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Date and Time of the Query: 2019-06-20 T07:44:26 PDT
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Notes for object NSCS J145715+222009

8 note(s) found in NED.


1. 2007MNRAS.376.1073Z
Re:MS 1455.0+2232
Cl 1455+2232 . Chapman et al. (2002) present a previous analysis of these submm
data, while Cooray et al. (1998) discuss a 28.5-GHz survey for point sources.

2. 2007A&A...472..727B
Re:ZwCl 1454.8+2233
4.5 ZW CL 1454.8+2233 - This cluster is very discrepant with respect to the
behavior of other clusters in the L_bol_-T relationship given in Sect. 6. ZW CL
1454.8+2233 was identified as a relaxed cluster hosting a massive cooling flow
by Allen et al. (1996) using ASCA and ROSAT data. A 10 Ks Chandra observation
revealed the presence of two surface brightness edges on opposite sides of the
X-ray peak which were discussed by Mazzotta et al. (2001) under the hypothesis
of a merging scenario. The 90 Ks Chandra observation analyzed by us confirms a
very disturbed morphology. The surface brightness profile is inadequately
described by a {beta}-model (the probability to accept the spatial fit is lower
then 0.1%) both for the presence of the cooling core and for the presence of
some surface brightness jumps. For this reason no values for R_c_ and {beta} are
indicated in Table 2. On the other hand for the spectral analysis a
single-temperature model was accepted. The null-hypothesis probability is about
5%, a little less than the t hreshold indicated in Sect. 2.3. We tried also to
use a cooling flow spectral model mkcflow added to a mekal model but the
improvement in the fit is minimal. The thermal complexity of this cluster, which
could explain the peculiarity of its behavior in the L_bol_-T relation,
convinced us to exclude it from the fit of the L_bol_-T relation.

3. 2002MNRAS.330..755F
Re:MS 1455.0+2232
MS 1455.0+2232: This cluster has the largest calculated value of R_30_
in our sample (3.75 arcmin) and, whilst this radius lies comfortably
within the central CCD, the radial density profile of this cluster
indicates that the cluster may well spill out into two of the
surrounding CCDs. To negate this problem, we use only the furthest CCD
from the cluster (with background area at least 12 arcmin distant) to
estimate our field population. This solution, whilst increasing the
statistical error on the blue fraction estimate, will prevent any
cluster contamination of our field sample.

4. 2002ApJS..139..313D
Re:ZwCl 1454.8+2233
5.37. Zw 7160 This cluster, also designated MS 1455+22, was one of
the clusters targeted in the weak lensing study by Smail et al.
(1995a). It has a possibly massive cooling flow (Allen et al.
1996), and it has one bright blue arc, discovered by Le Fevre
et al. (1994), plus several fainter red and blue arcs. A bright
"radial arc" in the southern part of the cD halo was found by
Newbury & Fahlman (1999), who also developed a strong lensing
model for this system. The dominant peak in the light
distribution in Figure 45 is caused by an elliptical galaxy
which is likely to be a field galaxy in front of the cluster,
since it has no associated X-ray emission (Smail et al. 1995a;
Mazzotta et al. 2001a) and is slightly bluer than early-type
galaxies at the cluster redshift. The data of Smail et
al. (1995a) are based on a longer integration time on a larger
telescope (the 4.2 m WHT), but with poorer seeing (0.9" in the I
band vs. 0.7" for our data) and a less sensitive CCD. The V-band
catalog used here actually has a slightly higher source density
than the I-band catalog they used for their weak lensing
measurements. The mass map presented here is similar to theirs
and appears elongated in the same direction, but we see no
evidence for the secondary "dark" peak visible in their mass
maps. We conclude that this is probably a noise peak. The peak
in the mass distribution is very closely centered on the cD
galaxy in the cluster center, and the mass distribution is
elongated in the same direction as the cD halo. Mazzotta et
al. (2001a) analyze Chandra data of Zw 7160 and find it to have
X-ray characteristics similar to RX J1720.1+2638 (see section
5.33) with a cool core bounded by sharp edges in the surface
brightness distribution to the north and south of the cluster
center. The most likely explanation for this structure is the
movement of a cooler, group-sized subhalo along the major axis
of the dark matter distribution in the cluster. As for RX
J1720.1+2638, Mazzotta et al. (2001a) propose that the cool core
corresponds to an old group-sized halo which was formed almost
at the same location as the cluster, instead of being a rem-
nant of a recent merger event involving an infalling subhalo
which was formed outside the main cluster. The main arguments
against the latter scenario are the "relaxed" overall appearance
of the X-ray surface brightness distribution and the possible
presence of a massive cooling flow. However, given the highly
elongated dark matter distribution seen in our mass map, it
appears that a merger scenario cannot be ruled out. Carlberg et
al. (1996) measure a velocity dispersion for Zw 7160 of 1133 +/-
140 km s^-1^, consistent with the result obtained from an SIS-type
model fit to our weak lensing data.

5. 1999ApJ...517..587L
Re:MS 1455.0+2232
MS 1455.0+2232 at z = 0.26, displays the highest signal-to-noise ratio
HRI surface brightness profile in this sample after Abell 2390. It is
highly radially symmetric and strongly peaked. This cluster has the
highest H{alpha} luminosity and the largest H{alpha} extent among the
D92 sample. Allen et al. (1996) estimate it to have one of the largest
cooling flows known, ~1500 M_sun_ yr^-1^. Our X-ray centroid lies at
R.A. (1950) = 14^h^55^m^00.4", decl. (1950) = 22^deg^32'36.0", which
is within ~5" of the optical center given by G94. The HRI surface
brightness profile is extremely well constrained by the slope of the
profile, and the values of the fitted parameters are insensitive to
choice of inner cutoff radius out to a value of 103 kpc. Therefore,
based on the surface brightness profile, we have chosen a cutoff of only
20 kpc, which provides a good statistical fit to the HRI data.
Our mass estimate is in close agreement with the X-ray derived mass
estimate of Allen et al. (1996), differing by only 5%. The gravitational
lensing mass estimates, based on a strong arc of unknown redshift at
52 h^-1^ kpc (WF97, from an arc in the Le Fevre et al. 1994 survey) and
weak lensing observed by Smail et al. (1995) at 237 h^-1^ kpc, are
larger by factors of 1.8 and 1.3, respectively.

6. 1999A&A...351..413M
Re:MS 1455.0+2232
MS 1455.0-2232 (1E 1455+2232)
Three observations were performed for this cluster. Each exposure time
was 4 ksec, 4 ksec, and 7 ksec. No correlation was found between sources
higher than 3{sigma} in the HRI field of view and objects cataloged in
HRASSCAT or ROSID. Since the exposure times of three observations were
comparable to each other and each exposure time is not long enough, we
chose the way to merge three files believing that the pointing of each
observation was completely identical. The position of the X-ray center
on HRI is (14^h^57^m^14.94^s^, +22^d^20^m^35.5^s^)(J2000). The position
of the X-ray center is consistent with that of the brightest cluster
member galaxy within the HRI pointing accuracy.

7. 1998A&A...330..801P
Re:E 1455+22
E1455+223 This cluster was observed by ASCA and ROSAT (Allen et al. 1996a) and
was shown to host a massive cooling flow. Our analysis reveals clearly the
presence of two non-resolved point sources at the cluster center (3.7{sigma}
level at least); since the HRI image we used is a merge of three separate
pointings (92Jan, 93Jan, 94Jul) we checked that the double source is not an
artifact due to small pointing offsets: this is not the case and, actually, the
presence of the double source is conspicuous in at least two individual
pointings. According to the APM data base, the two maxima are located within
the cD envelope and, thus, very probably related to the cooling flow. Again here
- as can be seen on Fig. 5 - there is a clear twist between the inner core and
scales 4-5. But like for MS 735 and A 2390 we find a good agreement between
alignment of the cD (PA is 36 deg. APM) and outer scale (PA at I_2_ is 39 deg.)

8. 1994ApJS...94..583G
Re:MS 1455.0+2232
Poor cluster with one and possibly two bright ellipticals. The galaxy to
the E is the brighter and is a radio emitter. It has strong {lambda}3727
[O II] emission with an equivalent width of 60 A (Mason et al. 1981). An
apparent gravitational arc is located slightly to the NE of this galaxy
(see Lefevre et al. 1994). In Donahue (1990) this cluster has the
strongest emission line flux (H{alpha} and [N II]) of their survey,
signifying a possible cooling flow.


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