Extensive HST ultraviolet spectra and multiwavelength observations of SN 2014J in M82 indicate reddening and circumstellar scattering by typical dust

Foley, R. J.; Fox, O.; McCully, C.; Phillips, M. M.; Sand, David J.; Zheng, W.; Challis, P.; Filippenko, A. V.; Folatelli, G.; Hillebrandt, W.; Hsiao, E. Y.; Jha, Saurabh W.; Kirshner, R.; Kromer, M.; Marion, G. H.; Nelson, Matthew J.; Pakmor, Rüdiger; Pignata, G.; Röpke, F. K.; Seitenzahl, Ivo R.; Silverman, J. M.; Skrutskie, Michael F.; Stritzinger, M. D.

doi:10.1093/mnras/stu1378

Cited by 130 publications

(193 citation statements)

References 84 publications

Supporting

Mentioning

174

Contrasting

Order By: Relevance

“…For SN 2014J we also add E(B − V) = 1.37 mag (R V = 1.4) for M82. We refer to Amanullah et al (2014), Foley et al (2014), Goobar et al (2014), and Johansson et al (2014) for a discussion of those values. For the recession velocities to the supernovae, we use the host galaxy recessions, i.e., +241 ± 2 km s −1 for SN 2011fe and +203 ± 4 km s −1 for SN 2014J (de Vaucouleurs et al 1991).…”

Section: Introductionmentioning

confidence: 99%

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

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

Self Cite

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

Section: Introductionmentioning

confidence: 99%

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

Lundqvist

Nyholm

Taddia

et al. 2015

A&A

Self Cite

121

View full text Add to dashboard Cite

show abstract

“…Their results, with reddening values of E(B − V) ∼ 1.3 and R V ∼ 1.4, are compatible with a power-law extinction, expected in the case of multiple scattering scenarios. In the same wavelength band, from UV to near infrared (NIR), Foley et al (2014) found reddening parameter values of E(B − V) ∼ 1.2 and R V ∼ 1.4. In this model, the extinction is explained to be caused by a combination of the galaxy dust and a dusty circumstellar medium.…”

Section: Introductionmentioning

confidence: 99%

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

“…This SN is highly reddened and thus offer the best opportunity to study the extinction property on its sightline. The extensive observations have revealed that the extinction curve derived for SN 2014J is highly steep with a very low value of R V ≃ 1.5 (e.g., Goobar et al, 2014;Amanullah et al, 2014;Foley et al, 2014;Marion et al, 2015). From a simultaneous fit to the extinction and polarization data, Hoang (2015) claim that both interstellar and circumstellar dust are responsible for the anomalous extinction property toward SN 2014J.…”

Section: Introductionmentioning

confidence: 99%

Properties of interstellar dust responsible for extinction laws with unusually low total-to-selective extinction ratios of R=1−2

Nozawa

2016

Planetary and Space Science

View full text Add to dashboard Cite

It is well known that the extinction properties along lines of sight to Type Ia supernovae (SNe Ia) are described by steep extinction curves with unusually low total-to-selective extinction ratios of R V = 1.0-2.0. In order to reveal the properties of interstellar dust that causes such peculiar extinction laws, we perform the fitting calculations to the measured extinction curves by applying a two-component dust model composed of graphite and silicate. As for the size distribution of grains, we consider two function forms of the power-law and lognormal distributions. We find that the steep extinction curves derived from the one-parameter formula by Cardelli et al. (1989) with R V = 2.0, 1.5, and 1.0 can be reasonably explained even by the simple power-law dust model that has a fixed power index of −3.5 with the maximum cut-off radii of a max ≃ 0.13 µm, 0.094 µm, and 0.057 µm, respectively. These maximum cut-off radii are smaller than a max ≃ 0.24 µm considered to be valid in the Milky Way, clearly demonstrating that the interstellar dust responsible for steep extinction curves is highly biased to smaller sizes. We show that the lognomal size distribution can also lead to good fits to the extinction curves with R V = 1.0-3.1 by taking the appropriate combinations of the relevant parameters. We discuss that the extinction data at ultraviolet wavelengths are essential for constraining the composition and size distribution of interstellar dust.

show abstract

Extensive HST ultraviolet spectra and multiwavelength observations of SN 2014J in M82 indicate reddening and circumstellar scattering by typical dust

Cited by 130 publications

References 84 publications

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

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

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

Properties of interstellar dust responsible for extinction laws with unusually low total-to-selective extinction ratios of R=1−2

Contact Info

Product

Resources

About