64 th Symposium June, 2009 John Pearson NASA Herschel Deputy Project Scientist Jet Propulsion Laboratory THE HERSCHEL SPACE OBSERVATORY, OPENING THE FAR INFRARED

2 64 th Symposium June, 2009 John Pearson - What is Herschel The Herschel Space Observatory (Herschel) Named for Wilhelm Herschel –Discoverer of Infrared radiation First comprehensive far infrared observatory in space Largest space based mirror to date Successfully launched on 14 May 2009 at 13:12 UTC Together with Planck onboard an Ariane 5 ECA from Europe's spaceport in Kourou, French Guiana Three instruments with 2500 Liters of superfluid He MISSION END: LAUNCH MASS:3400 kg MISSION PHASE:Commissioning

3 64 th Symposium June, 2009 John Pearson - Launch of Herschel & Planck 14 May 2009 at 13:12 UTC Together with Planck onboard an Ariane 5 ECA

4 64 th Symposium June, 2009 John Pearson - Why Go to Space 1/2? Typical transmission from Mauna Kea with 1mm H 2 O, 45 o R = 5000 Typical transmission from SOFIA (~14km) with 1µm H 2 O, 45 o R = THz 0.5 THz

5 64 th Symposium June, 2009 John Pearson - Why Go To Space 2/2? Thermal radiation from atmosphere and ambient telescopes is much brighter than the majority of the Far IR Universe –300K observation is like optical astronomy during the day! Herschel mirror is passively cooled to ~78K –Significant reduction in background relative to the Ground or even SOFIA Space can be a very stable thermal environment –Much easier too control many systematic effects on the experiment –Orbit L2 is away from Earth and Moon so that the Sun is always on one side  Telescope and cryostat always see cold space

6 64 th Symposium June, 2009 John Pearson - L2 Orbit Stable point Goes with Earth Around Sun loose Orbit no shadow

7 64 th Symposium June, 2009 John Pearson - Herschel Specifications telescope diameter 3.5 m telescope WFE 6  m telescope temp ~78 K abs/rel pointing (68%) < 3.7" (1.5")/ 0.3" science instruments 3 science data rate 100 kbps operational lifetime >3 years height 9 m launch mass 3400 kg power 1 kW orbit Lissajuous around L2 launch vehicle Ariane 5 CTA (15 February 2007)

8 64 th Symposium June, 2009 John Pearson - SPIRE - Spectral and Photometric Imaging Receiver SPIRE mm PI: M.J. Griffin 3-band imaging photometer - 250, 350, 500  m,  ~ 3 (simultaneous) - 4 x 8 arcminute field of view - 2f feedhorn array - Diffraction limited beams (17”, 24”, 35”) - Point Source Detection Limit (5 , 1 hour) ~3 mJy Imaging FTS  m - > 2 arcminute field of view - Spectral Resolution to 0.04 cm -1 -  ~ 600 at 250  m Observing Modes - 3 band photometry Survey Optimized - low to medium resolution spectroscopy - Chop, jiggle or micro-step for mapping - Beam steering mirror for point source peak up Key Science Objectives - Large Area Extragalactic Surveys - Spectroscopy of Galaxies - Initial mass functions in star formation

9 64 th Symposium June, 2009 John Pearson - PACS - Photodetector Array Camera & Spectrometer PACS  m PI: A. Poglitsch 2-band imaging photometer  m or  m simultaneously with  m 1.75 x 3.5 arcminute field of view Diffraction limited beams (6”, 9”, 14”) Point Source Detection Limit (5 , 1 hour) ~5 mJy Imaging spectrometer  m - Simultaneous imaging of 50”x50” FOV (5x5 pixels) -  ~ (  v ~ km/s), 16 pixels Observing Modes - Dual band Photometry - Single band Photometry - Line spectroscopy - Range spectroscopy Key Science Objectives - Large Area Extragalactic Surveys - Spectroscopy of Galaxies - Initial Mass Function of Cores and Clusters - HD and the D/H ratio

10 64 th Symposium June, 2009 John Pearson - HIFI- Heterodyne Instrument for Far Infrared HIFI:  m PI: Frank Helmich 7 channel heterodyne receiver - 5 dual polarization SIS bands from GHz - 2 dual polarization HEB bands from THz - DSB configuration >2.4 GHz IF each polarization - Autocorrelation spectrometer to 134 kHz resolution - Acousto-Optical spectrometer with 4 GHz coverage -  Minimum=f/1GHz, maximum 10 7 Observing Modes - Deep integration single pixel - Spectral scan - Position mapping of a single line Key Science Programs - Spectral Surveys (>30 objects) - Role of Water in the Universe Core Science Objectives - ISM in Milky Way - Late Stages of Stellar Evolution - Solar system - ISM in Galaxies - Star formation Focal Plane Unit LO Unit

11 64 th Symposium June, 2009 John Pearson - Herschel First Light First Herschel Image PACS Photometer in 3 “colors” Telescope is performing as expected

12 64 th Symposium June, 2009 John Pearson - Astronomical Importance of the Submm/Far IR Emission from a star forming region (~ K) with spectral lines imposed on the dust continuum Dusty galaxies emit mostly in the far-IR and these wavelengths probe their star formation properties and evolution CII at 158 µm, the brightest cooling line in the ISM. BICE Galactic CII map at very low spectral resolution (top); dust emission (bottom).

13 64 th Symposium June, 2009 John Pearson - Statistics and Physics of Early Galaxies After Guiderdoni et al. MNRAS 295, 877, 1998 Flux density (mJy) (  m) ,00010, L  Z = Unbiased survey of population of high-z dusty star-forming galaxies missed by current (and future) optical and near-IR surveys Large-scale structure in the high- redshift universe Star-formation history in galaxies at z out to 5 –Shallow maps near ecliptic poles (~400 sq. deg.) –Search for FIR background fluctuations (with Planck) –Deep survey (~100 sq. deg.) –Ultra-deep (~1 sq. deg.) for P(D) analysis –Cluster surveys: formation, S- Z effect, lensed galaxy counts PACS and SPIRE photometry Herschel Wavelength Range

14 64 th Symposium June, 2009 John Pearson - Star Formation and the Lifecycle of the Interstellar Medium Herschel spectroscopy and photometry will trace the dynamics and chemistry of each stage of this lifecycle, including: –Mechanisms for stars formation –The properties of gas and dust injected by dying stars into the interstellar medium –The chemical complexity and evolution of stars and the galaxy –Shocks in molecular clouds, –Photon-Dominated Regions, –Diffuse atomic clouds, –Hot Cores and proto-planetary disks around newly formed stars –Winds in dying stars –Planet forming disks FIR FIR line spectrum of nearby galaxies as templates for distant, possibly primordial galaxies PACS & HIFI

15 64 th Symposium June, 2009 John Pearson - Origin of the Molecular Universe (HIFI & PACS) Arp 220

16 64 th Symposium June, 2009 John Pearson - Protostellar & Early Stellar Properties Protostellar Infrared spectrum will be covered completely by PACS and SPIRE Characterize energy output and evolutionary state –Class 0 protostar B335 as seen by ISO and JCMT HIFI will characterize dynamics –Inflows, outflows, jets HIFI will characterize chemistry –Molecules –Molecular distribution –Molecular excitation

17 64 th Symposium June, 2009 John Pearson - Science Operations Guaranteed Time Key Projects (Selected) Open Time Key Projects (Selected) –Including NASA Theory/Laboratory Astrophysics (Selected) Observatory Commissioning (Now-Early July 2009) Performance Verification (July-September 2009) Science Demonstration (October 2009) Workshop on Early Science (~November 2009) Cycle 1 OT & GT call~Jan 2010 Cycle 1 GT deadline ~April 2010 Cycle 1 OT deadline ~June 2010 Cycle 2 OT & GT issue~Dec 2010 Cycle 2 GT deadline~March 2011 Cycle 2 GT selection~May 2011 Cycle 2 OT deadline~June 2011 Cycle 2 OT selection~September 2011 Cycle 3 is Helium permitting

18 64 th Symposium June, 2009 John Pearson - Links for More Information Web sites for the lastest information ESA – NASA Herschel Science Center – JPL and Caltech – –