A Catalogue of Galactic Radio Sources

Kesteven, M. J.

doi:10.1071/ph680369

Cited by 43 publications

(27 citation statements)

References 2 publications

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“…Below 11 GHz, the spectral index obtained by Morsi & Reich (1987a) is α = −0.26, which is consistent with our result. Adding new flux densities at 28, 40, 42, 44, 49, 61, 62, 64, 78, 95, 103, 105, 108, 111, 137, 139- Becker & Kundu (1975), (7) Dulk & Slee (1975), (8) Green (1974), (9) , (10) Kassim (1992), (11) Kothes & Reich (2001), (12) Morsi & Reich (1987b), (13) Milne et al (1969), (14) Reich et al (1984a), (15) Reifenstein et al (1970), (16) Slee (1977), (17) , (18) Shaver & Weiler (1976), (19) Tam et al (2002), (20) Angerhofer et al (1977), (21) Clark et al (1975a), (22) Dubner et al (1996), (23) Trushkin (1999), (24) Helfand et al (1989), (25) Reich et al (1986), (26) Clark et al (1975b), (27) Kesteven (1968), (28) Langston et al (2000), (29) Milne et al (1989), (30) Milne & Dickel (1975), …”

Section: Snr Spectramentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Sun

Reich

et al. 2011

A&A

119

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Aims. We study the spectral and polarization properties of supernova remnants (SNRs) using our λ6 cm survey data. Methods. We analyse data from observations taken as part of the Sino-German λ6 cm polarization survey of the Galactic plane. By using the integrated flux densities at λ6 cm together with measurements at other wavelengths from the literature, we derive the global spectra of 50 SNRs. In addition, from the observations at λ6 cm we obtain the polarization images of 24 SNRs. Results. We derive integrated flux densities at λ6 cm for 51 small SNRs with angular sizes smaller than 1 • . We are able to derive global radio spectral indices in all the cases except for Cas A. For the SNRs G15.1−1.6, G16.2−2.7, G16.4−0.5, G17.4−2.3, G17.8−2.6, G20.4+0.1, G36.6+2.6, G43.9+1.6, G53.6−2.2, G55.7+3.4, G59.8+1.2, G68.6−1.2, and G113.0+0.2, the spectra have been significantly improved. From our analysis, we argue that the object G16.8−1.1 is probably an H ii region instead of a SNR. Cas A shows a secular decrease in total intensity, and we measure a flux density of 688 ± 35 Jy at λ6 cm between 2004 and 2008. We detect polarized emission from 25 SNRs. For G16.2−2.7, G69.7+1.0, G84.2−0.8, and G85.9−0.6, the polarized emission is detected for the first time confirming that they are SNRs. Conclusions. High-frequency observations of SNRs are difficult but essential to determine their spectra and measure their polarization in particular towards the inner Galaxy, where Faraday effects are important.

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Section: Snr Spectramentioning

confidence: 99%

A Sino-Germanλ6 cm polarization survey of the Galactic plane

Sun

Reich

et al. 2011

A&A

119

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“…RCW 49 AND WESTERLUND 2 RCW 49 was identified as an optically visible H ii region by Rodgers et al (1960). It is also known as Kes 10 ( Kesteven 1968), G284.3À00.3, and Gum 29 (Gum 1955). The visual extinction toward the region is A V ¼ 5 6 mag (Carraro & Munari 2004;Rauw et al 2007;Ascenso et al 2007).…”

Section: Introductionmentioning

confidence: 99%

An X‐Ray Imaging Study of the Stellar Population in RCW 49

Tsujimoto

Feigelson

Townsley

et al. 2007

ApJ

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We present the results of a high-resolution X-ray imaging study of the stellar population in the Galactic massive star-forming region RCW 49 and its central OB association Westerlund 2. We obtained a $40 ks X-ray image of a $17 0 ; 17 0 field using the Chandra X-Ray Observatory and deep NIR images using the Infrared Survey Facility in a concentric $8:3 0 ; 8:3 0 region. We detected 468 X-ray sources and identified optical, NIR, and Spitzer MIR counterparts for 379 of them. The unprecedented spatial resolution and sensitivity of the X-ray image, enhanced by optical and infrared imaging data, yielded the following results: (1) The central OB association Westerlund 2 is resolved for the first time in the X-ray band. X-ray emission is detected from all spectroscopically identified early-type stars in this region.(2) Most ($86%) X-ray sources with optical or infrared identifications are cluster members in comparison with a control field in the Galactic plane. (3) A loose constraint (2-5 kpc) for the distance to RCW 49 is derived from the mean X-ray luminosity of T Tauri stars. (4) The cluster X-ray population consists of low-mass pre-main-sequence and earlytype stars as obtained from X-ray and NIR photometry. About 30 new OB star candidates are identified. (5) We estimate a cluster radius of 6 0 -7 0 based on the X-ray surface number density profiles. (6) A large fraction ($90%) of cluster members are identified individually using complimentary X-ray and MIR excess emission. (7) The brightest five X-ray sources, two Wolf-Rayet stars and three O stars, have hard thermal spectra.

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“…It remains undetected at radio frequencies (Archibald et al 2008). PSR J1846−0258 is located at the centre of supernova remnant (SNR) Kes 75 (G29.7-0.3, Kesteven 1968) and was resolved in a Chandra observation as a bright X-ray source surrounded by a diffuse pulsar wind nebula (PWN, Helfand et al 2003). The distance of SNR Kes 75 and PSR J1846−0258 has been under discussion for a long time.…”

Section: Introductionmentioning

confidence: 99%

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

Kuiper

Hermsen

2009

A&A

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Aims. PSR J1846−0258 is a young rotation-powered pulsar with one of the highest surface magnetic field strengths, located in the centre of SN-remnant Kes-75. In June 2006 a magnetar-like outburst took place. Using multi-year RXTE and INTEGRAL observations covering the epoch of the outburst, we aim to study the temporal and spectral characteristics of PSR J1846−0258 over a broad ∼3-300 keV energy range to derive constraints on theoretical scenarios aiming to explain this schizophrenic behaviour. Methods. We explored all publically available RXTE observations of PSR J1846−0258 to generate accurate ephemerides over the period January 30, 2000-November 7, 2007. Phase-folding procedures yielded pulse profiles for RXTE PCA (∼3-30 keV), RXTE HEXTE (∼15-250 keV) and INTEGRAL ISGRI (∼20-300 keV). The pulsed spectrum over the full ∼3-300 keV energy range was derived, as well as the total spectrum (including the pulsar wind nebula) over the 20-300 keV band with the ISGRI. The timing, spatial, and spectral analyses were applied for epochs before, during, and after the magnetar-like outburst to study the evolution of the high-energy characteristics. Results. ISGRI detected PSR J1846−0258/Kes-75 before outburst during 2003-2006 with a power-law-shape spectrum over the 20-300 keV energy range with photon index Γ = 1.80 ± 0.06 and energy flux (20-300 keV) of (6.62 ± 0.35) × 10 −11 erg/cm 2 s. More than 90 days after the onset of the outburst, still during the decay phase, the same spectral shape was measured (Γ = 1.75 +0.27 −0.31 ) with an indication for a 52% (2.3σ) enhanced total emission, while one year after the outburst the hard X-ray non-thermal emission of PSR J1846−0258/Kes-75 was found to be back to its pre-outburst values. PCA monitoring of PSR J1846−0258 before the outburst yielded phase-coherent ephemerides confirming the earlier derived breaking index of the spindown. During the outburst, incoherent solutions have been derived. We show that the radiative outburst was triggered by a major spin-up glitch near MJD 53 883 ± 3 with a glitch size Δν/ν in the range (2.0−4.4) × 10 −6 . Using all pre-outburst observations of ISGRI and HEXTE for the first time pulse profiles have been obtained up to 150 keV with a broad single asymmetric pulse. The pulse shape did not vary with energy over the 2.9-150 keV energy range, nor did it change during the magnetar-like outburst. The time-averaged pre-outburst ∼3-300 keV pulsed spectrum measured with the PCA, HEXTE, and ISGRI was fitted with a power-law model with Γ = 1.20 ± 0.01. A fit with a curved power-law model gives an improved fit. Around 150 keV the pulsed fraction approaches 100%. For the first 32 days of the magnetarlike outburst, the 3-30 keV pulsed spectrum can be represented with two power laws, a soft component with index Γ s = 2.96 ± 0.06 and a hard component with the pre-outburst value Γ h ∼ 1.2. Above ∼9 keV, all spectra during outburst are consistent with the latter single power-law shape with index ∼1.2. The 2-10 keV flux increased by a factor ∼5 and the 10...

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A Catalogue of Galactic Radio Sources

Cited by 43 publications

References 2 publications

A Sino-Germanλ6 cm polarization survey of the Galactic plane

A Sino-Germanλ6 cm polarization survey of the Galactic plane

An X‐Ray Imaging Study of the Stellar Population in RCW 49

High-energy characteristics of the schizophrenic pulsar PSR J1846-0258 in Kes 75

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