The Galactic Plane region near $\mathsf{\ell = 93\degr}$

Foster, Tyler; Routledge, D.; Kothes, R.

doi:10.1051/0004-6361:20034253

Cited by 16 publications

(19 citation statements)

References 29 publications

(33 reference statements)

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“…channels, line emission towards G152.4−2.1 shows no obvious cavity nor shell of neutral or molecular gas surrounding it (as an SNR evolving in a stellar wind bubble might; e.g. 3C 434.1, Foster et al 2004). Rather, the continuum boundary is sharply delimited by a wall of bright CO that systematically wraps the eastern boundary of the SNR from the south to the north.…”

Section: Hi and Co Velocities And Distancesmentioning

confidence: 99%

Two radio supernova remnants discovered in the outer Galaxy

Foster

Cooper

Reich

et al. 2013

A&A

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Context. New and existing large-scale radio surveys of the Milky Way at centimetre wavelengths can play an important role in uncovering the hundreds of expected but missing supernova remnants in the Galaxy's interstellar medium. We report on the discovery of two supernova remnants (SNRs) designated G152.4−2.1 and G190.9−2.2, using Canadian Galactic Plane Survey data. Aims. The aims of this paper are, first, to present evidence that favours the classification of both sources as SNRs, and, second, to describe basic parameters (integrated flux density, spectrum, and polarization) as well as properties (morphology, line-of-sight velocity, distance and physical size) to facilitate and motivate future observations. Methods. Spectral and polarization parameters are derived from multiwavelength data from existing radio surveys carried out at wavelengths between 6 and 92 cm. In particular for the source G152.4−2.1 we also use new observations at 11 cm done with the Effelsberg 100 m telescope. The interstellar medium around the discovered sources is analyzed using 1-arcmin line data from neutral hydrogen (H i) and 45-arcsec 12 CO(J = 1 → 0).Results. G152.4−2.1 is a barrel shaped SNR with two opposed radio-bright polarized flanks on the north and south. The remnant, which is elongated along the Galactic plane is evolving in a more-or-less uniform medium. G190.9−2.2 is also a shell-type remnant with east and west halves elongated perpendicular to the plane, and is evolving within a low-density region bounded by dense neutral hydrogen in the north and south, and molecular ( 12 CO) clouds in the east and west. The integrated radio continuum spectral indices are −0.65 ± 0.05 and −0.66 ± 0.05 for G152.4−2.1 and G190.9−2.2 respectively. Both SNRs are approximately 1 kpc distant, with G152.4−2.1 being larger (32 × 30 pc in diameter) than G190.9−2.2 (18 × 16 pc). These two remnants are the lowest surface brightness SNRs yet catalogued at Σ 1 GHz < ∼ 5 × 10 −23 W m −2 Hz −1 sr −1 .

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Section: Hi and Co Velocities And Distancesmentioning

confidence: 99%

Two radio supernova remnants discovered in the outer Galaxy

Foster

Cooper

Reich

et al. 2013

A&A

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“…• presented in Paper I (Foster & Routledge 2001) and Paper II (Foster Routledge & Kothes 2004) with a multi-wavelength study of the emission from SNR 3C 434.1 ( = 94…”

Section: Introductionmentioning

confidence: 99%

The Galactic plane region near $\ell$ = 93°

Foster

2005

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New Canadian Galactic Plane Survey radio continuum, ROSAT X-ray, and optical line observations of supernova remnant (SNR) 3C 434.1 (G94.0+1.0) are presented. A radio spectrum of index α = 0.4 (where S ∝ ν −α ) confirms this SNR's emission signature as predominantly synchrotron, and suggests the SNR is in the Sedov expansion phase. The morphology of the remnant is compared in X-ray, optical, and radio continuum, and the brightest emission in all three wavelength regimes is from the eastern hemisphere of 3C 434.1, which marks where the SNR shock is interacting with the inside wall of its stellar wind bubble (SWB) home. The system is determined to be 4.5 kpc distant, residing in the Perseus Arm Spiral shock. From a deep Hα mosaic of the region, λ656 nm Hα line emission is observed that correlates well with radio synchrotron emission and anticorrelates with X-ray emission from the SNR. The origin of this optical emission is likely dense (n e = 40 cm −3 ) cooling H  from the wall of the SWB, where the SNR shock has penetrated and become radiative (v s ∼ 100 km s −1 ). The X-ray spectrum of this SNR between 0.5 and 2.4 keV is well modelled by a single-temperature thermal plasma (T e = 4.5 × 10 6 K, n e = 0.2 cm −3 ). The magnetic field of the bright radio synchrotron emission region is found (under the assumption of near equipartition) to be B ∼ 15 µG, a factor of 3 compression of the ambient ISM field (5 µG). The westward extension of 3C 434.1 is the result of ongoing free expansion of the shock into the lower density interior of the SWB. I use multiwavelength observations to arrive at a unique solution for an interaction model of 3C 434.1 with the SWB, from which the age (t = 25 000 yr) and mass ejected in the explosion (M ej = 15.5 M ) are determined. I also find an initial blast-wave velocity of 1350 km s −1 , typical of type 1b SNe.

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“…A spiral shock in the Perseus arm is "pushing" objects, including H ii regions, SNRs, and PWNe, towards the Galactic centre, giving them -from our point of view -a higher negative radial velocity, which makes them appear to be farther away than they actually are (Roberts 1972). Examples of this effect on distance estimates of SNRs and PWNe can be found for instance in Kothes et al ( , 2003 and Foster et al (2004) and most recently in Kothes & Foster (2012). SNRs and PWNe in particular rely heavily on kinematic With permission of Crown Copyright 2013 NRC Canada.…”

Section: Introductionmentioning

confidence: 80%

“…A18, page 4 of 10 around the SNR 3C434.1, where the receding cap is seen absorbing warm background H i emission (Foster et al 2004). …”

Section: H I Emission Around 3c 58mentioning

confidence: 99%

Distance and age of the pulsar wind nebula 3C 58

Kothes¹

2013

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Context. A growing number of researchers present evidence that the pulsar wind nebula 3C 58 is much older than predicted by its proposed connection to the historical supernova of A.D. 1181. There is also a great diversity of arguments. The strongest of these arguments rely heavily on the assumed distance of 3.2 kpc determined with H i absorption measurements.Aims. This publication aims at determining a more accurate distance for 3C 58 and at re-evaluating the arguments for an older age.Methods. I have re-visited the distance determination of 3C 58 based on new H i data from the Canadian Galactic Plane Survey and our recent improvements in the knowledge of the rotation curve of the outer Milky Way Galaxy. I also used newly determined distances to objects in the neighbourhood, which are based on direct measurements by trigonometric parallax. Results. I have derived a new more reliable distance estimate of 2 kpc for 3C 58. This makes the connection between the pulsar wind nebula and the historical event from A.D. 1181 once again much more viable.

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The Galactic Plane region near $\mathsf{\ell = 93\degr}$

Cited by 16 publications

References 29 publications

Two radio supernova remnants discovered in the outer Galaxy

Two radio supernova remnants discovered in the outer Galaxy

The Galactic plane region near $\ell$ = 93°

Distance and age of the pulsar wind nebula 3C 58

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