Contents of: J/AJ/137/4436/./notes.dat

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## (from tabmap V6.0 (2016-08-18)) 2020-07-04T14:07:24
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#-- J/AJ/137/4436 Coma cluster VLA survey (Miller+, 2009)
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#---Table: J/AJ/137/4436/./notes.dat Notes  (32 records)
#      Note A1     ---   Note code
#      Text A78    ---   Text of the note
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N|
o|
t|
e|Text
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a|Radio emission is resolved, providing a likely explanation for the somewhat
a| large radio-optical separation.
b|The morphology of the extended radio emission is consistent with that of the
b| optical. In the case of spiral galaxies this indicates that the radio
b| emission traces the galaxy disk, whereas for elliptical galaxies the center
b| of the galaxy appears to be where the radio emission originates.
c|Source appears to be the host of a radio double. The indicated separation is
c| for distance from optical source to midpoint of the radio counterparts listed
c| in the last two columns.
d|Source separation is greater than 3". See Figure 5.
e|Optical position for bright clump within larger galaxy.
f|Galaxy appears to be one member of a galaxy pair. Many of the possible
f| companions may be found in Table 3.
g|Radio emission is unresolved, but lies within the optical extent of the galaxy
h|Optical source not in SDSS catalog due to proximity to bright source, usually
h| the diffraction spike of a saturated star. The position represents the
h| coordinates of the peak of the object as measured directly in the
h| SDSS r band image.
i|Although the radio-optical separation is acceptable for the r magnitude of the
i| potential counterpart, visual inspection of the overlaid radio contours
i| strongly suggested the sources are unassociated.
j|The radio source was assigned to a galaxy with a smaller separation
j| (see Table 3).
k|Same comment as "a" plus the radio source is detected at less than 5{sigma}.
l|The radio morphology is that of a radio double source, and this optical
l| counterpart appears to be a chance superposition of a galaxy with one of the
l| lobes. The optical counterpart for the radio emission would be expected to
l| lie in between the lobes, and not coincident with one.
m|Visually appears offset. The radio emission also appears to be a lobe of a
m| separate FR2 type source, and hence not associated with this galaxy.
n|This radio source was assigned to a brighter galaxy with radio-optical
n| separation greater than 3''. It may be seen in Figure 5.
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