Deep optical study of the mixed-morphology supernova remnant G 132.7+1.3 (HB3)

Abstract

We present optical ccd images of the large supernova remnant (SNR) G132.7$+$1.3 (HB3) covering its full extent for the first time, in the emission lines of H$\alpha +$[N II], [S II] and [O III], where new and known filamentary and diffuse structures are detected. These observations are supplemented by new low-resolution long-slit spectra and higher-resolution images in the same emission lines. Both the flux-calibrated images and spectra confirm that the optical emission originates from shock-heated gas since the [S II]/H$\alpha$ $>$ 0.4. Our findings are also consistent with the recently developed emission line ratio diagnostics for distinguishing SNRs from H II regions. A multi-wavelength comparison among our optical data and relevant observations in radio, X-rays, $\gamma$-rays and CO bands, provided additional evidence on the interaction of HB3 with the surrounding clouds and clarified the borders of the SNR and the adjacent cloud. We discuss the supernova (SN) properties and evolution that led to the current observables of HB3 and we show that the remnant has most likely passed at the pressure driven snowplow phase. The estimated SN energy was found to be $\left(3.7\pm 1.5\right)\times 10^{51}$ erg and the current SNR age $\left(5.1\pm 2.1\right)\times 10^4$ yrs. We present an alternative scenario according to which the SNR evolved in the wind bubble cavity excavated by the progenitor star and currently is interacting with its density walls. We show that the overall mixed morphology properties of HB3 can be explained if the SN resulted by a Wolf-Rayet progenitor star with mass $\sim 34{\mathrm{M}}_{\odot }$.

20 pages, 8 figures, accepted for publication in MNRAS

References in corpus (12)

• The Evolution of Supernovae in Circumstellar Wind Bubbles II: Case of a Wolf-Rayet star
• Numerical Simulations of Supernova Remnant Evolution in a Cloudy Interstellar Medium
• The Thermal Composite Supernova Remnant Kes 27 as Viewed by CHANDRA: Shock Reflection from a Cavity Wall
• Non-equilibrium ionization in mixed-morphology supernova remnants
• Far UV and Optical Emissions from Three Very Large Supernova Remnants Located at Unusually High Galactic Latitudes
• The Metal-enriched Thermal Composite Supernova Remnant Kesteven 41 (G337.8-0.1) in a Molecular Environment
• Non-thermal radio supernova remnants of exiled Wolf-Rayet stars
• G107.0+9.0: A New Large Optically Bright, Radio and X-Ray Faint Galactic Supernova Remnant in Cepheus
• Exploring the differences of integrated and spatially resolved analysis using integral field unit data: The case of Abell 14
• Interaction between the Supernova Remnant HB 3 and the Nearby Star-Forming Region W3
• The radio spectrum and magnetic field structure of SNR HB3
• First optical detection from the supernova remnant G 15.1-1.6

Cited by in corpus (4)

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• Rectangular core-collapse supernova remnants: application to Puppis A
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• New X-ray Supernova Remnants in NGC 7793