 SN 2022jli on 3 July 2022 by ZTF | |
| Ic | |
| Date | May 5, 2022 |
|---|---|
| Constellation | Cetus |
| Right ascension | 00h 34m 45.694s[1] |
| Declination | −08° 23′ 12.16″[1] |
| Distance | 23 Mpc |
| Redshift | 0.005546[1] |
| Host | NGC 157 |
| Notable features | the only supernova that shows periodicity in its light curve |
| Peakapparent magnitude | 14 |
SN 2022jli is aType Ic supernova discovered in 2022 in thespiral galaxyNGC 157 at a distance of about 23 Mpc. Thelight curve of the supernova exhibited oscillations that are interpreted as an interaction of a companion star of the star that exploded with a compact object, probably aneutron star or ablack hole.[2]
SN 2022jli was discovered by astronomerLibert Monard [it] atKleinkaroo Observatory, who reported it to theTransient Name Server (TNS) on May 5, 2022, as AT 2022jli. The supernova was offset35.2″ north and15.88″ west of theNGC 157galactic core. It was independently detected by theAsteroid Terrestrial-impact Last Alert System (ATLAS) survey on May 16, 2022, and given the internal name ATLAS22oat. Due to an initial astrometric error in the TNS report, ATLAS incorrectly registered it as a separate object AT 2022jzy. This duplication was later removed from TNS records to confirm both discoveries as the same supernova SN 2022jli.[3]
Another supernova found in NGC 157 is SN 2009em.[3]
Photometry of SN 2022jli was obtained by theZwicky Transient Facility (internal name ZTF22aapubuy), ESA'sGaia space telescope (internal name Gaia22cbu),ASAS-SN,Liverpool Telescope,Las Cumbres Observatory, and theNeil Gehrels Swift Observatory. A single radio observation was made withMERLIN.[3]
The extensivephotometric observations reveal periodic undulations or bumps in the declininglight curve with a period of 12.5 ± 0.2 days. This repeating pattern of oscillations is observed across multiple filters and instruments over many cycles, the first unambiguous detection of periodicity in a supernova light curve. SN 2022jli displays an extreme early excess in luminosity that declines over about 25 days before rising to the main peak. The total rise time to maximum brightness is ≥59 days, much longer than typical for stripped-envelope core-collapse supernovae. At peak luminosity of 10^42.1 erg/s, SN 2022jli is within the normal brightness range for Type Ic supernovae. Simple light curve modeling indicates a large ejecta mass around 12 ± 6solar masses. Spectra show features typical of Type Ic supernovae, with iron, calcium and sodium P Cygni profiles. The velocities derived from Fe II lines are initially high at 8500 km/s but decline slowly over time. The source of the early excess and periodic oscillations is uncertain, but plausible explanations include interaction of the ejecta with circumstellar material or a binary companion star. The periodicity may arise from concentric shells of CSM or repeated episodes of accretion onto a compact object.[3]
Material was adapted from this source, which is available under aCreative Commons Attribution 4.02022 in space | ||
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