SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

Bietenholz, M. F.; Kamble, A.; Margutti, R.; Milisavljević, D.; Söderberg, A. M.

doi:10.1093/mnras/stx3194

Cited by 24 publications

(48 citation statements)

References 30 publications

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“…This is roughly consistent with the deceleration observed in the ejecta. The "b" component of the spectral profile may arise from the same hot spot found in the VLBI imaging (Bietenholz et al 2018).…”

Section: Light Curve Modelingmentioning

confidence: 78%

“…The shock front (v ≈ 10000 km s −1 ) would already be at 10 17 cm at that epoch, indicating that the CSM shell was more extended than previously thought. With a prolonged interaction with such dense medium, one might expect the forward shock of the SN to substantially slow down, but the radio imaging of the SN using very long baseline interferometry (VLBI) showed that the velocity of the shock barely decreased during the first 1000 days (Bietenholz et al 2018). They also showed in the resolved VLBI image at 1057 days that the CSM was likely asymmetric.…”

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confidence: 99%

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Supernova 2014C: Ongoing Interaction with Extended Circumstellar Material with Silicate Dust

Tinyanont¹,

Lau

Kasliwal³

et al. 2019

ApJ

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Supernova (SN) 2014C is a unique explosion where a seemingly typical hydrogen-poor stripped envelope SN started to interact with a dense, hydrogen-rich circumstellar medium (CSM) a few months after the explosion. The delayed interaction suggests a detached CSM shell, unlike in a typical SN IIn where the CSM is much closer and the interaction commences earlier post-explosion; indicating a different mass loss history. We present near-to mid-infrared observations of SN 2014C from 1-5 years after the explosion, including uncommon 9.7 µm imaging with COMICS on the Subaru telescope. Spectroscopy shows that the interaction is still ongoing, with the intermediatewidth He I 1.083 µm emission present out to our latest epoch 1639 days post-explosion. The last Spitzer /IRAC photometry at 1920 days post-explosion further confirms ongoing CSM interaction. The 1-10 µm spectral energy distributions (SEDs) can be explained by a dust model with a mixture of 69% carbonaceous and 31% silicate dust, pointing to a chemically inhomogeneous CSM. The inference of silicate dust is the first among interacting SNe. An SED model with purely carbonaceous CSM dust is possible, but would require more than 0.22 M of dust, which is an order of magnitude larger

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Section: Light Curve Modelingmentioning

confidence: 78%

mentioning

confidence: 99%

Supernova 2014C: Ongoing Interaction with Extended Circumstellar Material with Silicate Dust

Tinyanont¹,

Lau

Kasliwal³

et al. 2019

ApJ

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“…Most notable is the remarkable SN 1987A, for which a complex CSM ring was directly imaged (e.g., Jakobsen et al 1991;Panagia et al 1991). Others include, e.g., SNe 1979C, 1986J, 1997eg, 1998S, 1993J, 2005kd, 2006jc, 2006gy, 2008iz, 2010jl, 2011dh, and 2014C (e.g., Leonard et al 2000Smith et al 2007;Foley et al 2007;Hoffman et al 2008;Chandra et al 2009b;Bietenholz et al 2010;Martí-Vidal et al 2011;Bietenholz et al 2012;Katsuda et al 2016;Kimani et al 2016;Dwarkadas et al 2016;Bartel et al 2017;Bietenholz et al 2018), many of which are classified as type IIn.…”

Section: Line Structurementioning

confidence: 99%

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

Quirola-Vásquez

Bauer

Dwarkadas

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present X-ray spectra spanning 18 years of evolution for SN 1996cr, one of the five nearest SNe detected in the modern era. Chandra HETG exposures in 2000, 2004, and 2009 allow us to resolve spectrally the velocity profiles of Ne, Mg, Si, S, and Fe emission lines and monitor their evolution as tracers of the ejecta-circumstellar medium (CSM) interaction. To explain the diversity of X-ray line profiles, we explore several possible geometrical models. Based on the highest signal-to-noise 2009 epoch, we find that a polar geometry with two distinct opening angle configurations and internal obscuration can successfully reproduce all of the observed line profiles. The best fit model consists of two plasma components: (1) a mildly absorbed (2×10 21 cm −2 ), cooler (≈2 keV) with high Ne, Mg, Si, and S abundances associated with a wide polar interaction region (half-opening angle ≈58 • ); (2) a moderately absorbed (2×10 22 cm −2 ), hotter ( > ∼ 20 keV) plasma with high Fe abundances and strong internal obscuration associated with a narrow polar interaction region (half-opening angle ≈20 • ). We extend this model to seven further epochs with lower signal-to-noise ratio and/or lower spectral-resolution between 2000-2018, yielding several interesting trends in absorption, flux, geometry and expansion velocity. We argue that the hotter and colder components are associated with reflected and forward shocks, respectively, at least at later epochs. We discuss the physical implications of our results and plausible explosion scenarios to understand the X-ray data of SN 1996cr.

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“…It was classified as a hydrogen-poor Type Ib SN (Kim et al 2014) indicating a mass loss before its explosion. Over the course of one year, it evolved into an Hα emission prominent type IIn SN implying its interaction with nearby circumstellar shell (Milisavljevic et al 2015;Margutti et al 2017;Bietenholz et al 2018). A series of Chandra observations was proposed after the explosion of SN 2014C, which provide multiple observations of NGC 7331 in X-ray.…”

Section: Introductionmentioning

confidence: 99%

“…Using the Chandra and NuSTAR data, we obtained the X-ray light curve of SN 2014 by fitting a tbabs*apec model in 0.3 -30 keV, the variation of column density, the plasma temperature and the photon indexes.The close and open circles represent the unabsorbed and absorbed luminosities respectively. Based on 8.4 GHz VLBI data of SN 2014C, the measured denstiy fluxes and the fitted angular outer radius of a spherical shell model estimated inBietenholz et al (2018) are also plotted for reference. All the errors are at 90% confidence level.…”

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confidence: 99%

A Multi-epoch X-Ray Study of the Spiral Galaxy NGC 7331

Jin

Kong²

2019

ApJ

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X-ray point sources in galaxies are dominated by X-ray binaries (XRBs) that are variables or transients and whether their variability would alter the X-ray luminosity functions (XLF) is still in debate.Here we report on NGC 7331 as an example to test this with 7 Chandra observations. Their detection limit is 7×10 37 erg s −1 in the 0.3 -8.0 keV energy range by assuming a power-law spectral model with a photon index of 1.7. We detected 55 X-ray sources. Thirteen of them are variables for which 3 of them are transients and some of the sources possess a bimodal luminosity-hardness ratio feature, which is often observed among X-ray binaries. Nine more ultra-luminous X-ray sources are found comparing to previous studies and 8 are likely to be low-mass or high-mass XRBs. Twenty-one optical counterpart candidates are found based on the Hubble Space Telescope images, but we cannot rule out the possibility of positional coincidence. The spectral analysis of SN 2014C shows a trend of increasing soft photons and decreasing hydrogen column densities as its outer shell expands. We fit the 7 incompleteness-corrected XLFs to both a power-law (PL) and a power-law with an exponential cut-off (PLC) model using Bayesian method, which is the first time used in XLF fitting. The hierarchical PLC model can describe the XLF of NGC 7331 best with a slope of ∼ 0.5 and a luminosity cut-off around 8×10 38 erg s −1 . This study proves that multi-epoch observations decrease the deviation due to the variable luminous sources in XLFs.

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SN 2014C: VLBI images of a supernova interacting with a circumstellar shell

Cited by 24 publications

References 30 publications

Supernova 2014C: Ongoing Interaction with Extended Circumstellar Material with Silicate Dust

Supernova 2014C: Ongoing Interaction with Extended Circumstellar Material with Silicate Dust

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

A Multi-epoch X-Ray Study of the Spiral Galaxy NGC 7331

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