Radio Recombination Lines (RRLs) are spectral lines emitted during recombination ( Plasma recombination?). They are observed at radio frequencies.
Lines
- Due to the formation of atoms through the recombination of electrons and ions [1]
- Lines come from transitions between highly excited atomic levels. [1]
- At radio frequencies, referred to as 'Radio Recombination Lines'. [1]
- Emitted by hydrogen atoms [2]
- In the interstellar medium, can have quantum levels up to n=1000, and with radiuses of the order of a tenth of a millimetre. [1]
- Maser effects [2]
- Low frequencies contaminated by synchrotron emission. [2]
Implications
- Probe of the gas in star-forming regions. [1]
- Depends on gas densities and temperatures. [1]
- Can estimate electron temperatures. [3] [2]
- Can estimate star formation rates. [2]
- Dust attenuation [2]
Observations
Solar system
- Detected in the Sun. [1]
Galactic regions
Nearby galaxies
The first extragalactic detection of RRLs beyond the Magellanic clouds was the H166α line in Messier 82 in 1977. [5]
| Galaxy | First detection | Lines observed | Telescopes |
|---|---|---|---|
| Circinus Galaxy | 2008 [6] | H92α [6] | |
| Messier 33 | 2004 [7] | H110α [7] | |
| Messier 82 | 1977 [5] |
H26α, [8] H27α, [8] H29α, [8] H30α, [9] H41α, [8] H53α, [10] H85α, [11] H92α, [3] [10] H102α, [12] [11] H166α [5] |
36.6m telescope at Haystack Observatory, [3] Algonquin Radio Observatory [12], Westerbork Synthesis Radio Telescope [5] |
| NGC 253 | 1977 [13] | Algonquin Radio Observatory [12], ALMA [2] | |
| NGC 1808 | 2008 [6] | H92α [6] |
References
- ^ a b c d e f g Gordon, M. A.; Sorochenko, R.L. (2008). Radio recombination lines: their physics and astronomical applications. New York: Springer. ISBN 978-0-387-09604-9.
- ^
a
b
c
d
e
f
g
h Bendo, G. J.; Beswick, R. J.; D'Cruze, M. J.; Dickinson, C.; Fuller, G. A.; Muxlow, T. W. B. (1 May 2015). "ALMA observations of 99 GHz free-free and H40 line emission from star formation in the centre of NGC 253". Monthly Notices of the Royal Astronomical Society: Letters. 450 (1): L80–L84.
doi:
10.1093/mnrasl/slv053.
{{ cite journal}}: no-break space character in|title=at position 46 ( help) - ^ a b c d Chaisson, E. J.; Rodriguez, L. F. (June 1977). "Detection of extragalactic radio recombination line emission from M82". The Astrophysical Journal. 214: L111. doi: 10.1086/182453.
- ^ Alves, Marta I. R.; Davies, Rodney D.; Dickinson, Clive; Davis, Richard J.; Auld, Robbie R.; Calabretta, Mark; Staveley-Smith, Lister (April 2010). "Diffuse radio recombination line emission on the Galactic plane between l=36° and 44°". Monthly Notices of the Royal Astronomical Society. doi: 10.1111/j.1365-2966.2010.16595.x.
- ^ a b c d Shaver, P. A.; Churchwell, E.; Rots, A. H. (March 1977). "Stimulated Recombination Line Emission from M 82". The Astronomy & Astrophysics. 55: 435.
- ^
a
b
c
d Roy, A. L.; Goss, W. M.; Anantharamaiah, K. R. (May 2008). "Detection of the H92α recombination line from the starbursts in the Circinus galaxy and NGC 1808". Astronomy and Astrophysics. 483 (1): 79–88.
doi:
10.1051/0004-6361:20077405.
{{ cite journal}}: no-break space character in|title=at position 65 ( help) - ^ a b Araya, Esteban; Baan, Willem A.; Hofner, Peter (October 2004). "Studies of Extragalactic Formaldehyde and Radio Recombination Lines". The Astrophysical Journal Supplement Series. 154 (2): 541–552. doi: 10.1086/423246.
- ^ a b c d Seaquist, E. R.; Carlstrom, J. E.; Bryant, P. M.; Bell, M. B. (July 1996). "Millimeter Recombination Line Emission in the Starburst Galaxy M82". The Astrophysical Journal. 465: 691. doi: 10.1086/177454.
- ^ Seaquist, E. R.; Kerton, C. R.; Bell, M. B. (July 1994). "Millimeter recombination lines and the state of ionized gas in M82". The Astrophysical Journal. 429: 612. doi: 10.1086/174348.
- ^ a b Rodriguez‐Rico, C. A.; Viallefond, F.; Zhao, J.‐H.; Goss, W. M.; Anantharamaiah, K. R. (December 2004). "Very Large Array H92α and H53α Radio Recombination Line Observations of M82". The Astrophysical Journal. 616 (2): 783–803. doi: 10.1086/425109.
- ^ a b Bell, M. B.; Seaquist, E. R. (July 1978). "Radio Recombination Line Studies of M82 and Other Galaxies". The Astrophysical Journal. 223: 378. doi: 10.1086/156272.
- ^ a b c Bell, M. B.; Seaquist, E. R. (April 1977). "Detection of the H 102a Recombination Line in M 82". The Astronomy & Astrophysics. 56: 461.
- ^ a b Seaquist, E. R.; Bell, M. B. (1977). "Detection of the H102α Recombination Line in NGC253". The Astronomy & Astrophysics. 60: L1.
-
^ Mebold, U.; Shaver, P. A.; Bell, M. B.; Seaquist, E. R. (Feb 1980).
"Radio recombination lines from NGC 253". Astronomy & Astrophysics. 82: 272.
{{ cite journal}}: Cite has empty unknown parameter:|1=( help)
Further reading
- Gordon, M. A.; Sorochenko, R.L. (2008). Radio recombination lines: their physics and astronomical applications. New York: Springer. ISBN 978-0-387-09604-9.
Radio Recombination Lines (RRLs) are spectral lines emitted during recombination ( Plasma recombination?). They are observed at radio frequencies.
Lines
- Due to the formation of atoms through the recombination of electrons and ions [1]
- Lines come from transitions between highly excited atomic levels. [1]
- At radio frequencies, referred to as 'Radio Recombination Lines'. [1]
- Emitted by hydrogen atoms [2]
- In the interstellar medium, can have quantum levels up to n=1000, and with radiuses of the order of a tenth of a millimetre. [1]
- Maser effects [2]
- Low frequencies contaminated by synchrotron emission. [2]
Implications
- Probe of the gas in star-forming regions. [1]
- Depends on gas densities and temperatures. [1]
- Can estimate electron temperatures. [3] [2]
- Can estimate star formation rates. [2]
- Dust attenuation [2]
Observations
Solar system
- Detected in the Sun. [1]
Galactic regions
Nearby galaxies
The first extragalactic detection of RRLs beyond the Magellanic clouds was the H166α line in Messier 82 in 1977. [5]
| Galaxy | First detection | Lines observed | Telescopes |
|---|---|---|---|
| Circinus Galaxy | 2008 [6] | H92α [6] | |
| Messier 33 | 2004 [7] | H110α [7] | |
| Messier 82 | 1977 [5] |
H26α, [8] H27α, [8] H29α, [8] H30α, [9] H41α, [8] H53α, [10] H85α, [11] H92α, [3] [10] H102α, [12] [11] H166α [5] |
36.6m telescope at Haystack Observatory, [3] Algonquin Radio Observatory [12], Westerbork Synthesis Radio Telescope [5] |
| NGC 253 | 1977 [13] | Algonquin Radio Observatory [12], ALMA [2] | |
| NGC 1808 | 2008 [6] | H92α [6] |
References
- ^ a b c d e f g Gordon, M. A.; Sorochenko, R.L. (2008). Radio recombination lines: their physics and astronomical applications. New York: Springer. ISBN 978-0-387-09604-9.
- ^
a
b
c
d
e
f
g
h Bendo, G. J.; Beswick, R. J.; D'Cruze, M. J.; Dickinson, C.; Fuller, G. A.; Muxlow, T. W. B. (1 May 2015). "ALMA observations of 99 GHz free-free and H40 line emission from star formation in the centre of NGC 253". Monthly Notices of the Royal Astronomical Society: Letters. 450 (1): L80–L84.
doi:
10.1093/mnrasl/slv053.
{{ cite journal}}: no-break space character in|title=at position 46 ( help) - ^ a b c d Chaisson, E. J.; Rodriguez, L. F. (June 1977). "Detection of extragalactic radio recombination line emission from M82". The Astrophysical Journal. 214: L111. doi: 10.1086/182453.
- ^ Alves, Marta I. R.; Davies, Rodney D.; Dickinson, Clive; Davis, Richard J.; Auld, Robbie R.; Calabretta, Mark; Staveley-Smith, Lister (April 2010). "Diffuse radio recombination line emission on the Galactic plane between l=36° and 44°". Monthly Notices of the Royal Astronomical Society. doi: 10.1111/j.1365-2966.2010.16595.x.
- ^ a b c d Shaver, P. A.; Churchwell, E.; Rots, A. H. (March 1977). "Stimulated Recombination Line Emission from M 82". The Astronomy & Astrophysics. 55: 435.
- ^
a
b
c
d Roy, A. L.; Goss, W. M.; Anantharamaiah, K. R. (May 2008). "Detection of the H92α recombination line from the starbursts in the Circinus galaxy and NGC 1808". Astronomy and Astrophysics. 483 (1): 79–88.
doi:
10.1051/0004-6361:20077405.
{{ cite journal}}: no-break space character in|title=at position 65 ( help) - ^ a b Araya, Esteban; Baan, Willem A.; Hofner, Peter (October 2004). "Studies of Extragalactic Formaldehyde and Radio Recombination Lines". The Astrophysical Journal Supplement Series. 154 (2): 541–552. doi: 10.1086/423246.
- ^ a b c d Seaquist, E. R.; Carlstrom, J. E.; Bryant, P. M.; Bell, M. B. (July 1996). "Millimeter Recombination Line Emission in the Starburst Galaxy M82". The Astrophysical Journal. 465: 691. doi: 10.1086/177454.
- ^ Seaquist, E. R.; Kerton, C. R.; Bell, M. B. (July 1994). "Millimeter recombination lines and the state of ionized gas in M82". The Astrophysical Journal. 429: 612. doi: 10.1086/174348.
- ^ a b Rodriguez‐Rico, C. A.; Viallefond, F.; Zhao, J.‐H.; Goss, W. M.; Anantharamaiah, K. R. (December 2004). "Very Large Array H92α and H53α Radio Recombination Line Observations of M82". The Astrophysical Journal. 616 (2): 783–803. doi: 10.1086/425109.
- ^ a b Bell, M. B.; Seaquist, E. R. (July 1978). "Radio Recombination Line Studies of M82 and Other Galaxies". The Astrophysical Journal. 223: 378. doi: 10.1086/156272.
- ^ a b c Bell, M. B.; Seaquist, E. R. (April 1977). "Detection of the H 102a Recombination Line in M 82". The Astronomy & Astrophysics. 56: 461.
- ^ a b Seaquist, E. R.; Bell, M. B. (1977). "Detection of the H102α Recombination Line in NGC253". The Astronomy & Astrophysics. 60: L1.
-
^ Mebold, U.; Shaver, P. A.; Bell, M. B.; Seaquist, E. R. (Feb 1980).
"Radio recombination lines from NGC 253". Astronomy & Astrophysics. 82: 272.
{{ cite journal}}: Cite has empty unknown parameter:|1=( help)
Further reading
- Gordon, M. A.; Sorochenko, R.L. (2008). Radio recombination lines: their physics and astronomical applications. New York: Springer. ISBN 978-0-387-09604-9.