ner_tags: O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O O O O B-Telescope O O O O O O O O O O O O O O O O O O B-Wavelength O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O B-Wavelength O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O B-Wavelength O B-Wavelength O O O O O O O O O O O B-Wavelength O O O O O O O O O
tokens: because of enhanced mass outflow from the circumbinary disc. In the first case, we note the apparent dimming of the ruff on days 23 and 26 is suggestive that the effect may be partly artefactual. We also note that the ruff's extent of ≳50 mas is at the upper limit of angular scales to which the VLBA is sensitive, because the shortest VLBA baselines give only sparse coverage of the centre of the uv -plane. The third case is intriguing given optical observations of Blundell et al. ( 2011 ) that provided evidence that the inner circumbinary disc structure was disrupted during a flare in 2004 October. In the 2003 July observations, there are hints of detachment between the core components and the radio ruff from day 31 onwards, raising the possibility that the enlarged ruff is a manifestation of an ejected circumbinary disc. However, this would require a very fast outflow speed – at 5.5 kpc, 50 mas corresponds to a physical size of 4 × 10 13 m. To cover this in ∼10 d would require an outflow speed exceeding 40 000 km s −1 , which seems improbably high (cf. Mioduszewski et al. 2004 ). 5.4 The unified picture Despite the lack of contemporaneous optical and radio monitoring data, there are enough similarities between what we see in these milliarcsecond-scale observations and what is seen at other scales and frequencies that we can draw out some general characteristics. In Fig. 4 , we see that jet launch speeds appear to fall over a period of about 30 d before the flare begins and jet speeds increase dramatically on or around day 15. A similar decline in speed is seen in the optical jet lines in fig. 6(e) of Blundell et al. ( 2011 ), where jet speeds decline from ∼0.27 c to ∼0.24 c over the 20 d prior to a flare. Both in the 2011–2012 observations, and during the latter half of the 2003 campaign, we see bright, fast ejections, punctuated by gaps of 5 to 10 d. Again, almost identical behaviour is seen by Blundell et al. ( 2011 ) in the optical jet lines, where the intensity of the optical jet lines is lowest in the days immediately preceding the start of the flare. This stands in contrast to the behaviour of the jet in the early days of the 2003 campaign, where the jet has a more steady character. The difference is most clearly seen by comparing the first and last frame of Fig. 3 (noting that the images of all epochs are contoured to the same minimum level): in the first frame we see faint bolides set against an apparently steady background flow, while in the last we see a succession of bright, compact bolides separated by gaps of low/no emission. Taken together, we note that the variations in both the speeds of the optical emission lines and the speeds determined by the milliarcsecond scale bolides possess remarkably similar characteristics. In the absence of simultaneous, time-resolved optical and radio observations, this coincidence is intriguing evidence that the ejecta revealed by optical emission are indeed directly related to the ejecta seen