A Low Latitude Survey from lII = 27° to 38° at 1410 and 2650 MHz

Beard, M.; Kerr, F. J.

doi:10.1071/ph690121

Cited by 23 publications

(13 citation statements)

References 3 publications

(3 reference statements)

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“…In particular, measurements at 1.4 GHz by Giacani et al (1997) (S1.4GHz = 210 ± 20 Jy) and Castelletti et al (2007) (S1.4GHz = 300 ± 7 Jy) are inconsistent. Our result at 1.55 GHz (S1.55GHz = 214.4 ± 6.4 Jy) is comparable within 1σ with the former and most other Lband flux measurements obtained in the '60s (Beard & Kerr 1969;Pauliny-Toth et al 1966;Scheuer 1963;Leslie 1960). Our measure-ment at 7.0 GHz (S7GHz = 93.7 ± 4.0 Jy) is in agreement with Hollinger & Hobbs (1966): S8.3GHz = 95 ± 23 Jy.…”

Section: Based On the Values Insupporting

confidence: 92%

Imaging of SNR IC443 and W44 with the Sardinia Radio Telescope at 1.5 and 7 GHz

Egron

Iacolina

Loru

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Observations of supernova remnants (SNRs) are a powerful tool for investigating the later stages of stellar evolution, the properties of the ambient interstellar medium, and the physics of particle acceleration and shocks. For a fraction of SNRs, multi-wavelength coverage from radio to ultrahigh-energies has been provided, constraining their contributions to the production of Galactic cosmic rays. Although radio emission is the most common identifier of SNRs and a prime probe for refining models, high-resolution images at frequencies above 5 GHz are surprisingly lacking, even for bright and well-known SNRs such as IC443 and W44. In the frameworks of the Astronomical Validation and Early Science Program with the 64-m single-dish Sardinia Radio Telescope, we provided, for the first time, single-dish deep imaging at 7 GHz of the IC443 and W44 complexes coupled with spatially-resolved spectra in the 1.5 − 7 GHz frequency range. Our images were obtained through on-the-fly mapping techniques, providing antenna beam oversampling and resulting in accurate continuum flux density measurements. The integrated flux densities associated with IC443 are S 1.5GHz = 134 ± 4 Jy and S 7GHz = 67 ± 3 Jy. For W44, we measured total flux densities of S 1.5GHz = 214 ± 6 Jy and S 7GHz = 94 ± 4 Jy. Spectral index maps provide evidence of a wide physical parameter scatter among different SNR regions: a flat spectrum is observed from the brightest SNR regions at the shock, while steeper spectral indices (up to ∼ 0.7) are observed in fainter cooling regions, disentangling in this way different populations and spectra of radio/gamma-ray-emitting electrons in these SNRs.

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Section: Based On the Values Insupporting

confidence: 92%

Imaging of SNR IC443 and W44 with the Sardinia Radio Telescope at 1.5 and 7 GHz

Egron

Iacolina

Loru

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…In Fig. 7, the measurement at 2.7 GHz (Beard et al 1969) is likely to be an overestimate, for the authors quote this source as extended, while it is a point-like source at all other frequencies. Excluding this flux density as well as those measurements at 300 GHz, a weighted least square fit to the flux density measurements betweeen 1.6 and 85 GHz gives a spectral index of α = −0.14 ± 0.03 (S ν ∝ ν α ).…”

Section: Radio Continuummentioning

confidence: 99%

“…Radio continuum observations of RCW 121 were carried out at 2.7 (Beard et al 1969) and 4.85 GHz (Wright et al 1994).…”

Section: Introductionmentioning

confidence: 99%

Molecular gas associated with RCW 121 and RCW 122

Arnal

Duronea

Testori

2008

A&A

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Aims. We analyse the distribution of the molecular gas towards the region containing the open cluster Havlen-Moffat 1 (HM 1) the Wolf-Rayet stars WR 87, WR 89, and WR 91, and the star forming regions RCW 121 and RCW 122, with the aim of looking for a possible physical relationship among these objects. Methods. We used the carbon monoxide observations carried out at λ ∼ 2.6 mm with the 4 m NANTEN radiotelescope; new flux density determinations derived from already existing radio continuum surveys at 2. 417, 5, 8.35, and 14.35 GHz; continuum flux density determinations available in the literature; and the Midcourse Space Experiment (MSX) and the Improved Reprocessing of the IRAS Survey (IRIS) databases. Results. Adopting a distance of 5 kpc for RCW 121 and RCW 122, we found a giant molecular cloud (GMC) with a linear extent of ∼100 × 20 pc to be associated with galactic star-forming regions. The total mass of this GMC is of the order of 1.2 × 10 6 solar masses and its mean radial velocity is about -15 km s −1 . Within the GMC there are individual molecular gas concentrations, having total molecular masses in the range from 4.6 × 10 4 M (RCW 122 C) to 2.2 × 10 5 M (RCW 122). The CO profiles observed toward the peak of the molecular concentrations are broad, with typical full-width half-maximum around 6 to 7 km s −1 , and show line asymmetries and/or double-peaked shape that change with the observed position within a given CO concentration. An analysis of the MSX and IRAS databases show that each CO concentration has a strong IR counterpart. The dust temperature of these concentrations range from 46 K (RCW 121) to 76 K (RCW 122 C). Their infrared luminosity are a few times 10 5 L . The new radio continuum flux density determinations are in good agreement with previous determinations at other frequencies, and confirm the thermal nature of RCW 121 and RCW 122. Based on the newly-determined 5 GHz flux density, we found that to power these Hii regions, each of them must harbour a sizable number of O type stars. Under the assumption that all the ionizing stars have a O7 V spectral type, at least ∼8 and ∼4 of these stars would be needed to ionize RCW 122 and RCW 121, respectively.

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“…G35.6−0.4 is Galactic radio source detected in several early radio surveys (Beard & Kerr 1969; Altenhoff et al 1970), and listed as a SNR in several early catalogues (Milne 1970; Downes 1971; Ilovaisky & Lequeux 1972; Milne 1979). 1 The extent of the source was given as ∼10 arcmin, although this was not well defined by the available observations, as they had resolutions of only about 7 arcmin at best.…”

Section: Introductionmentioning

confidence: 99%

Re-identification of G35.6−0.4 as a supernova remnant

Green¹

2009

Monthly Notices of the Royal Astronomical Society

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G35.6−0.4 is an extended radio source in the Galactic plane which has previously been identified as either a supernova remnant or an H ii region. Observations from the Very Large Array Galactic Plane Survey at 1.4 GHz with a resolution of 1 arcmin allow the extent of G35.6−0.4 to be defined for the first time. Comparison with other radio survey observations show that this source has a non‐thermal spectral index, with S∝ν−0.47±0.07. G35.6−0.4 does not have obvious associated infrared emission, so it is identified as a Galactic supernova remnant, not an H ii region. It is ≈15 × 11 arcmin2 in extent, showing partial limb brightening.

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A Low Latitude Survey from lII = 27° to 38° at 1410 and 2650 MHz

Abstract: SummaryThis paper presents contour maps of a region of the Milky Way at 1410 and 2650 MHz. A list of sources with values of flux densities and peak temperatures is given.

Cited by 23 publications

References 3 publications

Imaging of SNR IC443 and W44 with the Sardinia Radio Telescope at 1.5 and 7 GHz

Imaging of SNR IC443 and W44 with the Sardinia Radio Telescope at 1.5 and 7 GHz

Molecular gas associated with RCW 121 and RCW 122

Re-identification of G35.6−0.4 as a supernova remnant

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