1. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari FIR & Sub-mm Astronomy comes of age Herschel Space Observatory Observing Opportunities Mattia Vaccari - University of Padova Alberto Franceschini & Giulia Rodighiero Thanks also to Carol, Jim, Matt, Michael, Seb & all the ISOCAM, ELAIS, SHADES, SWIRE, SPIRE & SCUBA2 folks

2. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Big open question #1 Most massive galaxies are (and ~60% of local mass in stars is in) ellipticals They exist at least up to z ~2 How did massive ellipticals form ? When ? Role of merging ? In situ SF ? (hot issue for decades...)

3. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Big open question #2 Ellipticals and bulge dominated spirals (spheroids) contain BHs Tight correlations exist between BH masses and spheroid masses How does the BH know about its surrounding galaxy ? What is the link between AGN and galaxy activity ? How do they relate with merging events ?

4. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari UV/Opt/NIR FIR/Sub-mm Sky Brightness (nW/m 2 /sr) 1101001000 100 1000 10 1 Wavelength [  m] The FIR & Sub-mm Universe

5. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari The effects of dust extinction and the degeneracy of optical observables Degeneracy is old-fashioned Time for panchromatic SEDs Sanders & Mirabel 1996 Lagache et al 2005

6. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari The integrated background light in the far-infrared and sub-millimeter region of the spectrum is approximately equal to the integrated background light in the optical and UV part of the spectrum. To develop a complete understanding of galaxy formation, this background light must be resolved into galaxies and their physical properties must be characterized. The Cosmic Infrared Background Resolved Into Discrete Sources

7. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari PWV = 1.0 mm PWV = 0.5 mm PWV = 0.2 mm PWV = 0.1 mm PWV ~ Chajnantor 30% PWV ~ Dome C 30% Minier et al 2007 Into Thin Air : FIR & Sub-mm Atmospheric Transmission vs Precipitable Water Vapor Lower atmospheric transmission is generally coupled with higher (sky & instrumental) background and temporal variability

8. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari FIR & Sub-mm : In The Beginning…  IRAS  COBE  Spitzer  Single-Pixel cameras  SHARC@CSO & SCUBA@JCMT & MAMBO@IRAM  And btw : the future doesn’t look too bad either (JCMT, LMT, ALMA, SPICA, FIRI…

9. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  Herschel is an ESA cornerstone mission –spacecraft, launch (scheduled for 31 Oct 2008) and operations provided by ESA –instruments ‘nationally’ funded with international collaborators  Herschel is the first space facility to completely cover this part of the far infrared and submillimeter (60 - 670  m) range –large (3.5 m) aperture, low emissivity (~5%), passively cooled (70-90 K) telescope –cryogenically cooled focal plane science instruments with >3 years lifetime –total absence of atmospheric absorption and emission –full spectral access with low and stable background  Herschel has unique and complementary characteristics –first 4-m class space telescope ever, has much larger aperture than missions with cryogenically cooled telescopes (IRAS, ISO, Spitzer, Akari,…) –larger & colder aperture, better ‘site’, and more observing time than balloon- and air-born instruments (~1000 SOFIA flights per year) –larger field of view than interferometers  PACS - PI : Albrecht Poglitsch, MPE, Garching, Germany –imaging photometry and spectroscopy over 57-210  m  SPIRE - PI : Matt Griffin, Univerity of Wales, Cardiff, London, United Kingdom –imaging photometry and spectroscopy over 200-670  m  HIFI - PI : Thijs de Graauw, SRON, Groningen, The Netherlands –very high resolution spectroscopy over 480-1250 and 1410-1910 GHz (157-625  m) The Herschel Mission

10. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  telescope diameter 3.5 m  telescope WFE 6-10  m  telescope temperature 70-90 K  abs/rel pointing (68%) < 1.5”-3.0” / 0.3”  science instruments 3  science data rate 100 kbps  operational lifetime >3 years  height 9 m  width 4.5 m  launch mass 3300 kg  power 1 kW  orbit Lissajous around L2  launch vehicle (with Planck) Ariane 5  launch date 31 Oct 2008 The Herschel Spacecraft

11. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari The Actual Spacecraft Launch : 31 Oct 2008

12. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  Study the formation and evolution of galaxies in the early universe –how and when did galaxies form? –is there an unknown population of high-z IR galaxies? –star formation rates? bolometric luminosities? –Starburst vs AGN fraction? –‘connect’ near-IR and sub-mm galaxies  Study the formation of stars and physics of the interstellar medium –how do stars form out of the interstellar medium? –circulation/enrichment of the interstellar medium - astrochemistry –detailed studies of nearby (resolvable) galaxies - templates  Study cometary, planetary, and satellite atmospheres –history of the solar system –pristine material in comets –important water lines Herschel Main Science Objectives The Young & Cold & Dusty Universe

13. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  PACS - Photodetector Array Camera and Spectrometer –PI : Albrecht Poglitsch, MPE, Garching, Germany –imaging photometry and spectroscopy over 57-210  m –2 bolometer arrays for photometry, 2 stressed Ge:Ga arrays for spectroscopy  SPIRE - Spectral and Photometric Imaging Receiver –PI : Matt Griffin, University of Wales, Cardiff, United Kingdom –imaging photometry and spectroscopy over 200-670  m –3 bolometer arrays for photometry, 2 bolometer arrays for spectroscopy  HIFI - Heterodyne Instrument for FIRST –PI : Thijs de Graauw, SRON, Groningen, The Netherlands –very high resolution spectroscopy over 480-1250 and 1410-1910 GHz –SIS and HEB mixers, auto-correlator and AOS spectrometers  University of Padova Involvement –Alberto Franceschini : SPIRE Co-I –Giulia Rodighiero : PACS High-z Science Consortium Member –Mattia Vaccari : SPIRE Associate Scientist & ICC Scientist Herschel Instruments

14. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  Photometry –PACS - simultaneous 2 colour fully-sampled (0.5F ) imaging with FOV 1.75x3.5 arcmin and R~2.5 centred at 75/110 and 170  m –SPIRE - simultaneous 3 colour 2F imaging with FOV 4x8 arcmin and R~2.5 centred at 250, 350, and 500  m –for larger fields ‘on-the-fly’ mapping, mosaicing –sensitivity is somewhat wavelength and observing mode dependant, very roughly 1mJy - 1  - 1 hour, confusion limit is important  Spectroscopy –PACS - 5x5 spatial x 16 spectral pixels, FOV 0.8 arcmin, R~1000 –SPIRE - FTS spectro-photometry/scopy, R ~20-100, FOV 2.6 arcmin –HIFI - heterodyne spectroscopy with R up to 10 7, 2 orthogonal polarisations, 4000 spectral channels per polarisation, single pixel on the sky, mapping by ‘on-the fly’ or mosaicing observations Herschel Observing Capabilities

15. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  - Lifetime > 3 yrs  - Launch in 2008 - Orbit at L2  - Telescope - 3.5-m diam, T < 90 K, em. ~ 4%  (the first 4-m telescope in space)  Instruments  - PACS Spectrophotometry 57 - 210  m  - SPIRE Spectrophotometry 200 - 670  m  - HIFI Heterodyne 480 - 1250 and 1410 - 1910 GHz  Main Science goals  - Formation and evolution of galaxies in the early universe  - Formation of stars, physics and chemistry of the ISM  - Comets, planets: bodies and atmospheresHERSCHEL

16. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari PACS

17. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari PACS

18. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari 3-band Imaging Photometer - 250, 360, 520  m (simultaneous) -  ~ 3 -4 x 8 arcmin field of view -Diffraction limited beams (17, 24, 35”) Imaging Fourier Transform Spectrometer -200 - 670  m (complete range covered simultaneously) -2.6 arcmin field of view -  = 0.04 cm -1 (  ~ 20 - 1000 at 250  m) SPIRE Observing Capabilities

19. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari SPIRE Detector Arrays 200 – 325  m 37 detectors 315 – 670  m 19 detectors Spectrometer 8 arcmin Photometer 500  m 43 detectors 350  m 88 detectors 4 arcmin  Sets of detectors with exactly overlapping beams on the sky 250  m 139 detectors  Beam FWHM

20. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Chopping 126” and nodding, using detector sets A, B, C7-point jiggle mapAngular step  ~ 5”Total flux and position fittedCompared to single accurately pointed observation, S/N for same total integration time is only degraded by ~ 20% at 250  m ~ 13% at 360  m ~ 6% at 520  m  Photometer Observing Modes Point-Source Jiggle Photometry

21. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Telescope pointing fixed or in raster mode Chopping ± 2 arcmin 64-point “jiggle” pattern for full spatial sampling Available FoV = 4 x 4 arcmin Photometer Observing Modes Field Jiggle Map

22. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Most efficient mode for large-area surveys Telescope scans continuously at up to 60”/sec. Scan parameters optimised for full spatial sampling and uniform distribution of integration time Map of large area is built up from overlapping parallel scans Overlap region 235” 12.5 o Photometer Observing Modes Scan Mapping

23. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Herschel Focal Plane ZZ SPIRE Spectrometer Field HIFI Field YY SPIRE Photometer Field PACS Field Y Z X Sun Sunshield Telescope Primary Mirror Focal Plane Coordinates Spacecraft Coordinates

24. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Estimated Sensitivity : Photometry (5  1 hr) Point source/ sparse map (7-point) Scan map Jiggle map

25. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari FTS Spectral Line Resolving Power (Ds = 0.04 cm -1 )

26. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari FTS Spectrophotometry Resolving Power (  = 1 cm -1 )

27. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Estimated Sensitivity: Line Spectroscopy (5  1 hr) Point source/ sparse map Fully-sampled map  = 0.04 cm -1

28. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Estimated Sensitivity: Spectrophotometry (5  1 hr) Point source/ sparse map Fully-sampled map  = 1 cm -1

29. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Herschel Reflector Emissivity (Fischer et al., Applied Optics, 43, 3765, 2004) SPIRE range

30. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Herschel AO Schedule (31 Oct 2008 Launch) Overall (3-yr Baseline Mission) Observing Time Breakdown : ~ 1000 days ~ 20000 hrs Guaranteed Time (GT) = 32% & Open Time (OT) = 68% GT = 30% each to 3 PIs, 7% to HSC, 3% divided between 5 Mission Scientists  Commissioning, Performance Verification & Science Demonstration L - L+6m  Routine Science Operations L+6m - L+42 m  GT & OT Key Projects AO Issue 01 Feb 2007  GT Key Projects Proposal AO Deadline 05 Apr 2007 (~ 5000 hr)  GT Key Projects Results Announcement 05 Jul 2007  OT Key Projects Proposal AO Deadline 25 Oct 2007 (~ 5500 hr)  OT Key Projects Results Announcement 28 Feb 2008  GT & OT Cycle 1 Projects AO Issue 28 Feb 2008  GT Cycle 1 Projects Proposal AO Deadline 03 Apr 2008 (~ 1000 hr)  GT Cycle 1 Projects Results Announcement 05 Jun 2008  OT Cycle 1 Projects AO Deadline Late 2008 (~ 5000 hr)  GT & OT Cycle 2 Projects AO Deadline Late 2009 (~ 500 hr + 3000 hr)  Extra Time (0.5 yr “expected” extended mission) Later (~ 3000 hr)

31. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari  University –Alberto Franceschini : SPIRE Co-I –Giulia Rodighiero : PACS High-z Science Consortium Member –Mattia Vaccari : SPIRE Associate Scientist & ICC Scientist –Gabriele Mainetti : newly hired PhD student  Observatory –Gianfranco De Zotti : SPIRE Consultant –Pasquale Panuzzo (2003-2006) : SPIRE ICC Scientist  Main focus is on high-z galaxy studies through a coordinated program of PACS GT (PEP) and SPIRE GT (HERMES) surveys and on the PACS & SPIRE Instrument Control Centers (ICCs)  PEP + HERMES ~ 1500 hr and arguably the largest single space astronomy project ever (at a very reasonable 50,000 Euros/hr) Padova Involvement

32. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Herschel EG GT Survey Wedding Cake http://astronomy.sussex.ac.uk/~sjo/Hermes/FieldsFinal.pdf http://astronomy.sussex.ac.uk/~sjo/Hermes/FieldsFinal.pdf NameAreaField PACS Time SPIRE Time 70110170250350500 -deg^2 - hr mJy Clusters- - 80100 Level 10.04 GOODS-S 23010+301.0 3.34.04.6 Level 20.04 GOODS-N 27102.02.83.06.78.19.2 Level 30.25 GOODS-S 34252.26.26.710.512.714.5 0.25 Groth Strip 34252.26.26.710.512.714.5 0.25 Lockman 34252.26.26.710.512.714.5 Level 42 COSMOS 110506.09.810.521.125.529.1 2 XMM-LSS 11050189.810.521.125.529.1 Level 510 Spitzer 1852001816.918.023.628.532.5 Level 650 Spitzer -15018-120617484 Time : PACS (659) SPIRE (850) Harwit (10) (Spitzer Depths)

33. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Money-wise…  Herschel budget envelope is a pretty round billion Euros  This means a ~ 130 million Euros Italian contribution  Nominal mission is 20,000 hr of science observing  Herschel time sells at a very reasonable 50,000 Euros/hr

34. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Where do we go from here?  Herschel will launch on 31 Oct 2008 but in the meantime –EARA Herschel WorkShop (18-19 Feb @ IAP) –ASI/INAF Herschel Open Time WorkShop (10-12 Mar @ ASI) –Open Time AO Issue & Deadline expected in March & Late 2008  Look up info & watch out for updates at http://herschel.esac.esa.inthttp://herschel.esac.esa.int  Note that SCUBA2@JCMT (450/850  m) and AZTEC@LMT (1.1 mm) are also coming online sometime over the next year or so  Well, looking forward to launch…

35. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Thanks! Well, looking forward to launch… Mattia Vaccari mattia@mattiavaccari.net www.mattiavaccari.net

36. AstroPizza 16 Jan 2008 Herschel Mattia Vaccari Thanks! “Don't clap too loudly - it's a very old world” Tom Stoppard, Rosencrantz and Guildenstern are dead Mattia Vaccari mattia@mattiavaccari.net www.mattiavaccari.net