High angular resolution Sunyaev-Zel'dovich observations of MACS J1423.8+2404 with NIKA

16 Pages·2016·3.48 MB·English

A&A586,A122(2016) Astronomy
DOI:10.1051/0004-6361/201527616 &
(cid:13)c ESO2016 Astrophysics
High angular resolution Sunyaev-Zel’dovich observations
of MACS J1423.8+2404 with NIKA: Multiwavelength analysis
R.Adam1,2,B.Comis1,I.Bartalucci3,A.Adane4,P.Ade5,P.André3,M.Arnaud3,A.Beelen6,B.Belier7,A.Benoît8,
A.Bideaud5,N.Billot9,O.Bourrion1,M.Calvo8,A.Catalano1,G.Coiffard4,A.D’Addabbo8,10,F.-X.Désert11,
S.Doyle5,J.Goupy8,B.Hasnoun6,I.Hermelo9,C.Kramer9,G.Lagache12,S.Leclercq4,J.-F.Macías-Pérez1,
J.Martino6,P.Mauskopf5,13,F.Mayet1,A.Monfardini8,F.Pajot6,E.Pascale5,L.Perotto1,E.Pointecouteau14,15,
N.Ponthieu11,G.W.Pratt3,V.Revéret3,A.Ritacco1,L.Rodriguez3,G.Savini16,K.Schuster4,A.Sievers9,
S.Triqueneaux8,C.Tucker5,andR.Zylka4
1 Laboratoire de Physique Subatomique et de Cosmologie, Université Grenoble-Alpes, CNRS/IN2P3, 53 rue des Martyrs,
38000Grenoble,France
e-mail:[email protected]
2 LaboratoireLagrange,UniversitéCôted’Azur,ObservatoiredelaCôted’Azur,CNRS,Blvddel’Observatoire,CS34229,
06304NiceCedex4,France
3 LaboratoireAIM,CEA/IRFU,CNRS/INSU,UniversitéParisDiderot,CEA-Saclay,91191Gif-Sur-Yvette,France
4 InstitutdeRadioAstronomieMillimétrique(IRAM),38400Saint-Martind’HèresGrenoble,France
5 AstronomyInstrumentationGroup,UniversityofCardiff,CardiffCF103XQ,UK
6 Institutd’AstrophysiqueSpatiale(IAS),CNRSandUniversitéParisSud,91440Bures-sur-Yvettes,France
7 Institutd’ÉlectroniqueFondamentale(IEF),UniversitéParis-Sud,91400Orsay,France
8 InstitutNéel,CNRSandUniversitédeGrenoble,France
9 InstitutdeRadioAstronomieMillimétrique(IRAM),18012Granada,Spain
10 DipartimentodiFisica,SapienzaUniversitàdiRoma,PiazzaleAldoMoro5,00185Roma,Italy
11 InstitutdePlanétologieetd’AstrophysiquedeGrenoble(IPAG),CNRSandUniversitédeGrenoble,France
12 Aix-MarseilleUniversité,CNRS,LAM(Laboratoired’AstrophysiquedeMarseille)UMR7326,13388Marseille,France
13 SchoolofEarthandSpaceExplorationandDepartmentofPhysics,ArizonaStateUniversity,Tempe,AZ85287,USA
14 UniversitédeToulouse,UPS-OMP,InstitutdeRechercheenAstrophysiqueetPlanétologie(IRAP),31062Toulouse,France
15 CNRS,IRAP,9Av.colonelRoche,BP44346,31028ToulouseCedex4,France
16 UniversityCollegeLondon,DepartmentofPhysicsandAstronomy,GowerStreet,LondonWC1E6BT,UK
Received22October2015/Accepted16December2015
ABSTRACT
TheprototypeoftheNIKA2camera,NIKA,isadual-bandinstrumentoperatingattheIRAM30-mtelescope,whichcanobserve
theskysimultaneouslyat150and260GHz.OneofthemaingoalsofNIKA(andNIKA2)istomeasurethepressuredistributionin
galaxyclustersathighangularresolutionusingthethermalSunyaev-Zel’dovich(tSZ)effect.Suchobservationshavealreadyproved
tobeanexcellentprobeofclusterpressuredistributionsevenatintermediateandhighredshifts.However,animportantfractionof
clusters host sub-millimeter and/or radio point sources, which can significantly affect the reconstructed signal. Here we report on
<20arcsecangularresolutionobservationsat150and260GHzoftheclusterMACSJ1423.8+2404,whichhostsbothradioandsub-
millimeterpointsources.WeexaminethemorphologicaldistributionofthetSZsignalandcompareittootherdatasets.TheNIKA
data are combined with Herschel satellite data to study the spectral energy distribution (SED) of the sub-millimeter point source
contaminants.Wethenperformajointreconstructionoftheintraclustermedium(ICM)electronicpressureanddensitybycombining
NIKA,Planck,XMM-Newton,andChandradata,focusingontheimpactoftheradioandsub-millimetersourcesonthereconstructed
pressureprofile.Wefindthatlarge-scalepressuredistributionisunaffectedbythepointsourcesbecauseoftheresolvednatureof
theNIKAobservations.Thereconstructedpressureintheinnerregionisslightlyhigherwhenthecontributionofpointsourcesare
removed.Weshowthatitisnotpossibletosetstrongconstraintsonthecentralpressuredistributionwithoutaccuratelyremovingthese
contaminants.ThecomparisonwithX-rayonlydatashowsgoodagreementforthepressure,temperature,andentropyprofiles,which
allindicatethatMACSJ1423.8+2404isadynamicallyrelaxedcoolcoresystem.Thepresentobservationsillustratethepossibilityof
measuringthesequantitieswitharelativelysmallintegrationtime,evenathighredshiftandwithoutX-rayspectroscopy.Thiswork
ispartofapilotstudyaimingatoptimizingtSZobservationswiththefutureNIKA2camera.
Keywords.techniques:highangularresolution–galaxies:clusters:individual:MACSJ1423.8+2404–
galaxies:clusters:intraclustermedium
1. Introduction to both the matter content of the Universe and its dynamics
because they form throughout its expansion history. Their for-
Inthestandardscenarioofstructureformation,clustersofgalax- mation process is well understood and clusters have been used
iesformthroughthehierarchicalmergingofsmallergroupsand to place constraints on cosmological parameters (e.g., Planck
accretion of surrounding material. These clusters are sensitive Collaboration XXIX 2014). However, the complex baryonic
ArticlepublishedbyEDPSciences A122,page1of16
A&A586,A122(2016)
physics occurring during cluster formation, such as feedback observestheskyat150and260GHzwithanangularresolution
from active galactic nuclei (AGN), or nonthermal processes of 18 and 12 arcsec full width at half maximum (FWHM), and
occurring during mergers or in the presence of intracluster hasalreadybeenusedtoimagethetSZeffecttowardthegalaxy
medium (ICM) turbulence or coherent motion, is still unclear clusters RXJ1347.5-1145 and CLJ1226.9+3332 (see Adam
(seeforexampleBorgani&Kravtsov2011).Thisleadstoscat- et al. 2014, 2015). In the present paper we discuss observa-
terandbiasesintheobservable–massscalingrelationsneededto tions of the intermediate redshift cluster MACSJ1423.8+2404
compare to theory, limiting the use of clusters as cosmological at z = 0.545, which contains both radio and sub-millimeter
probes. galaxiesandwhichwehaveusedasatestcasetoinvestigatethe
The thermal Sunyaev-Zel’dovich effect (tSZ; Sunyaev & impact of such contaminating objects on the reconstruction of
Zel’dovich 1972, 1980) is produced by the inverse Compton thepressureofclustersobservedwithNIKA2.
interaction of cosmic microwave background (CMB) photons
with the energetic electrons in the ICM. This tSZ effect leads
MACSJ1423.8+2404 is a massive cluster from the
toaspectraldistortionoftheCMBobservableatmillimeterand
MACS catalog (Massive Cluster Survey; Ebeling et al. 2001),
sub-millimeter wavelengths that is directly proportional to the
forwhichawealthofmultiwavelengthdatahavebeenobtained.
line-of-sight integral of the electronic pressure distribution in
Schmidt & Allen (2007), in a study of relaxed clusters with
the ICM. The integrated tSZ flux is related to the overall ther- Chandra, reported a virial mass M = 4.52+0.79 × 1014 M ,
malenergyoftheclusterandisthereforeexpectedtoprovidea vir −0.64 (cid:12)
indicatingthatitindeedisamassiveobject.Theclusterwasob-
lowscattermassproxywithasmalldependenceonthedynam-
served by the BIMA interferometer (LaRoque et al. 2003) and
ical state of the cluster or the exact gas physics (e.g., da Silva
by the Sunyaev-Zel’dovich Array (SZA), as part of a sample
etal.2004;Motletal.2005;Nagai2006).Furthermore,resolved
used to constrain the cluster pressure profile (Bonamente et al.
tSZobservationsareverysensitivetotheoverpressurecausedby
mergersandhaveprovedtobeveryefficientforprobingcluster 2012). The large-scale structure of MACSJ1423.8+2404 was
investigated, using its red sequence galaxy density distribution
astrophysics (see, for example, results by Pointecouteau et al.
(Kartaltepe et al. 2008), showing a very relaxed morphology.
1999; Komatsu et al. 2001; Korngut et al. 2011; Adam et al.
Guennou et al. (2014) studied the structure of the cluster using
2014,2015;Youngetal.2015;Mroczkowskietal.2015).This
ChandraX-raydataaspartofthedarkenergyAmericanFrench
is particularly true at high redshifts since, unlike other probes,
the tSZ signal does not suffer from cosmological dimming and team survey. They observed a strong X-ray emission, slightly
elongated, and only low significance substructures were found.
is only limited by the sensitivity and angular resolution of the
observations. Detailed reviews of the tSZ effect can be found Themorphologyoftheclusterwasalsostudiedfromadetailed
gravitationallensing/opticalanalysisbyLimousinetal.(2010),
in Birkinshaw (1999), Carlstrom et al. (2002), and Kitayama
whonoticedthatMACSJ1423.8+2404isnearlyfullyvirialized,
(2014).
elongated,andshowsverylittlesubstructure(seealsothestrong
During the past few years, tremendous achievements have
lensing results by Zitrin et al. 2011, as part of a sample of 12
been made in the tSZ community with the production of
MACS clusters). The temperature profile obtained by Morandi
catalogues of more than 1000 objects by Planck (Planck
etal.(2010)usingChandradatashowsatypicalcoolcoreform
CollaborationXXIX2014),theAtacamaCosmologyTelescope
withalowcentraltemperature(∼3keV)andapeakat∼7keVat
(ACT; Hasselfield et al. 2013), and the South Pole Telescope
about300kpcawayformthecenter.Thebrightestclustergalaxy
(SPT; Reichardt et al. 2013; Bleem et al. 2015), at >1 arcmin
(BCG) hosts a central AGN that is visible as a point source in
angular resolution. X-ray observations have shown that, when
radio observations (Condon et al. 1998; LaRoque et al. 2003;
scaled to a characteristic radius, the cluster pressure profile
Cobleetal.2007;Bonamenteetal.2012).ThisAGNisrespon-
shows a low dispersion (Arnaud et al. 2010). This profile has
sible for the presence of two cavities detected in the Chandra
now been well measured at intermediate scales in the nearby
X-ray image (Hlavacek-Larrondo et al. 2012). Another radio
Universe with tSZ observations (Plagge et al. 2010; Planck
source is located at about 1.5 arcmin southwest with respect to
Collaboration V 2013c; Sayers et al. 2013a), but has not been
the X-ray peak. Cluster members, foreground, and background
deeplyexploredathighredshiftandintheclustercoresbecause
(including lensed sources) sub-millimeter galaxies are detected
ofthelackofhighangularresolutionobservations.Theinvesti-
by Herschel, as observed during the Herschel Lensing Survey
gationofthisprofileisnonethelessnecessarytomakebetteruse
(HLS;Egamietal.2010;Rawleetal.2012).
oftheavailabletSZclustersampleswhenrelatingthetSZsignal
toclustermass.
In the context of high angular resolution tSZ observations, This paper is organized as follows. The observations per-
oneofthemainchallengestofaceistheremovalofthecontam- formed at the IRAM 30-m telescope are briefly presented in
ination from point sources, as needed for example in the case Sect. 2. In Sect. 3, we discuss the processing of radio and sub-
of Bolocam observations (Sayers et al. 2013b). Indeed, galaxy millimeterpointsourcesandtheirimpactontheradialtSZflux
clusterscontaingalaxiesthatcanhostradiosourcesorasignifi- density profile. The data reduction of the XMM-Newton and
cantamountofdust.Inaddition,clustersatintermediateredshift Chandra X-ray observations is presented in Sect. 4. We com-
provideoptimallenses,whichcanmagnifysub-millimeterback- pare the NIKA observations to other multiwavelength datasets
groundgalaxies(see,e.g.,Adametal.2015).Foregroundgalax- in Sect. 5. In Sect. 6, we reconstruct the radial pressure dis-
iescanalsobelocatedinprojectionneartheclusterunderstudy. tribution of MACSJ1423.8+2404 and explore the impact of
IntSZobservations,theseobjectsappearaspoint-likecontami- the presence of the point sources. The pressure profile is com-
natingsources.TheNewIRAMKidsArray(NIKA)isthepro- bined with the electronic density of X-ray data to derive the
totypeofNIKA2,thenextgenerationcontinuuminstrumentfor thermodynamic distribution of the ICM. Conclusions and per-
the Institut de Radio Astronomie Millimétrique (IRAM) 30-m spectives for NIKA2 are provided in Sect. 7. Throughout this
telescopenearGranada,Spain(seeMonfardinietal.2010,2011; paper we assume a flat ΛCDM cosmology, according to the
Bourrion et al. 2011, 2012; Calvo et al. 2013; Catalano et al. latest Planck results (Planck Collaboration XIII 2015), with
2014,formoredetailsontheNIKAcamera).TheNIKAcamera H0 =67.8kms−1Mpc−1,ΩM =0.308,andΩΛ =0.692.
A122,page2of16
R.Adametal.:ResolvedtSZobservationsofMACSJ1423.8+2404
2. ObservationsattheIRAM30-mtelescope to unity at scales that are smaller than the field of view. The
withNIKA transferfunctionvanishessmoothlyatlargerangularscales(see
Adametal.2015).
2.1. ThethermalSunyaev-Zel’dovicheffect
The tSZ effect (Sunyaev & Zel’dovich 1972, 1980) results in a 2.3. RawNIKAobservations
distortion of the CMB blackbody spectrum relative to the pri-
maryCMBintensity,I ,(e.g.,Birkinshaw1999) The NIKA maps that we obtained are presented in Fig. 1.
0
The 150 GHz map reveals a negative decrement, as expected
∆ItSZ =y f(ν,T ). (1) from the tSZ effect at this frequency, with a maximum signif-
I e icance of 4.5σ. The morphology of the signal has a ring-like
0
shape,asaconsequenceofthecontaminationbytheradiopoint
The function f(ν,T ) gives the characteristic frequency depen-
e source at the cluster center, which fills in the tSZ signal. The
denceofthespectrum.Thesmalldependanceontheelectronic
260GHzmapdoesnotshowanysignificanttSZsignal.Atthis
temperature,T ,arisesfromrelativisticcorrectionsforwhichwe
e frequency, extrapolating from the 150 GHz map, we expect a
usetheresultsofItohetal.(1998).TheComptonparameter,y,
peak of ∼1 mJy/beam, which is below the level of the noise
givestheamplitudeofthedistortionandisrelatedtotheline-of-
standarddeviation.Weobservea3σpositivepeakaround(RA,
sightintegraloftheelectronicpressure,P ,as
e Dec)=(14:23:53,+24:03:45),whichcorrespondstoa2σpos-
(cid:90)
σ itive peak in the 150 GHz map owing to the presence of a
y= T P dl. (2)
m c2 e sub-millimeter source. Another peak is also seen around (RA,
e Dec) = (+14:23:48, +24:04:15). The radio and sub-millimeter
TheparameterσT istheThomsoncrosssection,me istheelec- pointsourcecontaminationisdiscussedindetailinSect.3.
tron rest mass, and c the speed of light. The total integrated The significance of the NIKA maps was calculated using
tSZ flux, Ytot, is then given by the aperture photometry per- MonteCarlorealizations.First,anoisemapwasobtainedfrom
formedontheComptonparametermap. the half difference of two equivalent subsets. After having nor-
In the NIKA bands, the tSZ signal is expected to be faint malized the noise map by the integration time per pixel, the
(y∼10−4fortypicalmassiveclusters)anddiffuse.Itisnegative noise spectral distribution was computed with the POKER soft-
at150GHzandpositiveat260GHz. ware (Ponthieu et al. 2011), which properly accounts for in-
complete sky coverage due to the scanning around the cluster.
The noise power spectrum was modeled as a function of angu-
2.2. Observingconditions,scanningstrategy,calibration,
anddatareduction lar scale k, as P (k) = A +A (k )(cid:16)k(cid:17)β. The parameter
noise white cor 0 k0
MACSJ1423.8+2404wasobservedduringthefirstNIKAopen Awhite representstheintrinsicdetectornoiseand Acor andβgive
theamplitudeandtheslopeoftheresidualdetector-detectorat-
pool in February 2014. We collected 1.47 h of on-target data.
mosphericcorrelationsinthemap.Thismodelwasusedtogen-
The atmospheric conditions were stable and the mean opacity
erateMonte-Carlonoisemaprealizations,n,accountingforthe
wasmeasuredtobe0.14and0.15,atthesourcelocation,at150 i
integrationtimeperpixel.Thenoiserealizationsweresmoothed
and260GHz,respectively,asdetailedinCatalanoetal.(2014).
bythesame10arcsecGaussianfilterusedtodisplaythecluster,
Themeanelevationofthesourcewas30.8deg.
and the standard deviation across the Monte-Carlo realizations
The scanning strategy adopted was the same as that used
for CLJ1226.9+3332, detailed in Adam et al. (2015). Briefly, allowedustocomputetherootmeansquaremapand,therefore,
the signal-to-noise contours shown in Fig. 1. The noise stan-
eachscanconsisted19subscansof6arcminlengthseparatedby
dard deviation on the flux of point sources at the center of the
10 arcsec steps made alternately at constant azimuth and con-
mapis0.8and2.9mJyat150and260GHz,accountingforre-
stantelevation(relativetothemapcenter).Thepointingcenter
waschosentobeat(RA,Dec2000)=(14:23:47.8,+24:04:40.0) duction filtering effects. The mean noise standard deviation of
the displayed maps within a radius of 60 arcsec, after apply-
basedontheArchiveofChandraClusterEntropyProfileTables
ing the Gaussian smoothing, is 0.39 and 1.3 mJy/beam at 150
catalog(ACCEPT;Cavagnoloetal.2009).
and260GHz,respectively.Thefullnoisecovariancematrixwas
The detailed calibration procedure can be found in Adam
also computed as the mean of the noise covariance over all the
et al. (2015) and we only summarize the main results here. realizations,C = 1 (cid:80)NMCnnT,anditisusedintheanalysisas
Uranuswasusedastheprimarycalibrator.TheGaussianbeam NMC i=1 i i
FWHM was measured to be 18.2 and 12.0 arcsec at 150 and describedinSect.6.
260 GHz, respectively. The nearby quasar 1354+195 was used
to correct the pointing, for which the error is estimated to be
2.4. Astrophysicalcontaminants
less than 3 arcsec. The overall calibration uncertainty was es-
timated to be 7% at 150 GHz and 12% at 260 GHz. The Inadditiontotheinstrumentnoiseandatmosphericnoiseresid-
NIKAbandpasseswereusedtoconvertthefluxsurfacebright- uals, diffuse astrophysical emission may give rise to an extra
ness to Compton parameter. We obtained −10.9 ± 0.8 and sourceofnoisethatcannotbereducedbyincreasingtheobserv-
3.5 ± 0.5 Jy/beam per unit of Compton parameter at 150 and ingtime.Inthefollowing,weconsiderthecontaminationfrom
260 GHz, respectively. The effective number of detectors was CMB and cosmic infrared background (CIB) anisotropies, and
117 at 150 GHz and 136 at 260 GHz, corresponding to an in- Galacticemissions(dust,synchrotron,andfree-free).
stantaneousfieldofviewof1.9and1.8arcmin,respectively. The Galactic latitude of MACSJ1423.8+2404 is high
The removal of the atmospheric and electronic correlated (68.99◦), implying low contamination of the cluster field by
noise,consistingofthesubtractionofthecorrelatedsignalinthe Galacticemissions(PlanckCollaborationetal.2015b).Toesti-
timelinesacrossthedetectorarrays,wasperformedasinAdam matethiscontamination,weusetheHEALPixsoftware(Górski
et al. (2015). The resulting signal filtering was estimated using etal.2005)toextract60arcmin×60arcminpatches,centered
simulations. The observed transfer function was flat and close on the cluster coordinates, of the nine Planck channel maps
A122,page3of16
A&A586,A122(2016)
Fig.1.NIKAmapsat150GHz(left)and260GHz(right)inunitsofsurfacebrightness.Thesignificanceisgivenbytheblackcontoursstarting
at±2σwith1σspacing.Themapsaresmoothedwithanextra10arcsecGaussianfilterfordisplaypurposesandtheeffectivebeamFWHMis
representedasawhitecircleinthebottomleftcornerofeachpanel.ThewhitecrossesindicatetheX-raycenter.
at 30, 44, 70, 100, 143, 217, 353, 547, and 857 GHz (Planck about 5 with respect to the clustering component. Taking the
Collaborationetal.2015a),towhichwesubtracttheCMBmap NIKA transfer function and beams into account, we obtain a
(Planck Collaboration et al. 2015c). We find that CMB emis- standarddeviationofthefluctuationsof0.13and0.38mJy/beam
sion dominates over the low frequency Galactic components, at 150 and 260 GHz in the NIKA bands. This extra source of
i.e.,synchrotronandfree-free,atallfrequencies.TheCMBalso noise is therefore subdominant with respect to the instrument
dominatesoverthethermaldustemission,athigherfrequencies, noise and atmospheric noise residual at both frequencies, con-
up to 353 GHz, where the amplitude of the fluctuations of the tributingtoabout1%ofthenoisewhensummedquadratically;
twoaresimilar.Intheconsideredfield,theCMBthereforedom- wedonotaccountforthecontributionofthisextranoisesource
inatesoverthediffuseGalacticemissionsintheNIKAbandsat inthepresentpaper.
the Planck angular resolution. This is be even more true at the
smaller scales probed by NIKA as Galactic diffuse emissions
havepowerspectrathatarestronglydecreasingwiththespatial
scale(powerlawwithanindexofabout−2.5). 3. Radioandsub-millimeterpointsources
To estimate the level of contamination arising from
3.1. Radiopointsources
CMB fluctuations, we use the CAMB software (Lewis et al.
2000) to compute the CMB power spectrum with the lat-
Very Large Array (VLA) data at 4.8 GHz were used
estPlanckcosmologicalparameters(PlanckCollaborationXIII
by LaRoque et al. (2003) to detect radio sources toward
2015) as input. The spectrum is computed up to multipole
MACSJ1423.8+2404. Two sources were detected within the
(cid:96) = 44000 (corresponding to the NIKA angular resolution)
NIKA field and we used the coordinates obtained by LaRoque
and serves to generate CMB realization via the POKER soft-
et al. (2003) as a reference (see Sect. 5 and Fig. 4). The first
ware (Ponthieu et al. 2011). The simulated CMB maps are
source, hereafter RS1, is located within the central BCG, near
produced on a 5 arcmin × 5 arcmin field and are convolved
theX-raycenter.Thesecond,hereafterRS2,islocatedatabout
with the NIKA transfer function including the beam smooth-
1.5arcmintowardthesouthwest.ThefluxofRS1wasmeasured
ing.WefindthattheCMBfluctuationsareabout15×10−3 and
at various radio wavelengths between 1.4 GHz and 30 GHz,
7×10−3mJy/beam,whichisnegligiblewithrespecttotheinstru-
while the flux of RS2 was only measured at 1.4 and 4.8 GHz.
mentnoiseandatmosphericnoiseresidualat150and260GHz,
WelistinTable1thefluxesmeasuredforbothsourcesandthe
respectively.Therefore,weneglecttheCMBfluctuationsandall
correspondingreferences.
theGalacticdiffuseemissionthatarethemselvesfainterthanthe
To estimate the expected flux of each source in the
CMBfluctuations.
NIKA bands, we modeled their spectral energy distribution
sourFciensalalyc,cowuentiensgtimfoartethteheclcuosntetrriibnugtioonf dfruosmty esxtatrr-afgoarlmacintigc (SED)byFν = F1GHz(cid:16)1GνHz(cid:17)αradio.ThefluxesreportedinTable1
galaxies (CIB clustered anisotropies) and the shot noise from wereusedtofittheamplitudeoftheSED,F ,anditsslope,
1GHz
both dusty star-forming galaxies and radio sources. The clus- α . The best-fit parameters are reported in Table 2 for both
radio
tering from radio sources is negligible (Hall et al. 2010). The sources. We then simulated mock SEDs by sampling the pa-
clusteringtermiscomputedusingtheCIBpowerspectrummea- rameters within their error bars and accounting for the covari-
suredat143and217GHzbyPlanckCollaborationXXX(2014), ancebetweenthem.EachmockSEDwasthenintegratedwithin
modeled by a 1-halo and a 2-halo term, and extrapolated to the NIKA bandpasses to predict the expected flux at 150 and
theNIKAfrequencies.Theshotnoise,arisingfromunresolved 260GHz.Thehistogramofalltherealizationswasfittedwitha
sourcesbelow theNIKAdetection threshold,iscomputed with Gaussianfunctiontogivetheexpectedfluxesanduncertainties,
themodelfromBétherminetal.(2012)inthecaseofdustystar- whicharelistedforbothsourcesandbothNIKAfrequenciesin
forming galaxies and Tucci et al. (2011) for radio sources. At Table 2. The values of the spectral index α we obtain are
radio
the considered scales, the shot noise dominates by a factor of typicalforradiosources(seeforexampleWitzeletal.1979).
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R.Adametal.:ResolvedtSZobservationsofMACSJ1423.8+2404
Table1. Locationandfluxoftheradiosourcesobservedinthe4×4arcmin2fieldaroundMACSJ1423.8+2404.
Source Identifier Position 1.4GHz 4.8GHz 28.5GHz 30GHz
[mJy] [mJy] [mJy] [mJy]
RS1 NVSSJ142347+240439 14:23:47.78+24:04:42.8a 8.0±1.1b 4.40±0.03a 1.49±0.12c 2.0±0.2d
RS2 NVSSJ142345+240340 14:23:45.07+24:03:42.7a 7.2±0.5b 2.72±0.03a – –
References.(a)VLA;LaRoqueetal.(2003).bNVSS;Condonetal.(1998).(c)OVRO/BIMA;Cobleetal.(2007).dSZA;Bonamenteetal.(2012).
Table 2. Best-fit parameters and extrapolation of the fluxes in the NIKA bands of the radio sources in the 4 × 4 arcmin2 field around
MACSJ1423.8+2404.
Source RAoffset Decoffset(arcsec) F α 150GHz 260GHz
1GHz radio
[arcsec] [arcsec] [mJy] [mJy] [mJy]
RS1 0.3 2.6 10.39±0.30 −0.548±0.001 0.68±0.08 0.54±0.07
RS2 41.0 −57.3 9.39±0.69 −0.790±0.003 0.18±0.04 0.13±0.03
Notes.Thedegeneracybetweentheslopeα andtheamplitudeF hasbeenaccountedfortoextrapolatethefluxintheNIKAbands.See
radio 1GHz
textfordetails.
3.2. Sub-millimeterpointsources The positions and fluxes for all the sources are listed in
Table3.
WemakeuseoftheHerschelSpectralandPhotometricImaging
Receiver(SPIRE;Griffinetal.2010)andPhotoconductorArray Similarly, the fluxes of the sub-millimeter sources in the
NIKAfieldwereobtainedbyfittingtheamplitudeofaGaussian
Camera and Spectrometer (PACS; Poglitsch et al. 2010) data
model, using the NIKA FWHM at the source positions ex-
obtained during the Herschel Lensing Survey (HLS, Egami
etal.2010;Rawleetal.2012)1 toidentifysub-millimeterpoint pected from Herschel data. These were then corrected for the
filtering induced by the data reduction (∼15 percent for point
sources and compute their expected spectral energy distribu-
sources). Uncertainties were obtained from the standard de-
tion(SED)asseenbyNIKA,asdescribedbelow.TheHerschel
viation of the amplitudes recovered using Gaussian fits per-
data complement those from NIKA, both in terms of wave-
formed on the Monte-Carlo noise map realizations. The fluxes
length500,350,250,160,and100µm,andangularresolution,
FWHM =35.2,23.9,17.6,9.9,6.1arcsec,respectively. obtained and their uncertainties are summarized together with
the Herschel data in columns of Table 3. By stacking the flux
The PACS maps were produced using the maximum like-
of all the sources, assuming that they are independent, we ob-
lihood map maker MADmap (Cantalupo et al. 2010), pro-
tainedanaveragefluxof1.96±0.82mJyat260GHz(1.15mm)
vided as a PACS Photometer Level 2.5 Product. We used
and 0.46±,0.25 mJy at 150 GHz (2.05 mm), corresponding
the Herschel Source List Product, generated with the soft-
to a mean detection of 2.4 and 1.9σ, respectively. If we ex-
ware SUSSEXtractor (Savage & Oliver 2007), which con-
clude the two sources directly detected at the map level, the
tains the location and flux of the sources found around
MACSJ1424.8+2404.Thesourcesareextractedindependently detection reduces to 1.59 ± 0.89 mJy at 260 GHz (1.8σ) and
0.45 ± 0.25mJy(1.8σ)at150GHz.
for each frequency band, with a signal-to-noise threshold of 5.
The 250 µm channel is the most complete with 15 sources de- Only SMG02 and SMG06 are directly detected in the
tectedinthe4×4arcmin2 aroundthecluster,andweusedthis NIKA maps. To better constrain the fluxes in the NIKA bands,
250µmchannelasabaselinetodefinethesourcepositionsand we modeled the SED with a modified blackbody spectrum,
labels. The corresponding sources in the other channels were F = A (cid:16)ν(cid:17)βdust B (T ),whereA isanormalization,ν aref-
matched to the 250 µm ones on the basis of their positions. ν 0 ν0 ν dust 0 0
erencefrequency,β thedustspectralindex,andT thedust
Two sources peaking at high frequency were not present in the dust dust
temperature. We noticed a flux excess at 100 µm for most of
250 µm catalog and we relied on the 100 µm channel for their
thesourceswithrespecttothebest-fitSEDderivedfromallthe
properties.ByusingalltheHerschelfrequencybands,wethere-
other channels, which we attribute to the modified blackbody
fore found a total of 17 sub-millimeter sources, two of which
spectrum being too simplistic a description of the data at high
correspond to the excesses seen in the NIKA 260 GHz map.
frequency.Wethereforeexcludedthisfrequencyforconstraining
Becauseoftherelativelylowresolutionat500and350µm,afew
theSEDinthefollowing.Sinceweaimtosubtractthesourcesat
sourcesareconfusedwiththeirneighborsand,ingeneral,notall
150GHz,wealsoexcludedtheNIKAmeasurementatthisfre-
thesourcesareidentifiableinallthefrequencybandsinthecat-
quencyandonlycheckedthatpredictedandmeasuredfluxesare
alog. To obtain the fluxes of all sources in all bands, we fit the
consistent. For the SMG02 and SMG05 sources, the 150 GHz
amplitudeofaGaussianfunctiontoeachmapwiththeposition
datawerenotextractedbecauseofstrongcontaminationbythe
fixed at the source reference location and the FWHM fixed to
localtSZsignal.Atlargerradii,thefaint,slowlyvaryingtSZsig-
thatoftherespectiveHerschelchannels.Alocalbackgroundwas
nalisaccountedforbecausewealsofitforalocalbackground.
also fit. In order to account for the confusion in the flux uncer-
The tSZ impact on the fluxes of the other sources is therefore
tainties,wefitthesameGaussianfunctionatrandompositions,
neglected and a bias is only expected in the case of significant
where the noise is homogeneous, and use the dispersion as the
tSZsignalatscalescomparabletothebeam.
uncertainty. We checked that the sources present in the catalog
WeperformedaMarkovchainMonteCarlo(MCMC)anal-
have compatible fluxes with respect to those we recovered.
ysis to fit simultaneously for β and T . This approach
dust dust
1 Obs-IDs1342188159,1342188215and1342188216. allows us to sample the corresponding parameter space and
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A&A586,A122(2016)
Table3.Positionsandfluxesofthe17sub-millimetersourcesidentifiedinthe4×4arcmin2 fieldaroundMACSJ1423.8+2404,measuredby
fittingGaussianmodelstothemapsateachwavelengthasdescribedinSect.3.2.
Source 250µmsourceposition 100µm 160µm 250µm 350µm 500µm 1.15mm 2.05mm
[mJy] [mJy] [mJy] [mJy] [mJy] [mJy] [mJy]
SMG01 14:23:52.31+24:05:04.9 20.8±1.1 35.1±3.2 52.3±7.7 30.4±8.1 11.6±7.4 0.6±3.2 1.4±0.9
SMG02 14:23:48.16+24:04:20.0 12.4±1.4 21.0±3.1 35.8±9.8 24.1±7.4 16.3±7.2 4.8±2.9 ∗∗
SMG03 14:23:53.50+24:06:05.1 10.7±1.2 17.0±2.9 34.7±11.3 23.7±7.9 8.2±7.1 3.4±3.8 0.5±1.1
SMG04 14:23:42.42+24:04:38.8 11.5±1.4 17.7±3.0 29.1±10.8 21.3±8.0 4.4±7.5 2.6±3.2 0.4±0.9
SMG05 14:23:47.58+24:04:48.7 6.1±1.3 9.4±2.8 25.6±8.4 18.3±7.6 14.3±7.5 3.1±2.9 ∗∗
SMG06 14:23:53.32+24:03:48.5 2.9±1.4 8.5±3.1 20.6±9.6 14.9±8.0 1.8±7.7 8.2±3.4 1.0±0.9
SMG07 14:23:45.04+24:05:48.9 3.4±1.3 10.2±3.0 20.1±9.2 14.0±8.0 7.3±8.0 1.3±3.4 1.0±0.9
SMG08 14:23:49.16+24:02:46.1 −1.0±1.5 5.4±3.2 19.9±8.8 24.0±7.8 11.2±7.8 3.5±3.8 0.9±1.0
SMG09 14:23:43.27+24:02:50.2 2.4±1.3 5.8±3.3 12.6±8.6 13.8±7.7 19.4±7.8 2.5±4.1 −0.1±1.1
SMG10 14:23:44.55+24:03:18.4 −1.5±1.2 4.4±3.3 11.1±8.2 19.0±7.7 19.7±7.8 4.3±3.4 −0.2±0.9
SMG11 14:23:54.14+24:05:32.2 7.3±1.3 11.6±2.9 11.0±9.1 3.5±7.5 5.9±7.8 −1.6±3.7 0.3±1.0
SMG12 14:23:43.41+24:03:50.6 5.4±1.3 9.1±3.2 7.3±10.0 −1.9±7.6 −6.9±7.4 2.3±3.4 0.4±0.9
SMG13 14:23:50.13+24:06:17.4 11.7±1.3 8.9±3.1 6.4±7.5 −2.4±8.0 −10.5±7.7 −4.2±3.7 0.9±1.0
SMG14 14:23:47.36+24:05:49.6 3.9±1.3 5.5±2.9 7.9±8.6 10.9±7.8 4.7±7.4 0.3±3.2 −0.2±0.9
SMG15 14:23:40.95+24:05:08.7 2.4±1.3 3.1±3.3 6.6±9.1 6.8±8.2 8.2±7.4 −1.2±3.5 0.0±0.9
SMG16∗ 14:23:53.69+24:04:12.6 6.2±1.4 7.3±3.4 18.0±10.5 −4.0±7.7 −3.5±7.5 3.4±3.3 0.6±0.9
SMG17∗ 14:23:51.72+24:05:48.8 4.7±1.3 4.3±3.4 −14.6±9.7 −6.2±7.7 −7.4±7.4 −2.2±3.4 −0.1±0.9
Notes.ThefinaltwocolumnscorrespondtotheNIKAbands.(∗)Sourcesforwhichthepositionisestimatedbasedonthe100µmPACSchannel.
(∗∗)FluxeswhicharenotavailableduetothetSZcontamination.
Table4. OffsetwithrespecttotheX-raycenter,andfluxextrapolatedtotheNIKAchannelsforthe17sub-millimetersourcesidentifiedinthe
4×4arcmin2fieldaroundMACSJ1423.8+2404,obtainedfromtheSEDmodeldescribedinSect.3.2.
Source RAoffset Decoffset 1.15mm/260GHz 2.05mm/150GHz
[arcsec] [arcsec] [mJy] [mJy]
SMG01 −61.8 24.9 1.52±0.64 0.30±0.19
SMG02 −5.0 −20.0 2.39±1.10 0.62±0.42
SMG03 −78.1 85.1 1.51±0.79 0.35±0.26
SMG04 73.7 −1.2 1.05±0.67 0.25±0.21
SMG05 3.0 8.7 2.01±0.97 0.50±0.34
SMG06 −75.5 −51.5 1.13±1.12 0.31±0.39
SMG07 37.8 68.9 0.60±0.57 0.15±0.17
SMG08 −18.6 −113.9 2.53±1.17 0.60±0.40
SMG09 62.1 −109.8 2.15±1.51 0.55±0.47
SMG10 44.5 −81.6 3.79±1.56 0.97±0.55
SMG11 −86.8 52.2 0.09±0.12 0.02±0.03
SMG12 60.1 −49.4 0.05±0.07 0.01±0.02
SMG13 −31.9 97.4 0.05±0.06 0.01±0.01
SMG14 6.1 69.6 0.14±0.23 0.03±0.06
SMG15 93.8 28.7 0.13±0.28 0.03±0.07
SMG16∗ −80.6 −27.4 0.08±0.11 0.02±0.03
SMG17∗ −53.6 68.8 0.03±0.04 0.01±0.01
Notes. Despite the large uncertainties, these values allow to us estimate the impact of the contaminating sources on the reconstructed cluster
properties.(∗)Sourcesforwhichthepositionisestimatedbasedonthe100µmPACSchannel.
to automatically marginalize over A , which is highly degen- EachofthemodelSEDspectrawasintegratedwithintheNIKA
0
erate with the two other parameters. The Metropolis-Hasting bandpasses with the distribution of fluxes giving the expected
algorithmwasusedtosampletheparameterspace.Eachmodel valueanduncertainty.TheresultsaresummarizedinTable4.A
tested against the data was defined by a value of β and T similarfittingprocedurewasdevelopedbySayersetal.(2013c)
dust dust
and the normalization was linearly fit to the data. For NIKA, with SPIRE data to remove a contaminating signal from unre-
colorcorrectionsareexpectedtobenegligiblewithrespecttothe solved sources in Bolocam data. Our analysis also includes the
calibrationandstatisticaluncertainties(∼1−2%).Inthecaseof PACS 160 µm and NIKA 260 GHz photometric values, which
Herschel,weapplythecolorcorrectionsgiveninPoglitschetal. allows us to release the constraint on the slope parameter β in
(2010) for PACS and those available in the online documenta- contrasttothebaselinevalueof1.7usedbySayersetal.(2013c).
tion for SPIRE2. These coefficients were interpolated for each
modelwiththevaluesofβ andT ,andprovideasmallcor- 3.3. Surfacebrightnessprofile
dust dust
rectiontotheHerschelfluxes(∼5−10%).Wefinallyobtaineda
Figure 2 shows the flux density profiles at 150 and 260 GHz,
setofmodelsdistributedwithrespecttotheposteriorlikelihood.
whichisobtainedbyaveragingthesignalfromtheNIKAmaps
2 http://herschel.esac.esa.int/Docs/SPIRE/html/spire_ in Fig. 1 in radial bins around the X-ray center. Uncertainties
om.html#x1-830005.2.6 were computed using the noise realizations described in
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R.Adametal.:ResolvedtSZobservationsofMACSJ1423.8+2404
Fig.2.Profilesat150GHz(left)and260GHz(right),inunitsofsurfacebrightness,oftherawmap(blackdots)andthecontributionexpected
fromradioandsub-millimeterpointsources(greensolidline).Thegreendashedenvelopegivesthe68%confidenceintervalonthepointsource
profile.
Sect.2.3.Thefluxdensityprofilewascomputedforeachnoise surfacebrightnessisexpressedas
realizationandthestandarddeviationofalltherealizationsper
(cid:90)
radial bin provided the associated error bars. This allows us to 1
S = n2Λ(T ,Z)dl, (3)
accountforpixel–pixelnoisecorrelation.Wealsocomputedthe X 4π(1+z)4 e e
profileexpectedfromthepointsourcesforeachNIKAbandby
simulatingthecorrespondingmapsusingthepointsourcefluxes where Λ(T ,Z) is the cooling function, which depends on the
e
andpositionsgiveninTables2and4.Theprofilewasthencal- temperature and the ICM metallicity Z, and is roughly pro-
culated as for the NIKA maps and the error given by the dis- portional to T1/2. While X-ray imaging is mainly sensitive to
persionofMonteCarlorealizationsofthepointsourcemapsby e
the electronic density, the gas temperature can be estimated
randomlyvaryingtheirfluxeswithintheGaussianerrors.
fromX-rayspectroscopy.SeeforexampleBöhringer&Werner
The 150 GHz profile decreases smoothly toward the center (2010)forareview.
asaresultofthetSZsignal,exceptintheinner15arcsec,where
itrises.Thisisconsistentwiththepositivesignalexpectedfrom
the presence of radio and sub-millimeter emission from point- 4.1. Datapreparation
like sources in the cluster core. Outside the core, the cluster is
MACSJ1423.8+2404 was observed by the Chandra Advanced
detected,attheprofilelevel,upto60arcsecradius.
CCD Imaging Spectrometer (ACIS) for 115ks (obs-ID 4195)
The sub-millimeter sources shown in Fig. 4 are located in
and by the XMM-Newton European Photon Imaging Camera
two distinct regions. Two of them are within 30 arcsec from
(EPIC)for109ksintotal(obs-IDs720700301and720700401).
theX-raypeak,whereweexpectthetSZcontributiontobethe
XMM-Newton datasets were processed by applying the latest
strongest,whiletheothersareconcentratedinaringof70arcsec
calibration files via the Science Analysis System (SAS) ver-
inner radius and 130 arcsec outer radius. No source is seen
sion 14.0.0 and the calibration files available in May 2015.
around 50 arcsec from the cluster center. This source distribu-
Chandra datasets were processed with the Chandra Interactive
tionisreproduced,despitethelargeuncertaintiesinthe260GHz
AnalysisofObservation(CIAO)softwaresuiteversion4.7and
profile.Thereisanexcessnearthecenter,whichweattributeto
calibration database version 4.6.5. We applied the very faint
thesumoftSZandsub-millimetersources(oneofwhichisde- mode3filteringtotheChandradatasetstoreducecontamination
tected with NIKA at the map level). A dip can be seen around
fromthestationaryfluxofhighenergeticparticles.Werejected
1arcmin,andanotherexcessisseenaround100arcsecfromthe 
eventsforwhichthekeyword is>4(forMOS1,2)and
center, both due to the distribution of Herschel point sources.
>13(forPN)forXMM-Newton.
Overall, the NIKA 260 GHz profile is consistent with that ex-
TheChandraandXMM-Newtondatasetswereanalyzedus-
pectedfromtheobservedpointsourcedistribution.Adeficitof
ing the same technique, so unless otherwise stated, the proce-
sub-millimetersurfacebrightnesswasalsoobservedtowardfour
dures described in the following were applied to both datasets.
galaxyclustersbyZemcovetal.(2013)aftertheremovalofthe
Toremovesolarsoftprotonflarecontamination,wefollowedthe
detected sources. This phenomenon is due to the gravitational
procedures described in Pratt et al. (2007) and in the Chandra
lensingofthecosmicinfraredbackgroundemissioninducedby 4 for the XMM-Newton and Chandra datasets, re-
theclusters,andmightcontributetothedistributionweobserve
spectively,rejectingtimeintervalswherethecountrateexceeded
towardMACSJ1423.8+2404.
3σwithrespecttothemeanvalue.Wefoundnoflarecontamina-
tionintheChandradataset,thus,thefull115ksobservationwas
used;fortheXMM-Newtondataset,theusefulexposuretimewas
4. XMM-Newton andChandra X-raydatareduction
3 http://cxc.cfa.harvard.edu/cal/Acis/Cal_prods/
X-ray observations of galaxy clusters are sensitive to both the vfbkgrnd/
electronic density and the temperature of the ICM. The X-ray 4 http://cxc.harvard.edu/contrib/maxim/acisbg/COOKBOOK
A122,page7of16
A&A586,A122(2016)
Fig.3.MultiwavelengthdatasetofMACSJ1423.8+2404.Theoriginofthedataisgivenontopofeachmap.Themapshavebeensmoothedand
theirrangeadaptedforvisualizationpurposes.ThedisplayedPACSandSPIREmapshavebeenreprojectedtomatchtheNIKAmapgrids.The
10arcsecradiuscirclesshowthepointsourcelocationsinblack/whiteforsub-millimetersources(Table3)andmagentaforradiosources(Table1).
122ksforMOS1+MOS2and41ksforPN.Weranawaveletde- datasets from period D for Chandra, since the observation was
tectionalgorithmwithathresholdof5σonexposurecorrected performedin2003.Wecomputedtheweightsfortheinstrumen-
imagesinthe[0.7−7] keVand[0.3−2] keVbandsChandraand talbackgrounddatasetsbyapplyingthesamepointsourcemask-
XMM-Newton,respectively,toidentifypointsources.Theresult- ing andfiltering proceduresas for theobservation datasets. We
ing source lists were merged, inspected by eye, and used as a thensubtractedfromthesurfacebrightnessandtemperaturepro-
masktoremovepointsourcecontributionsfromtheanalysis. filestheinstrumentalbackgroundevaluatedusingthesedatasets.
The residual background component is composed of ther-
mal Galactic emission (Snowden et al. 1995) and the blending
4.2. Vignettingcorrection ofunresolveddistantpointsources,knownasthecosmicX-ray
background(Giacconietal.2001).Wedeterminedaregionfree
To correct for vignetting, we followed the procedure described from cluster emission and subtracted the residual mean back-
inArnaudetal.(2001),computingaweightforeachphoton,de- groundcountrateforthesurfacebrightnessprofileanalysis.For
finedastheratiooftheeffectiveareaattheaimpointtothatatthe the spectroscopic analysis, we extracted the spectrum from the
photonposition.Usingthesequantities,wecanperformimaging source-free region and fitted it with a multicomponent model
andspectroscopicanalysisasifthedetectorhadaflatresponse composed of two absorbed MEKAL thermal components and
equaltothatattheaimpoint.Theweightswerecomputedusing anabsorbedpowerlaw(fordetailsonthemodelused,seePratt
theevigweightroutineforXMM-Newton;weusedtheproce- etal.2009).Whenperformingfurtherspectroscopicanalysiswe
dure described in Bartalucci et al. (in prep.) for Chandra. We addedthebackgroundmodelasafixedcomponentwithanam-
alsocomputedtheeffectiveexposuretimeforeachphoton,pro- plitudescaledbytheratiooftheareaoftheregionofinterestto
ducingexposuremapsthattakebadpixelsandcolumnsintoac- thatofthesource-freebackgroundarea.TheX-rayspectrawere
count.Theresponsefilesforweightsandspectroscopicanalysis extracted and analyzed in the [0.3−10] keV and [0.7−10] keV
werecomputedwiththeappropriatetoolsinCIAO(mkarfand bandsforXMM-NewtonandChandra,respectively.
mkacisrmf)andSAS(arfgenandrmfgen).
5. Multiwavelengthcomparison
4.3. Backgroundsubtraction
Figure 3 presents a multiwavelength overview of
The X-ray background is due to diffuse sky emission and MACS J1423.8+2404, including the  survey (Faint
an instrumental component caused by the interaction of high Images of the Radio Sky at Twenty-Centimeters; Becker et al.
energetic particles with telescope instruments. To estimate 1995) observations at 1.4 GHz that provided the radio point
the instrumental component, we used datasets tailored to source locations. The two radio sources discussed in Sect. 3.2
isolate this component, namely  and 4 for are clearly visible on the map. The complementarity of the
XMM-Newton and Chandra, respectively. To match the ob- Herschel and NIKA instruments is clear; the NIKA bands
servation, these datasets were skycasted and normalized in complement the Herschel spectral coverage at lower frequen-
the [10−12], [12−14] keV and in the [9.5−10.6] keV band cies. In addition, the angular resolution of the NIKA bands is
for MOS1,2-PN and ACIS, respectively. We used background comparable to that of SPIRE at 250 µm and PACS at 160 µm,
A122,page8of16
R.Adametal.:ResolvedtSZobservationsofMACSJ1423.8+2404
6. Radialthermodynamicalreconstruction
30.0
The radial physical properties of the ICM were reconstructed
06:00.0 using two approaches. The first, detailed in Sect. 6.1, uses the
X-ray data alone. The electronic density and gas temperature
are directly measured and serve to reconstruct all the other
30.0
quantities.Thisapproachstronglydependsonthespectroscopic
temperature reconstruction. The second approach, detailed in
deg) 24:05:00.0 Sect. 6.2, consists of jointly fitting the tSZ data and the depro-
0 ( jectedelectronicdensityextractedfromtheX-raydata.Thepri-
0
0
Dec. J2 30.0 manadryasqusauncthititehsearmeetthheordefodreeptehnedpsroesnsluyrewaenadkleyleocntroXn-ircadyenspsietcy-,
troscopythroughelectronicdensityreconstruction.Thecompar-
04:00.0
isonofthetwoapproachesisgiveninSect.6.3.
30.0
6.1. X-rayradialthermodynamicprofiles
NIKA 150 GHz NIKA/Hershel SMG
03:00.0 Chandra photon counts NVSS radio sources We need to determine the temperature and electronic density
Zitrin et al. mass model HST f814W
profiles to compute the X-ray electronic pressure and entropy
56.0 54.0 52.0 14:23:50.0 48.0 46.0 44.0 42.0 40.0 profiles. The electronic density profiles was computed by ap-
R.A. J2000 (hr)
plying the regularized deconvolution and deprojection tech-
Fig.4. Composite multiwavelength overview image of nique described in Croston et al. (2006). We extracted the sur-
MACSJ1423.8+2404. Blue image: NIKA 150 GHz map show- face brightness profile from concentric annuli centered on the
ingthetSZsignal.Redimage:Chandraphotoncounts(Obs-ID04195) X-ray peak, (RA, Dec) = (14:23:47.9, +24:04:42.3), in the
tracing the electronic density. White contours: Surface mass distribu-
[0.3−2.5] keV and [0.7−2.5] keV bands from the three com-
tion model obtained by Zitrin et al. (2011, 2015) on a linear scale.
bined EPIC and ACIS cameras, respectively. After background
Yellow circles: (Sub-)millimeter sources candidate locations obtained
usingtheNIKA260GHzmap(solidline)andidentifiedusingHerschel subtraction,theprofileswererebinnedviaalogarithmicbinning
(dashed-line).Cyancircle:Locationoftheradiopointsourcespresent factor of 1.05 to have a 3σ significance for each bin, and were
inthefieldasobtainedfromVLA(LaRoqueetal.2003).Greenimage: point spread function (PSF) deconvolved using the analytical
HubbleSpaceTelescopeimageusingtheF814Wfilterobtainedbythe modelofGhizzardi(2001)forXMM-Newton.ForChandra,we
CLASH program (Postman et al. 2012) showing the location of the assumed that the PSF is negligible with respect to the width of
galaxies. thebins.
The deconvolved, deprojected surface brightness profiles
wereconvertedtodensityusingaconversionfactordetermined
from the projected temperature profile. This temperature pro-
filewasdeterminedbyextractingspectrafromconcentricannuli
allowingustobreaktheconfusioninthelowfrequencySPIRE centeredontheX-raypeak,andthewidthofeachannuluswas
bands in the crowded cluster environment for sources that defined to have a signal-to-noise ratio of 30 after background
are directly detected by NIKA. The Hubble Space Telescope subtraction. We measured the temperature in each bin by fit-
(HST) data from the Cluster Lensing And Supernova survey ting the spectrum with an absorbed MEKAL model, where the
with Hubble program (CLASH; Postman et al. 2012) show absorption was fixed to NH = 2.2×1020cm−3 (Kalberla et al.
the galaxy distribution. The (smoothed) Chandra X-ray image 2005), the redshift to z = 0.545, adding the scaled sky back-
tracesthegaselectronicdensityandisusedfurtherinSect.6. ground component discussed above. We fit with the paramet-
ricmodeldescribedinVikhlininetal.(2006)tointerpolatethe
Figure 4 shows a composite multiwavelength image of the
temperatureprofileforeachsurfacebrightnessbin.Theemissiv-
cluster. The figure includes the NIKA 150 GHz tSZ map, ityterm,ΛterminEq.(3),dependsweaklyontemperature,so
the Chandra X-ray photon counts, the NIKA and Herschel
thatthechangeweobtainonthedensityprofileusingChandra
sub-millimeter galaxy locations, the NVSS radio source lo-
temperature profile instead of XMM is less than 1% over the
cations, and the HST image from CLASH. We also provide, entire radial range. The differences in temperature reconstruc-
for visual comparison, the surface mass distribution model of
tion between Chandra and XMM-Newton (e.g., Schellenberger
MACSJ1423.8+2404 produced by Zitrin et al. (2011, 2015) et al. 2015) thus do not affect the electronic density. To depro-
withtheCLASHdata.Theimageprovidesadetailedpictureof
jectthetemperatureprofile,wemeasuredthespectroscopic-like
theclustercomplementingthediscussionofSect.1.TheNIKA
temperature(Mazzottaetal.2004)usingtheweightingscheme
150 GHz tSZ signal surrounds the cluster core. The hole seen
implementedinVikhlinin(2006),wheretheobservedtempera-
in the tSZ signal is coincident with the BCG and results from
tureprofileismodeledastheweightedsumofconcentricplasma
cancelingthetSZbytheradioandsub-millimetersignal,asdis- shellseachatadifferenttemperature.Asforthedensityprofiles,
cussedinSect.3.TheX-raymorphologyisverypeakedandthe wetakethePSFeffectsforXMM-Newtonintoaccount.
maximumoftheemissioncoincideswiththeBCG.Theelliptic-
Finally, M , the cluster mass enclosed within R 5, was
ityofthespatialmassdistributionisveryclearfromthestrong 500 500
calculated by iteration about the M −Y relation of Arnaud
lensing map, and is also visible in the X-ray map but less sig- 500 X
etal.(2010).
nificant.TheellipticityisnotvisibleinthetSZmapbecauseof
the limited signal-to-noise and the point source contamination.
Thegalaxydistributiondoesnotshowanyparticulargroupthat 5 R istheradiuswithinwhichthemeanclusterdensityisequalto
500
wouldbethesignofamergingevent. 500timesthecriticaldensityoftheUniverseatthecluster’sredshift.
A122,page9of16
A&A586,A122(2016)
6.2. ModelingoftheICMandjointtSZ/X-rayfittingprocedure procedure also marginalizes over nuisance parameters such as
thezeroleveloftheNIKAmap,thecalibrationuncertainty,and
To fit the tSZ and electronic density jointly, we modeled the
the central point source flux and position when included in the
ICM using the approach described in detail in Adam et al.
fit.FulldetailscanbefoundinAdametal.(2015).
(2015).AsseeninSect.5andasemphasizedbyMorandietal.
Theconstraintsobtainedonthepressureandelectronicden-
(2010),MACSJ1423.8+2404iselliptical.Nevertheless,weas-
sityprofilesarealmostindependent.However,eachmodelcom-
sumesphericalsymmetrybecausethisworkdoesnotfocusonits
paredtothedataincludesrelativisticcorrectionscomputedusing
geometry,butontheimpactofthepresenceofpointsourceson
theradialtemperatureprofile,givenbytheratiooftheelectronic
the pressure profile reconstruction. Moreover, the significance
pressure and density profiles, for each radial shell of the ICM.
oftheNIKA150GHztSZmapisnotsufficienttoconstrainany Thisessentiallyaffectstheconstraintonthepressureprofilebut
asymmetry. theeffectisverysmallcomparedtotheuncertainties.Therefore,
Theradialdistributionoftheclusterelectronicpressurewas
the constraint on the electronic density profile is driven by the
modeledbyagNFWprofile(Nagaietal.2007),describedby
X-ray data and that on the pressure is largely driven by the
P tSZ data. The Planck constraint on the overall tSZ flux is rel-
Pe(r)= (cid:18) (cid:19)c(cid:18) 0(cid:18) (cid:19)a(cid:19)b−c· (4) atively weak because of the location of the cluster on the sky
r 1+ r a andthenoiseinhomogeneity.However,Planck providesanup-
rp rp perlimitthatallowstheMCMCproceduretoavoidmodelsthat
divergeatlargescales,whereNIKAisnotsensitive.Planckand
Theparameter P isanormalizationconstant;r isacharacter-
0 p NIKAarethereforehighlycomplementarytoconstrainthepres-
isticradius;anda,b,andcsettheslopesatintermediate,large,
sureprofilefromsmalltolargescales.
and small radii, respectively. This model was chosen to allow
thedescriptionoftheprofileatallscales.Theelectronicdensity
was modeled by a Simplified Vikhlinin Model (Vikhlinin et al. 6.3. Results
2006),
MACSJ1423.8+2404 is known to be a typical cool core (e.g.,
ne(r)=ne01+(cid:32)rrc(cid:33)2−3β/2(cid:34)1+(cid:32)rrs(cid:33)γ(cid:35)−(cid:15)/2γ· (5) Mf(aou,obnra,dnc)dfoir=etsua(lc1.h.220c21l2u03s),t,e5sr.os49wb0ye5,Au0sr.en7da7u3thd6e)e.ptrTeahsl.seu(r2Xe0-1pra0roy)fiaplsehopataobrnaamseceloitunenres:t
provided by XMM-Newton is larger than that of Chandra, al-
Theparametern isthecentraldensity,r isthecoreradius,and
e0 c lowingustoprobetheclusterICMuptolargerradii.Wethere-
βisrelatedtotheslopeoftheprofile.Thesecondtermallowsa
foreusedtheXMM-Newtonresultsasareferenceandwecross-
steepening of the profile at large scales. The parameter (cid:15) gives
checkedourresultswiththeChandradata.
thechangeintheslope,r theradiusatwhichthetransitionoc-
s
curs, and γ the width of the transition. In the following, we set
γ = 3 since this value provides a good fit to all clusters con- 6.3.1. Impactofthepointsourcesatmillimeterwavelengths
sidered in the analysis of Vikhlinin et al. (2006). All the other
The impact of the point source contamination on the recon-
parametersarevariedwhenfittedtothedata.
structedpressureprofilewastestedbyconsideringthreedifferent
With the pressure and the density in hand, we compute the
temperatureprofileassumingtheidealgaslaw,k T (r) = Pe(r), cases:
B e ne(r)
andtheentropyprofileasK(r)= Pe(r) .Thetotalmass,assum- 1. The presence of point sources was ignored and we fit the
ing hydrostatic equilibrium, enclonsee(rd)5/w3 ithin r is then given by parameters P0 and rp, keeping the slope parameters fixed
to their baseline values. This case is referred to as model 1
(M1).
M (r)=− r2 dPe(r), (6) 2. The point sources were subtracted assuming the fluxes of
HSE µ m n (r)G dr Table 4 and we repeated the fit of model M1. This case is
gas p e
referredtoasmodel2(M2).
wherempistheprotonmass,GisNewton’sconstant,andµgas = 3. Thepointsourcesweresubtractedassumingthefluxesgiven
0.61themeanmolecularweightofthegas. inTable4,butpossibleresidualsofthecentralsourceswere
The parameter space was sampled using the MCMC ap- also fitted. In this case, we also released the constraints on
proachdetailedinAdametal.(2015),jointlyfittingthe150GHz theinnerandouterslopeparameters,candb,whicharealso
NIKAtSZmapandtheelectronicdensityprofilecomputedfrom fitted.Theintermediateslopeparameterawasheldfixedbe-
the X-ray data. We added an additional constraint on the to- causeitisstronglydegeneratewiththecharacteristicradius
tal tSZ flux of the cluster with the Planck Compton parame- r andtheouterslopeb.Thiscaseisreferredtoasmodel3
p
ter map (Planck Collaboration XXII 2015e). The tSZ models (M3).
were convolved with the effective transfer function of the ob-
servations, including the beam smoothing and the large-scale ComparisonoftheoutputpressureprofilefrommodelsM1and
filtering cutoff due to the removal of the atmospheric noise. M2(seeFig.5)allowsadirectestimationoftheimpactofpoint
MACSJ1423.8+2404 is not present in the Planck catalogue of sources. The use of model M3 was motivated by the large un-
tSZ sources (Planck Collaboration XXVII 2016), but we ob- certainties on the point source fluxes as shown in Table 4. As
tained an upper limit on its flux by integrating the Compton discussed in Sect. 3.3 and shown in Fig. 2, the sources that are
parameter map (Planck Collaboration XXII 2015e) using aper- intheouterregionoftheclusterdonotcontributesignificantly
ture photometry. The error on the flux was computed by per- to the radial flux density. However, this is not the case for the
forming the same measurement randomly around the cluster, centralsources,inparticular,forRS1andSMG05.Weexpecta
where the noise is homogeneous. The flux was measured to be significantcorrelationbetweenthefluxofthesesourcesandthe
YPlanck = (0.40±0.66)×10−3 arcmin2. The MCMC sampling pressure profile parameters related to the cluster core, such as
tot
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