| Issue |
A&A
Volume 529, May 2011
|
|
|---|---|---|
| Article Number | A93 | |
| Number of page(s) | 10 | |
| Section | Cosmology (including clusters of galaxies) | |
| DOI | https://doi.org/10.1051/0004-6361/201015955 | |
| Published online | 08 April 2011 | |
A weak-lensing analysis of the Abell 383 cluster ⋆
1
INAF Osservatorio Astronomico di Capodimonte, via Moiariello
16,
80131
Napoli,
Italy
e-mail: zhuoyi.huang@oa-roma.inaf.it
2
INAF – Osservatorio Astronomico di Padova, vicolo
dell’Osservatorio 5, 35122
Padova,
Italy
e-mail: mario.radovich@oapd.inaf.it
3
INAF – Osservatorio Astronomico di Roma, Monte Porzio,
00185
Roma,
Italy
4
Key Lab for Astrophysics, Shanghai Normal University,
100 Guilin Road,
200234
Shanghai, PR
China
Received:
20
October
2010
Accepted:
9
February
2011
Aims. We use deep CFHT and SUBARU uBVRIz archival images of the Abell 383 cluster (z = 0.187) to estimate its mass by weak-lensing.
Methods. To this end, we first use simulated images to check the accuracy provided by our Kaiser-Squires-Broadhurst (KSB) pipeline. These simulations include shear testing programme (STEP) 1 and 2 simulations, as well as more realistic simulations of the distortion of galaxy shapes by a cluster with a Navarro-Frenk-White (NFW) profile. From these simulations we estimate the effect of noise on shear measurement and derive the correction terms. The R-band image is used to derive the mass by fitting the observed tangential shear profile with an NFW mass profile. Photometric redshifts are computed from the uBVRIz catalogs. Different methods for the foreground/background galaxy selection are implemented, namely selection by magnitude, color, and photometric redshifts, and the results are compared. In particular, we developed a semi-automatic algorithm to select the foreground galaxies in the color–color diagram, based on the observed colors.
Results. Using color selection or photometric redshifts improves the
correction of dilution from foreground galaxies: this leads to higher signals in the inner
parts of the cluster. We obtain a cluster mass 
M⊙:
this value is ~20% higher than previous estimates and is more consistent the
mass expected from X-ray data. The R-band luminosity function of the
cluster is computed and gives a total luminosity
Ltot = (2.14 ± 0.5) × 1012 L⊙
and a mass-to-luminosity ratio
M/L ~ 300 M⊙/L⊙.
Key words: galaxies: clusters: individual: Abell 383 / galaxies: fundamental parameters / dark matter
Based on: data collected with the Subaru Telescope (University of Tokyo) and obtained from the SMOKA, which is operated by the Astronomy Data Center, National Astronomical Observatory of Japan; observations obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada-France-Hawaii Telescope (CFHT), which is operated by the National Research Council (NRC) of Canada, the Institute National des Sciences de l’Univers of the Centre National de la Recherche Scientifique of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS.
© ESO, 2011
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