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Table A.1.

Full target list of bright massive stars for the primary science case of the CubeSpec mission.

Name TIC RA dec B V Sp. Type v sin i bin Puls. Freq. Arad vel LPV study reference TESS var. Notes
(mag) (mag) (km s−1) (d−1) (km s−1)
Priority 1A: confirmed β Cep stars with pulsation analysis based on LPV in the literature
γ Peg 51942308† 00:13:14.15 15:11:00.94 2.61 2.84 B2 IV 5 ✓ 6.59 3.5 Y (Butkovskaya & Plachinda 2007) − 1
ϵ Per 187107884 03:57:51.23 40:00:36.78 2.71 2.89 B1.5 III 130 ✓ [5.30, 10.59] < 1 Y (De Cat et al. 2000) β Cep 1
ν Eri 229087301 04:36:19.14 -03:21:08.86 3.74 3.93 B2 III 20 [5.62, 5.76] < 20 Y (Aerts et al. 1994b) β Cep 2
η Ori 4254645 05:24:28.62 -02:23:49.73 3.18 3.35 B1 V + B2: 503 ✓ β Cep + EB 1
η Ori A 4254645 05:24:28.73 -02:23:49.31 3.42 3.59 B1 V 130 ✓ 7.69 < 1 Y (De Mey et al. 1996) β Cep + EB
β CMa 34590771 06:22:41.99 -17:57:21.31 1.73 1.97 B1 II-III ≃1 [3.97, 4.18] < 11 Y (Aerts et al. 1994b) β Cep 4
β Cru 405567821 12:47:43.27 -59:41:19.58 1.02 1.25 B1 IV 18 ✓ [5.23, 5.96] < 3 Y (Aerts et al. 1998) β Cep 1, 2
α Vir 178999156† 13:25:11.58 -11:09:40.75 0.74 0.97 B1 V 160 ✓ [0.50,7.50] < 4 Y (Smith 1985) − 1, 5
ϵ Cen 241398115 13:39:53.26 -53:27:59.01 2.08 2.30 B1 III 115 ? [5.69, 7.65] < 1 Y (Schrijvers 1999) β Cep 1, 6
ν Cen 166447153 13:49:30.28 -41:41:15.75 3.19 3.39 B2 IV 65 ✓ [2.35, 7.95] < 1 Y (Schrijvers & Telting 2002) β Cep + rot/bin 1
β Cen 328329822 14:03:49.41 -60:22:22.93 0.38 0.60 B1 III 100 ✓ [6.41, 6.51] < 4 Y (Ausseloos et al. 2002) β Cep 1, 2, 7
α Lup 129117325 14:41:55.76 -47:23:17.52 2.13 2.29 B1.5 III ≃1 [3.85, 4.22] < 7 Y (Mathias et al. 1994) β Cep 2
δ Lup 148415949 15:21:22.33 -40:38:51.02 3.00 3.19 B1.5 IV 190 ? 5.05 4 Y (Lloyd & Pike 1988) β Cep 1, 2
ϵ Lup 147226597 15:22:40.87 -44:41:22.61 3.19 3.37 B2 IV-V 40-170 ✓ 10.36 < 1 Y (Uytterhoeven et al. 2005a) β Cep 1, 6
β Sco 9921163† 16:05:26.23 -19:48:19.40 2.43 2.50 B1 V + B2 V 90 ✓ 5.77 < 14 Y (Holmgren et al. 1997) −
β1 Sco 9921163† 16:05:26.23 -19:48:19.63 2.55 2.62 B1 V 130 ✓ Y (Holmgren et al. 1997) −
ω1 Sco 161828468† 16:06:48.43 -20:40:09.09 3.92 3.97 B1 V 110 ≃15 15 Y (Telting & Schrijvers 1998) −
σ Sco 322928423† 16:21:11.32 -25:35:34.05 3.02 2.89 O9.5 V + B7 V 50 ✓ [4.05, 4.17] < 40 Y (Mathias et al. 1991) − 1, 2, 8
θ Oph 83852015† 17:22:00.58 -24:59:58.37 3.03 3.26 B2 V + B5 V 35 ✓ [7.12, 7.47] < 5 Y (Briquet et al. 2005) − 1, 2
λ Sco 465088681 17:33:36.52 -37:06:13.76 1.48 1.62 B2 IV + DA7.9 120 ✓ [3.57, 5.37] < 5 Y (Uytterhoeven et al. 2004) β Cep + EB 1, 2, 9
ι Her 164319891 17:39:27.89 46:00:22.80 3.63 3.80 B3 IV ≃0 ✓ ≃8 < 3 Y (Chapellier et al. 1987) β Cep + SLF 1, 2
κ Sco 147868882 17:42:29.28 -39:01:47.94 2.21 2.39 B1.5 III 115 ✓ [4.87, 5.00] < 2 Y (Uytterhoeven et al. 2005b) β Cep 1, 2
β Cep 321818578 21:28:39.60 70:33:38.57 3.01 3.23 B0.5 III 25 ✓ [4.92, 5.42] < 21 Y (Aerts et al. 1994a) β Cep 1
Priority 1B: stars that are known to exhibit LPV from pulsations in the literature
ζ CMa 124918771 06:20:18.79 -30:03:48.12 2.83 3.00 B2.5 V 25 ✓ Y (Telting et al. 2006) SLF 1
α Pyx 185815213 08:43:35.54 -33:11:10.99 3.50 3.68 B1.5 III 20 Y (Telting et al. 2006) SLF
δ Cru 390320354 12:15:08.72 -58:44:56.14 2.57 2.75 B2 IV 135 Y (Telting et al. 2006) β Cep
σ Cen 21165132 12:28:02.38 -50:13:50.29 3.72 3.91 B2 V 170 Y (Telting et al. 2006) β Cep
α Mus 327150358 12:37:11.02 -69:08:08.03 2.48 2.65 B2 IV 115 ? Y (Telting et al. 2006) SLF 1
ϕ Cen 359762838 13:58:16.27 -42:06:02.71 3.61 3.80 B2 IV 80 Y (Telting et al. 2006) β Cep
υ1 Cen 359916090 13:58:40.75 -44:48:12.91 3.67 3.87 B2 IV-V 125 Y (Telting et al. 2006) β Cep
β Lup 333947284 14:58:31.93 -43:08:02.27 2.46 2.68 B2 III 120 Y (Schrijvers 1999) β Cep
ρ Sco 77541886 15:56:53.08 -29:12:50.66 3.66 3.86 B2 IV-V 100 ✓ Y (Telting et al. 2006) β Cep 1
κ Cen 333950446 14:59:09.68 -42:06:15.11 2.93 3.13 B2 IV 30 ? Y (Telting et al. 2006) β Cep 1, 10
δ Sco 12725034† 16:00:20.01 -22:37:18.14 2.20 2.32 B0.3 IV 150 ✓ Y (Telting et al. 2006) − 1
υ Sco 175627991 17:30:45.84 -37:17:44.93 2.47 2.70 B2 IV 30 Y (Telting et al. 2006) SLF 11
Priority 1C: stars that exhibit high-frequency pulsation modes in TESS photometry but lack spectroscopic confirmation of LPV in the literature
ζ Cas 240669906 00:36:58.28 53:53:48.87 3.47 3.66 B2 IV 1012 N (Telting et al. 2006) β Cep 13
a Car 385220745 09:10:58.09 -58:58:00.82 3.25 3.40 B2 IV-V 30 ✓ N (Telting et al. 2006) β Cep + SLF 1, 10
ρ Cen 334217681 12:11:39.13 -52:22:06.41 3.81 3.96 B3 V 1403 ? β Cep 1, 14
α1 Cru 450568754 12:26:35.90 -63:05:56.73 1.10 1.28 B0.5 IV 1203 ✓ β Cep 1, 15
α2 Cru 450568754 12:26:36.44 -63:05:58.28 1.41 1.58 B1 V 2003 ✓ β Cep 1, 15
γ Mus 360263464 12:32:28.01 -72:07:58.76 3.73 3.88 B3 V 1903 β Cep/SPB 16, 17
β Mus 329162201 12:46:16.80 -68:06:29.22 3.38 3.04 B2 V + B3 V 14018 ✓ β Cep 1, 14, 19
η Lup 59095516 16:00:07.33 -38:23:48.15 3.19 3.41 B2.5 IV 19018 ? β Cep 1, 20
Priority 2: stars with high-amplitude g-mode pulsations (found in TESS light curves and LPV studies and/or photometry in literature)
γ Cas 51962733 00:56:42.53 60:43:00.27 2.29 2.39 B0.5 IV pe 29512 ✓ Y (Yang et al. 1988) SPB 1, 21
κ CMa 52982382 06:49:50.46 -32:30:30.52 3.68 3.89 B1.5 Ve 22022 Y (Rivinius et al. 2003) SPB 21
ω CMa 65903024 07:14:48.65 -26:46:21.61 3.64 3.82 B2.5 V e 8022 Y (Štefl et al. 2003) SPB 21
omi Vel 93549165 08:40:17.59 -52:55:18.80 3.44 3.63 B3/5(V) 40 ? Y (Aerts et al. 1999) SPB 1, 2
δ Cen 333670784 12:08:21.50 -50:43:20.74 2.39 2.52 B2 V ne 22022 ? Y (Rivinius et al. 2003) SPB 1, 14, 21
η UMa 219033887 13:47:32.44 49:18:47.76 1.67 1.86 B3 V 15012 N (Smith 2006) SPB
μ Cen 243647020 13:49:36.99 -42:28:25.43 3.27 3.43 B2 V npe 15522 ? Y (Rivinius et al. 2001) SPB 1, 14, 21
η Cen 128116539 14:35:30.42 -42:09:28.17 2.12 2.31 B2 V e 350 Y (Janot-Pacheco et al. 1999) SPB 23
ζ Oph 152859121† 16:37:09.54 -10:34:01.53 2.58 2.56 O9.2 IV nn 320 Y (Kambe et al. 1997) − 2, 21
α Ara 412724758 17:31:50.49 -49:52:34.12 2.78 2.95 B2 V ne 25022 Y (Rivinius et al. 2003) SPB 21
α Tel 90482097 18:26:58.42 -45:58:06.45 3.30 3.46 B3 IV 35 Y (Telting et al. 2006) SPB 1
Priority 3: stars dominated by SLF in TESS photometry
ϵ Cas 10510382 01:54:23.73 63:40:12.37 3.22 3.37 B3 Vp sh 3012 SLF 17
ζ Per 94367286 03:54:07.92 31:53:01.08 2.97 2.85 B1 Ib 4012 ? ≃3 Y (Simón-Díaz et al. 2010) SLF 1
π4 Ori 452810783 04:51:12.36 05:36:18.37 3.50 3.68 B2 III+B2 IV 3512 ✓ Y (Telting et al. 2006) SLF 1, 17
γ Ori 365572007 05:25:07.86 06:20:58.93 1.42 1.64 B2 V 55 N (Telting et al. 2006) SLF 4, 24
ζ Ori B 712837934 05:40:45.57 -01:56:35.59 3.50 3.70 O9.5 II-III (n) ✓ SLF 1, 25
ι Ori 427395774 05:35:25.98 -05:54:35.64 2.53 2.77 O9 III var 1303 ✓ SLF 1, 4, 26
ϵ Ori 427451176 05:36:12.81 -01:12:06.91 1.51 1.69 B0 Ia 6512 ≃13 Y (Simón-Díaz et al. 2010) SLF 4, 27
ζ Ori 11360636 05:40:45.53 -01:56:33.26 1.59 1.79 O9.7 Ib + B0 III ✓ SLF
ζ Ori A 11360636 05:40:45.53 -01:56:33.26 1.77 1.88 O9.2 Ib varNwk 1403 ✓ ≃12 Y (Simón-Díaz et al. 2010) SLF 25
κ Ori 66651575 05:47:45.39 -09:40:10.58 1.88 2.06 B0.5 Ia 6512 ≃10 Y (Simón-Díaz et al. 2010) SLF 4, 28
ϵ CMa 63198307 06:58:37.55 -28:58:19.51 1.29 1.50 B1.5 II 2512 ? SLF 1, 4, 28
omi2 CMa 80466973 07:03:01.47 -23:49:59.85 2.94 3.02 B3 Ia 3512 SLF 2, 4
χ Car 269407223 07:56:46.72 -52:58:56.39 3.27 3.43 B3 IV 953 N (Leone & Catanzaro 1998) SLF 1, 29
κ Vel 387106852 09:22:06.82 -55:00:38.40 2.32 2.47 B2 IV 5012 ✓ SLF 1, 10, 14, 15
ι Lup 242497929 14:19:24.22 -46:03:29.14 3.36 3.53 B2.5 IV 3703 SLF 30
τ Sco 205175750 16:35:52.95 -28:12:57.66 2.56 2.81 B0.2 V 012 N (Telting et al. 2006) SLF
γ Ara 325709821 17:25:23.66 -56:22:39.81 3.21 3.34 B1 Ib 2803 ? Y (Baade 1983) SLF 1
θ Ara 364875523 18:06:37.87 -50:05:29.31 3.58 3.66 B2 Ib 1203 Y (Baade 1983) SLF
α Pav 219974785 20:25:38.86 -56:44:06.32 1.79 1.92 B2 IV 40 ✓ Y (Telting et al. 2006) SLF 1, 15
No evidence of β Cep pulsations in the literature or in TESS light curves (but other variability may be present)
omi Per 101255849 03:44:19.13 32:17:17.69 3.88 3.83 B1 III 9012 ✓ N (Telting et al. 2006) rot/bin 1, 23, 31
π5 Ori 262435444 04:54:15.10 02:26:26.41 3.54 3.73 B2 III 9012 ✓ rot/bin 1, 23, 31
η Aur 122385146‡ 05:06:30.89 41:14:04.11 3.00 3.18 B3 V 9512 − 17, 32
δ Ori 50743469 05:32:00.40 -00:17:56.74 2.02 2.41 B0 III + O9 V 13012 ✓ Y (Kholtygin et al. 2007) EB+SLF 1, 4
ζ Tau 19704573† 05:37:38.69 21:08:33.16 2.84 3.03 B1 IV e sh 12512 ✓ Y (Rivinius et al. 2003) − 1, 21
σ Ori 11286198 05:38:44.77 -02:36:00.28 3.58 3.79 O9.5 V 9512 ✓ N (Telting et al. 2006) EB 4, 33
ϵ Car B 342884451‡ 08:22:30.88 -59:30:34.40 3.93 3.85 B2 V p −
i Car 357639411‡ 09:11:16.72 -62:19:01.13 3.77 3.94 B3 V 203 N (Telting et al. 2006) − 17
ρ Leo 392834850† 10:32:48.67 09:18:23.71 3.72 3.87 B1 Iab 5012 ? N (Aerts et al. 2018) − 1
θ Car 390442076 10:42:57.40 -64:23:40.02 2.54 2.76 B0 V p 15012 ✓ N (Telting et al. 2006) SLF 1, 34
ζ Cen 113350416 13:55:32.39 -47:17:18.15 2.33 2.55 B2.5 IV 2203 ✓ rot/bin 1, 15
γ Lup 171611328 15:35:08.45 -41:10:00.32 2.59 2.77 B2 IV 27018 ✓ rot/bin 1, 2, 15, 19
τ Lib 147883533 15:38:39.37 -29:46:39.90 3.48 3.64 B2.5 V 135 ✓ N (Telting et al. 2006) rot/bin 1, 30
π Sco 66744681† 15:58:51.11 -26:06:50.79 2.71 2.91 B1 V + B2: V: 100 ✓ ? (Telting et al. 2006) EB 1, 23
μ1 Sco 338104678 16:51:52.22 -38:02:50.64 2.82 2.98 B1 V + B 2403 ✓ EB 1, 23
μ2 Sco 338105219 16:52:20.15 -38:01:03.13 3.34 3.54 B2 IV 50 Y (Telting et al. 2006) EB 11
σ Sgr 91093307† 18:55:15.93 -26:17:48.21 1.92 2.07 B2 V 165 N (Telting et al. 2006) −

Notes. Columns are star name, TESS input catalogue (TIC) ID number, coordinates, B and V magnitudes, spectral type as listed by SIMBAD and projected rotation velocity, v sin i (if known). In the ‘bin’ column, a ‘✓’ symbol corresponds to if a binary or higher-order multiple system orbital solution has been determined, whereas a ‘?’ symbol means evidence for binarity has been found. The approximate frequency range of known β Cep pulsation modes and the corresponding radial velocities measured using previous LPV studies are also provided if available. A reference is provided for a dedicated search for LPVs caused by pulsations, which if successful is indicated by ‘Y’, unsuccessful by ‘N’ and inconclusive by ‘?’. We also provide a variability classification based on our analysis of TESS light curves. ( † ) Not observed by TESS to date, ( ‡ ) Problematic light curve extraction and/or dominated by systematics, (1) Evidence of multiplicity from Eggleton & Tokovinin (2008), (2) Stars known to have β Cep or SPB pulsations from Hipparcos photometry by Lefèvre et al. (2009), (3) Projected rotational velocity from Hoffleit & Jaschek (1991), (4) Detection of photometric variability using TESS data by Burssens et al. (2020), (5) Interferometric masses determined by Herbison-Evans et al. (1971), (6) Detection of photometric variability by Shobbrook (1972), (7) Interferometric masses determined by Davis et al. (2005) and Ausseloos et al. (2006), (8) Interferometric masses determined by North et al. (2007), (9) Interferometric masses determined by Tango et al. (2006), (10) Detection of photometric variability by Daszyńska-Daszkiewicz et al. (2017), (11) Classified as a constant photometric star by Handler & Schwarzenberg-Czerny (2013), (12) Projected rotational velocity from Abt et al. (2002), (13) Known magnetic SPB star Neiner et al. (2003), Briquet et al. (2007), (14) Detection of photometric variability by Jakate (1978), (15) Non-detection of photometric variability by Jerzykiewicz & Sterken (1977), (16) Identified as an SPB star from Hipparcos photometry by Aerts et al. (1999), (17) Identified as candidate pulsating star using Hipparcos photometry by Koen & Eyer (2002), (18) Projected rotational velocity from Wolff et al. (2007), (19) Non-detection of photometric variability by Jakate (1979), (20) Non-detection of photometric variability by Shobbrook (1978), (21) (Pulsating) Be star discussed in review paper by Rivinius et al. (2003), (22) Projected rotational velocity from Rivinius et al. (2003), (23) Identified as (possible) eclipsing binary using Hipparcos photometry by Lefèvre et al. (2009), (24) Detection of photometric variability by Krisciunas (1994), (25) Detection of photometric variability by Buysschaert et al. (2017), (26) Detection of photometric variability using BRITE data by Pablo et al. (2017), (27) Detection of LPV also by Prinja et al. (2004), (28) Spectroscopic modelling performed by Haucke et al. (2018), (29) Detection of photometric variability by Elst (1979), (30) Non-detection of photometric variability by Sterken & Jerzykiewicz (1983), (31) Detection of photometric variability by Waelkens & Rufener (1983), (32) Detection of photometric variability using BRITE data by Strassmeier et al. (2020), (33) Spectroscopic modelling performed by Simón-Díaz et al. (2015), (34) Identified as candidate pulsating star using Hipparcos photometry by Adelman (2001).

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