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Ashall, C.; Bar, I.; Campbell, H.; Chen, T.-W.; Childress, M.; Elias-Rosa, N.; Harmanen, J.; Hosseinzadeh, G.; Johansson, J.; Kangas, T.; Kankare, E.; Kim, S.; Kuncarayakti, H.; Lyman, J.; Magee, M. R.; Maguire, K.; Malesani, D.; Mattila, S.; McCully, C. V.; Nicholl, M.; Prentice, S.; Romero-Cañizales, C.; Schulze, S.; Smith, K. W.; Sollerman, J.; Sullivan, M.; Tucker, B. E.; Valenti, S.; Wheeler, J. C.; Young, D. R. (December 12, 2016). "The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole".
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410:(SLSN) so far seen, but it was recognized as being unusual in several respects. The spectrum did not closely match other type I SLSNe and previous SLSNe have been discovered in relatively small active star-producing galaxies, not in the central regions of large galaxies. The double-peaked light curve is not expected from a SLSN and the total energy output approaches theoretical limits.
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One known method for producing extremely large amounts of energy is the tidal disruption of objects such as stars by a supermassive black hole. ASASSN-15lh occurred in the nucleus of a large passive galaxy where a supermassive black hole is likely. A black hole of the mass expected in the host galaxy
378:
The host galaxy for ASASSN-15lh is APMUKS(BJ) B215839.70â615403.9, much larger and more luminous than the Milky Way. The host galaxy has visual magnitude 18.5 and is red in color with a low rate of star formation. It maintained a steady brightness until the supernova lit up. The strongest parts of
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might be able to disrupt a star with a mass similar to the sun outside the event horizon and produce a hot accretion disc and luminous transient. It could also account for the temperature changes, rebrightening, and unusual spectral evolution. However, lack of hydrogen and/or helium lines in the
700:
Leloudas, G.; Fraser, M.; Stone, N. C.; van Velzen, S.; Jonker, P. G.; Arcavi, I.; Fremling, C.; Maund, J. R.; Smartt, S. J.; KrĂŹhler, T.; Miller-Jones, J. C. A.; Vreeswijk, P. M.; Gal-Yam, A.; Mazzali, P. A.; De Cia, A.; Howell, D. A.; Inserra, C.; Patat, F.; de Ugarte
Postigo, A.; Yaron, O.;
765:; I.B. Thompson; U. Basu; J.F. Beacom; D. Bersier; J. Brimacombe; J.S. Brown; P. Chen; E. Conseil; A.B. Danilet; E. Falco; D. Grupe; S. Kiyota; G. Masi; B. Nicholls; F. Olivares; G. Pignata; G. Pojmanski; G.V. Simonian; D.M. Szczygiel; P.R. Wozniak (July 24, 2015). Daniel W. E. Green (ed.).
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within the supernova explosion from a WO-type Wolf-Rayet star. The quark nova is produced by the neutron star remnant of the supernova and occurs a few days after the core collapse of the Wolf-Rayet star. This can reproduce many of the unusual features of the observed event but is somewhat
354:
The temperature of ASASSN-15lh at the time of maximum luminosity was 20,000 K, although it was hotter earlier in the outburst. By 50 days after the peak, the temperature had declined to 11,000 K and then remained relatively constant. The radius of ASASSN-15lh at peak brightness was over
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of very distant objects by extremely massive objects closer to Earth. However, this usually occurs with objects much more distant than ASASSN-15lh, and there are no observations indicating the presence of a galaxy cluster suitable to produce a lensing effect.
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was 17.4. From May 8 the possible supernova brightened until it reached a peak brightness of magnitude 16.9 on June 5. By
September the brightness had dropped to magnitude 18.2. There was an unusual "rebrightening" of up to 1.75 magnitudes at blue and
235:, Chile ; the team gave it the designation ASASSN-15lh. It appeared as a transient dot of light on an image and was confirmed with additional observations from other telescopes. The spectrum of ASASSN-15lh was provided by the 2.5-meter
982:
Leloudas, G.; Fraser, M.; Stone, N. C.; Van Velzen, S.; Jonker, P. G.; Arcavi, I.; Fremling, C.; Maund, J. R.; Smartt, S. J.; et al. (2016). "The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole".
429:
into polar jets that heat surrounding material. Again, the energy produced by ASASSN-15lh strains the theoretical limits of this type of explosion and the detailed properties are difficult to reproduce with a magnetar model.
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of ASASSN-15lh would normally swallow stars without a visible flare. The conditions for the production of a highly luminous flare from a TDE around a black hole of the expected mass are unusual, but a rapidly-spinning
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Godoy-Rivera, D.; Stanek, K. Z.; Kochanek, C. S.; Chen, Ping; Dong, Subo; Prieto, J. L.; Shappee, B. J.; Jha, S. W.; Foley, R. J.; Pan, Y.-C.; Holoien, T. W.-S.; Thompson, Todd. A.; Grupe, D.; Beacom, J. F. (2017).
961:
Ouyed, Rachid; Leahy, Denis; Welbanks, Luis; Koning, Nico (2016). "The
Superluminous (Type I) Supernova ASASSN-15lh : A case for a Quark-Nova inside an Oxygen-type Wolf-Rayet supernova remnant".
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The lack of hydrogen and helium features in the spectrum suggest an explosion originating in an object lacking both hydrogen and helium, which would imply a highly stripped star such as a massive
182:, and was the most luminous supernova-like object ever observed. At its peak, ASASSN-15lh was 570 billion times brighter than the Sun, and 20 times brighter than the combined light emitted by the
332:, one of the principal investigators at ASAS-SN, "If it was in our own galaxy, it would shine brighter than the full moon; there would be no night, and it would be easily seen during the day."
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Based on its redshift and location projected on the nucleus of a large galaxy, the distance of ASASSN-15lh is calculated at 1,171 Mpc, in a large luminous galaxy.
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The precise mechanism underlying the very large ASASSN-15lh explosion is still unknown, with speculation ranging from the presence of very large quantities of
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wavelengths, starting about 90 days after the maximum. This coincided with a plateau in the bolometric luminosity that lasted for 120 days.
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398:. Its unusual location in a relatively quiescent galaxy may offer clues for scientists to discover and observe similar events.
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Dong, S.; Shappee, B. J.; Prieto, J. L.; Jha, S. W.; Stanek, K. Z.; Holoien, T. W.- S.; Kochanek, C. S.; Thompson, T. A.;
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A possible supernova was first noticed during an observation on June 2015 by ASAS-SN's twin 14-cm telescopes located at
674:"Astronomers are baffled by a newly discovered cosmic explosion that shines 570 billion times brighter than the sun"
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One model for unusually luminous supernovae involves the conversion of rotational energy from a rapidly-spinning
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Later, other images were found to have been made of ASASSN-15lh as early as May 8, 2015. At this stage the
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event. It was first detected on June 14, 2015, located within a faint galaxy in the southern constellation
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S. Dong; B.J. Shappee; J.L. Prieto; S.W. Jha; K.Z. Stanek; T.W.-S. Holoien; C.S. Kochanek; T.A. Thompson;
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493:"The unexpected, long-lasting, UV rebrightening of the superluminous supernova ASASSN-15lh"
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The nature of ASASSN-15lh is disputed. The most popular explanations are that it is the
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Cowen, Ron (January 14, 2016). "Brightest-ever supernova still baffles astronomers".
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1042:"Explaining the most luminous supernovae with an inefficient jet-feedback mechanism"
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606:; et al. (January 15, 2016). "ASASSN-15lh: A highly super-luminous supernova".
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1108:'Brightest Supernova Ever' Was Actually Monster Black Hole's Violent Star Slashing
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Kerr Black Hole Eating Sun-like Star
Explains Superluminous Explosion ASASSN-15lh
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305:. At its brightest, it was approximately 50 times more luminous than the whole
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the galaxy's spectrum have wavelengths around 1 ÎŒm in the near infrared.
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also contributed observations. On July 24, the event formally received the
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is twice that of the previous brightest type-I superluminous supernova,
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Brightest supernova ever seen pushes theoretical models to the edge
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spectra of ASASSN-15lh poses a major problem for the TDE scenario.
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The initial hypothesis was that ASASSN-15lh was the most extreme
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The spectrum of ASASSN-15lh was relatively featureless, with no
44:(2017). The purple line shows the brightness of the host galaxy.
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Gilkis, Avishai; Soker, Noam; Papish, Oded (November 4, 2015).
908:"We've found the brightest ever supernova but can't explain it"
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galaxy, with an energy flux 570 billion times greater than the
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for ASASSN-15lh, plotted from data published by Godoy-Rivera
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absorption doublets were detected and used to confirm the
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Timeline of white dwarfs, neutron stars, and supernovae
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Unexpectedly bright visible objects can be produced by
882:"Supernova Has Energy of Hundreds of Billions of Suns"
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211:. Other hypotheses include: gravitational lensing; a
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lines, but two very broad absorption bands. Ionised
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1120:Superluminous Supernova Is The Brightest Ever Seen
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937:"Astronomers spot brightest supernova in history"
497:Monthly Notices of the Royal Astronomical Society
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16:2015 hypernova event in the constellation Indus
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735:"Found: The Most Powerful Supernova Ever Seen"
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438:One unusual explanation for ASASSN-15lh is a
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1771:Monte Agliale Supernovae and Asteroid Survey
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79:â61° 39′ 34.64″
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828:"Most-luminous supernova ever discovered"
802:"Brightest Supernova Baffles Astronomers"
779:Central Bureau for Astronomical Telegrams
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260:Central Bureau of Astronomical Telegrams
2360:Astronomical objects discovered in 2015
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233:Cerro Tololo Inter-American Observatory
172:All Sky Automated Survey for SuperNovae
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880:Bhanoo, Sindya N. (January 15, 2016).
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362:. The mass of ASSASN-15lh is 40
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443:speculative and not widely accepted.
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1116:Breaking Science News | Sci-News.com
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174:(ASAS-SN), with the appearance of a
1766:Katzman Automatic Imaging Telescope
935:Thomson, Jason (January 14, 2016).
906:Boyle, Rebecca (January 14, 2016).
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771:Central Bureau Electronic Telegrams
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800:Young, Monica (January 15, 2016).
733:Billings, Lee (January 14, 2016).
672:Jessica Orwig (January 14, 2016).
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1551:History of supernova observation
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241:Southern African Large Telescope
197:(hypernova) ever observed, or a
553:Young, Monica (July 12, 2015).
394:to the amplifying effects of a
50:SLSNe (Type Ic), SNSLSN-I
1796:SuperNova Early Warning System
1211:Common envelope jets supernova
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195:most luminous type I supernova
120:APMUKS(BJ) B215839.70â615403.9
1:
941:The Christian Science Monitor
555:"The Most Luminous Supernova"
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1786:Supernova/Acceleration Probe
1761:High-Z Supernova Search Team
1359:pulsational pair-instability
447:Tidal disruption event (TDE)
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168:astronomical transient event
7:
2049:ASASSN-V J213939.3-702817.4
1791:Supernova Cosmology Project
1299:Fast blue optical transient
1077:10.3847/0004-637X/826/2/178
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166:) is an extremely luminous
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1892:Indus in Chinese astronomy
243:was used to determine the
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1015:10.1038/s41550-016-0002
715:10.1038/s41550-016-0002
640:10.1126/science.aac9613
408:superluminous supernova
402:Superluminous supernova
258:SN 2015L from the
209:supermassive black hole
176:superluminous supernova
1887:List of stars in Indus
1876:Constellation of Indus
1806:Texas Supernova Search
1781:Sloan Supernova Survey
1399:Luminous blue variable
289:of ASASSN-15lh in the
199:tidal disruption event
2375:Indus (constellation)
1251:Phillips relationship
528:10.1093/mnras/stw3237
467:gravitational lensing
461:Gravitational lensing
330:Ohio State University
299:bolometric luminosity
256:supernova designation
161:supernova designation
2090:LHS 3844 b (Kua'kua)
383:Suggested mechanisms
2303:Astronomical events
1824:Category:Supernovae
1756:CalĂĄn/Tololo Survey
1441:Population III star
1349:Soft gamma repeater
1181:Type Ib and Ic
1068:2016ApJ...826..178G
1007:2016NatAs...1E...2L
806:Sky & Telescope
787:2015CBET.4120....1D
740:Scientific American
632:2016Sci...351..257D
559:Sky & Telescope
519:2017MNRAS.466.1428G
23:
1834:Commons:Supernovae
1486:Stellar black hole
1462:Pulsar wind nebula
1314:Gravitational wave
886:The New York Times
287:absolute magnitude
170:discovered by the
136:Other designations
127:apparent magnitude
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1324:Luminous red nova
1236:Carbon detonation
616:(6270): 257â260.
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1719:
1710:Vela Remnant
1675:SN 1006
1640:SN 1000+0216
1618:Cassiopeia A
1587:Most distant
1518:Local Bubble
1491:Compact star
1469:Neutron star
1206:Calcium-rich
1171:Type Ia
1049:
1045:
988:
984:
977:
956:
944:. Retrieved
940:
915:. Retrieved
911:
901:
889:. Retrieved
885:
875:
850:
844:
832:. Retrieved
821:
809:. Retrieved
805:
795:
774:
770:
756:
744:. Retrieved
738:
706:
702:
695:
683:. Retrieved
677:
613:
607:
562:. Retrieved
558:
500:
496:
464:
450:
437:
427:neutron star
424:
412:
405:
386:
377:
355:70,000
353:
334:
291:AB magnitude
284:
281:
264:
249:
230:
192:
163:
156:
155:
105:0.2326
41:
18:
2321:GRB 100621A
2311:ASASSN-15lh
1720:ASASSN-15lh
1670:SN 185
1628:Crab Nebula
1523:Superbubble
1513:Zombie star
1496:electroweak
1426:White dwarf
1375:Progenitors
1339:Pulsar kick
946:January 15,
917:January 15,
891:January 16,
834:January 15,
811:January 16,
746:January 16,
604:Morrell, N.
564:January 16,
503:(2): 1428.
374:Host galaxy
351:at 0.2326.
272:ultraviolet
157:ASASSN-15lh
89:megaparsecs
75:Declination
38:light curve
35:visual band
22:ASASSN-15lh
2370:Supernovae
2365:Hypernovae
2354:Categories
2316:GRB 060614
2280:Abell 3742
2249:ESO 235-58
2082:Exoplanets
1735:SN 2022jli
1730:SN 2018cow
1597:In fiction
1572:Candidates
1546:Guest star
1404:Supergiant
1382:Hypergiant
1344:Quark-nova
1246:Near-Earth
1229:Physics of
1157:Supernovae
1059:1511.01471
1052:(2): 178.
998:1609.02927
968:1611.03657
830:. phys.org
763:N. Morrell
623:1507.03010
510:1605.00645
474:References
440:quark-nova
434:Quark nova
278:Properties
223:spindown.
213:quark nova
68:22 2 15.45
2244:ESO 146-5
2095:Δ Indi Ab
1635:iPTF14hls
1539:Discovery
1329:Micronova
1278:Neutrinos
1271:Îł-process
1266:r-process
1261:p-process
1241:Foe/Bethe
1191:Hypernova
1110:Space.com
1103:Astronomy
1086:119159928
867:182077393
685:March 22,
537:119253925
392:nickel-56
345:magnesium
307:Milky Way
303:iPTF13ajg
227:Discovery
215:inside a
188:PS1-10adi
2341:Category
2114:Galaxies
2100:Ï Indi b
2054:LHS 3844
2002:Variable
1744:Research
1650:Kepler's
1592:Remnants
1479:magnetar
1450:Remnants
1354:Imposter
1319:Kilonova
1023:73645264
991:: 0002.
656:31444274
648:26816375
421:Magnetar
396:magnetar
389:decaying
367:☉
360:☉
349:redshift
337:hydrogen
245:redshift
221:magnetar
206:☉
164:SN 2015L
139:SN 2015L
101:Redshift
84:Distance
2254:IC 5152
2064:WASP-88
2059:WASP-46
1751:ASAS-SN
1645:Tycho's
1623:SN 1054
1606:Notable
1577:Notable
1287:Related
1164:Classes
1064:Bibcode
1003:Bibcode
783:Bibcode
628:Bibcode
609:Science
515:Bibcode
293:system
1501:exotic
1474:pulsar
1419:yellow
1387:yellow
1294:Failed
1122:Forbes
1084:
1021:
865:
851:Nature
654:
646:
535:
341:helium
322:joules
295:u band
87:1,171
42:et al.
2237:Other
2042:Other
1911:Bayer
1902:Stars
1565:Lists
1506:quark
1082:S2CID
1054:arXiv
1019:S2CID
993:arXiv
963:arXiv
863:S2CID
781:: 1.
709:(1).
652:S2CID
618:arXiv
533:S2CID
505:arXiv
250:Swift
180:Indus
145:[
125:Peak
92:3.82
2228:7199
2223:7196
2218:7191
2213:7124
2208:7096
2203:7090
2198:7083
2193:7064
2188:7061
2183:7049
2171:7041
2166:7038
2161:7029
2156:7022
2151:7014
2146:7007
2141:7004
2136:7002
2131:6984
2033:8331
2028:8269
1409:blue
1334:Nova
948:2016
919:2016
893:2016
836:2016
813:2016
775:4120
748:2016
687:2016
644:PMID
566:2016
131:16.9
117:Host
2123:NGC
1414:red
1392:Red
1072:doi
1050:826
1011:doi
855:doi
711:doi
636:doi
614:351
523:doi
501:466
339:or
328:of
315:1.1
311:Sun
2356::
2020:HR
1919:α
1080:.
1070:.
1062:.
1048:.
1044:.
1017:.
1009:.
1001:.
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939:.
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773:.
769:.
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723:^
705:.
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664:^
650:.
642:.
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626:.
612:.
574:^
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545:^
531:.
521:.
513:.
499:.
495:.
482:^
370:]
319:10
262:.
190:.
33:A
2176:B
2010:T
1992:Ï
1987:Ï
1982:Îż
1977:Ό
1972:Îș
1967:Îș
1962:Îč
1957:Ξ
1952:η
1947:ζ
1942:Δ
1937:ÎŽ
1932:Îł
1927:ÎČ
1868:e
1861:t
1854:v
1149:e
1142:t
1135:v
1088:.
1074::
1066::
1056::
1025:.
1013::
1005::
995::
989:1
971:.
965::
950:.
921:.
895:.
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857::
838:.
815:.
789:.
785::
750:.
717:.
713::
707:1
689:.
658:.
638::
630::
620::
568:.
539:.
525::
517::
507::
364:M
357:R
317:Ă
203:M
159:(
149:]
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