Catalogue of BRITE-Constellation targets I. Fields 1 to 14 (November 2013 - April 2016)

The BRIght Target Explorer (BRITE) mission collects photometric time series in two passbands aiming to investigate stellar structure and evolution. Since their launches in the years 2013 and 2014, the constellation of five BRITE nano-satellites has observed a total of more than 700 individual bright stars in 64 fields. Some targets have been observed multiple times. Thus, the total time base of the data sets acquired for those stars can be as long as nine years. Our aim is to provide a complete description of ready-to-use BRITE data, to show the scientific potential of the BRITE-Constellation data by identifying the most interesting targets, and to demonstrate and encourage how scientists can use these data in their research. We apply a decorrelation process to the automatically reduced BRITE-Constellation data to correct for instrumental effects. We perform a statistical analysis of the light curves obtained for the 300 stars observed in the first 14 fields during the first ~2.5 years of the mission. We also perform cross-identification with the International Variable Star Index. We present the data obtained by the BRITE-Constellation mission in the first 14 fields it observed from November 2013 to April 2016. We also describe the properties of the data for these fields and the 300 stars observed in them. Using these data, we detected variability in 64% of the presented sample of stars. Sixty-four stars or 21.3% of the sample have not yet been identified as variable in the literature and their data have not been analysed in detail. They can therefore provide valuable scientific material for further research. All data are made publicly available through the BRITE Public Data Archive and the Canadian Astronomy Data Centre.


Introduction
The BRIght Target Explorer (BRITE) Constellation 1 is the first nano-satellite mission to study the structure and evolution of the brightest stars in the sky.Providing photometric time series in two passbands for up to half a year continuously, BRITE-Constellation data are used to study different types of stellar variability, such as pulsations, wind phenomena, the feeding of decretion disks around Be stars, binarity, and rotational modulation (e.g.Weiss et al. 2021).A majority of the brightest stars are also some of the most massive and most luminous objects in the Milky Way.Consequently, a large fraction of the sample observed by BRITE-Constellation consists of stars with spectral types O and B. An overview of the BRITE-Constellation mission, including its history and selected scientific highlights, is provided in Weiss et al. (2021).
The BRITE-Constellation mission originally included six 20 cm cube-shaped nano-satellites that were funded by three countries (Austria, Canada, and Poland).Each satellite has a mass of about 7 kg, is stabilised on three axes, has access to almost the entire sky, and carries a 3 cm telescope that feeds an uncooled CCD detector (Weiss et al. 2014).Each partner country contributed a pair of BRITE satellites that were deployed into low Earth orbits, with one satellite equipped with a custom-defined red filter (transmitting in the range 550 -700 nm) and the other with a custom-defined blue filter (390 -460 nm).Five of the six nano-satellites were operational after launch; the sixth, named BRITE-Montréal, did not separate from the upper stage of its rocket and, hence, was never active.The BRITE-Constellation therefore consists of three satellites with a red filter, named BRITE-Toronto (BTr), UniBRITE (UBr), and BRITE-Heweliusz (BHr), and two satellites equipped with a blue filter, named BRITE-Austria (BAb) and BRITE-Lem (BLb).The 'r' and 'b' at the end of the abbreviations indicate whether the satellite is equipped with a red or blue filter, respectively.The paper by Pablo et al. (2016) provides more details on the detectors and the pre-launch and in-orbit tests.Popowicz et al. (2017) described the pipeline that was used to process the observed images, giving the instrumental magnitudes that were originally provided to users.
The nominal goal of the BRITE-Constellation mission was to observe stars brighter than V ∼ 4 mag, but the first observations showed that scientifically useful photometry could be easily obtained for stars down to V ∼ 6 mag.The faintest star ever observed by BRITE was the M-type subgiant HD 96265, with V = 8.03 mag.In addition, BRITE collected data for two novae, Nova Carinae 2018 (V906 Car) and Nova Reticulum 2020 (YZ Ret), which were tracked by red-filtered BRITE satellites until their V magnitudes dropped to about 9.8 mag and 8.7 mag, respectively.The brightest BRITE target was Canopus (α Car), with V = −0.72 mag.Despite the intentional large and position-dependent blurring of the images, all stars brighter than V ∼ 1 mag saturated the detectors when the integration times were of the order of 1 second.The light curves of saturated stars can still be used if the decorrelation parameters are chosen correctly, as the saturation is analogue.This means that the fullwell electron capacity of a pixel is translated into a digital signal smaller than the maximum allowed.The total flux from a star can therefore be measured, despite the overflow of charge to neighbouring pixels.
The field of view of each satellite is approximately 24 × 20 degrees, allowing observations of fields with typically 15 -20 bright stars, at least three of which must be brighter than V = 1 http://www.brite-constellation.at 3 mag.The observed fields are named according to the celes-63 tial constellations covered by them and numbered consecutively.64 A given field is observed for at least 15 minutes in each ∼100-65 minute orbit for up to six months (Weiss et al. 2014).Obser-66 vations of several fields are repeated every year (for example, 67 the Orion field), which currently results in observations cover-68 ing nine consecutive seasons for some objects.Table 1 lists the 69 names and properties of the first 14 fields, which are the subject 70 of this publication.

71
Since the launch of the first two BRITE satellites in Febru-72 ary 2013, a total of 716 stars contained in 64 fields have been 73 observed to date with publicly released data.Most of the stars 74 observed by the BRITE satellites have also been targeted by the 75 National Aeronautics and Space Administration Transiting Ex-76 oplanet Survey Satellite (TESS) mission (Ricker et al. 2015).A 77 combination of BRITE and TESS data provides a fruitful syn-78 ergy and excellent complementarity.Due to the different pass-79 bands used by BRITE-Constellation and TESS, a combination 80 of the data allows colour information to be extracted for the tar-81 gets.While the per-observation accuracy of TESS is much better 82 than that of BRITE, many of the much longer BRITE time series 83 with higher cadences provide a better frequency resolution.For 84 example, BRITE data can be very useful for studying pulsations 85 in binary systems based on Doppler shifts if the assignment of 86 frequencies to one of the two components is not clear.

87
In the present paper, the first in a series of three catalogue 88 papers in which we discuss all BRITE mission data, we pro-89 vide an overview of the astrophysical content of the BRITE-90 Constellation data obtained from the first 14 fields2 .The main 91 motivation for publishing this catalogue is to raise awareness 92 of the BRITE-Constellation data and its properties and to en-93 able non-experts to use it for reliable quantitative studies.The 94 present section introduces the BRITE-Constellation mission.In 95 Sect. 2 we discuss the properties of the BRITE data, including 96 statistical information on the first 14 BRITE fields.Section 3 is 97 devoted to a discussion of the variability of selected objects and 98 general information on the known variability.More details on 99 the BRITE-Constellation data, notes on data for the 300 stars in 100 Fields 1 -14, maps of the individual fields, and additional sup-101 plementary information are given in the appendices.The work is 102 summarised in Sect. 4. 103

Properties of the BRITE-Constellation data 104
In this first part of the BRITE-Constellation catalogue, we 105 present the data obtained in the first 14 BRITE fields, which were 106 observed between November 2013 and April 2016.The selec-107 tion of these particular fields for the first part of the catalogue is 108 based on the version of the BRITE data reduction pipeline that 109 was used for performing photometry on the BRITE CCD im-110 ages.For these 14 fields, the raw data include a reduced number 111 of decorrelation parameters.The format of these Data Release 112 2 (DR2), 3 (DR3), and 4 (DR4) data is described by Popowicz 113 et al. (2017). 3Within these first 14 fields, 300 individual stars 114 were observed; 208 of these more than once.Table 1 details  Data for the first 14 BRITE fields are available through the BRITE Public Data Archive (PDA) and the Canadian Astronomy Data Centre (CADC).The BRITE data were first processed through a reduction pipeline described by Popowicz et al. (2017).As they suffer from various instrumental effects (Pigulski et al. 2018c), a procedure called 'decorrelation' had to be applied (Sect.2.2).This procedure corrects the BRITE data for the strongest instrumental effects.The BRITE team has decorrelated the data for the 14 fields in question and these data are now available through the BRITE PDA and CADC.The decorrelated data form the basis for the results presented here.Detailed information about the BRITE data in the archives can be found in Appendix C.
The following is a brief overview of the BRITE observing modes, the necessary decorrelation process, and the properties of the data discussed here.
2.1.Observing modes: Stare mode versus chopping mode BRITE-Constellation data in Fields 1 -14 were obtained using two different observing modes.Initially, the BRITE satellites maintained a fixed orientation in the sky and the stars in fixed positions on the CCD.This observing mode is called the stare mode.It was used for the first eight fields (see Table 1).After two years from the onset of the BRITE mission, it became clear 156 that the number of hot pixels on the detectors was increasing, 157 seriously affecting the photometry.Therefore, a new observing 158 mode, the chopping mode, was tested at the end of 2014.

159
In this mode, the satellite changes pointing slightly between 160 consecutive exposures.The shifts are small, about 9 on the sky 161 or about 20 pixels.This mode forced a change of the subraster5 162 size to slightly wider than in the stare mode (Pablo et al. 2016).163 The BRITE reduction pipeline was adapted to this observing 164 mode, as described by Popowicz et al. (2017).In this mode, con-165 secutive images from alternating positions are subtracted to pro-166 vide differential images, almost free of hot pixels, which are then 167 used to extract photometric time series.Some residual hot pixels 168 may still remain, as the dark current in the used CCD sensor ex-169 hibits random-telegraph-signal noise (more details are given in 170 Popowicz & Farah 2020).The first field for which the chopping 171 mode was applied was Field 5 (Perseus I), and regular observa-172 tions in this mode have been carried out from mid-2015 to the 173 present.Figure 1 and Table 1 show which observing mode was 174 used for each field.More details on the two observing modes and 175 the corresponding versions of the BRITE data reduction pipeline 176 are given by Popowicz et al. (2017).Some attempts to obtain 177 point-spread-function (PSF) photometry were made (Popowicz 178 2018), but this method has finally not been utilised in the official 179 datasets.180

Description of the decorrelation process 181
The raw BRITE data suffer from instrumental effects, the most 182 important of which is the dependence of the stellar PSF on 183 changes in the temperature of the optics (Pablo et al. 2016).184 Measuring through a fixed aperture leads to the raw magnitudes 185 being strongly dependent on both the temperature of the optics 186 and the position of the star on the detector.The temperature of 187 the optics is not measured and only the temperature of the de-188 tector is known.These two temperatures may differ.Therefore, 189 many parameters are introduced into the decorrelation process, 190

212
All BRITE data from Fields 1 -14 were decorrelated by sev-213 eral members of the BRITE team.At least three team members 214 examined each dataset presented here.The decorrelation proce-215 dure is semi-automatic, but the final result may vary depending 216 on how the extreme data in each parameter space were discarded 217 and which intrinsic variability model was adopted.the noise increased rapidly when the area at and near the star's 241 profile was 'polluted' by hot pixels.For some time the scatter remained at this higher level until TJD ∼ 1130.At this time, the scatter increased again by a significant amount persisting until the end of the observations in this field.These jumps in scatter occurred more frequently before chopping mode was introduced in 2015, which greatly mitigated such effects.
In the following paragraphs the data characteristics for the first 14 fields of BRITE-Constellation observations are described in detail.
Field 1: The Orion I (Ori-I-2013) field was the first field in which a regular campaign following the commissioning phase of UBr and BAb was carried out.UBr was able to achieve stable pointing at the beginning of November 2013 and maintained it for a number of orbits.Consistent stability and hence data collection by both UBr and BAb began on 12 December 2013 and continued until the end of the planned observing time in mid-March 2014.All observations were performed in stare mode.Exposure times for both BAb and UBr were mostly set to one second, providing a high signal-to-noise ratio for most of the 15 stars selected in this field.Due to their brightness, α Ori (Betelgeuse) and β Ori (Rigel) caused saturation in the CCD images.The former star was saturated only in the red-filter UBr images, and the latter in both the red-filter UBr and blue-filter BAb images.
Field 2: The Centaurus I (Cen-I-2014) campaign was scheduled for full coverage by UBr and BAb in stare mode, starting in late March and early April 2014, respectively.UBr was set up to observe 30 stars; BAb initially observed 29 stars.However, data transfer to European ground stations was severely hampered by interference, so that the number of stars in the BAb setup was re-  5) in mmag (top number) and subtracted offsets in mag (bottom number).The light curve illustrates some instrumental effects, such as a different amount of scatter, gaps in data, offsets, and long-term trends.These effects result in the presence of very low frequencies in the FS reproduced close to the satellite's orbital frequency of 14.66 d −1 and its multiples.duced to 14 for the full time base.For the remaining stars, only the Orion II field were started by BAb and BTr, they were joined shortly after launch on 10 November 2014 by BHr, and finally BLb also joined on 12 December 2014 (Fig. 1).All satellites operated in stare mode.BAb also observed the Per I field regularly on each orbit again to test the capability of observing two fields per orbit.This test was stopped after 45 d due to a lack of fine pointing for about 50% of the orbits.Images of α Ori in the red filter (BTr and BHr) and β Ori in the red and blue filters were saturated.
Field 7: The Vela/Puppis I (VelPup-I-2014) field was observed by BAb and BTr starting in December 2014 in stare mode, which was changed to chopping mode in February 2015 for testing purposes.For the first four weeks, BAb combined observations with the Per I field, which showed better performance compared to previous tests.The chopping mode generally gave better noise levels, with a few specific exceptions described in the notes on individual stars.
Field 8: The Vela/Pictor I (VelPic-I-2015) field was the first test to verify that stars located relatively far (up to 31 • in this case) from the Galactic plane could be observed with a BRITE satellite.BHr operating in stare mode was assigned to observe this field.The pointing stability was poor at the beginning, but improved over time and overall good data were collected for 20 stars over almost 80 d.
Field 9: The Scorpius I (Sco-I-2015) field was the first observing run in which all satellites operated in chopping mode.UBr and BLb were assigned to this campaign for the entire observing run and BAb and BHr for shorter periods.The BAb data generally do not have good time coverage due to frequent failures to achieve fine pointing in this field.
Field 10: The Cygnus II (Cyg-II-2015) field was the second campaign for which all satellites were operating in chopping mode.UBr and BTr were assigned to this field for the entire observing period, while BAb and BLb provided shorter coverage.UBr and BAb had Sco I as an alternate field for scheduled observations.The performance of BAb was generally quite poor in terms of data production and quality.
Field 11: The Cassiopeia/Cepheus I (CasCep-I-2015) campaign was started with BAb, BHr and BLb.All three satellites had problems achieving fine pointing on many orbits.After about two months, observations by these three satellites were suspended.A few weeks later, observations of the Cas/Cep I field   5. To calculate absolute V magnitudes, M V , the apparent V magnitudes were taken from the catalogue of Paunzen (2015) or, if lacking in this catalogue, from the SIMBAD 7 database.They were transformed to absolute magnitudes using photo-geometric distances derived by Bailer-Jones et al. (2021) and based on the Gaia Early Data Release 3 (Gaia Collaboration et al. 2021) parallaxes.If the Gaia distances were lacking or unreliable (this was the case for about 30% of the stars in our sample), we used Hipparcos parallaxes (van Leeuwen 2007).The total absorption, A V , was estimated from the Gaia-2MASS three-dimensional map of absorption (Lallement et al. 2019) using their online tool 8 .The observed (B − V) colour indices were taken primarily from van Leeuwen (2007).If not available in this catalogue, they were taken from the SIMBAD database.Calculating E(B − V) colour excesses, we adopted a total-to-selective absorption ratio of A V /E(B−V) = 3.1.De-reddened colours shown in Fig. 5 were calculated as As can be seen from this figure, all stars from our sample are more luminous than the Sun.BRITE-Constellation prioritises the brightest stars in the sky, as can be seen in the histograms of V magnitudes of stars observed in blue and red BRITE passbands (Fig. 6).The median V magnitude of stars for our sample amounts to 4.10 mag.In Fig. 7, we show the distribution of spectral types (references are provided in the footnotes to Table A.1) observed in Fields 1 -14.It can be seen that, as mentioned in Sect. 1, the sample of BRITE stars is dominated by stars with the earliest spectral types, O and B. These stars account for 62% of the sample.

Known variability and VSX
For the sample of 300 BRITE stars discussed in this paper, we checked whether or not any variability has been found in the past or can be seen in the BRITE data.The most complete source of information on the known stellar variability is currently The International Variable Star Index (VSX 9 ; Watson et al. 2016) catalogue maintained by The American Association of Variable Star Observers.The VSX catalogue was initially populated with the data from the General Catalogue of Variable Stars 10 (GCVS; Samus' et al. 2017), but has been and is being updated based on both published papers and users' analyses.The VSX classification scheme was inherited from the GCVS, but has been extended and adapted to the current state of knowledge on stellar variability.
The variability types for known variable stars at the time of writing this text are listed in the sixth column of Table A.1.The meanings of the individual classifications can be found on the VSX web page.If there is a '-' in the sixth column, it means that the star has an entry in the VSX catalogue, for example because it was suspected to be variable, but no variability type was assigned.If the sixth column contains abbreviation 'n.e.' meaning 'no entry', this means that the star has no entry in the VSX catalogue.There are 64 such stars in our sample.

Variability from BRITE data
The variability of many of the stars in our sample has already in which a visual inspection of the light curves was performed and frequency spectra were calculated, allow for general comments on the variability.For example, for some stars eclipses are visible, which allows the type of variability to be easily defined.
In most cases, however, this inspection only allowed us to conclude that a star was variable or that variability was not detected.
The variability classification of the stars in our sample, based on the BRITE data, takes into account the two above-mentioned sources of information on variability: published papers and the inspection of light curves and frequency spectra.This classification is presented in the seventh column of Table A.1.It follows the VSX catalogue classification system.For stars for which we did not detect variability based on the BRITE data from Fields 1 -14, a '-' appears in the seventh column.Stars for which we have detected variability but have not investigated the nature of this variability in detail are marked as 'VAR'.
In order to present in a simple way the results of our BRITEbased classifications for the sample analysed, we divided all stars into seven broad categories: (i) pulsating stars, (ii) binary stars, Next, three stars showed a likely rotational modulation in their BRITE data, in two cases associated with another type of variability (WR and ACYG), obtained the VSX class ROT (after 539 rotational variability).Figure 10 shows HD 50123 as an example 540 for a light curve with rotational modulation.

541
All other stars showing variability, but of as yet unidentified 542 type, were assigned to the VSX type VAR.One star was assigned 543 the VAR type in addition to the dominating eclipse light curve.544 The VAR class has also been assigned to stars showing long-545 term variability, mostly red giants.The variability they show is 546 usually difficult to characterise if observations are short in com-547 parison to the timescale of the variability as is often the case 548 for BRITE datasets.In total, there are 86 stars in our sample as-549 signed to the VAR class.

550
The numbers above give a total of 191 stars (64% of the sam-551 ple) included in one of the six categories for which variability 552 was found in the BRITE data.For the remaining 109 stars (36% 553 of the sample) we did not find variability.These stars are marked 554 by '-' in the seventh column of Table A.1.Many of them are 555 known to be variable stars, however, which means that either 556 the BRITE data are too short in duration, which resulted in a 557 poor detection threshold, or the data are of insufficient quality to 558 detect the reported variability.The proportion of the number of 559 stars of each category in the total sample of 300 stars observed 560 by BRITE-Constellation in Fields 1 -14 is illustrated in Fig. 11.561 562 For 125 stars (or 41.7% of the total sample), there is agree-563 ment between the variability classes available from VSX and 564 those inferred from the BRITE data analysis.We considered 565 both classifications to be in agreement also when we assigned 566 the class VAR based on the BRITE data and there was a more de-567 tailed classification in VSX.For 64 stars (21.3% of the sample), 568 the VSX does not have an entry that we could compare to.In 569 addition, there are 24 stars that have a VSX entry '-' or 'CST' 570 (constant stars that have previously been identified as variable, 571 but do not actually show any variability) for which no variability 572 was found in the BRITE data.

573
For 39 stars (13.0% of the sample), the BRITE data do not 574 reveal any variability, whereas in VSX they have been assigned 575 different types of variability.The reasons why these stars were 576 not found as variables in the BRITE data may be different.The 577 most likely reason is an insufficient quality of the BRITE data or 578 very short coverage.A good example is β Cep, the prototype of 579 a class of variable stars for which the BRITE data have a time 580 base that is too short and a data quality that is too poor to reveal 581 its variability.

582
For another 42 stars (14.0% of the sample), the classifica-583 tion based on BRITE data can be considered more reliable in 584 comparison to previous literature results.These are also stars for 585 which no variability type was assigned in VSX, but they were 586 found variable in the BRITE data.Finally, for 6 stars (2.0% of 587 the sample) the classifications from VSX and BRITE are differ-588 ent (see Table A.1.These are ε Cas, ψ Per, η Tau, η Ori, a Car, 589 and κ Cen).

591
In this paper describing the first part of the catalogue of stars ob-592 served by BRITE-Constellation, we discussed the data obtained 593 in the first 14 fields between November 2013 and April 2016 by 594 the five operational BRITE nano-satellites.The V magnitudes of 595 the 300 stars in this sample range from −0.72 to 6.91, showing 596 that the BRITE satellites were able to obtain photometry for stars 597 much fainter than the originally assumed limit of V = 4.0 mag.598 Of the 14 fields, all but Field 8 (VelPic-I-2015) were located in 599 the Galactic plane, as this ensures the availability of a significant 600   of 86 stars known to be variable from BRITE data, which has not been analysed in detail and has not yet been used in scientific work.For another 115 stars (38% of the sample), BRITE data have been used in publications.However, new data have been secured for many of them since the first analysis.For these stars, it is still possible to obtain new results and, in particular, to find low-amplitude variability not detectable in a shorter dataset (see Weiss et al. 2021 as an example).Another advantage of the BRITE data is the temporal coverage, which for some stars spans nine consecutive seasons.Such a long coverage greatly improves the resolution in frequency, which can be important, for example, for studies of stars with dense pulsation spectra, such as SPBtype stars.HD 33328 (λ Eri, Fields 6 and 13): Known Be star.Field 6: Observed with BAb, BHr, BTr and BLb.Variability detected in all datasets, although the strongest frequency peak is at ∼2.85 d −1 in the FS of the BHr data and at half of this frequency in the FSa of the BAb, BTr, and BLb data.HD 34085 (β Ori, Rigel, Fields 1, 6, and 13): Field 1: Observed with BAb and UBr.The acquired CCD subraster of this star is severely overexposed resulting in low quality data.Field 6: Observed with BHr, BTr, BLb and BAb.The available data show some long-period variability.Due to the brightness of the star, the images were saturated and the origin of the variability may be partly instrumental.Field 13: Observed with UBr and BAb.The UBr data again show some long-period variability.The BAb dataset is shorter and scarcer, but displays a similar behaviour to the UBr dataset.
HD 34503 (τ Ori, Fields 1, 6, and 13):   The FS of the BTr data shows clear variability with the strongest 1282 peak at a frequency of 1.8503 d −1 , but additional frequencies 1283 can also be seen.The BLb dataset is shorter, but confirms the 1284 variability detected from the BTr data.The BRITE data were studied in detail by Baade et al. (2018a).1297 HD 48917 (10 CMa, Field 12): Known Be star, observed 1298 with BTr and BLb.The FS of the BTr data shows strong vari-1299 ability with the strongest peak at a frequency of 1.3364 d −1 .It is 1300 evident that several more frequencies are present.The BLb data 1301 have two large gaps but confirm the variability found from the 1302 BTr data.The FS of the BTr data shows a frequency of 0.07 d −1 , which corresponds to twice the frequency of the known ellipsoidal variability (Sterken et al. 1994).The BLb dataset is shorter, but confirms this variability.HD 128898 (α Cir, Field 2): Known roAp star.Observed with BAb, UBr, BLb, and BTr.The FS of the BAb data has the strongest peak at 0.225 d −1 .The strongest peak in the FS of the UBr data is located at the harmonic of this frequency.The roAp pulsations are also clearly detectable in the UBr and BAb datasets.The BLb and BTr datasets are shorter, but their FSa confirm the strongest peak found from the BAb data and the roAp pulsations.All available BRITE data of this star were analysed by Weiss et al. (2016) and Weiss et al. (2020).

1876
HD 191610 (28 Cyg, Fields 4 and 10): This is a known Be star.Field 4: Observed with BTr and BLb.The datasets are short and scarce, but show some complex variability.Field 10: Observed with BLb, UBr, and BTr.The FSa of the data reveal complex Be-type variability with the main peak at a frequency of 1.377 d −1 .The BRITE data for this star have been studied in detail by Baade et al. (2018a).   of a single target in its central part in the case of stare mode.In chopping mode, a star is located either one or the other side of the rectangular subraster.In addition to the positions of the subrasters, the exposure time and the time between exposures has to be specified as well as the central right ascension, declination and the roll angle with respect to the optical axis.It is important that the stellar profile and a number of neighbouring background areas are fully rendered in each subraster even when the pointing changes slightly from exposure to exposure.Data obtained by a given satellite are split into parts, called setups.Each observing run starts with an initial setup number (1), which is the first attempt to acquire the selected stars properly in the defined subrasters.Very often this first setup needs to be changed or optimised, and, hence, a new setup is generated during an early phase of an observing campaign.Furthermore, when stars (and new subrasters) are added or removed, a new setup is generated and uploaded to the respective satellite.During some observing runs, a slow drift on the orientation of a given satellite over time had been apparent and, therefore, a resetting of the subraster was needed in order to keep the stellar profiles well in range of the subraster borders.Also, a change in exposure time or observing cadence always results in a new setup.Hence, during a full campaign for each satellite several setups might have been utilised.In some cases only two or three were used to collect data over up to 180 d but it can be up to seven or more if needed.Data can also be split into setups during the initial reductions, that is, on the ground (see Appendix A of Popowicz et al. (2017)).
New setups introduced during observations can have an effect on the integrity of a light curve (time, magnitude) after reduction and even decorrelation as described in this paper.When a new setup changes the position of the star in a subraster from (too) close to the border to centre (or accidentally in reverse), jumps in the signal levels can occur.Jumps can also occur as a result of the reduction, because each setup is processed independently and for each setup an independent aperture is defined.Therefore, if a setup covers only a short part of a long period variable star light curve, the reduction and decorrelation of such a small segment can result in serious offsets that do not reflect the real long-term variability of the object.If setups are generated during the initial process of data reduction, no offsets or other changes in data quality are introduced.In this case, the light curve is split only into two or more parts.
In particular during this first phase of the BRITE-Constellation mission, many individual setups were required for technical reasons (such as the very first observations conducted with the individual satellites that needed testing or the change from stare mode to chopping mode).In later years of the BRITE-Constellation mission, the number of setups decreased and were introduced more often by the reduction process that required splitting the data into parts.

Appendix C.3: Recommendations on combining individual setups and datasets from different BRITE satellites
The decorrelated photometric time series contain the Barycentric Julian date, instrumental magnitudes and magnitudes with the mean instrumental magnitude of the given setup subtracted (see the headers of the files stored in the archives for more information).In many cases, the time series stored as individual setups can just simply be stitched together (e.g. if the setups were generated during the reduction process) without any issues.However, very often different setups can have different mean magnitudes, which causes different offsets to be taken into ac-count when combining them into a full light curve.A good example is shown in Figure 2: individual setups are marked with vertical lines and the numbers on top of the light curve illustrate the offsets that were applied and the σ med orbit parameter as a measure for the data quality.
There are some cases where combining different setups needs a bit more care.For any type of a long-period variable, for example, stitching together the time series with the mean magnitude subtracted will not yield a reliable result.Introducing individual offsets by adding constants to a given setup might be necessary to cover the intrinsic variability of the star.

Fig. 1 :
Fig. 1: Distribution of observations by the five BRITE satellites for Fields 1 to 14.The satellites are colour-coded (see the legend).Data obtained in the stare and the chopping observing modes (see Sect. 2.1) are shown with unfilled and filled bars, respectively.

Fig. 2 :
Fig. 2: Typical photometric sequence observed by BTr during a single orbit (top left), during ten consecutive orbits (top right), and for 80 days (lower panel).Grey dots stand for individual measurements, and red dots indicate orbit averages.The presented photometry is for the Be star HD 56139 (ω CMa) observed by BTr in Field 12 (CMa/Pup I).

Fig. 4 :
Fig. 4: Values of σ med orbit plotted as a function of instrumental BRITE magnitude.Data for different BRITE satellites are shown with different colours.
has observed 300 individual targets in the first 14 fields.The (B − V) 0 colour versus absolute V magnitude diagram for these stars is shown in Fig.

Fig. 5 .Fig. 6 :
Fig. 5. V-filter absolute magnitudes (M V ) plotted as a function of de-reddened (B−V) 0 colours for 300 stars observed in BRITE Fields 1 -14.Stars of different spectral types are plotted with different colours, explained in the legend.The Sun symbol ( ) denotes the location of the Sun.

452Fig. 7 :
Fig. 7: Histogram of the spectral types of stars observed with BRITE in Fields 1 -14.WR stars are placed to the left of the O-type stars in a separate class 'WR'; the carbon star V460 Cyg is marked with 'C' and added to the right of the M-type stars.Blue bars (left sides) illustrate the numbers for the blue-filter observations conducted by BAb or BLb, while red bars (right sides) show the numbers for the red-filter observations carried out by UBr, BTr, or BHr.

(
Fig. 8.Given the observed sample of stars (Fig. 5), the pulsators are mostly located on the upper main sequence.In addition to these 46 pulsating stars, a further six (3 BCEP and 3 DSCT) also show pulsational variability, although they were classified as binaries because eclipsing or proximity effects dominate their light curves.A few stars included in the Be category also show g-mode variability, which classifies them as SPB stars.The category 'binary stars' refers to stars in which binarity was detected via variability, which included eclipsing binaries and stars showing proximity effects.We did not distinguish different types of eclipsing binaries assigning to all eclipsing stars a single designation, E. In total, we included 27 stars into this category, although two more eclipsing stars were included in the category of pulsating stars, as pulsations dominate their light curves.The binary star category includes 15 stars classified as E and 12 stars in which proximity effects dominate: ELL (ellipsoidal variables; 5 stars), HB (heartbeat stars; 5 stars), and R (close binaries showing reflection effect; 2 stars).In 11 stars from the binary star category, there is also an additional variability characteristic for other categories.As an example for the group of binaries, the blue (BAb and BLb) and red (BHr and BTr) data for HD 35411 (η Ori) are shown in Fig. 9. Be stars show variability on different timescales that are included in the VSX catalogue as short-period variability (LERI, λ Eridani stars) and large-amplitude long-term variability (GCAS, γ Cassiopeiae stars); less specific overall variability in Be stars is designated simply BE in VSX if the data were not sufficient to characterise the variability more precisely.Our sample includes 16 Be stars; Fig. 2 shows BRITE data for HD 56139 (ω CMa) as an example.Many Be stars also show pulsations in g-modes, which resulted in SPB-type variability being attributed to them as well.Of the 16 Be stars in our sample, four showed clear SPB-type pulsations.We included 13 stars into the category of stars showing stochastic variability.The category comprises variable blue supergiants, ACYG (α Cygni, 11 stars), Wolf-Rayet (WR) stars (1 star), and luminous blue variables, SDOR (S Doradus, 1 star).In addition, in four other stars the stochastic variability (3 stars classified as ACYG and one classified as WR) was associated with the dominating rotational or ellipsoidal modulation.Since stochastic solar-type oscillations do not have a separate variability class in VSX, we assigned a VAR class to stars that exhibit this type of variability, for example those studied by Kallinger et al. (2019). 590 Fig.8: BRITE-Constellation observations of the β Cephei pulsator HD 29248 (ν Eri) in Field 6. Top panels show observations gathered by the blue-filter satellites, BAb and BLb, and bottom panels observations with the red-filter satellites, BHr and BTr.Left panels show the full light curve, the middle panels illustrate a 13-day-long subset of the light curve, and the right panels display the FSa of the combined blue-and red-filter data.Grey dots are the decorrelated data points, while the red and blue points mark the mean instrumental magnitudes per orbit.

Fig. 9 :Fig. 11 :
Fig.9: BRITE-Constellation observations of the eclipsing binary HD 35411 (η Ori) in Field 6. Top panels show observations gathered by the blue-filter satellites, BAb and BLb, and bottom panels observations with the red-filter satellites, BHr and BTr.Left panels show the full light curve, the middle panels illustrate the light curve phased with the orbital period of 7.989454 d, and the right panels display the FSa of the combined blue-and red-filter data.Grey dots are the decorrelated data points, while the red and blue points mark the mean instrumental magnitudes per orbit. 618

HD 20468 (Field 13 :
Field 5): No variability was detected in the UBr data.HD 20809 (Field 5): Observed with UBr.The FS of the data reveals a signal at frequency 2.25 d −1 .The available data have a short time coverage.HD 20902 (α Per, Field 5): No variability was detected in the UBr and BAb data.HD 21428 (34 Per, Field 5): No variability was detected in the UBr data.HD 21552 (σ Per, Field 5): Observed with UBr.The available dataset is long and the FS of the data shows some moderate variability at low frequencies.This K3-type star was included in the study ofKallinger et al. (2019).HD 22192 (ψ Per, Field 5): Known Be star, observed by UBr and BAb.The FS of the data reveals variability with a frequency of 0.986 d −1 .HD 22780 (Field 5): No variability was detected in the UBr data.HD 22928 (δ Per, Field 5): Observed by UBr and BAb.The FS of the UBr data shows clear variability with a frequency of ∼1.27 d −1 , but additional peaks can also be identified.The BAb data are of lower quality, but their analysis confirms the frequency peaks identified from the UBr observations.HD 23180 (O Per, Field 5): Observed with UBr and BAb.The FSa of the available data reveal clear variability with a frequency of 0.453 d −1 .HD 23230 (ν Per, Field 5): No variability was detected in the BAb data.HD 23302 (17 Tau, Field 5): No variability was detected in the BAb data.The FS of the UBr data shows only some weak variability at low frequencies.HD 23338 (19 Tau, Field 5): No variability was detected in the UBr or BAb data.HD 23408 (20 Tau, Field 5): Observed with UBr and BAb.Both datasets have long time bases.The FS reveals a significant peak at frequency of 0.965 d −1 .The light curve phased with the corresponding period does not show coherent variation, however.HD 23480 (23 Tau, Field 5): No variability was detected in the UBr or BAb data.HD 23630 (η Tau, Field 5): Known Be star, observed with UBr and BAb.The FSa show a single significant frequency at 0.03 d −1 .HD 23850 (27 Tau, Field 5): Observed with UBr and BAb.The FS of the UBr data reveals three strong peaks at frequencies of ∼0.41, ∼0.82 and ∼1.3 d −1 .The FS of the BAb data confirms the dominant frequency identified from the UBr observations.HD 24398 (ζ Per, Field 5): Observed with UBr and BAb.The UBr light curve shows irregular variability resulting in several peaks in the low-frequency domain of the FS, the highest of which occurs at 0.04 d −1 .The BAb data confirm the character of the variability, which fits the ACYG classification.HD 24640 (Field 5): No variability was detected in the BAb data.HD 24760 (ε Per, Field 5): Observed with UBr and BAb.The FSa of the available data show multi-periodic hybrid β Cephei/SPB variability with the dominant peak at a frequency of 5.898 d −1 .HD 24912 (ξ Per, Field 5): Observed with UBr and BAb.The FS of the UBr data shows clear variability with a frequency of 0.49 d −1 .The analysis of the BAb data confirmed the frequency detected based on the UBr observations.able dataset is short, but its FS reveals variability with a fre-1053 quency of 0.13 d −1 .1054 HD 25940 (48 Per, Field 5): Observed with UBr and BAb.1055 The UBr dataset is long and its FS shows variability with a fre-1056 quency of ∼2.26 d −1 , which is confirmed with the shorter and 1057 scarcer BAb dataset.1058 HD 25998 (50 Per, Field 5): No variability was detected in 1059 the UBr data.1060 HD 26322 (44 Tau, Field 5): Known δ Scuti star, observed 1061 with UBr.The δ Scuti variability is clearly present with the 1062 strongest peak in the FS at a frequency of 6.89 d −1 .1063 HD 26630 (µ Per, Field 5): No variability was detected in the 1064 UBr data.1065 HD 27396 (53 Per, Field 5): Observed with UBr.The FS of 1066 the available data shows multi-mode SPB-type variability with 1067 the strongest peak at a frequency of 0.46 d −1 .1068 HD 29248 (ν Eri, Fields 6 and 13): Known hybrid β Ce-1069 phei/SPB star.Field 6: Observed with BAb, BTr, BHr and BLb.1070 The available data clearly show the known β Cephei variability.1071 Field 13: Observed with BAb and UBr.The available data also 1072 show the known pulsations.BRITE data for this star were dis-1073 cussed in detail by Handler et al. (2017b) in combination with 1074 ground-based observations.1075 HD 30211 (µ Eri, Fields 6 and 13): Known SPB star and 1076 eclipsing binary.Field 6: Observed with BTr, BHr, BLb and 1077 BAb.The strongest frequency in the FS is found at ∼0.61 d −1 1078 for BTr, BHr, and BAb data and 0.69 d −1 for the BLb data, but 1079 the FSa show also the presence of many additional peaks.Field 1080 13: Observed with UBr and BAb.The available data confirm the 1081 variability seen in the data from Field 6. 1082 HD 30652 (π 3 Ori, Field 6): No variability was detected in 1083 the BTr data.1084 HD 30836 (π 4 Ori, Fields 6 and 13): Known spectroscopic 1085 binary.Field 6: Observed with BTr, BHr, BAb and BLb.The 1086 available data show clear variability with a period of ∼4.1 days.1087 Observed with BAb and UBr.The UBr data confirm 1088 the variability found from Field 6 data.The BAb data have a 1089 short time base and are scarce.1090 HD 31109 (ω Eri, Field 6).Known spectroscopic binary.Ob-1091 served with BHr and BLb.The FSa of the available data show a 1092 dominant peak at a frequency of ∼3.64 d −1 , but the star is multi-1093 periodic.The BLb light curve is shorter and noisier than that 1094 secured by BHr, but its analysis confirms the main frequency 1095 found from the BHr data.1096 HD 31139 (5 Ori, Field 6): Observed with BHr and BTr.1097 Some long-term variability may be present in the BHr data, but 1098 the data are inconclusive.The BTr light curve is only ∼8 d long 1099 and does not reveal any variation.1100 HD 31237 (π 5 Ori, Fields 1, 6, and 13): Known ellipsoidal 1101 binary variable with an SPB component.Field 1: Observed with 1102 BAb and UBr.The available data clearly show the ellipsoidal 1103 variability with a period of 1.85 d.Field 6: Observed with BHr, 1104 BTr, BLb and BAb.The period of 1.85 d is again clearly visi-1105 ble.Field 13: Observed with UBr and BAb.The UBr data con-1106 firm the periodicity found from Field 1 and 6 data.The BAb 1107 dataset is short and scarce.BRITE data are discussed in detail 1108 by Jerzykiewicz et al. (2020).

1109
HD 31767 (π 6 Ori, Field 6): No clear variability was detected 1110 in the BTr data.1111 HD 33111 (β Eri, Fields 1 and 6): Field 1: Observed with 1112 BAb and UBr.Variability was detected in both datasets, although 1113 the strongest peaks in the FSa were found at different frequen-1114 cies, 1.055 d −1 for the BAb data and 10.44 d −1 for the UBr data.Field 6: No variability was detected in the BTr data.
Field 13: No variability was detected in the BAb data.The available data have a short time base and are scarce.HD 33904 (µ Lep, Field 6): No variability was detected in the BTr and BAb data.The BAb dataset is scarce and of poor quality.
Field 1: No variability was detected in the BAb or UBr data.Field 6: No variability was detected in the BTr, BHr, BLb, or BAb data.Field 13: No variability was detected in the BAb data.According to Pigulski et al. (2018b), the star shows a weak heartbeat signal.HD 34816 (λ Lep, Field 6): Early B type star observed with BHr, BLb, and BTr.The FS of the BHr data shows the strongest frequency peak at 5.79 d −1 .The BLb and BTr data are of lower quality and do not show any variability.HD 35039 (22 Ori, Field 6): No variability was detected in the BTr data.HD 35369 (29 Ori, Field 6): No variability was detected in the BTr data.HD 35411 (η Ori, Fields 1, 6, and 13): Eclipsing binary star with an orbital period of 8 d.Field 1: Observed with BAb and UBr.Both datasets show eclipses and regular variability with a period of 0.432 d.Field 6: Observed with BTr, BHr, BLb and BAb.The data confirm the binary period and the additional regular variability.Field 13: Observed with UBr and BAb.Both datasets confirm the binary period and the additional variability.HD 35439 (ψ 1 Ori, Field 6): Observed with BTr, BHr and BLb.The FSa of the available data show several distinct peaks in the g-mode range and additional variability typical for Be stars.The first broad assessment of the complex variability observed by BRITE-Constellation was given by Baade et al. (2018c).HD 35468 (γ Ori, Fields 1, 6, and 13):Field 1: No variability was detected in the BAb and UBr data.Field 6: No variability was detected in the BTr, BHr, BLb and BAb data.Field 13: No variability was detected in the UBr and BAb data.HD 35715 (ψ 2 Ori, Fields 1 and 6): Field 1: Observed with BAb and UBr.The available data show ellipsoidal variability with a period 2.526 d.Field 6: Observed with BTr, BHr, BLb and BAb.The data confirm the main period of 2.526 d.Pigulski et al. (2017) found in the BRITE data several additional frequencies attributable to p modes.HD 36267 (32 Ori, Field 6): Observed with BTr, BHr and BLb.The data show variability with a period of 3.772 d.HD 36485/6 (δ Ori, Fields 1, 6, and 13): Massive eclipsing and spectroscopic binary.Field 1: Observed with BAb and UBr.The data clearly show eclipses with an orbital period of 5.733 d and some additional variability.Field 6: Observed with BTr, BHr, BLb, and BAb.The data confirm the binary period.Field 13: Observed with UBr and BAb.The data confirm the binary period.HD 36512 (υ Ori, Field 6): No variability was detected in the BTr, BHr, or BLb data.HD 36822 (φ 1 Ori, Field 6): No variability was detected in the BTr data.HD 36861/2 (λ Ori A/B, Fields 1, 6, and 13): Field 1: No variability was detected in the BAb and UBr data.Field 6: No variability was detected in the BTr, BHr and BLb data.The BAb light curve is scarce and does not show any variability.Field 13: No variability was detected in the BAb data.HD 36959/60 (Field 6): No variability was detected in BHr, BTr, BLb or BAb data.HD 37018 (42 Ori, Field 6): No variability was detected in the BTr and BAb data.HD 37022/41 (θ 1 /θ 2 Ori, Fields 6 and 13): Field 6: Observed with BTr and BAb.The FS of the BTr data shows some marginal variability with a frequency of 0.62 d −1 .No variability was detected in the BAb data.Field 13: No variability was detected in the UBr data.HD 37043 (ι Ori, Fields 1, 6, and 13): Known spectroscopic binary.Field 1: Observed with BAb and UBr.The FSa of the data show some variability in the low-frequency regime, but with no significant peaks.Field 6: Observed with BTr, BHr, BAb, and BLb.The FSa of these data confirm variability in the low-frequency domain without a clear periodicity.Field 13: Observed with UBr and BAb.The FSa of the data confirm the variability in the low-frequency domain as seen from Field 1 and 6 data.BRITE data of this star were discussed by Pablo et al. (2017b).HD 37128 (ε Ori, Fields 1, 6, and 13): B-type supergiant.

Field 1 :
Observed with BAb and UBr.Both datasets show similar long-term variability, but no clear periodicity.This is characteristic for α Cyg-type variability.Field 6: Observed with BAb, BTr, BHr, and BLb.The BAb dataset is scarce and does show variability.The other datasets are of excellent quality and their FSa show clear and strong variability at low frequencies.Field 13: Observed with UBr and BAb.The FSa of these data clearly show variability in the low-frequency regime, but without a clear periodicity.HD 37468 (σ Ori, Fields 1, 6, and 13): Field 1: Observed with BAb and UBr.The FS of the BAb data shows peak at a frequency of 0.84 d −1 .No variability was detected in the UBr data.

Field 6 :
Observed with BAb, BLb, BHr, and BTr.In the FSa of the BHr and BTr data, the strongest peak is located at a frequency of 1.68 d −1 , twice the frequency detected in the BAb data.In the FS of the BLb data the strongest peak lies again at frequency of 0.84 d −1 .The BAb dataset is shorter and scarce.Field 13: Observed with UBr and BAb.The FS of the UBr data shows two peaks at 0.84 and 2.52 d −1 .No variability was detected in the BAb data, which are of lower quality.HD 37490 (ω Ori, Fields 6 and 13): Field 6: Observed with BAb, BHr, BTr, and BLb.The data show variability with the main period of about 0.95 d.Field 13: No variability was detected in the UBr data.HD 37742/3 (ζ Ori A/B, Fields 1, 6, and 13): O-type spectroscopic binary showing stochastic variability typical for massive stars (Buysschaert et al. 2017b).Field 1: Observed with BAb and UBr.The BAb light curve shows a period of 3.275 d.The corresponding frequency is not dominant in the FS of the UBr data, but a phase fold with the same period reveals similar variability.Field 6: Observed with BAb, BHr, BTr, and BLb.The light curves show clear variability although the period of 3.275 d is not dominant in their FSa.Field 13: Observed with BAb and UBr.The FS of the UBr data clearly shows low-frequency variability.1243 The BAb data are scarcer, but its FS confirms the variability at 1244 low frequencies.1245 HD 38771 (κ Ori, Fields 1, 6, and 13): B-type supergiant.1246 Field 1: Observed with UBr and BAb.The FSa of the data show 1247 low-frequency signals with a dominating peak at a frequency of 1248 ∼0.44 d −1 .Field 6: Observed with BHr, BLb, BTr, and BAb.1249 The FSa of the BHr and BLb data show clear variability with 1250 the strongest peak at a frequency of 0.9 d −1 .The BTr dataset 1251 is shorter and its FS shows twice the frequency detected in the 1252 BHr and BLb data.The BAb data have a short time base and are 1253 scarce.Field 13: Observed with UBr and BAb.The FS of the 1254 UBr data shows variability in the low-frequency regime with a 1255 dominant peak at a frequency of 0.3016 d −1 .The BAb data are 1256 scarcer but its FS confirms the low-frequency variability.1257 HD 39060 (β Pic, Field 8): Young δ Scuti star, observed with 1258 BHr.The FS of the data reveals δ Scuti-type pulsations around 1259 43 d −1 .Studied in detail by Zwintz et al. (2019b), Mol Lous et al. 1260 (2018) and Kenworthy et al. (2021).1261 HD 39801 (α Ori, Betelgeuse, Fields 1, 6, and 13): Field 1: 1262 Observed with BAb and UBr, but the acquired CCD subraster of 1263 this star was severely overexposed.Field 6: Observed with BAb, 1264 BTr, BHr and BLb.The data show clear variability, although part 1265 of this variability can be instrumental due to strong saturation 1266 (Weiss et al. 2021).The BAb dataset is short and scarce.Field 1267 13: Observed with UBr and BAb.The UBr data show some vari-1268 ability.No variability was detected in the scarce BAb dataset.1269 HD 42933 (δ Pic, Field 8): Eclipsing binary, observed with 1270 BHr.The light curve clearly shows eclipses with a period of 1271 1.672 d. 1272 HD 44402 (ζ CMa, Field 12): Observed with BLb.The FS of 1273 the data shows a strong peak at a frequency of 0.2569 d −1 .The 1274 presence of additional frequencies is also evident.1275 HD 44743 (β CMa, Field 12): Known β Cep star.Observed 1276 with BTr and BLb.The FSa of the data show a clear peak at a 1277 frequency of 3.9791 d −1 .1278 HD 45348 (α Car, Field 8): No variability was detected in the 1279 BHr data.1280 HD 45871 (IY CMa, Field 12): Observed with BTr and BLb.1281

1285
HD 46328 (ξ 1 CMa, Field 12): Known magnetic β Cep-type 1286 pulsator.Observed with BHr, BTr, and BLb.The FSa of the BTr 1287 and BLb data show clear variability with the strongest peak at a 1288 frequency of 4.7717 d −1 .The BHr light curve has two large gaps, 1289 but the frequency detected in the BLb and BTr data is confirmed.1290 This star has been studied in detail using BRITE data by Wade 1291 et al. (2020).

1292
HD 47306 (N Car, Field 8): No variability was detected in 1293 the BHr data.1294 HD 47670 (ν Pup, Field 8): Observed with BHr.The FS of 1295 the data displays a significant peak at a frequency of 0.6575 d −1 .1296 1303 HD 49131 (HP CMa, Field 12): No variability was detected 1304 in the BLb or BTr data.HD 50013 (κ CMa, Field 12): Observed with BLb and BHr.FSa of both datasets show strong variability with a main peak at a frequency of 0.056 d −1 .HD 50123 (HZ CMa, Field 12): Observed with BTr and BLb.
HD 50337 (V415 Car, Field 8): No variability was detected in the BHr data.HD 50707 (15 CMa, Field 12): Observed with BTr, BHr, and BLb.The FSa of the data show clear β Cep-type pulsations with the strongest peak at a frequency of 5.418 d −1 .HD 50877 (o 1 CMa, Field 12): Observed with BHr.The light curve shows strong long-term variability.HD 50896 (EZ CMa, Field 12): Observed with BHr.The data show rotational modulation with a period of 3.656 d.They are discussed by Schmutz & Koenigsberger (2019).HD 51309 (ι CMa, Field 12): Observed with BTr, BHr, and BLb.The FSa of the data show variability with the strongest peak at a frequency of 0.077 d −1 , but additional frequencies that can be attributed to β Cep pulsations are evident.HD 52089 (ε CMa, Field 12): No variability was detected in the BHr or BLb data.HD 52670 (LS CMa, Field 12): Observed with BTr.The data show three eclipses, two primary and one secondary.HD 52877 (σ CMa, Field 12): Observed with BHr.The data show strong long-term variability with a period of about 34 d.HD 53138 (o 2 CMa, Field 12): Blue supergiant, observed with BHr and BLb.The FSa of the data reveal strong variability with low frequencies.HD 53244 (γ CMa, Field 12): No variability was detected in the BTr data.HD 54309 (FV CMa, Field 12): No variability was detected in the BLb data.HD 54605 (δ CMa, Field 12): No variability was detected in the BHr or BLb data.HD 55892 (QW Pup, Field 8): Observed with BHr.The FS of the data shows multi-periodic γ Dor-type pulsations with a dominant frequency of 0.975 d −1 .HD 56014 (27 CMa, Field 12): Observed with BLb, BHr, and BTr.The FSa of the data reveal multi-periodic variability with the strongest peak at a frequency of 0.7925 d −1 for this Be star.The BLb light curve is of lower quality, but confirms the variability seen in the other light curves.HD 56022 (OU Pup, Field 8): No variability was detected in the BHr data.HD 56139 (ω CMa, Field 12): Observed with BHr, BTr, and BLb.The data show strong variability, typical for Be stars (Fig. 2).HD 56455 (PR Pup, Field 8): Observed with BHr.The data are scarce, but its FS shows a significant frequency at 0.484 d −1 .HD 56855 (π Pup, Field 8): No variability was detected in the BHr data.HD 57060 (29 CMa, Field 12): Observed with BHr, BLb, and BTr.All datasets show clear eclipses with a period of about 4.4 d.HD 57061 (τ CMa, Field 12): Observed with BTr, BHr, and BLb.The FSa of the data are dominated by a frequency of 1.56 d −1 , corresponding to twice the orbital frequency of the known variability due to eclipses (van Leeuwen & van Genderen 1997).HD 58155 (NO CMa, Field 12): Observed with BTr and BLb.The BTr data reveal variability with a main period of 0.4774 d.The BLb dataset is shorter and scarce.HD 58286 (Field 12): No variability was detected in the BLb 1370 data.1371 HD 58343 (FW CMa, Field 12): Observed with BTr and 1372 BLb.The FS of the BTr data shows variability with the strongest 1373 peak at a frequency of 0.0772 d −1 .The BLb dataset is shorter 1374 and scarce.1375 HD 58350 (η CMa, Field 12): Blue supergiant, observed with 1376 BHr and BLb.The FS of the data shows strong low-frequency 1377 variability with the strongest peak at 0.1222 d −1 .1378 HD 61068 (PT Pup, Field 12): Observed with BLb and BTr.1379 The FSa of the data show β Cep-type variability with the 1380 strongest peak at a frequency of 5.9977 d −1 (see Handler 2017).1381 HD 61715 (MY Pup, Field 8): Known classical Cepheid.Ob-1382 served with BHr.The data show clear variability with a period 1383 of about 5.7 d. 1384 HD 62623 (3 Pup, Field 12): Observed with BHr and BLb.1385 The FSa of the data show low-frequency variability typical for 1386 α Cyg-type stars.1387 HD 62747 (V390 Pup, Field 12): Known binary system, ob-1388 served with BTr.The data show shallow eclipses with an orbital 1389 period of about 3.93 d. 1390 HD 63462 (o Pup, Field 12): Observed with BTr, BHr, and 1391 BLb.The FSa of all datasets show some low-frequency variabil-1392 ity around 0.05 d −1 .1393 HD 63744 (Q Pup, Field 7): No variability was detected in 1394 the BTr data.1395 HD 63922 (P Pup, Fields 7 and 8): Field 7: No variability 1396 was detected in the BAb or BTr data.Field 8: No variability was 1397 detected in the scarce BHr dataset.1398 HD 63949 (QS Pup, Field 8): No variability was detected in 1399 the BHr data.1400 HD 64440 (a Pup, Fields 7 and 8): Field 7: Observed with 1401 BAb and BTr.The FS of the BTr data shows a significant peak at 1402 ∼1.9 d −1 .No variability was detected in the scarce BAb dataset.1403 Field 8: No variability was detected in the BHr data.1404 HD 64740 (Fields 7, 8, and 14): Field 7: Observed with BAb 1405 and BTr.The FSa of the data show a clear peak at a frequency of 1406 0.7519 d −1 .In addition, the FS of the BTr data shows the pres-1407 ence of additional frequencies up to 2 d −1 .Field 8: No variability 1408 was detected in the scarce BHr dataset.Field 14: No variability 1409 was detected in the short and scarce BAb dataset.1410 HD 64760 (J Pup, Fields 7, 8, and 14): Field 7: Observed 1411 with BAb and BTr.The data show some indications for low-1412 frequency variability in the FS.Field 8: No variability was de-1413 tected in the scarce BHr data.Field 14: No variability was de-1414 tected in the short and scarce BAb data.1415 HD 65575 (χ Car, Fields 7, 8, and 14): Field 7: Observed 1416 with BTr and BAb.The FS of the BTr and BAb data show multi-1417 periodic variability with the strongest peaks at frequencies of 1418 0.6438 d −1 and 0.6126 d −1 , respectively.Field 8: Observed with 1419 BHr.The light curve is scarce, but its FS shows variability with 1420 a frequency of 0.66 d −1 .Field 14: No variability was detected in 1421 the short and scarce BAb dataset.1422 HD 65818 (V Pup, Fields 7, 8, and 14): Known eclipsing bi-1423 nary consisting of two B-type stars.Field 7: Observed with BTr 1424 and BAb.The data clearly show eclipses with the orbital period 1425 of about 1.45 d.Field 8: Observed with BHr.The dataset is rel-1426 atively short, but the variability is clearly detectable.Field 14: 1427 Observed with BAb.Again, the dataset is relatively short, but 1428 confirms the period found from the other BRITE observations.1429 HD 66811 (ζ Pup, Fields 7, 8, and 14): O-type supergiant.1430 Field 7: Observed with BTr and BAb.The FSa of the data show 1431 clear variability with a frequency of 0.562 d −1 .Field 8: Observed 1432 with BHr.The FS of the data shows the same frequency as detected in the Field 7 dataset.Field 14: No variability was detected in the short and scarce BAb data.The star was studied in detail by Ramiaramanantsoa et al. (2018a).HD 67523 (ρ Pup, Field 12): Known δ Sct star observed with BLb, BHr and BTr.The FSa of the data show the variability with the strongest peak at a frequency of 7.098 d −1 .HD 68243/73 (γ 1 /γ 2 Vel, Fields 7, 8, and 14): WR star.Field 7: Observed with BTr and BAb.The FSa of the data clearly show low-frequency variability.Field 8: Observed with BHr.The FS of the data confirms the low-frequency variability.Field 14: No variability was detected in the short and scarce BAb dataset.Using BRITE-Constellation data, γ Vel was studied in detail by Richardson et al. (2017b).HD 68553 (h 1 Pup, Field 7): Observed with BTr.The data show clear variability.HD 69142 (h 2 Pup, Field 7): No variability was detected in the short and scarce BTr dataset.HD 71129 (ε Car, Field 7): Observed with BAb and BTr.The BAb dataset is short, and its FS shows variability with the strongest frequency at 1.1289 d −1 .The BTr light curve confirms this variability.HD 72127 (Field 7): No variability was detected in the short and scarce BAb dataset.HD 73634 (e Vel, Field 7): No variability was detected in the BTr and short and scarce BAb datasets.HD 74006 (β Pyx, Field 7): No variability was detected in the BTr data and in the short and scarce BAb dataset.The star was included in the study by Kallinger et al. (2019).HD 74180 (b Vel, Field 7): No variability was detected in the BAb and BTr data.HD 74195 (o Vel, Fields 7 and 14): Field 7: Observed with BAb and BTr.The FSa of the data show pulsations with a main frequency of 0.3574 d −1 .Field 14: Observed with BAb.The dataset is relatively short and scarce, but its FS reveals variability with a frequency of 0.3597 d −1 .HD 74375 (d Car, Field 7): Observed with BAb and BTr.The FSa of the data show clear pulsational variability with the strongest peak at a frequency of 0.4202 d −1 .HD 74560 (HY Vel, Field 7): Observed with BAb.The dataset is short and scarce, but its FS shows variability with a frequency of 0.63 d −1 .HD 74575 (α Pyx, Field 7): Observed with BAb and BTr.The FSa of the data clearly show multi-periodic variability with the strongest peak at a frequency of 0.1876 d −1 .HD 74772 (d Vel, Field 7): No variability was detected in the BTr data and short and scarce BAb dataset.HD 74956 (δ Vel, Field 7): Known eclipsing binary, observed with BAb and BTr.The light curves show eclipses with the orbital period of 45.15 d.HD 75063 (a Vel, Field 7): Observed with BTr and BAb.The BTr dataset is short and shows weak variability.No variability was detected in the short and scarce BAb dataset.HD 75311 (f Car, Fields 7 and 14): Known Be star.Field 7: Observed with BTr.The FS of the data reveals complex variability, with multiple intrinsic frequencies.Field 14: No variability was detected in the short and scarce BAb dataset.HD 75821 (f Vel, Field 7): No variability was detected in the short and scarce BAb dataset.HD 76728 (c Car, Fields 7 and 14): Field 7: Observed with BTr and BAb.The FS of the BTr data shows variability with a frequency of 0.293 d −1 .No variability was detected in the BAb data.Field 14: No variability was detected in the short and scarce BAb dataset.HD 77002 (b 1 Car, Field 7): No variability was detected in 1497 the short and scarce BTr dataset.1498 HD 78004 (c Vel, Field 7): No variability was detected in the 1499 BTr dataset.The BAb dataset consists only of a few data points.1500 HD 78647 (λ Vel, Field 7): Observed with BTr and BAb.The 1501 BTr light curve shows complex long-term variability.The BAb 1502 dataset is short and scarce.1503 HD 79351 (a Car, Fields 7 and 14): Field 7: Observed with 1504 BTr and BAb.The FS of the BTr data shows multi-frequency 1505 variability with the strongest peak at a frequency of 0.3725 d −1 .1506 The FS of the BAb data confirms the multi-frequency variations, 1507 but the data are noisier.Field 14: No variability was detected in 1508 the short and scarce BAb dataset.1509 HD 79940 (k Vel, Field 7): No variability was detected in the 1510 short and scarce BTr data.1511 HD 80230 (g Car, Field 7): Observed with BTr.The light 1512 curve shows a dominant period of 12.17 d. 1513 HD 80404 (ι Car, Fields 7 and 14): Field 7: No variability 1514 was detected in the BTr and BAb data.Field 14: Observed with 1515 BAb.The dataset is short and scarce, but its FS shows variability 1516 with a frequency of 1.1509 d −1 .1517 HD 81188 (κ Vel, Fields 7 and 14): Field 7: Observed with 1518 BTr and BAb.The FS of the data shows multi-frequency vari-1519 ability with the strongest peak at a frequency of 0.2431 d −1 .1520 Field 14: No variability was detected in the short and scarce BAb 1521 dataset.1522 HD 82434 (ψ Vel, Field 7): No variability was detected in the 1523 BTr data and the short and scarce BAb dataset.1524 HD 82668 (N Vel, Field 7): Observed with BTr and BAb.The 1525 FS of the BTr data shows complex multi-frequency variability, 1526 while the BAb dataset is short and scarce.1527 HD 83183 (h Car, Field 7): No variability was detected in the 1528 BTr data and in the short and scarce BAb dataset.1529 HD 83446 (M Vel, Field 7): Observed with BTr and BAb.1530 The FS of the BTr data show δ Sct-type variability with the 1531 strongest peak at a frequency of 31.08 d −1 .The BAb dataset is 1532 shorter and of inferior quality.1533 HD 86440 (φ Vel, Field 7): No variability was detected in the 1534 BAb and BTr data.1535HD 118716 (ε Cen, Field 2): Known β Cep star, observed 1536 with BTr, BLb, UBr, and BAb.The FSa of the UBr and BAb data 1537 show clear pulsational variability with many frequencies and the 1538 strongest peak at a frequency of 5.8955 d −1 .The BTr and BLb 1539 datasets are scarce, but the main pulsation frequency can still be 1540 identified in the FSa of both datasets.1541 HD 120307 (ν Cen, Field 2): Observed by BTr, BLb, BAb 1542 and UBr.The BAb and UBr data are of excellent quality and 1543 show clear variability with a period of about 2.62 d.The BTr and 1544 BLb datasets are significantly shorter, but confirm the variability.1545 The variability is due to the reflection effect in a binary system 1546 (Jerzykiewicz et al. 2021).1547 HD 120324 (µ Cen, Field 2): Known Be star, observed by 1548 BLb, BTr, BAb, and UBr.The BAb and UBr data show signifi-1549 cant, possibly irregular variations.The BLb and BTr datasets are 1550 shorter, but confirm the variability.BRITE data of this star were 1551 studied in detail by Baade et al. (2016).

1552
HD 121263 (ζ Cen, Field 2): Heartbeat binary star observed 1553 with BAb, UBr, BLb, and BTr.In the FSa of the BAb and UBr 1554 data the strongest peaks lie at a frequency of 0.1244 d −1 , cor-1555 responding to a period of ∼8.026 d.The datasets from BLb and 1556 BTr are shorter, but confirm the detected period.1557 HD 121743 (φ Cen, Field 2): Observed with UBr, BTr, BAb, 1558 and BLb.The FSa of the BAb and BLb data show the strongest 1559 and UBr data show the strongest peak at frequency of ∼5.6 d −1 .1592 The BTr and BLb data have shorter time bases, but confirm this 1593 variability.1594 HD 126354 (τ 2 Lup, Field 2): Observed with UBr, BAb, and 1595 BTr.The FS of the UBr data shows an instrumental frequency of 1596 about 1 d −1 and a few lower-amplitude peaks.The BAb dataset 1597 has a gap in the middle and the BTr dataset has shorter time 1598 base, but their FSa confirm the frequencies found from the UBr 1599 dataset.1600 HD 127381 (σ Lup, Field 2): Observed with UBr, BAb, and 1601 BTr.The FS of the UBr data shows a clear peak at a frequency of 1602 0.33 d −1 .The BAb dataset has a gap in the middle of the run.The 1603 BTr dataset is significantly shorter, but both datasets confirm the 1604 variability detected from the UBr observations.1605 HD 127972/3 (η Cen, Field 2): Known Be star, observed with 1606 BTr, BLb, UBr, and BAb.The FSa of the UBr and BAb data 1607 show clear variability with the strongest peak at a frequency of 1608 1.55 d −1 .The BTr and BLb datasets are shorter, but their analysis 1609 confirmed the main frequency found from the UBr and BAb data.

1610
BRITE data of this star were studied in detail byBaade et al.

1612
HD 128345 (ρ Lup, Field 2): Observed with UBr, BAb, and 1613 BTr.The FS of the UBr data shows clear variability with a fre-1614 quency of 2.245 d −1 .The BAb dataset has a gap in the middle of 1615 the run, but its analysis confirms this variability.The BTr dataset 1616 is shorter and of poorer quality.1617 HD 128620/1 (α Cen, Field 2): Observed with BAb, BTr, and 1618 BLb.The BAb light curve shows a period of 29.85 d.The BTr 1619 and BLb datasets are shorter and of poorer quality.Due to the 1620 brightness of the star, the acquired CCD subraster is severely 1621 overexposed and parts of the light curves have increased scatter. 1622 HD 129056 (α Lup, Field 2): Known β Cep-type star.Observed with BAb, UBr, BTr, and BLb.The β Cep variability is seen in the FSa of the BAb and UBr data with the main peak at a frequency of 3.8487 d −1 and several smaller peaks at other frequencies.The BTr and BLb datasets are shorter, but their FSa confirm the strongest peak found in the analysis of the BAb and UBr datasets.HD 129116 (b Cen, Field 2): No variability was detected in the UBr, BAb, and BTr data.HD 130807 (o Lup, Field 2): Observed with UBr, BAb and BTr.The FS of the UBr data shows several significant frequencies with the strongest peak at a frequency of 1.106 d −1 .The BAb dataset has a gap in the middle of the run and the BTr dataset is significantly shorter, but FSa of both confirm the strongest frequency found in the FS of the UBr data.The variability of this magnetic star was described by Buysschaert et al. (2019).HD 132058 (β Lup, Field 2): Observed with UBr, BAb, BTr, and BLb.The UBr and BAb data show variability with a main period of 3.632 d.The BTr and BLb data have significantly shorter time bases, but confirm the main period obtained from the UBr and BAb data.HD 132200 (κ Cen, Field 2): Observed with UBr, BAb, BTr, and BLb.The FSa of the UBr and BAb data show multiple significant frequencies around ∼0.698 d −1 .The BTr and BLb datasets are significantly shorter, but their analysis confirms this variability.HD 133242/3 (π Lup, Field 2): No variability was detected in the BTr data.HD 134481/2 (κ Lup, Field 2): No variability was detected in the UBr, BAb, and BTr data.The BAb dataset has a gap in the middle of the run and the BTr dataset is rather short.HD 134505 (ζ Lup, Field 2): No variability was detected in the UBr, BAb, BTr, and BLb data.The BTr and BLb datasets are short.HD 135379 (β Cir, Field 2): Observed with UBr, BAb, and BTr.The FSa of the UBr and BAb data show low-frequency variability.The BAb dataset has a gap in the middle of the run and the BTr data have a relatively short time base.HD 135734 (µ Lup, Field 2): No variability was detected in the UBr, BAb, and BTr data.The BTr dataset is short.HD 136298 (δ Lup, Fields 2 and 9): Field 2: Observed with UBr, BAb, BTr, and BLb.The FSa of the UBr and BAb data show several significant frequencies in the domain of SPB stars, with the strongest peak at ∼1.27 d −1 .The BTr and BLb datasets are significantly shorter, but their FSa confirm the strongest peak discovered from the UBr and BAb observations.Field 9: Observed with BAb, BLb, BHr, and UBr.The FSa of the data show a clear signal at 5.902 d −1 as well as many other frequencies.The BRITE data for this star were discussed by Cugier & Pigulski (2017).HD 136415/6 (γ Cir, Field 2): Observed with UBr, BAb, and BTr.The FS of the UBr data shows a few significant frequencies, the strongest signal at 2.46 d −1 and the second strongest at 4.49 d −1 .The BAb dataset has a large gap in the middle of the run and does not show any variability.The BTr dataset is signifi-HD 151804 (V973 Sco, Field 9): Observed with BHr.The FS 1788 of the data exhibits a typical stochastic low-frequency signal of 1789 evolved O-type stars.1790 HD 151890 (µ 1 Sco, Field 9): Observed with UBr, BHr, and 1791 BLb.The FSa of the data show strong variability with a fre-1792 quency of 1.383 d −1 , corresponding to half of the known 1.446 d 1793 orbital period.1794 HD 151985 (µ 2 Sco, Field 9): Observed with BLb, BHr and 1795 UBr.The FSa of the BLb and BHr data show a weak signal at 1796 1.383 d −1 , the same as detected in the nearby (5.8 apart) µ 1 Sco.1797This means that the photometry pipeline did not separate well 1798 the contribution from both stars.The FS of the UBr data shows a 1799 somewhat weaker signal at this frequency, but also at twice this 1800 value (i.e.2.765 d −1 ).1801 HD 157056 (θ Oph, Field 3): This well known β Cephei star 1802 was observed by UBr.The dataset is short and scarce, but its 1803 FS reveals the most prominent pulsation frequency of 7.118 d −1 .1804 This star was studied in detail using BRITE data by Walczak 1805 et al. (2019).

1806
HD 157792 (b Oph, Field 3): Observed by UBr.No variabil-1807 ity was detected in the short and scarce UBr dataset.1808 HD 157919 (d Oph, Field 3): Observed by UBr.No variabil-1809 ity was detected in the short and scarce UBr dataset.1810 HD 158408 (υ Sco, Field 3): Observed with UBr.The dataset 1811 is short and scarce, but the light curve shows signal with a period 1812 of 2.47 d. eclipsing β Cep star.Observed with UBr.The dataset is short and 1815 scarce and its FS shows a high amplitude peak at a frequency of 1816 4.679 d −1 .1817 HD 159433 (Q Sco, Field 3): No variability was detected in 1818 the short and scarce UBr dataset.1819 HD 159532 (θ Sco, Field 3): Observed with UBr.The dataset 1820 is short and scarce and shows a period of ∼13 d. these data is at 1.76 d −1 .1873 HD 189849 (15 Vul, Field 10): Observed with BAb, BTr and 1874 UBr.No variability was detected in UBr and BTr data.The BAb 1875 light curve is scarce and of poor quality.
HD 192577/8 (31 Cyg, Fields 4 and 10): Field 4: Observed with BTr, UBr, and BLb.The BTr data reveal complex variability.The UBr and BLb datasets are short and scarce.Field 10: No variability was detected in the scarce BLb and BAb datasets.HD 192640 (29 Cyg, Fields 4 and 10): Known δ Sct-type variable.Field 4: Observed with BTr and BLb.The FSa of the data show many peaks at frequencies typical for a δ Sct star, the highest lies at a frequency of 37.4 d −1 .Field 10: Observed with BAb, BTr, and UBr.A very similar to Field 4 δ Sct-type variability can be seen in these data.HD 192685 (QR Vul, Field 10): Observed with BTr, BLb, and UBr.The FS of the 156-d long BTr data shows strong and complex variability with the main peak at a frequency of 0.195 d −1 .The BLb dataset is short and UBr dataset is of poor quality.HD 192806 (23 Vul, Field 4): Observed with BTr.The data do not show any prominent variability, but several low-frequency peaks can be seen in their FS.HD 192909/10 (o Cet, Field 4): Observed with BTr and UBr.The BTr light curve shows some strong and complex variability.No variability was detected in the short and scarce UBr dataset.HD 193092 (Field 4): No variability was detected in the BTr data.HD 193237 (P Cyg, Fields 4 and 10): Blue supergiant with known variability.Field 4: Observed with BTr, BLb, and UBr.The BTr and BLb light curves show strong variability.The UBr dataset is short and scarce.Field 10: Observed with BTr, UBr, BLb, and BAb.The BTr data show clear variability.The UBr, BLb, and BAb datasets are shorter.The BRITE data for this star were investigated in detail by Elliott et al. (2022).HD 194093 (γ Cyg, Fields 4 and 10): Field 4: Observed with BTr, BLb, and UBr.The BTr light curve shows some lowamplitude long-term variability, while the BLb data do not reveal any variability.The UBr dataset is short and scarce.Field 10: No variability was detected in the UBr, BAb and BLb data.HD 194317 (39 Cyg, Field 4): Observed with BTr and UBr.The FS of the BTr data reveals a significant peak at a frequency of 0.76 d −1 .The UBr dataset is short and scarce.HD 194335 (Field 10): Known Be star.No variability was detected in the BLb data.HD 195068/9 (43 Cyg, Field 10): Observed with BTr and BLb.The FS of the BTr data clearly shows γ Dor-type pulsations with the main frequency at 1.25 d −1 .No variability was detected in the short BLb dataset.The star was studied in detail by Zwintz et al. (2017).HD 195295 (41 Cyg, Fields 4 and 10): Field 4: No variability was detected in the BTr, UBr and BLb data.Field 10: No variability was detected in the UBr data.HD 195556 (ω 1 Cyg, Field 10): Observed with BAb and BTr.The BAb dataset is of poor quality.The BTr dataset is only 12.4 days long and shows evidence of long-term variability.HD 196093/4 (47 Cyg, Field 4): Observed with BTr and UBr.The BTr data show complex variability.The UBr dataset is scarce.HD 197345 (α Cyg, Fields 4 and 10): Field 4: Observed with BTr, BLb, and UBr.The FSa of the BTr and BLb data show clear variability at low frequencies; the UBr dataset is scarce.

Field 10 :
Observed with UBr, BAb, and BLb.The FSa of the data show variability at low frequencies.HD 197912 (52 Cyg, Field 4): No variability was detected in the short BTr and in the short and scarce BLb and UBr datasets.HD 197989 (ε Cyg, Fields 4 and 10): Field 4: No variability was detected in the BLb and BTr data or in the short and scarce UBr dataset.Field 10: No variability was detected in the BAb, BLb, and UBr data.The star was included in the study by Kallinger et al. (2019).HD 198183 (λ Cyg, Fields 4 and 10): Field 4: Observed with BLb, UBr, and BTr.The BLb and UBr datasets are short.The BTr data show complex variability.Field 10: Observed with BTr, UBr, BLb, and BAb.A complex variability is clearly present in the BTr data and less evident in the UBr data.The BAb dataset is of poor quality, the BLb dataset is short.HD 198478 (55 Cyg, Fields 4 and 10): Field 4: Observed with BTr and BLb.The FS of the BTr data shows complex lowfrequency variability.The BLb dataset is short and scarce.Field 10: Observed with BTr, BAb, UBr, and BLb.The BTr light curve shows complex variability, which is less evident in the BAb light curve due to the sparsity and low quality of the data.The FS of the UBr data shows low-frequency variability.The BLb dataset is short.HD 198639 (56 Cyg, Field 10): No variability was detected in the BTr or BAb data.HD 198726 (T Vul, Fields 4 and 10): Classical Cepheid.

Field 4 :
Observed with BTr and UBr.The BTr light curve shows variability with a period of ∼4.44 d.The UBr dataset is shorter, but the variability is clearly detectable despite the sparsity of the data.Field 10: Observed with BTr.The light curve shows variability with the same period as in the Field 4 observations.HD 198809 (31 Vul, Field 4): The UBr dataset is short and scarce.No variability was detected.HD 199081 (57 Cyg, Fields 4 and 10): Field 4: Observed with BLb and BTr.The FSa of the data show strong frequency at 0.934 d −1 .Field 10: Observed with BTr, BAb, UBr, and BLb.The FS of the BTr data shows multiple frequencies below ∼1.1 d −1 ; the strongest peak is at a frequency of 0.934 d −1 .The BAb and UBr datasets are shorter, but the low-frequency variability is confirmed in their FSa.The BLb dataset is of poor quality.HD 199629 (ν Cyg, Fields 4 and 10): Field 4: No variability was detected in the UBr data.Field 10: No variability was detected in the UBr data.HD 200120 (59 Cyg, Fields 4 and 10): Known Be star.Field 4: No variability was detected in the short and scarce BLb dataset.Field 10: Observed with BTr, BAb, and BLb.The FS of the BTr data shows clear variability with frequencies between ∼1.5 and 2.2 d −1 .The BAb and BLb datasets are short and scarce.HD 200310 (60 Cyg, Field 10): Known Be star, observed with BTr, BAb, and BLb.The FS of the BTr data shows clear variability with frequencies below 4 d −1 .The BAb dataset is shorter and of poorer quality.The BLb dataset is scarce.HD 200905 (ξ Cyg, Field 4): Observed with BTr and UBr.The BTr light curve shows variability with a period of ∼17.3 d.No variability was detected in the short and scarce UBr dataset.HD 201078 (DT Cyg, Fields 4 and 10): Classical Cepheid.Field 4: Observed with BTr and UBr.The light curves show classical Cepheid variability with a period of ∼2.5 d.Field 10: Observed with BTr and BLb.The BTr light curve shows variability with the same period as the Field 4 data.The BLb light curve is short, but the variability can also be seen.HD 201251 (63 Cyg, Field 4): No variability was detected in 2004 the BTr data or in the short and scarce UBr dataset.2005 HD 201433 (V389 Cyg, Field 10): This is a triple system 2006 with SPB pulsations, observed with BTr and BLb.The BTr light 2007 curve shows SPB-type pulsations, confirmed also in the BLb 2008 data despite their scarcity.The BRITE data of this star were dis-2009 cussed in detail by Kallinger et al. (2017).2010 HD 202109 (ζ Cyg, Fields 4 and 10): Field 4: No variability 2011 was detected in the BLb and BTr data or in the short and scarce 2012 UBr datasets.Field 10: No variability was detected in the UBr 2013 and BAb data or in the short and scarce BLb dataset.2014 HD 202444 (τ Cyg, Fields 4 and 10): Field 4: No variability 2015 was detected in the BLb and BTr data or in the short and scarce 2016 UBr dataset.Field 10: No variability was detected in the BAb 2017 data or in the short and scarce BLb dataset.2018 HD 202850 (σ Cyg, Fields 4 and 10): Field 4: Observed with 2019 BTr, BLb, and UBr.The FSa of the BTr and BLb data show some 2020 low-frequency variability.The UBr dataset is short and scarce.2021 Field 10: Observed with BAb, BLb, and BTr.The FS of the BTr 2022 data shows low-frequency variability.The BAb and BLb datasets 2023 are shorter and scarce.2024 HD 202904 (υ Cyg, Fields 4 and 10): Known Be star.Field 2025 4: Observed with BTr, BLb, and UBr.The FS of the BTr data 2026 shows strong variability at very low frequencies.The FS of the 2027 BLb data reveals a frequency of ∼1.47 d −1 on the top of the lower 2028 frequency variability.The UBr dataset is short and scarce.Field 2029 10: Observed with BTr, BAb, and BLb.The FS of the BTr data 2030 shows clear variability with a frequency of 1.47 d −1 .The BAb 2031 and BLb datasets are shorter and scarce.2032 HD 203064 (68 Cyg, Fields 4 and 10): Field 4: No variability 2033 was detected in the BTr and BLb data.Field 10: No variability 2034 was detected in the BTr data or in the short and scarce BAb and 2035 BLb datasets.2036 HD 203156 (V1334 Cyg, Fields 4 and 10): Known classical 2037 Cepheid.Field 4: Observed with BTr and UBr.The light curves 2038 clearly show variability with a period of ∼3.3 d.Field 10: Ob-2039 served with BTr and BLb.The variability seen in the Field 4 2040 data is confirmed in the BTr dataset.The BLb dataset is short 2041 and scarce.2042 HD 203280 (α Cep, Field 11): No variability was detected in 2043 the short BLb dataset.2044 HD 205021 (β Cep, Field 11): The BHr and BLb datasets are 2045 very sparse and not useful for scientific analysis.2046 HD 205435 (ρ Cyg, Field 10): No variability was detected in 2047 the good-quality BTr and UBr data or in the short and scarce 2048 BLb dataset.2049 HD 206570 (V460 Cyg, Field 4): No variability was detected 2050 in the BTr data.2051 HD 207260 (ν Cep, Field 11): Observed with BHr and BLb.2052 The FS of the BHr data shows weak low-frequency variability.2053 The BLb dataset is short and of lower precision.2054 HD 209790 (ξ Cep, Field 11): No variability was detected in 2055 the BHr data and in the short BLb dataset.2056 HD 209975 (19 Cep, Field 11): Observed with BHr and BLb.2057 The FSa of the BHr data show some stochastic low-frequency 2058 variability.The BLb dataset is short and scarce.2059 HD 210745 (ζ Cep, Field 11): No variability was detected in 2060 the BHr data.2061 HD 211336 (ε Cep,Field 11): Known δ Sct-type pulsator, ob-2062 served with BTr, BLb, and BHr.The FSs of the BTr and BLb 2063 data show δ Sct-type variability.The BHr dataset is short and 2064 not usable.

Full
light curves obtained by different BRITE satellites using the same filter can be combined by subtracting the mean magnitude from each light curve individually.Data taken in different BRITE filters can be combined after subtracting the mean magnitudes only if the amplitudes are expected to be similar in both bands or if the observations in one filter are scaled to the amplitude of the other.Appendix D: Data quality per satellite

Figures
Figures D.1 to D.5 illustrate the noise properties for each of the five BRITE-Constellation instruments individually.

Fig
Fig. D.2: Values of σ med orbit plotted as a function of instrumental BRITE magnitude for BAb setups.
Fig. D.3: Values of σ med orbit plotted as a function of instrumental BRITE magnitude for BTr setups.
Fig. D.4: Values of σ med orbit plotted as a function of instrumental BRITE magnitude for BLb setups.

5 :
Fig. D.5: Values of σ med orbit plotted as a function of instrumental BRITE magnitude for BHr setups.

Table 1 :
Pigulski et al. (2018c)-Constellation observations of the first 14 fields.thedataand subtracted at each iteration step, plays an 205 important role in the decorrelation process.It is sufficient if the 206 variability model takes into account only the strongest variability 207 so that the time series can be assumed to be dominated by instru-208 mental effects.The decorrelations themselves include one-and 209 two-dimensional dependences of residual magnitudes on decor-210 relation parameters.Details of the entire procedure are described 211 byPigulski et al. (2018c).
Notes.Columns are: field identification (Field), BRITE satellite (Sat), equatorial coordinates of the centre of the observed field for epoch 2000.0(RA2000 , DEC 2000 ), setup number(s) (Setup(s)), observation start and end dates (Observation start, Observation end) in the format [yyyy.mm.dd], observation time span in days (Time span), the number of stars in the field (N stars ), and the observing mode used (S: stare mode, Ch: chopping mode).thenumber increasing as the reduction pipeline evolved.In DR2, 191 there are four parameters, in DR3 six, in DR4 seven and finally, 192 in DR5, nine parameters.All parameters are available for each 193 observational point in the raw photometry, except for the orbital 194 phase, which is calculated by the decorrelation pipeline.A de-195 scription of the meaning of the decorrelation parameters is avail-196 able in Appendix B of Popowicz et al. (2017).197The goal of the decorrelation process is to eliminate the final 198 dependence of magnitudes on the known instrumental parame-199 ters.The problem we face here is that the raw data also contain 200 the intrinsic variability, which is what we are most interested in.201 The decorrelation therefore aims to separate the intrinsic vari-202 ability from the variability caused by instrumental effects.For 203 this reason, the choice of an appropriate variability model, which 204 is fitted to Therefore, we 218

Table A .
1: General information on the 300 BRITE-Constellation target stars included in Fields 1 to 14.