The exceptional X-ray evolution of SN 1996cr in high resolution

Quirola-Vásquez, J.; Bauer, F. E.; Dwarkadas, Vikram V.; Badenes, Carles; Brandt, W. N.; Nymark, Tanja; Walton, D. J.

doi:10.1093/mnras/stz2858

Cited by 12 publications

(13 citation statements)

References 141 publications

(264 reference statements)

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“…The forward shock interacting with a high-density medium would be the most straightforward explanation for the rise in X-ray emission. On a longer timescale, the contribution to the X-ray flux from the reverse shock may be expected to dominate at some time after the shock has interacted with the dense CSM, as suggested by simulations, and analysis of the emission line profiles, of SN 1996cr (Dwarkadas et al 2010;Quirola-Vásquez et al 2019).…”

Section: Constraints From X-raysmentioning

confidence: 96%

Seven Years of SN 2014C: A Multiwavelength Synthesis of an Extraordinary Supernova

Thomas

Wheeler

Dwarkadas

et al. 2022

ApJ

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SN 2014C was originally classified as a Type Ib supernova, but at phase ϕ = 127 days, post-explosion strong Hα emission was observed. SN 2014C has since been observed in radio, infrared, optical and X-ray bands. Here we present new optical spectroscopic and photometric data spanning ϕ = 947–2494 days post-explosion. We address the evolution of the broadened Hα emission line, as well as broad [O iii] emission and other lines. We also conduct a parallel analysis of all publicly available multiwavelength data. From our spectra, we find a nearly constant Hα FWHM velocity width of ∼2000 km s−1 that is significantly lower than that of other broadened atomic transitions (∼3000–7000 km s−1) present in our spectra ([O i] λ6300; [O iii] λ λ4959, 5007; He i λ7065; [Ca ii] λ λ7291, 7324). The late radio data demand a fast forward shock (∼10,000 km s−1 at ϕ = 1700 days) in rarified matter that contrasts with the modest velocity of the Hα. We propose that the infrared flux originates from a toroidal-like structure of hydrogen surrounding the progenitor system, while later emission at other wavelengths (radio, X-ray) likely originates predominantly from the reverse shock in the ejecta and the forward shock in the quasi-spherical progenitor He-wind. We propose that the Hα emission arises in the boundary layer between the ejecta and torus. We also consider the possible roles of a pulsar and a binary companion.

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Section: Constraints From X-raysmentioning

confidence: 96%

Seven Years of SN 2014C: A Multiwavelength Synthesis of an Extraordinary Supernova

Thomas

Wheeler

Dwarkadas

et al. 2022

ApJ

Self Cite

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“…D.1, also Fig. 4), which is unusual but have been seen in a small number of SNe, such as SN1987A and SN1996cr (Quirola-Vásquez et al 2019;Dwarkadas 2014). Likewise, the flux of the relatively bright Xp5 is rather stable over 16 yr without a sign of declining.…”

Section: X-ray Variability Of Snr Candidatesmentioning

confidence: 70%

“…Compared to SN1993J, the L 2−8 of which dropped below 10 37 erg s −1 after 20 yr (Kundu et al 2019), all our X-ray SNRs have L 4−8 > 10 37 erg s −1 , despite some of their ages, which are known to be >20 yr from radio observations. Since our X-ray SNRs are all embedded in the starbursting molecular disc, the surrounding dense interstellar medium (ISM) could amplify X-ray brightness, as suggested for the X-ray-luminous class of Type IIn SNe (Fox et al 2000;Ofek et al 2013;Chandra et al 2015;Ross & Dwarkadas 2017;Quirola-Vásquez et al 2019).…”

Section: Supernova Ratementioning

confidence: 88%

X-ray supernova remnants in the starburst region of M 82

Iwasawa

2021

A&A

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We searched for X-ray supernova remnants (SNRs) in the starburst region of M 82, using archival data from the Chandra X-ray Observatory with a total effective exposure time of 620 ks with an X-ray spectroscopic selection. Strong line emission from Fe XXV at 6.7 keV is a characteristic spectral feature of hot, shocked gas of young SNRs and is distinctive among the discrete sources in the region populated by X-ray binaries. We selected candidates using narrow-band imaging aimed at the line excess and identified six (and possibly a seventh) X-ray SNRs. Two previously known examples were recovered by our selection. Five of them have radio counterparts, including the radio supernova SN2008iz, which was discovered as a radio transient in 2008. It shows a hard X-ray spectrum with a blueshifted Fe K feature with v ≈ −2700 km s−1, both of which suggest its youth. The 4–8 keV luminosities of the selected SNRs are in the range of (0.3–2.5)×1038 erg s−1. We made a crude estimate of the supernova rate, assuming that more luminous SNRs are younger, and found νSN = 0.06 (0.03–0.13) yr−1, in agreement with the supernova rates estimated by radio observations and the generally believed star formation rate of M 82, although the validity of the assumption is questionable. A sum of the Fe XXV luminosity originating from the selected X-ray SNRs consists of half of the total Fe XXV luminosity observed in the central region of M 82. We briefly discuss its implications for starburst winds and the Fe XXV emission in more luminous starburst galaxies.

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“…Compared to SN1993J, the L 2−8 of which dropped below 10 37 erg s −1 after 20 yr (Kundu et al 2019), all our X-ray SNRs have L 4−8 > 10 37 erg s −1 , despite some of their ages, which are known to be > 20 yr from radio observations. Since our X-ray SNRs are all embedded in the starbursting molecular disc, the surrounding dense interstellar medium (ISM) could amplify X-ray brightness, as suggested for the Xray-luminous class of Type IIn SNe (Fox et al 2000;Ofek et al 2013;Chandra et al 2015;Ross & Dwarkadas 2017;Quirola-Vásquez et al 2019).…”

Section: Supernova Ratementioning

confidence: 88%

X-ray supernova remnants in the starburst region of M82

Iwasawa

2021

Preprint

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We searched for X-ray supernova remnants (SNRs) in the starburst region of M82, using archival data from the Chandra X-ray Observatory with a total effective exposure time of 620 ks with an X-ray spectroscopic selection. Strong line-emission from Fe xxv at 6.7 keV is a characteristic spectral feature of hot, shocked gas of young SNRs and distinctive among the discrete sources in the region populated by X-ray binaries. We selected candidates using narrow-band imaging aimed at the line excess and identified six (and possibly a seventh) X-ray SNRs. Two previously known examples were recovered by our selection. Five of them have radio counterparts, including the radio supernova SN2008iz, which was discovered as a radio transient in 2008. It shows a hard X-ray spectrum with a blueshifted Fe K feature with v ≈ −2700 km s −1 , both of which suggest its youth. The 4-8 keV luminosities of the selected SNRs are in the range of (0.3-2.5)×10 38 erg s −1 . We made a crude estimate of the supernova rate, assuming that more luminous SNRs are younger, and found ν SN = 0.06 (0.03-0.13) yr −1 , in agreement with the supernova rates estimated by radio observations and the generally believed star formation rate of M82, although the validity of the assumption is questionable. A sum of the Fe xxv luminosity originating from the selected X-ray SNRs consists of half of the total Fe xxv luminosity observed in the central region of M82. We briefly discuss its implications for starburst winds and the Fe xxv emission in more luminous starburst galaxies.

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The exceptional X-ray evolution of SN 1996cr in high resolution

Cited by 12 publications

References 141 publications

Seven Years of SN 2014C: A Multiwavelength Synthesis of an Extraordinary Supernova

Seven Years of SN 2014C: A Multiwavelength Synthesis of an Extraordinary Supernova

X-ray supernova remnants in the starburst region of M 82

X-ray supernova remnants in the starburst region of M82

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