Transcript Kavli Futures II – August 3-5 2016

Equipping ALMA For the Next Decade and Beyond
Crystal Brogan
Deputy NA ALMA Program Scientist
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Kavli Futures II – August 3-5 2016
ALMA Science Frontiers
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First Billion Years
Evolution of Galaxies to the Star Formation Peak
Local galaxies, Milky Way and the ISM
Star and planet formation
Exoplanet characterization
The Sun and Solar System
“level I” science goals:
1. The ability to detect spectral line emission from CO or C+ in a normal galaxy like
the Milky Way at a redshift of z = 3, in less than 24 hours of observation
2. The ability to image the gas kinematics in a solar-mass
protostellar/protoplanetary disk at a distance of 150 pc, enabling one to study
the physical, chemical, and magnetic field structure of the disk and to detect the
tidal gaps created by planets undergoing formation
3. The ability to provide precise images at an angular resolution of 0.1”
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ALMA Status at the Start of Cycle 4
• ALMA now operates at or close to the original (re-baselined)
capabilities and meets Level I Science Goals
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Bands 3, 4, 6, 7, 8, 9, 10 (3mm to 350 um)
High fidelity imaging, mosacing
Long baselines
Flexible correlator (up to 16 narrow spws, or 8 GHz BW)
Polarization (though somewhat restricted)
• However > 15 years have passed since ALMA specifications
were written and construction began
• Cutting-edge technology has advanced tremendously over the
past decade and a half
• We are very fortunate to have built into the operations plan a
vigorous ALMA Development Budget
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Expanding ALMA’s Scientific Discovery Space:
ALMA Development
• Ramped up to steady-state level by FY2015
– 5M (NA) + 5M (EU) + 3.6M (EA) per year [in principle, subject to funding]
– Funds split into
• STUDIES (~10% budget) typically 1 year in duration
• PROJECTS (Remainder) usually take a few years to completion
– Study calls every year, Projects every 2-3 years
– First priority was to build de-scoped ALMA capabilities (receiver bands 1, 2, &
5, VLBI)
• ALMA Integrated Science Team and Science Advisory Committee
(with community input), developed Pathways To Developing ALMA
(ALMA2030)
• Pathways informs discussions leading to assembly of a costed Board
approved long term Future Vision (to be finalized April 2017)
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Development Areas for ALMA 2010-2030
There are clear science drivers for improving
• Sensitivity / Speed
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Collecting area / UV coverage
Instantaneous bandwidth
Instantaneous spectral coverage at high spectral resolution / Data Rate
Hardware Sensitivity
Mapping speed / Increased FOV
Calibration (WVR, Tsys, phase connection)
• New / Expanded Discovery Space
– Tunable Frequency range (all accessible frequencies)
– Angular Resolution
– More Flexible Spectral Tuning Options
• Reduce Time to Science Discovery (Impact and Usability)
– Science Ready Data Products (beyond reference imaging for QA2)
– Archival research tools
– Analysis Tools
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(A Few) Example Science Drivers
• Imaging Protostars & protoplanetary disks
– Disk morphology, composition, kinematics, evolution (sensitivity,
spectral grasp, resolution, imaging precision)
• Characterization of planets
– Astrometry: measuring stellar reflex motions (resolution)
– Transit measurements (sensitivity, spectral grasp)
• Galaxies
– Probing central masses of starbursts & black holes (resolution,
sensitivity)
– Characterizing evolution and chemical content of ISM and feedback
(sensitivity, spectral grasp)
• First Galaxies
– From metal formation in the first stars, to the peak of star formation
(sensitivity, spectral grasp)
– Identification, imaging, composition and kinematics of the first
galaxies (sensitivity, resolution, spectral grasp)
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TW Hya at 1 AU resolution
(Andrews+2016)
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Process
Leverage community strengths in hardware, software, and
techniques to enact a science-driven upgrade plan for ALMA
• Through responses to community Calls, ALMA partners select a collection
of Studies which detail the ultimate goals of the ALMA Development
Vision
• As a result of Studies, Projects may be undertaken to improve capabilities
or to realize new capabilities according to the Vision
• Prioritization then leads to a Plan to achieve Vision
• Current goals include
– Maximizing sensitivity and throughput by increasing bandwidth
– Completing and upgrading receiver complement to provide that bandwidth
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Progression of ALMA Development Components
ALMA Development Study
Next Gen ALMA Data Viewer
Unleashing Large Dataset Science
ALMA Development Project
CARTA
ALMA Data Mining Toolkit
ALMA Enhancement
Implementation/CASA 2017
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ADMIT (Sept 2016)
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ADMIT: ALMA Data Mining Toolkit
 First-view science data products produced by pipeline: spectra, line ID, moment maps, etc
 Toolkit allows user to generate their own science products from cubes.
 Developed by University of Maryland, University of Illinois, and NRAO
Products shown created by automated ADMIT pipeline
Moment 0
Example
Spectrum
for line ID
Moment 1
Moment 2
Identification of common lines
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Moment maps for lines
Progression of ALMA Development Components
ALMA Development Study
ALMA B1 (35 to 50 GHz) Study
Mm/Submm VLB with ALMA
ALMA Development Project
ALMA B1 Project, Construction
ALMA Phasing Project
ALMA Enhancement
Planned Completion 2019
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Cycle 4 VLBI
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ALMA Phasing Project (APP)
(NA + Partners)
Phase-up ALMA and record the summed signal for
mm/sub--‐mm VLBI:
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Band 3 Phasing test with
7 antennas (colors)
Project accepted in 2012, CDR in May 2013
Hardware Accepted: Dec 2014
• Includes new extremely accurate Hydrogen maser clock
now used throughout ALMA
Commissioning: Jan 2015 -Sept 2016
Initially only continuum, spectral lines later
• Key Science: Testing general relativity using the black hole shadow
General relativity predicts that the shadow of a black hole should be circular (middle panel), but a
black hole that violates the no-hair theorem could have a prolate (left) or oblate (right) shadow.
Future images of nearby supermassive black holes will be able to test this prediction. (figures
courtesy D. Psaltis and A. Broderick)
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Other Impending Development Payoffs
Project: Band 5 (EU + Partners)
Freq range: 165 to 211 GHz
Study 2011 (building on earlier design work)
Project 2012-2017
Deployed on APEX 2015 (SEPIA, see below)
ALMA SV underway (Arp220, SgrB2, AGB star)
Expected to be offered in Cycle 5
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Arp220
Galametz+2016
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Wide range of studies underway:
• Band 2 & Band 2+3 designs
• Spectral resolution and Bandwidth upgrade
to current correlator
• Double IF-bandwidth digitization design
• New Digital correlator design
• Sideband separating receiver for Band 9
• Extension of phasing ALMA (Band 7)
• Transients with Phased ALMA
• GPU Spectrometer for TP Array
• Multi-pixel array feeds
• Improving calibration of atmospheric
spectral features
• Chip evaluation for 2nd generation ALMA
receivers
• Central LO expansion to allow 5 sub-arrays
• Spectral line data analysis software
(XCLASS, MAGIX)
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Opportunities for the Immediate Future (NA)
• Results of NA 2016 Call for Studies Announced Soon
• New NA Call for Projects 10 October
– Overall funding pool is expected to be larger than previously, before
Development funding reached its steady-state value
• New NA Call for Studies also foreseen for FY2017
– Some studies which could not be funded during the current Call may
be accommodated, should PIs be able to garner resources, address
concerns expressed in reviews
– Emphasis on next-generation concepts that address the 2030 Future
Vision
• Be part of the conversation on the Future Vision…
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Upcoming Workshops (Please Join Us)
https://science.nrao.edu/science/meetings/2016/na-alma-dev-program-workshop
Free registration open, also option to join remotely
Sneak peak of the ALMA 2030 Future Vision
http://go.nrao.edu/alma5years
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Early bird registration and
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posters extended to Aug. 8
www.nrao.edu
science.nrao.edu
The National Radio Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc.
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