Spectrum of the Radio Source 4C 50.11/NRAO 150

• Published in: Nature (London) 1968-01, Vol.217 (5131), p.832-833
• Main Authors: HUGHES, V. A., POTTER, R. V.
• Format: Article
• Language: English
• Subjects: Humanities and Social Sciences; letter; multidisciplinary; Science; Science (multidisciplinary)
• ISSN: 0028-0836; 1476-4687
• DOI: 10.1038/217832a0

MOST extra-galactic radio sources have a spectrum which over a limited frequency range is of the form S αν −α , where S is the flux density and ν is the frequency. The spectral index α is usually constant over a considerable frequency range, which implies a straight spectrum when plotted logarithmically, the average value over all sources being 0.75 with a range from about 0.2 to 1.3. For some sources, however, α changes slowly with frequency with the result that the spectra are concave or convex 1–3 . It is believed that the radiation is produced by the synchrotron mechanism, where energy losses by the electrons can lead in time to an increase in the slope 4,5 and where, in addition, different component sources may contribute to the overall spectrum. High frequency observations by Dent and Haddock 6 showed that two sources, 3 C 84 (NGC 1275, a Seyfert galaxy) and 3 C 279 (a quasi-stellar source), have spectra which decrease in flux density from about 38 MHz towards higher frequencies, but beyond 3,000 MHz the slope of the spectrum is positive. This suggested the presence of a small diameter component which had a low frequency cut-off due to synchrotron self-absorption 7 and stimulated a search for other sources with similar spectra. Kellermann (personal communication) has recently observed fourteen sources with irregular spectra, of which some have a tendency towards these latter characteristics, but so far there have been no published spectra similar to 3 C 84 and 3 C 279. Recent observations at the frequencies of 3,200, 6,600 and 10,600 MHz, however, using the 150 foot telescope of the Algonquin Radio Observatory, when combined with the observations by other observers 8–11 , have shown that the source 4 C 50.11/NRAO 150 is of this form but with the addition of two apparent peaks at frequencies of about 350 and 9,000 MHz. The source is included in the list by Kellermann, but details of the characteristics failed to show up because of the omission of low frequency observations and the new measurements between 5,000 and 15,000 MHz.