Date and Time of the Query: 2019-08-20 T06:24:02 PDT
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Notes for object UGC 09799

13 note(s) found in NED.

1. 2008ApJS..177..148F
Re:3C 317
4.2.9. 3C 317 (Abell 2052; UGC 09799); z = 0.034457 3C 317 is a slightly
elongated elliptical with an unresolved nucleus. Two small elliptical galaxies
are present in the field of view, one is located 7" to the northeast, and the
second one 9" to the northwest. The image of this galaxy taken by Martel et al.
(2002) shows a peculiar UV filament ~4 kpc south of the nucleus. This filament
is described as a region of active star formation likely triggered by a recent
merger by Martel et al. (2002). The data were first published by Quillen et al.

2. 2004MNRAS.347..771W
Re:PKS 1514+07
3.4.13 1514+07 (3C 317) There is no obvious UV excess in this galaxy. We
detect both the [O II] and [O III] lines and from these deduce an
average redshift of z = 0.034 [z = 0.035 previously quoted by Tadhunter
et al. (1993)]. The best fit to the continuum of this galaxy is with a
single 15-Gyr component. However, this fit is not ideal ({chi}^2^ =
1.33), probably as a result of differential refraction, since the
airmass for the observations of this source was relatively high (1.33).

3. 2003A&A...403..889T
Re:3C 317
3C 317. This radio galaxy is the main member of the cooling flow cluster
A 2052: its X-ray properties (from HRI observations) were analyzed by
Rizza et al. (2000) who did not find strong evidence of a compact
core. The PSPC flux from the inner region (c.r. = 0.23 +- 0.01 s^-1^,
total exposure of 9240 s from two pointings of 1992 and 1993) is
consistent with the emission from a plasma with T = 1.4^+0.2_-0.1_ keV
and metallicity = 0.60^+0.15_-0.10_ ({chi}^2^_r_ = 1.2), while a simple
power law is not acceptable ({chi}^2^_r_ = 3). If we fix the metallicity
to 0.5 a better fit is obtained at 94% of confidence including a
non-thermal component, that appears very flat ({alpha}_x_ {approx}0.1)
even though the determination of the slope is very uncertain. The flux
results to be {approx}7.4 x 10^-13^ erg cm^-2^ s^-1^. This object has
been observed in September 2000 with the ACIS-S detector on Chandra, for
a total exposure of 36754 s. The core emission has been fit to an
unabsorbed power law with {alpha}_x_ = 1.00^+0.15^ -0.15_ and flux
{approx}2.1 x 10^-13^ erg cm^-2^ s^-1^ in the Rosat energy range
(Blanton et al. 2002; no jet-like structure has been detected). This
emission is ~3.5 times weaker than deduced in the 1993/93 observations
and has a steeper spectrum. However the spectral parameters obtained
from the PSPC data are affected by large statistical fluctuations and we
have verified that they are consistent with the Chandra results at the
{approx}2{sigma} level. Then it is not possible to argue about a
variability of the nuclear X- ray emission. For the analysis of the SED
we have adopted the 1992/1993 observations, closer in time to the HST

4. 2002ApJS..139..411A
Re:3C 317
3C 317-The UV image of 3C 317 is presented in Figure 23a. It displays a
relatively bright nucleus and smooth host galaxy starlight. A very blue
almost linear filament is evident in the UV image. The filament is
~2 kpc in length and is located ~4 kpc south of the nucleus. Martel et
al. (2001) show that the color of the filament is most consistent with
a recent episode of star formation but is not sufficient to represent
the inferred amount of cooling gas if the cooling flow model is
correct. This source is an example of the presence of star formation
which is not obviously correlated with the location of dust.

5. 2001A&A...380..471B
Re:UGC 09799
1514+072 - UGC9799, our measure of the velocity dispersion is very close
to the mean value of 247 km s^-1^ quoted in Hypercat.

6. 1999ApJS..122...81M
Re:3C 317
3C 317. - The isophotes of the core of this elliptical galaxy seem to
extend toward a very faint, dark band located 2" (1.4 kpc) to the
northeast of the nucleus and oriented in a north-south direction. This
may be an extremely faint dust lane. The nucleus is likely unresolved.
Two small elliptical-shaped galaxies are located nearby at distances of
7" (5 kpc) and 9" (7 kpc) to the northeast and north, respectively.

7. 1998ApJS..114..177Z
Re:3C 317
3C 317.--3C 317 is a FR I radio source that is identified with a cD galaxy in
the Abell cluster A2052 and may also be a cooling flow galaxy (Heckman et al.
1989). Baum et al.'s (1988) H{alpha}+[N II] emission, that is close to the
nucleus, subtends east to west, but then the features are bent and fade off to
the north. The optical image R band (F702W) and U band (F370LP) shows a much
less dramatic behavior, with relatively round inner contours and elliptical
ones (in the F702W filter) farther out. No nuclear disk is visible. No UV flux
(F220W) was detected after 900 s integration.

8. 1996MNRAS.281..509S
Re:3C 317
3C 317 A LINER spectrum is seen with strong [O II] {lambda}3727. The
signal-to-noise ratio around the [S III] line is very low.

9. 1994A&AS..105..211S
Re:PKS 1514+07
The radio flux and the radio spectral index have been taken from Condon
et al. (1991).

10. 1993MNRAS.263.1023M
Re:3C 317
1514+07 (3C 317). This radio galaxy is shown by our VLA image to have an
unusual asymmetric core-halo-type structure. Baum et al.(1988) also show
an H{alpha} +[N II] map.

11. 1976RC2...C...0000d
Re:[RC2] A1514+07
= 3C 317
= 4C 07.40
In Abell 2052
Description and Classification:
Ap. J., 140, 35, 1964.
P.A.S.P., 80, 129, 1968.
Ap. J., 140, 35, 1964.
Photometry (UBVR):
A.J., 75, 695, 1970.
Ap. J., 178, 1, 1972.
Ap. J., 178, 25, 1972.
Ap. J., 183, 731, 1973.
Radio Observations:
Ap. J., 142, 106, 1965.
Ap. J., 144, 216, 1966.
Ap. J., 148, 367, 1967.
A.J., 78, 1030, 1973.
X-rays (in Abell 2052):
Ap. J. (Letters), 185, L13, 1973.
Ap. J. (Letters), 188, L41, 1974.

12. 1973UGC...C...0000N
Re:UGC 09799
Brightest in cluster or very rich group not included in CGCG
Companion 0.9, 304, 0.25 x 0.18
{15 14.3} +07 11 at 1.1, 164, 0.50 x 0.45, spiral, m={15.5}
15 14.3 +07 14 at 2.0, 4, 0.20 x 0.18, m=15.6
{UGC incorrectly notes "15 14.2" and "15.6". H. Corwin}

13. 1964ApJ...140...35M
Re:3C 317
No. 38.-cD2 in D4 envelope. Three condensations in-or projected on-envelope.
Outstandingly brightest galaxy in cluster A2052, richness 0.

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