Radio perspectives on the Monoceros SNR G205.5+0.5

Xiao, Li; Zhu, Meiping

doi:10.1051/0004-6361/201218938

Cited by 19 publications

(21 citation statements)

References 39 publications

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“…Xiao & Zhu (2012) showed that the radio spectral index (α) of the remnant is about −0.41, derived from 21 cm, 11 cm, and 6 cm radio continuum data, which is generally consistent with the result of previous works (Dickel & Denoyer 1975;Graham et al 1982). Throughout this paper, all directions are described in Galactic coordinates to match the MWISP CO survey.…”

Section: Snr G2055+05 (Monoceros Nebula)supporting

confidence: 91%

“…Odegard (1986) suggested that the SNR is probably located behind the Rosette Nebula because of the absorption of the remnant's nonthermal emission by the southern H ii region Sh 2-275. Xiao & Zhu (2012) also suggested that the SNR is probably associated with the Rosette Nebula because of the identified western partial shell structures at ∼ 15 km s −1 using the new Arecibo HI 21 cm data. The remnant displays contrasting optical filamentary structures mainly on its northwestern, western, and southwestern edges.…”

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 90%

“…They estimated the emission-weighted average kinematic distance of 1.6 kpc for these MCs, which is in agreement with the photometric distance to the Rosette Nebula. Recently, Xiao & Zhu (2012) revealed partial neutral hydrogen shell structures outside the western boundary of the remnant. The interesting HI shell in the velocity interval of 5-25 km s −1 seems to relate to SNR G205.5+0.5 and the Rosette Nebula, which strengthens the association between them.…”

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

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Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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We present CO observations toward three large supernova remnants (SNRs) in the third Galactic quadrant using the Purple Mountain Observatory Delingha 13.7 m millimeter-wavelength telescope. The observations are part of the high-resolution CO survey of the Galactic plane between Galactic longitudes l = −10• to 250• and latitudes b = −5• to 5• . CO emission was detected toward the three SNRs: G205.5+0.5 (Monoceros Nebula), G206.9+2.3 (PKS 0646+06), and G213.0−0.6. Both of SNRs G205.5+0.5 and G213.0−0.6 exhibit the morphological agreement (or spatial correspondences) between the remnant and the surrounding molecular clouds (MCs), as well as kinematic signatures of shock perturbation in the molecular gas. We confirm that the two SNRs are physically associated with their ambient MCs and the shock of SNRs is interacting with the dense, clumpy molecular gas. SNR G206.9+2.3, which is close to the northeastern edge of the Monoceros Nebula, displays the spatial coincidence with molecular partial shell structures at V LSR ∼ 15 km s −1 . While no significant line broadening has been detected within or near the remnant, the strong morphological correspondence between the SNR and the molecular cavity implies that SNR G206.9+2.3 is probably associated with the CO gas and is evolving in the low-density environment. The physical features of individual SNRs, together with the relationship between SNRs and their nearby objects, are also discussed.

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Section: Snr G2055+05 (Monoceros Nebula)supporting

confidence: 91%

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 90%

Section: Snr G2055+05 (Monoceros Nebula)mentioning

confidence: 99%

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Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Zhou

Yang

et al. 2017

ApJ

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“…The SNR and H ii region are thought to be interacting (Davies et al 1978;Smith 1973;Jaffe et al 1997;Fountain et al 1979;Gosachinskii & Khersonskii 1982). The polarization data presented by Xiao & Zhu (2012) do not cover the interface region between the two objects and show that the magnetic field in the Rosette Nebula is largely parallel to the Galactic plane. However, at a frequency of 5 GHz the observed polarization vectors are the result of either highly rotated background polarized synchrotron emission, considering the high RMs of about 500 rad m −2 measured in the nebula (Sect.…”

Section: The Rosette Nebula and The Mon Ob2 Molecular Cloudmentioning

confidence: 98%

“…Part of the northern Monoceros region has also been studied in polarization at radio frequencies by Xiao & Zhu (2012). These authors focused on the supernova remnant (SNR) Monoceros Loop, G205.7+0.1, north-west of the Rosette Nebula.…”

Section: The Rosette Nebula and The Mon Ob2 Molecular Cloudmentioning

confidence: 99%

Planckintermediate results

Aghanim

Alves

Arnaud

et al. 2016

A&A

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Planck has mapped the polarized dust emission over the whole sky, making it possible to trace the Galactic magnetic field structure that pervades the interstellar medium (ISM). We combine polarization data from Planck with rotation measure (RM) observations towards a massive starforming region, the Rosette Nebula in the Monoceros molecular cloud, to study its magnetic field structure and the impact of an expanding H ii region on the morphology of the field. We derive an analytical solution for the magnetic field, assumed to evolve from an initially uniform configuration following the expansion of ionized gas and the formation of a shell of swept-up ISM. From the RM data we estimate a mean value of the line-of-sight component of the magnetic field of about 3 μG (towards the observer) in the Rosette Nebula, for a uniform electron density of about 12 cm −3 . The dust shell that surrounds the Rosette H ii region is clearly observed in the Planck intensity map at 353 GHz, with a polarization signal significantly different from that of the local background when considered as a whole. The Planck observations constrain the plane-of-the-sky orientation of the magnetic field in the Rosette's parent molecular cloud to be mostly aligned with the large-scale field along the Galactic plane. The Planck data are compared with the analytical model, which predicts the mean polarization properties of a spherical and uniform dust shell for a given orientation of the field. This comparison leads to an upper limit of about 45• on the angle between the line of sight and the magnetic field in the Rosette complex, for an assumed intrinsic dust polarization fraction of 4%. This field direction can reproduce the RM values detected in the ionized region if the magnetic field strength in the Monoceros molecular cloud is in the range 6.5-9 μG. The present analytical model is able to reproduce the RM distribution across the ionized nebula, as well as the mean dust polarization properties of the swept-up shell, and can be directly applied to other similar objects.

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Binary companions of nearby supernova remnants found withGaia

Boubert

Fraser

Evans

et al. 2017

A&A

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Aims. We search for runaway former companions of the progenitors of nearby Galactic core-collapse supernova remnants (SNRs) in the Tycho-Gaia astrometric solution (TGAS). Methods. We look for candidates among a sample of ten SNRs with distances 2 kpc, taking astrometry and G magnitude from TGAS and B, V magnitudes from the AAVSO Photometric All-Sky Survey (APASS). A simple method of tracking back stars and finding the closest point to the SNR centre is shown to have several failings when ranking candidates. In particular, it neglects our expectation that massive stars preferentially have massive companions. We evolve a grid of binary stars to exploit these covariances in the distribution of runaway star properties in colour -magnitude -ejection velocity space. We construct an analytic model which predicts the properties of a runaway star, in which the model parameters are the location in the grid of progenitor binaries and the properties of the SNR. Using nested sampling we calculate the Bayesian evidence for each candidate to be the runaway and simultaneously constrain the properties of that runaway and of the SNR itself. Results. We identify four likely runaway companions of the Cygnus Loop (G074.0−08.5), HB 21 (G089.0+04.7), S147 (G180.0+01.7) and the Monoceros Loop (G205.5+00.5). HD 37424 has previously been suggested as the companion of S147, however the other three stars are new candidates. The favoured companion of HB 21 is the Be star BD+50 3188 whose emission-line features could be explained by pre-supernova mass transfer from the primary. There is a small probability that the 2 M candidate runaway TYC 2688-1556-1 associated with the Cygnus Loop is a hypervelocity star. If the Monoceros Loop is related to the on-going star formation in the Mon OB2 association, the progenitor of the Monoceros Loop is required to be more massive than 40 M which is in tension with the posterior for our candidate runaway star HD 261393.

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Radio perspectives on the Monoceros SNR G205.5+0.5

Cited by 19 publications

References 39 publications

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Molecular Environments of Three Large Supernova Remnants in the Third Galactic Quadrant: G205.5+0.5, G206.9+2.3, and G213.0–0.6

Planckintermediate results

Binary companions of nearby supernova remnants found withGaia

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