Astrophys Space Sci

1978

DOI: 10.1007/bf00644521

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Radio emission of the NGC 1499 nebula at decametric wavelengths

V. V. Krymkin¹

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Emissivity Calculations1

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Cited by 4 publications

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“…Similar to a single dish telescope (Kassim 1987), we observe Fig. 3 to show an example absorption feature.…”

Section: Emissivity Calculationsmentioning

confidence: 58%

Galactic synchrotron emissivity measurements between 250° <l< 355° from the GLEAM survey with the MWA

¹

,

Hurley‐Walker

²

,

³

et al. 2016

Mon. Not. R. Astron. Soc.

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Synchrotron emission pervades the Galactic plane at low radio frequencies, originating from cosmic ray electrons interacting with the Galactic magnetic field. Using a low-frequency radio telescope, the Murchison Widefield Array (MWA), we measure the free-free absorption of this Galactic synchrotron emission by intervening H regions along the line of sight. These absorption measurements allow us to calculate the Galactic cosmic-ray electron emissivity behind and in front of 47 detected H regions in the region 250 • < l < 355 • , |b| < 2 • . We find that all average emissivities between the H regions and the Galactic edge along the line of sight (ǫ b ) are in the range of 0.24 ∼ 0.70 K pc −1 with a mean of 0.40 K pc −1 and a variance of 0.10 K pc −1 at 88 MHz. Our best model, the Two-circle model, divides the Galactic disk into three regions using two circles centring on the Galactic centre. It shows a high emissivity region near the Galactic centre, a low emissivity region near the Galactic edge, and a medium emissivity region between these two regions, contrary to the trend found by previous studies.

“…Similar to a single dish telescope (Kassim 1987), we observe Fig. 3 to show an example absorption feature.…”

Section: Emissivity Calculationsmentioning

confidence: 58%

Galactic synchrotron emissivity measurements between 250° <l< 355° from the GLEAM survey with the MWA

¹

,

Hurley‐Walker

²

,

³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

Synchrotron emission pervades the Galactic plane at low radio frequencies, originating from cosmic ray electrons interacting with the Galactic magnetic field. Using a low-frequency radio telescope, the Murchison Widefield Array (MWA), we measure the free-free absorption of this Galactic synchrotron emission by intervening H regions along the line of sight. These absorption measurements allow us to calculate the Galactic cosmic-ray electron emissivity behind and in front of 47 detected H regions in the region 250 • < l < 355 • , |b| < 2 • . We find that all average emissivities between the H regions and the Galactic edge along the line of sight (ǫ b ) are in the range of 0.24 ∼ 0.70 K pc −1 with a mean of 0.40 K pc −1 and a variance of 0.10 K pc −1 at 88 MHz. Our best model, the Two-circle model, divides the Galactic disk into three regions using two circles centring on the Galactic centre. It shows a high emissivity region near the Galactic centre, a low emissivity region near the Galactic edge, and a medium emissivity region between these two regions, contrary to the trend found by previous studies.

Parameters of the magnetic field in the Local Galactic ARM Derived from low Frequency Absorption Measurements in the Ionized Gas

1990

Galactic and Intergalactic Magnetic Fields

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No abstract

Observations of the gaseous nebulae W80 and Sh119 at four decameter frequencies

1992

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No abstract

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