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Millimetre Studies of High-z Quasars
and Galaxies
March 27-31, 2006
Venice
Pierre Cox
IRAM
Grenoble, France
The spectrum of a ULIRG: a `field guide’
• Non-thermal radio
• Thermal dust
- Dominated luminosity
- Hotter in AGN
- Mid-IR spectral features
(missing in AGN)
• Molecular and atomic lines
- mm CO/HCN
- far-IR: C/N/O
- mid-IR: C-C/C=C/H2
Luminosities involved:
3x1011 <L/Lsun< 1014
From Blain (2003)
March 27-31, 2006
Venice
Deep Field Sources
15”/10”
SCUBA/
MAMBO
Source identification critical (usually through RC, Chapman et al. 2004)
Pointed Observations
- Sources selected from optical (SDSS) and radio (VLA):
Quasars (radio-quiet), radio-galaxies
- Position well known; redshifts known (1<z<6.4)
March 27-31, 2006
Venice
-> poster
Tdust = 52 K
Beta = 1.5
L_FIR = 4x1012 x S250(mJy) L_sun for z=0.5 to 8
SFR = 1400 x S250(mJy)M_sun/yr (very high)
M_dust = 1.4x108 x S250(mJy) M_sun
March 27-31, 2006
Venice
Beelen et al. 2005
March 27-31, 2006
Venice
CO Survey of submm Galaxies
SMM J02396-0134
SMM J02399-0136
SMM J04431+0210
SMM J09431+4700
SMM J13120+4242
SMM J14011+0252
SMM J16368+4057
SMM J16359+6612
SMM J16366+4105
 18 radio-detected submm
galaxies with known
optical/near-IR redshift
detected in CO
 1<z<3.5
 Variety of profiles: 780+-230 km/s
 Mergers/Rotating Disks
Star Formation Rate: 720 Msun/yr
 MH2 ~ 3x1010 Msun
 Mdyn ~ 1011 Msun
 The submm-population consists of
gas rich and massive, composite
starbursts/AGN systems
(Greve et al. 2005; Neri et al. 2004;
Tacconi et al. 2006)
March 27-31, 2006
SMM J16371+4053
ERO J16450+4626
Venice
SMM J22174+0015
Subarcsecond Imaging Results
 < 0.5” (4 kpc)
Tacconi, Neri, Chapmanm Genzel et al. (2006)
March 27-31, 2006
Venice
 Compact sources
 Scaled-up versions and
more gas-rich of the local
ULIRG population
 Central densities and
potential well depths
comparable to those of
elliptical galaxies or
massive bulges
Fulfill the criteria of
maximal starbursts: initial
gas reservoir 1010-11 Msun is
converted to stars on a
timescale ~3-10 tdyn or a few
108 yr
J1148+5251 - The Most Distant QSO at z=6.42
Gunn Peterson trough
Fan et al. 2003; White et al. 2003
z-band (Keck – Djorgovski et al.)
 z=6.42; age~870 Myr
 one of the first luminous sources
 MBH ~ 1-5 x 109 Msun (Willot et al. 2003)
 Mdust ~ 108 Msun
(Bertoldi et al. 2003)
March 27-31, 2006
Venice
Dust continuum at 1.2 mm
CO(3-2)
46.6149 GHz
PdBI
continuum
VLA
March 27-31, 2006
Venice
Resolving the CO emission in J1148+5251
VLA A+B + C array; res.: 0.15” (~1 kpc)
 Two sources separated by 0.3”
(1.7 kpc at z=6.4) containing each
5 x 109 Msun

Not likely to be amplified

If gravitationally bound,
MDyn=4.5x1010 Msun
Walter et al. 2004
March 27-31, 2006
Venice
CO excitation in J1148+5251 (filled
circles), compared to NGC 253 (dashed)
 Mass:
LVG Model:
MH2 = 2 x 1010 Msun
Tkin= 100K, nH2=7x104 cm-3
Mdyn = 3 x 109 sin-2(i) Msun
 Mass in C and O: ~3x107 Msun
Bertoldi et al. (2003)
March 27-31, 2006
Venice
Multiple CO Lines
IRAM 30m CO multi-line survey (1, 2, 3mm bands) Weiss et al. (2006)
March 27-31, 2006
Venice
LVG solution Cloverleaf
CO LVG solution:
Disk radius: 1 kpc
excellent agreement with lens models !
log(n(H2)) = 4.2 cm-3
Tkin = 30 K
M(H2) = 8 1010 M
L’CO(1-0) = 4.4 1010 K km/s pc2
Xco = 1.8 M/ K km/s pc2
Weiss et al. (2005)
High Density Tracer: HCN
J1409+5628 (z=2.56)
High density tracer in starbursts: nH2 > 10(5) cm(-3)
APM08279+5255
APM08279+5255 (z=3.91)
Gao & Solomon
2004
Carilli et al. (2004)
March 27-31, 2006
Venice
Wagg et al. 2005
High Density Tracer: HCO+
APM08279+5255 (z=3.91)
Burillo et al. 2006
March 27-31, 2006
L’(HCO+) = 4 x 1010 K/(km/s pc2)
HCO+(5-4)/HCN(5-4) ~ 1
Venice
Search for Neutral Carbon [CI]
Cloverleaf (z=2.3)
CI ( 3P2-3P1 )
PdBI
F10214 (z=2.3)
CI ( 3P1-3P0 )
30m
CI ( 3P1-3P0 )
30m
SMM 14011 (z=2.5)
CI ( 3P1-3P0 )
30m
2nd extra galactic CI ratio
L’CI(21) / L’CI(10)= 0.5, Tex = 30 K
[CI]/H2 ~ 3 x 10(-5)
PSS2322 (z=4.12)
CI ( 3P1-3P0 )
PdBI
March 27-31, 2006
Venice
Barvainis et al. 1997;
Weiss et al. 2003, 2004;
Pety et al. 2004
[[CII] 158 microns emission line detected in
J1148+5251 at z=6.42
Probing the physics of a PDR at the end of the reionisation epoch
CO(7-6)
CII
CI(1-0)
March 27-31, 2006
Venice
[CII] in J1148+5251
 Done at the 30-meter
 Massive starburst (2000 Msun/yr)
 Significant metal enrichment
 The ratio of the [CII] line
luminosity to the total far-infrared
luminosity is about 0.06%, i.e. an
order of magnitude smaller than
has been observed locally
 One of the 3 key scientific goals
of the ALMA project.
Maiolino, Cox et al. (2005)
March 27-31, 2006
Venice
Conclusions
 Physics and (chemistry) of the ISM in the early Universe
 CO measurements  physical conditions of the dense,
warm (40-100 K) gas in star-forming galaxies at
high redshifts: massive (1010 M), compact (<4 kpc),
dense (104 cm-3) and enriched (abundances ~ solar)
 Detection of species other than CO: HCN, HCO+, [CI] and
[CII]
 Some sources have been resolved with 1 kpc (~0.2”)
 Studies in the very early universe (< 1 Gyr):
- Metal enrichment
- Dynamical masses
March 27-31, 2006
Venice