Feb 9 2007RAS Presidential Address TERAHERTZ SURVEYS the opening of the far-infrared and...

Feb 9 2007 RAS Presidential Address

TERAHERTZ SURVEYSthe opening of the far-infrared and

submillimetre windowsMichael Rowan-RobinsonImperial College London

• the Terahertz band• birth of Terahertz astronomy: 1961-1984• IRAS, JCMT, ISO• radiative transfer in dust clouds• SPITZER• the Terahertz background• the future


What is TERAHERTZ ?

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0.1-10 THz 30 microns - 3 mm

- a few terrestial windows

the Terahertz band


Low, F.J. & H.L. Johnson, “The Spectrum of 3C 273,” Ap.J. 141, 336-38 (1965). ()

Low, F.J., “The Performance of Thermal Detection Radiometers at 1.2 mm,” Proc. IEEE 53, 516 (1965).

Kleinmann, D.E. & F.J. Low, “Discovery of an Infrared Nebula in Orion,” Ap.J. 149, L1-L4 (1967) (22m)

Frank Low1961: the Gallium-doped Germanium bolometer and the Low dewar

Low, F.J., “Low-Temperature Germanium Bolometers,” J. Opt. Soc. Am. 51, 1300-04 (1961).


Frank Low: 1968: the far infrared background

Contribution of Infrared Galaxies to the CosmicBackground

Frank J. LowDepartment of Space Science, Rice University, Houston, Texas, and Lunarand Planetary Laboratory, University of Arizona, Tucson, Arizona

Wallace H. TuckerDepartment of Space Science, Rice University, Houston, Texas

Received 12 July 1968

The far-infrared background due to a superposition of infrared galaxies ofthe type recently observed is computed. It is shown that these galaxiescontribute an amount of energy to the universe roughly equal to thatradiated by the other galaxies and produce a far-infrared backgroundpeaking beyond 50 . m It is likel y that theyacc ount fo r mos t of theobser vedextragalacti c radi o backgroun d but no t 3the ° K microwavebackgroun .d

Phys. Rev. Lett. 21, 1538-41 (1968).


Frank Low: 1970: infrared galaxies

Low and Aumann, 1970, 162, L79

Low, 1970, ApJ 159, L173


Park, W. M.; Vickers, D. G.; Clegg, P. E.Submillimeter Radiation from the Orion Nebula 1970 AA 5, 325 (900 m)

Houck, J. R.; Soifer, B. T.; Pipher, Judith L.; Harwit, Martin Rocket-Infrared Four-Color Photometry of the Galaxy's Central Regions 1971 ApJ 169, 31L

1970-1978: QMC, Cornell, UCL, Harvard, Chicago, Caltech


Fazio, G. G.; Kleinmann, D. E.; Noyes, R. W.; Wright, E. L.; Zeilik, M., II; Low, F. J.: A High-Resolution Map of the Orion Nebula Region at Far-Infrared Wave-Lengths 1974 ApJ 192, 23

Nature 249, 530 - 532 (07 June 1974);

Narrow-band observations of galactic and extragalactic sources at 1 mmP. E. CLEGG, P. A. R. ADE & M. ROWAN-ROBINSONQueen Mary College, University of London, Mile End Road, London E1, UK

WE report the result of a search for discrete extragalactic sources of continuum radiation near 1.2 mm. The observations were made during a run of one week on the United States National Radio Astronomy Observatory (NRAO) 11-m telescope at Kitt Peak, Arizona.

Rowan-Robinson, M.: Astronomy at submillimetre wavelengths, 1974, New Scientist 67, 78

Elais J.H. et al, 1 millimeter continuum observations of extragalactic objects, 1978, ApJ 220, 25 (9 detected)

1970-1978


1970-1978Telesco, Harper, Loewenstein1976, ApJ 203, L53

NGC1068

Kuiper Airborne Observatory


1970: birth of THz molecular line astronomy

Wilson, Jefferts, Penzias, 1970, ApJ 161, L43


Phillips, T.; Rowan-Robinson, M.: “Molecules among the stars”1976, New Scientist 69, 170 - listed 32 molecules known (today 126 !)

molecular line astronomy


molecular line astronomy


molecular line astronomyPhillips, Keene, 1992, Proc IEEE 80, 1662

Orion MC


1974: memo from M.R-R to QMC group ‘Proposal for a large millimetre telescope’ - discusses (i) 30 m. telescope good to 1 mm, (ii) 10 m. telescope good to 350 m (which would have to be on Mauna Kea)

1975: Tom Phillips submits proposal for a submillimetre telescope to SERC review of radio-astronomy

1975 : SRC millimetre steering committee (chair Tom Phillips) concluded that it would be possible to construct a 15-metre diameter telescope capable of observing at wavelengths down to 750 µm. Final site selection was between Mauna Kea and La Palma.

1987: JCMT first light

1974: QMC floats the idea of a dedicated UK submillimetre telescope


IRAS

Horsehead Nebula


IRAS - cirrus and zodiacal dust bands

Low et al ,1984, ApJ 278, L19


IRAS - cirrus

south celestial pole


IRAS - zodiacal dust bands

Rowan-Robinson et al, 1991, MN 249, 729


IRAS - star forming regions

constellation OrionLMC


IRAS - ultraluminous infrared galaxies

Arp 220

Soifer et al, 1984, ApJ 283, L1: the remarkable infrared galaxy Arp 220


IRAS - AGN dust toriMiley et al, 1984, ApJ 278, L79: A 25 m component in 3C390.3


IRAS - dust debris disks

Aumann et al, 1984, ApJ 278, L23: discovery of a shell around Alpha Lyrae


IRAS - protostars


IRAS - non-discovery of Planet X

Walker and Rowan-Robinson, 1984, BAAS 16, 443


IRAS all-sky survey


IRAS - mapping the 3-D galaxy distribution

able to explain origin of our Galaxy’s motion with respect to the cosmic frame - the CMB dipole(Rowan-Robinson et al1991, 2001)


2MASS and AKARI• 2MASS provides a better picture of galaxy distribution at z<0.03• AKARI will allow us to study ir dipole to z ~ 0.3


Hyperluminous infrared galaxies

Rowan-Robinson, 2000, MN 316, 885

starburst dominated

IRAS F10214, z=2.3 galaxy

Teplitz et al 2006


HDFN at 850 mHughes et al 1996

impact of JCMT

SHADES

blank field surveys at 850 m showed that we were able to survey the whole universe to z = 5 with ultraluminous ir galaxies


SHADES counts at 850 m

Coppins et al, 2007, astro-ph/0609039


submillimetre galaxy redshift distribution

Chapman et al, 2005,

ApJ 622, 772


ISO


interstellar dust grains

size 50 A - 0.1 m (and larger ?)

composition: amorphous C graphite amorphous silicates crystalline silicates SiCPAHs

Brownlee particle


discovery of PAHs

Leger and Puget, 1984,AA 137, L5


what powers ultraluminous infrared galaxies ?

Genzel et al, 1998, ApJ 498, 579

Spoon et al, 2007, astro-ph/0611918


seds of ultraluminous infrared galaxies

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L:ISO R:SPITZER


the star formation

history of theuniverse

Rowan-Robinson ‘Cosmology’4th edition

Rowan-Robinson 2003


Radiative transfer models for infrared sources

• spherically symmetric dust clouds

- first accurate code 1980 (R-R, ApJS 234, 111)

- circumstellar dust shells 1981-3

- starbursts and ULIRGs 1993

• axially symmetric dust clouds

- first accurate code 1990 (Efstathiou and R-R, MN 245, 275)

- protostars 1991

- AGN dust tori 1995


Eftstathiou, R-R, Seibenmorgen, 2000, MN 313, 734• embedded phase, t < 107 yrs• expanding neutral shell, t = 107-108 years•at 108 yrs, indistinguishable from cirrus

Models for starburstgalaxies


Cirrus models for local galaxies• assume optically thin ism, extinction AV (not >> 1)

• starburst models, age t*, exponential decay time

• characterise galaxies by single mean intensity, = bolometric intensity/solar neighbourhood intensity

• for local galaxies, t* = 0.25 Gyr, = 5-11 Gyr

(Efstathiou and Rowan-Robinson 2003, MN 343, 322)


z<0.12 galaxies with cirrus sedsRowan-Robinson et al,2005, AJ 129, 1183 sources with good ISO-ELAIS and SPITZER-SWIRE data

templates


z=0.1-0.9 galaxies

fitted with cirrus or A220 template

A220 model: AV = 200, t* = 26 Myr (Efstathiou and RR 2001)


fitted with cirrus, A220 starburst and AGN dust torus templates

seds of z=0.1-2.2 galaxies/quasars


SPITZER


SPITZER’s chequered history• 1979 SIRTF conceived

• 1984 selection of SIRTF team, mission planned as Shuttle launch

• 1990 switch to Titan launch, 5.7 tonnes, 1m telescope, $2b

• 1993 descope to 2.7 tonnes, Atlas launch

• 1995 further descope to Delta launch, 0.75 tonnes, 85cm telescope, $450m, design lifetime 2.5 years, goal 5 years

• Aug 2003 launch, renamed SPITZER

• 2007, expected life 5.5 years


IC1396, the Elephant’s Trunk

- dark globule inside emission nebula (ionizing star is to left of frame)

- pair of newly formed stars have created cavity


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M51Sombrero

combined 3.6, 8 and 24 m images(SINGS consortium)


M82N2207/IC2163Stefan’s Qntet


SPITZER-IRS: IRAS F00183-7111, hyperluminous infrared galaxy

•IRS spectrum of the hyperluminous ir galaxy F00183-7111= IRAS P00182-7112(Spoon et al 2004)

• z = 0.327 (narrow line object), lg Lsb = 13.25


Layered SPITZER Surveys• Wide–shallow FLS GTO-shallow SWIRE

– greatest volume 4 8.5 49 sq deg

– rare luminous objects

– large-scale structure

• Confusion-limited GTO-deep GOODS-IRAC– maximum information 2.5 sq deg 300 sq arcmin

on faintest resolved sources

• Ultra-deep GTO-ultra GOODS-24 m– confusion distribution 150 300 sq arcmin


SWIRE Team and AssociatesCarol Lonsdale PI IPAC, Caltech Duncan Farrah, Maria PollettaHarding E (Gene) Smith Deputy PI UCSD Brian SianaMichael Rowan-Robinson Deputy PI Imperial College Tom Babbedge, Dave ClementsDave Shupe Liaison Scientist SSC/IPACJason Surace Data Processing/IRAC SSC/IPAC

Kevin (Cong) Xu Models IPACDeborah Padgett Galactic Science/MIPS SSC/IPACFan Fang Simulation/Models SSC/IPACAlberto Franceschini Spheroids/AGN Padua Stefano Berta, Giulia RodighieroDave Frayer EROs/MIPS SSC/IPAC

Glenn Morrison Radio IPACJoAnn O’Linger Galactic Science SSCSeb Oliver Large Scale Structure Sussex Payam Davoodi, Ian WaddingtonFrazer Owen Radio Deep Survey NRAOIsmael Perez-Fournon Nearby Galaxies IAC, Tenerife Alejandro Afonso-Luis, Evanthia

Hadtziminaoglou, Antonio Hernan-Caballero

Marguerite Pierre X-ray/XMM-LSS CEA, SaclayGordon Stacey Submm CornellOlivier Lefevre VVDS MarseilleSteve Serjeant ELAIS KentEduardo Gonzalez-Solares ELAIS IOA


ELAIS N1: 9 sq. deg

SWIRE 3.6 m survey in ELAIS-N1


Photometric redshiftsSWIRE-VVDS sample (with VVDS team, PI LeFevre)

VIRMOS-VLT Deep Survey spectra>1000 sources~3% rms in (1+z)<2% outliers

phot z method of RR 03, Babbedge et al 04, RR et al 05, some refinements

~ IRAC 3.6 and 4.5 m big help in reducing outliers

z = 1 2 3 4

red: gals, blue QSOs


Photometric redshiftsAll SWIRE Catalogue

VVDS: 9 optical bandsN1,N2: 5 optical bandsLockman: 3-4 optical bndsCDFS: 3 optical bands

z = 1 2 3 4


Redshift distributions

>=3 bands from U-8m

left: Suburu XDS, R<27.5

below: ELAIS-N1, r<23.5: for optically blank sources use 3.6-8 m for phot-z


SPITZER-IRS spectra of ELAIS sources• IRS spectra for 70 ELAIS-N1

and -N2 sources with S15> 1mJy validate the template fits

• most are ULIRGs, with z =1-3

• Filled circles: optical, ISO, SWIRE

( and MAMBO) data

• Solid curves: model seds

• Red curve: calibrated IRS data (Hernan-Caballero et al 2006)


seds of submillimetre galaxiesSHADES SXDS Clements et al 2007


COUNTS AT 24 m• 24 m differential counts (Shupe et

al, 2007, Papovich et al 2004)

• new model for ir counts (developed from RR 2001 models): independent evolution for each component, evolution has to flatten off at z < 0.5

M82cirrus

dust tori


Counts at 70-850 m• new SWIRE 70, 160

and SHADES 850 m differential counts (Afonso-Luis et al, 2007, in prep,

Coppins et al 2007)


The Terahertz background


History of the universeHistory of the universe


WMAP & QSO ResultsWMAP & QSO Results• Year 3 WMAP release has reduced the electron optical depth so the epoch of

reionization has been moved from z~17 down to z~10.9 (+2.7, -2.3), equivalent to 360Myr after Big Bang.

• Spectra of SDSS z~6 QSOs show hints that Universe was reionized at only somewhat higher z than 6.5.

Spergel et al. 2006

WMAP

From Fan et al.


a z ~ 6.7 galaxy detected by SPITZER

Egami et al, 2005, ApJ 618, L5:

z ~ 6.7 lensed

galaxy with

M = 109 Mo,

stellar age at least 50 Myr


the futureDarwin

TPF

ALMA

Herschel

Feb 9 2007RAS Presidential Address TERAHERTZ SURVEYS the opening of the far-infrared and...

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