Revisiting the distance, environment and supernova properties of SNR G57.2+0.8 that hosts SGR 1935+2154

Zhou, Ping; Zhou, Xin; Chen, Yang; Wang, Jie-Shuang; Vink, Jacco; Wang, Yuan

doi:10.48550/arxiv.2005.03517

Cited by 22 publications

(34 citation statements)

References 32 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Because 1 Throughout the paper, we adopt the Galatic electron model YMW16 encoded in the pygedm package of Python because this model is believed to give more reliable estimates than NE2001 in general (see Table 6 of Yao et al 2017). SNR G57.2+0.8 has possibly reached the end of the Sedov-Taylor phase or entered the snowplow phase due to the non-detection of X-ray emission (Kothes et al 2018;Zhou et al 2020), the DM SNR from the ionized medium (including shocked SN ejecta and shocked swept ambient medium 2 ), can be estimated by…”

Section: Constant Ismmentioning

confidence: 99%

“…Due to the position of the SGR at the geometric center of the SNR in a relatively uncrowded region of the Galactic plane (Gaensler 2014), to the distance estimates and approximate ages inferred for the SGR and the SNR, it is believed that they are likely physically related (Kothes et al 2018). Moreover, the relatively small age (3.6 kyr) of the SGR supports that its SNR should be visible (Zhou et al 2020). All these pieces of evidence strongly suggest a likely association between the SGR and the SNR.…”

Section: Introductionmentioning

confidence: 99%

“…In the literature, however, the distance of SNR G57.2+0.8 has a large range and remains highly debated even though various methods have been used, e.g., the statistical radio surface-brightness-to-diameter relation (∼ 9.1 kpc, Pavlović et al 2013), the empirical relation between the HI column density N H and the dispersion measure (DM) (11.7 ± 2.8 kpc, Surnis et al 2016), and the local standard of rest (LSR) velocity measure via HI absorption feature (12.5 ± 1.5 kpc, Kothes et al 2018), (4.5 − 9.0 kpc, Ranasinghe et al 2018), or via CO gas towards the SNR (6.6 ± 0.7 kpc, Zhou et al 2020). For SGR 1935+2154, Kozlova et al (2016) gave an upper limit < 10 kpc through the scattered correlation between the squares of the radii of the emitting areas and the corresponding black-body temperatures, and Mereghetti et al (2020) obtained 2.2 − 7.1 kpc through the observation of the bright dust-scattering X-ray ring.…”

Section: Introductionmentioning

confidence: 99%

See 2 more Smart Citations

On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

Zhong,

Dai,

Zhang

et al. 2020

Preprint

View full text Add to dashboard Cite

Owing to the detection of an extremely bright fast radio burst (FRB) 200428 associated with a hard X-ray counterpart from the magnetar soft gamma-ray repeater (SGR) 1935+2154, the distance of SGR 1935+2154 potentially hosted in the supernova remnant (SNR) G57.2+0.8 can be revisited. Under the assumption that the SGR and the SNR are physically related, in this Letter, by investigating the dispersion measure (DM) of the FRB contributed by the foreground medium of our Galaxy and the local environments and combining with other observational constraints, we find that the distance of SGR 1935+2154 turns out to be 9.0 ± 2.5 kpc and the SNR radius falls into 10 to 18 pc since the local DM contribution is as low as 0 − 18 pc cm −3 . These results are basically consistent with the previous studies. In addition, an estimate for the Faraday rotation measure of the SGR and SNR is also carried out.

show abstract

Section: Constant Ismmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

Zhong,

Dai,

Zhang

et al. 2020

Preprint

View full text Add to dashboard Cite

show abstract

“…79, J2000.0; Israel et al 2016) and the JPL planetary ephemeris DE 200. In the following, we adopt a distance of 6.6 kpc (Zhou et al 2020) and quote all uncertainties at 1σ confidence level (c.l. ).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

The X-ray reactivation of the radio bursting magnetar SGR 1935+2154

Borghese,

Zelati,

Rea

et al. 2020

Preprint

View full text Add to dashboard Cite

A few years after its discovery as a magnetar, SGR 1935+2154 started a new burst-active phase on 2020 April 27, accompanied by a large enhancement of its X-ray persistent emission. Radio single bursts were detected during this activation, strengthening the connection between magnetars and fast radio bursts. We report on the X-ray monitoring of SGR 1935+2154 from ∼3 days prior to ∼3 weeks after its reactivation, using Swift, NuSTAR, and NICER. We detected X-ray pulsations in the NICER and NuSTAR observations, and constrained the spin period derivative to | Ṗ | < 6×10 −11 s s −1 (3σ c.l.). The pulse profile showed a variable shape switching between single and double-peaked as a function of time and energy. The pulsed fraction decreased from ∼ 34% to ∼11% (5-10 keV) over ∼10 days. The X-ray spectrum was well fit by an absorbed blackbody model with temperature decreasing from kT BB ∼ 1.6 to 0.6-0.7 keV, plus a non-thermal component (Γ ∼ 1.2) observed up to ∼25 keV with NuSTAR. The 0.3-10 keV X-ray luminosity increased in less than four days from ∼ 4 × 10 33 erg s −1 to about 2.5×10 35 erg s −1 and then decreased again to 1.4×10 34 erg s −1 over the following three weeks of the outburst. We also detected several X-ray bursts, with properties typical of short magnetar bursts.

show abstract

“…We interpret and discuss the results in §4. We note that the estimated distance to SGR J1935+2154 ranges from ∼2 to 9 kpc (see Zhong et al 2020, and the references therein) including the most recent estimations from the dust-scattering halo of 4.5 +2.8 −1.3 kpc (Mereghetti et al 2020) and from the host supernova remnant of 6.6±0.7 kpc (Zhou et al 2020); here we use the distance of 9 kpc, consistent with Lin et al (2020).…”

mentioning

confidence: 90%

Fermi-GBM Observations of the SGR J1935+2154 Burst Forest

Kaneko,

Gogus,

Baring

et al. 2021

Preprint

View full text Add to dashboard Cite

During April and May 2020, SGR J1935+2154 emitted hundreds of short bursts and became one of the most prolific transient magnetars. At the onset of the active bursting period, a 130-s burst "forest", which included some bursts with peculiar time profiles, were observed with the F ermi/Gamma-ray Burst Monitor. In this paper, we present the results of time-resolved spectral analysis of this burst "forest" episode, which occurred on April 27 th , 2020. We identify thermal spectral components prevalent during the entire 130-s episode; high-energy maxima appear during the photon flux peaks, which are modulated by the spin period of the source. Moreover, the evolution of the νF ν spectral hardness (represented by E peak or blackbody temperature) within the lightcurve peaks is anti-correlated with the pulse phases extrapolated from the pulsation observed within the persistent soft X-ray emission of the source six hours later. Throughout the episode, the emitting area of the high-energy (hotter) component is 1-2 orders of magnitude smaller than that for the low-energy component. We interpret this with a geometrical viewing angle scenario, inferring that the high-energy component likely originates from a low-altitude hotspot located within closed toroidal magnetic field lines.

show abstract

Revisiting the distance, environment and supernova properties of SNR G57.2+0.8 that hosts SGR 1935+2154

Cited by 22 publications

References 32 publications

On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

On the Distance of SGR 1935+2154 Associated with FRB 200428 and Hosted in SNR G57.2+0.8

The X-ray reactivation of the radio bursting magnetar SGR 1935+2154

Fermi-GBM Observations of the SGR J1935+2154 Burst Forest

Contact Info

Product

Resources

About