dp - puetzfeld.orgpuetzfeld.org/files/gk2002_2.pdf · The cosmic micro w a v e bac kground Dirk P utzfeld Email: [email protected] WWW: . de/~ dp O ver view Motiv ation Historic

Thecosmicmicrowavebackground

DirkP�utzfeld

Email:[email protected]

W

W

W

:http://www.thp.uni-koeln.de/~dp

Overview

�

Motivation

�

HistoricroutetotheCMB

�

Historyoftheuniversewithinthestandardpicture

�

Processesa�ectingtheCMB

�

TheCOBEsatellite

�

Othermeasurementsofthebackgroundradiation

�

ComputerprogramsforCMBcalculations

�

Sensitivityofthespectrum

�

References

GK-Scienti�cComputing,K�oln,2002-07-10

SN

Iaresults

http://www.thp.uni-koeln.de/~dp

–0.6

–0.4

–0.2

00.

20.

40.

60.

8

0 0.5

1 1.5

�0

m

0

H0

=

65

�2 m

in

=

134:54

68:3%

95:4%

3032343638404244

0.2

0.4

0.6

0.8

11.

2

�

z

F13

3032343638404244

0.2

0.4

0.6

0.8

11.

2

�

z

F1,:::,F10,F13

k<

0

3032343638404244

0.2

0.4

0.6

0.8

11.

2

�

z

F11,F12,F14,:::,F27

k>

0

–1.2

5–1

.2–1

.15

–1.1

–1.0

5–1

–0.9

5–0

.9

0 0.02

0.04

0.06

0.08

0.1

0.12

�0

k0

H0

=

66

�2 m

in

=

138:03

95:4%

68:3%

3032343638404244

0.2

0.4

0.6

0.8

11.

2

�

z

C1,:::,C8

k<

0

FLRW

F13650.631.10134.541.51-0.7813.8Gyr

F28650.290.71135.261.51-0.56

Weyl-Cartan

C266-1.030.05

1.00-0.90138.0281.56-0.11018.4Gyr

C9690

-0.281

-0.5

292.8213.321

SN

Iaresults(othergroups,standardmodel)


Symbol

Ref.

Best-�tparameters

Comment

S1

[13]

fm0=�0:2;�0=0g

early�t(unphysical)

S2

[13]

fm0=0:4;�0=0:6g

P1

[11]

fm0=0:28;�0=0:72g

R1

[15]

fm0=0:24;�0=0:72g

MLCS

R2

[15]

fm0=0:2;�0=0:8g

Template

G1

[23]

fm0=�0:1;�0=0g

G2

[23]

fm0=0:4;�0=0:6g

MLCS

G3

[23]

fm0=0:3;�0=0:7g

Template

V1

[19]

fm0=0:28;�0=0:72;M

=23:94g

V2

[19]

fm0=0:79;�0=1:41;M

=23:91g

V15

[21]

fm0=0:33;�0=0g

1997�included

W1

[24]

fH0=65;m0=0:7;�0=1:2g

Combineddataset

SN

Iaresults(othergroups,non-standardmodels)


Symbol

Ref.

Best-�tparameters

Comment

B1

[22]

fm0=0:3;Rigid0=0:7g

Conformalmodel

V3

[19]

fm0=0:49;�0=0:51;M

=23:97g

��S

�

2

V4

[19]

fm0=1:86;�0=1:52;M

=23:95g

��S

�

2

V5

[19]

fm0=0:4;�0=0:6;M

=23:96g

��H

2

V6

[19]

fm0=0:98;�0=1:53;M

=23:91g

��H

2

V7

[19]

fm0=0:4;�0=0:6;M

=23:96g

��

V8

[19]

fm0=1:62;�0=1:59;M

=23:93g

��

V9

[20]

fm0=0:54;�0=0:46;M

=24:03g

Variable�

V10

[20]

fm0=1:76;�0=1:34;M

=24:03g

Variable�

V11

[21]

fm0=0:79;�0=1:41;w�=�1g

Quintessencemodel

V12

[21]

fm0=0:65;�0=1:22;w�=�1g

Quintess.model+1997�

V13

[21]

fm0=0:52;�0=0:48g

��H

2+1997�

V14

[21]

fm0=0:6;�0=0:4g

��S�

2+1997�

V16

[21]

f�0=�0:358;z max

=5g

QSSCmodel

T1

[25]

fz1=0:08;HII0

=HI 0=0:87;I 0=0:3;

Modelwithlocalvoid

HI 0=64;II0

=0:6;�II0

=0:3g

HistoricroutetotheCMB


1931

Lema^�tre

formulatedideaofahotbeginning

1934

Tolman

thermodynamichistoryofanexpandinguniverse

1941

Adams

interstellaremissionlines,lateridenti�edwithmoleculesatT�2:3K

1942

Chandrasekhar&

theorytherm.equilibrium&frozenabundancesathighenergies

Henrich

leadstoobservedcosmicabundances

1942,46Gamow

pointedoutnecessityofadynamicmodel

1948

Alpher,Bethe,Gamow

elementsbuiltupbyrapidneutroncapture

1948

Gamow

estimatedbaryonnumberdensitynatT�10

9K(T�n

1 3

!

T0�4K)

1948

Alpher&Herman

correctedsomenumericalerrorsT0�5K

1950

BellLabs

startworkonsatellitecommunication

1959

NASA

launchedECHO(passivere ector,100ftdiameterballoonmade

ofaluminizedpolyester,orbit800-900nmi,960MHz,2390Mhz)

1961

BellLabs

constructionofahornantennaHolmdel(NJ),50kmfromPrinceton

1963

Penzias&Wilson

antennaunused,conversionintoradiotelescope,toohighbackgrounds

1964

Smirnov

rediscussedworkofGamow,arrivedatT0�1�10K

1964

Doroshkevich&NovikovpointedoutusefulboundonradiationtemperaturefromBellreports

1965

Penzias&Wilson

BurkementionsPeebles,meetingwithPrincetongroup,twopapers

Dickeetal.

onobservedbackgroundandtheoreticalmodelinsamejournal

1978

Penzias&Wilson

Nobelprice

History of the universe http://www.thp.uni-koeln.de/~dp

recombination

nucleosynthesis

reheating

matter-radiation equivalence

inflation

big bang / bounce reionization

matter dominatedradiation dominatedvacuum dominated

Processes leading to CMB anisotropies http://www.thp.uni-koeln.de/~dp

CMBR Perturbations

observer movementpeculiar velocity of matter

at last scattering

fluctuations in the gravitational potentialon the last scattering surface

inhomogenities of radiation densityat last scattering

processes taking place along thephoton path

gravitational potential wells

compton scattering

wipe out processes

decoupling not instantaneous

reionization

COsmicBackgroundExplorer


�launched1989-11-18(Deltarocket)

�totalmass2270kg,altitude900km,0:8rpm

�scansfullskyeverysixmonths

(14orbitsperday)

�fullskycoveragemid-June1990,

heliumdepleted1990-09-21

�1991-09-07oneofthethreegyrosfailed,but

satellitestillinnominalorbit(2001-03-08)

Instruments

�Di�erentialMicrowaveRadiometer

�FarInfraRedAbsoluteSpectrophotometer

�Di�useInfraRedBackgroundExperiment

COsmicBackgroundExplorer-Detectors


DMR

FIRAS

DIRBE

2hornantennas

hornantenna7withdegreeview

19cmtelescope+abs.radiometer

di�erentialradiometers

Michelsoninterferometer(di�.op.)

420�42

0

�eldofview

nocooling

cooledto1:6K

cooledto1:6K

datarate250bps

datarate1362bps

datarate1716bps

31:5;53;90GHz

0:1�10mm

1:2�240�mbrightness

60degreesbet.anten.

alignedwithspinaxis

1:2;2:2;3:5�mlin.polarization

� uctuationsinthe

CMBbrightness

�4yeardataavailable

�stilloperationalin

allsixchannels

�CMBspectrum,dust,

andlineemissionfromgalaxy

�surveyedsky1.6times

�ceasedtooperatewhenliquid

heliumdepleted1990-09-21

�CIBbrightnessandpolariza-

tionmaps

�reduced

sensitivity

after

1990-09-21

�turnedo�Dec.1993

CMB spectrum http://www.thp.uni-koeln.de/~dp

100 200 300 400 500 600

Frequency [GHz]

2,65

2,7

2,75

Tem

pera

ture

[K]

COBE / FIRAS(Datapoints from Smoot astro-ph/9705101)

0 200 400 600 800 1000

Frequency [GHz]

0

0,5

1

1,5

2

Ene

rgy

dens

ity [1

0-25 J

s m

-3]

2.726 K blackbody

COBE / FIRAS(Data points from Smoot astro-ph/9705101)

OtherCMBexperiments(selection)


Satellites

MicrowaveAnisotropyProbe

launched2001-06-30

140degreesbet.detectors

2001-10-01arrivalatLagrangepointL2spinrate0.464rpm

1:5�10

6kmorbit

precessionrate1rph

2002-04-01�rstfullskyobservation

30%oftheskyeachday

missionlength2yearsatL2

passivecooling<95K

�rstskymapsexpectedend2002

850kg,667kbpsfor16min/day

RELIKT(USSR,Jul1983-Feb1984,estimationofthedipolemoment,

intensitymapat8mm,0.25rpm,orbitperiod.26days)

PLANCK(ESA,2004),PSI/FIRE(US),FarInfraRedSpaceTelescope(ESA),

LargeDeployableRe ector(NASA),RELIKT-2(USSR)

Balloonborne

MAX,Boomerang,MAXIMA,FIRS,MSAM,TopHat,ULISSE,

ARGO,BAM,ACE,BEAST,QMAP

Groundbased

Saskatoon(1987,93,94,95),ACME-HEMT(1988-89,90-91,94),

Python(1990,93),Tenerifegroup(1983,88-99),DASI(1999-2002)

Experimentalresults


Tegmark(2002)

ComputerprogramsforCMBcalculations


CMBFAST

CAMB

�U.Seljak,M.Zaldarriaga

�A.Lewis

�Fortran77(�15000lines)

�Fortran90(�10000lines)

�latestVersion4.0(2000)

�latestVersionMarch2002

�basedoncodeofBertschinger,Ma,Bode

�basedonCMBFAST2.4.1and3.2

�synchronousgauge

�gaugeinvariantvariables

�supportsOpenMP(upto16processors)

Parameters

Computationtimes

b;cdm;�;�;H0

�1min/set

T ;XHe;n

ml�;n

m �

standardgrids�2�10

6sets

�T;zre;xe

�4yr(onsingleCPU)

n;nscalar;ntensor

Sensitivityofthespectrum


050

010

0015

00

l

0

1e-0

9

2e-0

9

3e-0

9

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)(0

.05,

0.05

,0.9

,69)

(0.0

5,0.

15,0

.8,6

9)(0

.05,

0.25

,0.7

,69)

(0.0

5,0.

35,0

.6,6

9)(0

.05,

0.45

,0.5

,69)

(0.0

5,0.

55,0

.4,6

9)(0

.05,

0.65

,0.3

,69)

(0.0

5,0.

75,0

.2,6

9)(0

.05,

0.85

,0.1

,69)

050

010

0015

00

l

0

1e-0

9

2e-0

9

3e-0

9

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)(0

.046

2,0.

2538

,0.7

,50)

(0.0

462,

0.25

38,0

.7,5

5)(0

.046

2,0.

2538

,0.7

,60)

(0.0

462,

0.25

38,0

.7,6

5)(0

.046

2,0.

2538

,0.7

,70)

(0.0

462,

0.25

38,0

.7,7

5)(0

.046

2,0.

2538

,0.7

,80)

(0.0

462,

0.25

38,0

.7,8

5)(0

.046

2,0.

2538

,0.7

,90)

050

010

0015

00

l

0

1e-0

9

2e-0

9

3e-0

9

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)(0

.046

2,0.

1,0.

7,69

)(0

.046

2,0.

2,0.

7,69

)(0

.046

2,0.

3,0.

7,69

)(0

.046

2,0.

4,0.

7,69

)(0

.046

2,0.

5,0.

7,69

)(0

.046

2,0.

6,0.

7,69

)(0

.046

2,0.

7,0.

7,69

)(0

.046

2,0.

8,0.

7,69

)(0

.046

2,0.

9,0.

7,69

)(0

.046

2,1.

0,0.

7,69

)

050

010

0015

00

l

0

1e-0

9

2e-0

9

3e-0

9

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)(0

.1,0

.253

8,0.

7,69

)(0

.2,0

.253

8,0.

7,69

)(0

.3,0

.253

8,0.

7,69

)(0

.4,0

.253

8,0.

7,69

)(0

.5,0

.253

8,0.

7,69

)(0

.6,0

.253

8,0.

7,69

)(0

.7,0

.253

8,0.

7,69

)(0

.8,0

.253

8,0.

7,69

)(1

.0,0

.253

8,0.

7,69

)

050

010

0015

00

l

0

1e-0

9

2e-0

9

3e-0

9

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)(0

.046

2,0.

2538

,0,6

9)(0

.046

2,0.

2538

,0.1

,69)

(0.0

462,

0.25

38,0

.2,6

9)(0

.046

2,0.

2538

,0.3

,69)

(0.0

462,

0.25

38,0

.4,6

9)(0

.046

2,0.

2538

,0.5

,69)

(0.0

462,

0.25

38,0

.6,6

9)(0

.046

2,0.

2538

,0.7

,69)

(0.0

462,

0.25

38,0

.8,6

9)(0

.046

2,0.

2538

,0.9

,69)

(0.0

462,

0.25

38,1

.0,6

9)

1010

010

00

l

0

2e-1

0

4e-1

0

6e-1

0

8e-1

0

Cl, scalar

(0.0

462,

0.25

38,0

.7,6

9)

References


1.COBEhomepagehttp://space.gsfc.nasa.gov/astro/cobe/cobehome.html

2.MAPhomepagehttp://map.gsfc.nasa.gov/

3.PLANCKhomepagehttp://astro.estec.esa.nl/SA-general/Projects/Planck/

4.W.Hu,S.Dodelson:Cosmicmicrowavebackgroundanisotropies.

Ann.Rev.Astron.andAstrophys.(2002)LosAlamose-printArchiveastro-ph/0110414

5.U.Seljak,M.Zaldarriaga:A

lineofsightintegrationapproachtocosmicmicrowavebackground

anisotropies.LosAlamose-printArchiveastro-ph/9603033

6.A.Lewis,A.Challinor,A.Lasenby:EÆcientcomputationoftheCMBanisotropiesinclosedFRW

models.LosAlamose-printArchiveastro-ph/9911177

7.G.F.Smoot:TheCMBspectrum.LosAlamose-printArchiveastro-ph/9705101

8.D.Puetzfeld:AcosmologicalmodelinWeyl-Cartanspacetime:II.Magnitude-redshiftrelation.

acceptedbyClass.QuantumGrav.LosAlamose-PrintArchivegr-qc/0205052

9.D.Puetzfeld:AcosmologicalmodelinWeyl-Cartanspacetime:I.Fieldequationsandsolutions.

Class.QuantumGrav.19(2002)3263-3280LosAlamose-PrintArchivegr-qc/0111014

Documents

dp - puetzfeld.orgpuetzfeld.org/files/gk2002_2.pdf · The cosmic micro w a v e bac kground Dirk P utzfeld Email: [email protected] WWW: . de/~ dp O ver view Motiv ation Historic