Bibcode
van der Burg, R. F. J.; Aussel, H.; Pratt, G. W.; Arnaud, M.; Melin, J.-B.; Aghanim, N.; Barrena, R.; Dahle, H.; Douspis, M.; Ferragamo, A.; Fromenteau, S.; Herbonnet, R.; Hurier, G.; Pointecouteau, E.; Rubiño-Martín, J. A.; Streblyanska, A.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 587, id.A23, 16 pp.
Fecha de publicación:
3
2016
Revista
Número de citas
20
Número de citas referidas
17
Descripción
The Planck catalogue of SZ sources limits itself to a significance
threshold of 4.5 to ensure a low contamination rate by false cluster
candidates. This means that only the most massive clusters at redshift
z> 0.5, and in particular z> 0.7, are expected to enter into the
catalogue, with a large number of systems in that redshift regime being
expected around and just below that threshold. In this paper, we
follow-up a sample of SZ sources from the Planck SZ catalogues from 2013
and 2015. In the latter maps, we consider detections around and at lower
significance than the threshold adopted by the Planck Collaboration. To
keep the contamination rate low, our 28 candidates are chosen to have
significant WISE detections, in combination with non-detections in
SDSS/DSS, which effectively selects galaxy cluster candidates at
redshifts z ≳ 0.5. By taking r- and z-band imaging with MegaCam at
CFHT, we bridge the 4000 Å rest-frame break over a significant
redshift range, thus allowing accurate redshift estimates of
red-sequence cluster galaxies up to z ~ 0.8. After discussing the
possibility that an overdensity of galaxies coincides -by chance- with a
Planck SZ detection, we confirm that 16 of the candidates have likely
optical counterparts to their SZ signals, 13 (6) of which have an
estimated redshift z> 0.5 (z> 0.7). The richnesses of these
systems are generally lower than expected given the halo masses
estimated from the Planck maps. However, when we follow a simplistic
model to correct for Eddington bias in the SZ halo mass proxy, the
richnesses are consistent with a reference mass-richness relation
established for clusters detected at higher significance. This
illustrates the benefit of an optical follow-up, not only to obtain
redshift estimates, but also to provide an independent mass proxy that
is not based on the same data the clusters are detected with, and thus
not subject to Eddington bias.
Reduced images are available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/587/A23