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Title: Radio astronomical probes of cosmic reionization and the first galaxies


1
Radio astronomical probes of cosmic reionization
and the first galaxies Chris Carilli (NRAO),
McGill University, October 2009
  • Brief introduction to cosmic reionization
  • Objects within reionization recent observations
    of molecular gas, dust, and star formation, in
    the host galaxies of the most distant QSOs early
    massive galaxy and SMBH formation
  • Neutral Intergalactic Medium (IGM) HI 21cm
    telescopes, signals, and challenges
  • Dramatic advances with next gen instruments
    ALMA, EVLA

Wang, Walter, Wagg, Riechers, Fan, Strauss,
Bertoldi, Cox, Menten, Neri
2
Ionized
Neutral
Reionized f(HI) lt 10-5
3
Chris Carilli (NRAO) Berlin June 29, 2005
WMAP structure from the big bang
4
Hubble Space Telescope Realm of the Galaxies
5
Dark Ages
  • Last phase of cosmic evolution to be tested
  • Bench-mark in cosmic
  • structure formation
  • indicating the first
  • luminous structures

Cosmic Reionization
6
Constraint I Gunn-Peterson Effect
z
Barkana and Loeb 2001
7
Constraint I Gunn-Peterson Effect
  • End of reionization?
  • f(HI) lt1e-4 at z 5.7
  • f(HI) gt1e-3 at z 6.3
  • Limitation Universe becomes optically thick at
    low f(HI)

Fan et al 2006
8
Constraint II CMB large scale polarization
Thomson scattering during reionization
  • Scattering CMB local quadrapole gt polarized
  • Large scale horizon scale at reioniz 10s deg
  • Signal is weak
  • TE 10 TT
  • EE 1 TT

Hinshaw et al 2008
?e 0.084 /- 0.016
9
Constraint II CMB large scale polarization
  • Rules-out high ionization fraction at zgt 15
  • Allows for finite (0.2) ionization to high z
  • Most action occurs at z 8 to 14
  • Limitation broad range in allowed model
    parameters

Dunkley et al. 2008
10
Fan, Carilli, Keating ARAA 06
ltVolgt
GP gt First light occurs in twilight zone,
opaque for ?obs lt0.9 ?m
  • GP gt pushing into tail-end of reionization at z
    6
  • CMB pol gt substantial ionization fraction
    persists to z 11

11
Massive galaxy formation at z6 gas, dust, and
star formation in quasar host halaxies
  • Radio astronomy unveiling the cool, obscured
    Universe
  • mm continuum thermal emission from warm dust gt
    star formation
  • (sub)mm lines high order molecular lines,
    atomic fine structure lines gt ISM physics
  • (short) cm lines low order molecular lines gt
    gas mass, dynamics
  • cm continuum synchrotron emission gt star
    formation, AGN

Wilson et al.
HST / OVRO CO
cm/mm rich in line continuum diagnostics
12
Powerful suite of existing telescopes
  • IRAM 30m MAMBO sub-mJy sens at 250 GHz
    wide fields ? dust
  • IRAM PdBI sub-mJy sens at 90 and 230 GHz
    arcsec resol. ?mol. Gas, CII
  • VLA uJy sens at 1.4 GHz ? star formation
  • VLA lt 0.1 mJy sens at 20-50 GHz 0.2 resol.
    ? mol. gas (low order)

13
SDSS J11485258 z6.42
Why quasars?
  • Spectroscopic redshifts
  • Extreme (massive) systems
  • Lbol 1e14 Lo
  • MBH 1e9 Mo
  • Rapidly increasing samples
  • zgt4 gt 1000 known
  • zgt5 gt 100
  • zgt6 20
  • Note will not discuss MBH


J1148525 VLA CO3-2
14
QSO host galaxies MBH -- Mbulge relation
Haaring Rix
  • Most (all?) low z spheroidal galaxies have SMBH
    MBH0.002 Mbulge
  • Causal connection between SMBH and spheroidal
    galaxy formation
  • Luminous high z QSOs have massive host galaxies
    (1e12 Mo)

15
Dust and star formation MAMBO 250GHz surveys 1/3
of zgt2 quasars have S250 gt 2mJy
HyLIRG
  • Wang sample 33 quasars at zgt5.7 (mostly SDSS)
  • LFIR 0.3 to 1.3 x1013 Lo HyLIRG (47K, ß
    1.5)
  • Mdust 1.5 to 5.5 x108 Mo 10x MW (?125um
    19 cm2 g-1)

16
  • Dust formation at tunivlt1Gyr?
  • AGB Winds 1.4e9yr gt dust formation?
  • High mass star formation (Dwek, Shull, Nozawa)
  • Smoking quasars dust formed in BLR winds
    (Elvis)
  • Extinction toward z6.2 QSO and 6.3 GRB gt
    larger, silicate amorphous carbon dust grains
    formed in core collapse SNe vs. eg. graphite?

SMC, zlt4 quasars
Galactic
z6.2 quasar, GRB
Maiolino, Stratta
17
Dust heating star formation? Radio to near-IR
SED
Elvis SED TD 1000K
TD 47 K
  • FIR not correlated with LB
  • FIR excess 47K dust
  • Radio-FIR SED consistent with star forming
    galaxy gt
  • SFR 400 to 2000 Mo yr-1

Radio-FIR correlation
18
Fuel for star formation? Molecular gas 8 CO
detections at z 6 with PdBI, VLA
  • Mgas 0.7 to 3 x1010 (a/0.8) Mo
  • Accurate redshifts ? z 0.001 (vs. optical ? z
    gt 0.03)

19

CO excitation Dense, warm gas, thermalized to
6-5
Tk 50 K nH2 104.2 cm-3
J1148 J1048
Giant Molecular Cloud (50pc) 100 to 1000
cm-3 GMC cores (lt1pc) gt 104 cm-3
20
LFIR vs L(CO) integrated Kennicutt-Schmidt SF
law
  • Star formation efficiency(SFR/Mgas) increases
    with increasing SFR
  • Gas depletion timescale(Mgas/SFR) decreases with
    SFR
  • Need gas re-supply to build GE

SFR
1e3 Mo/yr
Index1.5
1e11 Mo
Mgas
FIR 1e10 Lo/yr gt tdep 3e8yr FIR 1e13
Lo/yr gt tdep 1e7yr
21
114852 z6.42 VLA imaging at 0.15 resolution
CO3-2 VLA
IRAM
0.3
1 5.5kpc
  • Size 6 kpc
  • Two peaks separated by 2kpc with sizes 1kpc,
    M(H2) 5 x109 Mo
  • TB 35 K gt approaching optically thick

22
Gas dynamics CO velocities
z4.19
z4.4
-150 km/s
150 km/s
  • Dynamical mass (r lt 3kpc) 0.4 to 2 x1011 Mo
  • M(H2)/Mdyn gt 10

23
Break-down of MBH -- Mbulge relation at very high
z Use CO rotation curves to get host galaxy
dynamical mass
High z QSO hosts Low z QSO hosts Other low z
galaxies
Perhaps black holes form first? but Lauer Bias
for optically selected quasars or All highly
inclined i lt 20o
Riechers
24
CII 158um (2P3/2 - 2P1/2)
  • Dominant ISM gas cooling line (Spitzer 1976)
  • Traces CNM and PDRs
  • COBE CII 10x more luminous than any other mm
    to FIR line in MW 1 Lgal
  • zgt4 gt FS lines observed in (sub)mm bands at zgt6
    gt Bure!

Bennett et al.
25
CII 158um search in z gt 6.2 quasars
  • J11485251 z6.42
  • SCII 10mJy
  • LCII 4x109 Lo (LNII lt 0.1LCII )
  • J16233112 z6.25
  • SCII 3mJy
  • S250GHz lt 1mJy

Kundsen, Bertoldi, Walter, Maiolino
26
Maximal star forming disk (Walter 2009)
1
PdBI 250GHz 0.25res
  • CII size 1.5 kpc gt SFR/area 1000 Mo yr-1
    kpc-2
  • Maximal starburst (Thompson, Quataert, Murray
    2005)
  • Self-gravitating gas disk
  • Vertical disk support by radiation pressure on
    dust grains
  • Eddington limited SFR/area 1000 Mo yr-1 kpc-2
  • eg. Arp 220 on 100pc scale, Orion SF cloud cores
    lt 1pc

27
Summary of cm/mm observations of 33 quasar host
galaxies at zgt5.7
J14253254 CO at z 5.9
J1048 z6.23 PdBI, VLA
  • Only direct probe of host galaxies of most
    distant quasars
  • 11 in dust gt Mdust gt 1e8 Mo Dust formation in
    Sne?
  • 10 at 1.4 GHz continuum Radio FIR SED gt SFR
    1000 Mo/yr
  • 8 in CO gt Mgas gt 1e10 Mo Fuel for star
    formation in galaxies, GMC core conditions over
    kpc-scales
  • 2 in CII gt maximal star forming disk 1000
    Mo yr-1 kpc-2

28
Building a giant elliptical galaxy SMBH at
tunivlt 1Gyr
10
  • Multi-scale simulation isolating most massive
    halo in 3 Gpc3
  • Stellar mass 1e12 Mo forms in series (7) of
    major, gas rich mergers from z14, with SFR ? 1e3
    Mo/yr
  • SMBH of 2e9 Mo forms via Eddington-limited
    accretion mergers
  • Evolves into giant elliptical galaxy in massive
    cluster (3e15 Mo) by z0

6.5
Li, Hernquist et al.
Li, Hernquist
  • Rapid enrichment of metals, dust in ISM (z gt 8)
  • Rare, extreme mass objects 100 SDSS z6 QSOs
    on entire sky

29
Cosmic Stromgren Sphere
  • Accurate host redshift from CO z6.419/0.001
  • Proximity effect photons leaking from
    6.32ltzlt6.419

White et al. 2003
z6.32
  • time bounded Stromgren sphere R 4.7 Mpc
  • tqso 1e5 R3 f(HI) 1e7yrs
  • f(HI) 1 (tqso/1e7 yr)

30
CSS 24 quasars with accurate zGP, zhost (mostly
CO, MgII)
  • ltRpgt 7.3 Mpc gt f(HI) 0.05 at z6 for
    tqso 107 yrs
  • Decrease ltRpgt from 9.4 Mpc at z5.7 to 4.0 Mpc
    at z6.4 gt increase in f(HI) by factor 9

Fan
Rp 7.3 7.1(z-6) Mpc
31
Fan, Carilli, Keating ARAA 2006
  • Not event but complex process, large
    variance zreion 14 to 6
  • Good evidence for qualitative change in nature
    of IGM at z6

ESO
32
Local ioniz.?
  • Current probes are all fundamentally limited in
    diagnostic power
  • Need more direct probe of process of reionization

ESO
33
Studying the pristine neutral IGM using
redshifted HI 21cm observations (100 200 MHz)
  • Large scale structure
  • cosmic density, ?
  • neutral fraction, f(HI)
  • Temp TK, TCMB, Tspin

1e13 Mo
1e9 Mo
34
Pathfinders 1 to 10 SKA
21CMA (China) 10,000 Dipole array working in
Western China 2008
MWA (MIT/CfA/ANU) 32 Tile array deployment in WA
2009
Site Type Freq MHz Area m2 Goal Date
GMRT India Parabola 150-165 4e4 CSS 2009
21CMA China Dipole 70-200 1e5 PS 2008
PAPER GB/Oz/SA Dipole 110-200 5e3 PS/CSS 2009
MWAdemo Oz Aperture 80-300 1e4 PS/CSS 2009
LOFAR NL Aperture 115-240 1e5 PS/CSS 2010
SKA ?? Aperture 30-300 1e6 Imaging ??
35
Signal I HI 21cm Tomography of IGM Furlanetto,
Zaldarriaga 2004
9
z12
  • ?TB(2) 10s mK
  • SKA rms(100hr) 4mK
  • LOFAR rms (1000hr) 80mK

7.6
36
Signal II 3D Power spectrum analysis
? only
LOFAR
? f(HI)
SKA
McQuinn 06
37
Signal III IGM after reionization cosmic web
Ly alpha forest at z3.6 (? lt 10)
Womble 96
  • N(HI) 1013 1015 cm-2, f(HI/HII) 10-5 --
    10-6 gt before reionization N(HI) 1018 1021
    cm-2
  • ?Lya 107 ?21cm gt neutral IGM opaque to Lya,
    but translucent to 21cm

38
Signal III Cosmic web before reionization HI
21Forest
z12
z8
19mJy
130MHz
159MHz
  • Perhaps easiest to detect
  • Only probe of small scale structure
  • Requires radio sources expect 0.05 to 0.5 deg-2
    at zgt 6 with S151 gt 6 mJy?
  • radio G-P (?1)
  • 21 Forest (10)
  • mini-halos (10)
  • primordial disks (100)

39
Signal IV Cosmic Stromgren spheres around z gt 6
QSOs
  • LOFAR observation
  • 20xf(HI)mK, 15,1000km/s
  • gt 0.5 x f(HI) mJy
  • Pathfinders Set first hard limits on f(HI) at
    end of cosmic reionization

5Mpc
Wyithe et al. 2006
Prediction first detection of HI 21cm signal
from reionization will be via imaging rare,
largest CSS
0.5 mJy
40
Challenge I Low frequency foreground hot,
confused sky
0.5 to 5.0 GHz
Haslam Eberg 408MHz
  • Coldest regions T 100 (?/200 MHz)-2.6 K
  • Highly confused 1 source/deg2 with S140 gt 1
    Jy
  • Synch. smooth 100MHz vs. 21cm lines 1 MHz
  • Dynamic range gt daily calibration errors lt 0.2
    (Datta )

41
Challenge II Ionospheric phase errors varying
e- content
  • TIDs fuzz-out sources
  • Isoplanatic patch few deg few km
  • Phase variation proportional to ?2
  • Solution Wide field rubber screen phase
    self-calibration using data-rich sky

15
Virgo A VLA 74 MHz Lane 02
42
Challenge III Interference
100 MHz z13
200 MHz z6
  • Solutions -- RFI Mitigation (Ellingson06)
  • Digital filtering
  • Beam nulling
  • Real-time reference beam
  • LOCATION!

Aircraft
Orbcom
TV
43
VLA-VHF 180 200 MHz Prime focus X-dipole
Greenhill, Blundell (SAO) Carilli, Perley (NRAO)
Leverage existing telescopes, IF, correlator,
operations
  • 110K DD/construction (CfA)
  • First light Feb 16, 05
  • Four element interferometry May 05
  • First CSS detection Winter 06/07

44
Project abandoned Digital TV
KNMD Ch 9 150W at 100km
45
RFI mitigation location, location location
100 people km-2
1 km-2
0.01 km-2
Chippendale Beresford 2007
46
PAPER Precisions Array to Probe the Epoch of
Reionization PI Backer (UCB), Bradley
(NRAO) Western Australian deployment in 2008
  • Optimize for reionization PS/CSS
  • FoV 30deg, short baselines lt 0.6km
  • Staged engineering GB06 8 stations ? WA08 8
    stations ? SA09 32

47
PAPER Staged Engineering
  • Broad band sleeve dipole flaps
  • FPGA-based pocket correlator from Berkeley
    wireless lab
  • S/W Imaging, calibration, PS analysis AIPY
    Miriad/AIPS gt Python CASA, including
    ionospheric peeling calibration

100MHz
200MHz
Beam response
BEE2 5 FPGAs, 500 Gops/s
48
PAPER in Green Bank2008 Mar
130-170 MHz 7 Dipole 24-hour integration
Parsons 2009
  • Current arrays First light at 1 Jy rms
  • Long campaigns in WA/SA in 2010 gt first limits
    to PS/CSS?

49
Giant steps in cm First galaxies and the EVLA
  • By building on the existing infrastructure,
    multiply ten-fold the VLAs observational
    capabilities, including
  • 10x continuum sensitivity (lt1uJy)
  • full frequency coverage (1 to 50 GHz)
  • 80x BW (8GHz)
  • Critical element Canadian WIDAR correlator
    (DRAO)!

50
Giant steps in (sub)mm First galaxies and
ALMA North American, European, Japanese, and
Chilean collaboration to build operate a large
millimeter/submm array at high altitude site
(5000m) in northern Chile -gt order of magnitude,
or more, improvement in all areas of (sub)mm
astronomy, including resolution, sensitivity, and
frequency coverage.
50 x 12m array
Atacama Compact Array 12x7m 4x12m TP
51
Pushing to normal galaxies spectral lines
100 Mo yr-1 at z5
cm telescopes low order molecular transitions --
total gas mass, dense gas tracers
(sub)mm high order molecular lines. fine
structure lines -- ISM physics, dynamics
52
Pushing to normal galaxies continuum A
Panchromatic view of 1st galaxy formation
100 Mo yr-1 at z5
cm Star formation, AGN
(sub)mm Dust, FSL, mol. gas
Near-IR Stars, ionized gas, AGN
53
  • EVLA Status
  • Antenna retrofits now 50 completed.
  • Early science start in Q1 2010 using new
    correlator, proposal deadline Oct 1, 2009
  • Full receiver complement completed 2012.

54
AOS Technical Building
  • ALMA status
  • Antennas, receivers, correlator in production
    best submm receivers and antennas ever!
  • Site construction well under way Observation
    Support Facility, Array Operations Site, first
    antennas at high site

Array operations center
Antenna commissioning in progress
  • North American ALMA Science Center (CVille)
    support early science Q4 2010, full ops Q4 2012

55
  • Probing the Dark Ages using a Lunar low frequency
    array
  • No interference
  • No ionosphere
  • Only place to study dark ages (lt 60 MHz)

10MHz
Recognized as top astronomy priority for NASA
initiative to return Man to Moon (Livio 2007)
RAE2 1973
56
J. Burns, PI Colorado
A2010 White paper lunar radio array (Lazio
) http//lunar.colorado.edu/
57
END
ESO
58
CII
z gt4
  • CII/FIR decreases with LFIR lower gas
    heating efficiency due to charged dust grains gt
    luminous starbursts are still hard to detect in
    C
  • Normal star forming galaxies are not much harder
    to detect
  • HyLIRG at zgt 4 no worse than low z ULIRG
  • Dont pre-select on dust

Malhotra, Maiolino, Bertoldi, Knudsen, Iono,
Wagg
59
Sources responsible for reionization
  • Luminous AGN No
  • Star forming galaxies maybe -- dwarf galaxies
    (Bowens05 Yan04)?
  • mini-QSOs -- unlikely (soft Xray BG Dijkstra04)
  • Decaying sterile neutrinos -- unlikely (various
    BGs Mapelli05)
  • Pop III stars zgt10? midIR BG (Kashlinsky05),
    but trecomb lt tuniv at z10

Needed for reion.
60
Signal I Global (all sky) reionization
signature
Signal 20mK lt 1e-4 sky
Feedback in Galaxy formation No Feedback
Possible higher z absorption signal via Lya
coupling of Ts -- TK due to first luminous
objects
Furlanetto, Oh, Briggs 06
61
S?
M82 radio-FIR SED All mechanisms ? massive star
formation rate
Thermal dust 20 -- 70K
z
Synchrotron
Radio-FIR
Free-Free
SFR (Mo/yr) 3e-10 LFIR (Lo/yr) SFR (Mo/yr)
6e-29 L1.4 (erg/s/Hz) ? (ULIRGs) 0.8 Mo (K km
s-1 pc2)-1
62
Building a giant elliptical galaxy SMBH at
tunivlt 1Gyr
10
  • Multi-scale simulation isolating most massive
    halo in 3 Gpc3
  • Stellar mass 1e12 Mo forms in series (7) of
    major, gas rich mergers from z14, with SFR ? 1e3
    Mo/yr
  • SMBH of 2e9 Mo forms via Eddington-limited
    accretion mergers
  • Evolves into giant elliptical galaxy in massive
    cluster (3e15 Mo) by z0

6.5
Li, Hernquist et al.
  • Rapid enrichment of metals, dust in ISM (z gt 8)
  • Rare, extreme mass objects 100 SDSS z6 QSOs
    on entire sky

63
Radio astronomy probing cosmic reionization
  • GP gtTwilight zone obs of 1st galaxies
    limited to near-IR to radio
  • Current mm/cm observations reveal coeval
    formation SMBH giant elliptical galaxies in
    spectacular starbursts at tunivlt1Gyr
  • Low freq pathfinders HI 21cm signatures of
    neutral IGM
  • SKA imaging of IGM

64
Chromatic aberration Frequency differencing with
MHz channels doesnt work well due to frequency
dependent far-out sidelobes
142, 174 MHz
Datta
  • Dynamic range requirements on calibration errors
  • Daily cal errors lt 0.2
  • Monthly cal errors lt 0.01
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