Diversity of Dust Properties in External Galaxies Confirmed by Polarization Signals from Type II Supernovae

Nagao, Takashi; Patat, F.; Maeda, Keiichi; Baade, D.; Mattila, S.; Taubenberger, S.; Kotak, R.; Cikota, Aleksandar; Kuncarayakti, H.; Bulla, Mattia; Maund, Justyn R.

doi:10.3847/2041-8213/aca47d

Cited by 4 publications

(1 citation statement)

References 45 publications

(54 reference statements)

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“…Adding to this energetic consideration the challenge of the delayed neutrino mechanism to explain the point-symmetric morphologies of some CCSN remnants identified in the last two years (e.g., Bear & Soker 2024;Soker 2024a,b,c), I conclude that the most likely explosion mechanism of the progenitors of SN 2024ggi and SN 2023ixf was the jittering jets explosion mechanism (JJEM). The JJEM can also account for the polarization of CCSNe and its correlation with the explosion energy (for the correlation, see Nagao et al 2024b), as well as for bipolar CCSNe (e.g., Nagao et al 2024a).…”

Section: The Implication Of Ementioning

confidence: 99%

A Pre-explosion Extended Effervescent Zone around Core-collapse Supernova Progenitors

Soker

2020

ApJ

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I propose a scenario according to which the dense compact circumstellar matter (CSM) that the ejecta of many core-collapse supernovae (CCSNe) collide with within several days after explosion results from a dense zone where in addition to the stellar wind there is gas that does not reach the escape velocity. In this effervescent zone around red supergiant (RSG) stars, there are dense clumps that are ejected from the vicinity of the RSG surface, rise to radii of tens of astronomical units, and then fall back. I consider two simple velocity distributions of the ejected clumps. I find that the density of the bound mass can be tens of times that of the escaping wind, and therefore can mimic a very high mass-loss rate. The dense effervescent compact CSM zone can (1) explain the collision of the ejecta of many CCSNe with a dense compact CSM days after explosion, (2) facilitate very high mass-loss rate if the star experiences powerful pre-explosion activity, (3) form dust that obscures the progenitor in the visible band, and (4) lead to an efficient mass transfer to a stellar companion at separations of tens of astronomical units, if it exists. The effervescent zone might exist for thousands of years and more, and therefore the effervescent CSM model removes the requirement from many type II CCSN progenitors to experience a very strong outburst just years to months before explosion.

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Section: The Implication Of Ementioning

confidence: 99%

A Pre-explosion Extended Effervescent Zone around Core-collapse Supernova Progenitors

Soker

2020

ApJ

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Spectropolarimetry of Type II supernovae

Nagao¹,

Mattila²,

Kotak³

et al. 2023

A&A

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We investigate the polarization spectra of hydrogen-rich core-collapse supernovae (Type II SNe). The polarization signal from SNe contains two independent components: intrinsic SN polarization and interstellar polarization (ISP). From these components, we can study the SN explosion geometry and the dust properties in their host galaxies or in the Milky Way. In this first paper, we employ a newly improved method to investigate the properties of the ISP components of 11 well-observed Type II SNe. Our analyses revealed that 10 of these 11 SNe showed a steady ISP component with a polarization degree of ≲1.0%, while one SN was consistent with zero ISP. As for the wavelength dependence, SN 2001dh (and possibly SN 2012aw) showed a non-Milky-Way-like ISP likely originating from the interstellar dust in their respective host galaxies: their polarization maxima were located at short wavelengths (≲4000 Å). Similar results have been obtained previously for highly reddened SNe. The majority of the SNe in our sample had uncertainties in the wavelength dependence of their ISP components that were too large for further consideration. Our work demonstrates that further investigation of the ISP component of the SN polarization, by applying this method to a larger SN sample, can provide new opportunities to study interstellar dust properties in external galaxies.

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Varying linear polarisation in the dust-free gamma-ray burst 210610B

Agüí Fernández,

de Ugarte Postigo,

Thöne

et al. 2024

A&A

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Long gamma-ray bursts (GRBs) are produced by the collapse of some very massive stars, that emit ultra-relativistic jets. When the jets collide with the interstellar medium they decelerate and generate the so-called afterglow emission, which has been observed to be polarised. We study the polarimetric evolution of the GRB\,210610B afterglow, at $z=1.1341$. This allows us to evaluate the role of geometric and/or magnetic mechanisms in the GRB afterglow polarisation. We observed GRB\,210610B using imaging polarimetry with CAFOS on the 2.2 m Calar Alto Telescope and FORS2 on the $4 m Very Large Telescope. Complementary optical spectroscopy was obtained with OSIRIS on the 10.4 m Gran Telescopio Canarias. We studied the GRB light-curve from X-rays to the optical bands and the Spectral Energy Distribution (SED). This allowed us to strongly constrain the line-of-sight extinction. Finally, we studied the GRB host galaxy using optical to NIR data to fit the SED and derive its integrated properties. GRB\,210610B had a bright afterglow with a negligible line-of-sight extinction. Polarimetry was obtained at three epochs: during an early plateau phase, at the time when the light curve breaks, and after the light curve steepened. We observe an initial polarisation of $ that goes to zero at the time of the break, and it then again increases to $ with a change in the position angle of $54 deg. The spectrum shows features with very low equivalent widths. This indicate a small amount of material in the line of sight within the host. The lack of dust and the low amount of material in the line of sight to GRB\,210610B allowed us to study the intrinsic polarisation of the GRB optical afterglow. The GRB polarisation signals are consistent with ordered magnetic fields in refreshed shock or/and hydrodynamics-scale turbulent fields in the forward shock.

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Diversity of Dust Properties in External Galaxies Confirmed by Polarization Signals from Type II Supernovae

Cited by 4 publications

References 45 publications

A Pre-explosion Extended Effervescent Zone around Core-collapse Supernova Progenitors

A Pre-explosion Extended Effervescent Zone around Core-collapse Supernova Progenitors

Spectropolarimetry of Type II supernovae

Varying linear polarisation in the dust-free gamma-ray burst 210610B

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