The following document lists the file notes.dat
from catalogue J/AJ/137/4436.
Also available:
plain copy of the file
with f77 program to read file
into arrays
or line by line
File is also available in
FITS,
Tab-separated format,
or in HTML.
## (from tabmap V6.0 (2016-08-18)) 2024-03-29T16:01:56 #--------------------------------------------------------------------------- #-- J/AJ/137/4436 Coma cluster VLA survey (Miller+, 2009) #-------------------------------------------------------------------------- #---Table: J/AJ/137/4436/./notes.dat Notes (32 records) # Note A1 --- Note code # Text A78 --- Text of the note -------------------------------------------------------------------------------- N| o| t| e|Text -|------------------------------------------------------------------------------ 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. --------------------------------------------------------------------------------