ALMA Presentation

1
Lunatic fringe probing the dark ages from the
dark side of the Moon C. Carilli (NRAO), Sackler
Cosmology Conf, Cambridge, MA, 2008
Judd
Jackie
2
Radio astronomy pushing into reionization gas,
dust, star formation in QSO host galaxies at zgt6
J11485251 z6.42

• Supermassive black hole
• Lbol 1e14 Lo
• Black hole 3 x 109 Mo
• Gunn Peterson trough gt near edge of
  reionization

• Host galaxy Massive reservoir of gas and dust
  fuel for galaxy formation
• Dust mass 7e8 Mo
• Gas mass 2e10 Mo

3
Fine structure lines CII 158um at z6.4

• Dominant ISM gas coolant star formation tracer
  
• zgt4 gt FS lines observed in (sub)mm bands
• CII size 6kpc molecular gas gt
  distributed star formation
• SFR 6.5e-6 LCII 3000 Mo/yr

IRAM 30m
CII
NII
Plateau de Bure
1
CII CO 3-2
4
Break-down of black hole -- bulge mass relation
at very high z BH forms first?
High z QSO hosts Low z QSO hosts Other low z
galaxies
5
Extreme downsizing building giant elliptical
galaxies SMBH at tuniv lt 1Gyr
10.5
Li et al.

• Radio detections at zgt5.7 only direct probe of
  host galaxies
• 10 dust (1/3 of QSO sample) gt dust mass gt 1e8
  Mo
• 4 CO gt gas mass gt 1e10 Mo
• 2 CII gt SFR gt 1000 Mo/yr

8.1

• Harvard models stellar mass 1e12 Mo forms in
  series of major, gas rich mergers starting at
  z14, driving SFR gt 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
• Rapid enrichment of metals, dust, gas within 1
  Gyr of Big Bang
• Currently limited to pathologic objects
  (HyLIRGs FIR gt 1e13 Lo)

6
AOS Technical Building
Atacama Large Millimeter Array an order of
magnitude, or more, improvement in all areas of
(sub)mm interferometry, at 5000m in Chile
(half-way to the Moon)

• ALMA will have uJy line sensitivity in few hours
  gt image gas, dust in normal galaxies (LBGs,
  LAEs) to z 10
• Early science Q4 2010

7

• Dark ages lt 90 MHz. HI 21cm signal is the only
  method for probing (linear) structure formation
  into Dark Ages. VLF gt possible lunar imperative?
• Reionization 100 MHz to 200 MHz, HI 21cm signal
  being explored by path-finders

Dark Ages 15 lt z lt 200
Age of enlightenment 6 lt z lt 15
8
Long History of Lunar Low Freq Telescope

• Gorgolewski 1965 Ionospheric opacity
• Ionosphere ?p 10 MHz
• ISM ?p 0.1 MHz
• Interstellar scattering gt size 1o (?/1 MHz)-2
• Faraday rotation gt no polarization
• z gt 140 gt not (very) relevant for HI 21cm
  studies, beyond dark ages

New window
Lunar window
ion. cutoff 30m
ISM cutoff 3km
9

• Return to moon is Presidential national security
  directive (an order, not a request).
• Summary of STScI Workshop, Mario Livio, Nov. 2006
• The workshop has identified a few important
  astrophysical observations that can potentially
  be carried out from the lunar surface. The two
  most promising in this respect are
• Low-frequency radio observations from the lunar
  far side to probe structures in the high redshift
  (10 lt zlt 100) universe and the epoch of
  reionization
• Lunar ranging experiments

Our concensus Lunar imperative awaits lessons
from ground-arrays
10
Heavy lifting future launch vehicles

• 10m diameter faring
• Lifting power 65 tons to Moon

Ares I
Ares V
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Lunar Advantage I Ionospheric phase distortions

• Size 1 (??????z)-2 lt typical scales of
  interest
• Scattering can lead to calibration errors gt
  dynamic range limits
• DR N/(21/2 ??rad)
• Required DR 1e6
• gt ?? lt 0.02o

Virgo A field, VLA 74 MHz Lane 02
12

• Lunar ionosphere?
• -- LUNA orbiter detected plasma layer gt 10 km
  above surface
• -- Apollo surfacesubsatellite detected
  photoionized layer extending to 100km
• -- ?p 0.2 to 1 MHz
• large day/night variation
• small ?e does not necessarily imply small
  electronic pathlength variations

Clementine (NRL) star tracker
See talk by J. Lazio
13
Advantage II Interference Lunar shielding of
Earths auroral emission at low freq (Radio
Astronomy Explorer 1975)
12MHz
Alexander 1975
14
The Moon is radio protected

• ARTICLE 22
• (ITU Radio Regulations)
• Space services
• Section V Radio astronomy in the shielded
  zone of the Moon
• 22.22 8 1) In the shielded zone of the Moon31
  emissions causing harmful interference to radio
  astronomy observations32 and to other users of
  passive services shall be prohibited in the
  entire frequency spectrum except in the following
  bands
• 22.23 a) the frequency bands allocated to the
  space research service using active sensors
• 22.24 b) the frequency bands allocated to the
  space operation service, the Earth
  exploration-satellite service using active
  sensors, and the radiolocation service using
  stations on spaceborne platforms, which are
  required for the support of space research, as
  well as for radiocommunications and space
  research transmissions within the lunar shielded
  zone.
• 22.25 2) In frequency bands in which emissions
  are not prohibited by Nos. 22.22 to 22.24, radio
  astronomy observations and passive space research
  in the shielded zone of the Moon may be protected
  from harmful interference by agreement between
  administrations concerned.

15

• Other advantages
• Easier deployment robotic or human
• Easier maintenance (no moving parts)
• Less demanding hardware tolerances
• Very large collecting area, undisturbed for long
  periods (no weather, no animals, not many people)

Miguel
Avi
16
Lunar challenges dark age signal sensitivity

• Statistical detection
• 1 SKA, 1 yr, 30MHz (z50), 0.1MHz
• TBsky 100 (?/200MHz)-2.7 K
• 1.7e4 K
• At l3000, k0.3 Mpc-1
• Signal 2 mK
• Noise PS 1 mK
• Requires few SKAs

17
Other challenges

• Array data rates (Tb/s) gtgt telemetry limits,
  requiring in situ processing, ie. low power super
  computing (LOFAR/Blue Gene 0.15MW)
• RFI shielding How far around limb is required?
• Thermal cycling (mean) 120 K to 380 K
• Radiation environment
• Regolith dielectric/magnetic properties

Lunar shielding at 60kHz Takahashi Woan
Apollo 15
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Solution polar craters of eternal darkness,
peaks of eternal light eternal power
Tsiolkovsky crater (100 km diameter) 20S 129E
But how sharp is the knifes edge?
Apollo 15
19

• DALI - LAMA A path to enlightenment
• NASA funded joint design study
• Dark Ages Lunar Interferometer (Lazio)
• Lunar Array for Measuring 21cm Anisotropies
  (Hewitt)

Science (Loeb, Furlanetto) Science requirements
(Carilli, Taylor) Antennas (Bradley,
MacDowall) Receivers (Backer, Ellingson) Correlato
r (Ford, Kasper) Data communication (Ford,
Neff) Site selection (Hoffman, Burns) Deployment
(de Weck, DeMaio) Engineering power/mech/therm
Goal DS2010 white paper with mission concept,
(rough) costing, and technological roadmap
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• Interim programs
• Orbiter RFI, ion
• First dipoles environ., phase stability
• Global signal

lt2010 mission concept study
2010 -- 2020 technology development
2020 -- 2025 Design/Fabrication/Test
2026 operations
21
Budget WAG (Hewitt/LARC)
ARES V Launch fee 700M Total 2G
22
Say, its only a PAPER moon Sailing over a
cardboard sea But it wouldn't be make-believe If
you believed in me
Don
Rich
23
END
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SMA
Pushing to first normal galaxies spectral lines
cm telescopes low order molecular transitions --
total gas mass, dense gas tracers
, GBT
(sub)mm high order molecular lines. fine
structure lines -- ISM physics, dynamics

• FS lines will be workhorse lines in the study of
  the first galaxies with ALMA.
• Study of molecular gas in first galaxies will be
  done primarily with cm telescopes

ALMA will detect dust, molecular and FS lines in
1 hr in normal galaxies (SFR 10 Mo/yr
LBGs, LAEs) at z 6, and derive z directly from
mm lines.
25

• European Aeronautic Defence and Space
  Corporation/ASTRON (Falcke)
• Payload 1000 kg (Ariane V)
• 100 antennas at 1-10 MHz 1/10 SKA

26

Continuum SED and CO excitation ISM physics at
z6.42
Elvis QSO SED
50K
NGC253
Radio-FIR correlation
MW

• FIR excess -- follows Radio-FIR correlation
  SFR 3000 Mo/yr
• CO excitation starburst nucleus Tkin 100K,
  nH2 1e5 cm-3

27

• Deployment
• Javelin
• ROLS polyimide circuit-imprinted film
• Dipoles robotic with rover
• Dipoles manually

28
Chippendale Beresford 2007
Lunar advantage II terrestrial interference
shielding
100 people km-2
100 people km-2
1 km-2
1 km-2
0.01 km-2
0.01 km-2
Moon?
0 km-2