NuSTAR Detection of a Hard X-Ray Source in the Supernova Remnant-molecular Cloud Interaction Site of IC 443

Zhang, Shuo; Tang, Xiaping; Zhang, Xiao; Sun, Lei; Gotthelf, E. V.; Zhang, Zhiyu; Li, Hui; Cheng, Allen; Pasham, Dheeraj; Baganoff, Frederick K.; Perez, K.; Hailey, Charles J.; Mori, Kaya

doi:10.3847/1538-4357/aabe7c

Cited by 13 publications

(5 citation statements)

References 62 publications

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“…A lot of studies are made on IC 443 through out the whole spectrum, from gamma ray to radio (e.g. Fesen 1984;Welsh & Sallmen 2003;Acero et al 2016;Zhang et al 2018;Koo et al 2016;Gao et al 2011a;Planck Collaboration et al 2016). It interacts with the nearby MC, and the CO observation revealed a half molecular ring structure surrounding the SNR, from east to north (Su et al 2014).…”

Section: Discussionmentioning

confidence: 99%

A Systematic Study of the Dust of Galactic Supernova Remnants. I. The Distance and the Extinction

Zhao

Jiang

et al. 2020

ApJ

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By combining the photometric, spectroscopic, and astrometric information of the stars in the sightline of SNRs, the distances to and the extinctions of 32 Galactic supernova remnants (SNRs) are investigated. The stellar atmospheric parameters are from the SDSS−DR14/APOGEE and LAMOST−DR5/LEGUE spectroscopic surveys. The multi-band photometry, from optical to infrared, are collected from the Gaia, APASS, Pan-STARRS1, 2MASS, and WISE surveys. With the calibrated Gaia distances of individual stars, the distances to 15 of 32 SNRs are well determined from their produced extinction and association with molecular clouds. The upper limits of distance are derived for 3 SNRs. The color excess ratios E(g P1 − λ)/E(g P1 − r P1 ) of 32 SNRs are calculated, and their variation with wavebands is fitted by a simple dust model. The inferred dust grain size distribution bifurcates: while the graphite grains have comparable size to the average ISM dust, the silicate grains are generally larger. Along the way, the average extinction law from optical to near-infrared of the Milky Way is derived from the 1.3 million star sample and found to agree with the CCM89 law with R V = 3.15. the sightline towards the SNR are selected, and their interstellar extinctions are calculated. Secondly, the distance to the SNR is estimated from the position where the extinction increases sharply due to the higher dust density of the SNR than its foreground ISM. Last, the extinction law and the dust properties of the SNR are derived. It should be clarified that the dust of SNR is merely produced by the SN ejecta. The dust produced by the SN ejecta is hardly more than a solar mass, which is shown by the case of young SNRs. For example, Matsuura et al. (2015) derived 0.8 M for SN 1987A, Bevan et al. (2017) derived ∼1.1 M for Cas A, and Owen & Barlow (2015) 0.6 M for the Crab Nebula.However, the expansion of the SN shock waves can sweep up massive enough ambient interstellar dust to produce relative large extinction jumps, in particular so considering that many SN explosions occur in large molecular clouds (MCs). Draine (2009) estimated the ISM mass to be swept by a SN explosion of about 1000 M . Compared to Paper I, we make a few important improvements: (1) the stellar distance is measured by Gaia and extracted from the newly released Gaia DR2 catalog. The distance from the Gaia parallax is a geometrical measurement without dependence on stellar model and interstellar extinction; (2) the extinction curve is derived from optical to IR, which reveals more accurately the properties of the SNR dust, whereas Paper I only studied the NIR extinction law that might be universal (Wang & Jiang 2014); (3) the study is systematic by including many more SNRs and the conclusion will be drawn from a wider range of SNRs.The paper is organized as follows. In Section 2, we describe the data sets and objects used in this work and the quality control to build the star sample. The methods underpinning the determination of intrinsic color indices and extinctions are introduced i...

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Section: Discussionmentioning

confidence: 99%

A Systematic Study of the Dust of Galactic Supernova Remnants. I. The Distance and the Extinction

Zhao

Jiang

et al. 2020

ApJ

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“…The X-ray emission from IC 443 is composed of extended thermal X-ray emission and a number of isolated hard X-ray sources whose emission includes both thermal and non-thermal components (e.g., Petre et al 1988;Bocchino & Bykov 2000Bocchino et al 2008). The latter could be a product of the SNR ejecta (or the pulsar wind nebula; PWN) and the surrounding shocked molecular clumps (see Zhang et al 2018, and references therein). The gamma-ray emission from IC 443 seems to be associated with the interaction of cosmic rays accelerated at the shock front and the nearby molecular clouds (Tavani et al 2010;Abdo et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Modeling the mixed-morphology supernova remnant IC 443

Ustamujic

Orlando

Greco

et al. 2021

A&A

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Context. The morphology and the distribution of material observed in supernova remnants (SNRs) reflect the interaction of the supernova (SN) blast wave with the ambient environment, the physical processes associated with the SN explosion, and the internal structure of the progenitor star. IC 443 is a mixed-morphology (MM) SNR located in a quite complex environment: it interacts with a molecular cloud in the northwestern and southeastern areas and with an atomic cloud in the northeast. Aims. In this work, we aim to investigate the origin of the complex morphology and multi-thermal X-ray emission observed in SNR IC 443 through the study of the effect of the inhomogeneous ambient medium in shaping its observed structure and an exploration of the main parameters characterizing the remnant. Methods. We developed a 3D hydrodynamic (HD) model for IC 443, which describes the interaction of the SNR with the environment, parametrized in agreement with the results of the multi-wavelength data analysis. We performed an ample exploration of the parameter space describing the initial blast wave and the environment, including the mass of the ejecta, the energy and position of the explosion, as well as the density, structure, and geometry of the surrounding clouds. From the simulations, we synthesized the X-ray emission maps and spectra and compared them with actual X-ray data collected by XMM-Newton. Results. Our model explains the origin of the complex X-ray morphology of SNR IC 443 in a natural way, with the ability to reproduce, for the first time, most of the observed features, including the centrally-peaked X-ray morphology (characteristic of MM SNRs) when considering the origin of the explosion at the position where the pulsar wind nebula CXOU J061705.3+222127 was at the time of the explosion. In the model that best reproduces the observations, the mass of the ejecta and the energy of the explosion are ~7 M⊙ and ~1 × 1051 erg, respectively. From the exploration of the parameter space, we find that the density of the clouds is n > 300 cm−3 and that the age of SNR IC 443 is ~8000 yr. Conclusions. The observed inhomogeneous ambient medium is the main property responsible for the complex structure and the X-ray morphology of SNR IC 443, resulting in a very asymmetric distribution of the ejecta due to the off-centered location of the explosion inside the cavity formed by the clouds. It can be argued that the centrally peaked morphology (typical of MM SNRs) is a natural consequence of the interaction with the complex environment. A combination of high resolution X-ray observations and accurate 3D HD modeling is needed to confirm whether this scenario is applicable to other MM SNRs.

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“…IC443 (Index Catalogue 443) is a SNR located in the constellation of Gemini at Galactic coordinates (𝑙, 𝑏) = (189.06 • , 3.24 • ); it is therefore found close to the Galactic anticentre, with a lower emission from the neighbouring background compared to W49 and W51, which are much closer in projection to the Galactic bulge. This source has been extensively observed throughout the whole spectrum, including radio (Kundu & Velusamy 1972;Green 1986;Castelletti et al 2011;Mitra et al 2014;Planck Collaboration et al 2016a;Egron et al 2016Egron et al , 2017, optical (Fesen 1984;Ambrocio-Cruz et al 2017), X-ray (Petre et al 1988;Matsumura et al 2017;Greco et al 2018;Hirayama et al 2019;Zhang et al 2018) and 𝛾-ray (Torres et al 2003;Tavani et al 2010) frequencies. IC443 angular size is ∼ 45 (Green 2014); the related supernova event occured in between 3 (Petre et al 1988) and 30 kyr ago (Olbert et al 2001), with more recent estimates favouring ∼ 20 kyr (Lee et al 2008).…”

Section: Ic443mentioning

confidence: 98%

QUIJOTE scientific results -- V. The microwave intensity and polarisation spectra of the Galactic regions W49, W51 and IC443

Tramonte,

Génova-Santos,

Rubiño-Martín

et al. 2023

Preprint

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We present new intensity and polarisation maps obtained with the QUĲOTE experiment towards the Galactic regions W49, W51 and IC443, covering the frequency range from 10 to 20 GHz at ∼ 1 deg angular resolution, with a sensitivity in the range 35-79 𝜇K beam −1 for total intensity and 13-23 𝜇K beam −1 for polarisation. For each region, we combine QUĲOTE maps with ancillary data at frequencies ranging from 0.4 to 3000 GHz, reconstruct the spectral energy distribution and model it with a combination of known foregrounds. We detect anomalous microwave emission (AME) in total intensity towards W49 at 4.7𝜎 and W51 at 4.0𝜎 with peak frequencies 𝜈 AME = (20.0 ± 1.4) GHz and 𝜈 AME = (17.7 ± 3.6) GHz respectively; this is the first detection of AME towards W51. The contamination from ultra-compact HII regions to the residual AME flux density is estimated at 10% in W49 and 5% in W51, and does not rule out the AME detection. The polarised SEDs reveal a synchrotron contribution with spectral indices 𝛼 s = −0.67 ± 0.10 in W49 and 𝛼 s = −0.51 ± 0.07 in W51, ascribed to the diffuse Galactic emission and to the local supernova remnant respectively. Towards IC443 in total intensity we measure a broken power-law synchrotron spectrum with cut-off frequency 𝜈 0,s = (114 ± 73) GHz, in agreement with previous studies; our analysis, however, rules out any AME contribution which had been previously claimed towards IC443. No evidence of polarised AME emission is detected in this study.

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NuSTAR Detection of a Hard X-Ray Source in the Supernova Remnant-molecular Cloud Interaction Site of IC 443

Cited by 13 publications

References 62 publications

A Systematic Study of the Dust of Galactic Supernova Remnants. I. The Distance and the Extinction

A Systematic Study of the Dust of Galactic Supernova Remnants. I. The Distance and the Extinction

Modeling the mixed-morphology supernova remnant IC 443

QUIJOTE scientific results -- V. The microwave intensity and polarisation spectra of the Galactic regions W49, W51 and IC443

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