ERRATUM: “THE RADIO SURFACE BRIGHTNESS TO DIAMETER RELATION FOR GALACTIC SUPERNOVA REMNANTS: SAMPLE SELECTION AND ROBUST ANALYSIS WITH VARIOUS FITTING OFFSETS” (2013, ApJS, 204, 4)

Pavlović, Marko Z.; Urošević, D.; Vukotić, Branislav; Арбутина, Б.; Göker, Ümit Deniz

doi:10.1088/0067-0049/205/1/10

Cited by 25 publications

(68 citation statements)

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“…The empirical power-law relation between the radio brightness and the linear diameter is also used to determine the distance of SNRs once the radio brightness has been measured. This method suffers the errors from the dispersion of the empirical relation that the power-law index varies from about 2 to 6 (Case & Bhattacharya 1998;Guseinov et al 2003;Pavlović et al 2013), and the index error can be as large as 40% (Zhu & Tian 2014).…”

Section: Introductionmentioning

confidence: 99%

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: Introductionmentioning

confidence: 99%

Distances to the supernova remnants in the inner disk

Wang

Zhang

Jiang

et al. 2020

A&A

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“…Similar dependence exists in Σ − D relations simulated in this paper as a consequence of hierarchical distribution of matter in a fractal cloud. The indication of such a dependence is also seen in empirical relations from Pavlović et al (2013) for 28 SNRs in molecular clouds associated with dense ambient medium,…”

Section: σ − D Relations For Supernova Remnantsmentioning

confidence: 54%

“…This is called the orthogonal regression. The results from Pavlović et al (2013) showed that the orthogonal regression gives the most stable fit parameters estimates and should be favoured over the other types of regressions.…”

Section: σ − D Relations For Supernova Remnantsmentioning

confidence: 99%

“…On the other hand, the Σ − D relation is most often (almost in all cases) calibrated with a vertical regression. However this type of regression tends to underestimate the slope β especially at its larger values (Pavlović et al 2013). Thus, we select the orthogonal regression as a preferred fitting procedure for the work done in this paper.…”

Section: σ − D Relations For Supernova Remnantsmentioning

confidence: 99%

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Interstellar medium structure and the slope of the radio Σ–Drelation of supernova remnants

Kostić

Vukotić

Urošević

et al. 2016

Mon. Not. R. Astron. Soc.

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We analyze the influence of fractal structure of the interstellar matter (ISM) density on the parameter values for the radio surface brightness to diameter (Σ − D) relation for supernovae remnants (SNRs). We model a dense ISM as a molecular cloud with fractal density structure. SNRs are modelled as spheres of different radius scattered in the modelled ISM. The surface brightness of the SNRs is calculated from the simple relation Σ ∝ ρ 0.5 D −3.5 and also from the parametrized more general form Σ ∝ ρ η D −β0 . Our results demonstrate that empirical Σ − D slopes that are steeper than the ones derived from theory, might be partly explained with the fractal structure of the ambient medium into which SNRs expand. The slope of the Σ − D relation steepens if the density of the regions where SNRs are formed is higher. The simple geometrical effects combined with the fractal structure of the ISM can contribute to a steeper empirical Σ − D slopes, especially for older remnants, and this is more pronounced if Σ has a stronger dependence on ambient density.

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“…For D < 36.5 pc, β = −2.47. Pavlović et al (2013) used orthogonal regression to replace the previous used vertical regression and the newly calculated slope, β = −4.8, is significantly steeper than those in previous works.…”

Section: The Empirical Surface Brightness(σ) -Diameter(d) Relationmentioning

confidence: 93%

Distances of Galactic supernova remnants

Zhu¹,

Wu²

2013

Proc. IAU

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Supernova remnants (SNRs) play a key role in understanding supernovae explosion mechanisms, exploring the likely sources of Galactic cosmic rays and the chemical enrichment of interstellar medium (ISM). Reliable distance determinations to Galactic SNRs are key to obtain their basic parameters, such as size, age, explosion energy, which helps us to study their environment and interstellar medium. We review the methods to determine the distances to SNRs and highlight the kinematic distance measurement by Hi absorption and CO emission observations.

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ERRATUM: “THE RADIO SURFACE BRIGHTNESS TO DIAMETER RELATION FOR GALACTIC SUPERNOVA REMNANTS: SAMPLE SELECTION AND ROBUST ANALYSIS WITH VARIOUS FITTING OFFSETS” (2013, ApJS, 204, 4)

Cited by 25 publications

References 0 publications

Distances to the supernova remnants in the inner disk

Distances to the supernova remnants in the inner disk

Interstellar medium structure and the slope of the radio Σ–Drelation of supernova remnants

Distances of Galactic supernova remnants

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