january 30 2006alma na cost/management review1 atacama large millimeter array science ipt al wootten...

January 30 2006 ALMA NA Cost/Management Review 1

Atacama Large Millimeter Array

Science IPT

Al Wootten – NRAONA ALMA Project Scientist

ALMA NA Cost/Management Review January 30 – February 1 2006


Overview

• History – MMA Science group began formal life June 1998 – NA Group holds weekly (usually) telecons.

• Joined with LSA science group June 1999. • Groups very dispersed but with centers in NAOJ,

Garching, Cambridge, IRAM, Tucson, AOC and NAASC.– Pan-ALMA (including JP) telecons monthly.– Detailed agendas and minutes available on web of meetings

since June 1998.


Near-term Deliverables

• Configuration: Extended configuration design– Strawman available, redesign under way to accommodate

environmental concerns, road and fiber design– Draft delivered February, ground truthed (with Site IPT), then final

March– Concern: availability of personnel should antenna complement

further decrease

• Requirements– Clarifications made on major items as a result of System

Requirements Review– Continuing discourse with other IPTs– Documents on subsidiary items under development: RF

Membrane, Solar Filter, Quarter-Wave plate, Amplitude Calibration Device


Near-term Deliverables (2)

• The IPT will support Prototype System Integration activities at the ATF with evaluation of the prototype ALMA interferometer.– Begin implementation of the ALMA Calibration Plan at the

ATF facility.– Further development of commissioning plan for Chile

• Evaluation of ALMA Water Vapor Radiometer, to be installed on SMA– Mitigation plan under way owing to late availability of ATF– More appropriate site for tests (atmosphere, baselines)– Uses two prototype instruments

• Purchase, use of OSF weather station, purchase of AOS instruments– Instruments defined (basically duplication of instruments

commissioned at ATF already)– ICD with Site drafted, imminent submission


WBS Summary

• 1.09.380 Science: Further work on the following items:

– Array Configuration: finishing design for long baselines– Simulations: packages used throughout ALMA, total power imaging

stability requirements, nutator requirements, mosaicing and on the fly interferometry

• Delivered simulators in Gildas, aips++, sensitivity simulator online

– Calibration: Testing, leading to commissioning of Calibration Plan• Development of Calibrator listing• Amplitude: tests at ATF of amplitude calibration device, including total power

calibration• Phase: WVR implementation and interplay with fast switching

– First tests at SMA; ATF implementation may follow

– Imaging: Commissioning of ALMA Imaging Pipeline • Development of algorithms


WBS Summary

• 1.09.380.3040 Phase 2 Science Support– Maintenance of scientific priorities and goals

• Now as a split activity run by NA (1.09.380.3040NA) and EU (1.09.380.3040EU)

– Includes activities through testing at the ATF• 1.09.380.3050 Phase 2 Site Characterization (following approved

document ALMA-90.05.00.00-001-A-SPE & interface milestone ALMA-20.01.04.00-90.05.13.00-A-ICD) – N.B. This activity is subsumed within 3040NA for NA.– No longer staffed owing to Baseline Change Proposal (BCP) cost

savings• management and maintenance of the site infrastructure • design, development, and deployment of instrumentation for monitoring of

atmospheric conditions, • data collection, analysis and modeling the effects of the atmosphere on

incoming radio waves


WBS Summary

• 1.09.380.3070 ALMA Commissioning in Chile (NA/EU)– Commissioning and Science Verification (CSV) involves testing and optimization

of the ALMA system• Goal is to ensure that the science requirements are met• An element of commissioning is Scientific Verification• Commissioning and SV carried out by the same team

– Commissioning involves initial tests, interaction with Systems Integration and other IPTs to identify and resolve faults, optimization, training of operations staff

» Augmentation necessary for multiple antenna designs included in current budget

– SV done to verify and document performance of an observing mode for users» Continuing and incremental activity» Tests the end to end system» Demonstration Science is a part of the SV process» This WP does not cover work at the ATF

• There is a gradual handover of the commissioning activity to Operations during 2009-2011.


Issues

• Phase correction remains challenging• Science is ‘top of the food chain’; schedule can get set

back by any item below which is late


Science IPT Structure

ALMA Board

JAOIncl. ALMA Project Scientist

Now T. Wilson

Science IPTProject Scientists

Instrument Scientists

ASAC

AstronomyCommunity

Configuration Calibration Imaging Site Charac-terization

SSR Liaisons Operations,Verification

Others

ConfigurationWorking Group(Quasi-active)

CalibrationWorking Group

SiteWorking Group(Quasi-active)

(J. Conway)M.HoldawayA. OtarolaK-I Morita

J.MangumM.Holdaway(A.Stirling)D.EmersonB. Vila-Vilaro

M.HoldawayS.Myers

Unstaffed R.Lucas Project ScientistsR.Laing

R.Warmels (Web)Project Scientists (Outreach)M. Hogerheijde (DRSP)

Operations GroupA.Wootten

(in reconstitution)

Project Regional Managers


Progress to Date: Overview

• Requirements defined and promulgated, overall and for subsystems• Design Reference Science Plan developed and maintained

– Calibration aspects added– Employed to assess impact of BCPs on project

• Configuration staked to 4km, strawman design to full extent of array developed

• Site characterization data since 1995, >80% complete– Data still produced, collected on periodic visits

• Calibration Plan maintained, revised• Attendance at most reviews, often panel member(s)• Imaging simulators developed, algorithms published

– Maintenance of the ALMA Sensitivity Calculator


Progress to Date: Requirements

• Three regional ‘Instrument Scientists’ review and report• Reference Documents delivered

– ALMA Scientific Specifications and Requirements (ALMA-90.00.00.00-001-A- SPE) approved 2005 June by CCB, ASAC comment delivered 2005 Nov, awaiting Board action

– Secondary documents produced for elaboration, clarification• Nutator requirements published• Also RF Membrane, Solar filter, quarter wave plate requirements

• System Requirements Review– Chaired by Science IPT, arranged by SE, attended by all IPTs– Periodic meetings to review requirements and their flowdown

between Science, SE and other IPTs


Progress to Date:Design Reference Science Plan

• Submitted Dec 2003. Web version: http://www.strw.leidenuniv.nl/~alma/drsp.html• ~130 proposals from ~80 astronomers provides a quantitative reference for

– developing the science operations plan, – for performing imaging simulations, – for software design, and – for other applications within the ALMA project. Specifically, it can be used to:

• allow cross-checking of the ALMA specifications against "real" experiments• allow a first look at the time distribution for

– configurations– frequencies– experimental difficulty (fraction of projects pushing ALMA specs)

• start developing observing strategies• derive input for the Computing IPT• be ready in case some ALMA rescoping is required, or in case some ALMA

specifications cannot be met.

• Currently in active use by the project– Assessment of calibration accuracies needed– Assessment of impact of project baseline change proposals, including evaluation of

the impact of a fewer-antenna ALMA on individual DRSPs.


Three Year Duration

• Theme 1: Galaxies and Cosmology: 40% = 14.4 months = 10500 hr• Theme 2: Star and Planet Formation: 30% = 10.8 months = 7880 hr• Theme 3: Stars and their evolution: 20% = 7.2 months = 5250 hr• Theme 4: Solar system: 10% = 3.6 months = 2620 hr• Employ sensitivities on the ESO ALMA Web at:

– http://www.eso.org/projects/alma/science/bin/sensitivity.html

– Based on ALMA memo 393.

• Maintained to keep the DRSP abreast of the field by Michiel Hogerheijde


Statistics Receiver Bands

% of timeBand 3 Band 6 Band 7 Band 9 Total

Galaxies 22 30 32 16 100

Star formation 24 28 38 10 100

Stars 16 26 31 27 100

Solar system 4 38 51 7 100

Total 20 30 37 13 100


Some initial DRSP conclusions

• Overall distribution over receiver bands reasonably consistent with weather statistics

• Fraction of continuum-only programs varies per receiver band and theme: Band 6 pre-dominantly line; Band 7 and 9 large fraction continuum

• Fraction of proposals which require total power continuum of order 35%

• Fraction of proposals which require baselines of at least 1 km 50-60% (with peak around 0.1-0.2”)


5000m Chajnantor site

ALMA

APEX

CBI

Site Char


Design


Progress to Date: Configuration

– Configuration • Configuration group work began 1998, several

reviews, culminating in contract with Conway and Holdaway as mentors

• Plan for 64 antenna ALMA approved– Inner, outer configurations, first Early Science

configs, reconfiguration• Plan for 50+ configuration submitted, staked on

site• Includes reconfiguration plan


Basis for Redesign

• The Executives requested an analysis of the baseline, based on currently available funding. Accordingly, the JAO asked the Science IPT for a design for a 50 antenna array which could provide excellent imaging along with the possibility of extension to 64 antennas.

• Science IPT renewed contract with Conway, asked Conway and Holdaway to produce such a design before the end of Summer 2005.

• Principles of Design– Imaging shall be done in a single configuration when practicable.– Continuous reconfiguration scheme preferable.


Status

• Configuration optimization complete to <4km– Full set of optimized intermediate configurations– Total of 151 + ~35 dedicated pads, compared to 216 previously.

• 11 of these, mostly in close-packed array, to be built only for N=64.– Outer configuration strawman reaches 4mas at 950 GHz

• Awaits synchronization with Environmental concerns (Vizcacha avoidance and new road/fiber plan)

• Ground-truthing on the site– Nyman, Rivera, Holdaway perfect the mask– Otarola, Stirling, Rivera to Chajnantor 2005 August– Assess conformance of actual landforms to Digital Elevation Model (perhaps

300m errors)– Iteration of Conway-chosen locations with John to determine these final locations

• Final version then produced by2005 August 17.– Comments solicited by the Board from the ASAC have been favorable.


Close-packed Configuration Features

• Basically unchanged from previous 60 pad design

• 9 outer pads, 1 inner pad subtracted• Imaging performance verified (ALMA

Memos 428, 430)• Extended NS configuration outside (-55º,

+15º)—no transit shadowing to +35º, 16 additional pads

• Two reserved pads to be built for 64 antenna array.


Intermediate Configurations

• Can support nearly continuous reconfiguration– ~20 configurations within 4km– Four antennas moved at a time

• Resolution change 1.174

– Two per day per transporter– Almost certainly will not actually schedule this pace!

• 10% Stretch (ALMA Memo 119) on spiral design, constrained by terrain mask.

• Three pads to maintain short spacings• Two pads to accommodate NS extension• Inward reconfiguration opposite of outward except for

innermost shadowed configurations• I, O configurations differ slightly for inner 15.


Progress to Date: Calibration

• Calibration – Calibration Working Group (J. Mangum, leader) holds monthly telecons

with agendas and minutes• https://wikio.nrao.edu/bin/view/ALMA/AlmaCal

• Includes representatives from currently operating millimeter interferometers, other IPTs

– Calibration Specifications and Requirements (ALMA-90.03.00.00-001-B-SPE)—approved 2002-Nov-26; updated document in revision

– ALMA Calibration Plan (SCID-90.03.00.00-007-A-PLA)—revised yearly; in third version

– WVR implementation on SMA under way– Amplitude Calibration Device review (05Aug25)– ATF to be testbed for plan

• DRSP used as foil for plan

https://wikio.nrao.edu/bin/view/ALMA/AlmaCal

https://wikio.nrao.edu/bin/view/ALMA/AlmaCal


Phase Correction

To achieve:• Diffraction-limited operation at sub-mm wavelengths on baselines up to 14

km

• Corresponds to 0.01 arcsec resolution requirement

• To achieve at ALMA’s highest frequencies (~950 GHz), require phase errors

< 50 microns on baselines of 14 km • Typical atmospheric phase fluctuations at Chajnantor:

• 90-400μm on 300m baselines at 25-75% level

• Corresponds to fluctuations of ~300-1200μm at 14km

• Atmospheric phase correction essential


Simulations of phase correction

• AIPS++ code written by Mark Holdaway• Combines Mark’s fast switching simulator with our 3-D simulations of

atmosphere• WVR simulated using `am’ radiative transfer code to calculate brightness

temperatures (Scott Paine)


Phase correction strategy

To use a combination of:• Fast switching

• Measure phase from a nearby point source calibrator• Measures total atmospheric phase• Intermittent (every ~10s of seconds) • Gives phase along a different line of sight

• Water vapour radiometry• 183 GHz radiometers four channels

• Sensitive only to wet component• Continuous, on source• Two prototype WVRs built by Cambridge and Onsala now ready for

testing, planned at SMA


Pre-production ALMAWater Vapor RadiometerOperating in an SMA Antenna on Mauna Kea(January 19, 2006)

Photo courtesy ofMagne Hagstrom &Ross Williamson

Relay mirrors


Phase Correction Conclusions

• Now have realizations of the atmosphere at Chajnantor for day and night conditions

• Dry and wet fluctuations have different distributions depending on time of day

• Have developed simulations of FS+WVR phase correction• Future plans:

– Investigate different phase correction strategies– Validation of the two ALMA prototype WVRs on SMA

• Second prototype on SMA Jan 19• Tests through April 2006.


Rebaselining Changes

• Scope: IPT costs are mostly personnel– Site Characterization is adopted BCP item; salaries and travel

eliminated.– Travel cut is adopted BCP item.– Commissioning WBS evolved from Science WBS: several positions shift

to Commissioning as AIV proceeds.• Some additional effort needed to commission multiple antenna designs

• Budget is determined by level of effort– Testing of prototype two element interferometer with prototype

electronics at ATF by Science IPT staff assisted by other IPTs– Expertise then transferred to Chilean commissioning

• Schedule dependencies– Schedule of prototype deliveries at ATF– AIV schedule in Chile


Interactions

• ALMA-J interaction – Complete integration of Science IPT occurs at every level– There are not expected to be problems in this process

– Fomalont visiting JP to discuss ACA calibration aspects next week.

• Operations interaction – Need a full team with a JAO Project Scientist in place to ensure successful CSV process with transition to HSO/Operations. Currently, PS interact with JAO, proto-ARCs.

• Problems specific to Science –The CSV work at the ATF and in Chile depend on the schedule being met by other IPTs. To ensure communication, CIPT members attend most ScIPT telecons; PS attends CIPT/SSR telecons; NA PS and IS attend PSI telecons; PS attends Board, JAO/MIPT telecons and maintains presence in JAO/Santiago. Wootten produces ‘Biweekly Calendar’ of goings-on around the Project.


AOS 6 Ant Array

Evaluation Complete

1.09 Science Summary Schedule20072006 20092008 20112010 2012

41 2 3 41 2 3 41 2 3 41 2 3 41 2 3 41 2 3 41 2 3

(Data from IPS as of 2006Jan13)

ATF Testing Support

OS

F/A

OS

Commissioning Antenna Array – Finish dates

16th 32nd 50th

Science Verification

AT

F

`

Jan ’10 Early Science

Mar ’09 Early Science Decision Point

Call for Proposals / Early Science Preparation

Sept ’12 Start of Full Science

8th

OSF Integration – Start dates

1st 16th 32nd 50th3rd2nd

SE

&I

Re

fere

nc

eATF Testing

8th

June ’06 ATF First Fringes

SC

IEN

CE

SU

MM

AR

Y

Site Characterization

Science Support OSF

Time Now


Budget

• NA CTC estimate is 4.97 million Y2K. This consists of 75% for salaries and travel; no major external contracts– DOE Contingency is 5.1% ($228K for NA)– DOE Contingency is a 0.1% reduction in the planned contingency from

the plan of 2002 March 12.– Probability-weighted Risk Contingency estimate: $155K for NA)

• Assumptions & dependencies are based on the Integrated Project Plan

• Bases of estimates:– Present staff is nearly complete in NA and EU

• Attempts to hire a JAO Project Scientist to lead science in CSV in Chile so far not successful (N.B. JAO PS not in Science IPT budget)

• Currently, regional Project Scientists plan to rotate through JAO PS position on a four month turno until antennas arrive in Chile; a virtual cost

– Commissioning effort adds staff in Chile augmented by postdocs• Recovery plans for budget problems

– Delay in hiring of postdocs


Science – Changes since Garmish

• BCPs– 20% travel reduction; site characterization labor & travel

reduction $M (0.1)

• 2 Antenna Impact– additional effort & associated costs $M 0.2


Commissioning


1.09 Science NRAO Cost Estimate

By Calendar Year in Year 2000 (K$)

Totals

$0

$200

$400

$600

$800

$1,000

$1,200

< 2004 2005 2006 2007 2008 2009 2010 2011 2012

Yea

r 20

00 (

K$)

Budget $956 $555 $629 $871 $726 $695 $288 $22 $0 $4,741

Contingency $0 $34 $39 $56 $41 $39 $17 $2 $0 $228

Totals Y2K$ $956 $589 $668 $927 $767 $734 $305 $24 $0 $4,970


1.09 Science NRAO Cost Estimate

By Fiscal Year in FTEs

0.0

1.0

2.0

3.0

4.0

5.0

6.0

7.0

8.0

9.0

FT

E Y

ears

1.09 Science 5.4 4.5 5.3 8.5 8.5 8.0 2.0 0.0 0.0

< 2004 2005 2006 2007 2008 2009 2010 2011 2012


BOE Distribution by Confidence Number1.09 Science

(Contingency not included)

Yea

r 20

00 (

K$)

Total

$0

$500

$1,000

$1,500

$2,000

$2,500

$3,000

1 Actual Bid 2 Vendor Quotation 3 EngineeringEstimate

4 ParametricEstimate

5 Best Guess 6 In-process

Budget $956 $1,094 $2,614 $0 $0 $225 $4,889

Values shown reflect the current estimate as of 1/20/06Values shown reflect the current estimate as of 1/20/06


Risk Register


Conclusions

• The ALMA Science IPT is reaching the end of the Requirements establishment phase and entering a period of verification

• Implementation of the WVR is being detailed, in conjunction with work on the SMA

• Preparations for commissioning and beyond, in terms of planning, interim configuration planning, definitions of supported modes continue


www.alma.infoThe Atacama Large Millimeter Array (ALMA) is an international astronomy facility. ALMA is a partnership between Europe, North America and Japan, in cooperation with the Republic of Chile. ALMA is funded in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC), in Europe by the European Southern Observatory (ESO) and Spain. ALMA construction and operations are led on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI), on behalf of Europe by ESO, and on behalf of Japan by the National Astronomical Observatory of Japan.


Evolution of thermal fluctuationsH

eig

ht

/ km

0

0.6

-0.3 0.3Horizontal distance / km


Correction process: WVR


WVR: rms error

january 30 2006alma na cost/management review1 atacama large millimeter array science ipt al wootten...

Documents

alma calibration plan

alma commissioning i

prototype alma interferometer

na group

approved document alma

site ipt

spe interface milestone

sma atf implementation