General Imaging Fourier Transform Imaging Photometer

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Imaging Fourier Transform Spectrometer Simultaneous imaging observation of the whole spectral band 37 and 19 pixels Wavelength Range: 194-313, 303-671 μm Resolution: 0.04, 0.24, 0.83 cm -1 Circular FOV 2.0‘ diameter, beams 17-21”, 29-42” Spectrometer Sensitivities* Photometer Sensitivities* For more information please refer to the Observer’s Manual or visit one of these sites: http://herschel.esac.esa.int, http://www.spire.rl.ac.uk, http://www.herschel.caltech.edu Imaging Photometer Simultaneous observation in 3 bands 139, 88, and 43 pixels Wavelengths: 250, 350, 500 μm / ~ 3 FOV 4' x 8', beams 18.1'', 25.2'', 36.6'' General Beam Steering Mirror T= 0.3 K by 3 He sorption cooler. Hexagonally packed Spider-web bolometer arrays. * Quoted figures represent in-orbit results as of May 2010 SPIRE is one of three scientific instruments on board of ESA’s Herschel Space Observatory, exploring the Universe at infrared wavelengths between 194 and 671 μm. Spectral and Photometric Imaging Receiver Extragalactic confusion noise (mJy 1) Small and Large Map (mJy, 1, one repeat A+B scan, nominal speed) 10.8 7.5 9.0 6.8 6.3 5.8 7.0 7.0 7.0 Point Source (mJy, 7-point mode, one repeat ABBA) 500 350 250 Wavelengths (μm) SLW SSW Beam Splitter Optical Bench Spectrometer Detector Box FTS Mechanism S-Cal Photometer Cover Beam Steering Mirror SPIRE Optical Bench PLW PMW Sorption Cooler PSW Photometer Detector Box Optical Sub-bench Cone Support Spectrometer Cover Telescope Beam Detector Assembly Feedhorn array without covering filter 300 mK stage Connection to 3 He fridge Kevlar suspension 2K stage and interface to SPIRE 2K box Version 5, May 2010 The SPIRE Consortium: SPIRE is being designed and built by a consortium of institutes and university departments from across Europe, Canada and the USA, under the leadership of a Pricipal Investigator (Professor M.J. Griffin) located at the University of Wales, Cardiff. The member institutes are: Astronomy Technology Centre (ATC), Edinburgh; Observatoire de Meudon (DESPA), Paris; CEA, Service des Basses Temperatures (SBT), Grenoble; Goddard Space Flight Center (GSFC), Maryland; Instituto de Astrofisica de Canarias (IAC), Tenerife; Insitut d'Astrophysique Spatiale (IAS), Orsay; Imperial College London; Instituto di Fisica dello Spazio Interplanetario (IFSI), Rome; Jet Propulsion Laboratory (JPL), Pasadena; Laboratoire de Marseille (LAM), Marseille; Mullard Space Science Laboratory (MSSL), Holmbury St. Mary; Padova Observatory, Padova; University of Wales, Cardiff; Rutherford Appleton Laboratory (RAL), Chilton; CEA, Service d'Astrophysique (Sap), Saclay; University of Colorado, University of Lethbridge, Canada; Stockholm Observatory, Sweden 0.24 cm -1 140-310 140-300 cont. flux (mJy, 5, 1h) 0.83 cm -1 0.04 cm -1 40-88 40-86 cont. flux (mJy, 5, 1h) 830-1830 830-1790 cont. flux (mJy, 5, 1h) 1.00-2.20 1.00-2.15 Line flux (10 -17 Wm -2 , 5, 1h) 303-671 194-313 Wavelengths (μm)

Transcript of General Imaging Fourier Transform Imaging Photometer

Page 1: General Imaging Fourier Transform Imaging Photometer

Imaging Fourier Transform

SpectrometerSimultaneous imaging observation of the whole

spectral band

37 and 19 pixels

Wavelength Range: 194-313, 303-671 μm

Resolution: 0.04, 0.24, 0.83 cm-1

Circular FOV 2.0‘ diameter, beams 17-21”, 29-42”

Spectrometer Sensitivities*Photometer Sensitivities*

For more information please refer to the Observer’s Manual or visit one of these sites: http://herschel.esac.esa.int, http://www.spire.rl.ac.uk, http://www.herschel.caltech.edu

Imaging PhotometerSimultaneous observation in 3 bands

139, 88, and 43 pixels

Wavelengths: 250, 350, 500 μm

/ ~ 3

FOV 4' x 8', beams 18.1'', 25.2'', 36.6''

GeneralBeam Steering

Mirror

T= 0.3 K by 3He

sorption cooler.

Hexagonally packed

Spider-web

bolometer arrays.

* Quoted figures represent in-orbit results as of May 2010

SPIRE is one of three scientific instruments on board of ESA’s Herschel

Space Observatory, exploring the Universe at infrared wavelengthsbetween 194 and 671 μm.

Spectral and Photometric Imaging Receiver

Extragalactic confusion noise (mJy 1 )

Small and Large Map (mJy, 1 , one repeat A+B scan,

nominal speed)

10.87.59.0

6.86.35.8

7.07.07.0Point Source (mJy, 7-point mode, one repeat ABBA)

500350250Wavelengths (μm)

SLW

SSW

Beam SplitterOptical Bench

Spectrometer

Detector Box

FTS Mechanism S-Cal

Photometer Cover

Beam Steering Mirror

SPIRE Optical Bench

PLW PMW Sorption

Cooler

PSW

Photometer Detector Box

Optical Sub-bench

Cone Support

Spectrometer

Cover

Telescope Beam

Detector Assembly

Feedhorn array without

covering filter

300 mK

stage

Connection

to 3He fridge

Kevlar

suspension

2K stage and

interface to

SPIRE 2K box

Vers

ion 5

, M

ay 2

010

The SPIRE Consortium: SPIRE is being designed and built by a consortium of institutes and university departments from across Europe, Canada and the USA, under the leadership of a Pricipal Investigator (Professor M.J. Griffin) located at the University of

Wales, Cardiff. The member institutes are: Astronomy Technology Centre (ATC), Edinburgh; Observatoire de Meudon (DESPA), Paris; CEA, Service des Basses Temperatures (SBT), Grenoble; Goddard Space Flight Center (GSFC), Maryland; Instituto de

Astrofisica de Canarias (IAC), Tenerife; Insitut d'Astrophysique Spatiale (IAS), Orsay; Imperial College London; Instituto di Fisica dello Spazio Interplanetario (IFSI), Rome; Jet Propulsion Laboratory (JPL), Pasadena; Laboratoire de Marseille (LAM),

Marseille; Mullard Space Science Laboratory (MSSL), Holmbury St. Mary; Padova Observatory, Padova; University of Wales, Cardiff; Rutherford Appleton Laboratory (RAL), Chilton; CEA, Service d'Astrophysique (Sap), Saclay; University of Colorado,

University of Lethbridge, Canada; Stockholm Observatory, Sweden

0.24 cm-1 140-310140-300 cont. flux (mJy, 5 , 1h)

0.83 cm-1

0.04 cm-1

40-8840-86 cont. flux (mJy, 5 , 1h)

830-1830830-1790 cont. flux (mJy, 5 , 1h)

1.00-2.201.00-2.15Line flux (10-17 Wm-2, 5 , 1h)

303-671194-313Wavelengths (μm)

Page 2: General Imaging Fourier Transform Imaging Photometer

These investigations require the ability to carry out large area

deep photometric imaging surveys at far-infrared and

submillimetre wavelengths, and to follow up these observations

with spectroscopy of selected sources.

SPIRE exploits the unique advantages of Herschel: its large-

aperture, cold, low-emissivity telescope; the complete lack of

atmospheric emission giving access to the poorly explored 194-

671 μm range, and the large amount of high quality observing

time. SPIRE has unmatched sensitivity for deep photometry and

moderate-resolution spectroscopy.

Although SPIRE has been optimized for the two main

scientific programs, it offers the astronomical

community unique observing capabilities to tackle

many other astrophysical topics: giant planets, comets,

the galactic interstellar medium, nearby galaxies,

ultraluminous infrared galaxies, and active galactic

nuclei. Its capabilities will remain unchallenged by the

ground based and the airborne observatories which

are planned to come into operation over the next

decade.For more information please visit one of these sites:

http://herschel.esac.esa.int, http://www.spire.rl.ac.uk, http://www.herschel.caltech.edu

Log L

(L )

1000 100 10 1 0.1

12

7

9

11

8

10

13

12 13 14 15 16

Log ( rest ) (Hz)

rest (μm)

Sanders & Mirabel

Ann. Rev. Astron.

Astrophys. 34, 749,1996

SPIRE’s photometric bands, together with those of PACS,

will cover emission of very cold dust, an interval where many

ultraluminous infrared galaxies radiate most of their energy.

SPIRE

PACS

SPIRE is one of 3 scientific instruments on board of ESA’s Herschel

Space Observatory, exploring the Universe at infrared wavelengthsbetween 194 and 671 μm.

Spectral and Photometric Imaging Receiver

SPIRE is designed to exploit Herschel’s capabilities in addressing

two of the most prominent questions of modern astrophysics:

•How and when did galaxies form?

The investigation of the statistics and

physics of galaxies and large scale

structure formation at high redshift;

•The life cycle of stars

The study of the earliest

phases of star formation

and the evolutionary

life cycle of stars to their

end phase.

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