data show some indications for low-frequency variability in the FS. Field 8:
No variability was detected in the scarce BHr data. Field 14: No variability
was detected in the short and scarce BAb data.

HD 65575 ($\chi$ Car, Fields 7, 8 & 14): Field 7: Observed with BTr and BAb.
The FS of the BTr and BAb data show multi-periodic variability with the
strongest peaks at frequencies of 0.6438 d-1 and 0.6126 d-1, respectively.
Field 8: Observed with BHr. The light curve is scarce, but its FS shows
variability with a frequency of 0.66 d-1. Field 14: No variability was
detected in the short and scarce BAb data set.

HD 65818 (V Pup, Fields 7, 8 & 14): Known eclipsing binary consisting of two
B-type stars. Field 7: Observed with BTr and BAb. The data clearly show
eclipses with the orbital period of about 1.45 d. Field 8: Observed with BHr.
The data set is relatively short, but the variability is clearly detectable.
Field 14: Observed with BAb. Again, the data set is relatively short, but
confirms the period found from the other BRITE observations.

HD 66811 ($\zeta$ Pup, Fields 7, 8 & 14): O-type supergiant. Field 7: Observed
with BTr and BAb. The FSa of the data show clear variability with a frequency
of 0.562 d-1. Field 8: Observed with BHr. The FS of the data shows the same
frequency as detected in the Field 7 data set. 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 ($\rho$ Pup, Field 12): Known $\delta$ 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 ($\gamma^{1}$/$\gamma^{2}$ Vel, Fields 7, 8 & 14): Wolf-Rayet
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 data set. Using BRITE-Constellation data, $\gamma$
Vel was studied in detail by Richardson et al. (2017b).

HD 68553 (h1 Pup, Field 7): Observed with BTr. The data show clear
variability.

HD 69142 (h2 Pup, Field 7): No variability was detected in the short and
scarce BTr data set.

HD 71129 ($\varepsilon$ Car, Field 7): Observed with BAb and BTr. The BAb data
set 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
data set.

HD 73634 (e Vel, Field 7): No variability was detected in the BTr and short
and scarce BAb data sets.

HD 74006 ($\beta$ Pyx, Field 7): No variability was detected in the BTr data
and in the short and scarce BAb data set. 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 & 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 data set 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 data set is short and
scarce, but its FS shows variability with a frequency of 0.63 d-1.

HD 74575 ($\alpha$ 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 data set.

HD 74956 ($\delta$ 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 data set is
short and shows weak variability. No variability was detected in the short and
scarce BAb data set.

HD 75311 (f Car, Fields 7 & 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
data set.

HD 75821 (f Vel, Field 7): No variability was detected in the short and scarce
BAb data set.

HD 76728 (c Car, Fields 7 & 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 data set.

HD 77002 (b1 Car, Field 7): No variability was detected in the short and
scarce BTr data set.

HD 78004 (c Vel, Field 7): No variability was detected in the BTr data set.
The BAb data set consists only of a few data points.

HD 78647 ($\lambda$ Vel, Field 7): Observed with BTr and BAb. The BTr light
curve shows complex long-term variability. The BAb data set is short and
scarce.

HD 79351 (a Car, Fields 7 & 14): Field 7: Observed with BTr and BAb. The FS of
the BTr data shows multi-frequency variability with the strongest peak at a
frequency of 0.3725 d-1. The FS of the BAb data confirms the multi-frequency
variations, but the data are noisier. Field 14: No variability was detected in
the short and scarce BAb data set.

HD 79940 (k Vel, Field 7): No variability was detected in the short and scarce
BTr data.

HD 80230 (g Car, Field 7): Observed with BTr. The light curve shows a dominant
period of 12.17 d.

HD 80404 ($\iota$ Car, Fields 7 & 14): Field 7: No variability was detected in
the BTr and BAb data. Field 14: Observed with BAb. The data set is short and
scarce, but its FS shows variability with a frequency of 1.1509 d-1.

HD 81188 ($\kappa$ Vel, Fields 7 & 14): Field 7: Observed with BTr and BAb.
The FS of the data shows multi-frequency variability with the strongest peak
at a frequency of 0.2431 d-1. Field 14: No variability was detected in the
short and scarce BAb data set.

HD 82434 ($\psi$ Vel, Field 7): No variability was detected in the BTr data
and the short and scarce BAb data set.

HD 82668 (N Vel, Field 7): Observed with BTr and BAb. The FS of the BTr data
shows complex multi-frequency variability, while the BAb data set is short and
scarce.

HD 83183 (h Car, Field 7): No variability was detected in the BTr data and in
the short and scarce BAb data set.

HD 83446 (M Vel, Field 7): Observed with BTr and BAb. The FS of the BTr data
show $\delta$ Sct-type variability with the strongest peak at a frequency of
31.08 d-1. The BAb data set is shorter and of inferior quality.

HD 86440 ($\phi$ Vel, Field 7): No variability was detected in the BAb and BTr
data.

HD 118716 ($\varepsilon$ Cen, Field 2): Known $\beta$ Cep star, observed with
BTr, BLb, UBr and BAb. The FSa of the UBr and BAb data show clear pulsational
variability with many frequencies and the strongest peak at a frequency of
5.8955 d-1. The BTr and BLb data sets are scarce, but the main pulsation
frequency can still be identified in the FSa of both data sets.

HD 120307 ($\nu$ Cen, Field 2): Observed by BTr, BLb, BAb and UBr. The BAb and
UBr data are of excellent quality and show clear variability with a period of
about 2.62 d. The BTr and BLb data sets are significantly shorter, but confirm
the variability. The variability is due to the reflection effect in a binary
system (Jerzykiewicz et al. 2021).

HD 120324 ($\mu$ Cen, Field 2): Known Be star, observed by BLb, BTr, BAb and
UBr. The BAb and UBr data show significant, possibly irregular variations. The
BLb and BTr data sets are shorter, but confirm the variability. BRITE data of
this star were studied in detail by Baade et al. (2016).

HD 121263 ($\zeta$ Cen, Field 2): Heartbeat binary star observed with BAb,
UBr, BLb and BTr. In the FSa of the BAb and UBr data the strongest peaks lie
at a frequency of 0.1244 d-1, corresponding to a period of $\sim$8.026 d. The
data sets from BLb and BTr are shorter, but confirm the detected period.

HD 121743 ($\phi$ Cen, Field 2): Observed with UBr, BTr, BAb and BLb. The FSa
of the BAb and BLb data show the strongest peak at a frequency of 0.88 d-1.
This signal is weaker in the FSa of the UBr and BTr data, however.

HD 121790 ($\upsilon^{2}$ Cen, Field 2): No variability was detected in the
BAb data or UBr data sets. The BAb observations have a large gap in the middle
of the run. The BTr data set is short and scarce.

HD 122451 ($\beta$ Cen, Field 2): Observed with BAb, UBr, BTr and BLb. As this
star is very bright, the acquired CCD subraster was overexposed and parts of
the light curves have high scatter. The FS of the BAb data shows multi-
frequency pulsations with the strongest peak at a frequency of 0.8689 d-1. The
UBr data are of similar quality. The BTr and BLb data sets are shorter.

HD 122980 ($\chi$ Cen, Field 2): Observed with BAb, UBr and BTr. The BAb data
set has a gap in the centre and does not show any significant variability. The
FS of the UBr data shows the strongest peak at $\sim$1.002 d-1, which is of
instrumental origin. The BTr data set is significantly shorter and does not
show any variability.

HD 125238 ($\iota$ Lup, Field 2): Observed with UBr, BAb and BTr. The UBr data
set has the longest time base and best quality and its FS shows several peaks
in the low frequency domain; the strongest peak is located at a frequency of
0.2974 d-1. The BAb data set has a gap in the centre and the BTr data set has
a significantly shorter time base. The FSa of both data sets confirm the low-
frequency variability detected in the UBr data.

HD 125823 (a Cen, Field 2): Observed with UBr, BTr and BAb. The UBr light
curve reveals rotational variability with a period of $\sim$8.85 d. The BAb
light curve has a gap in the centre, but confirms the period obtained with the
UBr data. The BTr light curve is significantly shorter, but the variability is
consistent with that seen in the UBr and BAb light curves.

HD 126341 ($\tau^{1}$ Lup, Field 2): Known $\beta$ Cep-type pulsator, observed
with BAb, UBr, BTr and BLb. The FSa of the BAb and UBr data show the strongest
peak at frequency of $\sim$5.6 d-1. The BTr and BLb data have shorter time
bases, but confirm this variability.

HD 126354 ($\tau^{2}$ Lup, Field 2): Observed with UBr, BAb and BTr. The FS of
the UBr data shows an instrumental frequency of about 1 d-1 and a few lower-
amplitude peaks. The BAb data set has a gap in the middle and the BTr data set
has shorter time base, but their FSa confirm the frequencies found from the
UBr data set.

HD 127381 ($\sigma$ Lup, Field 2): Observed with UBr, BAb and BTr. The FS of
the UBr data shows a clear peak at a frequency of 0.33 d-1. The BAb data set
has a gap in the middle of the run. The BTr data set is significantly shorter,
but both data sets confirm the variability detected from the UBr observations.

HD 127972/3 ($\eta$ Cen, Field 2): Known Be star, observed with BTr, BLb, UBr
and BAb. The FSa of the UBr and BAb data show clear variability with the
strongest peak at a frequency of 1.55 d-1. The BTr and BLb data sets are
shorter, but their analysis confirmed the main frequency found from the UBr
and BAb data. BRITE data of this star were studied in detail by Baade et al.
(2016).

HD 128345 ($\rho$ Lup, Field 2): Observed with UBr, BAb and BTr. The FS of the
UBr data shows clear variability with a frequency of 2.245 d-1. The BAb data
set has a gap in the middle of the run, but its analysis confirms this
variability. The BTr data set is shorter and of poorer quality.

HD 128620/1 ($\alpha$ Cen, Field 2): Observed with BAb, BTr and BLb. The BAb
light curve shows a period of 29.85 d. The BTr and BLb data sets are shorter
and of poorer quality. Due to the brightness of the star, the acquired CCD
subraster is severely overexposed and parts of the light curves have increased
scatter.

HD 128898 ($\alpha$ 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
data sets. The BLb and BTr data sets are shorter, but theis 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).

HD 129056 ($\alpha$ Lup, Field 2): Known $\beta$ Cep-type star. Observed with
BAb, UBr, BTr and BLb. The $\beta$ 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 data sets are shorter, but
their FSa confirm the strongest peak found in the analysis of the BAb and UBr
data sets.

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 data set has a gap in the middle of the run
and the BTr data set 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 ($\beta$ 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 ($\kappa$ Cen, Field 2): Observed with UBr, BAb, BTr and BLb. The
FSa of the UBr and BAb data show multiple significant frequencies around
$\sim$0.698 d-1. The BTr and BLb data sets are significantly shorter, but
their analysis confirms this variability.

HD 133242/3 ($\pi$ Lup, Field 2): No variability was detected in the BTr data.

HD 134481/2 ($\kappa$ Lup, Field 2): No variability was detected in the UBr,
BAb and BTr data. The BAb data set has a gap in the middle of the run and the
BTr data set is rather short.

HD 134505 ($\zeta$ Lup, Field 2): No variability was detected in the UBr, BAb,
BTr and BLb data. The BTr and BLb data sets are short.

HD 135379 ($\beta$ Cir, Field 2): Observed with UBr, BAb and BTr. The FSa of
the UBr and BAb data show low-frequency variability. The BAb data set has a
gap in the middle of the run and the BTr data have a relatively short time
base.

HD 135734 ($\mu$ Lup, Field 2): No variability was detected in the UBr, BAb
and BTr data. The BTr data set is short.

HD 136298 ($\delta$ Lup, Fields 2 & 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 $\sim$1.27 d-1. The BTr
and BLb data sets 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 ($\gamma$ 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 data set has a large gap in
the middle of the run and does not show any variability. The BTr data set is
significantly shorter, but its FS confirms the two strongest peaks found in
the FS of the UBr data.

HD 136504 ($\varepsilon$ Lup, Fields 2 & 9): Field 2: Observed with UBr, BAb,
and BTr. The UBr light curve shows a clear period of $\sim$4.55 d; some
smaller peaks in the FS of the UBr data might also be intrinsic. The BAb data
set has a gap in the middle of the run, but confirms the main period found
from the UBr observations. The BTr data set is too short for any conclusive
analysis. Field 9: Observed by BLb. The BLb light curve was analysed by Pablo
et al. (2019), who identified a weak intrinsic signal at the orbital
frequency. The light curve is otherwise free of any obvious variability.

HD 136664 ($\phi^{2}$ Lup, Field 9): No variability was detected in the noisy
BHr data set.

HD 138690 ($\gamma$ Lup, Fields 2 & 9): Close visual double, one component of
which is a single-lined spectroscopic system with an orbital period of 2.8 d.
Field 2: Observed with UBr, BAb, BTr and BLb. The UBr and BAb data show clear
variability with the orbital period. The BTr and BLb data sets are
significantly shorter, but the same variability can also be identified. Field
9: Observed with BLb, UBr, BHr and BAb. The FSa of the BLb, UBr and BHr data
show a clear peak at 0.351 d-1, corresponding to the orbital period. The BAb
data set is short and scarce. A detailed analysis of the BRITE data of this
star was presented by Jerzykiewicz et al. (2021).

HD 139127 ($\omega$ Lup, Field 2): No variability was detected in the short (8
days long) UBr data set.

HD 139365 ($\tau$ Lib, Field 9): Early B-type spectroscopic binary exhibiting
a heartbeat. Observed with BHr, UBr and BLb. The data show variability with
the orbital period of 3.45 d. These results were first reported by Pigulski et
al. (2018b).

HD 141556 ($\chi$ Lup, Field 9): No variability was detected in the BLb, BHr
or UBr data.

HD 142669 ($\rho$ Sco, Field 9): Observed with BLb, UBr and BHr. The BLb light
curve exhibits small scatter and its FS reveals a highly significant signal at
0.3697 d-1. This frequency is also found in the FS of the BHr data. The UBr
data are of inferior quality and show no significant signal. When phased
according to the corresponding period, the BLb and BHr data yield a light
curve that is consistent with ellipsoidal variability.

HD 143018 ($\pi$ Sco, Field 9): Observed with BAb, BHr, BLb and UBr. The FSa
of the data show clear variability with the most prominent frequency at 1.2735
d-1 which is twice the orbital frequency. The data were analysed in detail by
Pigulski et al. (2017), who found also pulsation with a frequency
corresponding to a p mode.

HD 143118 ($\eta$ Lup, Field 9): Observed with BLb, UBr and BHr. The FS of the
BLb data shows a weak signal at 0.206 d-1. No signal was detected in the
noisier UBr and the shorter BHr data sets.

HD 143275 ($\delta$ Sco, Field 9): This is an early B-type Be star in an
extraordinarily eccentric, 10.8-yr spectroscopic binary. Observed by BLb, UBr
and BAb. The FSa of the data show a weak low-frequency variation.

HD 144217/8 ($\beta^{1}/\beta^{2}$ Sco, Field 9): Observed with UBr, BLb and
BAb. The FSa of the UBr and BLb data show a signal at 0.448 d-1 with a
possible triplet structure. The BAb data set is sparse.

HD 144294 ($\theta$ Lup, Field 9): No variability was detected in the BLb
data.

HD 144470 ($\omega^{1}$ Sco, Field 9): No variability was detected in the BLb,
BHr, UBr and BAb data.

HD 145482 (c2 Sco, Field 9): Observed with BHr. The FS of the data shows clear
signals at 0.173 d-1 and 1.177 d-1.

HD 145502/1 ($\nu$ Sco, Field 9): Observed with UBr and BLb. The FS of the UBr
data shows a clear signal at $0.172$ d-1 and possible additional peaks at
0.824 d-1 and 1.174 d-1 with a possible triplet centred at 1.574 d-1. The BLb
data set is of insufficient length to reveal the signal.

HD 147165 ($\sigma$ Sco, Field 9): This is a binary system consisting of two
early B-type main-sequence components, with the primary star exhibiting
$\beta$ Cep-type pulsations. Observed by BHr, BLb, UBr and BAb. The FSa of the
data show complex variability with a principal peak at 4.0509 d-1, but with
several other peaks of comparable amplitude. The BRITE observations were first
discussed and interpreted by Pigulski et al. (2018a).

HD 148478/9 ($\alpha$ Sco, Antares, Field 9): M-type supergiant, observed by
UBr, BLb and BAb. The light curves show long-term variability.

HD 148688 (V1058 Sco, Field 9): Early B-type supergiant, observed by BHr. The
FS of the data shows stochastic low-frequency variability typical for evolved
B-type stars.

HD 148703 (N Sco, Field 9): Eccentric eclipsing binary system observed by BHr,
UBr and BLb. The BHr and UBr light curves reveal eclipses. The orbital period
of the system is long and the BLb light curve does not cover any eclipse.

HD 149038 ($\mu$ Nor, Field 9): Observed with BHr. The FS of the data shows
the typical stochastic low-frequency signal characteristic of evolved O and
B-type stars.

HD 149404 (V918 Sco, Field 9): Evolved, post-Roche-lobe overflow non-eclipsing
O-type binary, observed with BHr. The FS appears as typical for an O-type
supergiant with a strong peak at 0.205 d-1 corresponding to half the 9.84-d
orbital period. A detailed study of the BHr data (in combination with the SMEI
data) was presented by Rauw et al. (2019).

HD 149438 ($\tau$ Sco, Field 9): No variability was detected in the UBr, BHr
and BLb data. The BLb measurements show some minor contamination due to
scattered moonlight near dates of lunar conjunction.

HD 151680 ($\varepsilon$ Sco, Field 9): No variability was detected in the BLb
and UBr data.

HD 151804 (V973 Sco, Field 9): Observed with BHr. The FS of the data exhibits
a typical stochastic low-frequency signal of evolved O-type stars.

HD 151890 ($\mu^{1}$ Sco, Field 9): Observed with UBr, BHr and BLb. The FSa of
the data show strong variability with a frequency of $1.383$ d-1,
corresponding to half of the known 1.446 d orbital period.

HD 151985 ($\mu^{2}$ Sco, Field 9): Observed with BLb, BHr and UBr. The FSa of
the BLb and BHr data show a weak signal at 1.383 d-1, the same as detected in
the nearby (5.8$\arcmin$ apart) $\mu^{1}$ Sco. This means that the photometry
pipeline did not separate well the contribution from both stars. The FS of the
UBr data shows a somewhat weaker signal at this frequency, but also at twice
this value which is 2.765 d-1.

HD 157056 ($\theta$ Oph, Field 3): This well known $\beta$ Cephei star was
observed by UBr. The data set is short and scarce, but its FS reveals the most
prominent pulsation frequency of $7.118$ d-1. This star was studied in detail
using BRITE data by Walczak et al. (2019).

HD 157792 (b Oph, Field 3): Observed by UBr. No variability was detected in
the short and scarce UBr data set.

HD 157919 (d Oph, Field 3): Observed by UBr. No variability was detected in
the short and scarce UBr data set.

HD 158408 ($\upsilon$ Sco, Field 3): Observed with UBr. The data set is short
and scarce, but the light curve shows signal with a period of 2.47 d.

HD 158926 ($\lambda$ Sco, Field 3): The star is known to be an eclipsing
$\beta$ Cep star. Observed with UBr. The data set is short and scarce and its
FS shows a high amplitude peak at a frequency of $4.679$ d-1.

HD 159433 (Q Sco, Field 3): No variability was detected in the short and
scarce UBr data set.

HD 159532 ($\theta$ Sco, Field 3): Observed with UBr. The data set is short
and scarce and shows a period of $\sim$13 d.

HD 160578 ($\kappa$ Sco, Field 3): Known $\beta$ Cep-type star. Observed with
UBr. The data set is short and scarce and its FS shows a high amplitude peak
at a frequency of $5.001$ d-1.

HD 161471 ($\iota^{1}$ Sco, Field 3): No variability was detected in the short
and scarce UBr data set.

HD 161592 (X Sgr, Field 3): Classical Cepheid, observed with UBr. The data set
is short and scarce but clearly shows the variability with the known period of
7.1 d.

HD 161892 (G Sco, Field 3): No variability was detected in the short and
scarce UBr data set. The star was included in the study of Kallinger et al.
(2019).

HD 164975 ($\gamma^{1}$ Sgr, Field 3): Classical Cepheid, observed with UBr.
The data set is short and scarce, but clearly shows variability with a period
of 7.7 d.

HD 165135 ($\gamma^{2}$ Sgr, Field 3): No variability was detected in the
short and scarce UBr data set. The star was included in the study of Kallinger
et al. (2019).

HD 166937 ($\mu$ Sgr, Field 3): Observed with UBr. The data set is short and
scarce with some indication of variability.

HD 167618 ($\eta$ Sgr, Field 3): Observed with UBr. The light curve is short
and scarce and shows an irregular long-term variability.

HD 168454 ($\delta$ Sgr, Field 3): No variability was detected in the short
and scarce UBr data set.

HD 169022 ($\varepsilon$ Sgr, Field 3): No variability was detected in the
short and scarce UBr data set.

HD 169916 ($\lambda$ Sgr, Field 3): No variability was detected in the short
and scarce UBr data set.

HD 173300 ($\phi$ Sgr, Field 3): No variability was detected in the short and
scarce UBr data set.

HD 186882 ($\delta$ Cyg, Fields 4 & 10): Field 4: No variability was detected
in the BLb, UBr and BTr data sets. Field 10: No variability was detected in
the BAb, BLb and UBr data.

HD 187849 (19 Cyg, Field 4): Observed with BTr. The data set is relatively
short and shows strong and clear variability with a period of $\sim$28.4 d.

HD 188892 (22 Cyg, Fields 4 & 10): Field 4: No variability was detected in the
short and scarce BLb data set. Field 10: No variability was detected in the
BTr and UBr data.

HD 188947 ($\eta$ Cyg, Field 4): No variability was detected in the BTr, UBr
and BLb data. The star was included in the study by Kallinger et al. (2019).
BTr data are of good quality, but UBr and BLb data sets are short and scarce.

HD 189178 (Field 10): No variability was detected in the short BTr data set.

HD 189687 (25 Cyg, Fields 4 & 10): Known Be star. Field 4: Observed with BLb.
The data set is short and scarce, but shows the evidence of weak variability.
Field 10: Observed with BTr and UBr. Twelve days of BTr data show clear and
complex variability. The 17 days long UBr light curve has inferior quality and
does not show the variability. The strongest signal in the FS of these data is
at 1.76 d-1.

HD 189849 (15 Vul, Field 10): Observed with BAb, BTr and UBr. No variability
was detected in UBr and BTr data. The BAb light curve is scarce and of poor
quality.

HD 191610 (28 Cyg, Fields 4 & 10): This is a known Be star. Field 4: Observed
with BTr and BLb. The data sets 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).

HD 192577/8 (31 Cyg, Fields 4 & 10): Field 4: Observed with BTr, UBr and BLb.
The BTr data reveal complex variability. The UBr and BLb data sets are short
and scarce. Field 10: No variability was detected in the scarce BLb and BAb
data sets.

HD 192640 (29 Cyg, Fields 4 & 10): Known $\delta$ Sct-type variable. Field 4:
Observed with BTr and BLb. The FSa of the data show many peaks at frequencies
typical for a $\delta$ 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 $\delta$
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 data set is short and UBr data set 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 data set.

HD 193092 (Field 4): No variability was detected in the BTr data.

HD 193237 (P Cyg, Fields 4 & 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 data set is short and scarce. Field 10: Observed
with BTr, UBr, BLb and BAb. The BTr data show clear variability. The UBr, BLb
and BAb data sets are shorter. The BRITE data for this star were investigated
in detail by Elliott et al. (2022).

HD 194093 ($\gamma$ Cyg, Fields 4 & 10): Field 4: Observed with BTr, BLb and
UBr. The BTr light curve shows some low-amplitude long-term variability, while
the BLb data do not reveal any variability. The UBr data set 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 data set 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 $\gamma$ Dor-type pulsations with the main frequency at
1.25 d-1. No variability was detected in the short BLb data set. The star was
studied in detail by Zwintz et al. (2017).

HD 195295 (41 Cyg, Fields 4 & 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 ($\omega^{1}$ Cyg, Field 10): Observed with BAb and BTr. The BAb
data set is of poor quality. The BTr data set 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 data set is scarce.

HD 197345 ($\alpha$ Cyg, Fields 4 & 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 data set 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 data sets.

HD 197989 ($\varepsilon$ Cyg, Fields 4 & 10): Field 4: No variability was
detected in the BLb and BTr data or in the short and scarce UBr data set.
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 ($\lambda$ Cyg, Fields 4 & 10): Field 4: Observed with BLb, UBr and
BTr. The BLb and UBr data sets 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 data set is of poor quality, the BLb data set is short.

HD 198478 (55 Cyg, Fields 4 & 10): Field 4: Observed with BTr and BLb. The FS
of the BTr data shows complex low-frequency variability. The BLb data set 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 data set is short.

HD 198639 (56 Cyg, Field 10): No variability was detected in the BTr or BAb
data.

HD 198726 (T Vul, Fields 4 & 10): Classical Cepheid. Field 4: Observed with
BTr and UBr. The BTr light curve shows variability with a period of $\sim$4.44
d. The UBr data set 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 data set is short and scarce. No
variability was detected.

HD 199081 (57 Cyg, Fields 4 & 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
$\sim$1.1 d-1; the strongest peak is at a frequency of 0.934 d-1. The BAb and
UBr data sets are shorter, but the low-frequency variability is confirmed in
their FSa. The BLb data set is of poor quality.

HD 199629 ($\nu$ Cyg, Fields 4 & 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 & 10): Known Be star. Field 4: No variability was
detected in the short and scarce BLb data set. Field 10: Observed with BTr,
BAb and BLb. The FS of the BTr data shows clear variability with frequencies
between $\sim$1.5 and 2.2 d-1. The BAb and BLb data sets 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 data set is shorter and of poorer quality. The BLb data set is scarce.

HD 200905 ($\xi$ Cyg, Field 4): Observed with BTr and UBr. The BTr light curve
shows variability with a period of $\sim$17.3 d. No variability was detected
in the short and scarce UBr data set.

HD 201078 (DT Cyg, Fields 4 & 10): Classical Cepheid. Field 4: Observed with
BTr and UBr. The light curves show classical Cepheid variability with a period
of $\sim$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 the BTr data or in
the short and scarce UBr data set.

HD 201433 (V389 Cyg, Field 10): This is a triple system with SPB pulsations,
observed with BTr and BLb. The BTr light curve shows SPB-type pulsations,
confirmed also in the BLb data despite their scarcity. The BRITE data of this
star were discussed in detail by Kallinger et al. (2017).

HD 202109 ($\zeta$ Cyg, Fields 4 & 10): Field 4: No variability was detected
in the BLb and BTr data or in the short and scarce UBr data sets. Field 10: No
variability was detected in the UBr and BAb data or in the short and scarce
BLb data set.

HD 202444 ($\tau$ Cyg, Fields 4 & 10): Field 4: No variability was detected in
the BLb and BTr data or in the short and scarce UBr data set. Field 10: No
variability was detected in the BAb data or in the short and scarce BLb data
set.

HD 202850 ($\sigma$ Cyg, Fields 4 & 10): Field 4: Observed with BTr, BLb and
UBr. The FSa of the BTr and BLb data show some low-frequency variability. The
UBr data set is short and scarce. Field 10: Observed with BAb, BLb and BTr.
The FS of the BTr data shows low-frequency variability. The BAb and BLb data
sets are shorter and scarce.

HD 202904 ($\upsilon$ Cyg, Fields 4 & 10): Known Be star. Field 4: Observed
with BTr, BLb and UBr. The FS of the BTr data shows strong variability at very
low frequencies. The FS of the BLb data reveals a frequency of $\sim$1.47 d-1
on the top of the lower frequency variability. The UBr data set is short and
scarce. Field 10: Observed with BTr, BAb and BLb. The FS of the BTr data shows
clear variability with a frequency of 1.47 d-1. The BAb and BLb data sets are
shorter and scarce.

HD 203064 (68 Cyg, Fields 4 & 10): Field 4: No variability was detected in the
BTr and BLb data. Field 10: No variability was detected in the BTr data or in
the short and scarce BAb and BLb data sets.

HD 203156 (V1334 Cyg, Fields 4 & 10): Known classical Cepheid. Field 4:
Observed with BTr and UBr. The light curves clearly show variability with a
period of $\sim$3.3 d. Field 10: Observed with BTr and BLb. The variability
seen in the Field 4 data is confirmed in the BTr data set. The BLb data set is
short and scarce.

HD 203280 ($\alpha$ Cep, Field 11): No variability was detected in the short
BLb data set.

HD 205021 ($\beta$ Cep, Field 11): The BHr and BLb data sets are very sparse
and not useful for scientific analysis.

HD 205435 ($\rho$ Cyg, Field 10): No variability was detected in the good-
quality BTr and UBr data or in the short and scarce BLb data set.

HD 206570 (V460 Cyg, Field 4): No variability was detected in the BTr data.

HD 207260 ($\nu$ Cep, Field 11): Observed with BHr and BLb. The FS of the BHr
data shows weak low-frequency variability. The BLb data set is short and of
lower precision.

HD 209790 ($\xi$ Cep, Field 11): No variability was detected in the BHr data
and in the short BLb data set.

HD 209975 (19 Cep, Field 11): Observed with BHr and BLb. The FSa of the BHr
data show some stochastic low-frequency variability. The BLb data set is short
and scarce.

HD 210745 ($\zeta$ Cep, Field 11): No variability was detected in the BHr
data.

HD 211336 ($\varepsilon$ Cep,Field 11): Known $\delta$ Sct-type pulsator,
observed with BTr, BLb and BHr. The FSs of the BTr and BLb data show $\delta$
Sct-type variability. The BHr data set is short and not usable.

HD 213306 ($\delta$ Cep, Field 11): This is the prototype of classical
Cepheids. Observed by BTr, BLb and BHr. The data are of excellent quality and
show variability with a period of $\sim$5.4 d.

HD 216228 ($\iota$ Cep, Field 11): No variability was detected in the
relatively short BHr data set.

HD 218376 (1 Cas, Field 11): No variability was detected in the short BLb and
BHr data sets.

HD 220652 (4 Cas, Field 11): Observed with BHr. The data set is short and its
FS shows some low-frequency variability.

HD 221253 (AR Cas, Field 11): Known eclipsing and spectroscopic binary.
Observed with BLb and BHr. The light curves show clear eclipses with an
orbital period of $\sim$6.1 d.

HD 224572 ($\sigma$ Cas, Field 11): No variability was detected in the BAb
data set.

HD 225289 (V567 Cas, Field 11: No variability was detected in the short BHr
data set.

##  Appendix C Format of BRITE-Constellation data in the archives

###  C.1 Contents of the BRITE-Constellation data in the archives

All decorrelated BRITE-Constellation data described and illustrated in this
article are freely available for download from the BRITE Public Data Archive
(PDA)141414https://brite.camk.edu.pl/pub and the Canadian Astronomy Data
Centre (CADC)151515https://www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/en/.

Both databases provide the data as ASCII files split into setups (explained in
Appendix C.2). For each setup, five different files are available. They
contain the original time series (i.e., before the decorrelation procedure),
the decorrelated time series, the time series containing averages per
satellite orbit, the variability model used in the decorrelation, and the log
file generated by the software during the decorrelation. All files have
headers that describe their contents in detail. The files containing
photometric time series (i.e., original, decorrelated and orbit averaged data)
include columns with the Heliocentric or Barycentric Julian Date, instrumental
magnitudes including errors and magnitudes with the mean instrumental
magnitude of the given setup subtracted. Observations with the largest errors
are filtered out during the decorrelation process. For further analyses, the
provided errors in magnitudes can be used to filter the data if needed.

###  C.2 BRITE-Constellation photometry subrasters and setups

The following brief explanation of the subrasters and setups used for BRITE-
Constellation observations provides essential guidance for a better
understanding of BRITE-Constellation data. More details are given in Popowicz
et al. (2017).

The full frame CCD images of the BRITE-Constellation satellites cannot be
transferred to ground at the cadence taken in space which is typically about
20 s. Therefore, in the context of BRITE photometry, the expression
‘subrasters’ concerns the definition of which parts of the full frame CCD are
rendered into images before transmitting to the ground. For that the $(x,y)$
starting position on the CCD is provided and the $x$ and $y$ size of each
subraster is required. In stare mode, those regions of interest or subrasters
are 24 $\times$ 24 pixels in size, while in chopping mode they are rectangular
and cover 24 $\times$ 48 pixels. Typically 15 to 30 subrasters are set up for
each satellite and observing campaign. With a few exceptions, each subraster
contains the profile of a single target in its central part in the case of
stare mode. In chopping mode, a star is located either on 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
utilized. 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.

###  C.3 Recommendations on combining individual setups and data sets 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
cause different offsets to be taken into account 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 $\sigma_{\rm orbit}^{\rm
med}$ 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.

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 12 to 16 illustrate the noise properties for each of the five BRITE-
Constellation instruments individually.

Figure 12:  Values of $\sigma_{\rm orbit}^{\rm med}$ plotted as a function of
instrumental BRITE magnitude for UBr setups. Figure 13:  Values of
$\sigma_{\rm orbit}^{\rm med}$ plotted as a function of instrumental BRITE
magnitude for BAb setups. Figure 14:  Values of $\sigma_{\rm orbit}^{\rm med}$
plotted as a function of instrumental BRITE magnitude for BTr setups. Figure
15:  Values of $\sigma_{\rm orbit}^{\rm med}$ plotted as a function of
instrumental BRITE magnitude for BLb setups. Figure 16:  Values of
$\sigma_{\rm orbit}^{\rm med}$ plotted as a function of instrumental BRITE
magnitude for BHr setups.

##  Appendix E Field maps

Sky maps of the Fields 1 to 14 observed by BRITE-Constellation are shown in
Figs. 17, 18 and 19: Observed stars are marked as red filled circles where the
size of the symbol corresponds to the magnitude. The black numbers next to
those symbols are HD identifiers (see Table 2). The names of the stellar
constellations are given in blue.

Figure 17: BRITE-Constellation field maps: Fields 1 to 6.

Figure 18: BRITE-Constellation field maps: Fields 7 to 12.

Figure 19: BRITE-Constellation field maps: Fields 13 and 14.