WFRF:(Ihanec N.)
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 04003naa a2200709 4500 | |
| 001 | oai:DiVA.org:su-188182 | |
| 003 | SwePub | |
| 008 | 201230s2020 | |||||||||||000 ||eng| | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1881822 URI |
| 024 | 7 | a https://doi.org/10.1093/mnras/staa20652 DOI |
| 040 | a (SwePub)su | |
| 041 | a engb eng | |
| 042 | 9 SwePub | |
| 072 | 7 | a ref2 swepub-contenttype |
| 072 | 7 | a art2 swepub-publicationtype |
| 100 | 1 | a Short, P.4 aut |
| 245 | 1 0 | a The tidal disruption event AT2018hyz-I. Double-peaked emission lines and a flat Balmer decrement |
| 264 | c 2020-09-02 | |
| 264 | 1 | b Oxford University Press (OUP),c 2020 |
| 338 | a print2 rdacarrier | |
| 520 | a We present results from spectroscopic observations of AT 2018hyz, a transient discovered by the All-Sky Automated Survey for Supernova survey at an absolute magnitude of M-V similar to -20.2 mag, in the nucleus of a quiescent galaxy with strong Balmer absorption lines. AT 2018hyz shows a blue spectral continuum and broad emission lines, consistent with previous TDE candidates. High cadence follow-up spectra show broad Balmer lines and He I in early spectra, with He II making an appearance after similar to 70-100 d. The Balmer lines evolve from a smooth broad profile, through a boxy, asymmetric double-peaked phase consistent with accretion disc emission, and back to smooth at late times. The Balmer lines are unlike typical active galactic nucleus in that they show a flat Balmer decrement (H alpha/H beta similar to 1.5), suggesting the lines are collisionally excited rather than being produced via photoionization. The flat Balmer decrement together with the complex profiles suggests that the emission lines originate in a disc chromosphere, analogous to those seen in cataclysmic variables. The low optical depth of material due to a possible partial disruption may be what allows us to observe these double-peaked, collisionally excited lines. The late appearance of He II may be due to an expanding photosphere or outflow, or late-time shocks in debris collisions. | |
| 650 | 7 | a NATURVETENSKAPx Fysik0 (SwePub)1032 hsv//swe |
| 650 | 7 | a NATURAL SCIENCESx Physical Sciences0 (SwePub)1032 hsv//eng |
| 653 | a black hole physics | |
| 653 | a galaxies: active | |
| 653 | a galaxies: individual: AT 2018hyz | |
| 653 | a transients: tidal disruption events | |
| 700 | 1 | a Nicholl, M.4 aut |
| 700 | 1 | a Lawrence, A.4 aut |
| 700 | 1 | a Gomez, S.4 aut |
| 700 | 1 | a Arcavi, I.4 aut |
| 700 | 1 | a Wevers, T.4 aut |
| 700 | 1 | a Leloudas, G.4 aut |
| 700 | 1 | a Schulze, S.4 aut |
| 700 | 1 | a Anderson, J. P.4 aut |
| 700 | 1 | a Berger, E.4 aut |
| 700 | 1 | a Blanchard, P. K.4 aut |
| 700 | 1 | a Burke, J.4 aut |
| 700 | 1 | a Castro Segura, N.4 aut |
| 700 | 1 | a Charalampopoulos, P.4 aut |
| 700 | 1 | a Chornock, R.4 aut |
| 700 | 1 | a Galbany, L.4 aut |
| 700 | 1 | a Gromadzki, M.4 aut |
| 700 | 1 | a Herzog, L. J.4 aut |
| 700 | 1 | a Hiramatsu, D.4 aut |
| 700 | 1 | a Horne, Keith4 aut |
| 700 | 1 | a Hosseinzadeh, G.4 aut |
| 700 | 1 | a Howell, D. Andrew4 aut |
| 700 | 1 | a Ihanec, N.4 aut |
| 700 | 1 | a Inserra, C.4 aut |
| 700 | 1 | a Kankare, E.4 aut |
| 700 | 1 | a Maguire, K.4 aut |
| 700 | 1 | a McCully, C.4 aut |
| 700 | 1 | a Müller Bravo, T. E.4 aut |
| 700 | 1 | a Onori, F.4 aut |
| 700 | 1 | a Sollerman, Jesperu Stockholms universitet,Institutionen för astronomi,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)solle |
| 700 | 1 | a Young, D. R.4 aut |
| 710 | 2 | a Stockholms universitetb Institutionen för astronomi4 org |
| 773 | 0 | t Monthly notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 498:3, s. 4119-4133q 498:3<4119-4133x 0035-8711x 1365-2966 |
| 856 | 4 | u https://academic.oup.com/mnras/article-pdf/498/3/4119/33787392/staa2065.pdf |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-188182 |
| 856 | 4 8 | u https://doi.org/10.1093/mnras/staa2065 |
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