45 years of developments around the CIB

1967-2012

Jean-Loup PugetInstitut d’Astrophysique Spatiale

CNRS, Université Paris Sud

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- from CIB to CIB anisotropies- early interest and predictions for the Cosmic Backgrounds- the search for the CIB-evolution of

the ideasthe technologythe data analysis

leading to the observations- what to we hope to learn today Herschel, Planck, SPT, ACT,…

Cosmic backgrounds: CMB, CIB, Gamma,…

• UV redshifted in near IR cosmic background– following the observation of the CMB (1965), work developed on the cosmic backgrounds at

other frequencies– one key “astrophysical cosmology” question was

“where is integrated radiation from the nucleosynthesis of the heavy elements we see today”– Partridge and Peebles 1967

“Are young galaxies visible ?”

(ApJ 148,377) , young galaxies

700 times more luminous than

the milky way, z =10-30

Sciama and Rees 1967

(ApJ 147, 868) heavy elements

detectable or not in the E.G.M

• mid IR line cosmic background• FIR cosmic background20/04/23

Growing interest for a FIR redshifted in submm cosmic background (1/2)

– F. Low The Infrared-Galaxy Phenomenon 1970 (ApJ 159, L173)– 50-300 µm observations of the Galactic center and NGC1068 and M82

(2 1012 and 6 1011 Lo) by Franck Low and H. Aumann 1970, (ApJ 162, L79)

– in 1972 the Fundamental panel of ESRO (not yet ESA !) asked me a report on what can space observations bring to cosmology and fundamental physics and I stressed the potential measurements of the cosmic backgrounds

– the driving questions were two fold: • the opacity of the universe to ultra high energy particles and photons

• learning about the early stages of galaxy formation and the history of nucleosynthesis

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predictions from a report to ESRO (1972)

windows in foregrounds

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Puget J.L. 1972, report to the fundamental physics panel of ESRO

CMBEBL / CIB

ZodiZodi

CIRES project

Growing interest for a FIR-submm CB (2/2) – Setti and Woltjer: Infrared Background and Universal Cosmic Rays 1971 (Nature Phys Sc 231,

57)

– J.L. Puget, F.W. Stecker, J. Bredekamp :

Photonuclear interactions of ultrahigh

energy cosmic rays and their astrophysical

consequences1976, (ApJ 205, 638),

F.W. Stecker, J.L. Puget, G. Fazio

Cosmic far infrared background at high galactic

lattitudes 1977, (ApJ let 214, L 1)

the relative contribution to FIR

luminosity from

galactic nuclei vs star formation

remained unclear for 20 years

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1994

1996

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predictions of the anisotropies of the CIB Not only the SED of the CIB but its angular power spectrum was

predicted to be a powerful tool to explore the star formation history in the universe

R. Bond, B. Carr and C. Hogan 1986 (ApJ 306, 428), 1991 (MNRAS) , D. Scott and M. White (A &A 346,1), Z. Haiman and L. Knox 2000 (ApJ)

This is still to come !

In the 80s it was not clear what was the best strategy to search

the CIB for two reasons:- what fraction of the UV stellar energy was absorbed by dust and re-

emitted in the FIR ? (near IR or FIR CIB ?) - COBE-DIRBE was aiming at both - in the e.m. spectrum where are the best extragalactic “windows”

between the foregrounds ? - solar system : zodi cloud scattering solar radiation, zodi emission

- interstellar dust emission in the FIR

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high latitude sky emission

21 Sept 2010 - Orsay Hervé Dole, IAS - HDR - la nuit n'est pas noire

8Leinert et al., 1997, A&ASS

integrated emission of galaxies: visible vs infrared output

• the heavy elements (and associated dust) abundance in the universe is increasing with time

• a naïve view would thus predict a decreasing FIR/visible ratio with redshift

• a few galaxies had been shown to have a large ratio but the bulk of the galaxies were expected to have rather small one

(a few percent)

• some marginal measurements (rocket from M. Harwit’s group and balloon observations by Frank Low near the galactic center and Olthof and van Duinen along the galactic ridge of the Milky Way had shown signs of the strong diffuse FIR emission which were not well accepted

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FIR diffuse galactic emission was measured in a balloon experiment (AGLAE) using 2K cooled bolometers with NEP of 2 10-14 W/ rt Hz- 40% of the luminosity of our galaxy comes out in FIR - IRAS showed that 1/3 of the energy output of galaxies in the local universe comes out in the FIR (Soifer,Neugebauer,Houck 1987,ARAA 25,187)

-IRAS also found a class of luminous star burst IR dominated galaxies (IRAS 10214 was at the time the second most luminous object in the universe)

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Serra, et al, 1978, (ApJ 222, L21, ), 1979 Serra et al (A&A 50,247), Gispert, et al 1982, (A&A 106,293)Caux et al 1984 ( A&A 137,1)

SED and luminosity function of infrared galaxies

• the mid infrared emission from the ISM in our galaxy and in other galaxies was interpreted as due to out of equilibrium emission by very small grains and PAHs (Puget, Leger 1989 ARAA, 27,161)

• the PAHs molecules emit mostly at 6-9 and 12-15 µm

• ISO detected a large number of galaxies at 15 µm with a peak around 1 mJy which could only be due to the redshifted 6-9 µm emission of a strongly evolving population of luminous galaxies (1011 Lo) at z about 1

• this was implying a surprising result that the IR/visible output ratio was incresing with redshift

Lagache et al 2003 (MNRAS, 338,555), Lagache, Puget, Dole 2005 (ARAA 43 727)

• later SPITZER was shown to be affected by a similar phenomenon at 24 µm (E. Le Floc’h, H. Dole)

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• High |b| average: Td=17.5 K, NH)250m=10-25 cm2 (Boulanger et al 1996 A&A 312, 256)

• Interstellar Cirrus spectrum for a column density of NH=1020 cm-2

IRAS/COBE/ISOIRAS/COBE/ISO

IRAS

DIRBE

FIRASISO

CIB

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– Detect LIRGs and ULIRGs up to z~3

PAH features passing through the filter

First results:- SWIRE, Guaranteed time obs., FLS- L= 5 1011-1014 L @ z=1-3

- zmed ~1 (~30% z>1.5)- Starburst. At high z,

SFR>500M /yr

(e.g. Lonsdale et al. 04, Le Floc’h et al. 04, Yan et al. 04, 05, Bell et al. 05)

Galaxies at z>1 : SPITZER (24 m)

Caputi et al. 2005

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z < 0.3

z < 2

z < 1.3

z < 1

z < 0.8

Predictions for Redshifts

Lagache, Dole, Puget et al, 2004, ApJS, 154

For S24 < 0.2 mJy: ~30% of z > 2 galaxiesbimodal contribution:

• 0.3 < z < 1 (11 to 13 µm features) peaks at 0.5 mJy

•1.6 < z < 2.5 (6 to 9 µm features) peaks at 0.2 mJy

•min contribution 1.1 < z < 1.6

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star formation history and CIB: implications of this evolution of our understanding of galaxy evolution

• normal galaxies emit typically one half of their energy in the mid and FIR (large dust grains + VSG-PAHs)

• the FIR/visible ratio increases from z=0 to 1

• the L* of the galaxies dominating the integrated emission increases with redshift (by one order of magnitude from 0 to 1)

• the visible light traces the old low mass stars, the FIR traces the UV of the massive stars absorbed by dust thus the star formation rate

• the FIR and submm CIB traces the star formation rate and should peak around 150 µm and the best wavelength to detect it is near the minimum between the ISM emission and the CMB (300 µm).

• the near IR CIB could trace the very early galaxies near reionization (Ly alpha at z=10-15) which could be detected near the minimum between the zodi scattering and emission (2-3 µm)

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the detection of the CIB with FIRAS

• detecting an isotropic background is notoriously difficult; astronomers like to do differential measurements not absolute ones

• although on COBE the DIRBE experiment was planned for the detection of the CIB and the FIRAS was planned to measure the CMB and its main foreground spectra (ISM dust) it seemed in the mid 90s the best instrument for the detection for the CIB

• absolute measurements means black bodies filling the beam to calibrate and excellent control of straylight from far side lobes

•

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• the problem was not the sensitivity of FIRAS but the component separation problem, remember that the first CMB spectrum with 104 signal to noise shown at the ASS in Washington was with 7 minutes of data !

• the NEP of the 4 bolometers was about 10-14 W/rt Hz

• but FIRAS was a double difference polarizing FTS spectrometer with a very large throughput

• two schools of thinking were opposed on this question:– use of the COBE data alone because the astrophysical data were not controlled well

enough

– use of a tracer of the diffuse ISM at high latitude (HI 21 cm survey with very good correction for far side lobes contribution:

the Burton & Hartmann Dwingeloo survey)

- for the near IR the main problems were the faint stars and the zodiacam scattering and emission

-

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• The dust/gas correlation at high Galactic latitude, F. Boulanger et al 1996, (A&A 312, 256).

• Tentative detection of a cosmic far-infrared back-ground with COBE, J.L. Puget et al : 1996, (A&A 308, L5), Fixsen et al 1998 (ApJ 508 523)

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CIB: Les fluctuations

• Distribution spectrale des galaxies IR:

• Redshift: différentes contributions aux différentes => Décorrélation des fluctuations d’une à une autre

z= 0.1, 0.5, 1, 3, 5, 10

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modèle: CIB SED et contributions

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H. Dole

Zodiacal scattered and emitted spectrum

Interstellar at high latitude

COBE DIRBE and FIRAS residuals after foregrounds removal

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quelles galaxies contribuent à l’EBL ?

20/04/23Lagache, Puget, Dole, 2005, ARAA

x3

spectre de galaxie infrarouge redshifté

From M. Griffin

Stacking w/ S24>0uJy

Cosmic Infrared Background

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Dole et al 2006, A&A 451, 417

Extragalactic Background Light

COB CIB

COB/CIB~1.0

COB~20 to 35

CIB~24 to 27

Dole et al., 2006, A&A, 451, 41720/04/23

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The 6 fields studied by Planck for CIBnote that Planck HFI has 52 bolometers with NEP 10-17 W/rt Hz

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evolution of galaxies:luminosity function vs mass function

• The luminosity function shows rapidly increasing L* with redshift (Bettermin, 2010)

• at z> 0.5 the FIR luminosity per comoving volume becomes larger than the optical-UV one

• the FIR traces the star formation not the stellar mass already formed

• so far up to z around 3 the FIR still dominates the radiation output

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Open questions

• what is the redshift at which the FIR per comoving volume start to decrease sharply ?

• Why the star formation rate is not high within the baryonic matter in collased DM halos of 109 Mo near the reionization redshift ?

• says differently why Kennicut’s law breaks down at high z ?• these questions are difficult to answer because summ observations

lack sensitivity and resolution to find the very distant FIR galaxies (except ALMA !)

• the CIB anisotropies might give us the answers before these ALMA deep surveys are carried out: Planck, ACT, SPT,….

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CIB opacity to TeV gamma rays

Photon-photon interaction can produce pairs if E . > 2 (me c2 )2

1 TeV 1eV or 1 µmFlares have been observed in 6 Blazars by HESS.The analysis of the absorption in their spectra gives

constraints on the CB in the optical and IR Can be done to get an absolute upper limit on the CB

at a given frequency or assume a shape and give a limit on its normalization.

This method is very useful when deep counts are already available. The Gamma rays give a tool to check if there is or not a missed component

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modèle: CIB SED et contributions

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