Radio, Millimeter and Submillimeter Planning Group
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Transcript of Radio, Millimeter and Submillimeter Planning Group
Radio, Millimeter and Submillimeter Planning Group
Martha P. Haynes (Cornell University)on behalf of the RMSPG
Astronomy and Astrophysics Advisory CommitteeFebruary 15, 2005
R*M*S Planning GroupPremise: Recommendations as outlined in:
Astro & Astrophys in the New MilleniumFrom the Sun to the Earth – And BeyondConnecting Quarks with the CosmosNew Frontiers in the Solar System
Objective: Update/Implementation PlanMembership: Same as 2000 AASC Radio/Submm Panel
•Martha Haynes, Cornell/NAIC•Geoff Blake, Caltech•Don Campbell, Cornell•John Carlstrom, Chicago•Neal Evans, Texas•Jackie Hewitt, MIT
•Ken Kellermann, NRAO•Alan Marscher, BU•Jim Moran, Harvard•Steve Myers, NRAO•Mark Reid, SAO•Jack Welch, Berkeley
– A community “volunteer” effort– Funding to date provided by AUI– No special interaction with AUI/NRAO director
http://www.astro.cornell.edu/~haynes/rmspgSite includes a compilation of RMS facilities
R*M*S Astronomy
• RMS science addresses a broad range of key astrophysical questions, either uniquely (e.g. CMB, microarcsec imaging, nanosecond pulsar timing, radar) or in complement with other datasets.
• RMS facility portfolio (National + University facilities) provides observing capability over 5 orders of magnitude in wavelength (10 MHz to 1+ THz) and angular scales down to 100 microarcseconds.
• Support for the RMS community is crucial. – Effective return on facilities investment– Balance of large versus small science– Hands-on training of next generation
• The US program is arguably foremost in the world and almost exclusively in the NSF domain.
Key points
Foremost Science Questions
• How did the Universe begin? (CMB experiments)
• What is the fate of the Universe? (SKA)
• How did the “Dark Ages” end? (MWA, PaST, LWA, SKA)
• When and how did the first galaxies form? (ALMA, CSO/CCAT, EVLA, VLBA/HSA, GBT, surveys)
• When and how did supermassive black holes form? (EVLA, ALMA, SKA, VLBA/HSA)
• Was Einstein right? (Arecibo, GBT, EVLA, SKA)
• How do stars and substellar objects form? (CSO/CCAT, LMT, ALMA, CARMA, SMA, VLBA/HSA)
• How do planets form? (ALMA)
• Does extraterrestrial life exist? (ATA, Arecibo)
RMS: Centimeter to Meter Wavelengths National Center Facilities
Arecibo 0.3 - 10 GHz 3.5’ at 21cm Collecting area
GBT 0.1 - 115 GHz 9’ at 21 cm Unblocked aperture
EVLA 0.1 - 50 GHz 0.4” at 6cm Imaging array
VLBA 0.3 - 96 GHz .001” at 86 GHz Imaging array
•National facilities are the world’s best radio telescopes.
•There are no comparable “private” facilities but partnership needed with university community for future developments (surveys, ATA, LWA, MWA, SKA).
•National centers provide both access and leadership.
“The radio astronomy community is justifiably proud of both its national centers, NRAO and NAIC, ...”
2000 AASC Radio & Submillimeter Panel Report
Arecibo: Revolutionized Capabilities
Exploit the big dish’s HIGH SENSITIVITY and RADAR capability• Surveys with ALFA (galactic and extragalactic)• Pulsar surveys and timing (tests of GR)• Statistical characterization of continuum transients• High Sensitivity Array for VLBI (time domain, mJy VLBI)• Solar System radar• SKA testbed: wide bandwidth (2-11 GHz) focal plane array• Partnerships for surveys, instrumentation, software etc.
GBT: Revolutionized Capabilities
• Unblocked aperture (galactic HI)• Active surface (high frequencies)• Full steerability (70% of sky)• Location in NRQZ (low RFI)• Wide frequency coverage
– 3mm bolometer array– Wideband spectrometer– Dynamic scheduling
Exploit the GBT’s unique characteristics:
EVLA: Revolutionized CapabilitiesMultiply by at least 10X the capabilities of the VLA
• Increased continuum sensitivity by 2 – 40 X• Complete frequency coverage from 1 – 50 GHz• Noise limited imaging in all bands• Huge increase in spectral capabilities
– Correlator contributed by Canada• Increase spatial resolution by 10X (NM Array)• e2e user access tools and data products
VLBA/HSA: sub-mJy at sub-mas• The VLBA is the world’s only dedicated VLBI array.
– Full complement of instrumentation– Time critical images of motions and source evolution– Unparalleled astrometry (microarcsec accuracy)
• High Sensitivity Array (HSA) + Arecibo/GBT/VLA– Sub-milliarcsec resolution at sub-mJy levels
• eVLBI: (near) real-time imaging
RMS: Centimeter to Meter WavelengthsDevelopment program for this decade
• Enhance capabilities of existing instruments, emphasizing unique capabilities of Arecibo, EVLA, GBT , VLBA and HSA
• Develop new approaches, leading towards Next Generation Radio Telescope = SKA
– EVLA-II: the path to the high frequency SKA– ATA: demo of “large N/small D” concept– MWA: 80-300 MHz for EOR/transients– LWA: 15-80 MHz to open new window
• Develop a dedicated Solar capability = FASR
• Make telecopes easier to use and produce uniform, publicly accessible images and data products (e2e)
• Foster the training of young scientists
• Foster the preservation of the radio spectrum
• Educate the public about RMS science
RMS: Millimeter to Submillimeter Wavelengths
ALMA 84 – 950 GHz 0.02” at 1 mm Imaging array
CARMA 115-345 GHz 0.10” at 1 mm Imaging array
SMA 180-900 GHz 0.15” at 0.45mm Imaging array
LMT 75-345 GHz 6” at 3 mm Collecting area
CSO 180–900 GHz 30” at 1 mm Surveys, spectroscopy
SPT 90-1500 GHz 1’ at 2mm Surveys, SZ effect
ARO 65-490 GHz 21” at 1 mm Molecular searches
• Technological developments and new facilities at superb sites are revolutionizing astronomy in the millimeter to submillimeter range.
• ALMA and the SMA will provide exquisite detail over small fields. Other facilities will provide the source surveys and spectroscopy (especially redshifts).
ALMA: Imaging Origins• CO or CI emission from Milky Way at z = 3
• Gas kinematics in protostars and protoplanetary disks around young Sun-like stars at 150 pc
• Detection of gaps created by forming planets in disks
• Precision imaging at angular resolution of 0.1”
Partners: North America, Europe, JapanMREFC funded 2002-2010; completion 2012Partial array science 2007-8Location at 5000 m in Atacama altiplano
RMS: Millimeter to Submillimeter Wavelengths
Developments for MS in the ALMA era
• Development of large bolometer arrays for wide area mapping
• Enhancement of high sensitivity, broadband spectroscopic capabilities (z-machines)
• Large aperture (25 m class) submillimeter Atacama Telescope (CCAT)
• Millimeter VLBI using ALMA, LMT, JCMT, CSO, CCAT (Schwarschild radius scale in Sgr A*, M87, Cen A)
• Foster a growing MS community at all levels
• Foster the training of young scientists
• Educate the public about RMS science
In this decade, M*S is maturing as a field.
Ground-based CMB Experiments
• Direct observations of the CMB lie uniquely in the domain of RMS astronomy.
• Ground based experiments probe CMB anisotropy and polarization on different scales and thus complement results from space missions.
• RMS surveys critical for foreground determination.
Task Force on CMB ResearchRay Weiss’ presentation tomorrow
Solar Radio AstronomyFASR = Frequency Agile Solar Radio Telescope
• FASR was endorsed by the 2000 AASC as well as the Solar and Space Physics equivalent “From the Sun to the Earth - and Beyond”.
• A proposal to conduct D&D on FASR will be submitted to NSF GEO/ATM.
• Dedicated to solar “weather”, FASR will be a data machine not a PI facility.
Role of RMS University Community• University groups use the RMS facilities for their research.
• Targeted experiments (CMB, SZA, EOR, surveys) are carried out by university research groups, leading to science results as well as the production of public access data products.
• Instrument development is carried out by university groups for both university and national facilities.
• The ATA is the “large-N/small D” SKA demonstrator.
• Millimeter-wave interferometry expertise has historically resided principally in the universities.
• The MS university facilities complement ALMA scientifically, providing hybrid configurations, redshift machines and wide area surveys.
• University facilities train the next generation by involving students in instrument development and operations in ways that e.g., ALMA, as a huge international project, cannot.
R*M*S Astronomy: Technology Drivers
• Huge advances in digital technology– Real-time imaging for EVLA/VLBA– Signal processors for pulsars, spectroscopic surveys,
solar studies, transient detection, rfi mitigation– Electronic “steering”
• Huge advances in “camera” technology– Bolometer arrays– Focal plane arrays for centimeter bands
• Superb sites– Possibilities for submillimeter/FIR from the ground
(Atacama, South Pole)– Low RFI environment for low frequencies (Mileura)
– Innovative designs for large apertures – Low frequency arrays (LWA, MWA, PaST)– Large N/small D (ATA, SKA)
RMS: Radio to Millimeter to Submillimeter Wavelengths
•RMS science addresses forefront questions from unique perspective which adds to the view derived at other wavelengths.
•Ground based CMB experiments and RMS surveys to determine foregrounds in combination with space missions will characterize anisotropy and polarization.
•Radar studies of NEAs; thermal emission from KBOs
•Deep space probe tracking (VLBA/VLA/GBT/Arecibo)
•Space weather (FASR, Arecibo)
•Technology development (wideband receivers, bolometer arrays, cm-band focal plane arrays, high speed data transmission, rfi mitigation, large N/small D, etc).
•Space VLBI offers the highest resolution.
Synergies with NASA/DOE facilities/missions
RMS: Radio to Millimeter to Submillimeter Wavelengths
• Must maintain healthy portfolio of large (expensive) facilities but also develop the next generation instruments.
• Must provide adequate support for fast, targeted experiments/surveys by university research groups.
• Must nurture innovative technology development to drive future science discoveries.
• Must support community to use the facilities efficiently and effectively, to train the next generation, and to educate the public.
RMS is not alone in these challenges.
RMS facilities provide a suite of instruments with little overlap in capability; constrained budgets are a reality.
Principal Challenges in 2005
10 mas
`Astronomical Discovery Space’ The Frequency-Resolution Plane
10 mas
Coverage of various future/currentinstruments is shown.
Upper limit set by diffraction, or detector.
Lower limits set bytelescope or antennafield of view.
RMS: Radio to Millimeter to Submillimeter Wavelengths
RMS: Radio to Millimeter to Submillimeter Wavelengths
Radio, Millimeter and Submillimeter (RMS) Facility AcronymsALMA Atacama Large Millimeter/Submillimeter Array MSArecibo 305m telescope of NAIC RARO Arizona Radio Observatory MSATA Allen Telescope Array RCARMA Combined Array for Millimeter Astronomy MCCAT Cornell-Caltech Atacama Telescope SCSO Caltech Submillimeter Astronomy SDSNA Deep Space Network Array REVLA Expanded Very Large Array RFASR Frequency Agile Solar Radiotelescope RGBT Green Bank Telescope RMLMT Large Millimeter Telescope MLWA Long Wavelength Array RMWA Mileura Widefield Array RSKA Square Kilometer Array RSMA Submillimeter Array SSPT South Pole Telescope SVLBA Very Long Baseline Array R
More R*M*S AcronymsEVLA I :
• First phase of EVLA project• Begun 2001; Expected completion 2012• Modernize existing facility: correlator, receivers, software
EVLA II• 2nd phase of EVLA project• Proposal submitted 2004; under review• Increase angular resolution by 10X with additional antennas
spread throughout New Mexico
eVLBI: (Near) real-time VLBI imaging by transmission of data over internet to central correlator (vs physical shipment of disks)
e2e: “End-to-end” development of software tools for users to aid from proposal submission to observations to data reduction
HSA: High Sensitivity Array (VLBA + VLA + GBT + Arecibo)
Large N/Small D: Large number of small diameter dishes
NAIC: National Astronomy and Ionosphere Center
NMA: New Mexico Array
NRAO: National Radio Astronomy Observatory
RMS: Radio, Millimeter and Submillimeter