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Notes for object ABELL 2390

8 note(s) found in NED.


1. 2008ApJ...687..899R
Re:ABELL 2390
A2390.-The U-band image shows a very blue, elongated region in the core,
extending southeast to northwest some 4"-5" in length.

2. 2007MNRAS.376.1073Z
Re:ABELL 2390
Abell 2390. These submm data are discussed in Barger et al. (1999) and Edge et
al. (1999), while Benson et al. (2003) provide a measurement of the SZ effect in
this cluster using SuZIE II.

3. 2007ApJ...655...30V
Re:ABELL 2390
Fritz et al. (2005) present the FP relation in Abell 2390 at z = 0.228. We
corrected the listed velocity dispersions to our fiducial aperture following
Jorgensen et al. (1995b), using 1.5" x 2.8" as the extraction aperture. The
listed rest-frame Gunn r surface brightnesses were converted back to observed
WFPC2 I_814_ magnitudes using <{mu}_814_>_e_ = <{mu},r,z>_e_ - 0.75 (see Fritz
et al. 2005). We converted
<{mu}>_e_ to {mu}_e_ and transformed to the (COSMIC camera) I band using
(Holtzman et al. 1995)
I = I_814_ - 0.037(B-I + 0.007 (B-I)^2^ +0.00.
The B - I colors were determined from the listed B and I aperture
magnitudes. These are not corrected for extinction; we applied corrections
of 0.476 mag to B and 0.214 mag to I (see Fritz et al. 2005). Rest-frame B
surface brightnesses were determined using
B_z_ = I + 0.47(B-I) +0.51.
Based on listed zero-point uncertainties, the uncertainty in the photometric
transformations is estimated at 0.03 mag.
In contrast to our own measurements of the FP in distant clusters, no
effort was made to determine parameters in the same way as the Jorgensen
et al. (1995b) studies at low redshift. There is therefore a systematic
uncertainty of ~5% in the velocity dispersions, which is caused by
possible differences in the fitting region, choice of templates, and
fitting methodology. This corresponds to an uncertainty of 0.031 in
log(M/L_B_). Combined with a 0.05 mag uncertainty due to the
transformations and the fact that the FP was determined in red rest-frame
bands, we estimate that the total systematic uncertainty is 0.037 in
log(M/L_B_).

4. 2005ApJ...624..606J
Re:ABELL 2390
A2390 (z = 0.23): This cluster has a large-scale extension to the east, as well
as a pointy or triangular extension to the northwest, giving it an odd
appearance. It also has some very small scale structure in the core. A2390 was
observed twice with Chandra, but we use only the observation at a focal plane
temperature of -120^deg^C.

5. 1999NewA....4..141G
Re:ABELL 2390
A 2390. The extended emission in this cluster is uncertain, because of
the presence of a discrete strong source (Owen et al., 1993).

6. 1999ApJ...517..587L
Re:ABELL 2390
Abell 2390, at z = 0.23, is one the best-studied clusters at higher
redshifts. It is extremely bright in X-rays, providing one of the
highest signal-to-noise ratio surface brightness profiles in our
sample. There are ROSAT HRI, ROSAT PSPC, and ASCA data available. There
are multiple arcs and arclets visible that have been used for
gravitational lensing studies. It has been estimated to have a large
(~250 h^-2^ M_sun_ yr^-1^) cooling flow (Pierre et al. 1996;
Rizza et al. 1997).
The HRI surface brightness profile is relatively smooth - apparently a
good candidate for a simple {beta} model fit. The emission is noticeably
elliptical. We see dramatic jumps in emission near the core in this
profile. This is probably the signature of the cooling flow, and we have
used only data outside of 39 h^-1^ kpc for our fit.
Our X-ray centroid lies at R.A. (1950) = 21^h^51^m^14.1^s^,
decl. (1950) = 17^deg^27'33.1", which is within 1" of the measurements
of Pierre et al. (1996) and A98.
Our fits to {beta} and r_core_ differ with the X-ray analyses of both
Rizza et al. (1997) and Pierre et al. (1996) by up to ~30% because of
details of the analyses, primarily methods of accounting for the effect
of the cooling flow. We note, however, that our mass estimates are in
good agreement with both works. We see a large discrepancy between our
X-ray analysis and that of A98, who find an r_core_ 4 times smaller than
ours. Combined with their mean temperature of 14.5 keV, compared with
the value of 8.9 keV from Mushotzky & Scharf (1997), and a large fitted
intrinsic N_H_ column, this yields a mass profile far in excess of our
own. We attribute the difference in r_core_ partly to our subjective
method of accounting for the peaked cooling flow on the profile but also
note that the A98 r_core_ value is much smaller than values for typical
clusters. The details of the A98 spatial analysis are in preparation
and may shed some light on our differences.
Gravitational lensing estimates for the mass based on weak lensing
(Squires et al. 1996, with the mass value calculated by WF97) and a
strong arc at z = 0.913 (discovered by Pello et al. 1991 and with the
mass calculation performed by Pierre et al. 1996) are higher than our
X-ray mass by a factor of 1.8 and 1.4, at radii of 602 and 92 h^-1^ kpc,
respectively. A98 also report a mass estimate based on the same strong
gravitational arc at a radius of 87 h^-1^ kpc, which is 2.3 times
greater than our X-ray-derived estimate.

7. 1998MNRAS.301..328R
Re:ABELL 2390
A2390: An ideal case for this study, A2390 has HRI, PSPC and ASCA data
available, as well as a very well studied galaxy population (Abraham
et al. 1996). There are also several gravitational arcs and arclets
present in the inner and outer regions of this X-ray-luminous cluster.
In agreement with Pierre et al. (1996), we detect the presence of a
central cooling flow in A2390. Our value of
L_X_ = 1.04 x 10^45^ h^-2^ erg s^-1^ is consistent with that of
Pierre et al., thus supporting the claim that the Einstein luminosity
of 3.85 x 10^44^ h^-2^ erg s^-1^ in the band 0.7-3.5 keV was erroneously
low. Both our analysis and that done by Pierre et al. show substructure
in the X-ray emission in the form of isophotal twisting in the core and
excess emission in the north-west. Pierre et al. estimate this component
to be ~1/15 M_cluster_. This is consistent with the conclusion, reached
by Abraham et al. from analysis of the velocity distribution, that A2390
is accreting an old group of galaxies. The axis of elongation for the
X-ray emission is aligned with that for the cluster galaxy members
(Squires et al. 1996; Pierre et al. 1996). The total mass of the cluster
derived from the lensing analysis is 19.5 +/- 6.5 x 10^14^ M_sun_ at a
radius of 1.15 Mpc (Squires et al. 1996), within 95 per cent agreement
with the CNOC model (Carlberg et al. 1996).

8. 1998A&A...330..801P
Re:ABELL 2390
A2390 The properties of this massive cooling flow - and lensing - cluster have
been studied in detail by Pierre et al. (1996). A slight rectification is
needed: the significance of residual possibly associated to galaxy # 314 is
between 2.3-3{sigma} (and not 3 {sigma} at least, as stated in the 1996
paper). The central elongated feature has also a size comparable to that of the
cD but their position angle are very different: the PA of the cD is -49 deg
(Pierre et al. 1996) and that of the core ~90 deg. On larger scales we found
PA(I_2_)=-56 deg which is comparable to that of the cD.


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