SN 2010jl

SN 2010jl was a luminous type IIn supernova that was discovered on November 3, 2010, in the irregular galaxy UGC 5189A. It is 48.9 ± 3.4 Mpc distant from the solar system. It showed an infrared excess which lasted for over 1400 days.[1]

Discovery[edit]

2010jl was discovered during the Puckett Observatory Supernova Search, by Newton & Puckett with a 0.40-m reflector at Portal, Arizona. The discovery was made on Nov. 3.52 UT and was confirmed on Nov. 4.50.[2] Follow-up spectroscopy showed broad emission and narrow-line emission from hydrogen and helium leading to a classification of type IIn.[3][4]

Infrared excess[edit]

SN 2010jl with Hubble STIS on 2011-01-23

CSM interaction[edit]

The classification as type IIn showed that the supernova was interacting with the circumstellar medium (CSM). The supernova itself produces the broad emission, the flash-ionized circumstellar medium produces on the other hand the type IIn typical narrow-line emission features.[1] Observations with Chandra-ACIS X-ray showed absorption features caused by circumstellar matter. At the time of the observation it was one of the most luminous supernovae observed in X-rays.[5]

Infrared echo[edit]

Observations with Hubble detected near-infrared excess that lasted for 400 days. While the early near-infrared detection is dominated by the supernova, the later near-infrared detection becomes more dominated by the infrared echo. The echo is caused by pre-existing circumstellar dust that does not interact with the supernova, but that scatters the light of the supernova.[6]

New dust[edit]

A later study with Gemini and Spitzer showed that infrared excess persisted until the end of the observations on day 1367 after the discovery. This very late detection of infrared excess cannot be explained with an infrared echo alone. Between days 260 and 464 the near-infrared jumps in brightness and then slowly fades until day 1000. The jump in near-infrared brightness is explained with the formation of new dust.[1]

The formation of new dust can be shown by several other features. 2010jl showed on the one hand infrared excess caused by thermal radiation of the newly formed dust. It also showed blueshift of the emission-lines, which is caused by the dust blocking the material that is further away from our line of sight. A third line of evidence is increased fading in the optical, which could not be shown due to lacking observations in a specific time-span. It was determined that the supernova produced about 0.005-0.01 M☉ (about 5-10 Jupiter masses) of predominantly carbon dust grains by the day 1400.[1]

2010jl-like supernovae[edit]

Type II supernovae that have similar mid-infrared light curves when compared to 2010jl. The second brightening is marked with a black circle. Data is from NEOWISE

Following the discovery of 2010jl, several other type IIn supernovae with long-lasting infrared excess were discovered. Their H- and K-band and mid-infrared light curve is dominated by two increases of the brightness.[7] The first increase appears during the discovery and is attributed to the CSM interaction and the light echo. The second increase is attributed to the formation of new dust. After the second increase the infrared light curve shows a fading.

The following 2010jl-like supernovae are known: SN 2014ab,[8] SN 2015da[7] and SN 2017hcc.[9] The supernova ASASSN-15ua is also mentioned to be similar to 2010jl.[7] Additionally there are type II supernovae with mid-infrared light curves that are similar to 2010jl.[10]

References[edit]

  1. ^ a b c d Bevan, A. M.; Krafton, K.; Wesson, R.; Andrews, J. E.; Montiel, E.; Niculescu-Duvaz, M.; Barlow, M. J.; De Looze, I.; Clayton, G. C. (2020-05-01). "Disentangling Dust Components in SN 2010jl: The First 1400 Days". The Astrophysical Journal. 894 (2): 111. arXiv:2004.01503. Bibcode:2020ApJ...894..111B. doi:10.3847/1538-4357/ab86a2. ISSN 0004-637X.
  2. ^ Newton, J.; Puckett, T. (2010-11-01). "Possible Supernova in UGC 5189A". Central Bureau Electronic Telegrams. 2532: 1. Bibcode:2010CBET.2532....1N.
  3. ^ Benetti, S.; Bufano, F.; Vinko, J.; Marion, G. H.; Pritchard, T.; Wheeler, J. C.; Chatzopoulos, E.; Shetrone, M. (2010-11-01). "Supernova 2010jl in UGC 5189A". Central Bureau Electronic Telegrams. 2536: 1. Bibcode:2010CBET.2536....1B.
  4. ^ Yamanaka, M.; Okushima, T.; Arai, A.; Sasada, M.; Sato, H. (2010-11-01). "Supernova 2010jl in UGC 5189A". Central Bureau Electronic Telegrams. 2539: 1. Bibcode:2010CBET.2539....1Y.
  5. ^ Chandra, Poonam; Chevalier, Roger A.; Irwin, Christopher M.; Chugai, Nikolai; Fransson, Claes; Soderberg, Alicia M. (2012-05-01). "Strong Evolution of X-Ray Absorption in the Type IIn Supernova SN 2010jl". The Astrophysical Journal. 750 (1): L2. arXiv:1203.1614. Bibcode:2012ApJ...750L...2C. doi:10.1088/2041-8205/750/1/L2. ISSN 0004-637X.
  6. ^ Fransson, Claes; Ergon, Mattias; Challis, Peter J.; Chevalier, Roger A.; France, Kevin; Kirshner, Robert P.; Marion, G. H.; Milisavljevic, Dan; Smith, Nathan; Bufano, Filomena; Friedman, Andrew S.; Kangas, Tuomas; Larsson, Josefin; Mattila, Seppo; Benetti, Stefano (2014-12-01). "High-density Circumstellar Interaction in the Luminous Type IIn SN 2010jl: The First 1100 Days". The Astrophysical Journal. 797 (2): 118. arXiv:1312.6617. Bibcode:2014ApJ...797..118F. doi:10.1088/0004-637X/797/2/118. ISSN 0004-637X.
  7. ^ a b c Tartaglia, L.; Pastorello, A.; Sollerman, J.; Fransson, C.; Mattila, S.; Fraser, M.; Taddia, F.; Tomasella, L.; Turatto, M.; Morales-Garoffolo, A.; Elias-Rosa, N.; Lundqvist, P.; Harmanen, J.; Reynolds, T.; Cappellaro, E. (2020-03-01). "The long-lived Type IIn SN 2015da: Infrared echoes and strong interaction within an extended massive shell". Astronomy and Astrophysics. 635: A39. arXiv:1908.08580. Bibcode:2020A&A...635A..39T. doi:10.1051/0004-6361/201936553. ISSN 0004-6361.
  8. ^ Moriya, T. J.; Stritzinger, M. D.; Taddia, F.; Morrell, N.; Suntzeff, N. B.; Contreras, C.; Gall, C.; Hjorth, J.; Ashall, C.; Burns, C. R.; Busta, L.; Campillay, A.; Castellón, S.; Corco, C.; Davis, S. (2020-09-01). "The Carnegie Supernova Project II. Observations of SN 2014ab possibly revealing a 2010jl-like SN IIn with pre-existing dust". Astronomy and Astrophysics. 641: A148. arXiv:2006.10198. Bibcode:2020A&A...641A.148M. doi:10.1051/0004-6361/202038118. ISSN 0004-6361.
  9. ^ Moran, S.; Fraser, M.; Kotak, R.; Pastorello, A.; Benetti, S.; Brennan, S. J.; Gutiérrez, C. P.; Kankare, E.; Kuncarayakti, H.; Mattila, S.; Reynolds, T. M.; Anderson, J. P.; Brown, P. J.; Campana, S.; Chambers, K. C. (2023-01-01). "A long life of excess: The interacting transient SN 2017hcc". Astronomy and Astrophysics. 669: A51. arXiv:2210.14076. Bibcode:2023A&A...669A..51M. doi:10.1051/0004-6361/202244565. ISSN 0004-6361.
  10. ^ Thévenot, Melina (2020-12-01). "Mid-Infrared Detections of SNe II with NEOWISE". Research Notes of the American Astronomical Society. 4 (12): 243. Bibcode:2020RNAAS...4..243T. doi:10.3847/2515-5172/abd415. ISSN 2515-5172.
Retrieved from "https://en.wikipedia.org/w/index.php?title=SN_2010jl&oldid=1204151475"