1. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #1 Star Formation from Herschel deep surveys B. Altieri, on behalf of PEP (PACS Extragalactic Probe, PI D. Lutz ) GT Key Program consortium GOODS-Herschel (PI, D. Elbaz) OT Key program Elbaz+11, Popesso+11, Rodighiero+11, Mullaney+11

2. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #2 Credit: WMAP –Half of the energy created in the Universe since the CMB has been reprocessed into the IR –Herschel covers the IR peak and pushes into the submillimetre Importance of the FIR & submm

3. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #3 Collaborators (60): Fr, US, G, UK, Gr, It, Can, ESO, ESA 362.6 hours (100m & 160m PACS + 31h SPIRE) GOODS-Herschel ( Herschel Open Time Key Program ) The Great Observatories Origins Deep Survey : far IR imaging with Herschel 1.cosmic SFR density : normal galaxies up to z ∼ 1, LIRGs up to z ∼ 2, ULIRGs to z~4 2.bridge IR and UV up to z ∼ 1.5... 4 3.identify missing obscured AGNs making the missing cosmic X-ray background (30 keV) Herschel: 350 cm Deepest images of the sky in the 2 GOODS fields : 1818 sources down to 1 mJy at 100 m, 2.6 mJy@160m, 5mJy@250m, 8mJy@350m, 10mJy@500m X UV U B V I Z J H K 3.6m 4.5m 5.8m 8m IRS16 MIPS24 radio 2x10 -16 erg/s/cm 2 ~28AB 22AB ~1 Jy 50 Jy 20 Jy 1 2 Jy 70% complete spec z ~30% phot z GOODS-North 100 160 250 GOODS-South 24 100 160 10'x15' 10'x10'

4. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #4 Collaborators (60): Fr, US, G, UK, Gr, It, Can, ESO, ESA 362.6 hours (100m & 160m PACS + 31h SPIRE) GOODS-Herschel ( Herschel Open Time Key Program ) The Great Observatories Origins Deep Survey : far IR imaging with Herschel 1.cosmic SFR density : normal galaxies up to z ∼ 1, LIRGs up to z ∼ 2, ULIRGs to z~4 2.bridge IR and UV up to z ∼ 1.5... 4 3.identify missing obscured AGNs making the missing cosmic X-ray background (30 keV) Herschel: 350 cm Deepest images of the sky in the 2 GOODS fields : 1818 sources down to 1 mJy at 100 m, 2.6 mJy@160m, 5mJy@250m, 8mJy@350m, 10mJy@500m X UV U B V I Z J H K 3.6m 4.5m 5.8m 8m IRS16 MIPS24 radio 2x10 -16 erg/s/cm 2 ~28AB 22AB ~1 Jy 50 Jy 20 Jy 1 2 Jy 70% complete spec z ~30% phot z GOODS-North 100 160 250 GOODS-South 24 100 160 10'x15' 10'x10' 70% complete spec z ~30% phot z

5. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #5 mir and far IR consistent with local SEDs (Chary & Elbaz 01) up to z~1.5 (blue, green dots) at z>1.5: "mid-IR excess" (Daddi +07, Papovich +07) (orange, red dots) Elbaz +10, 11, Nordon +10 The mid-IR excess problem... SED evolution/AGN/k-correction ?... CE01 L IR (Herschel) L IR (from 24m using CE01)

6. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #6 The mid-IR excess problem... SED evolution/AGN/k-correction ?... Elbaz +11 L IR (Herschel) L IR (from 24m using CE01) L IR (Herschel) L 8 (rest-frame from Spitzer)

7. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #7 Elbaz +11 IR main sequence : 2 modes of star formation ?

8. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #8 IR main sequence : the role of SF compactness >3x10 10 L  kpc -2 radio size NVSS & FIRST 20cm: 1" ~ 0.5 kpc res° 13.2  m compactness : 3.6" ~ 1.7 kpc resolution Spitzer-IRS spectroscopy (spatial profile along slit) & IRAC-8mm imaging (Diaz-Santos +10) Elbaz +11

9. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #9 IR main sequence : the role of SF compactness Local L 8 (rest-frame) L IR (IRAS) Elbaz +11 IR8 = L IR / L 8  IR

10. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #10 L8L8 L IR (IRAS) sSFR= SFR / M * (Gyr -1 )  IR R SB =sSFR/sSFR(Main Seq.) IR8 = L IR / L 8 SFR M*M* Galaxies with an excess in IR8, IR surface brightness and sSFR are the same !  high IR8 ~ compact starbursts

11. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #11 SF in distant excess IR8 galaxies is more compact in rest-frame UV HST ACS-B(4350Å) @z~0.7  2700Å HST ACS-V(6060Å) @z~1.2  2700Å HST ACS-I(7750Å) @z~1.8  2700Å

12. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #12 Proto-typical IR SED of Main Sequence and Starburst galaxies Main Sequence Starburst (high IR8, sSFR) Model fit: 2 components, "diffuse ISM" and "star forming region" Range of dust temperatures but ISM range wide T dust (ISM)~ 18 K, T dust (SF)~ 50 K Main Sequence : broad far-IR bump 15 – 50 K, strong PAH features, ISM= 38 %, SF= 62 % SED Starbursts : peaked far-IR bump 45 – 50 K, weak PAH features, ISM= 0 %, SF= 100 % SED Nordon +11

13. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #13 IR8=L IR /L 8 as a tracer of star formation geometry (  mergers) Galliano +08

14. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #14 Improving the bolometric correction for SF galaxies Unique IR SED for all galaxies: main sequence Elbaz +11

15. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #15 ConclusionsTwo Distant (U)LIRGs = normal star-forming galaxies + large Mgas, long-lasting (Gyrs) IR8= L IR /L 8 universal among star-forming galaxies  geometry of SF regions (robust / fragile dust ratio) High IR8 values for compact starbursts with high SFR / M* (mergers) Main Sequence galaxies (disk-like) dominate the cosmic SFR density at all redshifts !  The fall in cosmic SFR driven by the decrease in gas mass not merger rate Starbursts= mergers between late-types, ~10% of cosmic SFR density IR SED for MS and SB galaxies  bolometric correction  LIRG = SB at z~0 but MS at z~1 if M*>5x10 10 M  (ULIRG@z=2, M*>2x10 11 M  ) IR dominated by star formation in AGNs (L X <10 42-44 erg s -1 ) Next: improve SED library by bins in sSFR, IR8, Lir Two modes of star formation

16. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #16 The Σ(SFR)/M ~z relation up to z~1.6 Black points: clusters Magenta points: groups Red star: the Bullet cluster Blue region: field galaxy halos Black points: clusters Magenta points: groups Red star: the Bullet cluster Blue region: field galaxy halos

17. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #17 The Σ(SFR)/M ~z relation up to z~1.6 Conclusions: pre-processing ruled out quenching effect takes place after merger/accretion (likely environmental) Reversal of SFR-density at z> 1.5 Conclusions: pre-processing ruled out quenching effect takes place after merger/accretion (likely environmental) Reversal of SFR-density at z> 1.5

18. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #18 The Σ(SFR)/M ~z relation up to z~1.6 Future: HSC GT1 and hopefully OT2 time to search for proto-clusters + 100h of Herschel/PACS (PI P. Popesso) to observe 8 groups/clusters in the cluster desert at 1.5 < z < 2 Future: HSC GT1 and hopefully OT2 time to search for proto-clusters + 100h of Herschel/PACS (PI P. Popesso) to observe 8 groups/clusters in the cluster desert at 1.5 < z < 2 Cluster desert

19. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #19

21. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #21 Star Formation from Herschel deep surveys B. Altieri, on behalf of PEP (PACS Extragalactic Probe, PI D. Lutz ) GT Key Program consortium GOODS-Herschel (PI, D. Elbaz) OT Key program Elbaz+11, Popesso+11, Rodighiero+11, Mullaney+11

22. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #22 Document title | Author Name | Place | Data doc | Programme | Pag. 22

23. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #23 Searching for buried AGNs with IR8 deboosted from starburstiness X-ray AGNsPower-law AGNs high IR8 : 15%  19% low IR8 : 33%  70% high & low IR8 : ~11%  ~22%

24. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #24 Searching for buried AGNs with IR8 deboosted from starburstiness 2% 17% 25% +15% src with high IR8

25. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #25 what is the redshift by which half of the stars that we see today were formed ? (Peebles 1988, The epoch of galaxy formation) z0 – 2.52.5 – 55 - ∞ votes in 198828 54 4 Marchesini +09 50% z~1 15% z~2 8% z~3 Le Borgne, Elbaz, Ocvirk, Pichon 10  SFR (M  yr -1 Mpc - 3 ) redshift  star (M  Mpc - 3 ) ~85 % ~15% <5% (% age after recombination)

26. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #26 Star Formation from Herschel deep surveys B. Altieri, on behalf of PEP (PACS Extragalactic Probe, PI D. Lutz ) GT Key Program consortium GOODS-Herschel (PI, D. Elbaz) OT Key program Elbaz+11, Popesso+11, Rodighiero+11, Mullaney+11

27. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #27 Collaborators (60): Fr, US, G, UK, Gr, It, Can, ESO, ESA 362.6 hours (100m & 160m PACS + 31h SPIRE) GOODS-Herschel ( Herschel Open Time Key Program ) The Great Observatories Origins Deep Survey : far IR imaging with Herschel 1.cosmic SFR density : normal galaxies up to z ∼ 1, LIRGs up to z ∼ 2, ULIRGs to z~4 2.bridge IR and UV up to z ∼ 1.5... 4 3.identify missing obscured AGNs making the missing cosmic X-ray background (30 keV) Herschel: 350 cm Deepest images of the sky in the 2 GOODS fields : 1818 sources down to 1 mJy at 100 m, 2.6 mJy@160m, 5mJy@250m, 8mJy@350m, 10mJy@500m X UV U B V I Z J H K 3.6m 4.5m 5.8m 8m IRS16 MIPS24 radio 2x10 -16 erg/s/cm 2 ~28AB 22AB ~1 Jy 50 Jy 20 Jy 1 2 Jy 70% complete spec z ~30% phot z GOODS-North 100 160 250 GOODS-South 24 100 160 10'x15' 10'x10'

28. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #28 The ‘infrared main sequence’ for star-forming galaxies Document title | Author Name | Place | Data doc | Programme | Pag. 28 Main Sequence galaxies (disk-like) dominate the cosmic SFR density at all redshifts ! The fall in cosmic SFR driven by the decrease in gas mass not merger rate Elbaz+ 2011

29. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #29 The typical Spectral Energy Distribution of main-sequence and starburst galaxies: 2 modes of star formation Starbursts= mergers between late-types, ~10% of cosmic SFR density 90% 10%

30. Bruno Altieri | Toledo 2011 | 23 Nov. 2011 | vg #30 Conclusions Distant (U)LIRGs = normal star-forming galaxies + large Mgas, long-lasting (Gyrs) IR8= L IR /L 8 universal among star-forming galaxies  geometry of SF regions High IR8 values for compact starbursts with high SFR / M* (mergers) Main Sequence galaxies (disk-like) dominate the cosmic SFR density at all redshifts !  The fall in cosmic SFR driven by the decrease in gas mass not merger rate Starbursts= mergers between late-types, ~10% of cosmic SFR density IR SED for MS and SB galaxies  bolometric correction  LIRG = SB at z~0 but MS at z~1 if M*>5x10 10 M  (ULIRG@z=2, M*>2x10 11 M  ) IR dominated by star formation in AGNs (L X <10 42-44 erg s -1 ) TBD: improve SED library by bins in sSFR, IR8, Lir