Radio, Millimeter and Submillimeter Planning Group

Transcription

1 Radio, Millimeter and Submillimeter Planning Group Martha P. Haynes (Cornell University) on behalf of the RMSPG Astronomy and Astrophysics Advisory Committee February 15, 2005

2 R*M*S Planning Group Premise: Recommendations as outlined in: Astro & Astrophys in the New Millenium From the Sun to the Earth And Beyond Connecting Quarks with the Cosmos New Frontiers in the Solar System Objective: Update/Implementation Plan Membership: 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 Site includes a compilation of RMS facilities A community volunteer effort Funding to date provided by AUI No special interaction with AUI/NRAO director

3 R*M*S Astronomy Key points 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.

4 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)

5 RMS: Centimeter to Meter Wavelengths National Center Facilities Arecibo GHz 3.5 at 21cm Collecting area GBT GHz 9 at 21 cm Unblocked aperture EVLA GHz 0.4 at 6cm Imaging array VLBA 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, AASC Radio & Submillimeter Panel Report

6 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.

7 GBT: Revolutionized Capabilities Exploit the GBT s unique characteristics: Unblocked aperture (galactic HI) Active surface (high frequencies) Full steerability (85% of sky) Location in NRQZ (low RFI) Wide frequency coverage 3mm bolometer array Wideband spectrometer Dynamic scheduling

8 EVLA: Revolutionized Capabilities Multiply 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

9 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

10 RMS: Centimeter to Meter Wavelengths Development 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: MHz for EOR/transients LWA: 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

11 RMS: Millimeter to Submillimeter Wavelengths ALMA GHz 0.02 at 1 mm Imaging array CARMA GHz 0.10 at 1 mm Imaging array SMA GHz 0.15 at 0.45mm Imaging array LMT GHz 6 at 3 mm Collecting area CSO GHz 30 at 1 mm Surveys, spectroscopy SPT GHz 1 at 2mm Surveys, SZ effect ARO 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).

12 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, Japan MREFC funded ; completion 2012 Partial array science Location at 5000 m in Atacama altiplano

13 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.

14 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 Research Ray Weiss presentation tomorrow

15 Solar Radio Astronomy FASR = 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.

16 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.

17 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)

18 RMS: Radio to Millimeter to Submillimeter Wavelengths Synergies with NASA/DOE facilities/missions 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.

19 RMS: Radio to Millimeter to Submillimeter Wavelengths RMS facilities provide a suite of instruments with little overlap in capability; constrained budgets are a reality. Principal Challenges in 2005 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.

20 `Astronomical Discovery Space The Frequency-Resolution Plane mas mas Coverage of various future/current instruments is shown. Upper limit set by diffraction, or detector. Lower limits set by telescope or antenna field of view.

21 RMS: Radio to Millimeter to Submillimeter Wavelengths

22 RMS: Radio to Millimeter to Submillimeter Wavelengths

23 Radio, Millimeter and Submillimeter (RMS) Facility Acronyms ALMA Arecibo ARO ATA CARMA CCAT CSO DSNA EVLA FASR GBT LMT LWA MWA PaST SKA SMA SPT VLBA Atacama Large Millimeter/Submillimeter Array 305m telescope of NAIC Arizona Radio Observatory Allen Telescope Array Combined Array for Millimeter Astronomy Cornell-Caltech Atacama Telescope Caltech Submillimeter Astronomy Deep Space Network Array Expanded Very Large Array Frequency Agile Solar Radiotelescope Green Bank Telescope Large Millimeter Telescope Long Wavelength Array Mileura Widefield Array Primeval Structure Telescope Square Kilometer Array Submillimeter Array South Pole Telescope Very Long Baseline Array MS R MS R M S S R R R RM M R R R R S S R

24 More R*M*S Acronyms EVLA I : First phase of EVLA project Begun 2001; Expected completion 2012 Modernize existing facility: correlator, receivers, software EVLA II 2 nd 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