HIGH REDSHIFT OBJECTS. Alain Omont (IAP)

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1 Post-Herschel FIR (20-500µm) science objectives HIGH REDSHIFT OBJECTS. Alain Omont (IAP) A deep spectral window into the young Universe complementary to JWST and ALMA Thanks to: F. Bertoldi, P. Cox, C. De Breuck, E. Falgarone, D. Flower, R. Neri, G. Pineau des Forêts D. Leisawitz and other contributors to U. Maryland workshops & SAFIR, SPECS, SPICA & SIRCE projects

2 Post-Herschel FIR (20-500µm) science objectives: High Redshift Objects Various redshift ranges in galaxy/agn evolution (z ~ ) Key astronomical issues Present near-future high-z FIR-submm achievements Between JWST & ALMA: drawbacks & advantages High-z capabilities of a cryogenic, 8-10m telescope - Galaxy formation: H 2 lines & PAH at z > 5 - Galaxy evolution, z ~ : spectral lines (+dust) - AGN environment & evolution High-z objectives for possible smaller telescopes Need for angular resolution prepare space interferometry Submm all-sky survey OUTLINE

3 z D phot (Gpc) ~ 300 million ~ 3.5 billion z ~ 7 20? - Reionization PopIII stars +1st galaxies -Formation of 1st galaxies Pop. II stars - First AGN z ~ 4 7 : Current frontier - Galaxies and QSOs detection - End of reionization z ~ 1.5-4: - Peak of star formation submm sources + LBGs - Peak of QSO activity - Proto-cluster formation z ~ : Final phase of active star formation - ISOCAM sources - Weak X-ray AGN - Cluster formation

4 High-z FIR Objects ULIRG X LIRG Very steep SED «inverse K corr.» Spiral PAHs X z= 10 1µm 10µm ///////////////////100/////////////////// 1000 z= 5 1µm 10µm ///////////////////100/////////////////// 1000 z= 2 1µm 10µm ///////////////////100/////////////////// 1000 z= 0 /////////////////////////////////////////// X

5 High redshift objects KEY ISSUES Cosmology Confirmation of standard ΛCDM model and parameters Identification of dark matter and energy Other issues of fundamental physics: inflation, etc. Formation and evolution of galaxies and structures Formation of first stars and galaxies; reionization Merging history History of star formation Formation of clusters and proto-clusters of galaxies Formation and evolution of massive black-holes Formation and growth Physics of their environment Relation with their host galaxy; parallel evolution Merging of massive black-holes

6 Main present near-future µm high-z achievements Extragalactic background and resolution into sources, Energy generation history COBE, ISO, SCUBA SIRTF, Astro-F, Herschel. Star formation history up to z ~ ISO, SCUBA SIRTF, Astro-F, Herschel, ALMA, JWST ULIRGs full census and properties SCUBA Herschel, ALMA, Astro-F, WISE Detection of galaxies at reionization epoch z ~ 20 ALMA, JWST Details of galaxy astrophysics/evolution up to z ~ 3-5 ALMA, JWST AGN/star-formation connection SZ/Ostriker-Vishniak effect from reionization ALMA, etc.

7 SCUBA(-MAMBO) census of high-z ULIRGs SCUBA(-radio) redshift distribution Chapman, Blain, Ivison, Smail 2003 Take advantage of steep submm spectrum Account for the whole submm background z at Keck for radio ones (~50%) (weak AGN?) History of star formation up to z~3-4 Small but uncertain number at z>4 CO detected at IRAM-PdB in 6-8 (Neri et al 2003) SCUBA (+MAMBO) submm counts Star-formation rate

8 Main present near-future µm high-z achievements AGN/star formation connection ISO/SWS: disentangling AGN & starburst lines in ULIRGs ISOCAM: strong correlation between 15µm & X-Ray (z~0.5-1) MAMBO/ IRAM-30m & SCUBA: Dust detection in ~70 high-z QSOs ( z=6.4) and ~15 radiogalaxies L FIR ~ Lo, starburst or AGN heating IRAM PdB (+OVRO, Nobeyama): CO detection in 15 z>2 QSOs or radiogalaxies z = 6.4 starburst mass of H 2 gas up to Mo, T up to 100K, n up to >10 4 cm -3 AGN/starburst connection in ~50% of SCUBA galaxies Many extensions of ISO work with SIRTF, Astro-F, WISE, Herschel Detailed extension of IRAM work with ALMA up to z~15

9 CO detection at z = 6.42 at VLA & IRAM-Plateau de Bure

10 CO detection at z = 6.42 Bertoldi et al. 2003a, Walter et al 2003, Bertoldi et al. 2003b

11 Between JWST & ALMA: drawbacks & advantages JWST: extraordinary sensitivity, peak of stellar emission high angular and spectral resolution ALMA: enormous advantage of steep submm dust & CO emission high velocity (heterodyne) & spatial (interferometry) resolution µm: - Large fraction of (starburst) galaxies energy emitted or redshifted - Crucial for dust enshrouded star formation and AGN - Main ISM atomic lines, H 2, redshifted PAH bands - Very sensitive detectors, weak zodiacal and Galactic background - No galaxy confusion limits for spectroscopy But: - Poor resolution with single apertures, very difficult interferometry - Strong galaxy confusion - Difficult heterodyne - No «inverse K correction» for dust and line emission

12 High-z FIR Objects ULIRG X LIRG Very steep SED «inverse K corr.» Spiral PAHs X z= 10 1µm 10µm ///////////////////100/////////////////// 1000 z= 5 1µm 10µm ///////////////////100/////////////////// 1000 z= 2 1µm 10µm ///////////////////100/////////////////// 1000 z= 0 /////////////////////////////////////////// X

13 µm OIII OI OIII NII OI CII

14 Between JWST & ALMA: drawbacks & advantages JWST: extraordinary sensitivity, peak of stellar emission high angular and spectral resolution ALMA: enormous advantage of steep submm dust & CO emission high velocity (heterodyne) & spatial (interferometry) resolution µm: - Large fraction of (starburst) galaxies energy emitted or redshifted - Crucial for dust enshrouded star formation and AGN - Main ISM atomic lines, H 2, redshifted PAH bands - Very sensitive detectors, weak zodiacal and Galactic background - No galaxy confusion limits for spectroscopy But: - Poor resolution with single apertures, very difficult interferometry - Strong galaxy confusion - Difficult heterodyne - No «inverse K correction» for dust and line emission

15 20µm - 500µm Studies at z ~ (end of) reionization epoch are possible, including spectroscopy Detailed studies of galaxies and AGN at z ~ are easy WITH A LARGE (8-10m) SINGLE APERTURE TELESCOPE e.g. SAFIR ( H. Yorke) - Galaxy formation: (pristine) H 2 lines & PAH bands at z > 5 - Galaxy evolution, z ~ : MIS/star-formation lines - AGN environment & evolution

16 SAFIR capabilities in comparison SAFIR will offer orders of magnitude improvement in spectroscopic sensitivity point source detectivity ~ 10 4 ~ 10 2 R=1000 no confusion limits for spectroscopy! Also large increase in the number of pixels

17 8-10m High-z point sources, continuum sensitivity Detection of large starburst galaxies at z ~10 L* galaxies at z ~ 5 Confusion limited at λ>100µm At least similar sensitivity for starburst PAH features z determination SPICA Gravitational lens magnification - a few % of high z sources - factor ~ 2-10 ( 10-15) higher z or fainter objects * z ~ 5-10 range well studied * lens exploration of higher z *structures well traced at smaller z Arp 220 at z=10 M 82 at z=10 M 51 at z=5

18

19 8-10m Fine structure lines : CII, OI, OIII, NII, SiII, FeII, ArIII, etc. Enormous sensitivity gain vs SIRTF/Herschel Often extinction free, but not in Arp 220 some lines in absorption Cooling of the ISM; T and n diagnostic; ionization Element abundances chemical evolution of galaxies Width rotation, dynamical mass (but no heterodyne and spatially unresolved) Redshift determination tracing structures (high source density, large field of view) Combination with ALMA: submm molecular lines: CO, etc. IR molecular lines: H 2, HD, H 2 O, OH, etc. chemistry, isotopes Dust spectroscopy dust composition at all z in various environments

20 µm OIII OI OIII NII OI CII

21 8-10m Rotational H 2 lines J = 4 para H 2 Need warm molecular gas : T > 100 K because first line, J 2 0 (28µm) T up ~500 K Detected in local galaxies by ISO/SWS, surprisinly strong and extended, e.g. in non-starburst NGC 891 M H2 ~ Mo, T ~ 170 K Valentijn & van der Werf µm J = 3 ortho H 2 17 µm J = 2 28 µm J = J = 0 Detectable in massive galaxies (M H2 > 10 9 Mo) up to z = 10! (J 1148 at z=6.4 has M H2 ~ Mo) Detailed view of warm molecular gas at all redshifts up to z ~ 5 (PDRs, shocks, turbulence?) [H2EX for local H2 up to z~1].

22 8-10m Possibilty of detecting pristine H 2 in galaxy formation Detection of H 2 at z~10 requires about 10 9 Mo of warm H 2 H 2 cooling is crucial for the formation of the first stars and galaxies from pristine gas without metals However, typical (dust-free) «pristine» H 2 /H ~ 10-3, and masses of first condensations (Pop. III stars?) are too small for H 2 lines to be detectable Larger condensations can later collapse at T~10 4 K; however, their subsequent physics and that of H 2 are terribly complex and uncertain : photodissociation feedback of H 2, but maybe additional H 2 formation?? Detection of pristine H 2 is thus possible but uncertain It could be helped by (strong) lensing Anyway, large (starburst) galaxies with metals already abundant at z~5 (Bremer et al 2003) ; maybe reionization agents; H 2 detectable z=10 ( 15 with lensing)

23 8-10m High-z AGN Mid-IR (rest-frame), high ionization lines provide powerful extinction-free diagnostics of dust-enshrouded AGN : [MgV] 13.5, [OIV] 26, [ArV] 13, and [NeV] 14 and 24µm Very strong, detectable at very high z Very good discrimination AGN/starburst combining with HII lines: soft FeII,III, NeII, SIII, hard SiIV, NeIII, OIII AGN Broad lines dynamics of nuclear toroids mass of highly buried black-holes HII understanding correlation mass-bh/mass-bulge accretion history of universe (with X-ray missions) + Dust composition around high-z AGN

24 Interest of smaller missions at high redshift e.g. cold 3.5m at L2: SPICA ( T. Nakagawa) Severely limited by confusion for point source continuum But still very impressive spectral capability for PAH, fine structure & H2 lines, dust composition, including peak of starburst/agn activity at z ~ 2 However cannot tackle galaxy-formation/reionization epoch at z > 5 SPICA SPICA Arp 220 at z=10 H2EX (1.3m) is limited to the local universe F. Boulanger

25 Submillimeter whole sky survey V. Gromov e.g. SIRCE 2m Benford et al. Severely limited by confusion ( more ambitious 3.5m Lamarre) a few 10 7 sources at 500 µm >~ 10 mjy mostly typical SCUBA sources at z <~ 3 full sky view/structure of strong starburst/(agn) activity Complete census (~10 5 ) of strongly lensed ULIRGs A small, uncertain ( ?) fraction of sources at z > 7 : - strongly lensed - and/or AGN extremely luminous at λ ~ 60 µm SZ sources Main key special interests - First massive (dusty) condensations in the Universe - Very rare extremely lensed ULIRGs, especially at z>7, for ALMA, JWST, etc. - Maybe a few (lensed) strong radiosources at z~10 for tracing HI (21cm) at reionization?

26 Need for angular resolution in the far infrared Lack of angular resolution in the far-ir/submm is one of the Main drawbacks of single apertures compared to ALMA, JWST At high z, 1 arcsec = 8-4 kpc at z = 2-10 no access to galactic structure no discrimination of AGN environment source confusion in submm no resolution of lensed images Need for sensitive space interferometry, to be combined with high spectral resolution, e.g. SPECS ( Leisawitz) - highly demanding, long-term goal - need to begin to design, build and test the technology

27 Conclusions Sensitive far-infrared capabilities are mandatory to understand the high redshift Universe in complement of JWST and ALMA, for: - Dust-enshrouded star formation - Properties of the ISM, energy balance, chemical evolution,etc - AGN/host-galaxy connection & dust-enshrouded AGN - Dust properties - Galaxy formation and the role of pristine H 2 A large (8-10m) cold telescope has an enormous gain of capabilities, and is required for the most demanding objectives, especially at z >~4 A smaller (3-4m) aperture may achieve important goals Space FIR interferometry will be required to achieve high angular resolution combined with high spectral resolution A submm sky survey will trace star-formation peaks in whole Universe and increase ALMA/JWST discovery power by revealing unique (lensed) dusty sources One may expect seredenpitous discoveries from the enormous gain of capabilities of such future missions

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