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CMB & the Promise of an Indian Collaborative Space Mission

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CMB & the Promise of an Indian Collaborative Space Mission Status of CMB & the promise of an Indian collaborative space mission Astro-Particle Physics meet Tarun Souradeep IUCAA, Pune CGPA-IFTHEP@ IISER Pune On behalf of CMB-Bharat Feb. 25, 2018 (Indian CMB consortium) Cosmic “Super–IMAX” theater COBE – 0.5 Myr FIRAS Here & Now (14 Gyr) Transparent universe Opaque universe CMB Anisotropy & Polarization CMB temperature Tcmb = 2.725 K -200 K < T < 200 K Trms ~ 70 K TpE ~ 5 K TpB ~ 10-100 nK Temperature anisotropy T + two polarization TT modes E&B Four CMB spectra : Cl , EE BB TE Cl ,Cl ,Cl TB EB Parity violation/sys. issues: Cl ,Cl CMB anisotropy measurements 1st, 2nd and into the 3rd decade 1991-94 2001-2010 FIRS, Tenerife CAT, VSA, … 2009-2011 Boomerang, MAXIMA, BICEP 1&2,KECK Archeops, DASI, CBI, POLARBEAR, ACBAR, QUAD.,,, SPT, ACT SPIDER, .. CMBPol/COrE 2020+ 0' * 47"%&' ( )' .)01 2)* 74)."' * )5?"##) &75#++%5#)* %&&%' ( &) - CF0GH$. /012342567$I #$3) /1$9/: /;$5<F0$* + , - $ - CF0GH$A/1BCD3B07$$E$3) /1$9/: /;$5<F0$* + , - $ * + , - $. /012342567$8#$3) /1$9/: /;$5</0$=> ?@$ * + , - $A/1BCD3B07$EE$3) /1$9/: /;$5</0$=> ?@$ ! +7( $8)%&).7")&94#"%' ")5?7( )4"#A%' 9&)5L ' )&75#++%5#)%( )5#"* &)' .)7( , 9+7") "#&' +9I ' ( )7( / )&#( &%I A%5- )) Courtesy: Soumen Basak CMB Temperature at Planck Frequencies Credit: ESA, HFI & LFI consortia CMB Polarization at Planck Frequencies Credit: ESA, HFI & LFI consortia Foreground for CMB anisotropy Foreground for CMB Polarization Cleaning the background from its 7 veils Page 24 François R. Bouchet "Planck main cosmological results" 3% of the CMB sky replaced by a Gaussian Random realisation Planck CMB sky map Truly all-sky !!! Only 3% of sky replaced by constrained realization Planck Collaboration: The Planck mission AP CMB Foregrounds : Rich A&A science d 0 20 200 µKRJ @353 GHz p Fig. 21. Dust polarization amplitude map, P = Q2 + U2, at 353 GHz, smoothed to an angular resolution of 100, produced by the di↵use component separation process described in (Planck Collaboration X 2015) using Planck and WMAP data. Fig. 22. All-sky view of the magnetic field and total intensity of dust emission measured by Planck. The colours represent intensity. The “drapery” pattern, produced using the line integral convolution (LIC, Cabral & Leedom 1993), indicates the orientation of magnetic field projected on the plane of the sky, orthogonal to the observed polarization. Where the field varies significantly along the line of sight, the orientation pattern isirregular and difficult to interpret. 29 Fermi Planck multiple synergies Planck, Fermi, L & the “dark” gas AT > 10 G old radio eV gas & loops dust in clouds bubbles & haze SNRs blazars ck Isabelle Grenier Plan interstellar AIM, Paris Diderot & CEA Saclay radiation field on behalf of both collaborations SZ clusters from Planck Planck sky maps Statistics of CMB CMB Anisotropy Sky map => Spherical Harmonic decomposition l T ( ,) almYlm( ,) l2 ml * alm a l'''' m C l ll mm Gaussian Random field => Completely specified by angular power spectrum Dl = l(l+1)Cl : Dl : Power in fluctuations on angular scales of ~ /l radians Planck Angular power spectrum 2015 Planck CMB Polarization spectra EE: 2015 Planck CMB Polarization spectra TE Acoustic physics CMB Angular power spectrum 150 Mpc. (fig credit: W. Hu) CMB physics is very well understood & accurately computed CMB@IUCAA: CMBAns Boltzmann code by Santanu Das Multi-D Joint Posterior distribution P( parameters |Cl ) 2 Baryons: Ωbh 2 Cold Dark Matter: Ωmh Hubble constant : H0 Reionization Depth : t Primordial fluctuations – Spectral index: ns Amplitude: As Standard 6 parameter flat, LCDM model (S Das & TS : JCAP 2014) Cosmological Parameters 6-Parameter LCDM 1% 1.7% 0.04% 0.6% ’Standard’ cosmological model:1.3% Flat, LCDM with nearly Power Law (PL) primordial power spectrum 1.4% Paradigm of Hot & Dense early Universe i.e., ‘Big Bang’ model Cosmic “Super–IMAX” theater 0.5 Mega-years Here & Now (14 Giga-years) TransparentUniverse universe must have been at least (107x) hotter & 1021 x denser in its past Opaque universe COBE-FIRAS results strongly constrain any Energy input into the CMB in the not-so-early universe (z<105) 60 Ghz 600 Ghz E 2.5104 , E ( 500 5000m) Spectral distortions expected at ~10-8 level carry important cosmological information on its thermal history. A new emergent observational thrust area of CMB research ARCADE 2004 10 Ghz 30Ghz (figs: Bond, 1996) Paradigm of CMB flucs: Acoustic phenomena pre-recombination Plasma universe Paradigm of Structure formation? - Backbone of `precision’ cosmology Gravitational Instability Mildly Perturbed universe Present universe at z=0 at z=1100 Cosmic matter content tot b DM L H 0 Weak lensing: Light deflects due to gravity Projected LensingPlanck Collaboration: potentialThe Planck mission from Planck Planck Collaboration: Gra0vitational1 2lensing)Kby#lar(ge-scale&%(structures, )withPlanck Planckat theexpectedlevel. InSect. 3.3, we cross-correlatethe reconstructedlensingpotential withthelarge-angletemperature T⇥ anisotropiestomeasuretheCL correlationsourcedby theISW effect.Finally,thepowerspectrumof thelensingpotential ispre- sentedinSect. 3.4. Weusetheassociatedlikelihoodalone, and in combination with that constructed from the Planck temper- atureand polarization power spectra (Planck Collaboration XI 2015), toconstraincosmologicalPlanck Collaboration:parametersGra0vitational1inSect.2lensing3.5)K. by#lar(ge-scale&%(structures, )withPlanck Planckat theexpectedlevel. InSect. 3.3, we cross-correlatethe 3.1. Lensing potential reconstructedlensingpotential withthelarge-angletemperature 1 T⇥ ⇥ˆWF (Data) anisotropiesInFig.to2measurewe plotthetheCWL ienercorrelation-filteredsourcedminimumby the-varianceISW lensing effect.Finallyestimate,,the0gipo1venwer2)by+#spectrum( &%( , 6of) thelensingpotential ispre- sentedinSect. 3.4. W⇤−eusetheassociated−⇤ likelihoodalone, and Fig.2 Lensingpotential estimatedfromtheSMICAfull-mission d (ˆn) = ⇧ ⇤(ˆn⇥)⇥, fid K' L )* 7&&)/ #( &%5- ) in combination with• rthat#*constructed74&)5?#)Cfrom01 2the)k#Planc+/ )Lk%temper5?' 95-) CMBJ %,maps?)* 7&using&)/ #(the&%5-MV) estimator1 7&8) . The power spectrum of ⇥ˆWF = L ⇥ˆMV, (5) thismapformsthebasisof our lensinglikelihood. Theestimate atureand polarization$?po7wer( ,LM%spectra( , )&9⇥⇥"(,Planck.fid7$#)HCollaboration⇥"⇥%, LM?5( #&&)XI 2015), toconstraincosmological parametersCL + NinLSect. 3.5.⇥ hasbeenWiener filteredfollowingEq. (5), andband-limited to −⇤ • 1 #7&9"#*1#( 5)' .)?%, ?#")' "/ #")( ' ( R ⇥⇥, fid∆T(nˆ) −⇤ ∆T ˆn + d (ˆn) 8≤ L ≤ 2048. whereCL isthelensingpotential powerspectruminour fidu- V79&&%7( )$' ""#+7I ' ( )?#+4&)5' )"#$' ( &5"9$5) 3.1. Lensingcial modelpotential) and−⇤N⇥⇥ isthe−⇤noisepower spectrum of therecon- L ⌥ +#(1 &%( , )&%, ( 7+=)L ?%$?)%&)"#+75#/ )5' )5' 57+) d (ˆn) = ⇧ ⇤(ˆn) K#( &%( , )4' 5#( I 7+) ⇥ˆWF (Data) InFig.struction.2we plot)theAsWweienershall-filtereddiscussmminimum⇥inSect.-v4.5ariance, thelensinglensingpotential estimateisunstable⌅ h2 =for L < 8, and so we haveexcluded those * 7&&)7+' ( , )5?#)+%( #)' .)&%, ?5))) estimate,0gi1ven2−⇤)by+#( &%( ⇥, 6) modesFig.for11.)))all)W))>analysesiener- 4−⇤%-filtered$7+)inr941thislensing:eVpaper)A7+9,potential#as)'well.)/ 6as)estimates)inQ`⇥the] )7MV"with$*Fig.lensing%minimal( ))2 Lensingmaskingpotential(usingestimatedthe NILCfromcomponenttheSMICAseparatedfull-missionmap), in Galactic d (ˆn) = ⇧ ⇤(ˆn⇥)⇥, fid −⇤ 1 7&8) K' L )* 7&&)/ #( &%5- ) map.• coordinatesr #* 74&with)5?#a)CMoll01 2weide)k#+/projection)L %5?' 9(5Planck) CollaborationCMBJ %,maps?XV)* 72015&using&)/ #).(the&The%5-MV)reconstructionestimator. Thehasbeenpowerbandlimitedspectrum toof 8 L 2048 (where,• ⇥folloˆWF;∆( =wing/T(9$nˆ#)con&L−)$v⇤'ention,⇧""∆#⇥T+ˆ7MVLI ,is'ˆn (used+⇤)Hd#⌅as5L(ˆ⌃then#)#multipole( (5))01 2this)indekmap#+x/in)formsthe lensingthebasispoofwerourspectrum).lensinglikelihood. Theestimate As$a?visual7( ,LM%(illustration, )&9⇥⇥",.fid7$#of)H⇥the"⇥%, signal-to-noiseLM?5( #&&⇤) level inthelens- CL +4NL ⇥ hasbeenWiener filteredfollowingEq. (5), andband-limited to ingpotential estimate,'V(()⇤5?)=#)&in⇥8Fig.- )71+(3/−⇤we)%c5o&plots), "7a/simulation%#( 5=)?#(of$the#•= )MV1 #7&9"#*1#( 5)' .)?%, ?#")' "/ #")( ' ( R ⌥ f 8≤ L ≤ 2048. reconstruction,⇥⇥, fid∆T(nˆ)+#−as7⇤Awell#∆&)7Tas)/ %ˆnthe&I+(input$d5)(ˆ(n⇥')(realizationRV79&&%7used.( ) There- whereCL logicalisthemodelslensing2analysedpotential pominwer⇥thespectrum2015 Plancinourk papers.fidu- HoweVver7,9&&Compact%7( )$' "sources"#+7I 'are( )detected?#+4&)5in' )the"#$single-frequenc' ( &5"9$5) y maps and construction) in this ⇥data⇥ and&⌅%release,,⇥input(h75=9are"we#)clearly're⇤(g)ard01correlated,the2`⌅)combined) although⌅ TT, TEthe, recon-and EE assigned to one of two sub-catalogues, the PCCS2 or PCCS2E. cial model and−⇤NL isthe−⇤noisepower spectrum2of⇤therecon- +#( &%( , )&%, ( 7+=)L ?%$?)%&)"#+75#/ )5' )5' 57+) structiond has(ˆn)considerable=⌥⇧ ⇤(ˆn)94additionaleV −power3 due tonoise. Ascan )F;%247! #&I "&! #N! $$ struction.)AsPlancwekshallresultsdiscussasmpreliminaryinSect.4 4.5. ,Kthe#( &lensing%( ,M)4pl'potential5#( I 7+) The first of these allows the user to produce additional sub- 2 V(⇤)=⇥ ⇥ 1− e ˆWF estimatebeisseenunstable⌅ ⇥inhFig.=for1L, e<ven8,theandMV⇧so wereconstructionhave⇤excluded⌅⌃onlythosehasS/N ⇥*17&&catalogues)7+' ( , )5?at#)+higher%( #)' .reliabilities)&%, ?5))) than the target ⇥80 %(Sim.)reliabil- modesfor)))alla)))fe>analysesw- 4)modes%$7+)inr94around1this:eVpaper)A7L+9,4⇥#as)50.'well.)/ 6as)s)inQ`⇥the] )⇤7MV"$*lensing%( )) ity of the full catalogue. The total number of sources in the 8.4.2. LensingV(⇤lik)=elihood⇥ 1+−⇤cos map. • The;∆( /T(MV9$nˆ#)lensing&−)$⇤'
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