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LETTERS PUBLISHED: 12 DECEMBER 2016 | VOLUME: 1 | ARTICLE NUMBER: 0002 The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole G. Leloudas1,​2*, M. Fraser3, N. C. Stone4, S. van Velzen5, P. G. Jonker6,​7, I. Arcavi8,​9, C. Fremling10, J. R. Maund11, S. J. Smartt12, T. Krühler13, J. C. A. Miller-Jones14, P. M. Vreeswijk1, A. Gal-Yam1, P. A. Mazzali15,​16, A. De Cia17, D. A. Howell8,​18, C. Inserra12, F. Patat17, A. de Ugarte Postigo2,​19, O. Yaron1, C. Ashall15, I. Bar1, H. Campbell3,​20, T.-W. Chen13, M. Childress21, N. Elias-Rosa22, J. Harmanen23, G. Hosseinzadeh8,​18, J. Johansson1, T. Kangas23, E. Kankare12, S. Kim24, H. Kuncarayakti25,​26, J. Lyman27, M. R. Magee12, K. Maguire12, D. Malesani2, S. Mattila3,​23,​28, C. V. McCully8,​18, M. Nicholl29, S. Prentice15, C. Romero-Cañizales24,​25, S. Schulze24,​25, K. W. Smith12, J. Sollerman10, M. Sullivan21, B. E. Tucker30,​31, S. Valenti32, J. C. Wheeler33 and D. R. Young12 8 12,13 When a star passes within the tidal radius of a supermassive has a mass >10 M⊙ , a star with the same mass as the Sun black hole, it will be torn apart1. For a star with the mass of the could be disrupted outside the event horizon if the black hole 8 14 Sun (M⊙) and a non-spinning black hole with a mass <10 M⊙, were spinning rapidly . The rapid spin and high black hole the tidal radius lies outside the black hole event horizon2 and mass can explain the high luminosity of this event. the disruption results in a luminous flare3–6. Here we report ASASSN-15lh was discovered by the All-Sky Automated observations over a period of ten months of a transient, hith- Survey for Supernovae (ASAS-SN) on 14 June 2015 at a redshift of erto interpreted7 as a superluminous supernova8. Our data z =​ 0.2326. Its light curve peaked at V ≈​ 17 mag implying an abso- show that the transient rebrightened substantially in the lute magnitude of M =​ −​23.5 mag, more than twice as luminous ultraviolet and that the spectrum went through three differ- as any known supernova7. Our long-term spectroscopic follow-up ent spectroscopic phases without ever becoming nebular. Our reveals that ASASSN-15lh went through three different spectro- observations are more consistent with a tidal disruption event scopic phases (Fig. 1). During the first phase7, the spectra were than a superluminous supernova because of the temperature dominated by two broad absorption features. While these features evolution6, the presence of highly ionized CNO gas in the line appear similar to those observed in superluminous supernovae of sight9 and our improved localization of the transient in the (SLSNe; Supplementary Fig. 1), their physical origin is different. nucleus of a passive galaxy, where the presence of massive The features in SLSNe are due to O II8,15, but this would produce stars is highly unlikely10,11. While the supermassive black hole an additional strong feature at ∼4,400​ Å (Supplementary Fig. 2). 1Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel. 2Dark Cosmology Centre, Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, 2100 Copenhagen, Denmark. 3Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK. 4Columbia Astrophysics Laboratory, Columbia University, New York, New York 10027, USA. 5Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, Maryland 21218, USA. 6SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA, Utrecht, The Netherlands. 7Department of Astrophysics/IMAPP, Radboud University Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands. 8Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive Suite 102 Goleta, California 93117, USA. 9Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA. 10Department of Astronomy, The Oskar Klein Center, Stockholm University, AlbaNova, 10691, Stockholm, Sweden. 11Department of Physics and Astronomy, The University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK. 12Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast BT7 1NN, UK. 13Max-Planck-Institut für extraterrestrische Physik, Giessenbachstraße, 85748 Garching, Germany. 14International Centre for Radio Astronomy Research, Curtin University, GPO Box U1987, Perth, Western Australia 6845, Australia. 15Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK. 16Max-Planck Institut für Astrophysik, Karl-Schwarzschild-Strasse 1, 85748 Garching, Germany. 17European Southern Observatory, Karl-Schwarzschild-Strasse 2, 85748 Garching, Germany. 18Department of Physics, University of California Santa Barbara, Santa Barbara, California 93117, USA. 19Instituto de Asfrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, E-18008, Granada, Spain. 20Department of Physics, University of Surrey, Guildford GU2 7XH, UK. 21Department of Physics & Astronomy, University of Southampton, Southampton SO171BJ, UK. 22INAF - Osservatorio Astronomico di Padova, Vicolo dellOsservatorio 5, 35122 Padova, Italy. 23Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland. 24Instituto de Asrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile. 25Millennium Institute of Astrophysics, Nuncio Monseñor Sótero Sanz 100, Providencia, Santiago, 7500011, Chile. 26Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile. 27Department of Physics, University of Warwick, Coventry CV4 7AL, UK. 28Finnish Centre forAstronomy with ESO (FINCA), University of Turku, Väisäläntie 20, FI-21500 Piikkiö, Finland. 29Harvard–Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, Massachusetts 02138, USA. 30The Research School of Astronomy and Astrophysics, Mount Stromlo Observatory, Australian National University, Canberra Australian Capital Territory 2611, Australia. 31ARC Centre of Excellence for All-sky Astrophysics (CAASTRO), Australia. 32Department of Physics, University of California, Davis, California 95616, USA. 33Department of Astronomy, University of Texas at Austin, Austin, Texas 78712, USA. *email: [email protected] NATURE ASTRONOMY 1, 0002 (2016) | DOI: 10.1038/s41550-016-0002 | www.nature.com/natureastronomy 1 © 2016 Macmillan Publishers Limited, part of Springer Nature. All rights reserved. LETTERS NATURE ASTRONOMY a b 16 Hα +37 17 –15 (normalized) 10 λ F 18 ) +91 –1 A –8 –4 0 48 –2 3 –1 v (10 km s ) 19 cm –1 +14 +16 20 i – 1.4 magnitude +21 r – 0.7 10–16 AB +27 V +37 21 V (ASASSN) +45 g + 0.5 +57 +75 B + 1.2 +89 22 U + 1.9 +91 log(flux) + constant (erg s UVW1 + 1.9 +104 UVM2 + 2.3 +126 23 –17 UVW2 + 2.6 10 +134 50 0 50 100 150 200 250 300 +157 – +248 Rest-frame days +256 3,000 4,000 5,000 6,000 7,000 Figure 2 | The light curve evolution of ASASSN-15lh in the rest frame. Rest-frame wavelength (Å) The data are from LCOGT (gri) and Swift (other filters), supplemented by the ASASSN V band data7. We have adopted a peak time at 5 June 2015 (MJD 7 Figure 1 | Spectral sequence of ASASSN-15lh showing three spectroscopic 57178.5) . The light curves are shifted for clarity as indicated in the legend. phases. a, The main spectral features during the different phases are Error bars represent 1σ uncertainties. The optical bands show a monotonic highlighted with different colours. The two most recent spectra appear decline, but the UV bands show a rebrightening after 60 rest-frame days. redder due to the increased host contamination. Rest-frame A significant secondary dip is also observed in the bluest bands around phases are indicated, the spectra have been offset for clarity and the day +​120. The photometry has been corrected for foreground extinction and the host contribution has been removed (see Methods). Earth symbols mark the strongest telluric features. b, Detection of Hα​ (FWHM ~2,500 km s−1) in a telluric-free region of our best spectra. The magenta line is a telluric spectrum. invariable, within the present errors. The velocity of the Hα​ line (full-width at half-maximum (FWHM) ∼​2,500 km s−1) is different The feature at ∼4,100​ Å cannot be easily identified in the tidal disrup- from those of other features, implying that it is formed in a different tion event (TDE) framework either. Two possibilities are that it could emitting region. be due to absorption of Mg ii or high-velocity He ii16. After the initial The light curve evolution of ASASSN-15lh is shown in Fig. 2. broad absorption features disappeared, the spectra of ASASSN-15lh After the initial peak and decline, around 10 September (day +​60), were dominated by two emission features. A possible identifica- the UV started rebrightening, an effect that was more prominent tion for these features is He ii λλ3,202 and 4,686 Å, which are both in the far-UV bands18,20,21. The dense photometric follow-up with consistently blue-shifted by ∼​15,000 km s−1 (Supplementary Fig. 3). the Swift Gamma-Ray Burst Mission (Swift) and the Las Cumbres He ii emission is commonly seen in optically discovered TDEs4,5 Observatory Global Telescope Network (LCOGT) revealed that at different blueshifts, albeit typically at lower velocities, but it has ASASSN-15lh reached a secondary UV maximum at around +​110 not been seen in H-poor SLSNe. These features disappeared after days, followed by another decline. Interestingly, after day +​100, the day +​75 (measured in rest frame from the peak) and the later spec- colours of ASASSN-15lh remained almost constant for over 120 tra were mostly featureless, with the exception of two emission rest-frame days (Supplementary Fig. 5). By fitting a black body to the features at ∼​4,000 and 5,200 Å. The spectra remained much bluer multiwavelength photometry of ASASSN-15lh, we are able to esti- than those of SLSNe17 for many months after the peak and never mate the temperature evolution, black-body radius and bolometric revealed nebular features, even up to day +​256.
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  • Tidal Disruption Events in Active Galactic Nuclei

    Tidal Disruption Events in Active Galactic Nuclei

    The Astrophysical Journal, 881:113 (14pp), 2019 August 20 https://doi.org/10.3847/1538-4357/ab2b40 © 2019. The American Astronomical Society. All rights reserved. Tidal Disruption Events in Active Galactic Nuclei Chi-Ho Chan1,2 , Tsvi Piran1 , Julian H. Krolik3 , and Dekel Saban1 1 Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel 2 School of Physics and Astronomy, Tel Aviv University, Tel Aviv 69978, Israel 3 Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218, USA Received 2019 April 27; revised 2019 June 18; accepted 2019 June 18; published 2019 August 20 Abstract A fraction of tidal disruption events (TDEs) occur in active galactic nuclei (AGNs) whose black holes possess accretion disks; these TDEs can be confused with common AGN flares. The disruption itself is unaffected by the disk, but the evolution of the bound debris stream is modified by its collision with the disk when it returns to pericenter. The outcome of the collision is largely determined by the ratio of the stream mass current to the azimuthal mass current of the disk rotating underneath the stream footprint, which in turns depends on the mass and luminosity of the AGN. To characterize TDEs in AGNs, we simulated a suite of stream–disk collisions with various mass current ratios. The collision excites shocks in the disk, leading to inflow and energy dissipation orders of magnitude above Eddington; however, much of the radiation is trapped in the inflow and advected into the black hole, so the actual bolometric luminosity may be closer to Eddington. The emergent spectrum may not be thermal, TDE-like, or AGN-like.
  • Progenitors of Gamma-Ray Bursts and Supernovae

    Progenitors of Gamma-Ray Bursts and Supernovae

    Progenitors of Gamma-Ray Bursts and Supernovae Chris Fryer (LANL) Types of supernova and GRBs Engines and their progenitor requirements Massive star progenitors and the circumstellar medium (single vs. binary) Specific examples – What have we learned? Supernova Types • Supernovae are distinguished by spectra and light curves. • Unfortunately, in core- collapse, the dividing lines are more like guidelines. • There are many “stand- outs” among these supernovae (e.g. SN87A). SN types - Rates • Core-collapse (Ib/c, II) SNe make up 75% of all supernovae. • Most Ib/c are Ic supernovae. • Plateau SNe make up most of the type II class. • New classes include Broad Line (tied to GRBs?) and Superluminous Supernova GRB Types • GRBs have been roughly Levan et al. (2013) divided into short/hard and long/ soft bursts. • A new class of ultra-long bursts have been discovered. Core-collapse Supernovae (Type II, Ib/c): Powered by SN Engines the potential energy released in collapse Source of convection (advective acoustic vs. Rayleigh Taylor), energy transport (neutrinos, pressure waves), role of magnetic fields. Massive Star Progenitors (binaries vs. single stars) Thermonuclear Supernovae Ignition site/sites White dwarf (double Degenerate vs. single degenerate) Possible Fates under the Convective Paradigm • Explosion within first ~200 ms, normal supernovae • Explosion delayed, weak supernova, considerable fallback (BH formation – Collapsar type II for rotating systems) • No explosion (BH Formation – Collapsar type I for rotating systems) Supernovae/Hypernovae Nomoto et al. (2003) EK (Jets!) Failed SN? 13M~15M BHAD GRB and Magnetar Engines Massive star Collapse (LGRB, very long GRB), only a very small fraction of massive stars (0.01-0.1% the supernova rate).