Date and Time of the Query: 2019-06-26 T17:35:13 PDT
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Notes for object 3C 028

7 note(s) found in NED.

1. 2008ApJ...687..899R
Re:3C 028
3C 28.-An excess of UV flux has been detected in the CDG by Wills et al. (2002)
and was ascribed by them to active star formation.

2. 2006MNRAS.370.1893H
Re:3C 028
A1. 3C 28 - The core of this low-excitation source is undetected in both radio
and X-ray. We derive X-ray upper limits from the local count density, which is
high as the source lies in the centre of one component of the merging cluster
Abell 115 (e.g. Gutierrez & Krawczynski 2005). Limits on luminosities in
absorbed and unabsorbed components were derived assuming photon indices of 1.7
and 2.0, respectivelY.

3. 2006ApJS..164..307M
Re:3C 028
3C 28 is an elliptical elongated on the northwest to southeast direction. At
least two other sources are present in the field of view: one is on the edge of
the chip to the northwest and the second one is 10.3" to the southwest. This
galaxy is the cD of the X-ray cluster Abell 115 (McCarthy et al. 1995).

4. 2005ApJ...619..161G
Re:3C 028
Note that the morphology of 3C 28.0 is very similar at the
two wavelengths for which we have high-resolution radio maps,
1.4 GHz (Feretti et al. 1984) and 5 GHz (Riley & Pooley 1975).
The radio data show double-sided jets that have drilled two
channels through the compact X-ray-bright region at the subcluster
core. The jets transition into radio lobes immediately
as they leave the compact region. The radio lobes clearly avoid
the compact region. The Chandra data show no evidence for a
cavity or bubble associated with the radio lobes.

5. 2002AJ....124.1239H
Re:3C 028
3C 28: Although the optical position has been used for
measurements, a very faint core has been detected at 5 GHz
(C band) that is coincident with the optical ID
(J. T. Stocke 1999, unpublished).

6. 1999MNRAS.309..969H
Re:3C 028
3.1 3C 28
This low-excitation radio galaxy lies in the double X-ray cluster
Abell 115 (Feretti et al. 1984; Worrall, Birkinshaw & Cameron 1995). It
has a relaxed double radio structure with no detected radio core,
although thin radio filaments emerging from the host galaxy may suggest
that it is not an inactive object (Leahy, Bridle & Strom 1998). 3C 28
lies in the northern component of the X-ray cluster, with its lobes
straddling (within the ROSAT pointing accuracy) the peak in the X-ray
surface brightness. Radial profile fitting shows the source to be
significantly extended (Table 2). A point-like component is not
significant on an F-test. It seems likely that most of the emission from
the central peak originates in the central regions of a cooling flow, as
suggested by Feretti et al. (1984). We therefore take the best-fitting
point-like component as an upper limit on the AGN contribution.

7. 1995ApJS...99...27M
Re:3C 028
3C 28(z = 0.19; Fig. 8).-This giant elliptical galaxy is the dominant
member of the X-ray cluster Abell 115. An Einstein image of the cluster
is given in Feretti et al. (1984). The H{alpha} image shows a small curved
filament extending to the south-west. This filament lies in a region of
low surface brightness in the X-ray image. The radio source is a diffuse
FR I source (Feretti et al. 1984) that is rather typical of the cooling-
flow cluster sources described by Baum & Heckman (1987).

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