Distances and Evolutionary States of Supernova Remnant G18.9-1.1 and Candidate G28.6+0.0

Ranasinghe, S.; Leahy, D. A.; Wu, Tian

doi:10.4236/jhepgc.2020.61002

Cited by 3 publications

(4 citation statements)

References 28 publications

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“…Based on this evidence, we suggest that the remnant is associated with the +64.4 km s −1 MC, with the kinematic distance estimated as 3.8 ± 0.4 kpc. The near kinematic distance obtained here is consistent with the H I absorption result in previous work (Ranasinghe et al 2020).…”

Section: Appendix a Individual Snrssupporting

confidence: 93%

“…G18.9−1.1. A spatial correlation between this SNR and the MC at +25.6 km s −1 was found (Traverso et al 1999), and H I absorption features were detected up to ∼+23 km s −1 (Furst et al 1989;Ranasinghe et al 2020). Nevertheless, near-infrared H 2 lines were detected at +70 km s −1 by Lee et al (2020).…”

Section: Appendix a Individual Snrsmentioning

confidence: 81%

“…The SNRC may be associated with the +43.3 or +75.7 km s −1 components. The presence of H I absorption up to the tangent point shown by Ranasinghe et al (2020) indicates that the SNR is at a far kinematic distance. The kinematic distance of the +43.3 km s −1 component is estimated as 10.8 ± 0.4 kpc, and the far kinematic distance of the +75.7 km s −1 component is estimated as 8.2 ± 0.6 kpc.…”

Section: Data Availabilitymentioning

confidence: 97%

“…G28.56+0.00. This SNRC was considered to be related to a nearby H II region at +96.6 km s −1 , based on their very similar H I absorption spectra (Ranasinghe et al 2020). The east of the SNRC is adjacent to an H II region at +43 km s −1 .…”

Section: Data Availabilitymentioning

confidence: 99%

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A Systematic Study of Associations between Supernova Remnants and Molecular Clouds

Zhou,

Su,

Yang

et al. 2023

ApJS

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We universally search for evidence of kinematic and spatial correlation of supernova remnant (SNR) and molecular cloud (MC) associations for nearly all SNRs in the coverage of the Milky Way Imaging Scroll Painting CO survey, i.e., 149 SNRs, 170 SNR candidates, and 18 pure pulsar wind nebulae in 1° < l < 230° and −5.°5 < b < 5.°5. Based on high-quality and unbiased 12CO/13CO/C18O (J = 1–0) survey data, we apply automatic algorithms to identify broad lines and spatial correlations for molecular gas in each SNR region. The 91% of SNR–MC associations detected previously are identified in this paper by CO line emission. Overall, there could be as high as 80% of SNRs associated with MCs. The proportion of SNRs associated with MCs is high within the Galactic longitude less than ∼50°. Kinematic distances of all SNRs that are associated with MCs are estimated based on systemic velocities of associated MCs. The radii of SNRs associated with MCs follow a lognormal distribution, which peaks at ∼8.1 pc. The progenitor initial mass of these SNRs follows a power-law distribution with an index of ∼−2.3 that is consistent with the Salpeter index of −2.35. We find that SNR–MC associations are mainly distributed in a thin disk along the Galactic plane, while a small number are distributed in a thick disk. With the height of these SNRs from the Galactic plane below ∼45 pc, the distribution of the average radius relative to the height of them is roughly flat, and the average radius increases with the height when above ∼45 pc.

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Section: Appendix a Individual Snrssupporting

confidence: 93%

Section: Appendix a Individual Snrsmentioning

confidence: 81%

Section: Data Availabilitymentioning

confidence: 97%

Section: Data Availabilitymentioning

confidence: 99%

See 2 more Smart Citations

A Systematic Study of Associations between Supernova Remnants and Molecular Clouds

Zhou,

Su,

Yang

et al. 2023

ApJS

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Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo

Abbott

Abraham

et al. 2021

ApJ

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We present results of three wide-band directed searches for continuous gravitational waves from 15 young supernova remnants in the first half of the third Advanced LIGO and Virgo observing run. We use three search pipelines with distinct signal models and methods of identifying noise artifacts. Without ephemerides of these sources, the searches are conducted over a fRequency band spanning from 10 to 2 kHz. We find no evidence of continuous gravitational radiation from these sources. We set upper limits on the intrinsic signal strain at 95% confidence level in sample subbands, estimate the sensitivity in the full band, and derive the corresponding constraints on the fiducial neutron star ellipticity and r-mode amplitude. The best 95% confidence constraints placed on the signal strain are 7.7 × 10 −26 and 7.8 × 10 −26 near 200 Hz for the supernova remnants G39.2-0.3 and G65.7+1.2, respectively. The most stringent constraints on the ellipticity and r-mode amplitude reach 10 −7 and  10 −5 , respectively, at frequencies above ∼400 Hz for the closest supernova remnant G266.2-1.2/Vela Jr.

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Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants

Ranasinghe

Leahy

2022

ApJ

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We present a table of 215 supernova remnants (SNRs) with distances. New distances are found to SNR G51.26 + 0.11 of 6.6 ± 1.7 kpc using H i absorption spectra and to five other SNRs using maser/molecular cloud associations. We recalculate the distances and errors to all SNRs using a consistent rotation curve and provide errors where they were not previously estimated. This results in a significant distance revisions for 20 SNRs. Because of observational constraints and selection effects, there is an apparent deficit of observed number of Galactic SNRs. To investigate this, we employ two methods. The first method applies correction factors for the selection effects to derive the radial density distribution. The second method compares functional forms for the SNR surface density and selection function against the data to find which functions are consistent with the data. The total number of SNRs in the Galaxy is ∼3500 (Method 1) or in the range from ∼2400 to ∼5600 (Method 2). We conclude that the current observed number of SNRs is not yet complete enough to give a well-determined total SNR number or radial density function.

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Distances and Evolutionary States of Supernova Remnant G18.9-1.1 and Candidate G28.6+0.0

Cited by 3 publications

References 28 publications

A Systematic Study of Associations between Supernova Remnants and Molecular Clouds

A Systematic Study of Associations between Supernova Remnants and Molecular Clouds

Searches for Continuous Gravitational Waves from Young Supernova Remnants in the Early Third Observing Run of Advanced LIGO and Virgo

Distances, Radial Distribution, and Total Number of Galactic Supernova Remnants

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