List of luminous blue variable stars

Last updated

This is a list of luminous blue variable stars in order of their distance from Earth. [1] [2] [3]

Contents

List

Milky Way galaxy (confirmed LBVs)

Star systemNebulaMedian distance (ly)Stars in system Spectral type Apparent magnitude (V)Comments and references
P Cygni (34 Cygni)5251±1801B1-2 Ia-0ep4.82The closest luminous blue variable star to Earth
V4029 Sagittarii (HD 168607)6,0001B9Ia+8.12 to 8.29 [4] [5] near the Omega Nebula
V905 Scorpii (HD 160529)6,1001LBV6.66 [4] [5]
Eta Carinae (Eta Argus) Eta Carinae.jpg 7,5002O + B−1.0 to ~7.6part of Trumpler 16 in the Carina Nebula
MWC 930 (V446 Scuti) MWC 930 Spitzer IRAC.jpg 11,4001B5/9Iaeq11.51 [4]
WRAY 16-137 12,4001LBV15.5 [6] [5]
W1-243 15,0001LBV15.81 [4] in Westerlund 1
HR Carinae HR Carinae ESO MUSE (H-alpha).png 16,0002LBV+RSG8.42 [4] [5]
V481 Scuti (LBV G24.73+0.69) V481 Scuti Spitzer IRAC.jpg 17,0001LBV_B[e]: [4]
AG Carinae A closer look at Hubble's 31st anniversary snapshot (51484874537).jpg 17,000 ± 1,0001B6.96
EM* VRMF 55 (MN44) VRMF 55 Spitzer MIPS.png 18,000 or 35,0001LBV15 [6] [7]
[GKF2010] MN48 MN48 Spitzer.jpg 20,000115.83 [4] [5]
GCIRS 34W (WR 101db)25,0001Ofpe/WN9 [6] [8] in the galactic center
Pistol Star (V4647 Sgr) Pistol star and nebula.jpg 25,1141B>28part of the Quintuplet cluster
LBV G0.120-0.048 (V4998 Sgr) LBV G0.120-0.048.jpg 26,0001WN5b [6] near the Quintuplet cluster
FMM 362 (V4650 Sgr)26,0001LBV [6] near the Quintuplet cluster
AFGL 2298 (V1672 Aql)30,0001B8I [6]
V432 Carinae (Wray 15-751) V432 Carinae ESO MUSE H-alpha.png 33,0001LBV10.20Also known as AT 2019ooa [4] [5]
[GKM2012] WS1 WS1 unWISE W4.png 39,0001LBV15.31 [4] [5]
[GKF2010] MN58 MN58 Spitzer.jpg 1 [6]

Milky Way galaxy (candidate LBVs)

Star systemNebulaMedian distance (ly)Stars in system Spectral type Apparent magnitude (V)Comments and references
HD 148937 The nebula (NGC 6164-6165) surrounding HD 148937 as seen in visible light (eso2407a).tiff 3,8701O6f?p6.71 [6] central star of NGC 6164
MWC 349A (V1478 Cygni) V1479 Cygni Spitzer.jpg 4,5602–3B0-1.5 I + B0 III13.15 [6] maybe ejected from Cygnus OB2
HD 326823 4,7001WNpec9.03 [4] [5]
HD 168625 HD 168625 MUSE H-alpha.png 5,0001B6Ia+8.30–8.41 [4] [5] near the Omega Nebula
Cygnus OB2-12 5,5001B3–4 Ia+11.702 [4] [5] in Cygnus OB2
AS 314 5,6001B9Ia9.85 [6]
Zeta1 Scorpii 5,6001B1.5 Iae4.705 [4] [5]
G79.29+0.46 G79.29+0.46(2).png 5,7001B:I[e]15.1 [4] [5] in Cygnus X
WRAY 16-232 WRAY 16-232 Spitzer.jpg 6,8501Be12.5 [6] [5]
HD 80077 8,7001B2.5Ia+9.00 [4] [5]
HD 316285 HD 316285.png 10,8001B0Ieq9.60 [4] [5]
MWC 314 (V1429 Aquilae)15,0003B3Ibe9.79 - 10.1 [4] [5]
[SBW2007] 1 SBW 1 VPHAS+ H-alpha.png 18,5001B1Iab12.7 [4] [5]
Sher 25 Sher 25 Hubble WFC3 F656N.jpg 21,0001cLBV12.23 [4] [5] in NGC 3603
W51 LS1 (V1936 Aquilae) V1936 Aquilae Spitzer.jpg 22,0001O4I15.1 [4] [5]
WRAY 17-96 WRAY 17-96.png 22,0001cLBV~13.0 [4] [5]
[B61] 2 B61 2 Spitzer.jpg 22,0001LBV_B[e]:15.00 [6] [5]
WR 102ka 26,0001WN10 [6] near the galactic center
GCIRS 16SW 27,0001Ofpe/WN9 [6] in the galactic center
LBV 1806−20 28,0001cLBV [6] part of the 1806−20 cluster
Hen 3-519 Hubble's Blue Bubble (24908262259).jpg 28,0001WN11h10.85 [4] [5]
MSX6C G026.4700+00.0207 GAL 026.47+00.02.png 30,0001LBV_B [6] [9]

Magellanic Clouds

The Large Magellanic Cloud (LMC) is around 163 kly distant and the Small Magellanic Cloud (SMC) is around 204 kly distant

Host galaxyStar systemStars in system Spectral type Apparent magnitude (V)Comments and references
LMC S Doradus 1B8/9eq – F0/5:Iae8.6 – 11.5
LMCHD 269858 (R127)1B10.15
LMCHD 269006 (R71)1LBV10.55 [6]
LMCHD 269216 (SK −69 75)1OBe11.123 [6]
LMCHD 269582 (SK −69 142a)1WN10h11.093 [6]
LMCHD 269662 (R110)1A0Ia10.28 [6]
LMCHD 269700 (R116)1B1.5Iaeq10.54 [6]
LMCR143 (CPD-69 463)1F7Ia12.014 [6]
SMC HD 5980 (R14)3WN4+O7I:11.31 [6]
SMCHD 6884 (R40)1B9Ia0ek10.2 [6]

Andromeda Galaxy and Triangulum Galaxy

The Andromeda Galaxy (M31) is 2.5 Mly distant and the Triangulum Galaxy is around 3.2 Mly distant

Host galaxyStar systemStars in system Spectral type Apparent magnitude (V)Comments and references
AndromedaLGGS J004051.59+403303.01LBV16.989 [6]
Andromeda AE Andromedae (HV 4476)1LBV17.0–17.9 [6]
Andromeda AF Andromedae (HV 4013)1LBV17.325 [6]
AndromedaVar 15 ([WB92a] 370)1LBV18.450 [6]
AndromedaVar A-11LBV17.143 [6]
AndromedaUCAC4 660-0031111LBV16.39 [6]
TriangulumVar C1LBV16.429 [6]
TriangulumVar B1LBV16.208 [6]
Triangulum Var 83 1LBV15.4–16.6 [6]
TriangulumVar 2 (Y Trianguli)1Ofpe/WN918.22 [6]
Triangulum Romano’s Star (M33 V0532)1Ofpe/WN916.5–18.8 [6]

Single LBV Galaxies

Host GalaxyStar systemMedian distance (ly)Stars in system Spectral type Apparent magnitude (V)Comments and references
NGC 3109 AT 2018akx4,350,0001LBV17.5 - 19.28 [10]
NGC 2403 AT 2016ccd9,650,0001LBV18.0 - 19.95Also known as SNhunt225. [11] [12]
NGC 4214 SN 2010U9,700,0001LBV16 [13]
NGC 2363 NGC 2363-V1 10,800,0001LBV17.88One of the most luminous stars known.
NGC 45 AT 2018htr21,700,0001LBV17.469 [14]
NGC 2537 AT 2017be27,900,0001LBV18.349 - 18.5Distance from NED using redshift of host galaxy. [15]
NGC 4559 AT 2016blu 29,000,0001LBV15.9 – 19Repeated outbursts have been observed since January 2012. [16] [17]
NGC 7286 AT 2019mil32,400,0001LBV19Distance from NED using redshift of host galaxy. [18]
UGC 5829 AT 2021blu43,500,0001LBV18.17 - 21.62Distance from NED using redshift of host galaxy. [19]
NGC 4656 Variable in NGC 465643,700,0001LBV18Distance from NED using redshift of host galaxy. [20]
NGC 4389 AT 2022fnm44,700,0001LBV18.495 - 17.855Distance from NED using redshift of host galaxy. [21]
ESO 249- G 015AT 2020agp47,500,0001LBV18.463Distance from NED using redshift of host galaxy. [22]
NGC 908 AT 2021ablz56,000,0001LBV20.58 [23]
IC 5267A AT 2019oet60,000,0001LBV18.335Distance from NED using redshift of host galaxy. [24]
NGC 2748 PSN J09132750+762741061,300,0001LBV18.3 [25]
NGC 3423 AT 2019ahd65,600,0001LBV17.83 - 18.73Distance from NED using redshift of host galaxy. [26]
NGC 1385 AT 2020pju66,400,0001LBV17.3 - 19.73 [27]
NGC 718 AT 2019udc69,800,0001LBV17.53 - 19.09Distance from NED using redshift of host galaxy. [28]
SDSS J094838.45+332529.1AT 2020jev80,200,0001LBV18.74 - 20.33Distance from NED using redshift of host galaxy. [29]
NGC 6509 PSN J17592296+061726795,300,0001LBV18.5 [30]
NGC 4045 AT 2019wbg111,500,0001LBV17.7 -19.39Repeated outbursts observed since discovery. Distance from NED using redshift of host galaxy. [31]
NGC 4532 AT 2017des112,800,0001LBV18.817 - 19.85Distance from NED using redshift of host galaxy. [32] [33]
ESO 602- G 015AT 2022rmk113,200,0001LBV19.472 - 20.04Distance from NED using redshift of host galaxy. [34]
UGC 9113 AT 2017dau162,100,0001LBV19.32 - 21.32Distance from NED using redshift of host galaxy. [35]
MCG +07-07-070AT 2018kle180,200,0001LBV18.797 - 18.91Distance from NED using redshift of host galaxy. [36]
UGC 449 AT 2022oku239,100,0001LBV18.781 - 19.49Distance from NED using redshift of host galaxy. [37]
WISEA J010803.49+010843.7AT 2020zmn262,600,0001LBV20.31 - 20.85Distance from NED using redshift of host galaxy. [38]

See also

Related Research Articles

<span class="mw-page-title-main">Antlia</span> Constellation in the Southern Celestial Hemisphere

Antlia is a constellation in the Southern Celestial Hemisphere. Its name means "pump" in Latin and Greek; it represents an air pump. Originally Antlia Pneumatica, the constellation was established by Nicolas-Louis de Lacaille in the 18th century. Its non-specific (single-word) name, already in limited use, was preferred by John Herschel then welcomed by the astronomic community which officially accepted this. North of stars forming some of the sails of the ship Argo Navis, Antlia is completely visible from latitudes south of 49 degrees north.

<span class="mw-page-title-main">NGC 300</span> Galaxy in the constellation Sculptor

NGC 300 (also known as Caldwell 70 or the Sculptor Pinwheel Galaxy) is a spiral galaxy in the constellation Sculptor. It was discovered on 5 August 1826 by Scottish astronomer James Dunlop. It is one of the closest galaxies to the Local Group, and probably lies between the latter and the Sculptor Group. It is the brightest of the five main spirals in the direction of the Sculptor Group. It is inclined at an angle of 42° when viewed from Earth and shares many characteristics of the Triangulum Galaxy. It is 94,000 light-years in diameter, somewhat smaller than the Milky Way, and has an estimated mass of (2.9 ± 0.2) × 1010M☉.

<span class="mw-page-title-main">NGC 3184</span> Galaxy in the constellation Ursa Major

NGC 3184, the Little Pinwheel Galaxy, is a spiral galaxy approximately 40 million light-years away in the constellation Ursa Major. Its name comes from its resemblance to the Pinwheel Galaxy. It was discovered on 18 March 1787 by German-British astronomer William Herschel. It has two HII regions named NGC 3180 and NGC 3181.

<span class="mw-page-title-main">NGC 4725</span> Galaxy in the constellation Coma Berenices

NGC 4725 is an intermediate barred spiral galaxy with a prominent ring structure, located in the northern constellation of Coma Berenices near the north galactic pole. It was discovered by German-born British astronomer William Herschel on April 6, 1785. The galaxy lies at a distance of approximately 40 megalight-years from the Milky Way. NGC 4725 is the brightest member of the Coma I Group of the Coma-Sculptor Cloud, although it is relatively isolated from the other members of this group. This galaxy is strongly disturbed and is interacting with neighboring spiral galaxy NGC 4747, with its spiral arms showing indications of warping. The pair have an angular separation of 24′, which corresponds to a projected linear separation of 370 kly. A tidal plume extends from NGC 4747 toward NGC 4725.

<span class="mw-page-title-main">Merope (star)</span> B-type subgiant star in the constellation Taurus

Merope, designated 23 Tauri, is a star in the constellation of Taurus and a member of the Pleiades star cluster. It is approximately 440 light-years (135 pc) away.

<span class="mw-page-title-main">NGC 514</span> Spiral galaxy in the constellation Pisces

NGC 514 is a low-luminosity, intermediate spiral galaxy in the equatorial constellation of Pisces, located at a distance of approximately 83 million light-years from the Milky Way. It was discovered on 16 October 1784 by astronomer William Herschel. The general form of the galaxy is specified by its morphological classification of SAB(rs)c, which indicates it has a weak bar system at the core (SAB), an incomplete ring formation around the bar (rs), and somewhat loosely-wound spiral arms (c). This galaxy has an H II nucleus with an extended region that displays weak emission lines in the optical range, but not in the near infrared. The suspected supermassive black hole at the core has an estimated mass of 3.2×106 M☉.

<span class="mw-page-title-main">NGC 4559</span> Galaxy in the constellation Coma Berenicies

NGC 4559 is an intermediate spiral galaxy with a weak inner ring structure in the constellation Coma Berenices. Distance estimates for NGC 4559 range from about 28 million light-years to 31 million light-years, averaging about 29 million light-years. It was discovered on 11 April 1785 by German-British astronomer William Herschel.

<span class="mw-page-title-main">NGC 45</span> Spiral galaxy in the constellation Cetus

NGC 45 is a low surface brightness spiral galaxy in the equatorial constellation of Cetus. It was discovered on 11 November 1835 by the English astronomer John Herschel. The galaxy is located at a distance of 22 million light years and is receding with a heliocentric radial velocity of 466 km/s. It is located in the vicinity of the Sculptor Group, but is most likely a background galaxy.

Zeta<sup>1</sup> Scorpii Star in the constellation Scorpius.

Zeta1 Scorpii is a B-type hypergiant star in the constellation of Scorpius. It has an apparent visual magnitude which varies between 4.66 and 4.86. It is a member of the Scorpius OB1 association, and potentially of the open star cluster NGC 6231, also known as the "Northern jewel box" cluster. Around 36 times as massive as the Sun, it is also one of the most luminous stars known in the Galaxy, with an estimated bolometric luminosity of around 850,000 times that of the Sun and a radius 103 times that of the Sun.

<span class="mw-page-title-main">NGC 5806</span> Spiral galaxy in the constellation Virgo

NGC 5806 is an intermediate spiral galaxy in the constellation Virgo. It was discovered on February 24, 1786, by the astronomer John Herschel. It is located about 70 million light-years away from the Milky Way. It is a member of the NGC 5846 Group.

<span class="mw-page-title-main">V1429 Aquilae</span> Star in the constellation Aquila

V1429 Aquilae is a candidate luminous blue variable multiple star system located in the constellation of Aquila. It is often referred to by its Mount Wilson Observatory catalog number as MWC 314. It is a hot luminous star with strong emission lines in its spectrum.

<span class="mw-page-title-main">AS 314</span> Protoplanetary nebula in the constellation Scutum

AS 314, also known as V452 Scuti, is a protoplanetary nebula once believed to be a white hypergiant star or luminous blue variable located in the constellation of Scutum. It has an apparent magnitude of 9.85 and can be seen with small telescopes.

<span class="mw-page-title-main">HD 316285</span> Star in the constellation Sagittarius

HDE 316285 is a blue supergiant star in the constellation Sagittarius. It is a candidate luminous blue variable and lies about 6,000 light years away in the direction of the Galactic Center.

<span class="mw-page-title-main">NGC 4424</span> Spiral galaxy in the constellation Virgo

NGC 4424 is a spiral galaxy located in the equatorial constellation of Virgo. It was discovered February 27, 1865 by German astronomer Heinrich Louis d'Arrest. This galaxy is located at a distance of 13.5 million light years and is receding with a heliocentric radial velocity of 442 km/s. It has a morphological class of SB(s)a, which normally indicates a spiral galaxy with a barred structure (SB), no inner ring feature (s), and tightly-wound spiral arms (a). The galactic plane is inclined at an angle of 62° to the line of sight from the Earth. It is a likely member of the Virgo Cluster of galaxies.

<span class="mw-page-title-main">NGC 5917</span> Spiral galaxy in the constellation Libra

NGC 5917 is a spiral galaxy located in the constellation of Libra. It was discovered by English astronomer John Herschel on 16 July 1835. This galaxy is located at a distance of 90.4 ± 6.2 million light-years (27.73 ± 1.90 Mpc) from the Milky Way, and is receding with a heliocentric radial velocity of 1,934.1 km/s. It is interacting with the neighboring galaxy, PGC 54817, at an angular separation of 4.2′. Tidal tails extend from PGC 54817 to the halo of NGC 5917.

<span class="mw-page-title-main">NGC 1325</span> Galaxy in the constellation Eridanus

NGC 1325 is a flocculent spiral galaxy situated in the constellation of Eridanus. Located about 75 million light years away, it is a member of the Eridanus cluster of galaxies, a cluster of about 200 galaxies. It was discovered by William Herschel on 19 December 1799.

<span class="mw-page-title-main">V1936 Aquilae</span> Blue supergiant star in the constellation Aquila

V1936 Aquilae is a blue supergiant and candidate Luminous blue variable located in the nebula Westerhout 51, in the constellation Aquila, about 20,000 light years away. The star was originally identified as a massive star in 2000, and was thought to be an O-type supergiant. However, subsequent analyses have shown it to be not O but B-type, as well as being possibly an LBV.

<span class="mw-page-title-main">V4332 Sagittarii</span>

V4332 Sagittarii is a nova-like event in the constellation of Sagittarius. It was discovered February 24, 1994 at an apparent visual magnitude of 8.9 by Japanese amateur astronomer Minoru Yamamoto from Okazaki, Aichi, then confirmed by K. Hirosawa. Initially designated Nova Sagittarii 1994 #1, it was given the variable star designation V4332 Sgr. A spectra of the event taken March 4 lacked the characteristic features of a classical nova, with the only emission lines being of the Balmer series. Subsequent spectra showed a rapid decline in luminosity and a change of spectral type over a period of five days. By 2003, the object was ~1500 times less luminous than at peak magnitude and showed a spectrum of an M-type star.

References

  1. ↑ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR .
  2. ↑ Barry, Don C. (January 1970), "Spectral Classification of a and F Stars", Astrophysical Journal Supplement, 19: 281, Bibcode:1970ApJS...19..281B, doi:10.1086/190209.
  3. ↑ Frost, E. B. (December 1924), "Fourteen spectroscopic binaries", Astrophysical Journal, 60: 319–320, Bibcode:1924ApJ....60..319F, doi:10.1086/142868.
  4. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 Smith, Nathan; Aghakhanloo, Mojgan; Murphy, Jeremiah W.; Drout, Maria R.; Stassun, Keivan G.; Groh, Jose H. (2019). "On the Gaia DR2 distances for Galactic luminous blue variables". Monthly Notices of the Royal Astronomical Society. 488 (2): 1760–1778. arXiv: 1805.03298 . Bibcode:2019MNRAS.488.1760S. doi: 10.1093/mnras/stz1712 . S2CID   119267371.
  5. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e).
  6. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 17 18 19 20 21 22 23 24 25 26 27 28 29 30 31 32 33 34 35 Richardson, Noel D.; Mehner, Andrea (2018-07-01). "The 2018 Census of Luminous Blue Variables in the Local Group". Research Notes of the American Astronomical Society. 2 (3): 121. arXiv: 1807.04262 . Bibcode:2018RNAAS...2..121R. doi: 10.3847/2515-5172/aad1f3 . ISSN   2515-5172.
  7. ↑ Gvaramadze, V. V.; Kniazev, A. Y.; Berdnikov, L. N. (2015-12-01). "Discovery of a new bona fide luminous blue variable in Norma". Monthly Notices of the Royal Astronomical Society. 454 (4): 3710–3721. arXiv: 1509.08931 . Bibcode:2015MNRAS.454.3710G. doi: 10.1093/mnras/stv2278 . ISSN   0035-8711.
  8. ↑ Trippe, S.; Martins, F.; Ott, T.; Paumard, T.; Abuter, R.; Eisenhauer, F.; Gillessen, S.; Genzel, R.; Eckart, A.; Schödel, R. (2006-03-01). "GCIRS34W: an irregular variable in the Galactic Centre". Astronomy and Astrophysics. 448 (1): 305–311. arXiv: astro-ph/0510478 . Bibcode:2006A&A...448..305T. doi:10.1051/0004-6361:20053173. ISSN   0004-6361.
  9. ↑ Hou, L. G.; Gao, X. Y. (2014-02-01). "A statistical study of gaseous environment of Spitzer interstellar bubbles". Monthly Notices of the Royal Astronomical Society. 438 (1): 426–437. arXiv: 1311.4943 . Bibcode:2014MNRAS.438..426H. doi: 10.1093/mnras/stt2212 . ISSN   0035-8711.
  10. ↑ "AT 2018akx". Transient Name Server. IAU . Retrieved 31 August 2024.
  11. ↑ Bishop, David (9 November 2021). "LBV AT2016ccd in NGC 2403". Rochester Astronomy. Retrieved 31 August 2024.
  12. ↑ "AT 2016ccd". Transient Name Server. IAU . Retrieved 31 August 2024.
  13. ↑ Green, Daniel W. E. (7 February 2010). "Electronic Telegram No. 2163". Central Bureau for Astronomical Telegrams. Dept. of Earth and Planetary Sciences, Harvard University. Retrieved 31 August 2024.
  14. ↑ "AT 2018htr". Transient Name Server. IAU . Retrieved 30 August 2024.
  15. ↑ "AT 2017be". Transient Name Server. IAU . Retrieved 31 August 2024.
  16. ↑ Bishop, David (6 July 2021). "LBV 2016blu in NGC 4559". rochesterastronomy.org. Retrieved 9 August 2021.
  17. ↑ Aghakhanloo, Mojgan; Smith, Nathan; Milne, Peter; Andrews, Jennifer E.; Van Dyk, Schuyler D.; Filippenko, Alexei V.; Jencson, Jacob E.; Lau, Ryan M.; Sand, David J.; Wyatt, Samuel; Zheng, WeiKang (2022). "Recurring outbursts of the supernova impostor AT 2016blu in NGC 4559". Monthly Notices of the Royal Astronomical Society. 526 (1): 456. arXiv: 2212.09708 . Bibcode:2023MNRAS.526..456A. doi: 10.1093/mnras/stad2702 .
  18. ↑ "AT 2019mil". Transient Name Server. IAU . Retrieved 30 August 2024.
  19. ↑ "AT 2021blu". Transient Name Server. IAU . Retrieved 30 August 2024.
  20. ↑ Green, Daniel W. E. (24 March 2005). "Circular No. 8498". Central Bureau for Astronomical Telegrams. Dept. of Earth and Planetary Sciences, Harvard University. Retrieved 31 August 2024.
  21. ↑ "AT 2022fnm". Transient Name Server. IAU . Retrieved 15 August 2024.
  22. ↑ "AT 2020agp". Transient Name Server. IAU . Retrieved 30 August 2024.
  23. ↑ "AT 2021ablz". Transient Name Server. IAU . Retrieved 15 August 2024.
  24. ↑ "AT 2019oet". Transient Name Server. IAU . Retrieved 31 August 2024.
  25. ↑ Fox, Derek (12 February 2015). "Asiago spectroscopic observation of PSN J09132750+7627410". The Astronomer's Telegram. Retrieved 31 August 2024.
  26. ↑ "AT 2019ahd". Transient Name Server. IAU . Retrieved 30 August 2024.
  27. ↑ "AT 2020pju". Transient Name Server. IAU . Retrieved 15 August 2024.
  28. ↑ "AT 2019udc". Transient Name Server. IAU . Retrieved 30 August 2024.
  29. ↑ "AT 2020jev". Transient Name Server. IAU . Retrieved 30 August 2024.
  30. ↑ Green, Daniel W. E. (June 30, 2011). "Electronic Telegram No. 2754". Central Bureau for Astronomical Telegrams. Retrieved 1 September 2024.
  31. ↑ "AT 2022rmk". Transient Name Server. IAU . Retrieved 29 August 2024.
  32. ↑ "AT 2017des". Transient Name Server. IAU . Retrieved 31 August 2024.
  33. ↑ "Astronote 2022-36". Transient Name Server. IAU . Retrieved 31 August 2024.
  34. ↑ "AT 2022rmk". Transient Name Server. IAU . Retrieved 29 August 2024.
  35. ↑ "AT 2017dau". Transient Name Server. IAU . Retrieved 30 August 2024.
  36. ↑ "AT 2018kle". Transient Name Server. IAU . Retrieved 30 August 2024.
  37. ↑ "AT 2022oku". Transient Name Server. IAU . Retrieved 29 August 2024.
  38. ↑ "AT 2020zmn". Transient Name Server. IAU . Retrieved 30 August 2024.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.