OPTICAL AND NEAR-INFRARED POLARIMETRY OF HIGHLY REDDENED Type Ia SUPERNOVA 2014J: PECULIAR PROPERTIES OF DUST IN M82

Kawabata, Koji S.; Akitaya, Hiroshi; Yamanaka, Masahito; Itoh, R.; Maeda, Keiichi; Moritani, Yuki; Ui, Takahiro; Mori, K.; Nogami, Daisaku; Nomoto, Ken’ichi; Suzuki, N.; Takaki, K.; Tanaka, Masaomi; Ueno, Issei; Chiyonobu, Shingo; Harao, Tatsuya; Matsui, Rieko; Miyamoto, Hisakazu; Nagae, Osamu; Nakashima, A.; Nakaya, Hidehiko; Ohashi, Yoshiyuki; Ohsugi, T.; Komatsu, T.; Sakimoto, K.; Sasada, Mahito; Sato, Hideo; Tanaka, Hiroyuki; Urano, T.; Yamashita, Takuya; Yoshida, Michitoshi; Arai, Akira; Ebisuda, N.; Fukazawa, Yasushi; Fukui, A.; Hashimoto, Osamu; Honda, Satoshi; Izumiura, Hideyuki; Kanda, Yuka; Kawaguchi, Kotaro; Kawai, N.; Kuroda, D.; Masumoto, Kazunari; Matsumoto, Katsura; Nakaoka, Tatsuya; Takata, K.; Uemura, Makoto; Yanagisawa, K.

doi:10.1088/2041-8205/795/1/l4

Cited by 46 publications

(41 citation statements)

References 49 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, although compatible with an extinction law with a low value of R V ∼ 1.4 and consistent as well with previous mentioned results, Brown et al (2015), making use of Swift-UVOT data, suggested that most of the reddening is caused by the interstellar dust. Optical and NIR linear polarimetric observations of the source presented in Kawabata et al (2014) supports the scenario where the extinction is mostly produced by the interstellar dust. These evidences favor the doubledegenerate scenario for SN 2014J, where less circumstellar dust is expected than in cases with a giant companion star.…”

Section: Introductionsupporting

confidence: 66%

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Fernández-Barral¹,

Fruck²,

Blanch³

et al. 2017

AIP Conference Proceedings

View full text Add to dashboard Cite

Context. In this work we present data from observations with the MAGIC telescopes of SN 2014J detected in January 21 2014, the closest Type Ia supernova since Imaging Air Cherenkov Telescopes started to operate. Aims. We probe the possibility of very-high-energy (VHE; E ≥ 100 GeV) gamma rays produced in the early stages of Type Ia supernova explosions. Methods. We performed follow-up observations after this supernova explosion for 5 days, between January 27 and February 2 in 2014. We search for gamma-ray signal in the energy range between 100 GeV and several TeV from the location of SN 2014J using data from a total of ∼ 5.5 hours of observations. Prospects for observing gamma-rays of hadronic origin from SN 2014J in the near future are also being addressed. Results. No significant excess was detected from the direction of SN 2014J. Upper limits at 95% confidence level on the integral flux, assuming a power-law spectrum, dF/dE ∝ E −Γ , with a spectral index of Γ = 2.6, for energies higher than 300 GeV and 700 GeV, are established at 1.3 × 10 −12 and 4.1 × 10 −13 photons cm −2 s −1 , respectively. Conclusions. For the first time, upper limits on the VHE emission of a Type Ia supernova are established. The energy fraction isotropically emitted into TeV gamma rays during the first ∼ 10 days after the supernova explosion for energies greater than 300 GeV is limited to 10 −6 of the total available energy budget (∼ 10 51 erg). Within the assumed theoretical scenario, the MAGIC upper limits on the VHE emission suggest that SN 2014J will not be detectable in the future by any current or planned generation of Imaging Atmospheric Cherenkov Telescopes.

show abstract

Section: Introductionsupporting

confidence: 66%

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Fernández-Barral¹,

Fruck²,

Blanch³

et al. 2017

AIP Conference Proceedings

View full text Add to dashboard Cite

show abstract

“…4.4). We note that no LVG SNe in Benetti et al (2005) have v SiII ≥ 11 000 km s −1 around B-band maximum, but v SiII ≈ 11 750 km s −1 for SN 2014J at that epoch (Ashall et al 2014;Kawabata et al 2014;Marion et al 2015).…”

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 69%

“…The decline rate in this velocity (v SiII ) is calledv Si , and Maeda et al (2010a) Consulting the results of Kawabata et al (2014) and Marion et al (2015) for SN 2014J, we find thatv Si ∼55 km s…”

Section: Broad Lines Of Sn 2011fe and 2014jmentioning

confidence: 71%

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

121

View full text Add to dashboard Cite

Aims. This study aims at constraining the origin of the nearby Type Ia supernovae (SNe), 2011fe and 2014J. The two most favoured scenarios for triggering the explosion of the white dwarf supernova progenitor is either mass loss from a non-degenerate companion or merger with another white dwarf. In the former, there could be a significant amount of leftover material from the companion at the centre of the supernova. Detecting such material would therefore favour the single-degenerate scenario. Methods. The left-over material from a possible non-degenerate companion can reveal itself after about one year, and in this study such material was searched for in the spectra of SN 2011fe (at 294 days after the explosion) using the Large Binocular Telescope and for SN 2014J using the Nordic Optical Telescope (315 days past explosion). The observations were interpreted using numerical models simulating the expected line emission from ablated material from the companion star. λλ7291, 7324 could be traced for in any of the two supernovae. When systematic uncertainties are included, the limits on hydrogen-rich ablated gas are 0.003 M in SN 2011fe and 0.0085 M in SN 2014J, where the limit for SN 2014J is the second lowest ever, and the limit for SN 2011fe is a revision of a previous limit. Limits are also put on heliumrich ablated gas, and here limits from [O I] λ6300 provide the upper mass limits 0.002 M and 0.005 M for SNe 2011fe and 2014J, respectively. These numbers are used in conjunction with other data to argue that these supernovae can stem from double-degenerate systems or from single-degenerate systems with a spun-up/spun-down super-Chandrasekhar white dwarf. For SN 2011fe, other types of hydrogen-rich donors can very likely be ruled out, whereas a main-sequence donor system with large intrinsic separation is still possible for SN 2014J. Helium-rich donor systems cannot be ruled out for any of the two supernovae, but the expected short delay time for such progenitors makes this possibility less likely, especially for SN 2011fe. Published data for SNe 1998bu, 2000cx, 2001el, 2005am, and 2005cf are used to constrain their origin. We emphasise that the results of this study depend on the sought-after lines emerging unattenuated from the central regions of the nebula. Detailed radiative transfer calculations with longer line lists than are presently used are needed to confirm that this is, in fact, true. Finally, the broad lines of SNe 2011fe and 2014J are discussed, and it is found that the [Ni II] λ7378 emission is redshifted by ∼+1300 km s −1 , as opposed to the known blueshift of ∼−1100 km s −1 for SN 2011fe. [Fe II] λ7155 is also redshifted in SN 2014J. SN 2014J belongs to a minority of SNe Ia that both have a nebular redshift of [Fe II] λ7155 and [Ni II] λ7378, and a slow decline of the Si II λ6355 absorption trough just after B-band maximum.

show abstract

“…Four SNe Ia with high quality of polarization data (SNe 1986G, 2006X, 2008fp, and 2014J) exhibit anomalous polarization curves that rise toward UV wavelengths (Kawabata et al 2014;Patat et al 2015). Fitting the observational data with the typical ISM polarization law-Serkowski law-yields an anomalous value of peak wavelength (λ max < 0.2 µm) for SNe 2008fp and 2014J, which is much lower than the typical value λ max ∼ 0.55 µm in the Galaxy.…”

Section: Introductionmentioning

confidence: 93%

Properties and Alignment of Interstellar Dust Grains toward Type Ia Supernovae with Anomalous Polarization Curves

Hoang

2017

ApJ

View full text Add to dashboard Cite

Recent photometric and polarimetric observations of type Ia supernovae (SNe Ia) show unusually low total-to-selective extinction ratio (R V < 2) and wavelength of maximum polarization (λ max < 0.4 µm) for several SNe Ia, which indicates peculiar properties of interstellar (IS) dust in the SN hosted galaxies and/or the presence of circumstellar (CS) dust. In this paper, we use inversion technique to infer bestfit grain size distribution and alignment function of interstellar grains along the lines of sight toward four SNe Ia with anomalous extinction and polarization data (SNe 1986G, 2006X, 2008fp, and 2014J). We find that to reproduce low values of R V , a significant enhancement in the mass of small grains of radius a < 0.1 µm is required. For SN 2014J, a simultaneous fit to its observed extinction and polarization is unsuccessful if the entire data are attributed to IS dust (model 1), but a good fit is obtained when accounting for the contribution of CS dust (model 2). For SN 2008fp, our best-fit results for model 1 show that, to reproduce an extreme value of λ max ∼ 0.15 µm, small silicate grains must be aligned as efficiently as big grains. For this case, we suggest that strong radiation from the SN can induce efficient alignment of small grains in a nearby intervening molecular cloud via radiative torque mechanism. The resulting time dependence polarization from this RAT alignment model can be tested by observing at ultraviolet wavelengths.

show abstract

OPTICAL AND NEAR-INFRARED POLARIMETRY OF HIGHLY REDDENED Type Ia SUPERNOVA 2014J: PECULIAR PROPERTIES OF DUST IN M82

Cited by 46 publications

References 49 publications

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

Very-high-energy gamma-ray observations of the Type Ia supernova SN 2014J with the MAGIC telescopes

No trace of a single-degenerate companion in late spectra of supernovae 2011fe and 2014J

Properties and Alignment of Interstellar Dust Grains toward Type Ia Supernovae with Anomalous Polarization Curves

Contact Info

Product

Resources

About