Joint Scientific Opportunities of ALMA and GMT

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Joint Scientific Opportunities of ALMA and GMT

• Xiaohui Fan (Arizona)
• and the GMT SWG
• w/ help from Chris Carilli
• Mar 28, 2008

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(sub)mm astronomy unveiling the cold, obscured
universe
Wilson et al.
HST / OVRO CO
SCUBA
Cosmic Background Radiation
submm
Shirley et al.
B335 DSS
Opt/NIR
Franceschini 2000
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What is 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
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Technical Specifications

• 50 12-m antennas, 12 7-m antennas, 4 12-m Total
  Power
• Chajnantor 5000 m altitude site.
• Surface accuracy ?25 ?m, 0.6 reference pointing
  in 9m/s wind, 2 absolute pointing all-sky.
• Array configurations between 150m to 18km (ACA)
• 10 bands in 31-950 GHz Initially
• 86-119 GHz 3 125-169 GHz
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• 211-275 GHz 6 275-370 GHz
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• 385-500 GHz 8 602-720 GHz
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• 8 GHz BW, dual polarization.
• Flux sensitivity 0.2 mJy in 1 min at 345 GHz
  (median cond.).
• Interferometry, mosaicing total-power
  observing.
• Correlator 4096 channels/2GHz IF, full Stokes.
• Data rate 6MB/s average peak 60-150 MB/s.
• All data archived (raw images), pipeline
  processing.

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Giant Steps I Frequency and resolution
20mas at 0.9THz (300um)
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Giant Steps II Sensitivity
Index1.7
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Giant Steps III Image quality
HST quality imaging through with dense sampling
of uv plane
ACATP
Takakuwa et al. 2006
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Giant Steps IV Site quality
? 0.5 at 0.9 THz (300um)
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Giant Steps V Broad Band Spectroscopy

• Star forming Regions Line confusion limited
• Select lines as probes of density, temperature,
  excitation, evolutionary state, or dynamics
• Puts pressure on laboratory astrophysics, and
  data analysis/visualization S/W
• Extragalactic using ALMA to measure galaxyy
  redshifts

(Ziurys et al.)
SgrB2(N) 1 GHz spectrum using Band 6 mixer at the
SMT
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ALMA Site
ALMA
GMT
Santiago
San Pedro Mission
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ALMA Sites
To AOS (43km)
OSF Site (15km)
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Operations Support Facility, Dec 07
Visitors quarters
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First production antennas at OSF in Chile
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AOS Technical Building
AOS Technical Building March 2007
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• ALMA Status
• Antennas, receivers, correlator fully
  prototyped, now in production best (sub)mm
  receivers and antennas ever!
• Site construction well under way Observation
  Support Facility and Array Operations Site
• Cost to complete, including ALMA-J (then-yr)
  US1.2 Billion
• Timeline
• Q1 2007 First fringes at ATF (Socorro)
• Q1 2009 Three antenna array at AOS
• Q2 2010 First call for (early science)
  proposals
• Q4 2010 Start early science (16 antennas)
• Q4 2012 Full operations

ESO
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Key ALMA/GMT Science Goals

• Galaxy Formation and Evolution ALMA The
  ability to detect spectral line emission from CO
  or CII in a normal galaxy like the Milky Way at a
  redshift of z 3, in less than 24 hours of
  observation.
• Star and Planet Formation ALMA The ability to
  image the gas kinematics in protostars and in
  protoplanetary disks around young Sun-like stars
  at a distance of 150 pc
• High Resolution and High Fidelity Imaging ALMA
  The ability to provide images at an angular
  resolution of 0.01, and precise images at an
  angular resolution of 0.1.

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Magic of (sub)mm cosmology distance
independent method of studying objects in
universe from z0.8 to 10
current state-of-art
?obs 250GHz
FIR 1.6e12 L_sun
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ALMA Deep field normal galaxies at high z

• Detect current submm gal in seconds!
• ALMA deep survey 3days, 0.1 mJy (5s), 4
• HST few 1000 Gal, most at zlt1.5
• ALMA few 100 Gal, most at zgt1.5
• Parallel spectroscopic surveys, 100 and 200 GHz
  CO/other lines in majority of sources
• Redshifts, dust, gas masses
• High res. images of gas dynamics, star formation

HST
z lt 1.5
z gt 1.5
ALMA
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ALMAGMT normal galaxies during
reionization State of art Ly? galaxies in
COSMOS
NB850nm
Murayama et al. 07

• Ly??????????? 10 Mo/yr
• Galaxies responsible for reionization?
• MAMBO ltS250gt lt 2mJy gt SFRlt300
• VLA ltS1.4gt lt 2.5uJy gt SFRlt125
• ALMA - Detect dust (20uJy at 250GHz) in 3 hours
• Determine redshifts for dusty galaxies from mm
  spectroscopy

VLA Stacking analysis
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Probing High-z Galaxy/BH Formation

• SDSS J11485251
• z6.42, MBH3x109Msun
• Fine structure lines CII 158umdominant ISM
  gas cooling line, from with PDRs associated with
  star forming clouds
• ALMA
• Multiple ISM lines, broad-band spectroscopy
• Gas dynamics at sub-kpc
• GMT
• Galaxy morphology and stellar properties
• BH growth and accretion

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GMTALMA A Panchromatic view of galaxy formation
Arp 220 vs z
ALMA reveals the cool universe dust and gas, the
fundamental fuel for star formation
cm Star formation, AGN
(sub)mm Dust, molecular gas
GMT
Near-IR Stars, ionized gas, AGN
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GMTALMAStar Formation and Dynamics in Galaxies
Star Formation Rate in galaxies GMT UV, Ha ALMA
dust, molecular lines
Chemistry and gas dynamics GMT AO-aided
IFU ALMA high res CO map
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Probing Star Formation

• GMT
• AO imaging and resolved spectra
• Near-/mid-IR high resolution spectroscopy
• ALMA
• Dust continuum and multiple lines
• Probing detailed physical conditions of
  protostars
• Geometry, ionization, infall/outflow,
  accretion/jets, B field etc.

Brogan SMA CephA-East hot core HW2
(725pc) Disk, Double, or Outflow?
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Debris Disks and Protoplanets

• GMT direct AO imaging of planet formation
  zones
• ALMA disk imaging from dust continuum
• GMTALMA gas dynamics, temp and composition

ALMA 850 GHz 20mas
HST
Williams et al.
Wolf Simulation of nearby PP disk (eg. TW Hy)
5AU 0.1
S. Kenyon
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Indirect Detection of Planets

• ALMA would measure this motion accurately in its
  long configuration at submm wavelengths.
• ALMA could detect photospheres of e.g. 1000 stars
  well enough to detect a 5Jovian mass planet at
  5AU
• Inclination ambiguities for companions now known
  could be resolved.

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Summary

• ALMA will be a transformational facility for
  sub/mm astronomy order(s) of mag improvement in
  resolution, sensitivity and spectral coverage
• ALMA and GMT sample the same Southern sky and
  probe similar physical scales yet reveal
  different and complementary physical processes.
• ALMA and GMT have strong synergy in most key
  science areas
• First light (zgt7)
• Galaxy formation and evolution
• Star formation and ISM
• Planet and protoplanetary disk

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Complete Frequency Access
Construction Project Bands 3, 6, 7 9.
Proposed by Japan 4, 8 10. Post-construction
1, 2 5
N.B. Band 1 31.3-45 GHz not shown