Date and Time of the Query: 2019-06-16 T16:01:56 PDT
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Notes for object ABELL 1795

9 note(s) found in NED.

1. 2008ApJ...687..899R
Re:ABELL 1795
A1795.-The CDG is well known to harbor a tail of blue emission that is thought
to be due to star formation triggered by compression of the gas by the radio
source (McNamara et al. 1996a, 1996b; Pinkney et al. 1996; O'Dea et al. 2004).
The R- and I-band images were affected by scattered light, which was masked as
thoroughly as possible.

2. 2006MNRAS.372.1496S
Re:ABELL 1795
5.11 Abell 1795 - This is a cold front cluster (Markevitch, Vikhlinin & Mazzotta

3. 2006ApJ...643..730D
Re:Abell 1795
The central galaxy of Abell 1795 contains a famous extended filament of optical
line emission, mapped using long-slit spectroscopy by Cowie et al. (1983). The
central bright galaxy also hosts a compact radio source 4C 26.42 (Caswell &
Wills 1967). Chandra observations by Fabian et al. (2001) revealed a 40"
X-ray filament that substantially overlaps the optical emission line filament.
The results we report on this cluster agree well with previous X-ray results.
Our projected and deprojected one-temperature and two-temperature fits are in
excellent agreement with the Chandra data analysis by Ettori et al. (2002). They
also agree with the projected one-temperature, N_H_, and metallicity fits from
XMM-Newton analysis of Abell 1795 by Tamura et al. (2001b).

4. 2004ApJ...608..166N
Re:ABELL 1795
A1795. There is a Seyfert 1 galaxy, 1E 1346+26.7, 5' off-axis.
Normalizing the reference model to the MECS data gives a PDS estimate
of 0.3^+0.1^10^-2^ counts s^-1^. In the cluster center there is LINER
PKS 1346+26. Its flux estimate cannot be given because of the
projection with the bright cluster center. However, LINERS usually have
2-10 keV luminosities 1-3 orders of magnitude smaller than classical
Seyfert galaxies (Terashima et al. 2002). AGN RX J1343.9+2712 is outside
the PSPC image, and thus an flux estimate cannot be given. The field of
A1795, together with Coma, is unusual in its large number of
AGNs/QSOs. For A1795 this is probably not a problem though, because HXR
emission is negative (consistent with 0) and likely not significantly
contaminated by any AGNs. We will use the 1E 1346+26.7 estimate in the

5. 2002ApJ...576..688B
Re:ABELL 1795
A1795. A1795 is known to have soft excess emission from EUVE/DS
observations (Bonamente et al. 2001b). The EUVE excess was more
prominent at large radii (see, e.g., Fig. 4 of Bonamente et al. 2001b),
while the PSPC data analyzed here shows soft X-ray excess emission
extending from the central regions to the limits of the C-band
detection, at the level of {eta} = 10%-20%. There is no evidence of
C-band excess absorption in this analysis of PSPC data.

6. 2002ApJ...567..202E
Re:ABELL 1795
Abell 1795 contains the tailed radio source 4C 46.42. Van Breugel,
Heckman, & Miley (1984) present radio fluxes and estimate {alpha}~1.0 over
the radio range. Ge & Owen (1993) present the radio image and Faraday
rotation data. We use X-ray data from P98, W97, and ES91, and estimate
the density close to the radio source to be ~4 times the mean density in
the inner (IPC, PSPC) X-ray beam.

7. 1999MNRAS.306..857C
Re:ABELL 1795
The observed galaxy is associated with the radio source 4C+26.42.

8. 1998MNRAS.301..609B
Re:ABELL 1795
Abell 1795: Fig. 1k. This cooling flow cluster shows asymmetry in its
galaxy distribution (Oegerle, Fitchett & Hoessel 1989). However,
combined with velocity information, no optical substructure is present
(Girardi et al. 1997). The northern galaxy elongation is mimicked by
the X-ray emission, which also shows an excess to the north of the
cluster core (Briel & Henry 1996). The cooling flow is evidenced by a
lower temperature component to the X-ray emission (White et al. 1994;
Briel & Henry 1996), with T_cool_ ~ 2.1 +/- 0.3 Gyr, and
M^dot^ ~ 478 M_sun_ yr^-1^ (Edge et al. 1992). Recently, attention has
been focused on HST examination of the cD galaxy. This galaxy shows
excess H{alpha} and UV filaments, as well as a dust lane coincident with
the edges of the radio lobes (McNamara et al. 1996a,b; Pinkney et al.
1996), which may imply massive star formation in a cooling flow
(Smith et al. 1997).

9. 1997ApJ...482...41G
Re:ABELL 1795
This is a regular cluster with a central condensation (C). Hill & Oegerle
(1993) detected substructures significant only at about 97%. The VDP of
the main sample strongly decreases toward the cluster center. The low-
{sigma} core structure C contains a cD galaxy, whose velocity is
consistent with the mean velocity of the C structure and that of the
whole cluster. Moreover, a strong cooling flow was observed (Edge et al.
1992; Cardiel, Gorgas & Aragon-Salamanca 1995). All these findings
indicate that this cluster is a very relaxed cluster (see also the
discussion in Section 5.3). The better agreement of T with the {sigma} of
the MS - C sample rather than with the MS sample could confirm that the
galaxies in the core could have been slowed down by relaxation processes
(e.g., dynamical friction).

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