1 / 16

Distance of 24 Mpc

A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive stellar envelope. The complete story…. Distance of 24 Mpc. 5 kpc. In the outskirts of NGC7259. Sub-solar metallicity environment 0.4<Z<0.9 Zsun. Explosion2. Discovery. Explosion1. Supernova.

oriole
Download Presentation

Distance of 24 Mpc

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive stellar envelope

  2. The complete story… Distance of 24 Mpc 5 kpc In the outskirts of NGC7259 Sub-solar metallicity environment 0.4<Z<0.9 Zsun Explosion2 Discovery Explosion1 Supernova Outburst Outburst Outburst Supernova ? Impostor Now Aug 2009 Aug 2012 Sep 2012 Jul 2010 Sep 2010 May 2011 Oct 2011

  3. UV-Optical-NIR photometry SN2009ip eruptions plus 2012 double explosion Eruptions 2012 “Precursor bump” Major explosion

  4. Why is SN2009ip so interesting? We know the story of eruptions of the progenitor in the previous years The explosion has a luminous PRECURSOR Detection of the PROGENITOR star in pre-explosion images (Smith+10, Foley+11): the progenitor is a massive star with M>60 Msun SN2009ip vs. a sample of SNeIIn and the peculiar explosion 1961V

  5. Our observational campaign: VLA CARMA BAT Fermi-LAT 13-filter photometry + spectra UVOT & HST XMM XRT …no wavelength is left behind… The extensive monitoring is critical to: (i) constrain Erad, the temperature and radius of the emission; (ii) constrain the role of different emission processes that dominate at different wavelengths. Understand the global properties of the explosion

  6. The general picture: 40 days Low-energy explosion: Erad~3d49 erg NOT powered by Nickel! Mshell~0.1 Msun September 2012 The shock breaks out through the dense thick shell ejected by the first explosion August 2012 “shell ejection” A second explosions happens

  7. X-rays: they peak around the same time of the optical emission …however: Radio: Delayed peak due to free-free absorption Lx / Lopt < 10-4 As expected for a shock break out through a dense medium Lbol/1d4 SN2009ip is a weak radio and X-ray emitter!

  8. The metamorphosis in the optical: BUT…

  9. No sign of freshly synthesized material, yet See e.g. [OI]

  10. HST Low-res UVOT spectral campaign Nov 06 Oct 29

  11. Super SED around the time of the optical peak NIR excess of emission

  12. NIR campaign: NIR excess: t=tpk-4.5d The NIR excess is not due to line emission

  13. GeV photons and neutrinos from shock break-out Predicted muon and anti-muon neutrino fluence from SN 2009ip using the observables and explosion parameters according to the model by Murase et al. (2011). For this event, the atmospheric neutrino background is more severe since SN 2009ip occurred in the southern hemisphere. For better localized explosions, this plot shows how limits on the neutrino emission can be used to constrain the energy in cosmic rays (ECR). The collision of the ejecta with massive shells is expected to accelerate cosmic rays (CRs) and generate GeV gamma- rays (Murase et al. 2011; Katz et al. 2011) with fluence that depends both on the explosion and on the environment parameters. We use the parameters inferred from the modeling of the optical-UV emission with shock break out, to predict the expected GeVfluence. Fermi-LAT upper-limits are shown with black circles.

  14. NIR emitting material ejected during the previous years outbursts R>4d15 cm R~5d14 cm E~1d50 erg Mej~0.5 Msun DENSE and compact SHELL M~0.1 Msun (ejected by the 2012 precursor) The general picture is that of a massive star that repeatedly ejects massive shells of material on a time scale of years and less

  15. What triggers the sudden shell ejection? This is not clear. However, two observational facts are crucial to our understanding: Presence of a dominant time-scale common to eruption episodes and the major explosion, shared by completely independent events 40 days Note: this NOT a claim for periodicity Extreme similarity to SN2010mc, which implies: -- Causal connection between precursor and main explosion -- “SIMPLE” mechanism -- Important channel for mass loss

  16. Take-away message Evolved massive stars have a much less boring life than expected: they suffer repetitive shell ejection on short time scales, whose physical origin is not understood, questioning our current understanding of massive star evolution. SN2009ip (and 10mc) might have just shown us a new channel for impulsive and sustained mass loss. Smith 2010; Foley 2011; Fraser 2013; Levesque 2013; Mauerhan 2013; Ofek 2013; Pastorello 2013; Prieto 2012; Smith 2013; Soker 2013 Ref in the literature:

More Related