Core-collapse supernovae with the intermediate Palomar Transient - - PowerPoint PPT Presentation

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Core-collapse supernovae with the intermediate Palomar Transient - - PowerPoint PPT Presentation

Jun 04, 2023 168 likes •548 views

Core-collapse supernovae with the intermediate Palomar Transient Factory (iPTF) Francesco Taddia , Post-Doc, Astronomy Department, Stockholm University (Oskar Klein Centre) SURVEYS FOR ALL: a two-day mini-workshop in Lund, 1-2 February, 2016

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Core-collapse supernovae with the intermediate Palomar Transient Factory (iPTF)

Francesco Taddia, Post-Doc, Astronomy Department, Stockholm University (Oskar Klein Centre)

SURVEYS FOR ALL: a two-day mini-workshop in Lund, 1-2 February, 2016

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Outline

  • What is iPTF (and its continuation ZTF)?
  • What do we want to learn from the core-collapse

supernovae (SNe) found with iPTF? Investigating the connection between SNe and their massive progenitor stars.

  • Which iPTF projects on core-collapse SNe are

currently ongoing at the OKC?

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The intermediate Palomar Transient Factory (iPTF)

Palomar observatory P48

Partecipants: Caltech (PI: Shri Kulkarni) University of Wisconsin Los Alamos National Lab Oskar Klein Centre Weizmann Institute Kavli@Tokyo IUCAA + friends at LBL,Carnegie

The intermediate Palomar Transient Factory (iPTF) is a fully-automated, wide-field survey aimed at a systematic exploration of the optical transient sky. It started in 2013 as a continuation of PTF (2009-2012).

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(i)PTF Searching the sky

R-band sky coverage of PTF+iPTF, 2009-2015

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IPTF Followup Marshal

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OKC

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What do we want to learn from studying core-collapse supernovae?

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(i)PTF and core-collapse supernovae

1) (i)PTF found many CC-SNe (>700) of different types, allowing us to build large SN samples. 2) Many of them were found very early thanks to the high-cadence of (i)PTF. 3) (i)PTF is an untargeted survey, CC SNe are found in different types of host galaxies.

Gal-Yam et al. 2014, Nature

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Why is it important to find SN at early epochs? The flash spectroscopy method

Hydrostatic surface (<1012cm) Opaque (optically thick) wind (up to ~1013cm) Optically thin Wind, W-R emission lines Gal-Yam et al. 2014, Nature

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Why is it important to find SN at early epochs? The flash spectroscopy method

Hydrostatic surface (<1012cm) Opaque (optically thick) wind (up to ~1013cm) Optically thin Wind, W-R emission lines Nordic Optical Telescope Gal-Yam et al. 2014, Nature

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Which core-collapse supernovae are we mainly interested in?

1) Stripped-envelope core-collapse SNe: Type Ibc/IIb (Within iPTF we are responsible for the Type Ib/c). These supernovae lack hydrogen (sometimes even helium), which was stripped away from the progenitor star by either a companion star or strong winds. 2) Circumstellar-interacting supernovae (Type IIn, Ibn, Ia-CSM). These are supernovae whose ejecta interact with the material ejected by the progenitor system before collapse. 3) Other new or rare and peculiar SN events discovered by iPTF: e.g., 1987A-like supernovae.

  • We can study:

a) Single objects; b) Large SN samples; c) SN environments.

  • Our goal: characterizing the properties of the SN explosion and of its

progenitor star.

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Stripped-envelope SNe PTF12os and iPTF13bvn

Progenitor star in a binary system

Fremling et al. 2016, to be submitted

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Stripped-envelope SNe PTF12os and iPTF13bvn

Progenitor star in a binary system

Fremling et al. 2016, to be submitted

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SN 2011dh/PTF11eon

Ergon et al. 2014,2015

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iPTF15cna, a slowly-evolving stripped-envelope SN

Karamehmetoglu et al. in prep.

Slow light-curve evolution as compared to other stripped-envelope SNe

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Single, massive WR progenitor(?)

iPTF15cna, a slow-evolving stripped-envelope SN

Karamehmetoglu et al. in prep.

Slow light-curve evolution as compared to other stripped-envelope SNe

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Nyholm et al. In prep.

The circumstellar-interacting SN IIn iPTF13z and its bumpy light-curve

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Luminous blue variable progenitor star (?)

Nyholm et al. In prep.

The circumstellar-interacting SN IIn iPTF13z and its bumpy light-curve

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SN IIn spectra from (i)PTF

Roy et al. In prep. From spectral line analysis we can derive the CSM properties

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SN IIn spectra from (i)PTF

Roy et al. In prep. From spectral line analysis we can derive the CSM properties

Luminous blue variable progenitor star (?)

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Days since explosion Magnitudes

Long-rising SNe II from PTF and CCCP

Taddia et al. 2016,

arXiv:1601.07368

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Days since explosion Magnitudes

Long-rising SNe II from PTF and CCCP

Blue supergiant progenitor stars

Taddia et al. 2016,

arXiv:1601.07368

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Taddia et al. In prep.

SNe Ic-BL from PTF/iPTF

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Taddia et al. In prep.

SNe Ic-BL from PTF/iPTF

Energetic explosions of massive stars, sometimes associated with GRBs

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iPTF---->ZTF (Zwicky Transient Facility)

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Conclusions

1) iPTF finds many core-collapse supernovae, at early epochs and in different host galaxy types. 2)We are interested to map the connection between CC SNe and their progenitor stars. We study single objects, SN samples and SN environments. 3) We are particularly interested in stripped-envelope SNe. These are coming from binaries and from massive single stars. Some of them are associated with GRBs. 4) We are studying CSM interacting SNe, likely arising from LBVs. 5) SNe similar to SN 1987A are coming from BSGs. 6) ZTF will give us higher cadence and sky coverage.

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SN environments

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iPTF13dqy