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Date and Time of the Query: 2019-06-15 T20:03:12 PDT
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Notes for object ABELL 0478

7 note(s) found in NED.


1. 2008ApJ...687..899R
Re:ABELL 0478
A478.-Cardiel et al. (1998) found spectral evidence for significant star
formation in the CDG.

2. 2007MNRAS.376.1073Z
Re:ABELL 0478
Abell 478. This cluster has been a popular target for SZ effect experiments;
Radford et al. (1986) and Chase et al. (1987) discuss early attempts to measure
the SZ effect at 3 and 1.2 mm, respectively. More recently, Myers et al. (1997)
and Mason, Myers & Readhead (2001) discuss measurements of the SZ effect using
OVRO at 32 GHz, Udomprasert et al. (2004) measures this cluster's SZ effect with
CBI, and Lancaster et al. (2005) uses the VSA at 34 GHz as well.
Unfortunately, this cluster is a poor target for SZ effects at SCUBA's
shorter wavelengths. Knudsen, van der Werf & Jaffe (2003) have presented the
data discussed here and associate the bright point source near the centre of
this field with a high redshift, dusty quasar. Previously, Cox, Bregman &
Schombert (1995) discuss IRAS measurements of this cluster at 60 and 100 {mu}m.
Pointecouteau et al. (2004) and de Plaa et al. (2004) discuss the X-ray
properties of this cluster using recent XMM-Newton data, and Sun et al. (2003)
presents similar measurements with Chandra.

3. 2006MNRAS.372.1496S
Re:ABELL 0478
5.16 Abell 478 - This well-known CC cluster hosts a cold front (Markevitch,
Vikhlinin & Forman 2003) and possesses prominent X-ray cavities with coincident
radio lobes (Sun et al. 2003).

4. 2004MNRAS.352.1413S
Re:Abell 0478
Abell 478: MMR measured a Hubble constant H 0= 61^+33^_-21_ km s^-1^
Mpc^-1^ assuming an isothermal kT= 8.4 keV model with the {beta}-model
parameters {theta}_c_ = 1 arcmin, {beta}= 0.64 and n_e0_= 0.023 cm^-3^
from ROSAT. This temperature also accounts for the presence of a cooling
flow in the cluster core. Sun et al. (2003) improved upon the result by
MMR by determining the Comptonization parameter as a function of radius
from a deprojection of the Chandra data, and by extrapolating the
Chandra data with a {beta}-model based on a fit to the combined surface
brightness profile from Chandra and ROSAT. They used {beta}= 0.68 and
obtained a Hubble constant estimate H 0= 64+32 -18 km s^-1^ Mpc^-1^,
which lies between our value and the one obtained by MMR.

5. 2004MNRAS.352.1413S
Re:Abell 0478
3.2.3 Abell 478 Abell 478 was observed by Myers et al. (1997) at 32 GHz
and reanalysed by Mason et al. (2001, MMR). The observed decrement was
published as an average y-parameter, y= 7.52 +- 0.56x10^-5^, within the
telescope beam. Note that we use their value without the relativistic
correction, as we apply this correction to the X-ray model. We compare
the observed SZ decrement with the Chandra prediction using the
beam-switching technique described by Myers et al. (1997).

6. 1998A&A...330..801P
Re:ABELL 0478
A478 This image has been previously studied by White et al. (1994). Our analysis
shows a very elongated (not resolved) core, with possible 2 maxima; its PA is
significantly twisted with respect to the large scale cluster orientation which
is comparable to that of the cD (~35 deg. APM). The elongated central structure
is confined within the extent of the cD envelope.

7. 1996ApJS..105..191G
Re:ABELL 0478
A478.--The early-type galaxies in this cluster are much redder than expected,
both in g-r and in r-i. As noted by Bahcall & Sargent (1977), this cluster
is heavily reddened [they estimate a E(B-V) = 0.7 +/- 0.2]. The colors of the
early-type galaxies in this cluster would become as expected from the Virgo C-M
relation if the hydrogen column density is more than a factor of 3 higher than
the value interpolated from the catalog of Stark et al., i.e., if E(B-V) ~0.4.
This is the only case in which the value for E(B-V) found in the Burstein &
Heiles (1982) survey is significantly different from the Stark et al. (1992)
one: 0.24 against 0.1. Even the highest value falls a factor of 2 short of what
would be needed to bring A478 colors to "normal." However, the different values
in the two catalogs could indicate that the absorption in the direction of A478
is extremely patchy (the closest measurement reported by Stark et al. is
0.44^deg^ away from the position of the brightest galaxy in A478).


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