64 th symposium 22-26 june, 2009 john pearson nasa herschel deputy project scientist jet propulsion...

64th Symposium 22-26 June, 2009

John PearsonNASA Herschel Deputy Project Scientist

Jet Propulsion Laboratory

THE HERSCHEL SPACE OBSERVATORY, OPENING THE FAR INFRARED

264th Symposium 22-26 June, 2009John Pearson -

What is HerschelWhat is Herschel

The Herschel Space Observatory (Herschel)Named for Wilhelm Herschel– Discoverer of Infrared radiation

First comprehensive far infrared observatory in spaceLargest space based mirror to dateSuccessfully launched on 14 May 2009 at 13:12 UTC Together with Planck onboard an Ariane 5 ECA from Europe's spaceport in Kourou, French GuianaThree instruments with 2500 Liters of superfluid He

MISSION END:2011-2012LAUNCH MASS:3400 kgMISSION PHASE:Commissioning


Launch of Herschel & PlanckLaunch of Herschel & Planck

14 May 2009 at 13:12 UTC Together with Planck onboard an Ariane 5 ECA


Why Go to Space 1/2?Why Go to Space 1/2?

Typical transmission from Mauna Kea with

1mm H2O, 45o

R = 5000

Typical transmission from SOFIA (~14km)

with 1µm H2O, 45o

R = 5000

5 THz 0.5 THz


Why Go To Space 2/2?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


L2 OrbitL2 Orbit

Stable pointGoes with EarthAround Sun loose Orbit no shadow


Herschel SpecificationsHerschel 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)


SPIRE - SPIRE - Spectral and Photometric Imaging ReceiverSpectral and Photometric Imaging Receiver

SPIRE 200-680mm PI: M.J. Griffin3-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 - 200-670 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


PACS - PACS - Photodetector Array Camera & SpectrometerPhotodetector Array Camera & Spectrometer

PACS 57-210m PI: A. Poglitsch2-band imaging photometer• 57-72m or 72-105m simultaneously with 105-210m• 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 - 57-210 m - Simultaneous imaging of 50”x50” FOV (5x5 pixels) - ~ 1000-3000 (v ~ 150-300 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


HIFI- HIFI- Heterodyne Instrument for Far InfraredHeterodyne Instrument for Far Infrared

HIFI: 157-624m PI: Frank Helmich7 channel heterodyne receiver - 5 dual polarization SIS bands from 480-1272GHz - 2 dual polarization HEB bands from 1.44-1.91 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 107

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


Herschel First LightHerschel First Light

First Herschel ImagePACS Photometer in 3 “colors”Telescope is performing as expected


Astronomical Importance of the Submm/Far IR

Emission from a star forming region (~ 70-100 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).


Statistics and Physics of Early GalaxiesStatistics and Physics of Early Galaxies

After Guiderdoni et al. MNRAS 295, 877, 1998

Flu

x d

en

sit

y

(mJ

y)

(m)10 100 1,000 10,000

10,000

1000

100

10

1

0.1

1012L

Z = 0.1

0.5

1

3

5

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


Star Formation and the Lifecycle of the Interstellar MediumStar 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


Origin of the Molecular Universe (HIFI & PACS)Origin of the Molecular Universe (HIFI & PACS)

Arp 220


Protostellar & Early Stellar PropertiesProtostellar & 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


Science OperationsScience 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


Links for More InformationLinks for More Information

Web sites for the lastest information

ESA

– http://herschel.esac.esa.int/

NASA Herschel Science Center

– http://www.ipac.caltech.edu/Herschel/nhsc.shtml

JPL and Caltech

– http://herschel.jpl.nasa.gov/

– http://www.herschel.caltech.edu/

64 th symposium 22-26 june, 2009 john pearson nasa herschel deputy project scientist jet propulsion...

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