Correction: Corrigendum: The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole

Leloudas, G.; Fraser, M.; Stone, Nicholas C.; Velzen, S. van; Jonker, P. G.; Arcavi, I.; Fremling, C.; Maund, Justyn R.; Smartt, S. J.; Krìhler, T.; Miller-Jones, J. C. A.; Vreeswijk, P. M.; Gal‐Yam, A.; Mazzali, P. A.; De, A.; Howell, D. A.; Inserra, C.; Patat, F.; Postigo, A. de Ugarte; Yaron, O.; Ashall, C.; Bar, I.; Campbell, H.; Chen, Ting-Wan; Childress, M.; Elias‐Rosa, N.; Harmanen, J.; Hosseinzadeh, G.; Johansson, Joel; Kangas, T.; Kankare, E.; Kim, S.; Kuncarayakti, H.; Lyman, John; Magee, M.; Maguire, K.; Malesani, D.; Mattila, S.; McCully, C.; Nicholl, M.; Prentice, S.; Romero-Cañizales, C.; Schulze, S.; Smith, K. W.; Sollerman, J.; Sullivan, M. K.; Tucker, B.; Valenti, S.; Wheeler, J. C.; Young, D. R.

doi:10.1038/s41550-016-0034

Cited by 6 publications

(4 citation statements)

References 63 publications

(92 reference statements)

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“…Important reasons for this are the bright limit of ASAS-SN (m < 17 mag) and the manageable detection rate, allowing for near spectroscopic completeness (Brown et al 2019) and, thus, no selection bias in spectroscopically following-up and classifying transients. In the first two years of the ASAS-SN survey, they discovered four TDEs: ASASSN-14ae (Holoien et al 2014), ASASSN-14li (Holoien et al 2016b), ASASSN-15lh (Dong et al 2016, Leloudas et al 2016, and ASASSN-15oi (Holoien et al 2016a). The bright, nearby TDEs discovered by ASAS-SN allow for high signal-to-noise multiwavelength follow-up and spectroscopic monitoring.…”

Section: Optical Candidatesmentioning

confidence: 99%

“…However, a star could be disrupted outside the event horizon for this black hole mass if it was either a maximally spinning (Kerr) black hole or the star was massive (M > M ࣻ ). However, given the old stellar population of the host galaxy measured from stellar population synthesis fits to its SED, a spinning black hole was favored (Leloudas et al 2016). Furthermore, given that the tidal disruption radius, fallback timescale, and peak mass accretion rate have dependencies on black hole mass, one would expect the properties of the TDE flares to correlate with M BH .…”

Section: Correlations (Or Lack Thereof ) With Central Black Hole Massmentioning

confidence: 99%

See 1 more Smart Citation

Tidal Disruption Events

Gezari

2021

Annu. Rev. Astron. Astrophys.

189

124

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The concept of stars being tidally ripped apart and consumed by a massive black hole (MBH) lurking in the center of a galaxy first captivated theorists in the late 1970s. The observational evidence for these rare but illuminating phenomena for probing otherwise dormant MBHs first emerged in archival searches of the soft X-ray ROSAT All-Sky Survey in the 1990s, but has recently accelerated with the increasing survey power in the optical time domain, with tidal disruption events (TDEs) now regarded as a class of optical nuclear transients with distinct spectroscopic features. Multiwavelength observations of TDEs have revealed panchromatic emission, probing a wide range of scales, from the innermost regions of the accretion flow to the surrounding circumnuclear medium. I review the current census of 56 TDEs reported in the literature, and their observed properties can be summarized as follows: ▪ The optical light curves follow a power-law decline from peak that scales with the inferred central black hole mass as expected for the fallback rate of the stellar debris, but the rise time does not. ▪ The UV-optical and soft X-ray thermal emission come from different spatial scales, and their intensity ratio has a large dynamic range and is highly variable, providing important clues as to what is powering the two components. ▪ They can be grouped into three spectral classes, and those with Bowen fluorescence line emission show a preference for a hotter and more compact line-emitting region, whereas those with only Heii emission lines are the rarest class. Expected final online publication date for the Annual Review of Astronomy and Astrophysics, Volume 59 is August 2021. Please see http://www.annualreviews.org/page/journal/pubdates for revised estimates.

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Section: Optical Candidatesmentioning

confidence: 99%

Section: Correlations (Or Lack Thereof ) With Central Black Hole Massmentioning

confidence: 99%

Tidal Disruption Events

Gezari

2021

Annu. Rev. Astron. Astrophys.

189

124

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“…We compile all spectroscopically confirmed CCSN discovered by ASAS-SN (2013Holoien et al 2017aHoloien et al ,b,c, 2019, adopting any SN classifications and redshift estimates which were updated since the initial classification was made. There are two exceptions, both of which were claimed to be SLSN: ASAS-SN 15lh was classified as a SLSN-I (Dong et al 2016), but was omitted from the CCSN sample since it is not well understood whether this event is a SLSN or a tidal disruption event (Leloudas et al 2016;Margutti et al 2017) and ASAS-SN 17jz was re-classified as a SLSN-II, but its classification is ambiguous; it could be a very luminous SN-II (Xhakaj et al 2017) or alternatively it could be an AGN (Arcavi et al 2017). In any case, these events are not 'typical' CCSNe and we exclude them from the CCSN sample.…”

Section: Core Collapse Supernovaementioning

confidence: 99%

Core-collapse, superluminous, and gamma-ray burst supernova host galaxy populations at low redshift: the importance of dwarf and starbursting galaxies

Taggart,

Perley

2019

Preprint

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We present a comprehensive study of an unbiased sample of 84 nearby ( z = 0.016) corecollapse supernova (CCSN) host galaxies drawn from the All-Sky Automated Survey for Supernovae (ASAS-SN) for direct comparison to the nearest LGRB and SLSN hosts. We use public imaging surveys to gather multi-wavelength photometry for all CCSN host galaxies and fit their spectral energy distributions (SEDs) to derive stellar masses and integrated star formation rates. CCSNe populate galaxies across a wide range of stellar masses, from blue and compact dwarf galaxies to large spiral galaxies. We find 40 +6 5 per cent of CCSNe are in dwarf galaxies (M * < 10 9 M ) and 2 +3 1 per cent are in dwarf starburst galaxies (sSFR > 10 −8 yr −1 ). We reanalyse low-redshift SLSN and LGRB hosts from the literature (out to z < 0.3) in a homogeneous way and compare against the CCSN host sample. We find that the relative SLSN to CCSN supernova rate is increased in low-mass galaxies and at high specific starformation rates. These parameters are strongly covariant and we cannot break the degeneracy between them with our current sample. Larger unbiased samples of CCSNe from projects such as ZTF and LSST will be needed to determine whether host-galaxy mass (a proxy for metallicity) or specific star-formation rate (a proxy for star-formation intensity and potential IMF variation) is more fundamental in driving the preference for SLSNe and LGRBs in unusual galaxy environments.

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“…Given the peculiar nature of ASASSN-15lh (Dai et al 2015;Metzger et al 2015;Bersten et al 2016;Chatzopoulos et al 2016;Dong et al 2016;Godoy-Rivera et al 2017;Kozyreva et al 2016;Leloudas et al 2016;Sukhbold & Woosley 2016;van Putten & Della Valle 2017;Margutti et al 2017a), this transient is not part of the sample of bona fide SLSNe-I analyzed here. However, we discuss and compare the X-ray properties of ASASSN-15lh in the context of SLSNe-I in Section 4, 5.1 and 5.2.…”

Section: X-ray Observations and Analysismentioning

confidence: 99%

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

Margutti

Chornock

Metzger

et al. 2018

ApJ

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We present the results from a sensitive X-ray survey of 26 nearby hydrogen-poor superluminous supernovae (SLSNe-I) with Swift, Chandra, and XMM. This data set constrains the SLSN evolution from a few days until ∼2000 days after explosion, reaching a luminosity limit L x ∼10 40 erg s −1 and revealing the presence of significant X-ray emission possibly associated with PTF 12dam. No SLSN-I is detected above L 10 erg s-, suggesting that the luminous X-ray emission L x ∼10 45 erg s −1 associated with SCP 60F6 is not common among SLSNe-I. We constrain the presence of off-axis gamma-ray burst (GRB) jets, ionization breakouts from magnetar engines and the density in the sub-parsec environments of SLSNe-I through inverse Compton emission. The deepest limits rule out the weakest uncollimated GRB outflows, suggesting that if the similarity of SLSNe-I with GRB/SNe extends to their fastest ejecta, then SLSNe-I are either powered by energetic jets pointed far away from our line of sight (θ>30°), or harbor failed jets that do not successfully break through the stellar envelope. Furthermore, if a magnetar central engine is responsible for the exceptional luminosity of SLSNe-I, our X-ray analysis favors large magnetic fields B 2 10 14 >´G and ejecta masses M M 3 ej > ☉ , in agreement with optical/UV studies. Finally, we constrain the pre-explosion mass-loss rate of stellar progenitors of SLSNe-I. For PTF 12dam we infer M M 2 10 yr 5 1 <´--☉, suggesting that the SN shock interaction with an extended circumstellar medium is unlikely to supply the main source of energy powering the optical transient and that some SLSN-I progenitors end their lives as compact stars surrounded by a low-density medium similar to long GRBs and type Ib/c SNe.

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Correction: Corrigendum: The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole

Cited by 6 publications

References 63 publications

Tidal Disruption Events

Tidal Disruption Events

Core-collapse, superluminous, and gamma-ray burst supernova host galaxy populations at low redshift: the importance of dwarf and starbursting galaxies

Results from a Systematic Survey of X-Ray Emission from Hydrogen-poor Superluminous SNe

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