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List of stars in Pegasus
List of stars in Pegasus
List of stars in Pegasus
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This is the list of notable stars in the constellation Pegasus, sorted by decreasing brightness.

Name B F G. Var HD HIP RA Dec vis.
mag. 		abs.
mag. 		Dist. (ly) Sp. class Notes
ε Peg ε 8 11 206778 107315 21h 44m 11.14s +09° 52′ 30.0″ 2.38 −4.19 672 K2Ibvar Enif, Enf, Enir, Al Anf, Fom, Fum al Faras, Os Pegasi
β Peg β 53 217906 113881 23h 03m 46.33s +28° 04′ 56.8″ 2.44 −1.49 199 M2II-IIIvar Scheat, Sheat, Seat Alpheras, Menkib
α Peg α 54 218045 113963 23h 04m 45.62s +15° 12′ 19.3″ 2.49 −0.67 140 B9.5III Markab, Marchab, Menkib al Faras, Matn al Faras
γ Peg γ 88 886 1067 00h 13m 14.15s +15° 11′ 01.0″ 2.83 −2.22 333 B2IV Algenib; β Cep variable
η Peg η 44 215182 112158 22h 43m 00.13s +30° 13′ 16.7″ 2.93 −1.16 215 G2II-III.. Matar, Sad al Matar
ζ Peg ζ 42 214923 112029 22h 41m 27.67s +10° 49′ 53.0″ 3.41 −0.62 208 B8.5V Homam, Homan, Humam, Al Hammam
μ Peg μ 48 216131 112748 22h 50m 00.10s +24° 36′ 06.1″ 3.51 0.74 117 M2III Sadalbari, Sad al Bari, Sad al Nazi
θ Peg θ 26 25 210418 109427 22h 10m 11.82s +06° 11′ 52.0″ 3.52 1.16 97 A2V Baham, Biham, Sad al Baham
ι Peg ι 24 210027 109176 22h 07m 00.47s +25° 20′ 42.2″ 3.77 3.42 38 F5V
λ Peg λ 47 215665 112440 22h 46m 31.84s +23° 33′ 56.4″ 3.97 −1.45 395 G8II-III Sadalpheretz
1 Peg 1 203504 105502 21h 22m 05.13s +19° 48′ 15.7″ 4.08 0.71 154 K1III
κ Peg κ 10 206901 107354 21h 44m 38.70s +25° 38′ 42.0″ 4.14 1.40 115 F5IV Jih
ξ Peg ξ 46 215648 112447 22h 46m 41.44s +12° 10′ 26.7″ 4.20 3.15 53 F7V
π Peg π 29 210459 109410 22h 09m 59.25s +33° 10′ 41.8″ 4.28 −0.16 252 F5III Woo
9 Peg 9 206859 107348 21h 44m 30.69s +17° 21′ 00.2″ 4.34 −2.87 901 G5Ib
υ Peg υ 68 220657 115623 23h 25m 22.66s +23° 24′ 14.4″ 4.42 0.79 173 F8IV Alkarab
2 Peg 2 204724 106140 21h 29m 56.88s +23° 38′ 19.8″ 4.52 −1.14 442 M1III
55 Peg 55 42 218329 114144 23h 07m 00.26s +09° 24′ 34.3″ 4.54 −0.43 322 M2III
70 Peg 70 221115 115919 23h 29m 09.26s +12° 45′ 37.8″ 4.54 0.86 178 G8III
τ Peg τ 62 220061 115250 23h 20m 38.22s +23° 44′ 25.3″ 4.58 1.03 167 A5V Salm, Kerb, El Khereb, Markab; δ Sct variable
ψ Peg ψ 84 224427 118131 23h 57m 45.55s +25° 08′ 29.3″ 4.63 −0.98 432 M3III
56 Peg 56 218356 114155 23h 07m 06.74s +25° 28′ 06.0″ 4.76 −1.32 537 K0IIp
32 Peg 32 212097 110371 22h 21m 19.33s +28° 19′ 49.9″ 4.78 −1.57 607 B9III
35 Peg 35 33 212943 110882 22h 27m 51.48s +04° 41′ 47.1″ 4.78 1.33 160 K0III
χ Peg χ 89 1013 1168 00h 14m 36.11s +20° 12′ 24.1″ 4.79 −0.21 326 M2III
ο Peg ο 43 214994 112051 22h 41m 45.41s +29° 18′ 27.7″ 4.80 −0.05 305 A1IV
31 Peg 31 IN 212076 110386 22h 21m 31.07s +12° 12′ 18.6″ 4.82 −2.55 970 B2IV-V IN Peg; Be star
ν Peg ν 22 20 209747 109068 22h 05m 40.69s +05° 03′ 29.8″ 4.86 0.32 263 K4III
ρ Peg ρ 50 40 216735 113186 22h 55m 13.62s +08° 48′ 57.9″ 4.91 0.22 282 A1V
78 Peg 78 222842 117073 23h 43m 59.44s +29° 21′ 41.6″ 4.93 0.65 234 K0III
72 Peg 72 221673 116310 23h 33m 57.15s +31° 19′ 31.2″ 4.97 −1.16 548 K4III
57 Peg 57 43 GZ 218634 114347 23h 09m 31.45s +08° 40′ 37.8″ 5.05 −1.79 762 M4Sv GZ Peg
φ Peg φ 81 223768 117718 23h 52m 29.29s +19° 07′ 13.3″ 5.06 −0.58 437 M2III
14 Peg 14 207650 107763 21h 49m 50.68s +30° 10′ 27.4″ 5.07 0.23 302 A1Vs
16 Peg 16 OQ 208057 108022 21h 53m 03.76s +25° 55′ 30.5″ 5.09 −0.89 512 B3V OQ Peg; Be star
66 Peg 66 220363 115444 23h 23m 04.56s +12° 18′ 50.2″ 5.09 0.06 330 K3III
77 Peg 77 48 222764 117020 23h 43m 22.36s +10° 19′ 53.4″ 5.09 −1.91 817 M2III
59 Peg 59 45 218918 114520 23h 11m 44.19s +08° 43′ 12.5″ 5.15 0.70 253 A5Vn
σ Peg σ 49 39 216385 112935 22h 52m 23.77s +09° 50′ 08.0″ 5.16 3.02 88 F7IV
12 Peg 12 207089 107472 21h 46m 04.36s +22° 56′ 56.0″ 5.29 −2.41 1128 K0Ib
7 Peg 7 9 206487 107151 21h 42m 15.44s +05° 40′ 48.5″ 5.30 −0.72 522 M2III
82 Peg 82 HT 223781 117730 23h 52m 37.12s +10° 56′ 50.4″ 5.30 1.49 188 A4Vn HT Peg;δ Sct variable
71 Peg 71 HW 221615 116264 23h 33m 28.09s +22° 29′ 55.7″ 5.33 −0.90 575 M5IIIa HW Peg
13 Peg 13 6 V373 207652 107788 21h 50m 08.64s +17° 17′ 09.4″ 5.34 2.72 109 F2III-IV V373 Peg
210889 109654 22h 12m 47.81s +34° 36′ 17.0″ 5.34 0.87 256 K2III
64 Peg 64 220222 115355 23h 21m 54.93s +31° 48′ 44.9″ 5.35 −1.69 834 B6III
30 Peg 30 30 211924 110298 22h 20m 27.56s +05° 47′ 22.2″ 5.37 −1.88 918 B5IV
58 Peg 58 44 218700 114389 23h 10m 01.47s +09° 49′ 19.6″ 5.39 −1.00 619 B9III
51 Peg 51 217014 113357 22h 57m 27.85s +20° 46′ 07.3″ 5.45 4.52 50 G5V Helvetios,[1] has a planet b
5 Peg 5 205852 106787 21h 37m 45.37s +19° 19′ 06.9″ 5.46 0.49 321 F1IV
75 Peg 75 KS 222133 116611 23h 37m 56.77s +18° 24′ 02.2″ 5.49 1.17 239 A1Vn KS Peg; β Lyr variable
37 Peg 37 35 213235 111062 22h 29m 57.95s +04° 25′ 55.4″ 5.51 1.90 172 F5IVs
15 Peg 15 207978 107975 21h 52m 29.96s +28° 47′ 37.3″ 5.52 3.31 90 F6IVwvar
17 Peg 17 208565 108339 21h 56m 56.39s +12° 04′ 35.5″ 5.54 −0.11 440 A2Vnn
86 Peg 86 87 476 00h 05m 41.94s +13° 23′ 46.6″ 5.55 0.26 373 G5III
67 Peg 67 220599 115591 23h 24m 50.82s +32° 23′ 05.5″ 5.56 −0.40 506 B9III
87 Peg 87 448 729 00h 09m 02.34s +18° 12′ 43.3″ 5.57 0.81 292 G9III
34 Vul (34) 203344 105411 21h 21m 04.24s +23° 51′ 22.5″ 5.58 0.91 280 K1III
π1 Peg π1 27 210354 109352 22h 09m 13.68s +33° 10′ 21.0″ 5.58 0.89 283 G6III:
63 Peg 63 220088 115271 23h 20m 49.50s +30° 24′ 54.3″ 5.58 −0.05 435 M0III
36 Peg 36 34 213119 110986 22h 29m 07.95s +09° 07′ 44.7″ 5.60 −0.65 579 K5III
20 Peg 20 209166 108693 22h 01m 05.32s +13° 07′ 11.9″ 5.61 1.39 228 F4III
11 Peg 11 12 207203 107575 21h 47m 13.96s +02° 41′ 10.1″ 5.63 −0.15 467 A1V 27 Aquarii
73 Peg 73 221758 116355 23h 34m 38.21s +33° 29′ 50.2″ 5.63 0.77 305 K0III:
38 Peg 38 213323 111068 22h 30m 01.79s +32° 34′ 21.6″ 5.64 0.16 407 B9.5V
19 Peg 19 18 209167 108699 22h 01m 09.24s +08° 15′ 25.8″ 5.65 −0.71 609 K5III
4 Peg 4 7 205924 106856 21h 38m 31.87s +05° 46′ 18.0″ 5.66 2.02 174 A9IV-Vn
218792 114449 23h 10m 42.62s +17° 35′ 40.0″ 5.68 −0.27 505 K4III
208108 108060 21h 53m 37.37s +19° 40′ 06.2″ 5.69 1.45 230 A0Vs
23 Peg 23 209833 109056 22h 05m 34.65s +28° 57′ 50.4″ 5.69 0.84 304 B9Vn
214850 111974 22h 40m 52.52s +14° 32′ 55.9″ 5.72 3.14 107 G3V+...
210074 109209 22h 07m 28.52s +19° 28′ 31.6″ 5.74 1.81 199 F2V:
209761 109023 22h 05m 11.32s +26° 40′ 25.0″ 5.75 0.32 397 K2III
34 Peg 34 32 212754 110785 22h 26m 37.22s +04° 23′ 37.1″ 5.76 2.78 129 F7V
52 Peg 52 217232 113503 22h 59m 11.80s +11° 43′ 44.2″ 5.76 1.20 266 A7V
NZ Peg NZ 206043 106897 21h 39m 01.11s +20° 15′ 55.6″ 5.77 2.81 127 F2V γ Dor variable
80 Peg 80 51 HH 223637 117628 23h 51m 21.25s +09° 18′ 48.6″ 5.77 −1.20 807 M3III HH Peg
207840 107887 21h 51m 34.24s +19° 49′ 35.9″ 5.78 −0.49 584 B8III
210502 109471 22h 10m 37.46s +11° 37′ 28.8″ 5.78 −0.63 625 M1III
25 Peg 25 210129 109240 22h 07m 50.33s +21° 42′ 11.1″ 5.79 −0.86 698 B7Vn
213179 110992 22h 29m 10.21s +26° 45′ 47.6″ 5.79 −1.85 1098 K2II
85 Peg 85 224930 171 00h 02m 09.65s +27° 05′ 04.2″ 5.80 5.33 40 G3V
21 Peg 21 209459 108875 22h 03m 19.02s +11° 23′ 11.6″ 5.83 −0.27 541 B9.5V
NV Peg NV 204585 106062 21h 28m 59.76s +22° 10′ 45.9″ 5.84 −0.49 603 M4III
40 Peg 40 214567 111810 22h 38m 52.62s +19° 31′ 21.0″ 5.84 0.50 381 G8II
219139 114641 23h 13m 26.51s +11° 03′ 54.1″ 5.85 0.79 335 G5III:
IM Peg IM 216489 112997 22h 53m 02.28s +16° 50′ 28.5″ 5.86 0.93 316 K1III SB RS CVn variable
211006 109730 22h 13m 38.65s +28° 36′ 28.9″ 5.87 1.45 249 K2III
214995 112067 22h 41m 57.40s +14° 30′ 59.2″ 5.92 1.36 267 K0III:
HD 210702 210702 109577 22h 11m 51.33s +16° 02′ 26.1″ 5.93 2.19 182 K1III has a planet (b)
79 Peg 79 223461 117500 23h 49m 39.35s +28° 50′ 32.4″ 5.95 1.39 267 A2m
HN Peg HN 206860 107350 21h 44m 31.19s +14° 46′ 20.0″ 5.96 4.64 60 G0V BY Draconis variable
210762 109602 22h 12m 08.09s +24° 57′ 02.3″ 5.97 −3.88 3047 K0
HR 8799 V342 218396 114189 23h 07m 28.65s +21° 08′ 03.7″ 5.97 2.96 130 A5V V342 Peg; has four planets (b, c, d & e)
69 Peg 69 HV 220933 115806 23h 27m 40.37s +25° 10′ 02.5″ 5.99 0.73 367 A0MNp... HV Peg; α² CVn variable
47 G. Peg 47 222377 116768 23h 39m 54.99s +09° 40′ 38.4″ 5.99 2.16 190 A2m
18 Peg 18 17 209008 108612 22h 00m 07.92s +06° 43′ 02.8″ 6.00 −1.58 1069 B3III
212988 110873 22h 27m 46.22s +31° 50′ 23.9″ 6.00 −1.29 937 K2
206540 107173 21h 42m 32.95s +10° 49′ 27.6″ 6.06 −0.59 697 B5IV
IK Peg IK 204188 105860 21h 26m 26.61s +19° 22′ 32.2″ 6.08 2.76 150 A8m
210210 109276 22h 08m 17.26s +25° 32′ 37.0″ 6.08 1.40 281 F1IV
204862 106243 21h 31m 09.62s +12° 08′ 15.0″ 6.10 0.57 417 B9.5V
221662 116307 23h 33m 55.50s +20° 50′ 27.5″ 6.10 −1.42 1042 M3III
214200 111567 22h 36m 07.90s +35° 34′ 39.5″ 6.11 0.57 417 K0
V343 Peg V343 218395 114187 23h 07m 27.74s +32° 49′ 31.3″ 6.13 0.24 491 A3
23 Psc (23) 223755 117710 23h 52m 23.42s +21° 40′ 16.0″ 6.13 0.01 547 M2III
13 G. Peg 13 208110 108090 21h 53m 57.72s +06° 51′ 53.2″ 6.14 0.63 413 G0IIIs
218235 114081 23h 06m 18.00s +18° 31′ 03.4″ 6.16 2.98 141 F6Vs
206027 106872 21h 38m 45.16s +25° 29′ 55.7″ 6.18 0.65 416 G9III
V372 Peg V372 207223 107558 21h 47m 04.70s +17° 11′ 38.7″ 6.18 2.67 164 F3V
210460 109439 22h 10m 18.96s +19° 36′ 59.6″ 6.18 2.46 181 G0V
31 G. Peg 31 211976 110341 22h 20m 55.77s +08° 11′ 12.1″ 6.18 3.67 104 F6V
224303 118048 23h 56m 41.52s +22° 38′ 53.2″ 6.18 −0.15 603 M2III
3 Peg 3 6 205811 106783 21h 37m 43.61s +06° 37′ 06.2″ 6.19 1.71 257 A2V
60 Peg 60 218935 114526 23h 11m 49.31s +26° 50′ 51.3″ 6.19 1.84 242 G8III-IV
33 Peg 33 212395 110548 22h 23m 39.36s +20° 50′ 53.8″ 6.20 3.55 111 F7V
29 G. Peg 29 211287 109939 22h 15m 59.81s +08° 32′ 58.6″ 6.21 0.79 395 A1Vn
205541 106605 21h 35m 27.03s +24° 27′ 07.9″ 6.22 −0.41 689 A4V
417 716 00h 08m 52.07s +25° 27′ 46.3″ 6.24 0.69 419 K0III
225276 399 00h 04m 55.93s +26° 38′ 55.7″ 6.25 −0.11 610 K4IIIb
1048 1193 00h 14m 55.87s +22° 17′ 03.3″ 6.25 1.06 355 A1p
205539 106595 21h 35m 19.02s +28° 11′ 51.7″ 6.25 1.97 235 F0IV
212670 110696 22h 25m 40.68s +18° 26′ 39.3″ 6.26 0.05 568 K0
74 Peg 74 222098 116592 23h 37m 39.66s +16° 49′ 31.8″ 6.26 1.02 363 A1V
202128 104771 21h 13m 28.77s +15° 58′ 56.8″ 6.27 1.51 292 A7Vn
207563 107734 21h 49m 26.87s +20° 27′ 44.8″ 6.27 −2.49 1842 B2V
HO Peg HO 207932 107956 21h 52m 18.17s +21° 16′ 23.2″ 6.27 −1.69 1273 M8III
45 Peg 45 215510 112358 22h 45m 28.19s +19° 21′ 59.1″ 6.27 1.11 351 G6III:
207134 107502 21h 46m 23.84s +25° 33′ 48.1″ 6.28 0.98 374 K3III:
65 Peg 65 220318 115407 23h 22m 40.50s +20° 49′ 43.5″ 6.28 0.41 487 B9.5V
210594 109493 22h 10m 51.70s +30° 33′ 11.0″ 6.30 0.76 418 A8IV
214298 111649 22h 37m 04.86s +12° 34′ 36.8″ 6.30 −0.74 836 K5
76 Peg 76 222683 116972 23h 42m 43.81s +16° 20′ 08.5″ 6.30 0.82 406 K0
OY Peg OY 210090 109212 22h 07m 29.95s +18° 00′ 02.8″ 6.31 −1.00 945 M1
219927 115148 23h 19m 27.40s +34° 47′ 35.5″ 6.32 −0.33 697 B8III
GX Peg GX 213534 111191 22h 31m 34.37s +29° 32′ 34.2″ 6.33 0.85 408 A5m δ Sct variable
41 Peg 41 214698 111884 22h 39m 47.01s +19° 40′ 52.1″ 6.33 −0.12 635 A2V
219110 114607 23h 13m 04.01s +29° 26′ 29.8″ 6.34 0.78 422 G8III
213644 111296 22h 32m 46.90s +15° 51′ 47.6″ 6.35 −0.30 698 K0
208202 108119 21h 54m 17.44s +19° 43′ 05.3″ 6.36 1.12 364 K0III+...
209288 108766 22h 02m 01.37s +10° 58′ 25.7″ 6.36 −1.71 1342 B5IIIn
209693 108969 22h 04m 34.51s +32° 56′ 30.3″ 6.36 −0.99 962 G5Ia
210461 109445 22h 10m 22.02s +14° 37′ 47.7″ 6.36 0.79 424 K0III
214979 112032 22h 41m 31.28s +30° 57′ 57.1″ 6.36 −0.67 832 K5
219310 114742 23h 14m 36.42s +24° 06′ 10.4″ 6.36 0.41 504 K2III
215549 112368 22h 45m 34.64s +30° 26′ 36.3″ 6.37 2.59 186 K1III-IV
209709 109009 22h 05m 03.47s +14° 48′ 57.4″ 6.38 0.41 509 M2.5III:
211432 109977 22h 16m 29.66s +27° 48′ 14.5″ 6.38 0.94 399 G9III
220288 115389 23h 22m 28.58s +25° 55′ 06.6″ 6.38 −1.22 1079 K3III
2 G. Peg 2 204445 106021 21h 28m 24.83s +08° 11′ 44.6″ 6.39 −0.83 906 M1
HD 208527 208527 108296 21h 56m 23.98s +21° 14′ 23.4″ 6.39 −1.34 1148 M1III[2]
HR Peg HR 216672 113131 22h 54m 35.62s +16° 56′ 30.7″ 6.39 −0.97 967 S5,1
3 G. Peg 3 204603 106103 21h 29m 34.49s +06° 34′ 53.0″ 6.41 −0.60 823 K0
219291 114725 23h 14m 21.72s +29° 46′ 18.7″ 6.41 1.15 368 F6IVw
V354 Peg V354 221394 116119 23h 31m 43.05s +28° 24′ 12.7″ 6.41 0.57 481 A1p Sr(CrEu) α² CVn variable
221493 116187 23h 32m 29.03s +23° 50′ 37.2″ 6.41 −0.23 694 K5
204560 106064 21h 28m 59.92s +17° 54′ 21.3″ 6.42 0.31 544 K5
214203 111601 22h 36m 36.34s +11° 41′ 47.8″ 6.42 1.11 376 A1III
224758 34 00h 00m 23.87s +26° 55′ 05.7″ 6.43 1.95 256 F7.5IV-V
205011 106306 21h 31m 50.15s +23° 50′ 42.6″ 6.43 0.43 517 G8Ib
206793 107297 21h 43m 58.12s +22° 48′ 55.4″ 6.43 0.16 585 K2
39 Peg 39 V643 213617 111278 22h 32m 35.38s +20° 13′ 47.8″ 6.43 2.81 172 F1V V643 Pegasi; γ Dor variable
41 G. Peg 41 217166 113445 22h 58m 34.85s +09° 21′ 26.0″ 6.43 3.98 101 G2V+...
218101 113994 23h 05m 06.40s +16° 33′ 48.1″ 6.43 3.40 132 G8IV
218261 114096 23h 06m 31.71s +19° 54′ 39.0″ 6.44 4.18 92 F7V
221905 116465 23h 35m 55.94s +24° 33′ 39.6″ 6.44 −1.49 1254 M1III
205420 106527 21h 34m 33.97s +22° 45′ 16.7″ 6.45 2.25 226 F7V
28 Peg 28 210516 109458 22h 10m 30.18s +20° 58′ 40.8″ 6.45 −0.09 663 A3III
221113 115915 23h 29m 05.70s +23° 02′ 53.8″ 6.45 0.44 520 G9III
V363 Peg V363 224186 117986 23h 55m 54.63s +15° 13′ 49.1″ 6.45 −0.35 746 M3
209149 108632 22h 00m 26.71s +33° 00′ 20.8″ 6.46 2.35 217 F5III
PT Peg PT 212047 110346 22h 21m 00.05s +26° 56′ 06.6″ 6.46 −0.47 793 M4III
225292 410 00h 05m 01.13s +27° 40′ 29.3″ 6.47 0.88 427 G8II
434 728 00h 09m 00.16s +28° 14′ 51.2″ 6.47 1.16 377 A4Vm
205422 106550 21h 34m 45.89s +18° 19′ 44.0″ 6.47 −0.30 736 K2
10 G. Peg 10 206689 107271 21h 43m 39.79s +07° 31′ 43.7″ 6.47 0.89 426 K0
219196 114686 23h 13m 59.34s +19° 38′ 02.1″ 6.47 −0.47 795 K2
213025 110907 22h 28m 11.15s +27° 01′ 08.0″ 6.48 0.63 482 G8III
205603 106643 21h 36m 05.09s +15° 04′ 56.0″ 6.50 0.82 447 G8II
HD 208897 208897 108513 21h 58m 59.64s +19° 01′ 13.4″ 6.50 2.48 208 K0 has a planet (b)
210890 109691 22h 13m 10.01s +18° 16′ 47.6″ 6.50 −0.31 751 K2
211076 109788 22h 14m 18.45s +17° 11′ 22.4″ 6.50 1.07 398 K4III
61 Peg 61 219477 114844 23h 15m 46.28s +28° 14′ 52.5″ 6.51 −0.83 956 G5III
MT Peg 217813 113829 23h 03m 04.98s +20° 55′ 06.9″ 6.62 4.65 79 G1V BY Dra variable
HD 220773 220773 115697 23h 26m 27.0s +08° 38′ 38″ 7.09 160 F9 has a planet (b)
V376 Peg V376 209458 108859 22h 03m 10.77s +18° 53′ 03.6″ 7.65 4.28 154 F8-G0V has the transiting planet HD 209458 b (Osiris)
HD 219828 219828 115100 23h 18m 46.73s +18° 38′ 44.6″ 8.02 3.47 264 G0IV has two planets (b & c)
HD 214823 214823 111928 22h 40m 19.9s +31° 47′ 15″ 8.08 G0V has a planet (b)
HD 220197 220197 115359 23h 21m 58.0s +16° 37′ 57″ 9.00 210 F8V has a planet (b)
HIP 109600 109600 22h 12m 06.0s +29° 03′ 57″ 9.16 191 G5 has a planet (b)
BD+14°4559 104780 21h 13m 35.99s +14° 41′ 21.8″ 9.66 6.17 163 K2V Solaris,[3] has a planet (b)
HAT-P-8 22h 52m 09.86s +35° 26′ 49.6″ 10.17 3.36 750 has a transiting planet (b)
WASP-134 21h 50m 17.0s +04° 11′ 40″ 11.3 636 G4 has two transiting planets (b and c)
WASP-21 23h 09m 58.25s +18° 23′ 45.9″ 11.55 4.75 750 G3V Tangra,[4] has a transiting planet (b)
WASP-52 23h 13m 59.0s +08° 45′ 41″ 12 457 K2V Anadolu,[5] has a transiting planet (b)
WASP-60 23h 15m 58s +31° 27′ 46″ 12.18 1305 G1V Morava,[6] has a transiting planet (b)
WASP-10 23h 15m 58s +31° 27′ 46″ 12.7 7.9 290 K0V has a transiting planet (b)
WASP-102 22h 25m 51.4s +15° 51′ 24″ 12.73 G0 has a transiting planet (b)
WASP-114 21h 50m 40.0s +10° 27′ 47″ 12.74 1500 G0 has a transiting planet (b)
WASP-59 23h 18m 30.0s +24° 53′ 21″ 13 408 K5V has a transiting planet (b)
V391 Pegasi V391 22h 04m 12.2s +26° 25′ 08″ 14.57 3.84 4561 sdB has a planet (b)
Table legend:

See also

[edit]

References

[edit]
Revisions and contributorsEdit on WikipediaRead on Wikipedia

List of stars in Pegasus

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The list of stars in Pegasus is a catalog of the stellar objects lying within the boundaries of the constellation , one of the 88 modern constellations officially delineated by the (IAU) in 1930. Representing the mythical winged horse from , spans 1,121 square degrees across the northern celestial hemisphere, ranking as the seventh-largest constellation and visible primarily during autumn evenings for observers in the at latitudes between +90° and -60°. The constellation encompasses hundreds of stars of varying brightness, from naked-eye visible ones to fainter objects requiring telescopes, with its boundaries encompassing approximately 177 confirmed stellar members of 6.5 or brighter. Prominent among these stars is the asterism known as the Great Square of Pegasus, formed by three of Pegasus's brightest stars—Markab (α Pegasi, magnitude 2.48, a blue-white giant 133 light-years distant), Scheat (β Pegasi, magnitude 2.42, a red giant and semi-regular variable 196 light-years away), and Algenib (γ Pegasi, magnitude 2.84, a blue subgiant and pulsating variable 390 light-years distant)—along with Alpheratz (α Andromedae, magnitude 2.07, from the neighboring constellation Andromeda). The brightest star in Pegasus itself is Enif (ε Pegasi, magnitude 2.40, an orange supergiant approximately 690 light-years from Earth), located at the "nose" of the celestial horse and notable for its evolved status as one of the largest known stars in the sky. Other key stars include Matar (η Pegasi, magnitude 2.95, a yellow giant 214 light-years away) and 51 Pegasi (magnitude 5.49, a Sun-like star 50 light-years distant, famous as the host of 51 Pegasi b, the first exoplanet confirmed around a main-sequence star in 1995). This list highlights not only the brightest and Bayer-designated stars but also variables, double stars, and those hosting , with at least 19 confirmed exoplanet-hosting systems within 's boundaries as of 2023. Recent discoveries, such as the rocky BD+05 4868 Ab confirmed in 2025, continue to expand this count. The constellation's stars vary in spectral types from hot blue giants to cool red supergiants, reflecting a diverse evolutionary history, and serve as important references for locating deep-sky objects like the Messier 15. Overall, the stars of provide a rich field for astronomical study, blending mythological heritage with modern discoveries in stellar and .

Overview

Constellation Background

Pegasus is a large northern constellation that occupies an area of 1,121 square degrees in the sky, ranking seventh in size among modern constellations. It lies in the fourth quadrant of the (NQ4) and is bordered by Andromeda, Aquarius, , , Lacerta, Pisces, and . The constellation's boundaries, as defined by the (IAU), follow lines of and established in 1930 following the IAU's in 1928. These boundaries encompass a range from 21h 12.6m to 00h 14.6m and a range from +2.33° to +36.61°. In , Pegasus represents the immortal winged horse born from the neck of the Gorgon when she was slain by ; it was sired by , the god of the sea, and later tamed by the hero , who rode it to defeat the Chimera. Pegasus is prominently visible during autumn evenings from northern latitudes, culminating high in the sky in October for optimal observation.

Stellar Composition

The constellation Pegasus contains approximately 175 stars brighter than apparent magnitude 6.5, which are visible to the under favorable conditions. These stars form a diverse in terms of , with the brightest examples reaching magnitudes near 2.4 and contributing significantly to the constellation's prominent asterisms, while fainter members cluster around the visibility limit of magnitude 6. This distribution highlights Pegasus as a rich field for amateur astronomers, offering a mix of steady and variable lights across its 1,121 square degrees. The composition of these stars is dominated by G-type and K-type giants among the brighter cohort, such as Matar (G2II) and Sadalbari (G8III), due to the intermediate age of the in this sector of the , where stars have evolved beyond the over billions of years. Hotter main-sequence stars of B and A types, like Algenib (B2IV) and Markab (A0IV), are also represented, but O-type stars are notably absent, reflecting the scarcity of recent, massive in the local galactic disk. This assemblage typifies Population I stars, metal-rich and born in the plane of the , with evolved giants indicating a of steady evolution rather than bursts of youth. Distances to the brighter stars in Pegasus generally range from 100 to 500 light-years, as seen in examples like Homam (204 light-years) and Scheat (196 light-years), situating them within the solar neighborhood of the . Some extend farther, up to around 700 light-years, such as Enif at 672 light-years, which serves as a representative in the constellation's evolved population. Fainter naked-eye stars may reach distances of up to 2,000 light-years or more, though precise measurements from data confirm the overall proximity of the visible ensemble to our local galactic environment.

The Great Square Asterism

Component Stars

The Great Square asterism in is formed by four prominent stars: (Markab), Beta Pegasi (Scheat), Gamma Pegasi (Algenib), and Alpha Andromedae (Alpheratz, historically designated as Delta Pegasi). These stars outline a roughly square shape that spans approximately 15 degrees along each side, making it a distinctive feature visible to the under dark skies. Alpha Pegasi, known as Markab, occupies the southeast corner of the square. It is classified as an A0IV star with an apparent visual magnitude of 2.48 and lies at a distance of about 133 light-years from . Beta Pegasi, or Scheat, marks the northwest corner. This M2.5II-III red giant exhibits irregular variability with a mean apparent magnitude of 2.42 and is located approximately 196 light-years away. Gamma Pegasi, called Algenib, forms the southwest corner. It is a B2IV subgiant with an apparent visual magnitude of 2.84, situated at a distance of roughly 470 light-years. Alpha Andromedae, or Alpheratz, lies at the northeast corner and was traditionally included in Pegasus as Delta Pegasi before modern constellation boundaries reassigned it to Andromeda. This B8IVp has an apparent visual magnitude of 2.06 and is the closest of the four at about 97 light-years.

Observational and Historical Notes

The Great Square of Pegasus serves as a key seasonal marker in the northern hemisphere, rising into the evening sky around September, near the autumnal equinox, and becoming prominently visible high overhead by October. This positioning makes it an effective indicator of the shift to autumnal skies, transitioning observers from summer constellations to fall patterns. Historically, the asterism was recognized in Ptolemy's in the 2nd century CE, where the constellation was cataloged among the 48 ancient figures, with the square's stars outlining the winged horse's body. The Great Square has long aided in locating neighboring constellations, such as guiding observers to Andromeda via its shared star Alpheratz and to Pisces through its eastern extension. In cultural lore, the asterism symbolizes the winged horse Pegasus from Greek mythology, born from the blood of Medusa and tamed by Bellerophon to defeat the Chimaera, while Babylonians viewed the four stars as IKU, a celestial field plowed by an adjacent asterism. Its distinct shape has facilitated celestial navigation, serving as a reliable signpost for ancient astronomers and sailors to orient other sky features. For modern observers, the Great Square's apparent span of approximately 15 degrees across the sky makes it an accessible target for amateur astronomers, often employed to star-hop to deep-sky objects like the . However, the asterism lacks long-term alignment in , as its component stars lie at varying distances—Alpheratz at 97 light-years, Scheat at 196 light-years, Markab at 133 light-years, and Algenib at 470 light-years—causing their relative positions to gradually distort over millennia.

Bright Stars

Magnitude 2.0 to 2.5

The brightest stars in the constellation Pegasus, with apparent magnitudes ranging from 2.0 to 2.5, form key points in the celestial figure of the winged horse and are easily observable under suburban skies. These include Epsilon Pegasi (Enif), Beta Pegasi (Scheat), and Alpha Pegasi (Markab). Enif stands out as the most luminous and distant among them, representing the nose in the traditional asterism of Pegasus. Epsilon Pegasi, or Enif, is classified as a Ib with an of 2.39 and lies approximately 690 light-years away. It possesses a of about 12 solar masses and radiates with a of roughly 7,500 times that of the Sun, making it a prominent evolved star in the constellation. Beta Pegasi, commonly called Scheat, is a of spectral type M2.5 II-III, notable for spectral peculiarities including a low surface temperature of around 3,700 and strong emission relative to its visual brightness. Its fluctuates between 2.31 and 2.74 due to semi-regular variability, with details covered in the Variable Stars section. The table below summarizes the primary attributes of these stars:
Bayer designationCommon nameApparent magnitudeSpectral typeDistance (ly)Coordinates (RA, Dec J2000)
ε PegEnif2.39K2 Ib69021h 44m 11s, +09° 52' 30"
β PegScheat2.42 (var. 2.31–2.74)M2.5 II-III19623h 03m 46s, +28° 04' 58"
α PegMarkab2.48A0 IV13323h 04m 46s, +15° 12' 19"
Data sourced from SIMBAD astronomical database. Distances calculated from / parallaxes (1 pc ≈ 3.26 ly).

Magnitude 2.5 to 4.0

The stars in with apparent magnitudes between 2.5 and 4.0 form key elements in defining the constellation's distinctive shape, particularly contributing to the outline of the Great Square asterism and adjacent features visible to the under . These moderately bright stars include subgiants and main-sequence objects of various spectral types, ranging from hot B-type to cooler G-type, at distances from tens to hundreds of light-years. Their positions and motions provide insights into the local stellar population's dynamics. Gamma Pegasi, or Algenib, is a B2IV shining at magnitude 2.84, situated about 470 light-years distant, and also forms a corner of the Great Square; it exhibits a low projected rotational velocity of 8 km/s, atypical for B-type stars. Pegasi, known as Matar, is a G8II+F0V with a combined magnitude of 2.95 and a distance of roughly 196 light-years, briefly noted here for its role in extending the constellation's northern outline (detailed multiplicity in the Multiple Star Systems section). Further outlining the figure, Zeta Pegasi (Homam) is a B8.5IV subgiant of magnitude 3.41 at about 229 light-years, while Iota Pegasi, an F5V main-sequence star, appears at magnitude 3.77 and lies just 39 light-years away. The table below summarizes their key astrometric and photometric parameters.
Star NameApparent Magnitude (V)Spectral TypeDistance (ly)RA (J2000)Dec (J2000)Proper Motion (mas/yr, RA/Dec)
Gamma Pegasi (Algenib)2.84B2IV47000h 13m 14.2s+15° 11' 01"+0.49 / -10.73
Eta Pegasi (Matar)2.95G8II+F0V19622h 43m 00.1s+30° 13' 16"+19.96 / -18.97
Zeta Pegasi (Homam)3.41B8.5IV22922h 41m 27.7s+10° 49' 53"+77.22 / -11.38
Iota Pegasi3.77F5V3922h 07m 00.7s+25° 20' 42"+295.48 / +27.44

Variable Stars

Semiregular and Irregular Variables

Semiregular variables in are late-type giants or supergiants that display light curves with periods of variation interrupted by episodes of irregularity, typically resulting from non-radial pulsations and convective processes in their extended envelopes. These stars, classified under types such as SRc and SRd in the General Catalogue of Variable Stars (GCVS), show amplitudes generally less than 2 magnitudes and periods from 30 to several hundred days. The variability arises primarily from convective instabilities in the outer layers of these evolved stars, where large-scale turbulent motions lead to oscillatory modes that modulate brightness without strict periodicity. Beta Pegasi, commonly known as Scheat, exemplifies an SRd-type semiregular variable, an M2.5 giant with pulsation periods ranging from approximately 40 to 150 days and a visual of about 0.4 magnitudes. Its , as monitored by the American Association of Variable Star Observers (AAVSO), reveals semi-periodic brightenings interspersed with quieter phases, reflecting the interplay of multiple pulsation modes driven by convective turnover in its atmosphere. This variability causes Scheat's to fluctuate between 2.31 and 2.74.

Pulsating Variables

Pulsating variables in are stars whose brightness changes periodically due to the expansion and contraction of their outer layers, driven by instabilities in their interiors. These stars occupy specific regions in the Hertzsprung-Russell diagram, such as the for Delta Scuti types or the for RR Lyrae types, reflecting stages of post-main-sequence evolution where helium core burning or shell instabilities enable pulsations. In , these variables range from hot B-type stars with short periods to cooler Population II objects, offering probes into through asteroseismology. Observations reveal multiple modes in many cases, allowing modeling of internal density and rotation profiles. RT Pegasi exemplifies a classical , pulsating with a primary period of 0.51 days and a magnitude variation from 9.57 to 9.75, while exhibiting multiple modes that complicate its but enrich seismic analysis. XX Pegasi, an RR Lyrae ab-type star of Population II origin, shows a period of 0.58 days and amplitude from 10.2 to 11.0 magnitudes, typical of evolution after the phase where helium flashes trigger radial pulsations. Such stars in highlight the diversity of pulsation mechanisms, from high-order p-modes in Delta Scuti variables on or near the to fundamental mode pulsations in RR Lyrae stars. Delta Scuti variables like those in Pegasus are generally F-type stars (A-F spectral range) evolving through the classical , where partial ionization zones drive κ-mechanism pulsations with periods of hours to days and low amplitudes (up to 0.2 mag). RR Lyrae types, conversely, reside on the as evolved low-mass stars (~0.5-0.8 M⊙), pulsating radially with periods around 0.2-1 day and amplitudes of 0.5-2 mag, serving as standard candles due to their uniform absolute magnitudes near M_V ≈ 0.6. Multi-mode pulsators among them, such as certain Delta Scuti examples, reveal non-radial oscillations (l=1,2) that map internal convection zones. The following table summarizes key pulsating variables in Pegasus, focusing on brighter or well-studied examples with their primary periods, amplitude ranges, and spectral classifications (data as of 2020 unless noted):
Star NameTypePrimary Period (days)Magnitude RangeSpectral TypeNotes
γ PegasiBeta Cephei0.152.83–2.95B2 IVShort-period, non-radial modes dominant.
ζ PegasiSPB~1.03.41 (small amp.)B8 VSlowly pulsating B-star with monosinusoidal variation.
τ PegasiDelta Scuti0.04~4.58 (var. 0.1)A5 VMultiperiodic with periods 0.94–1.30 hours; rapid rotation.
IK PegasiDelta Scuti0.046.10–6.25A0 V; 22.9 cycles per day.
RT PegasiDelta Scuti0.519.57–9.75F5Multiple modes; classical short-period pulsator.
XX PegasiRR Lyrae ab0.5810.2–11.0APopulation II; location.
DY PegasiSX Phe0.07~10.5 (var. 0.3)A2-F0Population II subtype of Delta Scuti; short period.
GX PegasiDelta Scuti0.18 (multi)10.2–10.6F0Five observed frequencies; theoretical modeling applied.
BP PegasiDelta Scuti0.18 (double-radial)~10.0 (high amp.)F2High-amplitude; ASAS data reveals modes.
A notable discovery from 2017 is the rare triple-mode high-amplitude Delta Scuti star ROTSE1 J232056.45+345150.9 in , approximately 7,000 light years distant, pulsating in three directions simultaneously with periods around 0.1 days; at the time, it was one of only seven such objects known in the , though additional examples have since been identified (as of 2025, at least 11 known).

Multiple Star Systems

Double Stars

Visual double stars in the constellation are pairs of stars that appear close together in the sky and can be resolved with small telescopes, providing opportunities to observe orbital motion over time if they are physical binaries. These systems offer insights into and dynamics, with separations typically ranging from a few arcseconds to tens of arcseconds. Among the notable examples is Eta Pegasi, known as Matar, a bright with a faint companion that forms a striking visual pair. The primary component, Eta Pegasi A, is a G2II bright giant with an of 2.95, while the companion, Eta Pegasi B, is an F0V star with a magnitude of 8.12. The current separation between A and B is 90.4 arcseconds, making it easily resolvable even in modest instruments. The system is located at a distance of 214 years from . Another example is Iota Pegasi, a visual consisting of a primary F5V main-sequence star of magnitude 3.76 and a faint companion of magnitude approximately 11.4. The pair has a separation of about 123.7 arcseconds, likely an optical alignment rather than a physical binary, as no orbital motion has been confirmed. The lies 39 light years away. Orbital data for the wide pair is not established, but the primary itself is a close spectroscopic binary with a period of 10.2 days.
Bayer NameSeparation (arcsec)Position Angle (°)Magnitudes (A/B)
η Pegasi90.4338 (2000)2.95 / 8.12
ι Pegasi123.723 (2012)3.76 / 11.4
Note: Position angles are approximate and based on recent epochs; actual values may vary slightly due to proper motion. These double stars in Pegasus are particularly suitable for amateur astronomers, as their separations allow resolution with small telescopes of 4-inch or larger under good seeing conditions. For Eta Pegasi, the contrast between the bright primary and fainter companion creates a dramatic view at low magnifications (50x–100x), while Pegasi's pair requires higher power (150x+) to clearly separate the faint secondary against the primary's glow. Observations are best during autumn evenings when Pegasus is high in the sky.

Triple and Higher-Order Systems

In the constellation , triple and higher-order star systems are relatively rare but provide valuable insights into stellar formation and dynamical interactions. These hierarchical systems typically consist of an inner close binary orbited by a more distant companion, allowing for the study of orbital stability and evolutionary processes through combined visual, astrometric, and spectroscopic observations. One prominent example is κ Pegasi, a nearby triple system at approximately 115 light years, comprising a wide visual pair where one component is itself a close spectroscopic binary. The inner binary in κ Pegasi (components Ba and Bb) is a single-lined spectroscopic system with an of 5.9715 days and a semimajor axis of 0.087 AU, characterized by a low eccentricity of 0.0073, indicating a nearly . The primary Ba is an F5 IV , while Bb is inferred to be a late G or early dwarf based on mass function estimates. The outer orbit involves component A, another F5 IV , around the Ba-Bb pair, with a period of 4227 days (about 11.6 years), semimajor axis of 8.14 AU, eccentricity of 0.318, and inclination of 107.9°. The mutual inclination between the inner and outer orbits is 43.8°, which places the system near the threshold for Kozai-Lidov oscillations; these secular perturbations could induce eccentricity variations in the inner orbit, potentially influencing long-term dynamical stability without leading to ejection, as no disruptions have been observed over decades of monitoring. Another notable triple system is DI Pegasi, an Algol-type eclipsing binary with a distant tertiary companion detected through light-time effects in the timing of primary and secondary minima. The inner binary has an of 0.7118 days (17.07 hours), with spectroscopic elements including semi-amplitudes K₁ = 185.7 km/s for the primary and K₂ = 109.7 km/s for the secondary, yielding individual masses of approximately 1.19 M⊙ and 0.70 M⊙ assuming an edge-on orbit. The outer orbit has a period of about 54.6 years, attributed to the gravitational influence of the third component, though its separation remains uncertain at around 5 arcseconds, corresponding to approximately 1350 AU at the system's distance of about 880 light-years. This configuration highlights in the inner pair, with the tertiary providing constraints on the system's age and evolution. Higher-order systems in Pegasus include historical observations suggesting quadruple configurations, such as early spectroscopic analyses of κ Pegasi that identified four distinct line profiles under optimal conditions, implying an additional unresolved companion; however, modern confirms only three bound components, with the fourth likely a foreground or background interloper. Orbital eccentricities in these systems, ranging from near-zero in close pairs to moderate values like 0.318 in wider orbits, contribute to their stability by minimizing close encounters, while inclinations near 90°-125° enable detailed modeling of dynamics. These systems underscore the prevalence of hierarchical architectures in stellar multiples, aiding simulations of formation via fragmentation in protostellar disks.
System NameNumber of ComponentsInner Period (days)Inner Separation (AU)Outer Period (years)Outer Separation (arcsec / AU)
κ Pegasi35.970.08711.60.235 / 8.14
DI Pegasi30.712~0.00454.6~5 / ~1350

Exoplanet-Hosting Stars

Pegasus hosts approximately 20 unique stars with confirmed , encompassing over 40 planets discovered through various methods including , transit, and direct imaging, as of November 2025. This section focuses on landmark discoveries using the and transit methods.

Radial Velocity Discoveries

The method has yielded significant exoplanet discoveries around stars in the constellation , primarily identifying massive, short-period gas giants known as hot Jupiters through measurements of stellar Doppler shifts induced by planetary gravitational tugs. These detections rely on monitoring periodic variations in the star's semi-amplitude KK, which quantifies the amplitude of the wobble and provides constraints on the planet's minimum mass (msin⁡im \sin i), , and eccentricity. In , such systems highlight compact architectures where planets orbit at small semi-major axes, receiving intense stellar irradiation. One landmark discovery is , the first confirmed around a main-sequence star similar to the Sun, announced in 1995. Orbiting the G2V star ( 5.49), this has an of 4.23 days, a minimum of 0.46 MJ0.46 \, M_J (msin⁡im \sin i), near-zero eccentricity (e=0.01e = 0.01), and induces a stellar semi-amplitude of K=55.9 m/sK = 55.9 \, \mathrm{m/s}. The close-in orbit, at a semi-major axis of approximately 0.05 AU, challenged models of planetary formation and migration, suggesting dynamical processes that transport massive planets inward from wider orbits. Another notable system is HD 209458, a G0V star ( 7.65) hosting the HD 209458 b, detected via in 1999 and nicknamed the "" planet due to its evaporating atmosphere observed later. This planet has an orbital period of 3.52 days, a minimum mass of 0.63 MJ0.63 \, M_J (msin⁡im \sin i), low eccentricity (e<0.008e < 0.008), and a stellar semi-amplitude of K=84 m/sK = 84 \, \mathrm{m/s}, with a semi-major axis of 0.047 AU. The system's architecture exemplifies the hot Jupiter class, with the planet's proximity enabling detailed follow-up studies on atmospheric escape driven by stellar radiation.
Star NamePlanet(s)Discovery YearOrbital Period (days)Minimum Mass (msin⁡im \sin i, MJM_J)EccentricityRadial Velocity Semi-Amplitude KK (m/s)
51 Pegasi51 Pegasi b19954.230.460.0155.9
HD 209458HD 209458 b19993.520.63<0.00884

Transit Method Discoveries

The transit method has revealed several exoplanets orbiting stars in the constellation by detecting periodic dips in stellar brightness caused by planetary transits. This photometric approach allows direct measurement of planetary radii and inclinations, complementing radial velocity data for mass determinations. Among these, stands out as the first exoplanet confirmed via transit observations, orbiting the G0V star HD 209458 at a distance of approximately 157 light-years. HD 209458 b, a hot Jupiter with a radius of 1.38 Jupiter radii (R_J) and an orbital period of 3.524 days, was initially detected by radial velocity in 1999 but confirmed as transiting in 2000 through ground-based photometry showing a 1.5% depth in the star's light curve and an inclination of nearly 87 degrees. The planet's close-in orbit results in extreme temperatures exceeding 1,000 K, making it a benchmark for studying inflated gas giants. Transmission spectroscopy of its transit has provided key insights into its atmosphere, including the first detection of sodium absorption lines in 2002, indicating a hazy upper atmosphere with scattered stellar light. Further observations revealed an extended hydrogen envelope escaping the planet due to intense stellar irradiation, observed via Lyman-alpha absorption during transits, suggesting significant atmospheric mass loss over the planet's lifetime. Later studies using Hubble Space Telescope data confirmed the presence of silicate clouds and hazes, contributing to the planet's low albedo and influencing its transmission spectrum.
Host StarPlanetRadius (R_J)Transit Depth (%)Inclination (degrees)Orbital Period (days)Discovery Year
HD 209458HD 209458 b1.381.4886.13.5242000
While HD 209458 b remains the most studied transiting exoplanet in Pegasus, its atmospheric characterization via transmission spectroscopy highlights the method's power for probing exoplanet compositions and dynamics.

Other Notable Stars

Supergiant and Giant Stars

Supergiant and giant stars in Pegasus exemplify the late evolutionary stages of stars with initial masses ranging from about 2 to 20 solar masses, where core hydrogen exhaustion leads to shell burning and significant expansion. On the Hertzsprung-Russell diagram, these stars cluster in the cool, luminous upper-right region, distinct from the main sequence; giants (luminosity class III) form a horizontal branch for lower-mass stars undergoing helium shell burning, while supergiants (class I) occupy a more vertical extension for higher-mass counterparts, reflecting greater core contraction and higher luminosities from advanced fusion of heavier elements like helium to carbon and oxygen. This placement highlights their paths toward eventual mass loss, potentially culminating in planetary nebulae for giants or core-collapse supernovae for many supergiants. Prominent examples include ε Pegasi (Enif) and β Pegasi (Scheat), detailed in the Bright Stars section. For further reading on their parameters, see that section. Another notable giant is η Pegasi (Matar), a yellow giant of spectral type G2 II, with an effective temperature of about 4,930 K, radius of 68 R⊙, and bolometric luminosity around 95 L⊙, located 221 light-years away. The table below presents selected parameters for key supergiant and giant stars in Pegasus, emphasizing their scale and low surface gravities characteristic of evolved phases. Updated values reflect recent measurements as of 2025.
StarLuminosity ClassRadius (R⊙)log g (cgs)
ε Pegasi (Enif)Ib1831.01
β Pegasi (Scheat)II-III1091.20
η Pegasi (Matar)II682.3
These values derive from spectroscopic and interferometric analyses, illustrating the vast sizes and tenuous outer layers of such stars.

Stars with Unusual Spectral Features

In the constellation of Pegasus, several stars exhibit unusual spectral features characterized by atypical chemical compositions, distinguishing them from standard main-sequence or evolved stars of similar temperatures. These peculiarities often manifest as overabundances or depletions of specific elements, detectable through high-resolution . Notable examples include mercury-manganese (HgMn) stars, which show enhanced absorption lines from heavy elements like mercury (Hg) and (Ga), and Lambda Boötis (λ Boo) stars, which display underabundances in metals relative to solar values while maintaining normal levels of lighter elements like carbon, , and oxygen. One prominent HgMn star in Pegasus is 69 Pegasi (HD 220933), a chemically peculiar A0 III p Hg giant with enhanced spectral lines of mercury and gallium due to radiative levitation concentrating these elements in its atmosphere. High-resolution spectroscopic analyses of such stars reveal significantly stronger absorption lines for these anomalous elements compared to normal A-type stars, with equivalent widths for Hg II λ3984 often exceeding 100 mÅ in HgMn objects, indicating overabundances by factors of 100 to 10,000 relative to solar composition. These features arise primarily from atomic diffusion processes, where gravitational settling and radiative acceleration compete to segregate elements in stable stellar atmospheres lacking significant convection or magnetic fields, as proposed in foundational models of diffusion in upper main-sequence stars. Another example is (V342 Pegasi), a young A5 V λ Boo star in known for its depleted metals, particularly iron-peak elements like Fe, Cr, and Mn, at levels 0.5–1.0 dex below solar, while C, N, O, and S abundances remain near solar. Spectral line analyses confirm this through reduced equivalent widths for metal lines (e.g., Fe I lines around 10–50 mÅ weaker than in normal A stars) across the optical spectrum, consistent with selective depletion patterns. The prevailing formation theory attributes these anomalies to accretion of metal-poor gas from the (ISM), where dust grains lock up , leaving a volatile-enriched gas phase to accrete onto the star's surface, modulated by that prevents full mixing. This mechanism is supported by the star's youth and , which may supply such material. Alternative explanations for λ Boo peculiarities, such as binary mass transfer, have been considered but are less favored for field stars like due to the lack of detected companions contributing enriched material; instead, accretion better matches the observed uniform depletion patterns across the class. In HgMn stars like 69 Pegasi, diffusion alone suffices without invoking external accretion, as the anomalies align with equilibrium states in radiatively supported atmospheres. These processes highlight how weak mixing in A-type stars enables surface compositions to diverge dramatically from bulk stellar material.

References

  1. https://www.go-astronomy.com/constellations.php?Name=Pegasus
  2. https://theskylive.com/sky/constellations/pegasus-constellation
  3. https://www.constellation-guide.com/constellation-list/pegasus-constellation/
  4. https://skyandtelescope.org/astronomy-news/meet-enif-the-nose-of-the-winged-horse/
  5. https://www.skyatnightmagazine.com/advice/skills/great-square-pegasus
  6. https://science.nasa.gov/exoplanet-catalog/51-pegasi-b/
  7. https://mashable.com/article/planets-exoplanets-discovery-2025
  8. https://theplanets.org/constellations/pegasus-constellation/
  9. https://www.theoi.com/Ther/HipposPegasos.html
  10. https://www.space.com/16743-constellation-pegasus.html
  11. https://theskylive.com/sky/constellations/pegasus-bright-stars
  12. https://www.iflscience.com/where-is-our-home-in-the-galaxy-meet-the-orion-arm-74166
  13. https://www.almanac.com/night-sky-map-september-pegasus-measuring-sky
  14. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Markab
  15. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=1995ApJS...99..135A
  16. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2002yCat.2237....0D
  17. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2007A&A...474..653V
  18. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Scheat
  19. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=1989ApJS...71..245K
  20. http://simbad.cds.unistra.fr/simbad/sim-basic?Ident=Algenib
  21. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2024A&A...690A.176N
  22. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=Alpheratz
  23. http://simbad.cds.unistra.fr/simbad/sim-ref?bibcode=2003AJ....126.2048G
  24. https://earthsky.org/favorite-star-patterns/great-square-of-pegasus-wings-in-sept-equinox/
  25. https://astronomynow.com/2023/09/11/the-great-square-of-pegasus-heralding-autumn/
  26. http://www.ianridpath.com/startales/pegasus.html
  27. https://earthsky.org/tonight/star-hop-from-pegasus-to-the-andromeda-galaxy/
  28. https://www.recordonline.com/story/entertainment/local/2005/09/11/tracing-great-square-pegasus/51122420007/
  29. https://www.constellation-guide.com/great-square-of-pegasus/
  30. http://simbad.cds.unistra.fr/simbad/sim-basic?Ident=Epsilon%20Pegasi
  31. http://stars.astro.illinois.edu/sow/enif.html
  32. http://simbad.cds.unistra.fr/simbad/sim-basic?Ident=Beta%20Pegasi
  33. http://stars.astro.illinois.edu/sow/scheat.html
  34. http://simbad.cds.unistra.fr/simbad/sim-basic?Ident=Alpha%20Pegasi
  35. https://heasarc.gsfc.nasa.gov/W3Browse/all/gcvs.html
  36. https://iopscience.iop.org/article/10.1088/0004-637X/725/1/1170
  37. https://www.star-facts.com/scheat/
  38. https://www.aavso.org/vstarviewer/?starname=Beta%20Peg
  39. https://adsabs.harvard.edu/full/1908AnHar..57..211C
  40. https://arxiv.org/pdf/astro-ph/0307429
  41. https://iopscience.iop.org/article/10.3847/1538-4357/aca1c3
  42. https://ui.adsabs.harvard.edu/abs/1993A&A...268..546G/abstract
  43. https://ntrs.nasa.gov/citations/20070018016
  44. https://ui.adsabs.harvard.edu/abs/1992ApJ...400L..71K/abstract
  45. https://www.star-facts.com/ik-pegasi/
  46. https://www.randomastronomicalobject.com/object0161.html
  47. https://academic.oup.com/mnras/article/512/3/3551/6546166
  48. https://blog.smu.edu/research/2017/02/13/new-delta-scuti-rare-pulsating-star-7000-light-years-away-is-1-of-only-7-in-milky-way/
  49. https://www.degruyterbrill.com/document/doi/10.1515/astro-2022-0020/html
  50. http://www.alcyone.de/SIT/mainstars/SIT000661.htm
  51. https://theskylive.com/sky/stars/matar-eta-pegasi-star
  52. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=eta+peg
  53. https://chview.nova.org/solcom/stars2/iota-peg2.htm
  54. http://simbad.u-strasbg.fr/simbad/sim-id?Ident=iota+peg
  55. https://bestdoubles.wordpress.com/category/4-choose-a-constellation/pegasus/
  56. https://arxiv.org/pdf/astro-ph/0509406
  57. https://iopscience.iop.org/article/10.1088/0004-6256/147/6/145
  58. https://www.randomastronomicalobject.com/object0148.html
  59. https://ui.adsabs.harvard.edu/abs/1977RMxAA...3...85B
  60. https://exoplanetarchive.ipac.caltech.edu/
  61. https://exoplanetarchive.ipac.caltech.edu/overview/51%20Pegasi%20b
  62. https://exoplanetarchive.ipac.caltech.edu/overview/HD%20209458
  63. https://astronomy.swin.edu.au/cosmos/h/hertzsprung-russell%2Bdiagram
  64. https://ui.adsabs.harvard.edu/abs/2025Galax..13...81E/abstract
  65. https://ui.adsabs.harvard.edu/abs/2020MNRAS.496..832C/abstract
  66. https://arxiv.org/abs/astro-ph/9805051
  67. https://people.brandonu.ca/gulliver/files/2012/07/alpandpaper.pdf
  68. https://ui.adsabs.harvard.edu/abs/1991ApJ...372L..33C/abstract
  69. https://academic.oup.com/mnras/article/499/2/2701/5891252
  70. https://arxiv.org/abs/astro-ph/0112198
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