Date and Time of the Query: 2019-07-23 T11:30:47 PDT
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Notes for object ABELL 1835

6 note(s) found in NED.

1. 2007MNRAS.376.1073Z
Re:ABELL 1835
Abell 1835. This field contains two known lensed submm sources (Ivison et al.
2000) and has also been imaged at 1.1 mm with BOLOCAM (D. Haig, private
communication). In addition, a small amount of emission in the central regions
is detected at reasonable significance. Edge et al. (1999) associate this flux
with dust emission from the central galaxy; this is supported by the detection
of CO emission in this galaxy.
Grego et al. (2001) detect an SZ effect decrement at 30 GHz, and Cooray et
al. (1998) discuss point sources detected at the same frequency. Mauskopf et al.
(2000) and Benson et al. (2003) both find data consistent with a submm SZ
increment in this cluster using SuZIE I/II. Both Schmidt, Allen & Fabian (2001)
and Majerowicz, Neumann & Reiprich (2002) present X-ray measurements of this
cluster, finding a central ICM temperature of 4.0 and 4.4 keV, respectively.
Abell 1835 has a strong cooling flow, and thus exhibits a temperature gradient
between the centre and the hotter outer regions.

2. 2005MNRAS.359..417S
Re:ABELL 1835
A1835 - The multiple-image interpretation of Schmidt, Allen & Fabian
(2001) is ruled out by the new WFPC2 data presented in this paper,
specifically, the differences in surface brightness between K0, Kl and K3.
The absence of multiple-image constraints therefore results in a model
similar to those of A 209 and A 1763, with just a single free parameter -
the central velocity dispersion of the central cluster-scale mass

3. 2004MNRAS.352.1413S
Re:Abell 1835
Abell 1835: For this cluster, M00 measured a Hubble constant H_0_=
66^+38^ _-22_ km s^-1^ Mpc^-1^ for a kT= 9.8 keV isothermal model with
the {beta}-model parameters {theta}_c_= 13.2 arcsec, {beta}= 0.58 and
n_e0_ = 0.058 cm^-3^ from a fit to ROSAT data. This temperature was
obtained by allowing for a cooling flow component in the core of the
cluster. R02 obtained an angular diameter distance to the cluster which
implies H 0= 55.4+13.2 -8.8 km s^-1^ Mpc^-1^, based on a kT= 8.21 keV
isothermal model (no cooling flow correction). The difference between
these two measurements can be attributed to the different isothermal
temperatures and small differences in the assumed {beta}-model
parameters. Note also that the {beta}-model parameters used in these
studies are significantly different from those determined from Chandra
(Table 4) over a smaller range of radii. This explains the difference in
the predicted Hubble constant. However, the M00 result is consistent
with the result we obtain from the deprojected and extrapolated X-ray
data, which shows that it is possible to correct the {beta}-model
partially in the central region of the cluster when the surface
brightness profile observed with the ROSAT field of view is used. For
larger radii this approximation will fail, however, because of the fixed
{beta}-model slope.

4. 2004MNRAS.352.1413S
Re:Abell 1835
3.2.2 Abell 1835 The detection of the SZ effect in Abell 1835 was
published by Mauskopf et al. (2000, M00) using the SuZIE I and SuZIE II
bolometers. R02 have also published a detection using the OVRO
interferometer at 30 GHz, which provides a consistent, but more precise
determination of the Comptonization parameter. Here we compare our
Chandra Comptonization profiles with the co-added SuZIE I scans
published by M00, using their {phi}=-0.1 arcsec offset of the X-ray
cluster centre from the scan centre. To calculate their difference
channels D3 (two beams separated by 4.6 arcmin) and T123 (triple beam
chop of three beams separated by 2.3 arcmin) of the bolometer array we
followed the description given by M00.

5. 2002ApJS..139..313D
Re:ABELL 1835
5.22. A1835 is the most X-ray luminous cluster of galaxies in the
XBAC and BCS catalogs. From an analysis of 30 ks of Chandra
observations of this cluster, Schmidt, Allen, & Fabian (2001)
find a steep drop in the X-ray gas temperature from kT ~ 12 keV at
0.5 h^-1^ Mpc to kT~ 4 keV at the cluster core, and they find a
cooling flow with a mass deposition rate of 230^+80^_-50_ M_{sun}_
yr^-1^ . The cluster has a regular morphology in the X-ray image,
indicating that A1835 is a relaxed system. The presence of the
cooling flow and the optical appearance of the cluster also
indicate that all the constituents (galaxies, the hot
intracluster medium [ICM], and dark matter) of the cluster are
in dynamical equilibrium. The light map in Figure 31 is
contaminated by a bright fore-ground galaxy close to the north
edge of the field. The mass map shows a strong peak, well
aligned with the position of the central cD galaxy, and similar
peaks in the light and number density distributions. Several
blue arcs are visible around the cluster center. By fitting the
X-ray gas temperature profile to a Navarro, Frenk, & White
(1997) model of the mass density distribution, Schmidt et
al. (2001) obtain an effective velocity dispersion {sigma} =
1275^+150^_-100_ km s^-1^, consistent with, but slightly higher
than, our SIS model fit result given in Table 2. Schmidt et al.
(2001) also obtain a similar result by fitting their X-ray data
to a nonsingular isothermal sphere model, and the mass values we
plot in Figure 51 are also in good agreement with the best-fit
Navarro et al. (1997) model derived by Schmidt et al. (2001) for
the radial mass profile.

6. 1999MNRAS.306..857C
Re:ABELL 1835
We present three different observations of the same central cluster
galaxy, one from A92, and two from our May observing run at slightly
different position angles.

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