipse lasts approximately four times as long as primary eclipse. At V=7.46, V447 Cep is the brightest new eclipsing system in our sample. The light curve appears to have a short phase of totality. Finally, HD 254346 also shows some evidence for a reflection effect, suggesting the presence of a secondary similar to that of HD 339003. Follow-up observations of all these stars are underway.



  §.§.§ Stillstand Phenomenon
 
Some stars show the “stillstand phenomenon,” where the phased light curve shows a marked departure from a pure sinusoid. This rare phenomenon was first observed in a star in BW Vul <cit.>. As the brightness is increasing, the brightness stalls for some time, and then continues to increase towards its maximum value <cit.>. The ensuing decrease in brightness is relatively steep. Hydrodynamic models of BW Vul suggest that shocks generated below the photosphere can give rise to the stillstand phenomenon <cit.>. 

Only a handful of stars have been found to exhibit the stillstand phenomenon to date <cit.>. Of the four stars in the present sample that show the stillstand phenomenon, three have been previously reported as stars that have this characteristic (BW Vul, HD 173006, HD 180642). The fourth, HD 231124, is identified here for the first time, having been so far not known to pulsate. Light curves for these four stars are shown in Fig. <ref>, and they are marked in Table <ref>. 






  §.§.§ Other Non-sinusoidal and Unusual Behavior
 


Besides the four systems showing the stillstand phenomenon, there are two stars and three candidates with unusual or non-sinusoidal behavior that we briefly discuss below. These are shown in Fig. <ref>.

In the course of the discovery of pulsations in KK Vel, <cit.> noticed the non-sinusoidal light curve. <cit.> verified the presence of an additional frequency at twice the primary frequency, noticing differences in the color behavior between these frequencies. The primary frequency of KK Vel is somewhat variable. This was already pointed out by <cit.> who could not phase his three seasons of data (with photometry from 1980 to 1982) with a single frequency. He reported the main frequency to vary between f=4.6351±0.0001 and f=4.6361±0.0001 . <cit.> finds f=4.63637 ± 0.00003  d^-1 with observations in March 1987 and March 1988 with Walraven five-color observations, and November 22 1988 – January 25, 1989. Also in this work, we see evidence for a variable main pulsation frequency - and its amplitude. In the 2009/2010 observing season, the frequency was f=4.6342±0.0002  d^-1 with an amplitude of A=13.1±0.2 mmag, in 2012/13 f=4.63717±0.00004  d^-1 and A=21.2±0.4 mmag, and in 2013/14 f=4.63760±0.00004  d^-1, A=16.6±0.4 mmag. The amplitude and frequency variations are likely present on time scales shorter than a single observing season. Unfortunately, our data and the previous data are too sparsely sampled in time to facilitate a deeper analysis, although TESS observations may prove valuable in this regard. 




We have classified BD+35 4258 as a star. Apart from the single pulsation frequency (at P = 0.13174 d), the shape of the light curve suggests binary-induced or rotational variability with a base period of 0.67834 d (Fig. <ref>, top right), which appears rather short for an early B-type star. Vilnius photometry <cit.> and its calibration <cit.> indicates T_ eff≈ 26000 K, log g ≈ 3.9. From the Gaia DR2 parallax and Galactic reddening one can estimate M_v<-3.6. With bolometric corrections and the spectral type-temperature calibration by <cit.> one derives M_bol<-6.2, hence R>7.6 R_ for the star. A rotational modulation with a period of 0.67834 d hence requires v_rot>560 , which is close to breakup speed. Estimating a mass of 13 M_ for BD+35 4258 by placing it into a theoretical HR Diagram <cit.> and assuming a binary scenario with a massless companion and an orbital period of 0.67834 d requires a semimajor axis of R=7.6 R_, which is similar to the primary's radius. Alternative hypotheses would be SPB-type pulsation with a non-sinusoidal light curve <cit.> or a base period twice as long. Another possible scenario is that this signal arises from a close binary system with an orbital period of 0.67834 d which is not spatially resolved with respect to the B-type star in which we detect the pulsation. The light curve shape and period is suggestive of a close binary where both stellar surfaces are gravitationally deformed (i.e. an ellipsoidal variable).

The remaining stars discussed in this section are all classified as candidate pulsators. The light curve of HD 237204 (Fig. <ref>, middle left) can be decomposed into two frequencies related exactly by 2:3, suggesting binary-induced or rotational variability with a base period of 0.27172 d (Fig. <ref> middle left). Similar to the previously discussed star one can estimate T_ eff≈ 29000 K, M_v<-3.2 from Vilnius photometry <cit.> and the Gaia DR2 parallax. The bolometric corrections and the spectral type-temperature calibration by <cit.> then yields M_bol<-6.0, hence R>5.6 R_ for HD 237204. A rotational modulation with a 0.27172 d period thus requires v_rot>1000 , far above breakup speed. Estimating a mass of 15 M_ for HD 237204 in a possible binary scenario with a massless companion and an orbital period of 0.27172 d requires a semimajor axis of R=4.3 R_, smaller than the primary's radius. For these reasons we favor an interpretation in terms of pulsation, although the light curve shape with a descending branch steeper than the rising branch would be remarkable in this case.

ALS 1302 has two variability frequencies that are harmonically related and give rise to a light curve shape (Fig. <ref>, middle right) reminiscent of rotational or binary-induced variation. However, the base period (P=0.33514 d) would again be too short for such explanations. We appear to be left with an interpretation in terms of pulsation with an unusual light curve shape (e.g., see Fig. 6 of ).

The light curve of HD 339483 (Fig. <ref> bottom left) when phase-folded with respect to the strongest variability signal shows an unusual double-humped maximum. Just as for HD 237204, the short period of this signal (P=0.26852 d) effectively rules out a binary or rotational origin. The observation that the rising branch of the phase-folded light curve is steeper than the descending branch suggests that pulsation could be responsible for this variability; perhaps we are seeing a stillstand phenomenon shortly before light maximum, or a curious superposition of a base and a harmonic frequency (e.g., Fig. 1 by ). Although HD 339483 is classified as a classical Be star <cit.>, it is not clear that there is evidence to support this designation. None of the spectra that are published in the literature or are publicly available show evidence of the circumstellar disk characteristic of classical Be stars. This includes five optical spectra in the Be Star Spectra (BeSS) database[http://basebe.obspm.fr] that span the dates 2015 September 05 through 2018 September 12, five optical spectra with one observation taken 1998 August 3 and the next four taken between 2009 September and 2010 November <cit.>, an optical spectrum taken 1998 August 2 <cit.>, a K-band spectrum taken 1996 June 28 <cit.>, and an H-band spectrum taken 1996 June 29 <cit.>. There is, however, a somewhat nebulous feature that is readily apparent in the far-IR WISE W4-band photometry in the vicinity of this object <cit.> that may be responsible for the excess at long wavelengths. This star is classified as a star in <cit.>, and while they find the same frequency with ASAS and Hipparcos data as we find in the KELT data, the unusual shape of the phased data is not reported. 




  §.§.§ Stars with Frequency Splittings
 

stars often show nonradial pulsations. Stellar rotation introduces frequency splittings into the pulsation spectra, which can be used to determine their interior rotation <cit.>. Thus stars that show frequency splittings are highly interesting for asteroseismology, although it needs to be cautioned that such splittings may also occur by coincidence (see  for an example). We have examined the targets classified as stars for frequency splittings, keeping in mind that second-order effects of rotation make them somewhat uneven, in the sense that within a given pulsation mode multiplet the frequency separations of consecutive signals slightly decrease with increasing frequency <cit.>, and that some frequency multiplets may be incomplete. We found a total of 22 stars with frequency splittings (Fig. <ref>, Table <ref>) that could reveal their rotation rate. The splittings of two of those stars, IL Vel and V836 Cen, were already known; those of the 20 other stars are new discoveries and await confirmation and/or resolution of ambiguities via pulsational mode identification. Pinpointing possible rotational frequency splittings in this way is expected to be successful only in cases of slow to moderate rotation. For fast rotators (50% of breakup speed or more), the asymmetry of the rotationally split multiplets hampers their identification from the underlying frequency pattern only <cit.>.




lr  
2
Stars with detected frequency spacings and estimates of the first-order rotational splitting. For objects where several possible splittings were found, there is more than one solution.  
 
ID     Δ f 

      (d^-1)

TIC 5076425 = GSC 05124-02524      0.0895 or 0.1790

TIC 11696250 = HD 228699      0.068 or 0.136 or 0.273

TIC 25070410 = HD 166331      0.1500 or 0.2999

TIC 42365645 = HD 227977      0.0383 or 0.0484 or 0.0968 

TIC 65166720 = KP Per      0.025 or 0.049 or 0.098

TIC 93730538 = CD-49 3738      0.073 or 0.1388 or 0.146 or 0.291

TIC 101423289 = HD 86248      0.059 or 0.118

TIC 105517114 = HD 190336      0.070 or 0.140

TIC 159932751 = V836 Cen      0.0124

TIC 264613619 = V757 Per      0.0145

TIC 293680998 = IL Vel      0.0483

TIC 299821534 = HD 231124      0.221 or 0.443

TIC 308954763 = HD 232489      0.11 or 0.23

TIC 312626970 = HD 228461      0.114 or 0.227

TIC 312637783 = HD 228456      0.036 or 0.072

TIC 314833456 = BD+55 2899      0.0460

TIC 347486043 = HD 13338      0.0128 or 0.0257

TIC 348137274 = BD+56 477      0.0603 or 0.1206

TIC 348506748 = HD 14357      0.0865 or 0.1730

TIC 361324132 = HD 344894      0.079 or 0.159

TIC 393662110 = V372 Sge      0.0889 or 0.1779

TIC 461607866 = CD-44 4596       0.0346




Our results for V836 Cen deserve separate discussion. This star has been among the first to be successfully modeled asteroseismically <cit.>. <cit.> identified a radial oscillation, a rotationally split triplet of dipole modes and two components of a quadrupole mode. Our analysis adds two more components (one of which already tentatively reported by ) to the quadrupole mode quintuplet, of which four consecutive components are detected now (see Table in the Appendix). This reduces the previously four possibilities for which is the axisymmetric component of the quadrupole mode to two, and rules out the conjectured identification of this axisymmetric mode by <cit.>. Furthermore, the relative amplitudes of the oscillations in the two nonradial mode multiplets have changed in the ∼ two decades that lie between the two data sets. Also, whereas <cit.> find a first-order rotational splitting of 0.0121295 for the triplet of dipole modes, we obtain a slightly, but statistically significantly larger value of 0.01238±0.00002 . This suggests that the rotation rate in the resonant cavity of the dipole mode of V836 Cen has increased in the meantime, counter-intuitive to what would be expected from evolutionary stellar expansion.




  §.§.§ Galactic Distribution
 

Because stars are massive main sequence pulsators, they are relatively young stars. In most cases they should not have had the time to move away from the Galactic plane where they were formed. However, some interactions with other stars, such as a supernova disrupting a binary system <cit.> or ejection of a star from a young open cluster <cit.> are able to move a young star away from the Galactic plane. Given the interesting evolutionary histories such stars will have, they are of increased interest for asteroseismic investigations.

We have therefore computed the distance from the Galactic plane of our targets with parallaxes with a relative error below 25% and show the result with respect to Galactic longitude in Fig. <ref>; Table <ref> lists all stars that are located more than 400 pc off the Galactic plane. We also quote their radial velocities if available. Some of these stars have rather large radial velocities, adding evidence for a possible runaway nature.



lcr  
3
Stars located more than 400 pc away from the Galactic plane.  
 
ID     z     RV

      (kpc)     ()

3cstars

TIC 61516388 = HD 178987     -1.5±0.5     

TIC 251637508 = HD 186610     -0.8±0.2     +24.4 

TIC 308954763 = HD 232489     -0.5±0.1     -32.0 

TIC 349332755 = HD 160233     +0.42±0.04     +14.0 

TIC 392965683 = ALS 10332      -0.7±0.2     

3ccandidates

TIC 92193 = HD 130195      +1.3±0.2     

TIC  65516748 = HD 18100      -2.3±0.5     +76.0 

TIC 137489662 = HD 183535     +0.48±0.08     +14.0




We noticed that there are several stars that failed our criterion for the precision of their parallaxes, but that are rather faint (hence distant in any case) and that are located at relatively high Galactic latitude. These are therefore also good candidates for runaway stars. Among the pulsators, these are TIC 25070410 = HD 166331 (b=-14.1^o, RV=+33 ), TIC 101423289 = HD 86248 (b=-18.1^o, RV=+73 ), and TIC 287467101 = HD 140543 (b=-25.5^o); among the candidates, TIC 384540878 = CD-56 2603 (b=-6.6^o) stands out in this respect. Finally, we remark that V836 Cen (b=+20.2^o, RV=+66 ) has already been suspected to be far away from the Galactic plane <cit.>. There is no reliable and precise parallax for the star, but its luminosity has been derived asteroseismically <cit.>. Using these results and reddening estimates from <cit.> and Strömgren photometry, we find z≈430 pc for this star.




  §.§.§ Extreme Helium Stars
 

Extreme Helium stars are rare objects that are not main sequence B-type stars such as the pulsators. They are believed to be more likely the product of a merger of two white dwarfs than post-AGB objects that underwent a final Helium flash <cit.>. Nevertheless, two of these stars, V652 Her (a known pulsator) and HD 144941, survived the pre-selection criteria for pulsators or candidates.

HD 144941 was initially identified as having a tentative low-amplitude signal within the frequency range of the stars. However, further analysis suggests this detection was spurious. <cit.> have analyzed K2 photometry and find somewhat complex light variations with a period of 13.9 days and a full amplitude of 4 parts per thousand. This variability is attributed to rotation of an inhomogeneous surface. We do not recover this signal in the noisier KELT data. Further, the high-frequency signal that was tentatively detected in our original analysis (Table <ref>) is not found in the publicly available K2 data (within a limit of 40 μmag). The lack of pulsation in HD 144941, despite it lying in the instability strip, may be attributed to its low metallicity, as suggested by <cit.>, or the possible presence of a large organized magnetic field (which the implied surface inhomogeneities may be associated with) could act to suppress pulsation. 

V652 Her was readily detected in our analysis, but its dominating frequency is the first harmonic of the actual pulsation frequency due to the unusual light curve shape of this star <cit.>. Also, its rapid period change <cit.> is evident in our data that cannot be phased with a constant period. We show a comparison of the “instantaneous" period for our yearly data sets of V652 Her with the fit obtained by <cit.> to their earlier period measurements in Fig. <ref>. Given the ≈ 6-year gap between the latest measurements in this paper and the first ones in ours, the general trend of a decreasing pulsation period is still well preserved. However, systematic deviations are also visible, likely a consequence of the non-linear nature of the period change of this star.






§ DISCUSSION AND CONCLUSIONS
 
Through a periodicity analysis of light curves from the KELT survey for O- and B-type stars, we identify 113 pulsators, of which 89 are new discoveries. We identify a further 96 stars as candidates, a group that likely contains a mix of genuine stars, plus other O- and B-type variables. Additionally, we identify 27 stars that meet the pre-selection criteria, but are rejected upon a more scrupulous investigation. 

Our pre-selection was based on a visual inspection of the Fourier spectra of the KELT light curves. Based on our experience with these data, we derived some pre-selection criteria that can be used to facilitate more automatic identifications of pulsators and candidates from similar datasets. For stars to be pre-classified as pulsators, we required variability frequencies between 4 and 13 , a signal-to-noise ratio of the strongest signal in the amplitude spectrum to exceed 5, a light curve shape not indicative of binary-induced variability, and a spectral type between O9 and B5 (allowing for inaccurate spectral classifications). candidates would be stars not classified as that have to have frequencies between 3-15 , S/N>4 and spectral types O-B7. This pre-selection resulted in 148 identifications plus 90 candidates. 

The previously described criteria are necessary to be fulfilled, but not sufficient: after a careful literature search and taking into account their position in the HR Diagram, we had to reject seven stars (5%) pre-classified as stars as well as 18 candidates (20%; see Appendix A.3 for short discussions of each individual star). In addition, we moved 27 (18%) stars from to candidate status to err on the side of caution, but also “upgraded" three from candidate to because reliable spectral classifications not available in our input catalogue were found in the literature. Further, three stars selected as stars were found to be blended with a variable neighbor, and in all cases the neighbor is possibly of the correct spectral type and is so classified as a candidate. An additional three stars identified as candidates were rejected in this fashion. We conclude that a mistake-free selection of stars is not possible from analyzing light curves and spectral type information alone, but a reasonably clean sample for deeper investigation can be extracted using the criteria above. 

Among the 113 stars finally classified as , we found 22 (19%) with regular frequency spacings suggestive of rotational splitting of nonradial pulsation modes. In comparison, <cit.> detected only seven such stars in their total sample of 103 (i.e., 7%). This is probably a consequence of the lower noise level in our data, only about one third of that by <cit.>. The average number of pulsation modes detected per star is 3.14 in our data, whereas it is 1.93 in the work by <cit.>. On the other hand, the number of eclipsing binaries amongst the pulsators is three in this work and four in <cit.>. It is somewhat unfortunate that there is not yet a pulsator with more than three oscillation modes that is part of an eclipsing SB2 system.

Aside from the eclipsing binaries, we found some unusual light curve shapes for some of the pulsators. Whereas some of them can be associated with the stillstand phenomenon, others are more difficult to explain. The shapes of some of these light curves phenomenologically resemble those of close binary stars, but the associated periods are too short to be explained that way. Time-resolved spectroscopy of these objects would be valuable to understand their true nature.

Some of the pulsating stars or candidates reported here are located at rather large distances from the Galactic plane and are therefore candidate runaway stars. This is interesting both from the stellar evolutionary and asteroseismic point of view because the flight time of a runaway star provides a limit on the stellar age that can be imposed on seismic models <cit.>. Having such a constraint at hand could be of similar importance as basic stellar parameters from pulsators in eclipsing binaries.

These new discoveries (about a 70% increase over the currently known sample), plus previously known stars, will be targeted by the TESS mission. The high-quality TESS light curves will then be used to perform asteroseismic studies on this population, which will reveal valuable information about the interior structure and evolution of massive stars.




p2.5cmlcrcccccccccc 

4
Stars   
 
ID     TIC     Freq.        Amp.       num.       RA (2000)     Dec (2000)     V         SP     known?     cluster?     Rem.  

       ID      (d^-1)     (mmag)      modes                                  (mag)                                       
 
GSC 05124-02524     5076425     5.6387     36.3     4     18 35 53.63     -07 09 53.6     11.91     B3             M 

HD 339003     10891640     6.7997     12.7     2     19 51 02.86     +25 57 15.4     9.93     B0.5III             M 

HD 228699     11696250     7.5964     2.7     6     20 16 36.74     +37 41 12.8     9.46     B0.5III         IC 4996     M 

HD 228690     11698190     5.8721     9.3     4     20 16 29.22     +37 55 21.2     9.29     B0.5V             A 

HD 229085     13332837     6.8744     5.5     3     20 21 35.13     +38 36 47.8     9.8     B0V         NGC 6913      

HD 194205     13967727     4.4455     11.5     2     20 23 01.50     +39 20 40.5     9.08     B2III             A 

HD 166331     25070410     7.4476     12.6     6     18 09 50.41     +10 46 26.5     9.39     B1.5III             A, M  

CD-44 4876     29123576     7.7826     16.9     2     08 50 16.09     -45 23 02.5     10.94     B3/5             A 

CD-45 4663     29585482     8.0717     5.5     1     08 52 29.74     -45 37 03.9     11.31     B1/4              

KK Vel     31921921     4.6373     14.8     1     09 07 42.52     -44 37 56.8     6.78     B1.5II     SH05         M 

HD 227728     41327931     8.9711     1.2     2     20 06 49.54     +38 01 39.4     9.91     B2V              

HD 227977     42365645     7.8305     20.1     9     20 09 17.22     +37 30 07.9     9.68     B2III             A, M 

HD 228101     42940133     6.2998     4.1     6     20 10 36.69     +37 27 30.6     8.49     B1IV             A 

HD 228290     43881045     7.1226     7.5     1     20 12 20.66     +38 00 07.6     9.47     B1II              

HD 171305     44980675     5.1586     8.3     2     18 34 15.85     -04 48 48.8     8.72     B3III     PP08         A 

HD 253021     45799839     7.5753     3.7     2     06 11 42.41     +21 37 58.7     10.16     B2              

ALS 10035     55702566     6.5490     6.3     4     18 53 57.85     -03 48 49.0     11.4     B0.5III             A 

HD 178987     61516388     7.1466     7.6     2     19 12 59.64     -47 09 39.5     9.83     B2II     PP08         A, M 

KP Per     65166720     4.9558     15.5†    5     03 32 38.98     +44 51 20.7     6.41     B2IV     SH05         A, M 

HD 80279     75745359     7.2591     3.1     2     09 17 14.93     -46 16 30.2     9.45     B3II/III             A 

ALS 8706     80897625     4.4060     4.6     2     06 06 28.15     +27 18 32.3     11.68     B1IIIe             A 

TYC 2682-73-1     89756665     8.4179     3.8     2     20 05 57.78     +35 57 13.7     10.09     B1Vn              

HD 74339     93723398     5.2201     25.1     5     08 41 32.97     -48 01 30.7     9.38     B2III     PP08     IC 2395     A 

CD-49 3738     93730538     5.4451     7.2     5     08 41 38.55     -49 35 52.9     9.69     B3             M 

HD 86248     101423289     7.4897     6.2     6     09 56 33.26     -31 26 31.0     9.56     B3II     PP08         M 

HD 190336     105517114     4.4571     21.7     6     20 03 18.68     +33 26 59.7     8.62     B0.7II-III     JSH09         M 

HD 61193     123211175     7.1893     0.7     1     07 36 14.33     -42 04 56.2     8.2     B2Vn              

12 Lac     128821888     5.1789     7.6†    4     22 41 28.65     +40 13 31.6     5.22     B2III     SH05         A 

16 Lac     129538133     5.8503     4.4†    3     22 56 23.63     +41 36 13.9     5.58     B2IV     SH05         A 

HD 73568     141292310     4.5453     3.9     4     08 37 19.48     -45 12 26.0     8.36     B2III/IV     PP08         A 

V836 Cen     159932751     6.9661     8.2†    8     14 46 25.76     -37 13 20.1     8.05     B3V     SH05         A, M 

HD 225884     168996597     5.8220     2.9     5     19 48 15.12     +37 21 59.2     9.43     B5             A 

HD 180642     175760664     5.4869     28†    1     19 17 14.80     +01 03 33.9     8.29     B1.5II     SH05         A 

ALS 10186     180952390     6.6275     6.9     2     19 10 27.87     +02 07 32.3     11.67     B0.5V              

BD-02 4752     182714198     6.9779     7.0     2     18 49 25.06     -02 21 09.8     10.48     B0.5V             A 

HD 173006     184874234     5.8779     35.1     1     18 43 26.26     -05 46 47.7     10.06     B0.5IV     PP08         A, M 

HD 73918     185476952     8.2949     2     5     08 39 53.96     -30 29 59.9     9.7     B5III              

HD 33308     187483462     6.7355     0.9     1     05 11 07.96     +37 18 06.8     8.78     B3              

HD 172367     197332002     4.6882     8.5     2     18 40 09.71     -07 15 02.0     9.54     B2III             A 

HD 332408     216976987     6.7778     2.5     1     19 42 07.98     +28 59 45.6     8.94     B2IV             A 

ALS 9955     225687900     5.4431     23.9     2     18 45 34.43     -05 21 59.0     11.02     B1.5II             blend 

BD+35 4258     232846315     7.5905     2.9     1     20 46 12.66     +35 32 25.6     9.46     B0.5Vn             M 

HD 48553     234068267     5.5980     9.8     3     06 44 09.94     +02 23 29.6     9.08     B3     PP08          

HD 49330     234230792     10.8591     1.7     2     06 47 57.27     +00 46 34.0     8.95     B0nnep     H09         A 

BD+57 614     245719692     6.9250     2.4     2     02 42 19.47     +58 05 30.0     10.69     B2III             A 

BD+57 655     251196433     6.3730     6.5     3     02 53 28.41     +58 19 32.9     10.12     B2III         IC 1848      

ALS 7546     251250184     4.1204     16.3     5     02 55 36.68     +59 24 40.1     10.52     B3III         IC 1848      

ALS 7541     251250634     12.2005     1.9     2     02 54 57.47     +59 15 57.6     10.71     B2II         IC 1848      

HD 186610     251637508     5.4999     15.4     5     19 45 27.32     -03 09 06.6     9.7     B3n     PP08         M 

ALS 6426     255974332     4.8242     10.7     5     00 59 49.44     +64 39 37.4     10.99     B2III             A 

BD+56 488     264612228     6.2736     5.3     4     02 18 13.52     +57 21 30.9     10.1     B         NGC 869     M 

V611 Per     264613043     5.8246     3.2     1     02 18 29.83     +57 09 03.1     9.35     B0.5I/V     SH05     NGC 869     A 

V757 Per     264613619     4.0769     7.9     7     02 18 23.05     +57 00 36.7     8.43     B0.5III         NGC 869     A, M 

HD 14014     264615882     4.8970     6.3     6     02 18 00.02     +56 13 57.3     8.86     B0.5V              

V665 Per     264731122     4.1275     20.4     5     02 18 48.02     +57 17 07.9     9.38     B2V     SH05     NGC 869      

HD 232874     266338052     5.7400     5.6     3     04 02 15.74     +53 45 11.8     8.92     B2III             A 

ALS 12866     269228628     4.9919     44.6     3     23 17 13.70     +60 00 27.9     10.9     B0.5V             blend 

ALS 13180     272922818     8.0279     35     1     23 47 51.68     +61 05 45.9     11     B0III              

HD 345370     279236955     8.0541     18.8     4     19 56 58.66     +21 19 49.7     9.75     B2III              

BD+68 1373     279659875     5.8301     3.8     2     23 22 50.65     +69 00 34.7     9.14     B2III             A 

HD 343642     282529703     7.5007     11.2     2     19 01 46.01     +22 34 17.8     10.42     B3              

ALS 6392     283136444     7.9518     13.5     1     00 53 35.57     +60 47 08.7     10.32     B2IVnn              

HD 140543     287467101     5.6086     2.0     1     15 44 56.66     -21 48 53.9     8.88     B0.5IIIn             A, M 

HD 339039     287690192     8.2695     9.5     5     19 48 46.69     +24 48 21.0     9.69     B1.5V             A 

IL Vel     293680998     5.4598     28.7     4     09 17 31.15     -52 50 19.5     9.16     B2III     SH05         A, M 

HD 81370     295435513     7.7088     10.1     2     09 23 17.73     -52 44 52.3     8.81     B0.5IVn              

HD 298411     296570221     6.0909     5.4     5     09 26 27.12     -52 09 33.0     10.53     B2/5             blend 

HD 199021     297259536     11.3847     2.2     3     20 52 53.21     +42 36 27.9     8.49     B1IV             A 

HD 231124     299821534     4.5432     30.9     4     19 18 52.34     +14 19 41.0     11.1     B2III             A, M 

HD 232489     308954763     5.3769     7.5     7     01 39 12.85     +51 49 19.1     9.26     B5             A, M 

HD 228365     311943795     8.2886     4.8     4     20 13 01.17     +41 01 42.1     9.97     B1V             A 

HD 228461     312626970     4.7912     8.5     6     20 14 06.42     +38 14 38.4     9.56     B2II             M 

HD 228463     312630206     6.0847     17.3     12     20 14 03.30     +37 45 30.1     9.6     B1V             A 

HD 228456     312637783     8.1827     5.5     6     20 14 02.31     +36 48 07.0     10.2     B2IV             M 

HD 228450     312639883     5.9532     4.7     5     20 13 59.02     +36 32 37.9     9.24     B0.5p             blend 

BD+55 2899     314833456     4.1698     20.4     9     23 07 08.78     +56 00 21.1     10.29     B1IIIp             M 

HD 236664     331782797     7.9873     33.9     1     01 13 41.79     +59 05 57.4     10.05     B0.5V             

ALS 12345     337105253     5.9461     15.9     2     22 21 51.49     +60 17 09.7     10.43     B3V              

BD+64 1677     338076483     4.7785     2.8     2     22 31 13.58     +65 27 58.5     9     B2III-IV             A 

HD 13338     347486043     4.6360     6.3     4     02 12 19.17     +57 56 27.1     9.17     B1III             A, M 

BD+54 490     347684339     5.8959     3.5     2     02 14 20.11     +55 03 33.6     9.53     B1V              

BD+56 477     348137274     6.3488     6.1     3     02 17 04.49     +56 58 07.2     10.02     B         NGC 869     M 

BD+56 537A     348231245     6.8061     2.3     1     02 19 39.13     +57 16 13.2     10.34     B2V         NGC 869     blend 

BD+56 540     348232246     7.7903     3.2     1     02 19 42.66     +56 58 45.8     10.28     B0.6V         NGC 869     blend 

BD+56 560     348443241     5.1899     4.4     1     02 21 32.75     +57 34 07.1     10.24     B2III         NGC 884     A 

HD 14357     348506748     4.6030     2.5     6     02 21 10.44     +56 51 56.4     8.52     B2II/III         NGC 884     A, M 

BD+56 584     348607991     4.5816     3.8     3     02 22 29.86     +57 12 28.8     9.61     B0.7I     S13     NGC 884      

ALS 7146     348668924     5.5486     6.2     2     02 23 14.38     +58 09 49.5     10.56     B1V              

NGC 884 2579     348671634     4.4147     3.9     2     02 22 50.28     +57 08 50.7     11.91     B3e     S13     NGC 884      

HD 160233     349332755     7.6411     4.1     1     17 38 40.64     +04 20 09.8     9.04     B2IV/V             M 

HD 174298     357853776     10.2571     5.3     1     18 48 55.63     +24 03 21.1     6.53     B1.5IV     KE02          

HD 344775     360063836     5.1399     7.4     6     19 43 09.76     +23 26 15.7     10.36     B1III         NGC 6823     A 

HD 344894     361324132     6.5681     9.5     8     19 45 48.21     +23 11 42.7     9.61     B2IIIn             A, M 

BD+58 241     370128780     4.8896     1.6     1     01 27 54.88     +59 14 08.9     9.91     B1V             A 

V1143 Cas     372724051     5.2636     19.8     3     01 43 35.58     +64 02 06.8     10.86     B1     HM11     NGC 637     A 

BD+60 416     374038418     5.7341     1.6     1     02 01 44.21     +61 03 13.0     9.61     B0.5III              

HD 350202     377088966     4.2299     9.5     3     19 38 41.60     +20 07 46.8     10.3     B1.5III              

HD 344842     378429048     6.5255     6.3     1     19 41 44.28     +21 29 03.5     9.78     B2III              

BD+62 258A     389532846     4.3293     8.3     2     01 30 06.14     +63 34 57.2     10.32     B1IV              

ALS 10538     391082033     9.3965     24.3     1     19 48 53.68     +19 58 07.0     11.33     B1V              

HD 30209     391836737     6.1933     12.2     2     04 47 30.26     +42 19 11.8     8.39     B1.5V             A 

ALS 10332     392965683     6.0443     12.9     3     19 33 11.45     +01 56 44.2     12.07     B2             M 

V372 Sge     393662110     6.0859     17.5     6     20 09 39.59     +21 04 43.6     8.34     B0.5IIIe     H05         A, M 

NGC 663 4     399436828     5.1536     5.6†    1     01 46 39.00     +61 14 06.1     11.06     B5     SH05     NGC 663     A, blend 

CD-47 4562     400852783     6.8803     8.6     3     08 58 23.73     -48 11 08.7     10.9     B5V              

BW Vul     419354107     4.9741     27.6†    2     20 54 22.40     +28 31 19.2     6.54     B2III     SH05         A, M 

ALS 6331     421117635     5.2183     4.5     2     00 45 35.06     +63 21 07.4     10.55     B0.5V              

HD 14645     445619007     5.2131     1.7     1     02 24 01.13     +58 19 25.9     9.43     B0IVnn             A 

HD 344880     451932686     9.4929     1.3     1     19 45 42.31     +23 59 04.0     9.34     B0.5IIInn         Roslund 2     A, M 

HD 338862     452018494     8.6542     4.0     1     19 46 18.34     +27 27 37.4     9.92     B2V              

CD-44 4596     461607866     6.6530     5.6     7     08 36 59.62     -45 17 23.1     9.3     B1III             M 

HD 86214     469221047     4.4426     12.4     2     09 54 58.43     -59 49 46.7     9.21     B1III     PP08     NGC 3114     A 

HD 86162     469223889     7.8416     1.1     3     09 54 47.75     -59 16 03.3     9.21     B01/IV             A 

Table of stars identified in this work, including the ID, TESS Input Catalog (TIC) number, information about the primary frequency and number of modes, coordinates, V-band magnitude, and spectral type, a citation if the star is known to be a star, a note if the star is a known cluster member, and information about remarks. Stars labeled “M" in this column are discussed in the main paper text, stars labeled “A" are commented upon in the Appendix, while “blend” indicates at there are bright nearby sources contributing flux in the aperture used by KELT (and likewise with TESS). The citations for known stars are as follows: SH05 = <cit.>, H05 = <cit.>, PP08 = <cit.>, H09 = <cit.>, JSH09 = <cit.>, HM11 = <cit.>, S13 = <cit.>. †Amplitudes may be largely suppressed. 


p2.5cmlcrcccccccccc 

5
Candidate Stars  
 
ID     TIC     Freq.        Amp.       num.       RA (2000)     Dec (2000)     V         SP     known?     cluster?     Rem.  

       ID      (d^-1)     (mmag)      modes                                  (mag)                                       
 
HD 130195     92193     5.9765     1.6     1     14 47 31.92     -24 12 05.2     10.66     B6II             M

TYC 4032-93-1     11158867     12.9147     2.0     1     01 58 38.10     +60 05 55.7     10.68     B3             A 

TYC 3151-109-1     12249117     3.2891     3.0     1     20 17 43.65     +39 20 36.2     11.02     B5V             

ALS 7011     12647534     3.5118     5.7     1     02 15 24.53     +60 08 21.4     10.63     B0III         IC 1805     A

TYC 4050-1949-1     13839931     4.9542     3.9     1     02 30 19.98     +63 00 23.4     11.21     B7V         IC 1805     

TYC 3152-1307-1     13971092     9.6946     1.8     1     20 23 06.70     +38 49 15.6     10.62     B5         NGC 6913     A

HD 229171     13973539     3.5030     9.8     2     20 23 02.88     +38 27 20.8     9.38     B0.5IIIne         NGC 6913     A 

CD-44 4871     28949811     13.127     1.2     1     08 50 09.76     -44 37 22.5     10.44     B1/3V             A

CD-46 4639     29036690     7.9231     0.7     1     08 49 39.68     -46 50 53.2     10.05     B3He             A

HD 76307     29598925     4.0110     4.9     1     08 53 28.33     -47 31 07.6     9.27     B2/3V             A 

HD 76967     30569481     5.5781     5.2     2     08 57 54.00     -43 09 12.7     9.07     B3/5V             A 

HD 192003     43301361     8.8495     3.0     2     20 11 16.85     +38 13 48.0     8.85     B2IV             A 

ALS 7310     49721269     11.6465     1.3     2     02 33 43.00     +61 26 12.2     10.89     B2III         IC 1805     blend 

TYC 4030-800-1     53709049     6.6171     7.3     2     01 11 12.15     +61 06 06.2     11.96     B5             A 

BD+60 185     53961302     9.3790     1.5     1     01 13 05.69     +61 24 44.9     10.07     B7V             

BD+60 192     53968977     6.0136     9.5     1     01 14 30.29     +60 53 28.8     9.39     B5             A

HD 59259     60245596     6.4427     1.5     2     07 27 03.03     -44 10 40.2     9.95     B7/8V             

HD 18100     65516748     8.5481     1.6     1     02 53 40.81     -26 09 20.4     8.44     B5II/III             M 

HD 237204     72696935     7.3604     13.1     1     04 00 23.28     +56 54 05.7     9.18     B2III             M 

ALS 7879     72944678     3.3264     10.4     1     04 05 03.97     +56 13 06.3     11.79     B0p             

CD-45 4896     74197071     2.9677     4.7     3     09 08 50.23     -46 25 58.9     10.75     B7IV             A

HD 249179     78499882     3.7216     2.8     1     05 55 55.05     +28 47 06.4     10     B5ne             A

HD 67980     80814494     5.4045     2.3     1     08 08 44.04     -42 37 07.6     10.53     B7II             A

HD 74533     93923487     3.4462     1.2     1     08 42 28.52     -49 45 53.1     9.17     B5IV             

HD 74581     94000461     4.5450     15.1     1     08 42 47.92     -48 13 31.1     9.12     B6/8V         IC 2395     A 

HD 248434     114249288     3.1336     4.0     1     05 51 38.52     +21 32 28.1     10.68     B5ne             

HD 60794     123036723     4.7814     4.3     1     07 34 06.86     -46 38 37.7     8.73     B3/5IIIe             

HD 62894     123828144     5.5254     1.0     1     07 44 15.56     -43 01 04.2     9.6     B7/9e             A 

HD 183535     137489662     11.5196     1.6     1     19 28 38.16     +36 46 45.1     8.64     B5             A, M 

CD-44 4484     140309502     7.1391     3.2     1     08 30 53.51     -44 58 33.2     9.76     B5             A 

HD 72090     140429699     6.1756     1.6     1     08 28 52.24     -48 11 25.6     7.84     B6V             

CD-44 4571     141190209     4.7460     1.5     1     08 35 52.40     -44 39 23.5     10.88     B5V             

CD-46 4437     141903641     5.2911     5.8†    2     08 40 35.29     -47 14 08.4     10.24     —             A 
 
HD 279639     143530557     3.2317     4.1     3     04 18 03.37     +38 57 47.0     11.06     B7             A

CPD-52 1713     145672806     3.1628     1.8     1     08 51 15.55     -53 27 03.0     11.3     B7e             A 

HD 29332     155977294     4.4491     1.5     1     04 39 04.89     +41 15 00.0     8.71     B3ne             

TYC 2682-3173-1     172560369     8.9049     2.4     1     19 58 39.75     +37 00 23.3     11.72     B5             

CD-40 4269     184226481     3.7008     4.4     1     08 27 31.64     -41 24 48.4     10.35     B1/3             

HD 76554     190783321     15.5906     1.0     3     08 55 25.94     -41 04 43.9     8.33     B2Vne             A

BD+41 3731     193573033     3.5563     2.8     1     20 24 15.72     +42 18 01.4     9.84     B2/3ne         NGC 6910     

BD+41 3736     193608395     6.9397     2.6     2     20 24 33.90     +42 14 15.5     10.55     B6         NGC 6910     

HD 258853     207045768     6.1398     2.5     1     06 31 14.87     +09 47 25.0     8.83     B3Vnn             A

HD 261172     220238856     3.7193     11.3     3     06 38 31.56     +09 25 12.2     10.1     B2III         NGC 2264     

HD 261589     220298408     6.0890     5.1     1     06 39 44.90     +06 27 35.6     11.43     B7         NGC 2244     

ALS 9974     226144867     12.676     6.4     1     18 47 15.69     -05 00 57.5     12.21     B1V             

TYC 746-578-1     231149746     9.0529     2.9     2     06 41 53.08     +08 24 17.7     11.68     B6/9             A

HD 262595     231177417     5.9053     5.9     1     06 43 06.31     +07 36 03.8     11.19     B3/5             

TYC 750-467-1     231236273     9.6644     2.3     1     06 44 16.00     +10 28 11.8     11.26     B6/9         NGC 2264     

HD 339483     244327575     3.7241     17.8     1     20 04 00.75     +26 16 16.8     8.98     B1IIIe     KE02         M 

TYC 3324-92-1     252864874     5.3848     7.1     3     03 26 04.74     +50 49 46.6     11.33     B7         Melotte 20     A

BD+61 2515     272625912     3.3052     11.6     1     23 45 43.89     +62 17 31.2     10     B0.5V             

GSC 00155-00374     281533292     5.5399     7.9     1     06 38 13.40     +05 33 20.0     11.9     B7V         NGC 2244     

HD 333172     282737511     3.2152     6.9     1     19 57 53.88     +28 19 51.2     10.35     B1II             

ALS 14570     285122116     7.9203     1.1     1     00 49 11.38     +64 11 21.9     11.28     B3IV             

ALS 6915     285684866     3.0730     7.1     1     02 06 08.56     +63 22 11.8     10.24     B0.5:ep             

HD 69824     286352720     6.0635     3.6     2     08 16 38.69     -48 26 11.2     9.09     B4/6V     PP08         

HD 78507     290300414     4.3680     0.9     2     09 05 39.03     -62 06 12.6     8.12     B6V             A

GSC 01314-00792     294306184     7.2264     5.4     1     06 12 02.90     +15 23 10.0     11.5     B5             

ALS 1302     296449179     5.9676     8.6     1     09 25 42.12     -53 14 19.5     11.73     B3             M 

ALS 11602     297264447     8.7851     1.3     1     20 53 04.97     +43 37 13.2     11.21     B2Vn             

HD 260858     307944768     5.8902     1.2     1     06 37 46.71     +12 46 05.1     9.15     B6He             A

HD 220300     319302209     3.3830     8.7     1     23 22 10.46     +56 20 53.6     7.93     B6IVne             A 

V447 Cep     335484090     3.1845     18.1     1     22 10 59.56     +63 23 58.5     7.46     B1Vk             A, M 

BD+05 4404     345652701     3.1828     2.4     1     20 04 42.72     +05 33 19.6     10.47     B5             

V352 Per     347585038     3.6438     2.9     1     02 13 37.02     +56 34 14.3     9.31     B1III             A 

BD+56 579     348609224     3.9560     1.5     1     02 22 19.23     +57 37 12.9     10.88     B7IVe             A 

LS II +23 36     360749347     4.8883     11.8†    1     19 44 26.15     +23 17 54.1     10.68     OB             A 
 
CD-49 4294     364146227     3.0901     5.7     1     09 18 19.05     -50 18 46.9     11.24     B3/5             

ALS 6216     366108295     12.9568     2.0     1     00 28 37.71     +62 29 17.7     10.2     B0.5V             A 

BD+66 1651     368237682     7.2884     1.8     2     23 52 12.14     +67 10 07.5     9.97     B3Ve             A

HD 261630     369708912     3.2593     2.6     1     06 39 49.73     +05 04 37.7     10.07     B5         NGC 2244     

BD+55 334     370269139     5.9102     1.5     1     01 28 39.05     +56 21 04.3     10.41     B2e             A 

BD+57 579     372115570     3.9621     4.0     1     02 30 14.05     +57 40 30.3     10.09     B2III             A 

HD 236939     374696382     5.7791     3.6     1     02 04 33.68     +56 33 00.6     10.19     B5             

BD+29 3644     379932247     8.3034     2.4     1     19 33 49.91     +29 29 56.3     11.27     B5             blend 

HD 78206     384257658     3.6997     1.8     2     09 04 22.00     -59 09 24.9     8.84     B7/8V             A

CD-56 2603     384540878     3.5513     3.6     1     09 05 41.99     -57 00 02.9     11.76     B1III/Ve             M 

CPD-55 2071     386513392     3.1218     1.6     1     09 18 11.17     -56 01 33.3     10.8     B7e             

HD 42896     386693012     13.597     7.3     3     06 14 06.19     +20 10 10.9     8.62     B1Vnn             A

BD-09 4742     387153140     11.3216     2.1     2     18 28 20.13     -09 35 05.2     10.5     B2V             A

CD-47 4494     400080677     9.0207     0.6     1     08 54 20.85     -48 25 49.5     9.69     B5             

TYC 3683-1328-1     400533469     11.1849     4.5     1     01 39 47.92     +58 45 24.4     11.68     B5             

CD-48 4390     401847213     5.1564     4.9     1     09 04 23.69     -48 46 25.1     11.32     B4/6             

HD 280753     408941991     4.6168     1.4     1     05 18 05.96     +38 17 40.6     10.21     B3             

HD 277933     408991617     5.7713     1.4     1     05 17 51.12     +40 23 27.0     10.14     B3             

BD+61 77     419246605     8.0205     1.2     1     00 26 23.21     +62 45 38.9     9.61     B1IV             A 

ALS 6330     420545430     3.3131     2.5     1     00 45 17.23     +63 42 36.8     11.1     B1III             

TYC 4031-1324-1     421691939     6.0165     3.5     2     01 27 04.47     +60 49 08.1     11.07     B5             

BD+59 254     422533344     5.3948     3.8†    2     01 28 15.06     +60 13 45.8     10.07     A2             A 
 
HD 37115     427396133     5.9099     5.8     2     05 35 54.08     -05 37 42.3     7.4     B7Ve             A

CD-45 4501     430625041     5.7728     2.3†    1     08 45 19.49     -45 57 34.4     9.08      OB             A 
 
HD 298610     440971753     3.1712     4.1     2     09 39 00.81     -54 03 45.3     9.83     B2/4e             

HD 77769     447933173     5.4681     3.9     3     09 02 48.21     -46 57 48.9     9.37     B3IV     PP08         A

HD 19635     458911894     3.8763     2.4     3     03 12 56.84     +63 11 12.4     8.94     B4             A

BD+60 770     459014234     11.7894     10.8     5     04 00 49.57     +61 17 26.5     9.8     B5             A 
 
BD+62 647     459105076     10.9253     2.3     1     04 05 34.01     +62 47 28.6     9.58     B2V         NGC 1502     

TYC 8610-895-1     469095496     8.0080     4.3     1     09 53 23.95     -58 57 36.2     11.23     B5/7             blend 

Table of Candidate stars identified in this work, including the ID, TESS Input Catalog (TIC) number, information about the primary frequency and number of modes, coordinates, V-band magnitude, and spectral type, a citation if the star is known to be a star, a note if the star is a known cluster member, and information about remarks. Stars labeled “M" in this column are discussed in the main paper text, stars labeled “A" are commented upon in the Appendix, while “blend” indicates at there are bright nearby sources contributing flux in the aperture used by KELT (and likewise with TESS). The citations for candidate stars are as follows: PP08 = <cit.>, KE02 = <cit.>; some of these were already listed as candidates by <cit.>. †Amplitudes may be largely suppressed.



p2.5cmlcrcccccccccc 

6
Rejected stars  
 
ID     TIC     Freq.        Amp.       num.       RA (2000)     Dec (2000)     V         SP     known?     cluster?     Rem.  

       ID      (d^-1)     (mmag)      modes                                  (mag)                                       
 
TYC 4033-2268-1     12647620     3.5118     4.6     1     02 15 28.61     +60 09 44.6     11.69     B3         IC 1805     A
 
HD 221991     26283875     14.2427     0.8     1     23 36 32.16     +52 37 12.6     9.84     B5             A  

HD 75290     28709025     5.4869     1.9     3     08 47 33.74     -42 29 07.0     8.09     B3/5V         Trumpler 10     A 

HD 190088     40102236     5.2399     3.0     1     20 01 45.46     +38 44 06.9     7.86     B5             A 

HD 59446     60320306     7.0191     0.8     1     07 27 42.78     -47 24 50.4     7.59     B6II/III             A 

HD 144941     67985749     6.344     1.5     1     16 09 24.55     -27 13 38.2     10.02     B1/2II             A, M 

HD 72539     90134626     2.9852     1.6     2     08 31 22.31     -48 44 56.9     7.97     B5V             A 

o Vel     93549165     3.9746     0.7     1     08 40 17.59     -52 55 18.8     3.63     B3/5V             A 

HD 331621     102161004     3.3436     1.2     2     19 56 59.97     +31 17 16.0     9.98     B7             A 

HD 29450     118680798     4.6172     0.7     1     04 39 13.54     +22 39 08.1     8.57     B7V             A 

HD 62755     123754451     3.4328     0.8     5     07 43 23.09     -47 02 48.0     7.85     B5V             A 

HD 290564     138905907     8.6575     12.2     4     05 32 08.73     +00 07 36.8     11.2     B5             A 

CD-46 4432     141903541     5.2911     5.8     2     08 40 30.48     -47 12 35.2     10     B5             A 
  
HD 151654     157535787     12.5893     6.4     1     16 48 49.41     -03 36 39.4     8.6     B0.5V             A 

HD 181124     162012064     22.1863     2.2     3     19 19 18.34     -01 22 50.4     9.62     B5             A  

HD 35612     264485563     9.0839     0.8     1     05 26 06.00     +00 50 02.4     8.3     B7Vn             A 

TYC 4804-1086-1     281803267     3.9139     18.5     1     06 50 31.54     -02 19 45.9     11.91     B5             
 
HD 59325     291556636     3.7152     3.9     3     07 26 56.07     -51 11 07.0     10.55     B7V             A 


HD 190066     352529679     7.0184     15.6     0     20 02 22.10     +22 09 05.2     6.6     B1Iab             A  

ALS 10464     360661624     4.8883     11.8     1     19 44 21.08     +23 17 05.9     11.82     B0.5V             A 
 
V652 Her     377498419     18.6905     7.6     1     16 48 04.69     +13 15 42.4     10.51     B2He             A, M  

TYC 3315-1807-1     384992041     3.7614     44.1     1     03 21 39.63     +47 27 18.8     11.73     B7         Melotte 20     A 

HD 196035     417438983     4.0083     2.8     1     20 34 09.98     +20 59 06.7     6.47     B3IV             A 

TYC 4031-1770-1     422533347     5.3948     3.8     2     01 28 21.97     +60 14 43.9     10.94     B5             A 
  
HD 350990     424032547     5.0251     3.4     1     19 58 49.85     +20 31 29.9     10.32     B7II/III         Roslund 3     A  

TYC 1624-299-1     424032634     7.0305     1.4     1     19 58 41.30     +20 31 48.6     12.04     B7IVnnp         Roslund 3     A  

HD 254346     426520557     17.1232     4.2     4     06 16 57.32     +22 11 42.0     9.74     B2/3III             A, M 

CPD-45 2977     430625174     5.7728     2.3     1     08 45 10.44     -45 58 54.7     10.98     O9.5II             
 
TYC 4269-482-1     434178307     5.9868     1.9     2     22 50 26.49     +62 42 03.0     10.78     B5/8V             A 

HD 282433     446041643     4.4838     5.2     3     04 45 28.76     +30 16 54.4     9.52     B5             A 

Table of Candidate stars rejected in this work, including the ID, TESS Input Catalog (TIC) number, information about the primary frequency and number of modes, coordinates, V-band magnitude, and spectral type, a citation if the star is known to be a star, a note if the star is a known cluster member, and information about remarks. Stars labeled “M" in this column are discussed in the main paper text, stars labeled “A" are commented upon in the Appendix. 








*

J.L.-B. acknowledges support from FAPESP (grant 2017/23731-1). GH has been supported by the Polish NCN grant 2015/18/A/ST9/00578. LB acknowledges support from the NRF (South Africa) and thanks Mr Trevor Robinson for database assistance. DJS acknowledges support from the Pennsylvania State University's Eberly Research Fellowship. DJJ was supported through the Black Hole Initiative at Harvard University, through a grant (60477) from the John Templeton Foundation and by National Science Foundation award AST-1440254. This project makes use of data from the KELT survey, including support from The Ohio State University, Vanderbilt University, and Lehigh University, along with the KELT follow-up collaboration. This work has made use of data from the European Space Agency (ESA) mission Gaia (<https://www.cosmos.esa.int/gaia>), processed by the Gaia Data Processing and Analysis Consortium (DPAC, <https://www.cosmos.esa.int/web/gaia/dpac/consortium>). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research has made use of NASA's Astrophysics Data System. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of the BeSS database, operated at LESIA, Observatoire de Meudon, France: http://basebe.obspm.fr.



TESS, Gaia, KELT

astropy <cit.>,  
          Period04 <cit.> 
          
          
          







§ NOTES ON INDIVIDUAL STARS




 §.§ stars


TIC 11698190 = HD 228690: There is a slow drift in the light curve with a time scale of about 280 d that appears to be intrinsic to the star. There is also evidence for more pulsation frequencies than detected here.

TIC 13967727 = HD 194205: The frequency spectrum is complicated, suggesting the presence of more pulsation frequencies, but also binarity or rotational variability, or SPB-type pulsations, or any combination thereof.

TIC 25070410 = HD 166331: This star is listed as a spectroscopic binary by <cit.>. There are equally pulsation frequencies; see main paper text.


TIC 29123576 = CD-44 4876: The strongest pulsation frequency is likely to be variable in amplitude.

TIC 42940133 = HD 228101: Possible /SPB “hybrid" pulsator and/or rotational modulation/binarity.

TIC 44980675 = HD 171305: Possible /SPB “hybrid" pulsator.

TIC 55702566 = ALS 10035: More frequencies are present, but the periodogram is too complicated to push the analysis further. The low frequency detected indicates a possible /SPB “hybrid" pulsator, or rotational modulation/binarity.

TIC 61516388 = HD 178987: This is likely a “hybrid" pulsator.

TIC 65166720 = KP Per: The pulsation amplitudes for this star are probably underestimated because of its brightness. There are regular frequency spacings; see main paper text.

TIC 75745359 = HD 80279: Possible /SPB “hybrid" pulsator or rotational modulation/binarity.

TIC 80897625 = ALS 8706: The time scales of the temporal modulation of the variability amplitudes and phases of this Be star are different, which argues against a simple multifrequency beating phenomenon.

TIC 93723398 = HD 74339: There is a suspected F6=5.222037 , but unresolved from the strongest mode F1 in our data set (Table <ref>); <cit.> detected this mode.

TIC 128821888 = 12 Lac and TIC 129538133 = 16 Lac: The pulsation amplitudes of these bright famous stars are strongly suppressed in our data as simultaneous observations from other telescopes available to one of us (GH) show.


TIC 159932751 = V836 Cen: Perhaps the pulsation amplitudes we determined here are somewhat suppressed due to some saturation of this bright star. See Sect. <ref> for a detailed discussion of the pulsation spectrum.

TIC 168996597 = HD 225884: This is probably a /SPB “hybrid" pulsator, the pulsation frequency F4 (Table <ref>) has variable amplitude.

TIC 175760664 = HD 180642: The pulsation amplitudes of this well-studied bright star are probably somewhat suppressed in our data.

TIC 182714198 = BD-02 4752: This object shows binary induced or rotational modulation with a base period of 2.629 d.

TIC 184874234 = HD 173006: This star shows the stillstand phenomenon <cit.>. We detect more harmonics of the pulsation frequency than these authors, and also a very low frequency that appears to be real.

TIC 197332002 = HD 172367: This rapidly rotating star (v sin i = 240 , ) is possibly a /SPB “hybrid" pulsator.

TIC 216976987 = HD 332408: Possible shallow (≈ 3 mmag) eclipses with a 8.5862-d period.

TIC 234230792 = HD 49330: The CoRoT data of this Be star have been analysed in detail by <cit.>; an alias of the strongest pulsation frequency in the latter paper is the strongest signal in our data.

TIC 245719692 = BD+57 614: Possible /SPB “hybrid" pulsator or rotational modulation/binarity.

TIC 255974332 = ALS 6426: This heavily reddened star could be a /SPB “hybrid" pulsator or show the effects of rotational modulation/binarity.

TIC 264613043 = V611 Per: This star could be a binary or rotationally modulated with a short period of 1.3277 d.

TIC 264613619 = V757 Per: This star was among the candidates of <cit.> and is confirmed here. It also has regular frequency spacings; see main paper text.

TIC 266338052 = HD 232874: This star could be a binary or an ellipsoidal variable or undergo rotational modulation with a period of 3.0358 d.

TIC 279659875 = BD+68 1373: This star shows some evidence for binary- or rotationally induced variability with a period of 3.2719 d.

TIC 287467101 = HD 140543: This high Galactic latitude, high luminosity star (Sect. <ref>) may show “hybrid" /SPB pulsations. <cit.> suggested that it could have formed in the Galactic halo and noted “irregularly shaped lines" in his spectra of HD 140543, perhaps an effect of nonradial pulsation.

TIC 287690192 = HD 339039: There appear to be many more pulsation modes of type present in this star, yet daily aliasing and possible amplitude variations precluded their reliable detection. Some g-mode pulsations of the SPB type may also be present.

TIC 293680998 = IL Vel: We find a fourth signal in addition to the known mode triplet of the star <cit.>; the presence of more pulsation frequencies is also indicated.

TIC 297259536 = HD 199021: Possible /SPB “hybrid" pulsator or rotational modulation/binarity.

TIC 299821534 = HD 231124: Possible /SPB “hybrid" pulsator or rotational modulation/binarity. There are regular frequency spacings; see main paper text.

TIC 308954763 = HD 232489: Strömgren photometry <cit.> places this possible /SPB “hybrid" pulsator or binary into the domain in the HR Diagram, unlike its commonly quoted literature spectral type of B5 <cit.>. There are regular frequency spacings; see main paper text.

TIC 311943795 = HD 228365: The frequency spectrum of the star contains two signals between the common and SPB domains, perhaps an effect of rapid rotation. Our frequency analysis was hampered by some aliasing problems.

TIC 312630206 = HD 228463: We were able to detect as many as twelve independent mode frequencies for this star (Table  <ref>), but the density of the frequency spectrum and some aliasing ambiguities hampered the identification of a possible rotational frequency splitting.

TIC 338076483 = BD+64 1677: Possible /SPB “hybrid" pulsator.

TIC 347486043 = HD 13338: There are regular frequency spacings; see main paper text. We also find a binary or rotationally induced variation with a period of 1.7404 d.

TIC 348443241 = BD+56 560: Possible /SPB “hybrid" pulsator.

TIC 348506748 = HD 14357: Possible /SPB “hybrid" pulsator or rotational modulation/binarity. There are regular frequency spacings; see Sect. <ref>.

TIC 360063836 = HD 344775: The signal F3 in Table <ref> is likely an artifact from amplitude/frequency variations of F1.

TIC 361324132 = HD 344894: The signal F5 in Table <ref> is likely an artifact from amplitude/frequency variations of F1. There are regular frequency spacings; see Sect. <ref>.

TIC 370128780 = BD+58 241: Possible /SPB “hybrid" pulsator or rotational modulation/binarity.

TIC 372724051 = V1143 Cas: The signals listed for this object are the combination of the star's pulsations and that of a nearby ellipsoidal variable, V1142 Cas (cf. ).

TIC 391836737 = HD 30209: There are probably more pulsation frequencies in the domain, but apparent amplitude/frequency variations of the dominant signal hamper their reliable detection.

TIC 393662110 = V372 Sge: Again, there is evidence for several more pulsation frequencies in the domain, but apparent amplitude/frequency variations of the strongest signals hamper their reliable detection. There are also several possibilities for repetitive frequency splittings (Sect. <ref>).

TIC 399436828 = NGC 663 4: Whereas our algorithms originally identified this variable with the open cluster member NGC 663 2, a search in the surroundings revealed that in reality we recovered the pulsations of the known star NGC 663 4. NGC 663 2 is thus rejected.

TIC 419354107 = BW Vul: The pulsation amplitudes of this famous “stillstand" star are suppressed in our data due to its brightness.

TIC 445619007 = HD 14645: Possible binary or rotational variable with a period of 1.58293 d.

TIC 451932686 = HD 344880: This is an eclipsing binary with an eccentric orbit and a long period; see main paper text for details.

TIC 469221047 = HD 86214: As for TIC 80897625, the amplitudes and phases of the two stellar oscillation modes are modulated in time. However, the present case is better described by a narrow frequency triplet (Δ f = 0.00327 ) and a frequency quadruplet (Δ f = 0.00492 ), respectively. We nevertheless prefer to list the two strongest signals only as we cannot rule out intrinsic amplitude/phase modulation.

TIC 469223889 = HD 86162: Possible /SPB “hybrid" pulsator.



 §.§ Candidate stars


TIC 11158867 = TYC 4032-93-1: Even though the available spectral classification for this star is B3, its dereddened (B-V) color index and absolute magnitude rather point towards a /“hybrid" pulsator. We keep this star as a doubtful candidate.

TIC 12647534 = ALS 7011: We detected signals in both the and SPB domains. This star has a B-type neighbor separated by only 89" on the sky (TYC 4033-2268-1), and the frequency analysis of their data give consistent results. However, a blending analysis reveals that ALS 7011, and not TYC 4033-2268-1, is the source of this variability.

TIC 13973539 = HD 229171: The low frequency F2 we found for this Be star (cf. Table <ref>) shows a slow amplitude and phase drift. However, as the time scales of the amplitude and phase change are different, we suspect a rotational modulation.

TIC 28949811 = CD-44 4871: The literature on this star suggests it is of early B type, but the single frequency we found is unusually high for a star and its S/N is low.

TIC 29036690 = CD-46 4639: This is an intermediate Helium star located in the instability strip <cit.>.

TIC 29598925 = HD 76307: The absolute magnitude from the star's Gaia DR2 parallax is lower than expected given its spectral class.

TIC 30569481 = HD 76967: The relative amplitudes and values of the combination frequencies are unusual for a pulsator; the pulsation amplitudes may be variable as well. The Gaia DR2 parallax and Strömgren H_β are consistent with the classification of a mid B-type star, leading to the (inconclusive) suspicion it may be a rapidly rotating SPB star.

TIC 43301361 = HD 192003: Taken at face value, the frequency spectrum and Gaia DR2 parallax point towards an unevolved /SPB “hybrid" pulsator. However, an F0 star in 43" distance may introduce some /-type variability due to blending.

TIC 53709049 = TYC 4030-800-1: The B1V star BD+60 175 is located 116" from this object and is some 2.5 mag brighter. Therefore we are not sure whether the reported variability indeed originates from TIC 53709049.


TIC 53968977 = BD+60 192: Our frequency analysis is based on the first two seasons of data only.

TIC 74197071 = CD-45 4896: The pulsation spectrum of this star is rather unusual for a star and it is near (or even below) the low-luminosity end of the instability strip, hence it may be a rapidly rotating SPB pulsator.

TIC 78499882 = HD 249179: This Be star is located in a high-mass X-ray binary system, and shows brightness variations consistent with disk variability that is typical of Be stars. It is not clear whether the high-frequency periodic variability detected by us is indeed caused by pulsation.

TIC 80814494 = HD 67980: The Strömgren H_β index for this star implies a spectral type around B3 <cit.> instead of B7II.

TIC 94000461 = HD 74581: This is a close visual double star, hence it is unclear from which source the variability originates.

TIC 123828144 = HD 62894: There is an A-type star of equal brightness 24" distant from this object, which could be a pulsator.

TIC 137489662 = HD 183535: The Strömgren H_β index for this star implies a spectral type around B1 <cit.> rather than B5.

TIC 140309502 = CD-44 4484: There is some weak evidence for shallow (≈ 2 mmag) eclipses with a 13.721(7)-d period, but more precise photometry is required to confirm or reject this suspicion.

TIC 141903641 = CD-46 4437: In the light curve for CD-46 4432 we identified signals consistent with a possible /SPB “hybrid" pulsator. However, the blending analysis shows this signal originating in the close visual double star CD-46 4437. Since the spectral type of the brighter of this pair is possibly consistent with pulsation, we classify CD-46 4437 as a candidate.

TIC 143530557 = HD 279639 and TIC 145672806 = CPD-52 1713: Both stars are of later spectral type than usual stars. We suspect they are rapidly rotating g-mode pulsators, but cannot prove this as of yet.

TIC 190783321 = HD 76554: All literature information consistently suggests this is an early B-type star, but its oscillation frequencies would be rather typical for a star, and much higher than found among pulsators.

TIC 207045768 = HD 258853: This star is probably not luminous enough to fall into the strip, and each of the three variability frequencies is either the sum or the difference of the other two.

TIC 231149746 = TYC 746-578-1: The absolute magnitude of this star from its Gaia parallax is 2.6±0.1. This suggests that either there is a problem with the original spectral classification <cit.> or the parallax measurement.

TIC 252864874 = TYC 3324-92-1: The absolute magnitude of the star from Gaia DR2 and its pulsation frequencies suggest this is a star rather than a pulsator, and that perhaps there is a problem with the original spectral classification <cit.>.

TIC 290300414 = HD 78507: The spectral classification and absolute magnitude of this star suggest it could be a rapidly rotating SPB star. Amplitude and frequency variations apparently occurred during the time span of our observations.

TIC 307944768 = HD 260858: This Helium-rich star's absolute magnitude from the Gaia DR2 parallax and effective temperature <cit.> suggest it has evolved off the main sequence. This is interesting because there is no post-main sequence star known to date.

TIC 319302209 = HD 220300: The pulsation spectrum and basic parameters of this rapidly rotating Be star are more reminiscent of a rapidly rotating SPB star than of a pulsator. It has been detected as variable by the HIPPARCOS mission (reported by ), but only <cit.> described its variability in detail.

TIC 335484090 = V447 Cep: Besides the known short-period variability of this star (it was also classified as a candidate star by ), we discovered that it is an eclipsing binary; see main paper text.

TIC 347585038 = V352 Per: This star was already listed as a candidate by <cit.>.

TIC 348609224 = BD+56 579: This Be star has been identified as a visual double by Speckle Interferometry <cit.>, which may have had an effect on its Gaia parallax measurement.

TIC 366108295 = ALS 6216: This spectroscopic binary has a pulsation frequency quite high for a star; a 1.5 mag brighter B0.5 IV star is located 96" away and could have had an influence on the measured variability. Our blending analysis does not indicate a blend scenario, but this is so far not conclusive. 

TIC 368237682 = BD+66 1651: This Be and possible runaway star <cit.> shows variability in both the and SPB star frequency domains. Its luminosity computed from the Gaia DR2 parallax is much lower than expected for its B3Ve spectral class.

TIC 370269139 = BD+55 334 and TIC 372115570 = BD+57 579: These stars have several visual companions close enough to qualify as potential sources for the observed variability.


TIC 384257658 = HD 78206: Whereas the literature spectral classification is B7/8V, the star's absolute magnitude from the Gaia parallax corresponds to that of a B2V star.

TIC 386693012 = HD 42896: This rapidly rotating (v sin i = 318 , ) luminous star shows quite high variability frequencies for a star and several combinations thereof.

TIC 387153140 = BD-09 4742: The variability frequencies of this object are fairly high for a star and each of these three frequencies is either the sum or the difference of the other two.

TIC 419246605 = BD+61 77: Whereas this star is repeatedly classified with an early B spectral type in the literature, its absolute magnitude from the Gaia DR2 parallax is only +2.8. We note that the error on this parallax is unusually high and that the star has a visual companion one magnitude fainter 0.3" apart, which may have affected the parallax measurement adversely.

TIC 422533344 = BD+59 254: In the light curve for TYC 4031-1770-1 we identified signals consistent with pulsation. However, the blending analysis shows this signal originating in the neighboring star BD+59 254. The literature spectral type of BD+59 254 is A2, which is more consistent with pulsation. The frequencies we detect are more consistent with pulsation though, so it is unclear what the nature of this object is. 

TIC 427396133 = HD 37115: Because of some saturation issues (cf. ) with this data set and the removal of an apparent outburst of this Be star the results of our frequency analysis should be treated with caution.

TIC 430625041 = CD-45 4501: We identified signals consistent with pulsation in the light curve of CPD-45 2977. Our blending analysis shows this signal instead comes from CD-45 4501, which we estimate to have a spectral type consistent with pulsations. 

TIC 447933173 = HD 77769: Even though this star has three variability frequencies in the domain and has been classified as such a pulsator in the past <cit.>, it is cooler and less luminous than the pulsators of this class.

TIC 458911894 = HD 19635: Based on the available data it cannot be decided whether the detected triplet of frequencies is due to beating of multiple signals or due to amplitude/phase modulation of a single independent variation. In case of the interpretation as a triplet it should be noted that its frequency asymmetry is of the opposite sign than expected from the second-order effect of rotation <cit.>.

TIC 459014234 = BD+60 770: This is a visual double star with 8" separation with the primary classified with a B5 spectral type. The pulsation spectrum is reminiscent of that of a star, and the Gaia DR2 parallax appears to corroborate that. However, given the visual binarity we are not sure how accurate the parallax measurement is and keep the star in our list of candidates.




 §.§ Rejected stars



TIC 12647620 = TYC 4033-2268-1: The same signal exists in the light curves for both ALS 7011 and TYC 4033-2268-1, separated by 89”. Our blending analysis shows this signal as coming solely from ALS 7011, which we classify as a candidate. 

TIC 26283875 = HD 221991/TYC 4000-2127-1: This is a visual double star with 18" separation. The Gaia DR2 parallaxes of both objects show that they are A-type stars at very similar distance. We therefore conclude that at least one of them is a pulsator, responsible for the detected variability, and that the B5 spectral classification is erroneous.

TIC 28709025 = HD 75290: <cit.> give a spectral type of B9V, with is consistent with the measured Strömgren H_β index of 2.765 that suggests B8/9 <cit.>, and with the star's absolute magnitude M_v=-0.3 from its Gaia DR2 parallax. We conclude that this cannot be a star.

TIC 40102236 = HD 190088: As for the previous star, the Strömgren H_β index (2.748) and its absolute magnitude M_v=-0.1 from its Gaia DR2 parallax suggest this is a late B-type and not a star.

TIC 60320306 = HD 59446: Again, Strömgren photometry and the Gaia DR2 parallax of this star suggest a mid to late B spectral type. In addition, we are unsure that the detected variability is not an artifact of saturation in the images of this bright star.

TIC 67985749 = HD 144941: This is an extreme Helium star and therefore not of the type; see Sect. <ref>.

TIC 90134626 = HD 72539: Also in this case, Strömgren photometry and the Gaia DR2 parallax of this star consistently point towards a mid to late B spectral type. The variability is therefore likely due to SPB-type pulsation, with frequencies pushed towards the domain by rapid rotation.

TIC 93549165 = o Vel: This is a very bright prototype SPB star <cit.>. The variability detected in our light curves is certainly not due to the star, but an instrumental artifact.

TIC 102161004 = HD 331621: This is another case of a star that shows variability frequencies close to the range, but its absolute magnitude is far below that of the known pulsators.

TIC 118680798 = HD 29450: Likewise, this star is too cool and not luminous enough to be even close to the domain in the HR Diagram, as literature Strömgren photometry and the Gaia DR2 parallax demonstrate.

TIC 123754451 = HD 62755: Also in this case, literature Strömgren photometry and the Gaia DR2 parallax strongly argue against an interpretation of this star's variability as being caused by pulsations due to its low effective temperature and luminosity.


TIC 138905907 = HD 290564: The absolute magnitude of this star and UBV photometry <cit.> suggest that this is an late A/early F star and hence the variability we detected is of the type. Therefore our pre-selection of this star was based on an incorrect spectral classification.

TIC 141903541 = CD-46 4432: Initially identified as a possible /SPB “hybrid" pulsator. However, the blending analysis reveals that the signal originates in a source to the South-West, at the location of the close visual double CD-46 4437 (although we cannot resolve this visual double). Since it is possible that the brighter component is of the correct spectral type, we include CD-46 4437 as a candidate star. 

TIC 157535787 = HD 151654: There are two vastly different spectral classifications for this star in the literature, B0.5 V <cit.> and F0 <cit.>. Strömgren photometry and the Gaia DR2 parallax corroborate the latter. Hence this is a pulsator and not a star.

TIC 162012064 = HD 181124: This case is similar to the former: <cit.> classified this star as B5, but <cit.> as A3 IV. The absolute magnitude of the star derived from Gaia DR2, its (B-V)_0 colour index and the high pulsation frequencies are clearly that of a and not a star.

TIC 264485563 = HD 35612: This instance is similar to HD 62755. Again, the effective temperature from Strömgren photometry and the absolute magnitude from the Gaia DR2 parallax are incompatible with a classification. The weak variability signal is also not convincing.

TIC 281803267 = TYC 4804-1086-1: The signal in our light curve for this object is from a relatively bright W UMa type binary 3' to the South-East, V453 Mon. 

TIC 291556636 = HD 59325: Geneva photometry of the star <cit.> and its calibration <cit.> suggest that this is a mid to late B star on the main sequence. The Gaia DR2 parallax implies an absolute magnitude corresponding to a post main sequence star, but even so the star would not fall in any instability domain related to stars <cit.>. We conclude that this is most likely an SPB star with observed frequencies modified towards the domain by rapid rotation.


TIC 352529679 = HD 190066: The variability detected in the measurements of this star could be traced to the data quality being vastly different depending on whether the telescope was pointed East or West. Removing the poor observations, no variability remains.

TIC 360661624 = ALS 10464: Initially identified as a pulsator, but our blending analysis shows the signal coming from the star LS II +23 36, which is ∼1 mag brighter and lies 85” to the North-East. LS II +23 36 is included here as a candidate, as it may have a spectral type consistent with pulsations. 

TIC 377498419 = V652 Her: This is another extreme Helium star that fulfilled our pre-selection criteria. The frequency solution in Table <ref> is only informal due to the large rate of change of the pulsation period; see Sect. <ref>.

TIC 384992041 = TYC 3315-1807-1: A literature search readily shows that this is a close binary composed of a subdwarf star and a late-type main sequence companion <cit.>.

TIC 399436782 = NGC 663 2: Whereas our algorithms identified this variable with the open cluster member NGC 663 2, a search in the surroundings revealed that in reality we recovered the pulsations of the known star NGC 663 4 which is here categorized as a star.

TIC 417438983 = HD 196035: The variability detected for this bright star is an integer multiple of the sidereal daily alias, suggesting that there are saturation effects in the photometry. The effective temperature of the star from Strömgren and Geneva photometry and the absolute magnitude from the Gaia DR2 parallax are both too low to place the star at least close to the known domain in the HR diagram.

TIC 422533347 = TYC 4031-1770-1: Initially identified as a pulsator, but our blending analysis shows the signal coming from the neighboring star BD+59 254, which lies 77” to the South-West. BD+59 254 is included as a candidate.

TIC 424032547 = HD 350990 and TIC 424032634 = TYC 1624-299-1: These two stars are separated by only 122" on the sky; they are located in a dense region in the open cluster Roslund 3 that contains several stars of similar brightness, leading to blending and saturation issues. The variability detected for both of these stars occurs at frequencies that are integer multiple of the sidereal daily alias. These stars are also of too late spectral type and too low absolute magnitude to fall into the domain.

TIC 426520557 = HD 254346: The variability detected in this data set contains both pulsations and eclipses. Whereas the amplitude of the eclipses does not significantly change depending on whether the telescope is pointed East or West, the amplitudes of the pulsations do. Furthermore, the pulsating star HD 43385 that is more than one magnitude brighter than HD 254346 is located in 112" distance. Strömgren photometry places HD 43385 into the instability strip. Hence we interpret the observed variability by pulsations of HD 43385 in combination with eclipses of HD 254346, which itself shows no detectable pulsational variability; the eclipses are discussed in the main paper text.

TIC 430625174 = CPD-45 2977: The signal in our light curve comes from the V=9 neighbor 2' to the North-East, CD-45 4501, which is ∼2 mag brighter than CPD-45 2977 in the V-band. CD-45 4501 is categorized as a candidate. 

TIC 434178307 = TYC 4269-482-1: Strömgren photometry and the Gaia DR2 distance point towards a very late B or even an early A star. The detected variability signals have poor S/N. Thus there is no evidence that this could be a pulsator.

TIC 446041643 = HD 282433: The effective temperature from Strömgren photometry and the absolute magnitude from the Gaia DR2 parallax are incompatible with a classification. We allege that this is another case of a rapidly rotating SPB pulsator.








§ FREQUENCY TABLES


All recovered frequencies and their amplitudes are reported in Tables 7, 8, and 9.



 §.§ stars


lcr  
Frequencies and amplitudes determined for the stars. Formal error estimates determined according to <cit.> are given in braces in units of the last significant digit. †Amplitudes may be largely suppressed.

7
 
ID     Freq.        Amp.

      (d^-1)     (mmag)

3cTIC 5076425 

F1   	5.63875(1)   37(1) 

F2   	5.88842(1)   33(1) 

F3   	5.81121(2)   	20(1) 

F4   	5.45326(4)   10(1) 

3cTIC 10891640 

F1   	6.799702(4)   13.8(2)

F2   	5.960461(6)   8.4(2) 

F3   	0.162244(3)   4.5(2) 

F4   	6.8001(2)   2.8(2) 

3cTIC 11696250 

F1   	7.59638(1)   2.7(1) 

F2   	6.81487(1)   2.5(1)

F3   	3.96790(2)   1.8(1) 

F4   	5.28827(2)   1.7(1)

F5   	6.53336(3)   1.0(1)

F6   	5.55230(4)   0.9(1) 

3cTIC 11698190 

F1   	5.872054(5)   9.7(2) 

F2   	5.552150(6)   9.0(2) 

F3   	5.56928(1)   3.5(2) 

F4   	5.80301(3)   2.0(2) 

3cTIC 13332837 

F1   	6.874397(7)   5.5(2) 

F2   	6.48827(3)   1.5(2) 

F3   	8.63307(3)   1.3(2) 

3cTIC 13967727 

F1   	4.445459(3)   12.1(2) 

F2   	4.378370(3)   11.9(2)

F3=F1+F2   	8.823830(4)   1.9(2)

F4   	0.18282(1)   3.5(2)

F5   	0.36563(2)   1.9(2)

F6   	0.14505(3)   1.3(2) 

3cTIC 25070410 

F1   	7.447568(6)   12.2(2)

F2   	6.95940(1)   6.0(2) 

F3   	6.95362(2)   3.8(2)

F4   	7.23907(2)   3.2(2) 

F5   	6.63922(3)   2.6(2) 

F6   	6.93872(3)   2.4(2) 

3cTIC 29123576 

F1   	7.782614(8)   17.0(4)

F2   	7.32397(3)   i4.9(4) 

3cTIC 29585482 

F1   	8.07168(2)   5.5(3)

3cTIC 31921921 

F1   	4.637292(4)   14.9(2)

F2=2F1   	9.274585(9)   4.8(2)

F3=3F1   	13.91188(1)    1.2(2) 

3cTIC 41327931 

F1   	8.97107(3)   1.2(2) 

F2   	8.13509(3)   1.2(2)

3cTIC 42365645 

F1   	7.830516(2)   19.1(2)

F2   	7.794148(5)   8.0(2) 

F3   	7.908111(9)   4.2(2) 

F4   	7.94628(1)   4.1(2)

F5   	1.327791(6)   5.4(2)

F6   	7.831869(9)   4.6(2) 

F7=2F5   	2.65558(1)   2.7(2)

F8   	7.79322(2)   2.4(2)

F9   	7.60063(2)   1.9(2)

F10=3F5   	3.98337(2)   1.8(2)

F11=4F5   	5.31117(2)   1.1(2) 

F12   	7.70240(3)   1.4(2) 

F13   	7.83856(3)   1.3(2)

3cTIC 42940133 

F1   	6.299788(5)   4.32(9) 

F2   	6.921975(6)   3.99(9)

F3   	7.387334(6)   3.79(9)

F4   	7.164733(8)   2.66(9)

F5   	0.36111(2)   1.39(9)

F6   	6.72631(2)   1.19(9) 

F7   	6.78095(2)   1.17(9) 

F8   	0.32302(2)   0.93(9) 

F9=2F10   	0.32628(2)   0.79(9) 

F10   	0.16315(2)   0.70(9) 

3cTIC 43881045 

F1   	7.122573(3)   7.5(1)

3cTIC 44980675 

F1   	5.158542(6)   8.4(1) 

F2   	0.50941(2)   2.8(1) 

F3   	0.32240(3)   1.6(1) 

F4   	4.55869(3)   1.4(1) 

3cTIC 45799839 

F1   	7.575293(7)   3.6(1)

F2   	9.29511(1)   1.8(1) 

3cTIC 55702566 

F1   	6.54900(1)   6.5(3) 

F2   	6.88965(2)   5.0(3)

F3   	0.65842(3)   2.8(3) 

F4   	12.96233(4)   2.1(3) 

F5   	7.41737(4)   2.0(3) 

3cTIC 61516388 

F1   	7.14659(1)   7.5(2) 

F2   	0.25205(2)   4.1(2) 

F3   	0.28962(2)   3.3(2) 

F4   	7.08337(3)   2.2(2) 

3cTIC 65166720 

F1   	4.95583(1)   16.0(3)

F2   	5.04840(2)   10.8(3)

F3   	4.40346(4)   6.0(3) 

F4   	4.50767(7)   3.4(3) 

F5   	5.06972(8)   2.9(3) 

3cTIC 75745359 

F1   	7.25905(1)   3.1(1)

F2   	6.97609(6)   0.8(1) 

F3   	0.39610(6)   0.7(1) 

3cTIC 80897625 

F1   	4.40603(1)   4.7(3) 

F2   	4.33994(1)   4.4(3) 

3cTIC 89756665 

F1   	8.41789(1)   3.7(2) 

F2   	0.00819(2)   3.3(2) 

F3   	9.85740(3)   1.8(2) 

3cTIC 93723398 

F1   	5.220117(3)   29.2(3)

F2   	5.195248(6)   16.6(3)

F3   	5.23896(1)   9.5(3) 

F4   	5.255634(9)   9.9(3)

F5   	5.20529(1)   8.0(3) 

3cTIC 93730538 

F1   	5.445082(5)   6.8(1) 

F2   	6.286168(7)   5.4(1) 

F3   	5.74156(1)   3.6(1) 

F4   	6.00031(2)   2.0(1)

F5   	0.29368(2)   2.1(1) 

F6   	0.28095(2)   2.3(1)

F7   	0.25851(3)   1.3(1) 

F8   	5.60304(4)   0.9(1) 

3cTIC 101423289 

F1   	7.48973(1)   6.2(2) 

F2   	7.37917(1)   6.4(2) 

F3   	7.25335(2)   4.9(2)

F4   	8.35985(4)   1.7(2) 

F5   	6.96763(5)   1.4(2) 

F6   	6.81801(6)   1.3(2) 

3cTIC 105517114 

F1   	4.457141(2)   22.0(1)

F2   	4.666456(3)   11.6(1)

F3   	4.326864(3)   11.3(1) 

F4   	4.190111(4)   7.6(1) 

F5   	4.534389(6)   5.6(1) 

F6   	4.809343(6)   5.3(1)

F7=F1+F5   	8.991530(6)   1.8(1)

F8=2F1   	8.914282(3)   1.3(1)

F9=F1+F2   	9.123597(3)   0.9(1)

F10=F2+F4   	8.856567(5)   0.8(1)

F11=F2+F3   	8.993320(4)   0.9(1) 

F12=F4+F6   	8.999454(8)   0.9(1) 

F13=F1+F3   	8.784005(3)   0.8(1) 

F14=F2+F5   	9.200845(7)   0.4(1) 

F15=2F3   	8.653729(4)   0.5(1) 

3cTIC 123211175 

F1   	7.18926(4)   0.7(1) 

3cTIC 128821888 

F1   	5.178946(6)   7.5(2) 

F2   	5.06628(1)   3.4(2) 

F3   	5.49008(2)   2.4(2) 

F4   	5.33420(2)   2.0(2) 

F5=F1+F4   	10.513145(6)   1.4(2) 

3cTIC 129538133 

F1   	5.85028(2)   4.4(2) 

F2   	5.50260(2)   3.6(2) 

F3   	5.91130(3)   2.8(2) 

3cTIC 141292310b 

F1   	4.54498(3)   4.7(1) 

F2   	0.92020(6)   2.0(1) 

F3   	4.2052(1)   1.3(1) 

F4   	4.5765(1)   1.3(1) 

F5   	1.35078(9)   1.3(1) 

F6   	4.4974(1)   0.9(1) 

F7   	1.1585(1)   0.9(1) 

3cTIC 159932751 

F1   	6.966153(5)   8.5(1) 

F2   	6.461838(5)   8.0(1) 

F3   	6.449531(5)   8.2(1)

F4   	6.590981(9)   4.5(1) 

F5   	6.97869(1)   3.2(1) 

F6   	6.99092(2)   2.4(1)

F7   	6.43716(2)   2.4(1)

F8   	6.42472(4)   1.0(1) 

F9   	0.68311(4)   0.9(1) 

3cTIC 168996597 

F1   	5.82201(1)   2.9(1)

F2   	5.72972(1)   2.8(1)

F3   	0.39038(2)   1.6(1) 

F4   	8.22823(3)   1.4(1) 

F5   	0.36931(3)   1.4(1) 

3cTIC 175760664 

F1   	5.486894(4)   28.4(3)

F2=2F1   	10.973787(7)   4.6(3)

F3=3F1   	16.46068(1)   3.1(3)

F4=4F1   	21.94757(1)   1.6(3) 

3cTIC 180952390 

F1   	6.627465(9)   6.9(2) 

F2   	6.23117(2)   3.0(2) 

F3=F1+F2   12.85864(2)   1.3(2)

F4=2F1   	13.25493(2)   0.8(2) 

3cTIC 182714198 

F1   	6.97786(2)   7.0(4) 

F2=2F3   	0.76075(2)   6.9(4)

F3   	0.38037(1)   5.0(4)

F4   	6.41787(3)   3.7(4)

3cTIC 184874234 

F1   	5.877919(4)   36.1(4)

F2=2f1   	11.755838(7)   9.6(4)

F3=3f1   	17.63376(1)   5.4(4) 

F4=4f1   	23.51168(1)   2.9(4)

F5=5f1   	29.38960(2)   2.1(4) 

F6=6f1   	35.26752(2)   1.8(4) 

F7   	0.00567(1)   9.7(4)

3cTIC 185476952 

F1   	8.29493(2)   2.1(2) 

F2   	8.46231(3)   1.8(2) 

F3   	9.02509(3)   1.5(2) 

F4   	8.44342(5)   0.9(2) 

F5   	8.12972(5)   0.9(2) 

3cTIC 187483462 

F1   	6.73549(1)   0.90(7) 

F2   	0.47329(2)   0.52(7) 

3cTIC 197332002 

F1   	4.688242(9)   8.8(3) 

F2   	1.89627(1)   8.1(3)

F3   	0.14873(2)   5.1(3) 

F4   	5.89429(2)   4.2(3) 

3cTIC 216976987 

F1   	6.777856(8)   2.65(9)

F2   	0.23294(1)   1.59(9) 

F3   	1.76404(2)   0.93(9) 

F4=2F2   	0.46587(3)   0.48(9) 

3cTIC 225687900 

F1   	5.443056(5)   24.2(4) 

F2   	5.357764(9)   14.1(4) 

3cTIC 232846315 

F1   	7.59044(1)   3.0(2) 

F2=2f4   	1.47419(1)   3.0(2)

F3=4f4   	2.94838(2)   2.2(2) 

F4   	0.73709(1)   0.7(2) 

3cTIC 234068267 

F1   	5.598023(6)   9.6(2) 

F2   	5.53356(1)   4.5(2)

F3   	5.48953(4)   1.5(2) 

3cTIC 234230792 

F1   	10.85911(4)   1.7(2) 

F2   	6.94930(5)   1.2(2) 

3cTIC 245719692 

F1   	6.92500(5)   2.4(2) 

F2   	0.45300(6)   1.9(2) 

F3   	4.7635(1)   1.3(2) 

3cTIC 251196433 

F1   	6.37298(2)   6.5(2) 

F2   	4.12598(6)   2.0(2) 

F3   	5.66421(8)   1.5(2) 

3cTIC 251250184 

F1   	4.120389(9)   17.7(3)

F2   	4.03062(1)   14.2(3)

F3   	4.18986(2)   9.8(3) 

F4   	4.27198(3)   5.9(3) 

F5=2F3   	8.37973(3)   2.0(3)

F6=F2+F3   	8.22044(2)   1.2(3)

F7   	6.3903(1)   1.5(3)

F8=F1+F3   	8.31025(2)   1.1(3) 

3cTIC 251250634 

F1   	12.20049(7)   1.9(2)

F2   	9.04715(9)   1.4(2) 

3cTIC 251637508 

F1   	5.499909(4)   16.7(2)

F2   	5.461319(6)   12.7(2)

F3   	5.53836(2)   3.5(2) 

F4   	5.38249(3)   2.5(2) 

F5   	5.76330(4)   1.8(2)

F6=F1+F4   	10.88240(3)   1.3(2)

3cTIC 255974332 

F1   	4.82425(2)   11.0(4) 

F2   	4.91960(3)   7.6(4) 

F3   	0.18822(6)   3.6(4) 

F4   	4.61661(9)   2.4(4) 

F5   	4.3714(1)   2.2(4) 

F6   	5.26261(1)   2.2(4) 

F7=F1+F2   	9.74384(3)   1.5(4)

3cTIC 264612228 

F1   	6.27361(2)   5.8(2) 

F2   	6.27212(5)   2.3(2) 

F3   	5.78476(7)   1.7(2) 

F4   	5.90656(7)   1.8(2) 

3cTIC 264613043 

F1   	5.82463(2)   3.6(2) 

F2   	1.50635(5)   1.9(2)

3cTIC 264613619 

F1   	4.07690(1)   8.3(2)

F2   	4.19978(2)   3.6(2) 

F3   	4.04781(2)   3.8(2) 

F4   	4.22886(3)   2.9(2)

F5   	4.21448(4)   2.1(2) 

F6   	4.14531(7)   1.2(2)

F7   	4.03326(6)   1.4(2)

F8=F1+F2   	8.27668(3)   0.7(2) 

3cTIC 264615882 

F1   	4.89703(1)   6.6(2) 

F2   	4.74677(1)   5.6(2) 

F3   	4.38948(2)   4.2(2) 

F4   	4.62217(4)   2.0(2) 

F5   	4.30801(4)   1.9(2) 

F6   	4.20802(8)   1.1(2) 

3cTIC 264731122 

F1   	4.127522(6)   20.0(2)

F2   	3.98217(2)   8.3(2) 

F3   	4.00882(2)   7.2(2) 

F4   	4.06179(2)   5.5(2) 

F5   	3.95513(3)   4.6(2) 

3cTIC 266338052 

F1   	5.74001(1)   5.5(1) 

F2   	0.65881(3)   2.8(1) 

F3   	6.91081(6)   1.1(1)

F4   	0.32941(2)   0.7(1)

F5   	6.92586(8)   0.8(1) 

F6   	0.98822(4)   0.8(1)

3cTIC 269228628 

F1   	4.99191(6)   46(4)

F2   	4.83500(7)   38(4)

F3   	4.25270(9)   29(4)

3cTIC 272922818 

F1   	8.02788(4)   36(3)

3cTIC 279236955 

F1   	8.054088(2)   18.5(2)

F2   	7.731494(7)   5.9(2) 

F3   	7.83966(1)   2.9(2) 

F4   	8.23004(2)   2.4(2) 

F5   	0.32259(3)   1.2(2)

F6   	15.78558(4)   1.0(2) 

3cTIC 279659875 

F1   	5.83009(2)   3.8(1)

F2   	0.61126(8)   0.9(1) 

F3   	6.7508(1)   0.7(1) 

3cTIC 282529703 

F1   	7.500674(5)   11.2(2)

F2   	7.67644(2)   3.7(2) 

3cTIC 283136444 

F1   	7.95176(5)   14(1)

3cTIC 287467101 

F1   	5.60859(2)   2.0(1)

F2   	1.06253(4)   1.2(1) 

3cTIC 287690192 

F1   	8.269534(4)   9.6(1) 

F2   	7.662407(4)   8.6(1) 

F3   	7.824390(4)   8.4(1) 

F4   	0.63773(2)   2.0(1) 

F5   	8.78432(2)   1.9(1) 

F6   	1.12189(2)   1.4(1) 

F7   	8.75905(3)   1.1(1) 

3cTIC 293680998 

F1   	5.459807(3)   28.9(3) 

F2   	5.363247(4)   24.4(3)

F3   	7.22067(3)   3.4(3)

F4   	5.41455(4)   2.5(3) 

3cTIC 295435513 

F1   	7.70882(1)   10.8(2)

F2   	7.06709(5)   3.2(2) 

3cTIC 296570221 

F1   	6.090863(8)   5.4(1) 

F2   	6.04198(1)   3.7(1) 

F3   	6.06932(3)   1.5(1)

F4   	5.50062(4)   1.2(1) 

F5   	7.88333(4)   1.0(1) 

3cTIC 297259536 

F1   	11.38469(1)   2.11(8) 

F2   	9.94812(2)   1.02(8) 

F3   	0.61498(3)   0.59(8) 

F4   	9.44019(4)   0.47(8) 

3cTIC 299821534 

F1   	4.543190(4)   30.7(4)

F2=2F1   	9.086379(9)   3.3(4)

F3=3F1   	13.62957(1)   2.2(4) 

F4   	5.17349(4)   3.3(4)

F5   	5.62474(5)   2.8(4) 

F6   	0.35691(5)   2.5(4) 

F7   	6.05917(6)   2.4(4) 

3cTIC 308954763 

F1   	5.37689(1)   7.6(2) 

F2   	5.14309(2)   4.8(2) 

F3   	5.12346(3)   3.7(2) 

F4   	5.25366(5)   1.9(2) 

F5   	5.15901(5)   1.8(2) 

F6   	0.10893(8)   1.2(2) 

F7   	5.06220(8)   1.2(2) 

F8   	4.9591(1)   1.0(2) 

F9   	1.14400(9)   1.2(2) 

3cTIC 311943795 

F1   	8.28858(1)   4.8(3) 

F2   	2.42342(2)   3.0(3)

F3   	7.20570(2)   2.7(3)

F4   	3.46824(3)   1.9(3) 

F5   	7.09267(3)   1.8(3) 

F6   	8.09053(4)   1.7(3) 

3cTIC 312626970 

F1   	4.791218(4)   8.7(1) 

F2   	4.577946(4)   8.4(1) 

F3   	5.032253(5)   8.0(1)

F4   	5.420294(6)   6.6(1) 

F5   	4.551897(7)   5.5(1) 

F6   	4.86814(3)   1.2(1) 

F7=2F5   	9.10379(1)   1.1(1)

3cTIC 312630206 

F1   	6.084691(2)   16.9(2)

F2   	6.260011(4)   11.8(2) 

F3   	6.03265(1)   4.3(2) 

F4   	6.11064(1)   3.0(2)

F5   	6.94350(2)   2.7(2) 

F6   	6.59999(2)   1.9(2) 

F7   	6.97220(2)   1.9(2) 

F8   	6.68571(3)   1.5(2)

F9   	5.51236(3)   1.3(2) 

F10   	7.48618(3)   1.3(2) 

F11   	7.54980(3)   1.3(2) 

F12   	6.42436(4)   1.2(2) 

3cTIC 312637783 

F1   	8.182742(7)   5.5(2) 

F2   	8.05626(1)   3.7(2) 

F3   	7.62923(1)   3.6(2)

F4   	8.11316(2)   2.2(2) 

F5   	7.98128(2)   2.1(2)

F6   	8.13077(2)   2.0(2) 

3cTIC 312639883 

F1   	5.953170(6)   4.7(1) 

F2   	7.12450(2)   1.7(1) 

F3   	6.24850(2)   1.4(1) 

F4   	8.49087(2)   1.2(1) 

F5   	6.47017(3)   0.9(1)

3cTIC 314833456 

F1   	4.169867(9)   19.9(3) 

F2   	4.54123(1)   15.8(3) 

F3   	4.44952(2)   9.8(3) 

F4   	4.51831(2)   8.2(3) 

F5   	4.12392(3)   5.3(3) 

F6   	4.19268(3)   5.1(3) 

F7   	4.51793(2)   7.8(3) 

F8=F2+F3   	8.99075(2)   3.1(3)

F9   	4.14687(7)   2.6(3)

F10   	4.10055(7)   2.5(3)

F11=2F2   	9.08246(2)   1.6(3)

3cTIC 331782797 

F1   	7.98732(5)   33(3)

3cTIC 337105253 

F1   	5.94609(4)   15(1)

F2   	5.7712(1)   7(1)	

3cTIC 338076483 

F1   	4.77848(3)   2.8(1)

F2   	1.24129(6)   1.1(1) 

F3   	5.62774(9)   0.9(1) 

3cTIC 347486043 

F1   	4.63603(1)   6.5(1) 

F2=2F4   	1.14919(2)   3.2(1) 

F3   	4.78138(5)   1.6(1) 

F4   	0.57459(1)   1.6(1) 

F5   	4.58469(6)   1.2(1) 

F6   	4.61050(7)   1.1(1) 

3cTIC 347684339 

F1   	5.89589(2)   3.5(2) 

F2   	6.7620(1)   0.9(2) 

3cTIC 348137274 

F1   	6.34881(3)   6.2(3) 

F2   	6.23048(5)   3.7(3) 

F3   	6.10761(9)   2.0(3) 

3cTIC 348231245 

F1   	6.80616(5)   2.3(2) 

3cTIC 348232246 

F1   	7.79032(5)   3.2(3) 

3cTIC 348443241 

F1   	5.18990(3)   4.4(2) 

F2   	2.20500(6)   1.9(2)

3cTIC 348506748 

F1   	4.60303(2)   2.8(1) 

F2   	0.52494(3)   2.0(1) 

F3   	4.48614(6)   1.1(1) 

F4   	4.94911(6)   1.0(1) 

F5   	4.77749(7)   0.9(1) 

F6   	5.16733(8)   0.8(1) 

F7   	4.56422(8)   0.8(1) 

3cTIC 348607991 

F1   	4.58166(2)   3.9(2) 

F2   	1.96881(8)   1.2(2) 

F3   	5.01497(8)   1.2(2) 

F4   	5.39336(9)   1.1(2)

3cTIC 348668924 

F1   	5.54861(3)   	 6.2(4) 

F2   	5.05848(8)   	 2.4(4) 

3cTIC 348671634 

F1   	4.41466(4)   	 3.9(3) 

F2   	4.76344(9)   	 1.8(3)  

3cTIC 349332755 

F1   	7.64114(1)   	 4.1(2) 

3cTIC 357853776 

F1   	10.257111(6)   	 5.5(2) 

3cTIC 360063836 

F1   	5.139906(5)   	 8.0(2) 

F2   	5.52154(2)   	 2.2(2) 

F3   	6.14280(1)   	 3.6(2) 

F4   	4.44844(2)   	 1.5(2) 

F5   	5.71066(3)   	 1.5(2)  

F6   	5.55505(3)   	 1.1(2) 

3cTIC 361324132 

F1   	6.568133(3)   10.1(1) 

F2   	6.88566(1)   3.1(1) 

F3   	6.19274(2)   1.9(1)

F4   	6.35290(2)   1.6(1)

F5   	6.56536(2)   1.8(1) 

F6   	5.82671(3)   1.2(1)

F7   	7.05478(3)   0.9(1) 

F8   	8.21035(3)   1.0(1) 

3cTIC 370128780 

F1   	4.88959(7)   	 1.6(2)

F2   	0.10620(8)   1.5(2) 

3cTIC 372724051 

F1   	5.263577(6)   	 19.9(2) 

F2=2F4   	1.34570(1)   	 9.8(2) 

F3   	5.28665(2)   	 6.3(2) 

F4   	0.67285(1)   	 4.4(2) 

F5   	6.90514(8)   	 1.5(2) 

F6=2F1   	10.52715(1)   	 0.9(2) 

3cTIC 374038418 

F1   	5.73406(6)   1.6(2) 

3cTIC 377088966 

F1   	4.229863(4)   9.0(2) 

F2   	4.216205(7)   5.9(2) 

F3   	4.49732(2)   2.5(2)

3cTIC 378429048 

F1   	6.525448(5)   	6.4(1)

3cTIC 389532846 

F1   	4.32917(1)   8.7(2) 

F2   	4.33116(4)   3.1(2) 

3cTIC 391082033 

F1   	9.396502(8)   	 24.3(8) 

3cTIC 391836737 

F1   	6.193273(1)   12.36(8)

F2   	6.09952(2)   1.15(8) 

F3=2F1   	12.386546(2)   0.64(8)

3cTIC 392965683 

F1   	6.04430(2)   12.7(7)

F2   	6.12764(5)   4.2(7) 

F3   	6.81849(5)   4.3(7) 

3cTIC 393662110 

F1   	6.085935(2)   17.5(1) 

F2   	5.914236(5)   6.5(1) 

F3   	6.44171(1)   2.7(1) 

F4   	7.23376(1)   2.4(1) 

F5=2F1   	12.171870(4)   1.5(1) 

F6   	6.26979(2)   1.2(1) 

F7   	6.34677(3)   1.1(1) 

3cTIC 399436828 

F1   	5.15360(5)   5.5(4)†

3cTIC 400852783 

F1   	6.88034(1)   8.9(3) 

F2   	7.32561(1)   5.9(3) 

F3   	7.15369(4)   2.0(3) 

3cTIC 419354107 

F1   	4.974058(3)   29.5(3) 

F2   	4.94025(2)   5.5(3) 

F3=2F1   	9.948117(6)   4.1(3) 

F4=3F1   	14.92218(1)   2.6(3) 

F5=4F1   	19.89623(1)   1.8(3)

F6   	4.90630(2)   4.0(3) 

3cTIC 421117635 

F1   	5.21831(3)   4.4(2) 

F2   	4.73831(8)   1.5(2) 

3cTIC 445619007 

F1   	5.21307(6)   1.7(2) 

F2=2F4   	1.26348(8)   1.1(2)

F3=4F4   	2.5270(1)   1.2(2) 

F4   	0.63174(4)   0.6(2) 

3cTIC 451932686 

F1   	9.49288(2)   1.2(1) 

3cTIC 452018494 

F1   	8.654173(7)   4.0(1) 

3cTIC 461607866 

F1   	6.652979(6)   6.3(1) 

F2   	6.279407(6)   6.0(1) 

F3   	6.187924(8)   4.9(1) 

F4   	6.58081(1)   3.5(1) 

F5   	6.71918(1)   2.8(1)

F6   	7.77815(3)   1.3(1) 

F7   	6.24561(4)   1.0(1) 

3cTIC 469221047 

F1   	4.442633(7)   12.2(2) 

F2   	4.404679(7)   12.2(2) 

3cTIC 469223889 

F1   	7.84158(3)   1.1(1)

F2   	8.35141(5)   0.7(1)

F3   	6.79727(5)   0.7(1)

F4   	1.11389(5)   0.7(1)







 §.§ Candidate stars

lcr  
Frequencies and amplitudes determined for the Candidate stars. Formal error estimates determined according to <cit.> are given in braces in units of the last significant digit. †Amplitudes may be largely suppressed.

8
 
ID     Freq.        Amp.

      (d^-1)     (mmag)

3cTIC 92193 

F1   	5.97644(5)   1.6(2)

3cTIC 11158867 

F1   	12.91477(8)   2.0(3) 

F2   	1.54085(9)   1.8(3) 

3cTIC 12249117 

F1   	3.28913(1)   3.0(1) 

3cTIC 12647534 

F1   	3.51179(2)   5.7(3) 

F2   	1.24173(2)   5.5(3)

F3   	0.97933(7)   1.9(3) 

F4   	1.25678(8)   1.8(3)

F5   	1.27325(9)   1.4(3) 

3cTIC 13839931 

F1   	4.95417(6)   4.3(5) 

3cTIC 13971092 

F1   	9.69457(4)   1.8(3) 

3cTIC 13973539 

F1   	3.502964(3)   9.5(1)

F2   	1.38376(1)   2.7(1) 

F3   	4.83592(2)   1.2(1)

F4=2F1   	7.005929(6)   0.7(1) 

3cTIC 28949811 

F1   	13.12702(7)   1.2(2) 

3cTIC 29036690 

F1   	7.92305(5)   0.7(1) 

3cTIC 29598925 

F1   	4.01099(8)   4.0(3) 

F2   	2.24307(7)   4.5(3) 

F3   	0.7733(1)   3.1(3) 

F4   	1.5457(1)   2.2(3)

F5   	1.9355(1)   2.5(3)

3cTIC 30569481 

F1   	5.578126(6)   5.29(9) 

F2   	2.59672(2)   1.88(9)

F3=F2-F1   2.98140(2)   1.64(9) 

F4   	5.08676(3)   1.05(9) 

3cTIC 43301361 

F1   	8.849477(8)   3.02(9) 

F2   	11.13493(2)   1.31(9)

F3   	0.85774(2)   1.32(9) 

F4   	0.20085(3)   0.89(9) 

F5   	0.30264(3)   0.75(9) 

F6=2F3   	1.71548(3)   0.70(9) 

3cTIC 49721269 

F1   	11.64652(1)   1.3(2) 

F2   	5.82174(1)   1.2(2) 

3cTIC 53709049 

F1   	6.61713(9)   6.9(9) 

F2   	5.0123(1)   5.9(9) 

3cTIC 53961302 

F1   	9.37902(1)   1.5(3) 

F2   	1.03619(1)   1.4(3) 

3cTIC 53968977 

F1   	0.76616(6)   8.1(5) 

F2   	6.0136(1)   4.1(5)

3cTIC 60245596 

F1   	6.44274(3)   1.5(1)

F2   	3.18623(4)   1.1(1) 

F3   	11.03042(6)   0.8(1) 

3cTIC 65516748 

F1   	8.54807(7)   1.6(3) 

3cTIC 72696935 

F1   	7.360422(8)   13.3(2) 

F2   	11.04063(2)   1.1(2)

3cTIC 72944678 

F1   	3.32638(7)   10(1)

3cTIC 74197071 

F1   	2.96766(2)   4.7(2) 

F2   	3.01456(5)   1.7(2) 

F3   	5.76888(6)   1.3(2) 

3cTIC 78499882 

F1   	3.72163(1)   2.7(1) 

F2   	3.69110(2)   1.6(1) 

3cTIC 80814494 

F1   	5.40452(3)   2.2(2) 

3cTIC 93923487 

F1   	3.44624(3)   1.25(9) 

F2   	1.90157(3)   1.23(9) 

3cTIC 94000461 

F1   	4.545041(3)   15.1(1)

3cTIC 114249288 

F1   	3.133591(9)   4.0(2)

F2   	1.53094(1)   3.7(2) 

F3   	1.52246(2)   2.2(2) 

F4=F2+F3   	3.05339(2)   1.5(2)

3cTIC 123036723 

F1   	4.781420(8)   4.3(1) 

F2   	2.365317(9)   3.7(1)

F3   	2.33445(2)   2.1(1) 

F4   	2.44625(2)   1.5(1)

3cTIC 123828144 

F1   	5.52537(2)   1.02(7) 

F2   	0.96250(3)   0.77(7) 

3cTIC 137489662 

F1   	11.51964(1)   1.59(8) 

3cTIC 140309502 

F1   	7.13915(1)   3.3(1) 

F2   	0.07535(4)   0.8(1) 

F3   	0.15069(8)   0.5(1) 

F4   	0.2260(1)   0.5(1)

3cTIC 140429699 

F1   	6.17558(3)   1.6(1) 

3cTIC 141190209 

F1   	4.74596(5)   1.5(2) 

3cTIC 141903641 † 
 
F1   	5.29110(1)   5.9(2) 
 
F2   	0.23796(2)   3.2(2) 
 
F3   	0.14353(4)   1.3(2) 
 
F4   	6.13873(5)   1.1(2) 
 
3cTIC 143530557 

F1   	3.23172(1)   4.1(2) 

F2   	1.57798(3)   1.4(2) 

F3   	3.24230(4)   1.2(2) 

F4   	3.48728(4)   1.1(2) 

3cTIC 145672806 

F1   	3.16275(4)   1.8(2) 

3cTIC 155977294 

F1   	4.44906(1)   1.56(9) 

F2   	2.05883(2)   1.31(9) 

F3   	2.57197(3)   0.73(9) 

3cTIC 172560369 

F1   	8.90489(3)   2.5(3)

3cTIC 184226481 

F1   	3.70079(2)   4.5(3) 

3cTIC 190783321 

F1   	15.59057(4)   1.0(1) 

F2   	21.16694(5)   0.8(1) 

F3   	14.28699(5)   0.8(1) 

3cTIC 193573033 

F1   	3.55629(2)   2.7(2) 

3cTIC 193608395 

F1   	6.93971(3)   2.5(3) 

F2   	3.39643(3)   2.3(3) 

3cTIC 207045768 

F1   	6.13987(2)   2.5(2)

F2   	2.77901(2)   2.5(2)

F3=F1-F2   	3.36086(3)   1.9(2)

3cTIC 220238856 

F1   	3.71927(2)   10.9(8)

F2   	1.69782(3)   8.9(8) 

F3   	4.41429(3)   8.6(8) 

F4   	3.29601(3)   7.2(8) 

3cTIC 220298408 

F1   	6.08901(2)   5.1(3) 

3cTIC 226144867 

F1   	12.67603(3)   6.4(7) 

3cTIC 231149746 

F1   	9.05289(5)   2.9(5) 

F2   	12.23358(6)   2.5(5) 

3cTIC 231177417 

F1   	5.90535(6)   6(1) 

3cTIC 231236273 

F1   	9.66445(4)   2.4(3) 

3cTIC 244327575 

F1   	3.724081(2)   18.0(1)

F2=2F1   	7.448162(3)   2.7(1)

F3=3F1   	11.17224(5)   1.3(1)

F4   	0.61728(1)   2.1(1)

F5   	0.78466(2)   1.3(1)

F6=4F1   	14.896324(6)   0.6(1) 

3cTIC 252864874 

F1   	5.38477(4)   6.9(5) 

F2   	12.96472(8)   3.7(5) 

F3   	4.91754(9)   3.1(5) 

3cTIC 272625912 

F1   	3.30518(1)   11.6(2)

F2   	1.38055(2)   5.0(2)

3cTIC 281533292 

F1   	5.53994(3)   7.9(8) 

3cTIC 282737511 

F1   	3.215232(5)   6.9(1) 

F2   	0.72957(2)   1.7(1) 

F3   	0.27360(2)   1.5(1)

3cTIC 285122116 

F1   	7.9203(1)   1.1(2) 

3cTIC 285684866 

F1   	3.07295(2)   7.3(3) 

F2   	0.08417(2)   7.2(3) 

3cTIC 286352720 

F1   	6.06353(1)   3.6(1) 

F2   	5.99286(5)   0.7(1) 

3cTIC 290300414 

F1   	4.36798(3)   0.95(8) 

F2   	2.43643(4)   0.64(8)

F3   	5.41055(5)   0.61(8) 

3cTIC 294306184 

F1   	7.22638(6)   5(1) 

3cTIC 296449179 

F1=2F3   	5.967590(6)   9.2(2) 

F2   	1.95179(2)   2.5(2) 

F3   	2.983795(3)   2.6(2) 

3cTIC 297264447 

F1   	8.78504(4)   1.4(2) 

3cTIC 307944768 

F1   	5.89021(5)   1.2(2)

3cTIC 319302209 

F1   	3.383001(3)   8.5(4) 

F2   	2.687471(6)   4.6(4) 

F3   	1.880402(5)   5.1(4)

F4   	2.721681(6)   4.1(4) 

3cTIC 335484090 

F1   	3.18454(1)   18.1(3)

F2=2F9   	0.266751(8)   6.3(3) 

F3=6F9   	0.80025(2)   6.1(3) 

F4=4F9   	0.53350(2)   5.6(3) 

F5=8F9   	1.06700(3)   5.4(3) 

F6=10F9   	1.33375(4)   4.7(3) 

F7=12F9   	1.60050(5)   3.7(3) 

F8=14F9   	1.86725(6)   3.6(3) 

F9   	0.133375(4)   2.8(3) 

F10=16F9   	2.13400(6)   3.0(3) 

F11=5F9   	0.66688(2)   2.6(3) 

F12=18F9   	2.40076(7)   2.2(3) 

3cTIC 345652701 

F1   	3.18286(3)   2.4(2) 

3cTIC 347585038 

F1   	3.64383(3)   3.1(2) 

F2   	0.49554(5)   2.0(2)

F3   	1.41879(5)   1.8(2) 

3cTIC 348609224 

F1   	3.95599(8)   1.5(2) 

3cTIC 360749347 † 
 
F1   	4.88831(2)   	 12(1) 
 
3cTIC 364146227 

F1   	3.09012(3)   5.6(4) 

F2   	1.68288(5)   2.9(4) 

3cTIC 366108295 

F1   	12.95685(9)   	 2.0(3) 

3cTIC 368237682 

F1   	7.28839(5)   1.9(2)

F2   	0.37825(7)   1.4(2) 

F3   	1.83304(8)   1.1(2)

F4   	7.54582(8)   1.2(2) 

F5   	1.63789(8)   1.1(2) 

F6   	1.7997(1)   0.8(2) 

3cTIC 369708912 

F1   	3.25928(3)   2.5(2)

F2   	2.30628(3)   2.0(2) 

3cTIC 370269139 

F1   	5.91020(9)   1.5(3)

3cTIC 372115570 

F1   	3.96205(2)   4.0(2) 

3cTIC 374696382 

F1   	5.77910(4)   3.6(2) 

F2   	0.30931(8)   1.7(2)

F3   	0.28025(8)   1.6(2) 

3cTIC 379932247 

F1   	8.30337(4)   2.4(4)

3cTIC 384257658 

F1   	3.69970(2)   1.86(9) 

F2   	3.65490(4)   0.90(9) 

3cTIC 384540878 

F1   	3.55128(4)   3.6(4) 

3cTIC 386513392 

F1   	3.12176(3)   1.6(1) 

3cTIC 386693012 

F1    13.597032(2)   7.2(1) 

F2    16.249506(8)   2.3(1) 

F3=F2-F1    2.652474(8)   2.2(1) 

F4=2F1    27.194064(5)    0.9(1) 

F5=F1+F2    29.846538(8)   0.6(1) 

F6    13.60250(2)   0.9(1) 

3cTIC 387153140 

F1   	11.32157(3)   2.1(2) 

F2   	1.88019(4)   1.5(2) 

F3=F1+F2   	13.20176(4)   1.2(2) 

3cTIC 400080677 

F1   	9.02070(6)   0.6(1) 

3cTIC 400533469 

F1   	11.1849(1)   4.5(8)

3cTIC 401847213 

F1   	5.1564(1)   4.8(8) 

3cTIC 408941991 

F1   	4.61682(1)     1.5(1)

F2   	2.29288(2)     1.1(1)

3cTIC 408991617 

F1   	5.77126(2)   1.4(1) 

3cTIC 419246605 

F1   	8.02047(9)   1.3(2) 

3cTIC 420545430 

F1   	3.31306(7)   2.5(3) 

F2   	1.4800(1)   1.7(3) 

3cTIC 421691939 

F1   	6.01647(7)   3.3(4) 

F2   	5.73585(9)   2.7(4) 

3cTIC 422533344 † 
 
F1   	5.39483(7)   3.9(5) 

F2   	6.15953(9)   2.9(5) 

3cTIC 427396133 

F1   	5.90994(2)   5.8(3)

F2   	6.10060(3)   3.8(2)

3cTIC 430625041 † 
 
F1   	5.7728(1)    	 2.3(3) 
 
3cTIC 440971753 

F1   	3.17120(7)   4.1(3)

F2   	1.7627(1)   2.4(3) 

F3   	3.1851(1)   2.4(3) 

F4   	0.35458(1)   2.7(3) 

3cTIC 447933173 

F1   	5.46811(1)   3.9(1) 

F2   	5.82001(2)   2.8(1) 

F3   	2.70908(2)   2.3(1)

F4   	5.80719(3)   1.7(1) 

3cTIC 458911894 

F1   	3.87623(3)   2.5(2) 

F2   	3.85813(5)   1.6(2) 

F3   	3.89609(5)   1.5(2) 

3cTIC 459014234 

F1   	11.78938(1)   10.5(2)

F2   	13.58245(3)   3.7(2) 

F3   	11.01875(4)   3.0(2)

F4   	10.78396(5)   2.4(2) 

F5   	13.79750(9)   1.4(2) 
 
3cTIC 459105076 

F1   	10.92534(4)   2.3(2)

3cTIC 469095496 

F1   	8.00798(3)   4.2(3) 







 §.§ Rejected stars


lcr  
Frequencies and amplitudes determined for the rejected stars. Formal error estimates determined according to <cit.> are given in braces in units of the last significant digit.

9
 
ID     Freq.        Amp.

      (d^-1)     (mmag)

3cTIC 12647620 
 
F1   	3.51173(5)   4.8(4) 

F2   	1.24177(8)   3.0(4) 

3cTIC 26283875 
 F1   	14.24270(9)   0.8(1) 
 
3cTIC 28709025 
 F1   	5.48688(6)   1.9(1) 
 
F2   	5.5341(1)   0.7(1) 
 
F3   	4.9785(2)   0.7(1) 
 
3cTIC 40102236 
 F1   	5.239879(8)   3.0(1) 
 
F2   	2.76522(3)   0.9(1) 
 
3cTIC 60320306 
 F1   	7.01910(4)   0.80(9) 
 
3cTIC 67985749 
 F1   	6.34398(5)   1.5(2) 
 
3cTIC 90134626 
 F1   	2.98520(2)   1.5(1) 
 
F2   	3.65605(3)   1.1(1)
 
3cTIC 93549165 
 F1   	3.97459(7)   0.69(6) 
 
3cTIC 102161004 
 F1   	3.34360(3)   1.2(1) 
 
F2   	4.19498(5)   0.6(1) 
 
3cTIC 118680798 
 F1   	4.61715(3)   0.65(7) 
 
3cTIC 123754451 
 F1   	3.43280(3)   0.80(7) 
 
F2   	2.72317(3)   0.73(7) 
 
F3   	4.24874(3)   0.74(7) 
 
F4   	5.62140(4)   0.58(7) 
 
F5   	4.49144(5)   0.48(7) 
 
3cTIC 138905907 
 F1   	8.65749(1)   11.9(5)
 
F2   	12.46790(2)   5.5(5)
 
F3   	7.77313(3)   4.9(5) 
 
F4   	13.55768(4)   3.5(5) 
 
3cTIC 141903541 
 
F1   	5.29110(1)   5.9(2) 

F2   	0.23796(2)   3.2(2) 

F3   	0.14353(4)   1.3(2) 

F4   	6.13873(5)   1.1(2) 

3cTIC 157535787 
 F1   	12.58931(2)   6.4(2)
 
F2   	1.27797(3)   3.5(2) 
 
3cTIC 162012064 
 F1   	22.18628(3)   2.2(2) 
 
F2   	19.71143(3)   1.8(2) 
 
F3   	24.07994(4)   1.5(2) 
 
3cTIC 264485563 
 F1   	9.08388(6)   0.8(1) 
 
3cTIC 281803267 

F1   	3.91390(2)   19(1)

3cTIC 291556636 
 F1   	3.71521(2)   4.0(2) 
 
F2   	1.84478(2)   3.5(2) 
 
F3   	3.67380(3)   2.6(2)
 
F4   	2.98491(5)   1.5(2) 
 
3cTIC 352529679 
 n/a 
 
3cTIC 360661624 
 
F1   	4.88831(2)   	 12(1) 

3cTIC 377498419 
 F1   	18.69049(3)   7.0(5) 
 
F2   	9.34525(2)   2.8(5)
 
F3   	28.03574(4)   1.4(5) 
 
F4   	37.38098(6)   1.1(5)
 
3cTIC 384992041 
 F1   	3.76144(1)   44.5(8)
 
F2=2F1   	7.52289(2)   6.4(8) 
 
3cTIC 417438983 
 F1   	4.00826(2)   3.3(2) 
 
3cTIC 422533347 
 
F1   	5.39483(7)   3.9(5) 

F2   	6.15953(9)   2.9(5) 

3cTIC 424032547 
 F1   	5.02512(2)   3.5(3) 
 
3cTIC 424032634 
 F1   	7.03050(2)   1.4(1) 
 
F2   	2.40547(3)   1.2(1) 
 
3cTIC 426520557 
 F1   	17.123158(6)   2.07(7) 
 
F2   	12.96614(1)   1.36(7)
 
F3   	15.14342(1)   1.20(7) 
 
F4   	14.64399(2)   0.64(7) 
 
3cTIC 430625174 

F1   	5.7728(1)   2.3(3) 

3cTIC 434178307 
 F1   	5.9868(1)   1.9(4) 
 
F2   	16.7695(1)   1.9(4) 
 
3cTIC 446041643 
 F1   	4.483797(5)   5.3(1)
 
F2   	4.164086(8)   3.3(1) 
 
F3   	4.18027(2)   1.4(1) 
 






aasjournal


