Examples of Rawlings in a sentence
Lacy & Rawlings (1994) also noted the 1.5-arcsec displacement of ‘a’ from the line joining the radio hotspots, but this is not unusual among powerful radio galaxies (e.g. 3C 55 and 265 from Fernini et al.
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We first briefly revisit the three arguments of Lacy & Rawlings (1994) to favour ‘b’ as the radio galaxy.
The locations of the major emission lines are labelled, based on the observed wavelength of [O III] in component ‘a’ and the redshift difference reported in Lacy & Rawlings (1994).within the slit.
We therefore reach the opposite conclusion to Eales & Rawlings (1990) and Lacy & Rawlings (1994), namely that ‘a’, not ‘b’, is more likely to be the jet-producing AGN, although only a deeper radio observation revealing jets will provide a conclusive result.If ‘a’ is the core of the radio source, however, we are left with the problem of explaining the radio emission from galaxy ‘b’, which is several orders of magnitude more luminous than is typical of normal galaxies (e.g. Fabbiano et al.
Although it might seem perverse to demand the presence of a second AGN, very similar systems are known to exist, such as the two flat-spectrum ellipticals near the centre of the low-redshift giant radio galaxy 3C 326 (Rawlings et al.
The remaining argument of Lacy & Rawlings, which we study in more detail here, is the flat radio spectrum of ‘b’ compared with the steep spectrum of ‘a’ (Fernini et al.
A total of 112 min was spent on source, with spectra being taken at two positions along the slit with the usual ‘ABBA’ technique (e.g. Eales & Rawlings 1993).
In addition, the red colours of radio galaxies and the small scatter in the K-band Hubble diagram of their hosts (e.g. Eales & Rawlings 1996; q 2002 RAS Downloaded from https://academic.oup.com/mnras/article/334/3/511/1424270 by guest on 01 May 2021Simpson, Rawlings & Lacy 1999) imply that their stellar populations are old and consequently formed at an early epoch and, in models of structure formation, galaxies form first in the most overdense regions.
We will discuss thearm-length asymmetry further in Section 4.2.2.We also note that our new near-infrared spectroscopy clearly places ‘a’ on the [O III]– radio luminosity correlation of Jackson & Rawlings (1997), while our limit for ‘b’ falls far below it and is a factor of * 2 below all other upper limits.