Shocked Molecular Hydrogen and Broad CO lines from the Interacting Supernova Remnant HB 3

Rho, J.; Jarrett, T. H.; Tram, L. N.; Lim, W.; Reach, W. T.; Bieging, J.; Lee, H. -G.; Koo, B. -C.; Whitney, B.

doi:10.48550/arxiv.2105.10617

Cited by 3 publications

(5 citation statements)

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“…G132.7+01.3 has been studied in γ-rays, X-rays, radio, infrared and mm wavelengths (e.g. Routledge et al 1991;Fesen et al 1995;Lazendic & Slane 2006;Zhou et al 2016;Rho et al 2021, see also Introduction). Here we present the main results and conclusions regarding the properties and evolution of HB3 as extracted by the comparison of its emission properties in different electromagnetic bands.…”

Section: Comparison With Other Wavelengthsmentioning

confidence: 99%

“…This evidence was verified by multimeter observations of CO lines, conducted by Zhou et al (2016) which revealed a substantial amount of molecular gas around −43 km s −1 , being morphologically and dynamically correlated with HB3. Finally, shocked molecular hydrogen (H 2 ) and broad CO was recently detected in the near/mid infrared and millimeter bands, respectively, whose morphological and kinematic properties provide an additional evidence on the interaction of the SNR with the surrounding clouds (Rho et al 2021).…”

Section: Introductionmentioning

confidence: 99%

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

Boumis,

Chiotellis,

Fragkou

et al. 2022

Preprint

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We present optical ccd images of the large supernova remnant (SNR) G132.71.3 (HB3) covering its full extent for the first time, in the emission lines of Hα[N ], [S ] and [O ], 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 ]/Hα > 0.4. Our findings are also consistent with the recently developed emission line ratio diagnostics for distinguishing SNRs from H regions. A multi-wavelength comparison among our optical data and relevant observations in radio, X-rays, γ-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 3.7 ± 1.5 × 10 51 erg and the current SNR age 5.1 ± 2.1 × 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 ∼ 34 M .

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Section: Comparison With Other Wavelengthsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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

Boumis,

Chiotellis,

Fragkou

et al. 2022

Preprint

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“…We follow the same roadmap for prediction of CO line profile with IC443. Excition models were used to estimate shock properties in both observations of van Dishoeck et al (1993) and Rho et al (2021). Reach et al (2019) has developed theoretical line profile prediction for H 2 from various observation of IC443 B, C and G, which will served as useful shock diagnostic.…”

Section: Line Profile Fits For Ic443mentioning

confidence: 99%

Modeling CO Line Profiles in Shocks of W28 and IC44

Fuda¹,

Tram²,

Reach³

2021

Preprint

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Purely-rotational CO ( J = ±1) arising from magneto-hydrodynamic shock in supernova -molecular cloud interaction is an effective shock tracer. In this work we present a new theoretical radiative transfer framework for predicting the line profile of CO with the Paris-Durham shock model. We generated line profile predictions for CO emission produced by slow, magnetized C-shocks of ∼ 10 4 cm −3 and 35 ≤ V Shock ≤ 50 km s −1 . The numerical framework to reproduce CO line profile utilizes the Large Velocity Gradient (LVG) approximation and the omission of optically-thick plane-parallel slabs. With this framework, we generated predictions for various CO lines up to J = 16 at multiple locations in supernova remnants W28 and IC443. We found that CO line profile prediction offers robust constraints of shock velocity and preshock density while requiring fewer number of CO lines.

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“…SNR-MC interactions have been intensively studied by observations of the shocked regions by using both molecular and atomic gas tracers (see e.g., Wootten 1977;Denoyer 1979a,b;Wootten 1981;Denoyer 1983;Tatematsu et al 1985Tatematsu et al , 1987Fukui & Tatematsu 1988;Tatematsu et al 1990a,b;White et al 1987;van Dishoeck et al 1993;White 1994;Koo & Moon 1997a,b;Seta et al 1998Seta et al , 2004Wilner et al 1998;Arikawa et al 1999;Reach & Rho 1999Reach et al 2002Reach et al , 2005aNeufeld et al 2007;Yuan & Neufeld 2011;Gusdorf et al 2012;Anderl et al 2014;Reach et al 2019;Dell'Ova et al 2020;Rho et al 2021). Commonly, the rovibrational lines of H 2 and CO are notably used to characterize the SNR shocks.…”

Section: Introductionmentioning

confidence: 99%

“…Owing to a dipole moment, CO complements H 2 by probing the cooler and denser part in the shocked regions. Both the excitation diagram ("Boltzmann plot"), relation between the column density of the rotationally excited levels and their energy above the ground state , e.g., Neufeld et al 2007;Yuan & Neufeld 2011), and the resolved velocity profiles (e.g., Reach et al 2019;Rho et al 2021) have been used to constrain the physical properties of the shocked gas.…”

Section: Introductionmentioning

confidence: 99%

Submillimeter observations of molecular gas interacting with the supernova remnant W28

Мазумдар

Tram

Wyrowski

et al. 2022

A&A

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Context. Supernovae (SNe) inject large amounts of energy and chemically enriched materials into their surrounding interstellar medium and, in some instances, into molecular clouds (MCs). The interaction of a supernova remnant (SNR) with a MC plays a crucial role in the evolution of the cloud's physical and chemical properties. Despite their importance, only a handful of studies have been made addressing the molecular richness in molecular clouds impacted by SNRs. (Sub)millimter wavelength observations of MCs affected by SNRs can be used to build a census of their molecular richness, which in turn can motivate various chemical and physical models aimed at explaining the chemical evolution of the clouds. Aims. We carried out multi-molecule and multi-transition observations toward the molecular region F abutting the SNR W28, containing 1720 MHz OH masers, well-established tracers of SNR-MC interactions. We used the detected lines to constrain the physical conditions of this region. Methods. We used the APEX Telescope to observe molecular lines in the frequency range 213−374 GHz. We used non-local thermodynamic equilibrium (non-LTE) RADEX modeling to interpret the observational data. Results. We detected emission from multiple molecular species in the region, namely CH 3 OH, H 2 CO, SO, SiO, CN, CCH, NO, CS, HCO + , HCN, HNC, N 2 H + , CO, and from the isotopologues of some of them. We report the first detection of thermally excited (nonmaser) CH 3 OH emission toward a SNR. Employing non-LTE RADEX modeling of multiple H 2 CO and CH 3 OH lines, we constrained the kinetic temperature and spatial density in the molecular gas. The gas kinetic temperatures range from 60 to 100 K while the spatial density of the gas ranges from 9 × 10 5 to 5 × 10 6 cm −3 . We obtained an ortho-para ratio ∼2 for H 2 CO, which indicates that formaldehyde is most likely formed on dust grain surfaces and not in the gas phase. Conclusions. Our results show that molecules as complex as H 2 CO and CH 3 OH can be detected in SNR-MC interactions. This could motivate chemical modeling to explore their formation pathways.

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Shocked Molecular Hydrogen and Broad CO lines from the Interacting Supernova Remnant HB 3

Cited by 3 publications

References 75 publications

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

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

Modeling CO Line Profiles in Shocks of W28 and IC44

Submillimeter observations of molecular gas interacting with the supernova remnant W28

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