Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5

Suzuki, Hiromasa; Bamba, Aya; Enokiya, Rei; Yamaguchi, Hiroya; Plucinsky, Paul P.; Odaka, Hirokazu

doi:10.3847/1538-4357/ab80ba

Cited by 13 publications

(14 citation statements)

References 53 publications

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“…As mentioned above, the reported distances to G359.1-0.5 and G347.3-0.5 are controversial in the literature. For G359.1-0.5, our derived distance 3.29 ± 0.47 kpc confirmed that this SNR is in the foreground of the Galactic center at a distance of ∼4 kpc by Suzuki et al (2020). For G347.3-0.5, our extinction distance of 4.56 ± 0.58 kpc is consistent with the suggested distance of 6 ± 1 kpc by Slane et al (1999).…”

Section: Comparison With the Other Distancessupporting

confidence: 87%

“…Moreover, the distances to some SNRs are still controversial, such as SNR G359.1-0.5. As summarized in Suzuki et al (2020) and Eppens et al (2020), there are suggestions that the SNR located at the Galactic Center, 8.5 kpc, or the foreground of the Galactic center, ∼4 kpc. In addition, even the kinematic distances in the literature are inconsistent with each other.…”

Section: Comparison With Previous Workmentioning

confidence: 99%

“…( f ) The distances listed in this column d other are mainly kinematic distances fromGreen (2019b). The symbols , , •, , , ×, •, and denote distances determined by different methods fromVukotić et al (2019),Lee et al (2019),Ranasinghe & Leahy (2018),Misanovic et al (2010),Shan et al (2018),Kilpatrick et al (2016),Jackson et al (2008), andSuzuki et al (2020), respectively.…”

mentioning

confidence: 99%

“…The symbol * denotes distances summarized inStafford et al (2019). The symbols ∧, ∨, , denote distances fromHewitt & Yusef-Zadeh (2009),Slane et al (1999),Vukotić et al (2019),Suzuki et al (2020), respectively.…”

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confidence: 99%

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Distances to the supernova remnants in the inner disk

Wang

Zhang

Jiang

et al. 2020

A&A

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Context. Distance measurements of supernova remnants (SNRs) are essential as accurate estimates of physical size, dust masses, and some other properties of SNRs depend critically on accurate distance measurements. However, the determination of SNR distances is still a tough task. Aims. Red clump stars (RCs) have a long history of being used as standard candles. In this work, we take RCs as tracers to determine the distances to a large group of SNRs in the inner disk. Methods. We first selected RC stars based on the near-infrared (IR) color-magnitude diagram. Then the distance to and extinction of RC stars were calculated. To extend the measurable range of distance, we combined near-IR photometric data from the 2MASS survey with the deeper UKIDSS and VVV surveys. With the help of the Gaia parallaxes, we also removed contaminants, including dwarfs and giants. Because an SN explosion compresses the surrounding interstellar medium, the SNR region would become denser and exhibit higher extinction than the surroundings. The distance of an SNR is then recognized by the position where the extinction and its gradient is higher than that of the ambient medium. Results. A total of 63 SNRs distances in the Galactic inner disk were determined and divided into three Levels A, B, and C with decreasing reliability. The distances to 43 SNRs are well determined with reliability A or B. The diameters and dust masses of SNRs were estimated with the obtained distance and extinction.

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Section: Comparison With the Other Distancessupporting

confidence: 87%

Section: Comparison With Previous Workmentioning

confidence: 99%

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confidence: 99%

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confidence: 99%

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Distances to the supernova remnants in the inner disk

Wang

Zhang

Jiang

et al. 2020

A&A

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“…As a demonstration of the application of mkacispback to actual celestial observations, we applied this tool to the X-ray emission of the supernova remnant G359.1−0.5, which is relatively old among supernova remnants and thus is a faint and diffuse CCD Name source, where the particle-induced background is relatively important (e.g., Suzuki et al 2020). An image of G359.1−0.5 is shown in the left panel of Fig.…”

Section: Application To a Celestial Observationmentioning

confidence: 99%

Spatial and temporal variations of the Chandra ACIS particle-induced background and development of a spectral-model generation tool

Suzuki

Plucinsky

Gaetz

et al. 2021

A&A

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Context. In X-ray observations, estimating the particle-induced background is important, especially for faint and/or diffuse sources. Although software exists to generate total (sky and detector) background data suitable for a given Chandra ACIS observation, no public software exists to model the particle-induced background separately. Aims. We aimed to understand the spatial and temporal variations of the particle-induced background of Chandra ACIS obtained in the two data modes, VFAINT and FAINT. Methods. Observations performed with ACIS in the stowed position shielded from the sky and the Chandra Deep Field South data sets were used. The spectra were modeled with a combination of the instrumental lines of Al, Si, Ni, and Au and continuum components. The spatial variations of the spectral shapes were modeled by dividing each CCD into 32 regions in the CHIPY direction. The temporal variations of the spectral shapes were modeled using all the individual ACIS-stowed observations. Results. Similar spatial variations of the spectral shapes were found in VFAINT and FAINT data, which are mainly due to the inappropriate correction of charge transfer inefficiency for events that convert in the frame-store regions. The temporal variation of the spectral hardness ratio is ∼ 10% maximum, which seems to be largely due to solar activity. We modeled this variation by modifying the spectral hardnesses according to the total count rate. Incorporating these properties, we developed a tool, mkacispback, to generate the particle-induced background spectral model corresponding to an arbitrary celestial observation. As an example application, we used the background spectrum produced by the mkacispback tool in an analysis of the unresolved cosmic X-ray background in the CDF-S observations. We found intensities of 3.10 (2.98-3.21) × 10 −12 erg s −1 cm −2 deg −2 in the 2-8 keV band and 8.35 (8.00-8.70) × 10 −12 erg s −1 cm −2 deg −2 in the 1-2 keV band, which are consistent with or lower than previous estimates. Conclusions. We modeled the spatial and temporal variations of the particle-induced background spectra of the Chandra ACIS-I and the S1, S2, and S3 CCDs, and developed a tool to generate a spectral model for an arbitrary celestial observation.

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Spatially resolved X-ray study of the mixed morphology SNR G359.1-0.5

Eppens,

Albacete Colombo,

Combi

et al. 2022

Monthly Notices of the Royal Astronomical Society

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We present a detailed spatially resolved X-ray study of Chandra observations towards the central region of the supernova remnant (SNR) G359.1-0.5. We removed 168 point-like sources and performed an adaptive smoothing on the entire field-of-view of the Chandra ACIS-I observation. The images obtained show a extended X-ray emission below 4.0 keV that partially fills the interior of G359.1-0.5. In order to characterize the X-ray emission, we divide the emitting area into ten different regions inside the remnant. We identify the presence of at least four emission lines that confirm the thin thermal plasma origin. All spectral regions are well fitted by a recombining plasma model (VRNEI) with an absorbing column density range from 1.5 to 2.1 × 1022 cm−2, and electron temperatures from 0.14 to 0.19 keV. We also calculated an average electron density of 0.7 cm−3, estimated an age of 2.8 × 104 years for the remnant, which can be lower if the filling factor is considered, and an X-ray luminosity of 1.6 × 1035 erg s−1. Finally, we show that the X-ray emission is morphologically anti-correlated with adjacent CO clouds interacting with the SNR. Our results favour that the recombining plasma inside G359.1-0.5 could be explained via adiabatic cooling.

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Uniform Distribution of the Extremely Overionized Plasma Associated with the Supernova Remnant G359.1-0.5

Cited by 13 publications

References 53 publications

Distances to the supernova remnants in the inner disk

Distances to the supernova remnants in the inner disk

Spatial and temporal variations of the Chandra ACIS particle-induced background and development of a spectral-model generation tool

Spatially resolved X-ray study of the mixed morphology SNR G359.1-0.5

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