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Date and Time of the Query: 2018-12-12 T13:46:48 PST
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Notes for object UGC 00595

7 note(s) found in NED.


1. 2006ApJS..164..307M
Re:3C 029
A round, undisturbed elliptical with a bright central unresolved component
(nucleus). Several globular clusters are present in the field of view. This
galaxy has a faint compact nucleus in the optical and in the UV. The UV nucleus
was first detected by Allen et al. (2002).

2. 2003A&A...403..889T
Re:3C 029
3C 29. X-ray emission from this radio galaxy (observed in 1992 with an
exposure of 15 197 s), offset by {approx}30' in the FOV (centered on the
cluster A 119), has been detected with a {approx}3{sigma} confidence level
(c. r. = 5 +- 2 x 10^-3^ s^-1^). Assuming a power law spectrum with
{alpha}_x_ = 1.0 we deduce an unabsorbed flux of 1.0 x 10^-13^ erg
cm^-2^ s^-1^. The X-ray emission is consistent with that expected from
the correlation between the radio and X-ray core luminosities (Canosa et
al. 1999). To account for a possible contribution from a thermal hot
corona then, as for the data of HW99, this emission is assumed as an
upper limit to the core luminosity.

3. 2002ApJS..139..411A
Re:3C 029
3C29.-The UV image of this galaxy is presented in Figure 7a and has
been smoothed by a Gaussian with an FWHM of 3 pixels. The F702W image of
this galaxy, shown in Figure 7b, shows a very round and smooth light
distribution, with a relatively faint compact nucleus. At higher
contrast a distorted X-shaped dust lane is visible. This is seen more
clearly in the F555W image and in more detail in Sparks et al. (2000).
The two filaments that cross to form the X intersect at the
nucleus of the galaxy and extend approximately 1" out from the
nucleus. We note that the linear feature positioned ~2" northwest
of the nucleus in the F702W image published in Martel et al. (1999) is
an image processing artifact. The UV image consists of faint extended
galaxy emission, visible out to a 2" radius, and the compact nucleus is
detected. The UV image shows no evidence of the X-shaped dust feature
although this is likely due to the relatively low signal-to-noise
ratio of this observation. This image represents the first detection of
this object in the UV as it was undetected with the Faint Object Camera
(FOC) observation of Zirbel & Baum (1998). Neither the optical nor the
UV emission shows any relation to the radio jet axis.

4. 2001A&A...380..471B
Re:UGC 00595
0055-016 - UGC 595 - 3C 29, this galaxy belongs to the rich cluster A119
and is D26 in the Dressler (1980) list. Smith et al. (1990) measured a
velocity dispersion of 199 +/- 18 km s^-1^ but recently Wegner et al.
(1999) give a value of 253 +/- 17 km s^-1^ in better agreement with our
measurements.

5. 1999ApJS..122...81M
Re:3C 029
3C 29. - The host galaxy is very circular and smooth with no outstanding
morphological features. The nucleus is consistent with the PSF of the
WFPC2 camera.

6. 1998ApJS..114..177Z
Re:3C 029
3C 29.--This galaxy is a rather normal elliptical galaxy (see, e.g., Baum et
al. 1988). Smith's (1988) contour plot shows a very round galaxy, and the
higher resolution F702W HST image in Appendix A does not show any more detail.
The U-band FOC image (F370LP) shows a similar structure. No UV flux was
detected after 900 s integration with the F220W filter. At the 3{sigma} limit
above the sky, the maximum F220W magnitude that 3C 29 could have is 19.50.

7. 1993MNRAS.263..999T
Re:PKS 0055-01
0055-01 (3C 29). Weak [O III] {lambda}5007 and H{beta} emission lines are
detected. The continuum colours appear similar to those of early-type
galaxies, although the Ca II H & K absorption lines may be stronger than
average.


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