<i>XMM–Newton</i>studies of the supernova remnant G350.0−2.0

Карпова, А В; Shternin, P. S.; Zyuzin, D.; Danilenko, A.; Shibanov, Yu. A.

doi:10.1093/mnras/stw1898

Cited by 6 publications

(5 citation statements)

References 33 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…This is a crude approximation because actual Fe-L lines are ensembles of many different transitions, but it turned out to be sufficient for the present data given the energy resolution and statistics. Similar treatments are found in the analysis of other SNRs (e.g., Sawada & Koyama 2012, Sato et al 2016, and Karpova et al 2016. We found that combinations of a low-temperature CIE with the solar abundance and a high-temperature NEI with variable abundance gave relatively good fits.…”

Section: Single Ejecta Modelssupporting

confidence: 88%

Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3−0.9

Sawada

Tachibana

Uchida

et al. 2019

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

We present a 190 ks observation of the Galactic supernova remnant (SNR) G306.3−0.9 with Suzaku. To study ejecta properties of this possible Type Ia SNR, the absolute energy scale at the Fe-K band was calibrated to a level of uncertainty less than 10 eV by a cross-calibration with the Hitomi microcalorimeter using the Perseus cluster spectra. This enabled us for the first time to accurately determine the ionization state of the Fe Kα line of this SNR. The ionization timescale (τ ) of the Fe ejecta was measured to be log 10 τ (cm −3 s) =10.24±0.03, significantly smaller than previous measurements. Marginally detected Kα lines of Cr and Mn have consistent ionization timescales with Fe. The global spectrum was well fitted with shocked interstellar matter (ISM) and at least two ejecta components with different ionization timescales for Fe and intermediate mass elements (IME) such as S and Ar. One plausible interpretation of the one-order-of-magnitude shorter timescale of Fe than that of IME (log 10 τ =11.17±0.07) is a chemically stratified structure of ejecta. By comparing the X-ray absorption column to the H I distribution decomposed along the line of sight, we refined the distance to be ∼20 kpc. The large ISM-to-ejecta shocked mass ratio of ∼100 and dynamical timescale of ∼6 kyr place the SNR in the late Sedov phase. These properties are consistent with a stratified ejecta structure that has survived the mixing processes expected in an evolved supernova remnant.

show abstract

Section: Single Ejecta Modelssupporting

confidence: 88%

Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3−0.9

Sawada

Tachibana

Uchida

et al. 2019

Publications of the Astronomical Society of Japan

View full text Add to dashboard Cite

show abstract

“…Williams et al (2020). Some "blobs" with a significant 1.25 keV line emission were found also in a mixed-morphology SNR G350.0-2.0 by Karpova et al (2016). Therefore, more observations are needed to confirm or reject the apparent spectral excess in SNR G18.95-1.1.…”

Section: Discussionmentioning

confidence: 99%

Spatially resolved X-ray spectra of the Galactic SNR G18.95-1.1: SRG/eROSITA view

Bykov,

Uvarov,

Churazov

et al. 2021

Preprint

View full text Add to dashboard Cite

Aims. We study the X-ray emission of the galactic supernova remnant (SNR) G18.95-1.1 with the eROSITA telescope on board the Spectrum Röntgen Gamma (SRG) orbital observatory. In addition to the pulsar wind nebula that was previously identified and examined by ASCA and Chandra, we study the X-ray spectra of the bright SNR ridge, which is resolved into a few bright clumps. Methods. The wide field of view and the large collecting area in the 0.2 − 2.3 keV energy range of SRG/eROSITA allowed us to perform spatially resolved spectroscopy of G18.95-1.1. Results. The X-ray ridge of G18.95-1.1 is asymmetric, indicating either supernova ejecta asymmetry or their interaction with a cloud. The X-ray dim northern regions outside the pulsar wind nebula can be described by a thin thermal plasma emission with a temperature ∼0.3 keV and a solar composition. The X-ray spectra of a few bright clumps located along the southern ridge may be satisfactorily approximated by a single thermal component of the Si-rich ejecta at the collisional ionization equilibrium with a temperature of about 0.3 keV. The bright ridge can be alternatively fit with a single component that is not dominated by equilibrium ejecta with T∼ 0.6 keV. The high ratio of the derived Si/O abundances indicates that the ejecta originated in deep layers of the progenitor star. The plasma composition of a southern Si-rich clump and the bright ridge are similar to what was earlier found in the Vela shrapnel A and G.

show abstract

“…The ROSAT map of this source (see Fig. 1 in Karpova et al 2016) covers the entire SNR, showcasing that 350.0-2.0 is indeed a mixed morphology SNR. Leahy & Tian 2005;Araya 2013;Arias et al 2019b;Xiao et al 2022).…”

Section: Introductionmentioning

confidence: 85%

“…The authors identify some elongated filaments that could be associated with the SNR, and favour an interpretation whereby the source is actually more than one SNR aligned along the line of sight. Karpova et al (2016) observed G 350.0-2.0 with XMM-Newton, finding a plasma with mostly solar abundances and some regions of overabundant Fe. They estimated a distance of approximately 3 kpc, corresponding to a SNR diameter of 20 pc, and an age of ∼10 4 yr.…”

Section: Introductionmentioning

confidence: 98%

See 1 more Smart Citation

Two shell- and wing-shaped supernova remnants

Arias,

Zhou,

Chiotellis

et al. 2024

A&A

View full text Add to dashboard Cite

Supernova remnants (SNRs) are profoundly affected by their ambient medium. In particular, SNRs with a mixed morphology (characterised by a shell-like radio morphology and centrally filled X-ray emission) are thought to be the result of the interaction of a supernova explosion with a dense environment. In this work, we present carbon monoxide (CO) observations around two mixed morphology SNRs, VRO 42.05.01 and G 350.0-2.0, that look remarkably similar in continuum radio emission, showing what we refer to as a shell and wing shape. It has been proposed that the shell and wing shape is the result of environmental effects, in the form of a sharp density gradient or discontinuity. Therefore, our motivation for studying these two sources jointly is that if the dense molecular environment causes the development of these sources' shell and wing shape, then these two sources' environments must be similar. This is contrary to what we observe. In the case of VRO 42.05.01, we have found direct evidence of an interaction with its molecular environment, in the form of broadened 12CO line profiles, high to line ratios, and arc features in position-velocity space. We interpret some of these features to be associated with the SNR shock, and some of them to be due to the presence of a pre-supernova stellar wind. We have found no such features in the abundant molecular gas surrounding G 350.0-2.0. In addition to the spectral line analysis, we have used radio continuum data to make a spectral index map of G 350.0-2.0, and we see that the radio spectrum of G 350.0-2.0 steepens significantly at frequencies $<200$ MHz, much like that of VRO 42.05.01. In spite of their spectral and morphological similarities, these two sources look substantially different in their observed optical and infrared emission. The lack of large-scale correspondence between the radio continuum and the molecular material, in either case, as well as the differences in the excitation and morphological properties of the molecular gas surrounding both sources, lead us to conclude that the shell and wing morphology of these two sources is not due to interactions with a similar ambient molecular interstellar medium.

show abstract

XMM–Newtonstudies of the supernova remnant G350.0−2.0

Cited by 6 publications

References 33 publications

Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3−0.9

Ionization age of iron ejecta in the Galactic Type Ia supernova remnant G306.3−0.9

Spatially resolved X-ray spectra of the Galactic SNR G18.95-1.1: SRG/eROSITA view

Two shell- and wing-shaped supernova remnants

Contact Info

Product

Resources

About