TERAHERTZ SURVEYS
the opening of the far-infrared and
submillimetre windows
Michael Rowan-Robinson
Imperial 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
Feb 9 2007
RAS Presidential Address
What is TERAHERTZ ?
Quick Time™a nd a
dec ompr esso r
ar e nee ded to see this pictur e.
Feb 9 2007
RAS Presidential Address
the Terahertz band
0.1-10 THz
30 microns - 3 mm
- a few terrestial windows
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RAS Presidential Address
Frank Low
1961: the Gallium-doped
Germanium bolometer
and the Low dewar
Low, F.J., “Low-Temperature Germanium
Bolometers,” J. Opt. Soc. Am. 51, 1300-04 (1961).
Low, F.J. & H.L. Johnson, “The Spectrum of 3C 273,” Ap.J. 141, 336-38 (1965). (10m)
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) (22mm)
Feb 9 2007
RAS Presidential Address
Frank Low: 1968: the far infrared background
Contribution of Infrared Galaxies to the Cosmic
Background
Frank J. Low
Department of Space Science, Rice University, Houston, Texas, and Lun ar
and Planetary Laboratory, University of Arizona, Tucson, Arizona
Wallace H. Tucker
Department of Space Science, Rice University, Houston, Texas
Received 12 July 1968
Phys. Rev. Lett. 21, 1538-41 (1968).
The fa r-infrared ba ckground due to a su perposition of infrared ga laxies of
the t ype recentl y observed is comp uted. It is shown th at thes e galaxies
contribute an amou nt of ene rgy to the universe rough ly equal to that
radiated b y the oth er galaxies and p roduce a far-infrared background
peaking be yond 50 mmК. It is li kely that they account fo r most of th e
observed extragalactic radio ba ckground but no t the 3 ЎK microwa ve
background.
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RAS Presidential Address
Frank Low: 1970: infrared galaxies
Low and Aumann, 1970, 162, L79
Low, 1970, ApJ 159, L173
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RAS Presidential Address
1970-1978: QMC, Cornell, UCL,
Harvard, Chicago, Caltech
Park, W. M.; Vickers, D. G.; Clegg, P. E.
Submillimeter Radiation from the Orion Nebula 1970 AA 5, 325 (900 mm)
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
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1970-1978
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 mm
P. E. CLEGG, P. A. R. ADE & M. ROWAN-ROBINSON
Queen 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)
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RAS Presidential Address
1970-1978
Telesco, Harper, Loewenstein
1976, ApJ 203, L53
Kuiper Airborne Observatory
NGC1068
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1970: birth of THz molecular line
astronomy
Wilson, Jefferts, Penzias, 1970,
ApJ 161, L43
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molecular line astronomy
Phillips, T.; Rowan-Robinson, M.: “Molecules among the stars”
1976, New Scientist 69, 170 - listed 32 molecules known (today 126 !)
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molecular line astronomy
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RAS Presidential Address
molecular line
astronomy
Phillips, Keene, 1992, Proc IEEE 80, 1662
Orion MC
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RAS Presidential Address
1974: QMC floats the idea of a
dedicated UK submillimetre telescope
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 mm (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
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RAS Presidential Address
IRAS
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RAS Presidential Address
Horsehead Nebula
IRAS - cirrus and zodiacal dust bands
Low et al ,1984, ApJ 278, L19
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IRAS cirrus
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south celestial pole
IRAS - zodiacal dust bands
Rowan-Robinson et al, 1991, MN 249, 729
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IRAS - star forming regions
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LMC
RAS Presidential Address
constellation Orion
IRAS - ultraluminous infrared galaxies
Arp 220
Soifer et al, 1984, ApJ 283, L1:
the remarkable infrared galaxy Arp 220
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RAS Presidential Address
IRAS - AGN dust tori
Miley et al, 1984, ApJ 278, L79:
A 25 mm component in 3C390.3
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IRAS - dust debris disks
Aumann et al, 1984, ApJ 278, L23:
discovery of a shell around Alpha Lyrae
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IRAS - protostars
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IRAS - non-discovery of Planet X
Walker and Rowan-Robinson, 1984, BAAS 16, 443
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IRAS all-sky survey
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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 al
1991, 2001)
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RAS Presidential Address
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
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RAS Presidential Address
Hyperluminous infrared
galaxies
starburst dominated
IRAS F10214, z=2.3 galaxy
Rowan-Robinson, 2000, MN 316, 885
Teplitz et al 2006
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RAS Presidential Address
impact of
JCMT
HDFN at 850 mm
Hughes et al 1996
blank field surveys at 850 mm showed that we were able to survey the
whole universe to z = 5 with ultraluminous ir galaxies
SHADES
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RAS Presidential Address
SHADES counts at 850 mm
Coppins et al, 2007,
astro-ph/0609039
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submillimetre galaxy redshift
distribution
Chapman et al, 2005,
ApJ 622, 772
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ISO
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RAS Presidential Address
interstellar dust grains
size 50 A - 0.1 mm
(and larger ?)
composition:
amorphous C
graphite
amorphous silicates
crystalline silicates
SiC
PAHs
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RAS Presidential Address
Brownlee particle
discovery of PAHs
Leger and Puget, 1984,
AA 137, L5
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RAS Presidential Address
what powers ultraluminous
infrared galaxies ?
Spoon et al, 2007, astro-ph/0611918
Genzel et al, 1998, ApJ 498, 579
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RAS Presidential Address
seds of ultraluminous infrared galaxies
L:ISO
R:SPITZER
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are needed to see this picture.
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RAS Presidential Address
the star
formation
history of the
universe
Rowan-Robinson 2003
Rowan-Robinson
‘Cosmology’
4th edition
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RAS Presidential Address
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
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RAS Presidential Address
Models for starburst
galaxies
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
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RAS Presidential Address
Cirrus models for local galaxies
• assume optically thin ism,
extinction AV (not >> 1)
• starburst models, age t*,
exponential decay time t
• characterise galaxies by single
mean intensity, y = bolometric
intensity/solar neighbourhood
intensity
• for local galaxies, t* = 0.25 Gyr,
t = 5-11 Gyr
(Efstathiou and Rowan-Robinson
2003, MN 343, 322)
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RAS Presidential Address
z<0.12 galaxies with cirrus seds
Rowan-Robinson et al,
2005, AJ 129, 1183
sources with good
ISO-ELAIS and
SPITZER-SWIRE
data
templates
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RAS Presidential Address
z=0.1-0.9 galaxies
fitted with cirrus
or A220 template
A220 model:
AV = 200, t* = 26 Myr
(Efstathiou and
RR 2001)
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RAS Presidential Address
seds of z=0.1-2.2 galaxies/quasars
fitted with cirrus, A220
starburst and AGN
dust torus templates
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RAS Presidential Address
SPITZER
Feb 9 2007
RAS Presidential Address
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
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RAS Presidential Address
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
Feb 9 2007
RAS Presidential Address
QuickTime™ and a
MPEG-4 Video decompressor
are needed to see this picture.
Feb 9 2007
RAS Presidential Address
M51
Sombrero
combined 3.6, 8 and 24
mm images
(SINGS consortium)
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RAS Presidential Address
M82
N2207/IC2163
Stefan’s Qntet
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RAS Presidential Address
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
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RAS Presidential Address
Layered SPITZER Surveys
• Wide–shallow
FLS GTO-shallow
– greatest volume
4
– rare luminous objects
– large-scale structure
8.5
• Confusion-limited GTO-deep
– maximum information 2.5 sq deg
on faintest resolved sources
• Ultra-deep
– confusion distribution
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GTO-ultra
150
RAS Presidential Address
SWIRE
49 sq deg
GOODS-IRAC
300 sq arcmin
GOODS-24 mm
300 sq arcmin
SWIRE Team and Associates
Carol Lonsdale
PI
Harding E (Gene) Smith Deputy PI
Michael Rowan-Robinson Deputy PI
Dave Shupe
Liaison Scientist
Jason Surace
Data Processing/IRAC
Kevin (Cong) Xu
Models
Deborah Padgett
Galactic Science/MIPS
Fan Fang
Simulation/Models
Alberto Franceschini Spheroids/AGN
Dave Frayer
EROs/MIPS
Glenn Morrison
Radio
JoAnn O’Linger
Galactic Science
Seb Oliver
Large Scale Structure
Frazer Owen
Radio Deep Survey
Ismael Perez-Fournon Nearby Galaxies
IPAC, Caltech
UCSD
Imperial College
SSC/IPAC
SSC/IPAC
IPAC
SSC/IPAC
SSC/IPAC
Padua
SSC/IPAC
IPAC
SSC
Sussex
NRAO
IAC, Tenerife
Marguerite Pierre
X-ray/XMM-LSS
Gordon Stacey
Submm
Olivier Lefevre
VVDS
Steve Serjeant
ELAIS
Eduardo Gonzalez-Solares ELAIS IOA
Feb 9 2007
CEA, Saclay
Cornell
Marseille
Kent
Duncan Farrah, Maria Polletta
Brian Siana
Tom Babbedge, Dave Clements
Stefano Berta, Giulia Rodighiero
Payam Davoodi, Ian Waddington
Alejandro Afonso-Luis, Evanthia
Hadtziminaoglou,
Antonio Hernan-Caballero
RAS Presidential Address
ELAIS N1:
9 sq. deg
SWIRE 3.6 mm survey in ELAIS-N1
Feb 9 2007
RAS Presidential Address
Photometric redshifts
SWIRE-VVDS sample
(with VVDS team, PI
LeFevre)
VIRMOS-VLT Deep Survey
spectra
>1000 sources
~3% rms in (1+z)
<2% outliers
red: gals, blue QSOs
phot z method of RR 03,
Babbedge et al 04, RR et
al 05, some refinements
~ IRAC 3.6 and 4.5 mm
big help in reducing
outliers
Feb 9 2007
z=1
2
RAS3Presidential
4 Address
Photometric redshifts
All SWIRE Catalogue
VVDS: 9 optical bands
N1,N2: 5 optical bands
Lockman: 3-4 optical bnds
CDFS: 3 optical bands
Feb 9 2007
z=1
2
RAS Presidential
3
4 Address
Redshift distributions
left: Suburu XDS, R<27.5
below: ELAIS-N1, r<23.5: for optically
blank sources use 3.6-8 mm for phot-z
>=3 bands from U-8mm
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RAS Presidential Address
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)
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RAS Presidential Address
seds of submillimetre galaxies
SHADES SXDS Clements et al 2007
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RAS Presidential Address
COUNTS AT 24 mm
•
24 mm 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
cirrus
M82
dust tori
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RAS Presidential Address
Counts at 70-850 mm
•
new SWIRE 70, 160
and SHADES 850 mm
differential counts
(Afonso-Luis et al,
2007, in prep,
Coppins et al 2007)
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RAS Presidential Address
The Terahertz background
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RAS Presidential Address
History of the universe
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RAS Presidential Address
WMAP & 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.
WMAP
Spergel et al. 2006
Feb 9 2007
From Fan et al.
RAS Presidential Address
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
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RAS Presidential Address
Darwin
the future
ALMA
TPF
Feb 9 2007
RAS Presidential Address
Herschel