Global X-Ray Properties of the Vela and Puppis A Supernova Remnants

Silich, Emily; Kaaret, Philip; Zajczyk, A.; LaRocca, Daniel M.; Bluem, J.; Ringuette, Rebecca; Jahoda, K.; Küntz, K. D.

doi:10.3847/1538-3881/ab93d3

Cited by 9 publications

(6 citation statements)

References 23 publications

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“…HaloSat data on the Cygnus superbubble, a region of bright soft X-ray emission in the direction of local spiral arm, show that the temperature and absorption are consistent across different parts, suggesting a singular origin, potentially as a hypernova remnant [19]. HaloSat observations have also been used to make the first measurement of the total X-ray luminosity of the Vela supernova remnant using CCD-level energy resolution [20].…”

Section: Science Resultsmentioning

confidence: 99%

The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics

Feng¹,

Kaaret²

2022

Preprint

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Astronomical observations in the X-ray band are subject to atmospheric attenuation and have to be performed in the space. CubeSats offer a cost effective means for space-based X-ray astrophysics but allow only limited mass and volume. In this article, we describe two successful CubeSat-based missions, HaloSat and PolarLight, both sensitive in the keV energy range. HaloSat was a 6U CubeSat equipped with silicon drift detectors. It conducted an all-sky survey of oxygen line emission and revealed the clumpy nature of the circumgalactic medium surrounding the Milky Way. PolarLight is a dedicated X-ray polarimeter performing photoelectron tracking using a gas pixel detector in a 1U payload. It observed the brightest X-ray objects and helped constrain their magnetic field or accretion geometry. Onorbit operation of both missions for multiple years demonstrates the capability of CubeSats as an effective astronomical platforms. The rapid time scales for development and construction of the missions makes them particularly attractive for student training.

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Section: Science Resultsmentioning

confidence: 99%

The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics

Feng¹,

Kaaret²

2022

Preprint

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“…The blast-wave velocity can be estimated from X-ray observations. A recent analysis by Silich et al (2020), who examined X-ray emission from the entire Vela SNR, indicates that a two-temperature thermal plasma model provides the best fit to the X-ray data. The cooler of the two components, which Silich et al (2020) found to be in collisional ionization equilibrium at T = 2.2 × 10 6 K, implies a blast-wave velocity of v b ≈ 400 km s −1 .…”

Section: Discussionmentioning

confidence: 99%

“…A recent analysis by Silich et al (2020), who examined X-ray emission from the entire Vela SNR, indicates that a two-temperature thermal plasma model provides the best fit to the X-ray data. The cooler of the two components, which Silich et al (2020) found to be in collisional ionization equilibrium at T = 2.2 × 10 6 K, implies a blast-wave velocity of v b ≈ 400 km s −1 . This result for v b is in very good agreement with a determination based on a detailed examination of thermal and nonthermal X-ray emission from the Vela SNR by Mayer et al (2023).…”

Section: Discussionmentioning

confidence: 99%

Observations of Multiphase, High-velocity, Shocked Gas in the Vela Supernova Remnant*

Ritchey

2023

ApJ

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We present an analysis of high-resolution far-UV archival spectra obtained with the Space Telescope Imaging Spectrograph on the Hubble Space Telescope of the star HD 75309, which probes high-velocity shocked gas in the Vela supernova remnant (SNR). We examine high-velocity features from intrinsically strong absorption lines of O i, Si ii, Si ii*, C ii, C ii*, and Si iii. We also detect high-velocity components in the N v doublet and compare these features to observations of high-velocity O vi absorption, available from archival Far Ultraviolet Spectroscopic Explorer data. Kinetic temperatures are derived from the observed fractional abundances of the various ions, while gas densities and thermal pressures are obtained from the relative populations in excited fine-structure levels of C ii and Si ii. Our results indicate that the highly ionized species at high velocity probe gas in a region immediately behind a shock driven into an interstellar cloud, while the lower-ionization species trace material further downstream in the cooling region of the postshock flow. Low-velocity N v and O vi absorption may trace gas in a conductive boundary layer between the unshocked portion of the cloud and the hot X-ray-emitting intercloud medium. Temporal variations in high-velocity Ca ii absorption features observed toward HD 75309 further confirm the highly inhomogeneous nature of the interstellar medium interacting with the Vela SNR.

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“…Yusef-Zadeh et al (2003) give a prescription for estimating the ionization rate due to X-rays right at the edge of an SNR. Taking the X-ray luminosities of the Vela SNR and Puppis A reported by Silich et al (2020) and the X-ray flux of RX J0852−4622 reported by Takeda et al (2016) and using the methods of Yusef-Zadeh et al (2003) scaled up by a factor of 2 (for H 2 ionization), I compute the X-ray ionization rates at the edge of these SNRs. I find 3 × 10 −17 s −1 , 2 × 10 −18 s −1 , and 4 × 10 −15 s −1 for Vela, RX J0852−4622, and Puppis A, respectively.…”

Section: Cosmic-ray Ionization Ratesmentioning

confidence: 99%

Absorption-line Observations of H3+ and CO in Sight Lines Toward the Vela and W28 Supernova Remnants

Indriolo¹

2023

ApJ

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Supernova remnants act as particle accelerators, providing the cosmic-ray protons that permeate the interstellar medium and initiate the ion–molecule reactions that drive interstellar chemistry. Enhanced fluxes of cosmic-ray protons in close proximity to supernova remnants have been inferred from observations tracing particle interactions with nearby molecular gas. Here I present observations of H 3 + and CO absorption, molecules that serve as tracers of the cosmic-ray ionization rate and gas density, respectively, in sight lines toward the W28 and Vela supernova remnants. Cosmic-ray ionization rates inferred from these observations range from about 2 to 10 times the average value in Galactic diffuse clouds (∼3 × 10−16 s−1), suggesting that the gas being probed is experiencing an elevated particle flux. While it is difficult to constrain the line-of-sight locations of the absorbing gas with respect to the supernova remnants, these results are consistent with a scenario where cosmic rays are diffusing away from the acceleration site and producing enhanced ionization rates in the surrounding medium.

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Global X-Ray Properties of the Vela and Puppis A Supernova Remnants

Cited by 9 publications

References 23 publications

The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics

The HaloSat and PolarLight CubeSat Missions for X-ray Astrophysics

Observations of Multiphase, High-velocity, Shocked Gas in the Vela Supernova Remnant*

Absorption-line Observations of H3+ and CO in Sight Lines Toward the Vela and W28 Supernova Remnants

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