Low-frequency Carbon Recombination Lines towards HI self-absorption features in the Galactic Plane
A survey of radio recombination lines (RLs) in the Galactic plane ($l = $ 332\deg $\to$ 89\deg) near 327 MHz made using the Ooty Radio Telescope (ORT) has detected carbon RLs from all the positions in the longitude range 0\deg $< l < $ 20\deg and from a few positions at other longitudes. The c...
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04.10.2001
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Abstract | A survey of radio recombination lines (RLs) in the Galactic plane ($l = $
332\deg $\to$ 89\deg) near 327 MHz made using the Ooty Radio Telescope (ORT)
has detected carbon RLs from all the positions in the longitude range 0\deg $<
l < $ 20\deg and from a few positions at other longitudes. The carbon RLs
detected in this survey originate from ``diffuse'' \CII regions. Comparison of
the \lv diagram and the radial distribution of carbon line emission with those
obtained from hydrogen RLs near 3 cm from \HII regions and ``intense'' \CO
emission indicates that the distribution of the diffuse \CII regions in the
inner Galaxy is similar to that of spiral arm components. Towards several
observed positions, the central velocities of the carbon RLs coincide with \HI
self-absorption features suggesting an association of diffuse \CII regions with
cool \HI. The observed widths of the lines from the two species are, however,
different. We discuss possible reasons for the difference in the line widths. |
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AbstractList | A survey of radio recombination lines (RLs) in the Galactic plane ($l = $
332\deg $\to$ 89\deg) near 327 MHz made using the Ooty Radio Telescope (ORT)
has detected carbon RLs from all the positions in the longitude range 0\deg $<
l < $ 20\deg and from a few positions at other longitudes. The carbon RLs
detected in this survey originate from ``diffuse'' \CII regions. Comparison of
the \lv diagram and the radial distribution of carbon line emission with those
obtained from hydrogen RLs near 3 cm from \HII regions and ``intense'' \CO
emission indicates that the distribution of the diffuse \CII regions in the
inner Galaxy is similar to that of spiral arm components. Towards several
observed positions, the central velocities of the carbon RLs coincide with \HI
self-absorption features suggesting an association of diffuse \CII regions with
cool \HI. The observed widths of the lines from the two species are, however,
different. We discuss possible reasons for the difference in the line widths. |
Author | Kantharia, Nimisha G Anantharamaiah, K. R Roshi, D. Anish |
Author_xml | – sequence: 1 givenname: D. Anish surname: Roshi fullname: Roshi, D. Anish organization: National Centre for Radio Astrophysics, TIFR, Pune, India – sequence: 2 givenname: Nimisha G surname: Kantharia fullname: Kantharia, Nimisha G organization: National Centre for Radio Astrophysics, TIFR, Pune, India – sequence: 3 givenname: K. R surname: Anantharamaiah fullname: Anantharamaiah, K. R organization: Raman Research Institute, Bangalore, India |
BackLink | https://doi.org/10.48550/arXiv.astro-ph/0110121$$DView paper in arXiv |
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Snippet | A survey of radio recombination lines (RLs) in the Galactic plane ($l = $
332\deg $\to$ 89\deg) near 327 MHz made using the Ooty Radio Telescope (ORT)
has... |
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SubjectTerms | Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics Physics - Earth and Planetary Astrophysics Physics - High Energy Astrophysical Phenomena Physics - Instrumentation and Methods for Astrophysics Physics - Solar and Stellar Astrophysics |
Title | Low-frequency Carbon Recombination Lines towards HI self-absorption features in the Galactic Plane |
URI | https://arxiv.org/abs/astro-ph/0110121 |
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