SN 2022jli

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SN 2022jli
SN 2022jli image ZTF-sci-20220703459132-zg-size-7.0arcmin.png
SN 2022jli on 3 July 2022 by ZTF
Ic
DateMay 5, 2022
Constellation Cetus
Right ascension 00h 34m 45.694s [1]
Declination −08° 23 12.16 [1]
Distance23 Mpc
Redshift 0.005546 [1]
Host NGC 157
Notable featuresthe only supernova that shows periodicity in its light curve
Peak apparent magnitude 14

SN 2022jli is a Type Ic supernova discovered in 2022 in the spiral galaxy NGC 157 at a distance of about 23 Mpc. The light 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 a neutron star or a black hole. [2]

Contents

Discovery

Top: multicolor extinction-corrected light curves of SN 2022jli including photometric errors. Black lines along the bottom of the plot indicate spectroscopic observations. Open symbols are synthetic photometry performed on the EFOSC2 spectrum. Bottom: light curves after detrending with a second-degree polynomial fit including only the region after maximum light (vertical dashed line). Light curves of SN 2022jli.jpg
Top: multicolor extinction-corrected light curves of SN 2022jli including photometric errors. Black lines along the bottom of the plot indicate spectroscopic observations. Open symbols are synthetic photometry performed on the EFOSC2 spectrum. Bottom: light curves after detrending with a second-degree polynomial fit including only the region after maximum light (vertical dashed line).

SN 2022jli was discovered by astronomer Libert Monard  [ it ] at Kleinkaroo Observatory, who reported it to the Transient Name Server (TNS) on May 5, 2022, as AT 2022jli. The supernova was offset 35.2 north and 15.88″ west of the NGC 157 galactic core. It was independently detected by the Asteroid 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]

Observations

Photometry of SN 2022jli was obtained by the Zwicky Transient Facility (internal name ZTF22aapubuy), ESA's Gaia space telescope (internal name Gaia22cbu), ASAS-SN, Liverpool Telescope, Las Cumbres Observatory, and the Neil Gehrels Swift Observatory. A single radio observation was made with MERLIN. [3]

The extensive photometric observations reveal periodic undulations or bumps in the declining light 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 ± 6 solar 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]

Related Research Articles

<span class="mw-page-title-main">Supernova</span> Explosion of a star at its end of life

A supernova is a powerful and luminous explosion of a star. A supernova occurs during the last evolutionary stages of a massive star, or when a white dwarf is triggered into runaway nuclear fusion. The original object, called the progenitor, either collapses to a neutron star or black hole, or is completely destroyed to form a diffuse nebula. The peak optical luminosity of a supernova can be comparable to that of an entire galaxy before fading over several weeks or months.

<span class="mw-page-title-main">SN 1987A</span> 1987 supernova event in the constellation Dorado

SN 1987A was a type II supernova in the Large Magellanic Cloud, a dwarf satellite galaxy of the Milky Way. It occurred approximately 51.4 kiloparsecs from Earth and was the closest observed supernova since Kepler's Supernova in 1604. Light and neutrinos from the explosion reached Earth on February 23, 1987 and was designated "SN 1987A" as the first supernova discovered that year. Its brightness peaked in May of that year, with an apparent magnitude of about 3.

Timeline of neutron stars, pulsars, supernovae, and white dwarfs

<span class="mw-page-title-main">Messier 74</span> Face-on spiral galaxy in the constellation Pisces

Messier 74 is a large spiral galaxy in the equatorial constellation Pisces. It is about 32 million light-years away from Earth. The galaxy contains two clearly defined spiral arms and is therefore used as an archetypal example of a grand design spiral galaxy. The galaxy's low surface brightness makes it the most difficult Messier object for amateur astronomers to observe. Its relatively large angular size and the galaxy's face-on orientation make it an ideal object for professional astronomers who want to study spiral arm structure and spiral density waves. It is estimated that M74 hosts about 100 billion stars.

<span class="mw-page-title-main">History of supernova observation</span> Ancient and modern recorded observations of supernovae explosions

The known history of supernova observation goes back to 1006 AD. All earlier proposals for supernova observations are speculations with many alternatives.

<span class="mw-page-title-main">SN 2008ax</span> 2008 supernova event in constellation Canes Venatici

SN 2008ax was a helium-rich type Ib core-collapse supernova in the interacting galaxy NGC 4490. It was independently discovered on 3 March 2008 by LOSS and 4 March by Koichi Itagaki. The site had been monitored six hours before discovery, thus constraining the time of the explosion breakout. It was the third-brightest supernova of 2008. The brightness in the B-band peaked about 20 days after the explosion. X-ray emissions were detected from the event, which are most likely the result of shock heating from the supernova ejecta and circumstellar material.

<span class="mw-page-title-main">NGC 7424</span> Galaxy in the constellation Grus

NGC 7424 is a barred spiral galaxy located 37.5 million light-years away in the southern constellation Grus. Its size makes it similar to our own galaxy, the Milky Way. It is called a "grand design" galaxy because of its well defined spiral arms. Two supernovae and two ultraluminous X-ray sources have been discovered in NGC 7424.

<span class="mw-page-title-main">Type Iax supernova</span> Dwarf star remnant of a supernova

A type Iax supernova is a rare subtype of type Ia supernova, which leaves behind a remnant star, known as zombie star, rather than completely dispersing the white dwarf. Type Iax supernovae are similar to type Ia, but have a lower ejection velocity and lower luminosity. Type Iax supernovae may occur at a rate between 5 and 30 percent of the Ia supernova rate. Thirty supernovae have been identified in this category.

<span class="mw-page-title-main">NGC 157</span> Galaxy in the constellation Cetus

NGC 157 is an intermediate spiral galaxy in the constellation of Cetus, positioned about 4° east of the star Iota Ceti. This galaxy can be viewed from suburban skies using a moderate-sized telescope. It was discovered on December 13, 1783 by William Herschel. The compiler of the New General Catalogue, John Louis Emil Dreyer noted that NGC 157 was "pretty bright, large, extended, between 2 considerably bright stars". It is a relatively isolated galaxy; the nearest other galaxy of comparable luminosity lies at a separation of 4.2 Mly (1.3 Mpc).

<span class="mw-page-title-main">Hypernova</span> Supernova that ejects a large mass at unusually high velocity

A hypernova is a very energetic supernova which is believed to result from an extreme core-collapse scenario. In this case, a massive star collapses to form a rotating black hole emitting twin astrophysical jets and surrounded by an accretion disk. It is a type of stellar explosion that ejects material with an unusually high kinetic energy, an order of magnitude higher than most supernovae, with a luminosity at least 10 times greater. Hypernovae release so much of gamma rays they usually appear similar to a type Ic supernova, but with unusually broad spectral lines indicating an extremely high expansion velocity. Hypernovae are one of the mechanisms for producing long gamma ray bursts (GRBs), which range from 2 seconds to over a minute in duration. They have also been referred to as superluminous supernovae, though that classification also includes other types of extremely luminous stellar explosions that have different origins.

<span class="mw-page-title-main">SN 2018cow</span> Supernova event of June 2018 in the constellation Hercules

SN 2018cow was a very powerful astronomical explosion, 10–100 times brighter than a normal supernova, spatially coincident with galaxy CGCG 137-068, approximately 200 million ly (60 million pc) distant in the Hercules constellation. It was discovered on 16 June 2018 by the ATLAS-HKO telescope, and had generated significant interest among astronomers throughout the world. Later, on 10 July 2018, and after AT 2018cow had significantly faded, astronomers, based on follow-up studies with the Nordic Optical Telescope (NOT), formally described AT 2018cow as SN 2018cow, a type Ib supernova, showing an "unprecedented spectrum for a supernova of this class"; although others, mostly at first but also more recently, have referred to it as a type Ic-BL supernova. An explanation to help better understand the unique features of AT 2018cow has been presented. AT2018cow is one of the few reported Fast Blue Optical Transients (FBOTs) observed in the Universe. In May 2020, however, a much more powerful FBOT than AT 2018cow was reportedly observed.

<span class="mw-page-title-main">SN 2020oi</span> Extragalactic supernova in 2020

SN 2020oi was a supernova event in the grand design spiral galaxy known as Messier 100, or NGC 4321. It was discovered January 7, 2020 at an apparent magnitude of 17.28 by F. Forster and associates using the Zwicky Transient Facility. The position places it ~4.67″ north of the galactic nucleus. The supernova was not detected on an observation made three days before the discovery, and thus it must have begun during that brief period. The light curve peaked around January 13–18, depending on the wavelength, then declined rapidly over a period of 25 days before flattening into a more gradual decline. Observations of the spectrum made with the SOAR telescope showed this to be a type Ic supernova, with the progenitor being a massive star that had its outer envelope stripped. The initial velocity of the expanding photosphere was ~15,000 km/s.

<span class="mw-page-title-main">SN 2021aefx</span>

SN 2021aefx is a Type Ia supernova discovered in 2021 in the galaxy NGC 1566.

<span class="mw-page-title-main">IC 2759</span> Elliptical galaxy in the constellation of Leo

IC 2759 is a small type E elliptical galaxy located in the constellation of Leo. It is located 350 million light-years away from the Solar System and was discovered on April 24, 1897, by Guillaume Bigourdan. Sometimes IC 2759 is confused with the spiral galaxy, PGC 34882 which is located south of the galaxy.

<span class="mw-page-title-main">IC 5145</span>

IC 5145 is a type Sab spiral galaxy located in the constellation Pegasus. It is located 356 million light-years from the Solar System and was discovered by Edward Emerson Barnard, although the year he discovered it is unknown.

<span class="mw-page-title-main">NGC 3978</span>

NGC 3978 is a large intermediate spiral galaxy with a bar located in the constellation of Ursa Major. It is located 460 million light-years away from the Solar System and was discovered by William Herschel on March 19, 1790, but also observed by John Herschel on April 14, 1831.

<span class="mw-page-title-main">NGC 7222</span> Large barred spiral galaxy with a ring structure

NGC 7222 is a large barred spiral galaxy with a ring structure, located in the constellation Aquarius. It is located 570 million light-years away from the Solar System and was discovered by German astronomer, Albert Marth on August 11, 1864.

<span class="mw-page-title-main">IC 1050</span>

IC 1050 is a type Sbc spiral galaxy located in constellation Boötes. It is located 491 million light-years from the Solar System and has an approximate diameter of 130,000 light-years. IC 1050 was discovered by Stephane Javelle on June 3, 1892.

IC 4588 is a type E elliptical galaxy located in the constellation Serpens. It is located 729 million light-years from the Solar System and has a dimension of 0.30 x 0.3 arcmin meaning its diameter is 64,000 light-years across. IC 4588 was discovered by Stephane Javelle on July 15, 1903.

References

  1. 1 2 3 Bishop, David (January 9, 2024). "Bright Supernovae – 2022" . Retrieved 2024-01-13.
  2. "Missing link found: supernovae give rise to black holes or neutron stars". www.eso.org. Retrieved 12 January 2024.
  3. 1 2 3 4 5 Moore, T.; et al. (October 2023). "SN 2022jli: A Type Ic Supernova with Periodic Modulation of Its Light Curve and an Unusually Long Rise". The Astrophysical Journal Letters. 956 (1): L31. arXiv: 2309.12750 . Bibcode:2023ApJ...956L..31M. doi: 10.3847/2041-8213/acfc25 . ISSN   2041-8205. CC BY icon.svg Material was adapted from this source, which is available under a Creative Commons Attribution 4.0

Further reading