Hostname: page-component-586b7cd67f-tf8b9 Total loading time: 0 Render date: 2024-11-26T20:38:14.908Z Has data issue: false hasContentIssue false
  • English
  • Français

Galactic Carbon Recombination Lines near 327 MHz

Published online by Cambridge University Press:  26 May 2016

D. Anish Roshi ,
N.G. Kantharia  and
K. R. Anantharamaiah
D. Anish Roshi
Affiliation:
National Centre for Radio Astrophysics, TIFR, Pune, India
N.G. Kantharia
Affiliation:
National Centre for Radio Astrophysics, TIFR, Pune, India
K. R. Anantharamaiah
Affiliation:
Raman Research Institute, Bangalore, India

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

A survey of radio recombination lines (RRLs) in the Galactic plane (l = 332° − 0° − 89°) near 327 MHz made using the Ooty Radio Telescope (ORT) has detected carbon RRLs from all the positions in the longitude range 0° < l < 20° and from a few positions at other longitudes. The carbon lines detected in the survey are, most likely, emission counterparts of the absorption lines observed at frequencies below 150 MHz. Observations towards l = 13°.9, b = 0°.0 indicate that the broader (∼ 38 km s−1) carbon line detected in the lower resolution observation consists of multiple narrow components (∼ 10 km s−1) with different central velocities. The implications of the presence of such narrow components for the modeling of line emission is discussed.

Type
Part 6: Spectral Studies of our Galaxy
Information
Symposium - International Astronomical Union , Volume 199: The Universe at Low Radio Frequencies , 2002 , pp. 345 - 346
Copyright
Copyright © Astronomical Society of the Pacific 2002 

References

Erickson, W. C., McConnell, D., Anantharamaiah, K. R., 1995, ApJ, 454, 125 CrossRefGoogle Scholar
Kantharia, N.G. 1998, , .Google Scholar
Payne, H. E., Anantharamaiah, K. R., Erickson, W. C., 1989, ApJ, 341, 890 CrossRefGoogle Scholar