<table><caption>**Table 2**
The Full Sample (Including the Non-Be Stars)</caption><thead><tr><th>TIC ID</th><th>Common ID</th><th>ST</th><th>Data Quality</th><th>Be</th><th>Signals</th><th>N<sub>groups</sub></th><th>Typical groups</th><th>f<sub>g1</sub> (day<sup>-1</sup>)</th><th>f<sub>g2</sub> (day<sup>-1</sup>)</th><th>Stronger group</th><th>T<sub>mag</sub> (mag)</th><th>Contam. Ratio</th></tr></thead><tbody><tr><td>1748132</td><td>HD 75740</td><td>A0IIIe</td><td>0</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>9.56</td><td>0.0309</td></tr><tr><td>3178733</td><td>HD 147580</td><td>B7Ve</td><td>0</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>9.27</td><td>0.5010</td></tr><tr><td>4827953</td><td>V647 Mon</td><td>B1Vne</td><td>1</td><td>Y</td><td>S/G</td><td>1</td><td>N</td><td>...</td><td>...</td><td>...</td><td>9.04</td><td>0.0120</td></tr><tr><td>5528993</td><td>HD 89884</td><td>B5IIIe</td><td>1</td><td>Y</td><td>G</td><td>4</td><td>Y</td><td>1.22</td><td>2.45</td><td>g2</td><td>7.26</td><td>0.0011</td></tr><tr><td>6110321</td><td>SS 120</td><td>B8e:</td><td>1</td><td>Y</td><td>I/H/G</td><td>2</td><td>Y</td><td>2.76</td><td>5.42</td><td>g2</td><td>10.61</td><td>0.1028</td></tr><tr><td>10176636</td><td>V757 Mon</td><td>B3IV</td><td>1</td><td>Y</td><td>G</td><td>4</td><td>Y</td><td>0.84</td><td>1.60</td><td>g2</td><td>6.69</td><td>0.0046</td></tr><tr><td>10536200</td><td>CD-53 6689</td><td>B2.5IVne</td><td>1</td><td>Y</td><td>L/F+/G</td><td>3</td><td>Y</td><td>1.17</td><td>2.18</td><td>sim.</td><td>9.45</td><td>0.3303</td></tr><tr><td>11411724</td><td>StHA 52</td><td>B1.5V</td><td>1</td><td>U</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>7.62</td><td>0.0061</td></tr><tr><td>11559798</td><td>OY Hya</td><td>B5Ve</td><td>1</td><td>Y</td><td>I/L/G</td><td>2</td><td>Y</td><td>2.35</td><td>5.08</td><td>sim.</td><td>6.29</td><td>0.0009</td></tr><tr><td>11972111</td><td>HD 84567</td><td>B0.5IIIne</td><td>1</td><td>Y</td><td>S/I/L</td><td>0</td><td>N</td><td>...</td><td>...</td><td>...</td><td>5.97</td><td>0.0006</td></tr><tr><td>14088298</td><td>HD 33453</td><td>B8Vne</td><td>1</td><td>Y</td><td>G</td><td>2</td><td>Y</td><td>3.28</td><td>6.53</td><td>g1</td><td>8.10</td><td>0.0001</td></tr><tr><td>14498757</td><td>OT Gem</td><td>B2Ve</td><td>1</td><td>Y</td><td>S/L/F+/G</td><td>3</td><td>Y</td><td>2.12</td><td>4.01</td><td>g2</td><td>6.48</td><td>0.0125</td></tr><tr><td>14709809</td><td>RY Gem</td><td>A2Ve</td><td>1</td><td>N</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>8.72</td><td>0.0111</td></tr><tr><td>16688664</td><td>CP-45 8706</td><td>B9</td><td>0</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>10.28</td><td>0.3102</td></tr><tr><td>16902823</td><td>HD 159489</td><td>B1Ve</td><td>1</td><td>Y</td><td>S/L/F/G</td><td>3</td><td>Y</td><td>1.05</td><td>2.06</td><td>sim.</td><td>8.21</td><td>0.0471</td></tr><tr><td>19727094</td><td>HD 148692</td><td>B7Ve</td><td>0</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>/</td><td>8.65</td><td>0.9717</td></tr></tbody></table>

Note. The TIC numbers, common ID, and spectral type (as listed on the BeSS database) are given, along with the following information. Data quality: the availability of TESS data of reasonable quality. Values of 0 mean the system was either not observed by TESS in Cycle 1, or there were significant problems with the data (including severe blending where it cannot be determined from which source(s) the detected signals originate). Be: a value of “Y” means this a classical Be star, “S” means the classical Be designation may be suspect, but there is insufficient evidence to reject it, “U” means this is rejected as a classical Be star but the nature of the system is not necessarily known, and “N” marks systems known to be something other than a classical Be star. For any star with insufficient data or that is rejected from the sample, the remaining fields are filled with “/” symbols. Signals: values of “S” indicate the presence of stochastic variability, “I” is when isolated signals exist (and “I+” when there are harmonics), “L” is for when low-frequency signals dominate, “H” is when high-frequency signals exist, “F” is for systems with flickers (and “F+” when an enhancement in frequency groups accompanies one or more flickers), and “G” is if there are frequency groups. N<sub>groups</sub>: gives the number of groups identified in the light curve, but is somewhat approximate. Typical groups: values of “Y” indicate the system has groups in the typical configuration, “?” means this is unclear, and “N” means there are not groups in the typical configuration. The final three columns give the central frequency of g1 and g2 in systems with groups having the typical configuration, and note which is the stronger of these two groups (or “sim.” if they are of similar strength). The 12th column lists the TESS magnitude, and the final column shows the contamination ratio (the ratio of flux from neighboring stars in a typical aperture divided by the flux of the target star). Table 2 is published in its entirety in machine-readable format. A portion is shown here for guidance regarding its form and content.

(This table is available in its entirety in machine-readable form.)

## Appendix D
Plots and Data for Each Target in the Sample

Plots are made for each object in the sample, and are available on Zenodo: doi:10.5281/zenodo.6290288. Figure 13 provides an example for the star j Cen (=HD 102776, TIC 325170579). All of these plots follow the same format, where the top panel shows the TESS light curve (using all TESS sectors wherein the star was observed in cycle 1), and the next panel shows the data after removing longer-term trends. The middle panel shows the wavelet transform of the long-term detrended data. The last two panels show the frequency spectrum where a lighter gray color is used for the original light curve, and black is used for the long-term detrended data. The bottom-most panel is plotted with a log-log scale. The top frequency spectrum also plots the frequency spectrum stretched by factors of two (inverted, blue), and three (offset, orange) to allow for easy comparisons when groups or isolated signals

form a (rough) harmonic series (or do not). In the linear-scale frequency spectrum panel, the classifications of the system are printed in the top right, and if there are typical frequency groups, their “weighted center of mass” locations are marked with red triangles, and also with horizontal dotted lines in the wavelet plot. Plots of this format are made from 30 minutes data, and also 2 minutes data when available.

LC data files are made available on Zenodo for each object in this sample: doi:10.5281/zenodo.6290288. The 30 minutes data were extracted according to the methods outlined in Section 2. The 2 minutes data is also made available (when it exists), and was saved to a text file from the light curve fits files available for download from the TESS mission. Whenever possible, it is advisable to use the official light curve fits files, as to have more control over the data, keeping in mind that the often-used PDCSAP flux may suppress or distort longer-term trends.
<figure><img src="image_16.png" /><figcaption>**Figure 13.** Diagnostic plot for j Cen (=TIC 325170579). See Appendix D for an explanation of the various panels. The complete set of diagnostic plots is available on Zenodo: doi:10.5281/zenodo.6290288.</figcaption></figure>

ORCID iDs

Jonathan Labadie-Bartz https://orcid.org/0000-0002-2919-6786

Alex C. Carciofi https://orcid.org/0000-0002-9369-574X

Amanda Rubio https://orcid.org/0000-0002-2490-1562

Keegan Thomson-Paressant https://orcid.org/0000-0002-2926-5171

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