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Holoien, TWS, Neustadt, JMM, Vallely, PJ, Auchettl, K, Hinkle, JT, Romero-Cañizales, C, Shappee, BJ, Kochanek, CS, Stanek, KZ, Chen, P, Dong, S, Prieto, JL, Thompson, TA, Brink, TG, Filippenko, AV, Zheng, W, Bersier, D, Bose, S, Burgasser, AJ, Channa, S , De Jaeger, T, Hestenes, J, Im, M, Jeffers, B, Jun, HD, Lansbury, G, Post, RS, Ross, TW, Stern, D, Tang, K, Tucker, MA, Valenti, S, Yunus, S and Zhang, KD (2022) Investigating the Nature of the Luminous Ambiguous Nuclear Transient ASASSN-17jz. Astrophysical Journal, 933 (2). ISSN 0004-637X
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Investigating the nature of the luminous ambiguous nuclear transient ASASSN-17jz.pdf - Published Version Available under License Creative Commons Attribution. Download (8MB) | Preview |
Abstract
We present observations of the extremely luminous but ambiguous nuclear transient (ANT) ASASSN-17jz, spanning roughly 1200 days of the object's evolution. ASASSN-17jz was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN) in the galaxy SDSS J171955.84+414049.4 on UT 2017 July 27 at a redshift of z = 0.1641. The transient peaked at an absolute B-band magnitude of M B,peak = -22.81, corresponding to a bolometric luminosity of L bol,peak = 8.3 × 1044 erg s-1, and exhibited late-time ultraviolet emission that was still ongoing in our latest observations. Integrating the full light curve gives a total emitted energy of E tot = (1.36 ±0.08) × 1052 erg, with (0.80 ± 0.02) × 1052 erg of this emitted within 200 days of peak light. This late-time ultraviolet emission is accompanied by increasing X-ray emission that becomes softer as it brightens. ASASSN-17jz exhibited a large number of spectral emission lines most commonly seen in active galactic nuclei (AGNs) with little evidence of evolution. It also showed transient Balmer features, which became fainter and broader over time, and are still being detected >1000 days after peak brightness. We consider various physical scenarios for the origin of the transient, including supernovae (SNe), tidal disruption events, AGN outbursts, and ANTs. We find that the most likely explanation is that ASASSN-17jz was a SN IIn occurring in or near the disk of an existing AGN, and that the late-time emission is caused by the AGN transitioning to a more active state.
| Item Type: | Article |
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| Uncontrolled Keywords: | 0201 Astronomical and Space Sciences; 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics; 0306 Physical Chemistry (incl. Structural); Astronomy & Astrophysics |
| Subjects: | Q Science > QB Astronomy |
| Divisions: | Astrophysics Research Institute |
| Publisher: | American Astronomical Society |
| SWORD Depositor: | A Symplectic |
| Date Deposited: | 01 Nov 2022 10:03 |
| Last Modified: | 01 Nov 2022 10:15 |
| DOI or ID number: | 10.3847/1538-4357/ac74b9 |
| URI: | https://researchonline.ljmu.ac.uk/id/eprint/17983 |
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