Date and Time of the Query: 2019-05-22 T02:23:27 PDT
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Notes for object FBQS J121404.1+330945

2 note(s) found in NED.

1. 1998MNRAS.299.1159A
Re:TXS 1211+334
B1211+334: The optical identification is a QSO at z = 1.598 (Wills &
Wills 1976). The VLA map shows a compact double structure with the
brightest component to the East. The MERLIN map shows the same basic
configuration but with a faint central component; the model suggests
that the Eastern component is more compact than the West and that the
central component is resolved. Nevertheless the structure was
sufficiently intriguing that the source was observed with MERLIN at
22 GHz and with the VLBA as a possible lens candidate. The MERLIN
22-GHz map is dominated by the Eastern component, which the model shows
is very compact (< 4 mas); there is just a hint of the Western component
in the map but this is not required by the model. The VLBA map confirms
that the Eastern component is very compact, and if the brightest
component is the active core then there are two antiparallel jets
extended at position angles 40^deg^ and -140^deg^. Alternatively it
could be a one-sided core-jet with the active, rising spectrum, core at
the NE end. The Western component, not resolved by the MERLIN beam,
consists of a diffuse component, elongated perpendicular to the line
joining it with the core, and a faint component ~ 35 mas to the SW. The
faint central component in the MERLIN map is not visible. Clear spectral
and morphological differences rule this source out as a lens but
observations with higher surface brightness sensitivity are needed to
look for faint emission around and between the components in order to
make a reliable morphological classification.

2. 1976ApJS...31..143W
Re:B2 1211+33
1211+334: The object has reportedly been confirmed as a QSO with no redshift
given, by Schmidt(Grueff and Vigotti 1972; Pauliny-Toth et al. 1972). We found
it about 1 mag fainter than on the Sky Survey; this was confirmed by an
image-tube plate (1974 April). The line at 3165 A is too far beyond our
comparison spectrum to allow an accurate wavelength measurement. The adopted
redshift was measured from the {lambda}{lambda}1549, 1909 lines; {lambda}1397
is almost certainly present.

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