Date and Time of the Query: 2019-06-18 T22:01:42 PDT
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Notes for object ABELL 1914

8 note(s) found in NED.

1. 2007MNRAS.376.1073Z
Re:ABELL 1914
Abell 1914. This field only has about an hour of SCUBA integration time,
resulting in a very shallow map. Grego et al. (2001) and LaRoque et al. (2006)
give prior SZ effect measurements at 30 GHz, and Cooray et al. (1998) discuss
point sources in this cluster. Also, Jones et al. (2005) use the Ryle telescope
to measure the SZ effect in this cluster.

2. 2005MNRAS.357..518J
Re:ABELL 1914
3.7 A1914
A1914 was observed with the ROSAT PSPC for 8.6 ks in 1992 July. There are
several pieces of evidence to suggest that A1914 is undergoing a merger. The
ROSAT image (see Fig. 5) shows significant substructure in the core of the
cluster, but no evidence of a cooling flow. The temperature, measured from an
ASCA observation, is rather high at 8.56 +/- 0.39 keV. The Palomar Observatory
Sky Survey (POSS) optical image shows two distinct groups of galaxies with no
single dominant galaxy, and finally there is a diffuse steep-spectrum radio
source to the northeast of the cluster centre that is detected in the 300-MHz
Westerbork Northern Sky Survey (WENSS) (Rengelink et al. 1996) and 1.4-GHz NVSS
surveys. This raises the question of whether A1914 should be included in our
sample, as it is possible that the cluster gas might be far from hydrostatic
equilibrium and difficult to model. We choose to include it in our sample
because simulations (Grainger 2001) show that even including clusters with large
internal kinetic energies in their gas does not bias the sample average H_0_.
However, such clusters can have a large scatter about the mean value - this does
appear to be the case with A1914 and also with A2218.
We fitted a {beta}-model to the ROSAT PSPC image with the parameters given in
Table 2. The residuals (see Fig. 2) were noticeably poorer than those from the
fits to other clusters such as A1413; a Monte Carlo analysis shows that the
hypothesis that the true structure is a {beta}-model and that the features seen
result from Poisson noise can be rejected at the 4{sigma} level. A1914 was
observed with the RT on 19 occasions between 1996 March 6 and April 16; the
full-resolution radio image is shown in Fig. 5. There are clearly several radio
sources near the cluster centre, some of which are also detected in a VLA image
(Fig. 5). We used the VLA source positions and positions from a long-baseline RT
image to estimate the fluxes of nine sources; the fluxes found and subtracted
are shown in Table 3. Fitting the source-subtracted short-baseline data to the
X-ray-based model (Fig. 4) results in a value of H_0_= 119^+42^_-31_ km s^-1^
Mpc^-1^ with errors just from the SZ fitting, and H_0_= 119^+5 6^_-35_ km s^-1^
Mpc^-1^ including the other sources of random error. For {LAMBDA}CDM this
becomes H_0_= 129^+60^_-38_ km s^-1^ Mpc^-1^.

3. 2005ApJ...624..606J
Re:ABELL 1914
A1914 (z = 0.17): This cluster has two peaks surrounded by an outer roughly
elliptical envelope. The southeast peak extends and curves toward the northwest
peak. The temperature map shows a hot region between the two peaks suggesting
shock-heated gas (Govoni et al. 2004). In this observation, the 0.5 Mpc
aperture fell on two of the ACIS-I CCDs.

4. 2002ApJS..139..313D
Re:ABELL 1914
5.23. A1914 The mass peak is located inside the triangle formed by
the three brightest early-type cluster members and appears to have
extensions toward each of these galaxies. Both the light
distribution and the galaxy number density distribution in the
cluster are highly elongated, and both have peaks that coincide closely
with the mass peak. An analysis of the X-ray morphology of this cluster
by Buote & Tsai (1996) indicated that A1914 is a relaxed system, but
Jones et al. (2001) point to several pieces of evidence that suggest
other-wise, including the absence of a cooling flow, the high
X-ray temperature, the lack of a well-defined center in optical
images, and the fact that the X-ray data are very poorly fitted
by a {beta} model. Furthermore, Jones et al. (2001) derive a Hubble
constant H_0_ = 119^+46^_-38_ km s^-1^ Mpc^-1^ from SZ measurements in
this cluster, 1.6 {sigma} above the mean H_0_ value obtained from their
sample of five clusters. Our mass map also seems to indicate an
unrelaxed system, with a mass center that is significantly
offset from the brightest cluster galaxy. Several red and blue
arc candidates are visible near the mass center and around the
brightest cluster galaxy.

5. 2002ApJ...576..688B
Re:ABELL 1914
A1914. This cluster shows a behavior very similar to that of
A1361, with possible soft excess emission not to exceed ~ 20%-30%.

6. 2001ApJ...548..639K
Re:ABELL 1914
A1914. - A very steep spectrum source has been known to exist in this
cluster for quite some time (e.g., Kulkarni, Mantovani, & Pauliny-Toth
1990). The center of this cluster contains a number of point sources
visible in the FIRST images, at least two of which overlap the radio halo.
Accurately masking the point sources in the WENSS image was difficult due
to their small separation, so the actual error in our measurement may be
slightly greater than that quoted in Table 2.

7. 1999NewA....4..141G
Re:ABELL 1914
A 1914. A very steep spectrum radio source ({alpha} > 2) is reported by
Komissarov & Gubanov (1994). From higher resolution images
(Roland et al. (1985) and the image retrieved from the FIRST survey) it
is evident that the discrete sources cannot account for the extended

8. 1999MNRAS.306..857C
Re:ABELL 1914
This is a complex binary cluster, and we have only taken a spectrum of
the brighter (to the SW) of the two dominant galaxies. The radio
source 4C+38.39 is probably a radio halo and hence not associated with
the observed galaxy.

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