DISCOVERY OF AN OUTFLOW FROM RADIO OBSERVATIONS OF THE TIDAL DISRUPTION EVENT ASASSN-14li

Alexander, K. D.; Berger, E.; Guillochon, James; Zauderer, B. A.; Williams, Peter K. G.

doi:10.3847/2041-8205/819/2/l25

Cited by 225 publications

(337 citation statements)

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“…At a distance of 73 Mpc, this corresponds to a luminosity L ν = (7.7 ± 0.4) × 10 27 erg s −1 Hz −1 . This is slightly lower than the radio luminosity of the nearby thermal TDE ASSASN-14li (likely produced by a non-relativistic outflow; Alexander et al 2016;van Velzen et al 2016), an order of magnitude below the radio luminosity of the candidate TDE IGR J12580+0134 (possibly due to an off-axis jet; Irwin et al 2015;Lei et al 2016), and several orders of magnitude below the radio luminosities of relativistic TDEs like Swift J164449.3+573451 (ascribed to an on-axis relativistic jet; Zauderer et al 2011). Additional radio observations of XMMSL1 J0740-85 are planned and the time-evolution of the emission will be discussed in a future paper (Alexander et al, in prep.…”

Section: Radio Observationmentioning

confidence: 89%

“…However, the detection of spectral features around 6 keV, whether due to intrinsic absorption or ionised reflection, are more suggestive of non-jetted intrinsic emission. In this context the radio emission could be interpreted as a non-relativistic outflow akin to that seen in ASSASN-14li (Alexander et al 2016). The nature of the radio emission in XMMSL1 J0740-85 will be explored further in Alexander et al (in prep.…”

Section: Discussionmentioning

confidence: 99%

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XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

Saxton

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Komossa

et al. 2017

A&A

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Aims. We study X-ray bright tidal disruption events (TDE), close to the peak of their emission, with the intention of understanding the evolution of their light curves and spectra. Methods. Candidate TDE are identified by searching for soft X-ray flares from non-active galaxies in recent XMM-Newton slew data. Results. In April 2014, X-ray emission was detected from the galaxy XMMSL1 J074008.2-853927 (a.k.a. 2MASX 07400785-8539307), a factor 20 times higher than an upper limit from 20 years earlier. Both the X-ray and UV flux subsequently fell, by factors of 70 and 12 respectively. The bolometric luminosity peaked at L bol ∼ 2 × 10 44 ergs s −1 with a spectrum that may be modelled with thermal emission in the UV band, a power-law with Γ ∼ 2 dominating in the X-ray band above 2 keV and a soft X-ray excess with an effective temperature of ∼86 eV. Rapid variability locates the X-ray emission to within <73 R g of the nuclear black hole. Radio emission of flux density ∼1 mJy, peaking at 1.5 GHz was detected 21 months after discovery. Optical spectra indicate that the galaxy, at a distance of 73 Mpc (z = 0.0173), underwent a starburst 2 Gyr ago and is now quiescent. We consider a tidal disruption event to be the most likely cause of the flare. If this proves to be correct then this is a very clean example of a disruption exhibiting both thermal and non-thermal radiation.

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Section: Radio Observationmentioning

confidence: 89%

Section: Discussionmentioning

confidence: 99%

XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

Saxton

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Komossa

et al. 2017

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“…It is believed that many tidal disruption events (TDEs) go through a super-Eddington phase at early times (Alexander et al 2016;Socrates 2012;Lodato & Rossi 2011;Rees 1988;Zauderer et al 2011). A sub-class of active galactic nuclei (AGN) in the local universe, known as Narrow Line Seyfert 1 galaxies, are likely close to the Eddington limit and in some cases probably super-Eddington (Jin et al 2016;Castelló-Mor et al 2016;Zubovas & King 2013;Kawakatu & Ohsuga 2011;Collin & Kawaguchi 2004).…”

Section: Introductionmentioning

confidence: 99%

Spectra of black hole accretion models of ultraluminous X-ray sources

Narayan

Sądowski

Soria

2017

Monthly Notices of the Royal Astronomical Society

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We present general relativistic radiation MHD simulations of super-Eddington accretion on a 10M black hole. We consider a range of mass accretion rates, black hole spins, and magnetic field configurations. We compute the spectra and images of the models as a function of viewing angle, and compare them with the observed properties of ultraluminous X-ray sources (ULXs). The models easily produce apparent luminosities in excess of 10 40 erg s −1 for pole-on observers. However, the angle-integrated radiative luminosities rarely exceed 2.5 × 10 39 erg s −1 even for mass accretion rates of tens of Eddington. The systems are thus radiatively inefficient, though they are energetically efficient when the energy output in winds and jets is also counted. The simulated models reproduce the main empirical types of spectra -disk-like, supersoft, soft, hard -observed in ULXs. The magnetic field configuration, whether MAD ("magnetically arrested disk") or SANE ("standard and normal evolution"), has a strong effect on the results. In SANE models, the X-ray spectral hardness is almost independent of accretion rate, but decreases steeply with increasing inclination. MAD models with non-spinning black holes produce significantly softer spectra at higher values ofṀ , even at low inclinations. MAD models with rapidly spinning black holes are quite different from all other models. They are radiatively efficient (efficiency factor ∼ 10 − 20%), super-efficient when the mechanical energy output is also included (70%), and produce hard blazar-like spectra. In all models, the emission shows strong geometrical beaming, which disagrees with the more isotropic illumination favoured by observations of ULX bubbles.

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“…The latter can be determined through measurements of the in-band spectrum and/or multi-wavelength SED. Thus the CNM density profile can be readily obtained (Berger et al 2012;Alexander et al 2016). …”

Section: Jet Dynamics and Cnm Density Structurementioning

confidence: 99%

Catching jetted tidal disruption events early in millimetre

Yuan

Wang

Lei

et al. 2016

Mon. Not. R. Astron. Soc.

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Relativistic jets can form from at least some tidal disruption events (TDEs) of (sub-)stellar objects around supermassive black holes. We detect the millimeter (MM) emission of IGR J12580+0134 -the nearest TDE known in the galaxy NGC 4845 at the distance of only 17 Mpc, based on Planck all-sky survey data. The data show significant flux jumps after the event, followed by substantial declines, in all six high frequency Planck bands from 100 GHz to 857 GHz. We further show that the evolution of the MM flux densities are well consistent with our model prediction from an off-axis jet, as was initially suggested from radio and X-ray observations. This detection represents the second TDE with MM detections; the other is Sw J1644+57, an on-axis jetted TDE at redshift of 0.35. Using the on-and off-axis jet models developed for these two TDEs as templates, we estimate the detection potential of similar events with the Large Millimeter Telescope (LMT) and the Atacama Large Millimeter/submillimeter Array (ALMA). Assuming an exposure of one hour, we find that the LMT (ALMA) can detect jetted TDEs up to redshifts z ∼ 1 (2), for a typical disrupted star mass of ∼ 1 M ⊙ . The detection rates of on-and off-axis TDEs can be as high as ∼ 0.6 (13) and 10 (220) per year, respectively, for the LMT (ALMA). We briefly discuss how such observations, together with follow-up radio monitoring, may lead to major advances in understanding the jetted TDEs themselves and the ambient environment of the CNM.

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DISCOVERY OF AN OUTFLOW FROM RADIO OBSERVATIONS OF THE TIDAL DISRUPTION EVENT ASASSN-14li

Cited by 225 publications

References 51 publications

XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

XMMSL1 J074008.2-853927: a tidal disruption event with thermal and non-thermal components

Spectra of black hole accretion models of ultraluminous X-ray sources

Catching jetted tidal disruption events early in millimetre

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