The Expansion of the Young Supernova Remnant 0509-68.7 (N103B)

Williams, Brian J.; Blair, William P.; Borkowski, Kazimierz J.; Ghavamian, Parviz; Hendrick, S. P.; Long, Knox S.; Petre, Robert; Raymond, J. C.; Rest, A.; Reynolds, Stephen P.; Sankrit, Ravi; Seitenzahl, Ivo R.; Winkler, P. F.

doi:10.3847/2041-8213/aae08d

Cited by 22 publications

(18 citation statements)

References 27 publications

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“…Williams and Portegies Zwart, the latter only for Obs. ID 3810, Williams et al 2018), could be able to detect such a kind of emission. Table 3 shows the Obs.ID, the exposures, and the aim points of the selected observations.…”

Section: Searching For An X-ray Counterpartmentioning

confidence: 99%

A black hole detected in the young massive LMC cluster NGC 1850

Saracino

Kamann

Guarcello

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We report the detection of a black hole (NGC 1850 BH1) in the ∼100 Myr-old massive cluster NGC 1850 in the Large Magellanic Cloud. It is in a binary system with a main-sequence turn-off star (4.9 ± 0.4 M⊙), which is starting to fill its Roche Lobe and becoming distorted. Using 17 epochs of VLT/MUSE observations we detected radial velocity variations exceeding 300 km s−1 associated to the target star, linked to the ellipsoidal variations measured by OGLE-IV in the optical bands. Under the assumption of a semi-detached system, the simultaneous modelling of radial velocity and light curves constraints the orbital inclination of the binary to (38 ± 2)○, resulting in a true mass of the unseen companion of $11.1_{-2.4}^{+2.1}\, M_{\odot }$. This represents the first direct dynamical detection of a black hole in a young massive cluster, opening up the possibility of studying the initial mass function and the early dynamical evolution of such compact objects in high-density environments.

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Section: Searching For An X-ray Counterpartmentioning

confidence: 99%

A black hole detected in the young massive LMC cluster NGC 1850

Saracino

Kamann

Guarcello

et al. 2021

Monthly Notices of the Royal Astronomical Society

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“…From this they estimated that ≃ 15 − 45% of the SNRs Ia are SNIPs. However, the SNR Ia N103B that they did not list as a SNIP does interact with a CSM (e.g., Williams et al 2018). If I take the two SNRs that are known to interact with a CSM from the list of 13 SNRs, Kepler and N103B, I find the fraction of SNIPs to be ≈ 15%.…”

Section: Sn Ia Rates From Observationsmentioning

confidence: 99%

“…In Soker (2019b) I noted that the SNR Ia N103B does interact with a CSM (e.g., Williams et al 2018). I still estimated the fraction of SNIP as f SNIP ≃ 15 − 20%.…”

Section: Common Envelope To Explosion Delay (Ceed) Timementioning

confidence: 99%

Common envelope to explosion delay time of Type Ia supernovae

Soker

2019

Monthly Notices of the Royal Astronomical Society

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I study the rate of type Ia supernovae (SNe Ia) within about a million years after the assumed common envelope evolution (CEE) that forms the progenitors of these SNe Ia, and find that the population of SNe Ia with short CEE to explosion delay (CEED) time is ≈ few × 0.1 of all SNe Ia. I also claim for an expression for the rate of these SNe Ia that occur at short times after the CEE, t CEED 10 6 yr, that is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED times are different (at least to some extend) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so called SNe Ia-CSM, and the rate of SNe Ia that on a time scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core degenerate (CD) scenario, to the double degenerate (DD) scenario, to the double detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single degenerate (SD) scenario.

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“…A light echo from the SN was found by Rest et al (2005), from which they derived an age of ∼ 860 years. Further support for this young age is provided by expansion measurements from Chandra observations separated by 17 years (Williams et al 2018), where the overall average shock velocity is found to be in excess of 4000 km s −1 , and measurements of balmer dominated shocks with average velocity of 2070 ± 60 km s −1 by Ghavamian et al (2017). The Balmer dominated filaments are in locations with significant preshock neutral hydrogen.…”

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confidence: 89%

Locating the CSM Emission within the Type Ia Supernova Remnant N103B

Guest,

Blair,

Borkowski

et al. 2022

Preprint

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We present results from deep Chandra observations of the young Type Ia supernova remnant (SNR) 0509-68.7, also known as N103B, located in the Large Magellanic cloud (LMC). The remnant displays an asymmetry in brightness, with the western hemisphere appearing significantly brighter than the eastern half. Previous multi-wavelength observations have attributed the difference to a density gradient and suggested circumstellar material origins, drawing similarities to Kepler's SNR. We apply a clustering technique combined with traditional imaging analysis to spatially locate various emission components within the remnant. We find that O and Mg emission is strongest along the blast wave, and coincides with Spitzer observations of dust emission and optical emission from the non-radiative shocks. The abundances of O and Mg in these regions are enhanced relative to the average LMC abundances and appear as a distinct spatial distribution compared to the ejecta products, supporting the circumstellar medium (CSM) interpretation. We also find that the spatial distribution of Cr is identical to that of Fe in the interior of the remnant, and does not coincide at all with the O and Mg emission. 1. INTRODUCTION Type Ia supernovae are the result of a thermonuclear detonation of a white dwarf star at the Chandrasekhar mass. The path to explosion is likely to have multiple origins. The simple picture

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The Expansion of the Young Supernova Remnant 0509-68.7 (N103B)

Cited by 22 publications

References 27 publications

A black hole detected in the young massive LMC cluster NGC 1850

A black hole detected in the young massive LMC cluster NGC 1850

Common envelope to explosion delay time of Type Ia supernovae

Locating the CSM Emission within the Type Ia Supernova Remnant N103B

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