The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations
We present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped-envelope Type Ib SN into a strongly interacting Type IIn S...
| Main Authors: | , , , , , , , , , , , , , , |
|---|---|
| Format: | Journal article |
| Published: |
Oxford University Press
2016
|
| _version_ | 1797074285087424512 |
|---|---|
| author | Anderson, G Horesh, A Mooley, K Rushton, A Fender, R Staley, T Argo, M Beswick, R Hancock, P Pérez-Torres, M Perrott, Y Plotkin, R Pretorius, M Rumsey, C Titterington, D |
| author_facet | Anderson, G Horesh, A Mooley, K Rushton, A Fender, R Staley, T Argo, M Beswick, R Hancock, P Pérez-Torres, M Perrott, Y Plotkin, R Pretorius, M Rumsey, C Titterington, D |
| author_sort | Anderson, G |
| collection | OXFORD |
| description | We present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped-envelope Type Ib SN into a strongly interacting Type IIn SN within 1 yr. The AMI light curve clearly shows two distinct radio peaks, the second being a factor of 4 times more luminous than the first peak. This double bump morphology indicates two distinct phases of mass-loss from the progenitor star with the transition between density regimes occurring at 100-200 d. This reinforces the interpretation that SN 2014C exploded in a low-density region before encountering a dense hydrogen-rich shell of circumstellar material that was likely ejected by the progenitor prior to the explosion. The AMI flux measurements of the first light-curve bump are the only reported observations taken within ~50 to ~125 d post-explosion, before the blast-wave encountered the hydrogen shell. Simplistic synchrotron self-absorption and free-free absorption modelling suggest that some physical properties of SN 2014C are consistent with the properties of other Type Ibc and IIn SNe. However, our single frequency data does not allow us to distinguish between these two models, which implies that they are likely too simplistic to describe the complex environment surrounding this event. Lastly, we present the precise radio location of SN 2014C obtained with the electronic Multi-Element Remotely Linked Interferometer Network, which will be useful for future very long baseline interferometry observations of the SN. |
| first_indexed | 2024-03-06T23:33:57Z |
| format | Journal article |
| id | oxford-uuid:6cffdddb-d2a4-448d-aa6d-5165acf00ea9 |
| institution | University of Oxford |
| last_indexed | 2024-03-06T23:33:57Z |
| publishDate | 2016 |
| publisher | Oxford University Press |
| record_format | dspace |
| spelling | oxford-uuid:6cffdddb-d2a4-448d-aa6d-5165acf00ea92022-03-26T19:14:54ZThe peculiar mass-loss history of SN 2014C as revealed through AMI radio observationsJournal articlehttp://purl.org/coar/resource_type/c_dcae04bcuuid:6cffdddb-d2a4-448d-aa6d-5165acf00ea9Symplectic Elements at OxfordOxford University Press2016Anderson, GHoresh, AMooley, KRushton, AFender, RStaley, TArgo, MBeswick, RHancock, PPérez-Torres, MPerrott, YPlotkin, RPretorius, MRumsey, CTitterington, DWe present a radio light curve of supernova (SN) 2014C taken with the Arcminute Microkelvin Imager (AMI) Large Array at 15.7 GHz. Optical observations presented by Milisavljevic et al. demonstrated that SN 2014C metamorphosed from a stripped-envelope Type Ib SN into a strongly interacting Type IIn SN within 1 yr. The AMI light curve clearly shows two distinct radio peaks, the second being a factor of 4 times more luminous than the first peak. This double bump morphology indicates two distinct phases of mass-loss from the progenitor star with the transition between density regimes occurring at 100-200 d. This reinforces the interpretation that SN 2014C exploded in a low-density region before encountering a dense hydrogen-rich shell of circumstellar material that was likely ejected by the progenitor prior to the explosion. The AMI flux measurements of the first light-curve bump are the only reported observations taken within ~50 to ~125 d post-explosion, before the blast-wave encountered the hydrogen shell. Simplistic synchrotron self-absorption and free-free absorption modelling suggest that some physical properties of SN 2014C are consistent with the properties of other Type Ibc and IIn SNe. However, our single frequency data does not allow us to distinguish between these two models, which implies that they are likely too simplistic to describe the complex environment surrounding this event. Lastly, we present the precise radio location of SN 2014C obtained with the electronic Multi-Element Remotely Linked Interferometer Network, which will be useful for future very long baseline interferometry observations of the SN. |
| spellingShingle | Anderson, G Horesh, A Mooley, K Rushton, A Fender, R Staley, T Argo, M Beswick, R Hancock, P Pérez-Torres, M Perrott, Y Plotkin, R Pretorius, M Rumsey, C Titterington, D The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title | The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title_full | The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title_fullStr | The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title_full_unstemmed | The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title_short | The peculiar mass-loss history of SN 2014C as revealed through AMI radio observations |
| title_sort | peculiar mass loss history of sn 2014c as revealed through ami radio observations |
| work_keys_str_mv | AT andersong thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT horesha thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT mooleyk thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT rushtona thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT fenderr thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT staleyt thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT argom thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT beswickr thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT hancockp thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT pereztorresm thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT perrotty thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT plotkinr thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT pretoriusm thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT rumseyc thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT titteringtond thepeculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT andersong peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT horesha peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT mooleyk peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT rushtona peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT fenderr peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT staleyt peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT argom peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT beswickr peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT hancockp peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT pereztorresm peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT perrotty peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT plotkinr peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT pretoriusm peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT rumseyc peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations AT titteringtond peculiarmasslosshistoryofsn2014casrevealedthroughamiradioobservations |