NEWFIRM: the N OAO E xtremely W ide F ield IR I m ager

NEWFIRM: the NOAO Extremely Wide Field IR

Imager

Presented by Ron Probst, Project Scientist

NEWFIRMNOAO Extremely Wide Field Infrared Imager

NOAO Users Committee meeting 23 Oct 2003



NEWFIRM is …

An infrared camera with– Wide field of view ( 28 x 28 arcmin)

– Subarcsecond resolution ( 0.4 arcsec/pixel )

– High sensitivity ( throughput, QE, 4-m aperture)

– Near infrared capability ( 1-2.5 microns, 5<R<75)

…integrated into a system for– Deep wide field surveys ( efficient operation on telescope )

– Rapid data turnaround ( pipeline reduction )

– Public data access ( NVO archive )





Widefield deep IR imaging in the large telescope era

• Study of growth of structure and complexity in the Universe

• 1-2.4 μm region physically rich, readily accessible

• 6-10 meter telescopes: Superb image quality over small fields

• NOAO 4-m’s well matched to deep wide survey needs

• Variety of exciting science programs

• Widely recognized need for US competitiveness





Major science themes

Cosmological properties of the UniverseSupernova search at z > 1

Evolution of large scale structure Galaxy clustering evolution at z > 1

Formation and evolution of individual galaxiesAssembly and growth of galaxies at 1 < z < 3Assembly and present structure of Galactic disk and halo

Formation of stars and stellar systems Determination of the IMF in various environmentsMass, energy, and chemical exchange between stars and

ISM





NEWFIRM in the suite of US

facilities

Deep widefield imaging feeds high spatial and/or spectral resolution instruments on modern 4-10 m telescopes, public and private





NEWFIRM in a global context





Evolution of galaxies and galaxy clustering at 1 < z < 3

Track assembly and spatial clustering of galaxies with a mass-sensitive probe gravity driven phenomena

Compare with hierarchical formation theoriesAbundance of rich clusters tests CDM variants

Need large area for sample size, linear dimension comparable to power spectrum turnover length

Complementary observations: optical imaging survey (star formation rate sensitive)

Followup observations: spectroscopic redshifts, high resolution imaging (morphologies)

Added value: distant halo stars, high-z SN, QSOs, rare gal types





IMF, SFR, and YSOs in space and time

Quantify IMF and SFR in molecular clouds over large area, long timeQuantify range of lifetimes for disk accretion phase of YSOsInput to definition of disk properties during planetary system formation

Need very large area, moderate depth, multiple epochs

Complementary observations: optical and X-ray surveys, optical proper motionsFollowup observations: NIR spectral classification, selected deep L-band imaging,

high resolution O/IR imaging and spectroscopyAdded value: evolution of angular momentum, structure of convective stars; time

domain science





Executing the science programs

• Survey mode: large scale, long term, project team– Primary plus ancillary science; public archive for data mining

– Uniformity and rapid turnaround of data product

• General observer mode: short term, small group– Specific science goal, hands-on observing/reduction

– Large data volumes compared to present instruments

• Science advisory committee: small external group– Organization and execution of survey science

– Related scientific and technical issues





System elements: from photons to science

photons

4-m telescope

guider

NEWFIRMinstrument

IR arraymosaic

KPNO CTIO

MIP/NFTucsonLa SerenaORION:

NOAOUSNONASA AmesRaytheon

SW





Arraycontroller

Data handlingsystem

Science datapipeline

Scienceusers

MIP/MONSOONTucsonLa Serena

Sciencearchive

science

Data Products:3 teams +U. MarylandSurveys

PI scienceSpecial purpose

SW





OptomechanicalLayout





Invar36 Pedestal AlN Motherboard

Detector SCA

Alignment Locator

Output Current Mirrors

Light Baffles

Photo Courtesy RIO

Clock and Biases

Outputs 1-32

Outputs 33-64

Orion Focal Plane Module





System software components

• Observation control system: prep, setup, data taking– Code re-use from working systems

– NOAO and other sources

• Data handling system: capture, verify, transport data– SW technology from large physics experiments

– Initial deployment in place

• Pipeline to archive: high quality, uniform data reduction– Toolkit and methods from SQIID, DeepWide, Las Campanas

– MOSAIC pipeline is pathfinder for NEWFIRM





Project status October 2003

• Finishing detailed hardware design

• Initial hardware releases to La Serena, Tucson shops

• Optics in fabrication at vendors

• Filters received ( J H KS )

• MONSOON first light with IR array August 2003

• Negotiating detector foundry run

• Software tasks proceeding as planned

On schedule to first light 7/05





Back to the future

What does NEWFIRM bring to future efforts?

• Design solutions for large instruments

• Detector and acquisition system development

• Observing tools supporting high degree of automation

• Understanding of pipeline processing and its limits

• Archiving and cataloging tools and methods

• US community experience with large scale survey science

The SOAR Adaptive Optics System

Presented by Andrei Tokovinin, Project Scientist

SOAR Adaptive Optics SOAR Adaptive Optics

A. Tokovinin

Telescope system in Chile

Telescope system in Chile

Resolution ~0.3”Field 3’-5’Full sky coverageImaging+spectroscopy

We need:

Can it be done?Can we afford it?

Can it be done?Can we afford it?

Resolution is important!Resolution is important!

0.3” 0.7”

Resolution: 2-3 times

mlim [sky]: gain 0.5-1 mag (rival 8-m)

mlim [confusion]: gain 1-2 mag (half-way to HST)

Solution:Ground-layercompensatio

n

Solution:Ground-layercompensatio

n

Deformabe mirror

Rayleigh UV LaserGuide Star at 10km

Partial compensation of high layers

Good compensation of low layers

1’ 2’ 3’ seeing

Seeing at Cerro Pachon

Seeing at Cerro Pachon

A good night: January 15, 2003

• Median seeing: 0.67” (Gemini campaign) • Turbulence profiles:

May-Sept. 2002 at Tololo, January 2003 at Pachon

Free-atm. + ground layer:~1”

Free atmosphere only:~0.2”

Prediction for SOAR AOPrediction for SOAR AO

25% 50% 75%

β,” 0.94 1.11 1.33

0.5μm 0.38 0.53 0.71

0.7μm 0.22 0.31 0.49

1μm 0.17 0.22 0.30

[arcseconds]

21 nightsJanuary 2003

Sample science with SOAR AOSample science with SOAR AO

Photometry of distant supernovae Dynamics and kinematics of galaxies (with IFU)

Clusters in Galaxy, LMC (CMD)

Morphology of lensed galaxies Resolved nearby galaxies (CMD, star formation,

distance scale, post-AGB)

Planetary and symbiotic nebulae

Imaging+spectroscopy at high angular resolutionImaging+spectroscopy at high angular resolution

History of LMC clusters (K.Olsen)History of LMC clusters (K.Olsen)

Ground-based, 1”

SOAR AO, 0.3”

HST, 0.1”

Reaches turn-off

Photometric errorfrom crowding

Photometric errorfrom crowding

Science instruments for SOAR AOScience instruments for SOAR AO

• CCD imager: 2Kx2K, 0.08” pixels

• SOAR-Brazil IFU

(+ Fabry-Perot?)• Port for a “visitor”

AO instrument

• Adaptive secondary ($2M)

• WFS at each instrument (not planned)

• Pixel scale?

dedicated?1st light SOAR instruments or

…not a good solution!

SOAR AO on SOAR

SOAR AO on SOAR

Electronics

ISBAO module

CCDImager

AO module on ISB

AO module on ISB

LaserLaser Solid-state Nd:YAG laser DS20-355 (Photonics)

=355 nm, 8 W @ 10 kHz Cost $138K or cheaper Resource ~10000h (~5yr)

Tip-tilt: 2-3 NGS to V=18, complete sky coverageTip-tilt: 2-3 NGS to V=18, complete sky coverage

Safety: aircraft and satellite-safe, no visual hazardsSafety: aircraft and satellite-safe, no visual hazards

Control System Block Diagram

Planning and cost

Planning and cost

CoDR: April 2003 PDR: March 2004 Lab closed-loop: 2004 On the sky: 2005

Manpower Capital Total

MY K$ K$ K$

16.5 589 540 1.13

SOAR partners (MSU+UNC) apply for AODP fundingto build “set-and-forget” Rayleigh laser guide star for SOAR

SOAR partners (MSU+UNC) apply for AODP fundingto build “set-and-forget” Rayleigh laser guide star for SOAR

Affordable

A road into the future…

A road into the future…

Build reliable and productive AO system to enhance SOAR scienceand Demonstrate AO technology scalable to ELTs Build AO expertise for TMT and other projects Synergy with Gemini-S (MCAO, NICI)

Documents

NEWFIRM: the N OAO E xtremely W ide F ield IR I m ager