Planck 2013 results. XXXII. The updated Planck catalogue of Sunyaev-Zeldovich sources ⋆

A&A 581, A14 (2015)

DOI: 10.1051

0004-6361

201525787

ESO 2015

Astronomy

&

Astrophysics

Planck

2013 results. XXXII. The updated

Planck

catalogue

of Sunyaev-Zeldovich sources

?

Planck Collaboration: P. A. R. Ade

, N. Aghanim

, C. Armitage-Caplan

104

, M. Arnaud

, M. Ashdown

, F. Atrio-Barandela

J. Aumont

, H. Aussel

, C. Baccigalupi

, A. J. Banday

110

, R. B. Barreiro

, R. Barrena

, M. Bartelmann

108

, J. G. Bartlett

E. Battaner

113

, K. Benabed

107

, A. Benoît

, A. Benoit-Lévy

107

, J.-P. Bernard

110

, M. Bersanelli

, P. Bielewicz

110

, I. Bikmaev

J. Bobin

, J. J. Bock

, H. Böhringer

, A. Bonaldi

, J. R. Bond

, J. Borrill

101

, F. R. Bouchet

107

, M. Bridges

, M. Bucher

R. Burenin

100

, C. Burigana

, R. C. Butler

, J.-F. Cardoso

, P. Carvalho

, A. Catalano

, A. Challinor

, A. Chamballu

R.-R. Chary

, X. Chen

, H. C. Chiang

, L.-Y Chiang

, G. Chon

, P. R. Christensen

, E. Churazov

100

, S. Church

103

, D. L. Clements

S. Colombi

107

, L. P. L. Colombo

, B. Comis

, F. Couchot

, A. Coulais

, B. P. Crill

, A. Curto

, F. Cuttaia

, A. Da Silva

H. Dahle

, L. Danese

, R. D. Davies

, R. J. Davis

, P. de Bernardis

, A. de Rosa

, G. de Zotti

, J. Delabrouille

, J.-M. Delouis

107

J. Démoclès

, F.-X. Désert

, C. Dickinson

, J. M. Diego

, K. Dolag

112

, H. Dole

, S. Donzelli

, O. Doré

, M. Douspis

, X. Dupac

G. Efstathiou

, T. A. Enßlin

, H. K. Eriksen

, F. Feroz

, A. Ferragamo

, F. Finelli

, I. Flores-Cacho

110

, O. Forni

110

, M. Frailis

E. Franceschi

, S. Fromenteau

, S. Galeotta

, K. Ganga

, R. T. Génova-Santos

, M. Giard

110

, G. Giardino

, M. Gilfanov

100

Y. Giraud-Héraud

, J. González-Nuevo

, K. M. Górski

114

, K. J. B. Grainge

, S. Gratton

, A. Gregorio

, N, E. Groeneboom

A. Gruppuso

, F. K. Hansen

, D. Hanson

, D. Harrison

, A. Hempel

, S. Henrot-Versillé

, C. Hernández-Monteagudo

D. Herranz

, S. R. Hildebrandt

, E. Hivon

107

, M. Hobson

, W. A. Holmes

, A. Hornstrup

, W. Hovest

, K. M. Hu

enberger

G. Hurier

, N. Hurley-Walker

, A. H. Ja

, T. R. Ja

110

, W. C. Jones

, M. Juvela

, E. Keihänen

, R. Keskitalo

, I. Khamitov

105

T. S. Kisner

, R. Kneissl

, J. Knoche

, L. Knox

, M. Kunz

, H. Kurki-Suonio

, G. Lagache

, A. Lähteenmäki

, J.-M. Lamarre

A. Lasenby

, R. J. Laureijs

, C. R. Lawrence

, J. P. Leahy

, R. Leonardi

, J. León-Tavares

, J. Lesgourgues

106

, C. Li

, A. Liddle

M. Liguori

, P. B. Lilje

, M. Linden-Vørnle

, M. López-Caniego

, P. M. Lubin

, J. F. Macías-Pérez

, C. J. MacTavish

, B. Ma

D. Maino

, N. Mandolesi

, M. Maris

, D. J. Marshall

, P. G. Martin

, E. Martínez-González

, S. Masi

, M. Massardi

S. Matarrese

, F. Matthai

, P. Mazzotta

, S. Mei

109

, P. R. Meinhold

, A. Melchiorri

, J.-B. Melin

, L. Mendes

, A. Mennella

M. Migliaccio

, K. Mikkelsen

, S. Mitra

, M.-A. Miville-Deschênes

, A. Moneti

, L. Montier

110

, G. Morgante

, D. Mortlock

D. Munshi

, J. A. Murphy

, P. Naselsky

, A. Nastasi

, F. Nati

, P. Natoli

, N. P. H. Nesvadba

, C. B. Netterfield

H. U. Nørgaard-Nielsen

, F. Noviello

, D. Novikov

, I. Novikov

, I. J. O’Dwyer

, M. Olamaie

, S. Osborne

103

, C. A. Oxborrow

, F. Paci

L. Pagano

, F. Pajot

, D. Paoletti

, F. Pasian

, G. Patanchon

, T. J. Pearson

, O. Perdereau

, L. Perotto

, Y. C. Perrott

, F. Perrotta

F. Piacentini

, M. Piat

, E. Pierpaoli

, D. Pietrobon

, S. Plaszczynski

, E. Pointecouteau

110

, G. Polenta

, N. Ponthieu

, L. Popa

T. Poutanen

, G. W. Pratt

, G. Prézeau

, S. Prunet

107

, J.-L. Puget

, J. P. Rachen

, W. T. Reach

111

, R. Rebolo

, M. Reinecke

M. Remazeilles

, C. Renault

, S. Ricciardi

, T. Riller

, I. Ristorcelli

110

, G. Rocha

, C. Rosset

, G. Roudier

M. Rowan-Robinson

, J. A. Rubiño-Martín

, C. Rumsey

, B. Rusholme

, M. Sandri

, D. Santos

, R. D. E. Saunders

, G. Savini

M. P. Schammel

, D. Scott

, M. D. Sei

ert

, E. P. S. Shellard

, T. W. Shimwell

, L. D. Spencer

, J.-L. Starck

, V. Stolyarov

102

R. Stompor

, A. Streblyanska

, R. Sudiwala

, R. Sunyaev

100

, F. Sureau

, D. Sutton

, A.-S. Suur-Uski

, J.-F. Sygnet

, J. A. Tauber

D. Tavagnacco

, L. Terenzi

, L. To

olatti

, M. Tomasi

, D. Tramonte

, M. Tristram

, M. Tucci

, J. Tuovinen

, M. Türler

G. Umana

, L. Valenziano

, J. Valiviita

, B. Van Tent

, L. Vibert

, P. Vielva

, F. Villa

, N. Vittorio

, L. A. Wade

B. D. Wandelt

107

, M. White

, S. D. M. White

, D. Yvon

, A. Zacchei

, and A. Zonca

ffi

liations can be found after the references)

Received 2 February 2015

Accepted 18 February 2015

ABSTRACT

We update the all-sky

Planck

catalogue of 1227 clusters and cluster candidates (PSZ1) published in March 2013, derived from detections of the

Sunyaev–Zeldovich (SZ) e

ect using the first 15.5 months of

Planck

satellite observations. As an addendum, we deliver an updated version of

the PSZ1 catalogue, reporting the further confirmation of 86

Planck

-discovered clusters. In total, the PSZ1 now contains 947 confirmed clusters,

of which 214 were confirmed as newly discovered clusters through follow-up observations undertaken by the Planck Collaboration. The updated

PSZ1 contains redshifts for 913 systems, of which 736 (

∼

6%) are spectroscopic, and associated mass estimates derived from the

mass proxy.

We also provide a new SZ quality flag for the remaining 280 candidates. This flag was derived from a novel artificial neural-network classification

of the SZ signal. Based on this assessment, the purity of the updated PSZ1 catalogue is estimated to be 94%. In this release, we provide the full

updated catalogue and an additional readme file with further information on the

Planck

SZ detections.

Key words.

errata, addenda – large-scale structure of Universe – galaxies: clusters: general – catalogs

The catalogue is only available at the CDS via anonymous ftp to

cdsarc.u-strasbg.fr

(

130.79.128.5

) or via

http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/581/A14

Corresponding author: N. Aghanim

e-mail:

nabila.aghanim@ias.u-psud.fr

1. Introduction

Cluster samples selected by their Sunyaev–Zeldovich (SZ) sig-

nal have only recently reached significant sizes, for instance, the

Article published by EDP Sciences

A14, page 1 of 8

A&A 581, A14 (2015)

Early SZ (ESZ) catalogue from the

Planck

Satellite

(Planck

Collaboration VIII 2011; Planck Collaboration XXIX 2014),

and catalogues from the South Pole Telescope (SPT; Reichardt

et al. 2013; Bleem et al. 2015) and the Atacama Cosmology

Telescope (ACT; Marriage et al. 2011; Hasselfield et al. 2013).

These are now considered as new reference samples for cluster

studies and associated cosmological analyses.

The present note describes updates to the construction and

properties of the

Planck

catalogue of SZ sources PSZ1 (here-

after PXXIX2013, Planck Collaboration XXIX 2014), released

in March 2013 as part of the first

Planck

data delivery. The PSZ1

catalogue contains 1227 entries, including 683 so-called previ-

ously known clusters. This category corresponds to the associa-

tion of

Planck

SZ source detections with known clusters from the

literature. The association is set to the first identifier as defined

in the hierarchy adopted by PXXIX2013, namely: (i) identifica-

tion with MCXC clusters (Pi

aretti et al. 2011); (ii) identifica-

tion with Abell and Zwicky objects; (iii) identification with clus-

ters derived from SDSS-based catalogues (primarily from Wen

et al. 2012); (iv) identification with clusters from SZ catalogues

(Hasselfield et al. 2013; Reichardt et al. 2013); (v) searches in

the NED and SIMBAD databases. Considerable added value,

including consolidated redshift values, has been obtained by

compiling ancillary information. These redshifts include spec-

troscopic, photometric, and estimated values. Spectroscopic red-

shifts were preferentially reported, even when they were ob-

tained from the measurement of a single galaxy. Photometric and

estimated redshifts refer to values obtained from photo-

codes

or red sequence estimates, respectively. Masses were computed

for all clusters with redshift values.

Since its delivery in March 2013, we have continued to up-

date the PSZ1 catalogue by focusing on the confirmation of

newly discovered clusters in PSZ1. This process has first in-

volved updating the redshifts of some previously known clus-

ters (Sect. 2). We also made use of recent results from dedicated

follow-up observations conducted by the Planck Collaboration

with the RTT150 (Planck Collaboration Int. XXVI 2015) and

ENO telescopes (Planck Collaboration, in prep.), which together

allowed us to observe and measure estimated, photometric, and

spectroscopic redshifts for

∼

150 PSZ1 sources (Sect. 3.1). In

addition, we used published results from PanSTARRS (Liu et al.

2015) and from the latest SPT catalogue (Bleem et al. 2015), as

described in Sects. 3.3 and 3.4. For all clusters with redshifts, we

computed the estimated masses using the

mass proxy (Arnaud

et al., in prep. and PXXIX2013; Sect. 4). Finally, we revisited the

cluster-candidate classification scheme, which in PXXIX2013

was organised into three classes (

class-

1, 2, 3) in order of de-

creasing reliability. As described in Sect. 5, we now used the

SZ spectral energy distribution (SED) to refine the quality as-

sessment of the cluster candidates by adopting a new quality flag

derived from the artificial neural-network analysis developed by

Aghanim et al. (2015). In Appendix A, we describe the updated

PSZ1 catalogue including the new fields, specifying the redshift

type and associated reference.

Planck

(

http://www.esa.int/Planck

) is a project of the

European Space Agency (ESA) with instruments provided by two sci-

entific consortia funded by ESA member states (in particular the lead

countries France and Italy), with contributions from NASA (USA) and

telescope reflectors provided by a collaboration between ESA and a sci-

entific consortium led and funded by Denmark.

2. Redshift updates for previously known clusters

In the external validation process performed in PXXIX2013, a

total of 683 PSZ1 sources were associated with clusters pub-

lished in X-ray, optical, or SZ catalogues or with clusters found

in the NED or SIMBAD databases. We refer to these as pre-

viously known clusters. Their redshifts, when available, were

compiled from the literature and a consolidated value, prefer-

encially spectroscopic, was provided with the PSZ1 catalogue.

In the present update, we first re-examine the previously known

clusters of the PSZ1 catalogue.

The dedicated follow-up of

Planck

PSZ1 clusters with

RTT150 described in Planck Collaboration Int. XXVI (2015)

provided updates to the redshifts of 19 previously known clus-

ters. The follow-up of

Planck

PSZ1 clusters with ENO tele-

scopes additionally updated the redshifts of five previously

known clusters.

We updated the redshifts of ten PSZ1 sources associated with

SPT clusters provided in Bleem et al. (2015). Finally, we queried

the NED and SIMBAD databases and searched in the cluster cat-

alogues constructed from the SDSS data (Wen et al. 2012 and

Rozo et al. 2014) for additional spectroscopic redshifts. When

these were available, we report them in the updated version of

the PSZ1 catalogue. The full process led us to change the red-

shifts of 34 previously known PSZ1 clusters. We also changed

the published photometric redshift of one ACT cluster (ACT-CL

J0559-5249) to a spectroscopic redshift value.

In summary, 69 sources from the PSZ1 catalogue associ-

ated with previously known clusters now have updated redshifts.

Most of these consist of updates from photometric to spectro-

scopic values; however, eight redshifts were measured for the

first time for previously known clusters.

Planck

-discovered clusters

The PSZ1 catalogue contained 366 cluster candidates, classified

class-

1 to 3 in order of decreasing reliability, and 178

Planck

discovered clusters confirmed mostly with dedicated follow-up

programmes undertaken by the Planck Collaboration. Since the

delivery of the PSZ1 catalogue in March 2013, a number of ad-

ditional confirmations, including results from the community,

were performed and redshifts were updated from photometric

to spectroscopic values.

Combining the results from follow-up with the RTT150

(Planck Collaboration Int. XXVI 2015), ENO telescopes (Planck

Collaboration, in prep.), Liu et al. (2015), Rozo et al. (2014), and

Bleem et al. (2015), a total of 86 PSZ1 sources have been newly

confirmed as

Planck-

discovered clusters with measured photo-

metric or spectroscopic redshifts.

3.1. From RTT150 results

As part of the Planck Collaboration optical follow-up pro-

gramme, candidates were observed with the Russian Turkish

Telescope (RTT150

, Planck Collaboration Int. XXVI 2015)

within the Russian quota of observational time, provided by

the Kazan Federal University and Space Research Institute

(IKI, Moscow). Direct images and spectroscopic redshift mea-

surements were obtained using the TÜB

ITAK Faint Object

Spectrograph and Camera (TFOSC

). For the clusters with

http://hea.iki.rssi.ru/rtt150/en/index.php

http://hea.iki.rssi.ru/rtt150/en/

index.php?page=tfosc

A14, page 2 of 8

Planck Collaboration: Updated

Planck

catalogue of Sunyaev–Zeldovich sources

the highest redshift, complementary spectroscopic observations

were performed with the BTA 6 m telescope of the SAO RAS

using the SCORPIO focal reducer and spectrometer (Afanasiev

& Moiseev 2005).

These observations have confirmed and provided redshifts

for a total of 24 new candidates. Eleven of these have spectro-

scopic redshifts. We have updated the PSZ1 catalogue by includ-

ing these newly obtained redshifts.

3.2. From ENO telescopes

As part of the Planck Collaboration optical follow-up pro-

gramme, candidates were also observed at European Northern

Observatory (ENO

) telescopes, both in imaging (at IAC80,

INT, and WHT) and spectroscopy (at NOT, GTC, INT, and

TNG). The observations were obtained as part of proposals for

the Spanish CAT time and of an International Time Programme

(ITP), accepted by the International Scientific Committee of the

Roque de los Muchachos and Teide observatories. We sum-

marise here the main results of these observing programmes.

More details will be presented in a companion article (Planck

Collaboration, in prep.).

These observations have confirmed and provided new red-

shifts for a total of 26 candidates, which are reported in the up-

dated PSZ1 catalogue. These include the confirmation of 12 SZ

sources as newly discovered clusters: two

class

1 high-reliability

candidates, five

class

2, and five

class

3 candidates.

3.3. From PanSTARRS

Based on data from the Panoramic Survey Telescope and Rapid

Response System (PanSTARRS, Kaiser et al. 2002), Liu et al.

(2015) have searched for optical confirmation of the 237

Planck

SZ detections that overlap the PanSTARRS footprint.

We only report here the photometric redshifts for unambigu-

ously confirmed clusters. Of these, 15 objects were included in

the RTT150 follow-up, for which the redshifts are published in

Planck Collaboration Int. XXVI (2015), and three objects were

included in the ESO follow-up described above. In these cases,

we report the Planck Collaboration follow-up redshift values in

the updated PSZ1 catalogue. An additional two

Planck

clusters

confirmed by PanSTARRS have a counterpart in the Rozo et al.

(2014) catalogue, with spectroscopic redshifts that we update in

the PSZ1 catalogue.

A total of 40 Planck-discovered clusters are confirmed, for

the first time, by Liu et al. (2015) in the PanSTARRS survey. All

of these have photometric redshifts that we have reported in the

updated PSZ1 catalogue.

3.4. From SPT

A new catalogue of SZ clusters detected with the South Pole

Telescope (SPT) cluster catalogue was published in Bleem et al.

(2015). It provides an ensemble of spectroscopic and photomet-

ric redshifts. Four candidate

class

1 and 2 clusters from the

PSZ1 catalogue were confirmed and have photometric redshifts

in Bleem et al. (2015). These are included in the updated PSZ1

catalogue.

ENO:

http://www.iac.es/eno.php?lang=en

3.5. From SDSS-RedMapper catalogue

Comparison with the SDSS-based catalogue from Rozo et al.

(2014) provided confirmation and new redshift values for five

Planck-discovered clusters. This includes confirmation of two

Planck

cluster-candidates (one

class

2 and one

class

3 candi-

date). We use the spectroscopic redshift values available in the

Rozo et al. (2014) in the updated PSZ1 catalogue.

4. Mass estimate

The size-flux degeneracy discussed for example in Planck

Collaboration VIII (2011) and PXXIX2013 can be broken

when

is known, using the

500

–

500

relation between

500

and

500

see (Arnaud et al., in prep.). The

500

parameter, de-

noted

, is derived from the intersection of the

500

–

500

relation and the size-flux degeneracy curve. The SZ mass proxy

is equivalent to the X-ray mass proxy

For all the

Planck

clusters with redshifts,

was computed

assuming a flat universe with

Ω

3 and

Ω

7, allowing us to derive an homogeneously defined SZ mass

proxy, denoted

500

, based on X-ray calibration of the scaling

relations (see discussion in PXXIX2013)

. We show in Fig. 2 the

distribution of masses obtained from the SZ-based mass proxy

for all clusters with redshifts. Note that since we used an X-ray

calibration of the scaling relations, these masses are uncorrected

for any bias due to the assumption of hydrostatic equilibrium

in the X-ray mass analysis. The shaded black area shows the

distribution of masses for clusters with redshifts higher than 0.5.

They represent a total of 78 clusters.

5. Cluster candidates

Since the delivery of the

Planck

catalogue and with the confir-

mation in this addendum of 86 candidates as new clusters, the

updated PSZ1 catalogue now contains 280 cluster candidates. In

the original PSZ1, these latter were classified as

class

1 to 3 in

order of decreasing reliability; the reliability being defined em-

pirically from the combination of internal

Planck

quality assess-

ment and ancillary information (e.g., searches in RASS, WISE,

SDSS data). The updated PSZ1 catalogue contains 24 high-

quality (

class

1) SZ detections, whereas lower reliability

class

and 3 candidates represent 130 and 126 SZ sources, respectively.

With the updated PSZ1 catalogue, we now provide a new ob-

jective quality assessment of the SZ sources derived from an ar-

tificial neural-network analysis. The construction, training, and

validation of the network is based on the analysis of the SED

of the SZ signal in the

Planck

channels. The implementation is

discussed in detail by Aghanim et al. (2015). The neural net-

work was trained with an ensemble of three samples: the con-

firmed clusters in the PSZ1 calatogue with a good or high-quality

SZ signal; the

Planck

Catalogue of Compact Sources catalogue,

which represents detections in the IR and those induced by radio

source; and random positions on the sky as examples of noise-

induced, very low-reliability detections.

In practice, we provide for each SZ source of the updated

PSZ1 catalogue a neural-network quality flag,

, defined as

in Aghanim et al. (2015). This flag separates the high-quality

SZ detections from the low-quality sources such that

For a few clusters with redshifts that show pathological 2D posteri-

ors, it was not possible to estimate realistic masses.

A14, page 3 of 8

A&A 581, A14 (2015)

0.0

0.2

0.4

0.6

0.8

1.0

1.2

1.4

Redshift

500

[10

sol

]

PSZ1

SPT 2500deg

ACT

MaDCoWs

ROSAT

Fig. 1.

Distribution in the

–

plane of the

Planck

SZ cluster catalogue (open red circles; Planck Collaboration XXIX 2014) compared with those

from SPT (black; Reichardt et al. 2013; Bleem et al. 2015) and ACT (green; Marriage et al. 2011; Hasselfield et al. 2013), MaDCoWS (yellow;

Brodwin et al. 2015), and NORAS and REFLEX from the MCXC meta-catalogue (blue; Pi

aretti et al. 2011 and references therein). Some clusters

may appear several times as distinct points as a result of di

erences in the mass estimate between surveys. The black dotted lines show the

Planck

mass limit for the medium-deep survey zone at 20% completeness (as defined in Planck Collaboration XXIX 2014) for a redshift limit of

0.0

0.2

0.4

0.6

0.8

1.0

1.2

1.4

Redshift

100

150

200

PSZ1 all masses

PSZ1 masses > 5.10

•

Mass [10

•

]

100

150

200

PSZ1 all redshifts

PSZ1 z > 0.5

Fig. 2.

Distribution of redshifts (

left panel

) and masses (

right panel

) for the

Planck

SZ clusters. The black shaded area represents the population

of clusters with redshift higher than 0.5 (

right panel

) and mass higher than 5

(

left panel

identifies low-reliability SZ sources with a high degree of suc-

cess. Figure 4 summarises the number of sources for each class

Planck

cluster-candidates that are below and above the thresh-

old value of

4. The

class

1 cluster-candidates all have

except for one source, for which

39. The

fraction of good

4 SZ detections in the

class

2 category

is about 80%, while the fraction of

4 candidates drops to

about 30% for the

class

3 cluster-candidates.

6. Summary

We have updated the

Planck

catalogue of SZ-selected sources

detected in the first 15.5 months of observations. The catalogue

contains 1227 detections and was validated using external X-ray

and optical

NIR data, alongside a multi-frequency follow-up

programme for confirmation.

The updated PSZ1 catalogue now contains 947 confirmed

clusters, including 264 brand-new clusters, of which 214 have

A14, page 4 of 8

Planck Collaboration: Updated

Planck

catalogue of Sunyaev–Zeldovich sources

Table 1.

Summary of the updates of PSZ1v2 for each cluster or candidate type.

PSZ1 (2013)

PSZ1v2 (2015)

Number

Redshift

Updates

Number

Redshift

Type

Number

Type Number

“Previously known”

683

undef

−

undef

estim

−

estim

phot

−

phot

spec

552

spec

607

“Planck

−

discovered”

178

264

undef

−

undef

phot

122

spec

129

Class1

−

undef

−

undef

phot

−

phot

−

spec

−

spec

−

Class2

170

−

130

undef

170

−

undef

130

phot

−

phot

−

spec

−

spec

−

Class3

142

−

126

undef

142

−

undef

126

phot

−

phot

−

spec

−

spec

−

been confirmed by the Planck Collaboration follow-up pro-

gramme. The remaining 280 cluster candidates have been di-

vided into three classes according to their reliability, that is, ac-

cording to the quality of evidence that they are probably bona

fide clusters. To date, high-quality SZ detections in PSZ1 repre-

sent 24 sources, all of which are classified as high-quality clus-

ters by our neural-network quality-assessment procedure. Lower

reliability

class

2 and 3 candidates represent 130 and 126 SZ

sources, respectively (Table 1). We find that

∼

80% of the

class

candidates are classified as high-quality clusters by our neural-

network quality-assessment procedure, whereas only 35% of the

class

3 sources are considered high-quality SZ detections. Based

on this assessment, the purity of the updated PSZ1 catalogue

∼

94%.

A total of 913

Planck

clusters (i.e., 74.2% of all SZ detec-

tions) now have redshifts, of which 736 are spectroscopic val-

ues (i.e., 80.6% of all redshifts). The left-hand panel of Fig. 2

shows the redshift distribution of all clusters (red) and the dis-

tribution for the clusters with masses higher than 5

(shaded black). The median redshift of the PSZ1 catalogue is

about 0.23, and about 35% of the

Planck

clusters lie at redshifts

higher than

The origins and types of redshifts are shown in Fig. 3 (this

information is available in the updated catalogue). Association

with MCXC clusters (Pi

aretti et al. 2011) provides about 49

of the redshifts, all of which are spectroscopic. Follow-up obser-

vations undertaken by the Planck Collaboration provide 24

of the redshifts, about two thirds of which are spectroscopic.

SDSS-based catalogues yield 11

7% of the redshifts, more than

half of which are spectroscopic. NED and SIMBAD database

searches yield 5.9% of the redshifts, the vast majority of which

are spectroscopic. PanSTARRS data provide 4

4% of the red-

shifts, all of which are photometric. Finally, association with the

% of PSZ1 redshifts coming from

MCXC

FUs

SDSS

P-Starrs

MCXC

FUs

SDSS

P-Starrs

MCXC

FUs

SDSS

P-Starrs

Spectroscopic redshifts

Photometric redshifts

Estimated redshifts

Fig. 3.

Percentage of origin and type (photometric, spectroscopic) of

the redshifts reported in PSZ1. To date, associations with MCXC clus-

ters provide 49.8% of the redshifts, all spectroscopic. Follow-up ob-

servations by the Planck collaboration (FUs) provide 24.6% of the

redshifts, of which 64.73% are spectroscopic. Associations with clus-

ters from SDSS-based catalogues result in 11.7% of all redshifts, of

which 58.9% are spectroscopic. Redshifts from the NED and SIMBAD

databases represent 5.9% of all redshifts, 90.7% of which are spectro-

scopic. PanSTARRS data confirm 4.4% of the total redshift number,

all of them photometric. Finally, the association with SZ catalogues

(SPT and ACT) represents 3.5% of all redshifts, of which 71.9% are

spectroscopic.

SPT and ACT SZ catalogues represents

∼

5% of all redshifts,

most of which are spectroscopic.

For the

Planck

clusters with redshifts, we have provided

a homogeneously defined mass estimated from the Compton

-parameter. The

–

distribution of the

Planck

clusters is

A14, page 5 of 8

A&A 581, A14 (2015)

Number of candidates below/above Q

= 0.4

100

120

140

Class-3

Class-2

Class-1

Class-3

Class-2

Class-1

< 0.4

> 0.4

Fig. 4.

Number of

Planck

cluster-candidates below and above the

neural-network quality-flag threshold

4, denoting a high-quality

SZ detection, for each reliability class.

shown by open red circles in Fig. 1, where it is compared with

other large cluster surveys. Note that the masses are not ho-

mogenised and some clusters may appear several times as a re-

sult of di

erences in the mass estimation methods between sur-

veys. The

Planck

cluster distribution probes a unique region in

the

–

space occupied by massive,

≥

, high-

redshift (

≥

5) clusters. The

Planck

detections almost double

the number of massive clusters with redshift higher than 0.5 with

respect to other surveys.

Acknowledgements.

The development of

Planck

has been supported by: ESA;

CNES and CNRS

INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy);

NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and

RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA

(Canada); DTU Space (Denmark); SER

SSO (Switzerland); RCN (Norway); SFI

(Ireland); FCT

MCTES (Portugal); and PRACE (EU). The authors thank N.

Schartel, ESA

XMM-Newton

project scientist, for granting the DDT used for

confirmation of SZ

Planck

candidates. The authors thank TUBITAK, IKI, KFU

and AST for support in using RTT150; in particular we thank KFU and IKI

for providing significant amounts of their observing time at RTT150. We also

acknowledge the BTA 6 m telescope TAC for support of the optical follow-up

project. The authors acknowledge the use of the INT and WHT telescopes oper-

ated on the island of La Palma by the Isaac Newton Group of Telescopes at the

Spanish Observatorio del Roque de los Muchachos of the IAC; the NOT, oper-

ated on La Palma jointly by Denmark, Finland, Iceland, Norway, and Sweden,

at the Spanish Observatorio del Roque de los Muchachos; the TNG, operated

on La Palma by the Fundacion Galileo Galilei of the INAF at the Spanish

Observatorio del Roque de los Muchachos; the GTC telescope, operated on La

Palma by the IAC at the Spanish Observatorio del Roque de los Muchachos; and

the IAC80 telescope operated on the island of Tenerife by the IAC at the Spanish

Observatorio del Teide. Part of this research has been carried out with telescope

time awarded by the CCI International Time Programme. The authors thank the

TAC of the MPG

ESO-2.2m telescope for support of optical follow-up with WFI

under

Max Planck

time. Observations were also conducted with ESO NTT at

the La Silla Paranal Observatory. This research has made use of SDSS-III data.

Funding for SDSS-III (

http://www.sdss3.org/

) has been provided by the

Alfred P. Sloan Foundation, the Participating Institutions, the National Science

Foundation, and DoE. SDSS-III is managed by the Astrophysical Research

Consortium for the Participating Institutions of the SDSS-III Collaboration. This

research has made use of the following databases: the NED and IRSA databases,

operated by the Jet Propulsion Laboratory, California Institute of Technology,

under contract with the NASA; SIMBAD, operated at CDS, Strasbourg,

France; SZ cluster database (

http://szcluster-db.ias.u-psud.fr

) and

SZ repository operated by IDOC operated by IAS under contract with CNES

and CNRS.

Appendix A: Description of the updated PSZ1

catalogue

The updated

Planck

catalogue of SZ sources is available at PLA

and the SZ cluster database

The updated PSZ1 gathers in a single table all the entries of

the delivered catalogue mainly based on the

Planck

data and the

entries of the external validation information based on ancillary

data (Appendices B and C of Planck Collaboration XXIX 2014,

respectively). It also contains additional entries. It is provided in

a fits format, together with a readme file.

The updated catalogue contains, when available, cluster ex-

ternal identifications

and consolidated redshifts. We added two

new entries: the redshift type and the bibliographic reference.

The three entries associated with the consolidated redshift re-

ported in the catalogue are thus:

–

Type of redshift: a string providing the di

erent cases.

undef

: undefined

estim

: estimated from red sequence

phot

: photometric redshift

spec

: spectroscopic redshifts

–

Source of redshift: an integer value representing the origin

of the redshifts.

–1: No redshift available

1: MCXC updated compilation

2: Databases NED and SIMBAD-CDS

3: SDSS cluster catalogue from Wen et al. (2012)

4: SDSS cluster catalogue from Szabo et al. (2011)

5: SPT

6: ACT

7: Search in SDSS galaxy catalogue from Planck Collab.,

from Fromenteau 2010 and Fromenteau et al. (priv.

comm.)

8: SDSS catalogue from Rozo et al. (2014)

10: Pan-STARRS1 Survey confirmation

20:

XMM-Newton

confirmation from Planck Collab.

50: ENO confirmation from Planck Collab.

60: WFI-imaging confirmation from Planck Collab.

65: NTT-spectroscopic confirmation from Planck Collab.

500: RTT confirmation from Planck Collab.

600: NOT confirmation from Planck Collab.

650: GEMINI-spectroscopic confirmation from Planck

Collab.

–

Bibliographical references for the redshift.

We also added a new entry describing the quality of the SZ de-

tection in more detail. This is the flag

derived from the arti-

ficial neural-network SED-based quality assesssment described

in Aghanim et al. (2015).

References

Afanasiev, V. L., & Moiseev, A. V. 2005, Astron. Lett., 31, 194

Aghanim, N., Hurier, G., Diego, J.-M., et al. 2015, A&A, 580, A138

Bleem, L. E., Stalder, B., de Haan, T., et al. 2015, ApJS, 216, 27

Brodwin, M., Greer, C. H., Leitch, E. M., et al. 2015, ApJ, 806, 26

http://www.sciops.esa.int/index.php?page=

Planck_Legacy_Archive&project=planck

http://szcluster-db.ias.u-psud.fr

The external identification corresponds to the first identifier as

defined in the external validation hierarchy adopted in Planck

Collaboration XXIX (2014).

A14, page 6 of 8

Planck Collaboration: Updated

Planck

catalogue of Sunyaev–Zeldovich sources

Hasselfield, M., Hilton, M., Marriage, T. A., et al. 2013, J. Cosmol. Astropart.

Phys., 7, 8

Kaiser, N., Aussel, H., Burke, B. E., et al. 2002, in Survey and Other Telescope

Technologies and Discoveries, eds. J. A. Tyson, & S. Wol

, SPIE Conf. Ser.,

4836, 154

Liu, J., Hennig, C., Desai, S., et al. 2015, MNRAS, 449, 3370

Marriage, T. A., Acquaviva, V., Ade, P. A. R., et al. 2011, ApJ, 737, 61

aretti, R., Arnaud, M., Pratt, G. W., Pointecouteau, E., & Melin, J.-B. 2011,

A&A, 534, A109

Planck Collaboration VIII. 2011, A&A, 536, A8

Planck Collaboration XXIX. 2014, A&A, 571, A29

Planck Collaboration Int. XXVI. 2015, A&A, in press,

DOI: 10.1051

0004-6361

201424674

Reichardt, C. L., Stalder, B., Bleem, L. E., et al. 2013, ApJ, 763, 127

Rozo, E., Ryko

, E. S., Becker, M., Reddick, R. M., & Wechsler, R. H. 2014,

ArXiv e-prints [

arXiv:1410.1193

]

Szabo, T., Pierpaoli, E., Dong, F., Pipino, A., & Gunn, J. 2011, ApJ, 736, 21

Wen, Z. L., Han, J. L., & Liu, F. S. 2012, ApJS, 199, 34

APC, AstroParticule et Cosmologie, Université Paris Diderot,

CNRS

IN2P3, CEA

lrfu, Observatoire de Paris, Sorbonne Paris

Cité, 10 rue Alice Domon et Léonie Duquet, 75205 Paris Cedex

13, France

Aalto University Metsähovi Radio Observatory, Metsähovintie 114,

02540 Kylmälä, Finland

Academy of Sciences of Tatarstan, Bauman Str., 20, Kazan, 420111,

Republic of Tatarstan, Russia

African Institute for Mathematical Sciences, 6-8 Melrose Road,

Muizenberg, Cape Town, South Africa

Agenzia Spaziale Italiana Science Data Center, via del Politecnico

snc, 00133 Roma, Italy

Agenzia Spaziale Italiana, Viale Liegi 26, Roma, Italy

Astrophysics

Group,

Cavendish

Laboratory,

University

Cambridge, J J Thomson Avenue, Cambridge CB3 0HE, UK

Astrophysics & Cosmology Research Unit, School of Mathematics,

Statistics & Computer Science, University of KwaZulu-Natal,

Westville Campus, Private Bag X54001, 4000 Durban, South Africa

Atacama Large Millimeter

submillimeter Array, ALMA Santiago

Central O

ffi

ces, Alonso de Cordova 3107, Vitacura, Casilla 763

0355 Santiago, Chile

CITA, University of Toronto, 60 St. George St., Toronto, ON M5S

3H8, Canada

CNRS, IRAP, 9 Av. colonel Roche, BP 44346, 31028 Toulouse

Cedex 4, France

California Institute of Technology, Pasadena, California, USA

Centre for Theoretical Cosmology, DAMTP, University of

Cambridge, Wilberforce Road, Cambridge CB3 0WA, UK

Centro de Astrofísica, Universidade do Porto, Rua das Estrelas,

4150-762 Porto, Portugal

Centro de Estudios de Física del Cosmos de Aragón (CEFCA),

Plaza San Juan, 1, planta 2, 44001, Teruel, Spain

Computational Cosmology Center, Lawrence Berkeley National

Laboratory, Berkeley, California 92093-0424, USA

Consejo Superior de Investigaciones Científicas (CSIC), 28040

Madrid, Spain

DSM

Irfu

SPP, CEA-Saclay, 91191 Gif-sur-Yvette Cedex, France

DTU Space, National Space Institute, Technical University of

Denmark, Elektrovej 327, 2800 Kgs. Lyngby, Denmark

Département de Physique Théorique, Université de Genève, 24 Quai

E. Ansermet, 1211 Genève 4, Switzerland

Departamento de Física Fundamental, Facultad de Ciencias,

Universidad de Salamanca, 37008 Salamanca, Spain

Departamento de Física, Universidad de Oviedo, Avda. Calvo Sotelo

n, 33007 Oviedo, Spain

Department of Astronomy and Astrophysics, University of Toronto,

50 Saint George Street, Toronto, Ontario M5S 3H4, Canada

Department of Astronomy and Geodesy, Kazan Federal University,

Kremlevskaya Str., 18, 420008, Kazan, Russia

Department

Astrophysics

IMAPP,

Radboud

University

Nijmegen, PO Box 9010, 6500 GL Nijmegen, The Netherlands

Department of Electrical Engineering and Computer Sciences,

University of California, Berkeley, California, CA 94720-1770,

USA

Department of Physics & Astronomy, University of British

Columbia, 6224 Agricultural Road, Vancouver, British Columbia

Y6T 121, Canada

Department of Physics and Astronomy, Dana and David Dornsife

College of Letter, Arts and Sciences, University of Southern

California, Los Angeles, CA 90089, USA

Department of Physics and Astronomy, University College London,

London WC1E 6BT, UK

Department of Physics and Astronomy, University of Sussex,

Brighton BN1 9QH, UK

Department of Physics, Florida State University, Keen Physics

Building, 77 Chieftan Way, Tallahassee, Florida, FL 32306-4350,

USA

Department of Physics, Gustaf Hällströmin katu 2a, University of

Helsinki, 00014 Helsinki, Finland

Department of Physics, Princeton University, Princeton, New Jersey,

NJ 08544-0708, USA

Department of Physics, University of California, Berkeley,

California CA 94720-3840, USA

Department of Physics, University of California, One Shields

Avenue, Davis, California CA 95616, USA

Department of Physics, University of California, Santa Barbara,

California, CA 93106-9530, USA

Department of Physics, University of Illinois at Urbana-Champaign,

1110 West Green Street, Urbana, Illinois, IL 61701-3080 USA

Dipartimento di Fisica e Astronomia G. Galilei, Università degli

Studi di Padova, via Marzolo 8, 35131 Padova, Italy

Dipartimento di Fisica e Scienze della Terra, Università di Ferrara,

via Saragat 1, 44122 Ferrara, Italy

Dipartimento di Fisica, Università La Sapienza, P.le A. Moro 2,

00185 Roma, Italy

Dipartimento di Fisica, Università degli Studi di Milano, via Celoria,

16, 20133 Milano, Italy

Dipartimento di Fisica, Università degli Studi di Trieste, via A.

Valerio 2, 34127 Trieste, Italy

Dipartimento di Fisica, Università di Roma Tor Vergata, via della

Ricerca Scientifica, 1, 00133 Roma, Italy

Discovery Center, Niels Bohr Institute, Blegdamsvej 17, 2100

Copenhagen, Denmark

Dpto. Astrofísica, Universidad de La Laguna (ULL), 38206 La

Laguna, Tenerife, Spain

European Southern Observatory, ESO Vitacura, Alonso de Cordova

3107, Vitacura, Casilla 19001, Santiago, Chile

European Space Agency, ESAC, Planck Science O

ffi

ce, Camino

bajo del Castillo s

n, Urbanización Villafranca del Castillo,

Villanueva de la Cañada, 28692 Madrid, Spain

European Space Agency, ESTEC, Keplerlaan 1, 2201 AZ

Noordwijk, The Netherlands

Finnish Centre for Astronomy with ESO (FINCA), University of

Turku, Väisäläntie 20, 21500, Piikkiö, Finland

GEPI, Observatoire de Paris, Section de Meudon, 5 place J. Janssen,

92195 Meudon Cedex, France

Helsinki Institute of Physics, Gustaf Hällströmin katu 2, University

of Helsinki, 00014 Helsinki, Finland

INAF – Osservatorio Astrofisico di Catania, via S. Sofia 78, 95123

Catania, Italy

INAF

–

Osservatorio

Astronomico

Padova,

Vicolo

dell’Osservatorio 5, 35122 Padova, Italy

INAF – Osservatorio Astronomico di Roma, via di Frascati 33,

00040 Monte Porzio Catone, Italy

INAF – Osservatorio Astronomico di Trieste, via G.B. Tiepolo 11,

34143 Trieste, Italy

INAF Istituto di Radioastronomia, via P. Gobetti 101, 40129

Bologna, Italy

INAF

IASF Bologna, via Gobetti 101, 40129 Bologna, Italy

INAF

IASF Milano, via E. Bassini 15, 20133 Milano, Italy

INFN, Sezione di Bologna, via Irnerio 46, 40126, Bologna, Italy

A14, page 7 of 8

A&A 581, A14 (2015)

INFN, Sezione di Roma 1, Università di Roma Sapienza, Piazzale

Aldo Moro 2, 00185, Roma, Italy

IPAG: Institut de Planétologie et d’Astrophysique de Grenoble,

Université Joseph Fourier, Grenoble 1

CNRS-INSU, UMR 5274,

38041 Grenoble, France

ISDC Data Centre for Astrophysics, University of Geneva, ch.

d’Ecogia 16, 1290 Versoix, Switzerland

IUCAA, Post Bag 4, Ganeshkhind, Pune University Campus,

411 007 Pune, India

Imperial College London, Astrophysics group, Blackett Laboratory,

Prince Consort Road, London, SW7 2AZ, UK

Infrared Processing and Analysis Center, California Institute of

Technology, Pasadena, CA 91125, USA

Institut Néel, CNRS, Université Joseph Fourier Grenoble I, 25 rue

des Martyrs, 38042 Grenoble, France

Institut Universitaire de France, 103 Bd Saint-Michel, 75005 Paris,

France

Institut d’Astrophysique Spatiale, CNRS (UMR8617) Université

Paris-Sud 11, Bâtiment 121, 91405 Orsay, France

Institut d’Astrophysique de Paris, CNRS (UMR7095), 98bis boule-

vard Arago, 75014 Paris, France

Institute for Space Sciences, 077125 Bucharest-Magurale, Romania

Institute of Astronomy and Astrophysics, Academia Sinica, Taipei,

Taiwan, ROC

Institute of Astronomy, University of Cambridge, Madingley Road,

Cambridge CB3 0HA, UK

Institute of Theoretical Astrophysics, University of Oslo, Blindern,

0371 Oslo, Norway

Instituto de Astrofísica de Canarias, C

vía Láctea s

n, 38200 La

Laguna, Tenerife, Spain

Instituto de Física de Cantabria (CSIC-Universidad de Cantabria),

Avda. de los Castros s

n, 39005 Santander, Spain

Jet Propulsion Laboratory, California Institute of Technology, 4800

Oak Grove Drive, Pasadena CA 91109, California, USA

Jodrell Bank Centre for Astrophysics, Alan Turing Building, School

of Physics and Astronomy, The University of Manchester, Oxford

Road, Manchester, M13 9PL, UK

Kavli Institute for Cosmology Cambridge, Madingley Road,

Cambridge, CB3 0HA, UK

LAL, Université Paris-Sud, CNRS

IN2P3, 91898 Orsay, France

LERMA,

CNRS,

Observatoire

Paris,

avenue

l’Observatoire, 75014 Paris, France

Laboratoire AIM, IRFU

Service d’Astrophysique – CEA

DSM –

CNRS – Université Paris Diderot, Bât. 709, CEA-Saclay, 91191

Gif-sur-Yvette Cedex, France

Laboratoire Traitement et Communication de l’Information, CNRS

(UMR 5141) and Télécom ParisTech, 46 rue Barrault, 75634 Paris

Cedex 13, France

Laboratoire de Physique Subatomique et de Cosmologie, Université

Joseph Fourier Grenoble I, CNRS

IN2P3, Institut National

Polytechnique de Grenoble, 53 rue des Martyrs, 38026 Grenoble

Cedex, France

Laboratoire de Physique Théorique, Université Paris-Sud 11 &

CNRS, Bâtiment 210, 91405 Orsay, France

Lawrence Berkeley National Laboratory, Berkeley, California CA

94720, USA

MPA Partner Group, Key Laboratory for Research in Galaxies

and Cosmology, Shanghai Astronomical Observatory, Chinese

Academy of Sciences, Nandan Road 80, 200030 Shanghai, PR

China

Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str. 1,

85741 Garching, Germany

Max-Planck-Institut

für

Extraterrestrische

Physik,

Giessenbachstraße, 85748 Garching, Germany

McGill Physics, Ernest Rutherford Physics Building, McGill

University, 3600 rue University, Montréal, QC, H3A 2T8, Canada

MilliLab, VTT Technical Research Centre of Finland, Tietotie 3,

02 044 VTT Espoo, Finland

Moscow Institute of Physics and Technology, Dolgoprudny,

Institutsky per., 9, 141700 Dolgoprudry, Russia

National University of Ireland, Department of Experimental

Physics, Maynooth, Co. Kildare, Ireland

Niels Bohr Institute, Blegdamsvej 17, 2100 Copenhagen, Denmark

Observational Cosmology, Mail Stop 367-17, California Institute of

Technology, Pasadena, CA 91125, USA

Optical Science Laboratory, University College London, Gower

Street, London, WC1E 6BT, UK

SB-ITP-LPPC, EPFL, 1015 Lausanne, Switzerland

SISSA, Astrophysics Sector, via Bonomea 265, 34136, Trieste, Italy

SUPA, Institute for Astronomy, University of Edinburgh, Royal

Observatory, Blackford Hill, Edinburgh EH9 3HJ, UK

School of Physics and Astronomy, Cardi

University, Queens

Buildings, The Parade, Cardi

, CF24 3AA, UK

100

Space Research Institute (IKI), Russian Academy of Sciences,

Profsoyuznaya Str, 84

32, 117997 Moscow, Russia

101

Space Sciences Laboratory, University of California, Berkeley,

California CA 94720, USA

102

Special Astrophysical Observatory, Russian Academy of Sciences,

Nizhnij

Arkhyz,

Zelenchukskiy

region,

369167

Karachai-

Cherkessian Republic, Russia

103

Stanford University, Dept of Physics, Varian Physics Bldg, 382 via

Pueblo Mall, Stanford, California CA 94305-4060, USA

104

Sub-Department of Astrophysics, University of Oxford, Keble

Road, Oxford OX1 3RH, UK

105

TÜB

ITAK National Observatory, Akdeniz University Campus,

07058 Antalya, Turkey

106

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107

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Paris, France

108

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Philosophenweg 12, 69120 Heidelberg, Germany

109

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110

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France

111

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for Infrared Astronomy, MS 232-11, Mo

ett Field, CA 94035, USA

112

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Scheinerstrasse 1, 81679 Munich, Germany

113

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Cosmos, Facultad de Ciencias, 18071 Granada, Spain

114

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Warszawa, Poland

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