11Photo – John MacDonald

OSIRISOSIRIS The Latest Keck Instrument and its ScienceThe Latest Keck Instrument and its Science

James Larkin (UCLA)James Larkin (UCLA)

James Larkin (PI), Matthew Barczys, Sean Adkins, Ted Aliado, Paola Amico, George Brims,Randy Campbell, John Canfield, Thomas Gasaway, Allan Honey, Christof Iserlohe, ChrisJohnson, Alfred Krabbe, Evan Kress, David LaFreniere, James Lyke, Ken Magnone, Nick

Magnone, Michael McElwain, Juleen Moon, Andreas Quirrenbach, Gunnar Skulason, InseokSong, Michael Spencer, Jason Weiss and Shelley Wright

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OutlineOutline

•• Instrument overviewInstrument overview

•• Early ScienceEarly Science

•• Future DirectionsFuture Directions

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OSIRIS (OH-Suppressing OSIRIS (OH-Suppressing InfraRedInfraRed

Imaging Imaging SpectographSpectograph))

•• Spatial resolution at the Keck Diffraction Limit (<0.050Spatial resolution at the Keck Diffraction Limit (<0.050””))•• Spectral resolution (Spectral resolution ( // ) ~ 3800) ~ 3800

•• Full z, J, H, or K spectra with single exposure (16x64 Full z, J, H, or K spectra with single exposure (16x64 lensletslenslets))

•• Integrated Data Reduction PipelineIntegrated Data Reduction Pipeline

•• Low Low WavefrontWavefront Error Error

•• Integral Field SpectrographIntegral Field Spectrograph–– Spectra over a contiguous rectangular field.Spectra over a contiguous rectangular field.

x

y

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UCLA Infrared LabUCLA Infrared Lab

Founded in 1989 Founded in 1989 –– Part of UCO Part of UCO

Professors: Professors: Ian McLean and James LarkinIan McLean and James Larkin

Facilities: Facilities: 5,000 sq. ft. of Office, clean room and machining shop5,000 sq. ft. of Office, clean room and machining shop

PhD. Students: PhD. Students: Chris Crockett, Ian Chris Crockett, Ian CrossfieldCrossfield, Emily Rice, , Emily Rice, Erin SmithErin Smith, Shelley Wright, Shelley Wright

Engineering Staff: Engineering Staff: Ted Ted AliadoAliado, George Brims, John Canfield, Chris Johnson, Evan Kress,, George Brims, John Canfield, Chris Johnson, Evan Kress,

Ken Ken MagnoneMagnone, Jennifer Milburn, Alex , Jennifer Milburn, Alex VaucherVaucher, Eric Wang, Jason Weiss, Eric Wang, Jason Weiss

Major Instruments: Major Instruments: GEMINI, NAVYCAM, KCAMGEMINI, NAVYCAM, KCAM**, NIRSPEC, NIRSPEC**, FLITECAM, NIRC2, FLITECAM, NIRC2**

(Caltech led), OSIRIS(Caltech led), OSIRIS**, SHARC, SHARC**

Future Instruments: Future Instruments: GPI GPI –– IFU IFU**, MOSFIRE (with Caltech), IRIS, MOSFIRE (with Caltech), IRIS**

**Optimized for AOOptimized for AO

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OSIRIS is a lenslet-based spectrographOSIRIS is a lenslet-based spectrograph

Detector

Lenslet

Array

Collimator

Optics

Grating

Camera

OpticsFocal

Plane

Pupil Plane

AOFocus

ColdPupil

Filters

R. I. CollimatingDoublet

R.I. CameraDoublet

Reimaging Optics

Lenslet

Spectrograph

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Real Optical LayoutReal Optical Layout

AO Focus

ReimagingCollimators

Filters

ReimagingCameras

OSIRIS Optical LayoutOSIRIS Optical LayoutFold Mirror& Lenslet Array

SpectrographCollimator Mirrors (TMA)

Grating

Fold Mirror

SpectrographCamera Mirrors (TMA)

Hawaii-2 Detector

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Pupil Plane

1mm

AO Focus

LensletLenslet

ArrayArray

•• MEMs MEMs Optical - Optical - InfrasilInfrasil, biconvex elements. Thickness is 1.0 mm, biconvex elements. Thickness is 1.0 mmwith EFL of 0.8 mm. Pitch is 250 microns.with EFL of 0.8 mm. Pitch is 250 microns.–– 72x72 lenslet square area centered in 1.572x72 lenslet square area centered in 1.5”” diameter circular diameter circular

substrate.substrate.

•• ~98% fill factor~98% fill factor

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Dispersing Lenslet SpotsDispersing Lenslet Spots

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Dispersing Lenslet SpotsDispersing Lenslet Spots

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Dispersing Lenslet SpotsDispersing Lenslet Spots

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Lenslet GeometryLenslet GeometryThen more rows are added with same stagger so twopixels in the same column are separated by two pixelshorizontally and 32 pixels vertically.This can be extended to form a 16x16 group of spectra.

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Lenslet geometryLenslet geometry

•• To keep the spectra on theTo keep the spectra on thedetector, each group of 16x16 isdetector, each group of 16x16 isstaggered by 1 lenslet.staggered by 1 lenslet.

•• So Broadband mode, there areSo Broadband mode, there are64x16 spectra, but each group of64x16 spectra, but each group of16x16 are offset by 1 from the16x16 are offset by 1 from theprevious group.previous group.

•• In this mode, each spectrum canIn this mode, each spectrum canrun as far to the left or right asrun as far to the left or right asthe detector/filter allows. ~1600the detector/filter allows. ~1600pixels for each of 1024 spectra.pixels for each of 1024 spectra.

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Lenslet GeometryLenslet Geometry

•• By limiting the By limiting the bandpassbandpass

to less than 512 pixels,to less than 512 pixels,

additional groups can beadditional groups can be

added horizontally.added horizontally.

•• This is the narrow bandThis is the narrow band

mode (3078 spectra).mode (3078 spectra).

512 pixels

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•• Modes:Modes:

–– Broad Band (16x64 x 1700)Broad Band (16x64 x 1700)

–– Narrow Band (up to 48x64 x 400)Narrow Band (up to 48x64 x 400)

•• 22 Filters ( 88 possible data products)22 Filters ( 88 possible data products)

Two modes/Four Plate ScalesTwo modes/Four Plate Scales

1.681.68””x2.24x2.24””0.560.56””x2.24x2.24””0.0350.035””

4.84.8””x6.4x6.4””1.61.6””x6.4x6.4””0.100.10””

2.42.4””x3.2x3.2””0.80.8””x3.2x3.2””0.050.05””

0.960.96””x1.28x1.28””0.320.32””x1.28x1.28””0.020.02””

Narrow bandNarrow band

field of viewfield of viewBroad bandBroad band

field of viewfield of viewAngular Scale perAngular Scale per

LensletLenslet

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5% 5% Bandpass Bandpass OSIRIS SpectraOSIRIS Spectra

White Light (3072 spectra) Arc Lines (3072 spectra)White Light (3072 spectra) Arc Lines (3072 spectra)

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Raw dataRaw data

•• Raw spectra are very complex.Raw spectra are very complex.–– Separated by 2 pixels vertically.Separated by 2 pixels vertically.

–– Staggered by 32 pixels horizontallyStaggered by 32 pixels horizontally

–– Narrow band mode has additionalNarrow band mode has additional

spectra laid out end-to-end.spectra laid out end-to-end.

•• But Spectral format is extremely stableBut Spectral format is extremely stable–– No moving parts after No moving parts after lensletslenslets..

–– Fixed gravity vector.Fixed gravity vector.

–– Thermally controlled.Thermally controlled.

–– Vibrationally Vibrationally isolated.isolated.

18 pinholes (“stars”) with0.25” spacing.0.020” scale, hn3 filter.

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CalibrationsCalibrations

•• The wavelength solution is mapped for allThe wavelength solution is mapped for all

lenslets lenslets in all 22 filters (total of 46,511in all 22 filters (total of 46,511

independent spectra).independent spectra).

•• Point spread function (PSF) for each Point spread function (PSF) for each lenslet lenslet andand

each filter must be mapped to extract theeach filter must be mapped to extract the

spectra.spectra.

•• Done only one timeDone only one time - no spectral motion ever- no spectral motion ever

detected.detected.

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Hn3 Diffraction-limited pinholesHn3 Diffraction-limited pinholes

FWHM = 1.78 FWHM = 1.78 lenslets lenslets = 36 = 36 masmas..

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Kn3 Diffraction-limited pinholesKn3 Diffraction-limited pinholes

FWHM = 2.3 FWHM = 2.3 lenslets lenslets = 46 = 46 masmas

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Small pupils require fast Small pupils require fast lensletslenslets, which require a, which require a

fast spectrograph.fast spectrograph.

Large all metal off-axis optics - SSG Inc.Large all metal off-axis optics - SSG Inc.

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Six internal cryogenic mechanismsSix internal cryogenic mechanismsDesigned and built at UCLADesigned and built at UCLA

Really can just set the scale, the filter and theexposure time. Imager has a filter and exposuretime.

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ImagerImager

•• 2020”” field of view with 0.02 field of view with 0.02”” pixels. pixels.

•• 18 filters including all the broad bands from the spectrograph.18 filters including all the broad bands from the spectrograph.

•• Mounted to same optical benches in same Mounted to same optical benches in same dewardewar..

•• Identical to SHARC camera (first light on May 15, 2006).Identical to SHARC camera (first light on May 15, 2006).

20” Imager Field

Spectrograph FieldsCenter-to-center ~ 20”

Simultaneous PSF Measurements.Parallel deep imaging.Reference objects for stacking.

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First lightFirst light

•• Feb 22, 2005 Feb 22, 2005 ––clear with aboutclear with about11”” seeing seeing–– FWHM=0.043FWHM=0.043””

at Kat K

–– 40% 40% Strehl Strehl at Kat K

–– First target wasFirst target waswithin 0.15within 0.15”” of offield center.field center.

0.2”

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Br

[Ca VIII]

CO

H2HeIH2

H2

[Fe II]

nucleus

off-nucleus

[micron]

Flu

x [

a.u

.]

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Br

[Ca VIII]

CO

H2HeIH2

H2

[Fe II]

nucleus

off-nucleus

[micron]

Flu

x [

a.u

.]

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NGC 4151 - MapsNGC 4151 - Maps

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Titan Titan @2.1@2.1μμmmEach pixel=129 kmEach pixel=129 km

0.80.8””

Stratosphere SurfaceBouchez and OSIRIS Team

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LGS Observations of V723 LGS Observations of V723 CasCas

(Nova (Nova Cas Cas 1995)1995)Campbell, Campbell, LykeLyke, Team Keck, Team Keck

Diameter ~ 0.3”

Red: [Al IX]

Blue: [Si VI]

Green: Br

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8”

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8”

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Galactic CenterGalactic Center

•• First laser guide starFirst laser guide star

spectra of GC (May 2005)spectra of GC (May 2005)

•• K-Band, 0.020K-Band, 0.020””/lenslet/lenslet

•• Krabbe Krabbe et al. (2006)et al. (2006)

SGR A*

S0-2

0.3”

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Variability of Variability of Sgr Sgr A*A*

LaserShuttered

by TelescopeCrossing

SGR A*

• K-band 0.02”/lenslet

• 15 minutes per slice

Time

Ghez et al.

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M31 Bulge AbundancesM31 Bulge Abundances

•• 0.050.05”” scale scale

•• 60" = approx 225 pc from the60" = approx 225 pc from thenucleusnucleus

•• Rich, L. Rich, L. OrilgiaOrilgia, E. , E. ValentiValenti, R., R.MalleryMallery, A. Koch., A. Koch.

1.1”

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H+K image Carson, Larkin 2001

OSIRISOSIRIS•• 4c48.48:Radio Galaxy4c48.48:Radio Galaxy

(z=2.343, 11.1 Billion light years)(z=2.343, 11.1 Billion light years)

1.6”

14 kpc

[OIII] (500.7nm)

Steps=27 km/s1

2

3

4

Weiss and OSIRIS Team

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Resolved Kinematics in theRedshift Desert

Wright et al 2007

Shelley Wright

3939UCLAD. Law, C. D. Law, C. SteidelSteidel, D. , D. ErbErb, J. Larkin, S. Wright, et al. 2007, J. Larkin, S. Wright, et al. 2007

OSIRIS: Galaxies in the Early UniverseOSIRIS: Galaxies in the Early Universe

Observe spectral shiftsObserve spectral shifts

of hydrogen emissionof hydrogen emission

lines due to velocitylines due to velocity

offsets.offsets.

Velocity maps (centerVelocity maps (center

column) showcolumn) show

unexpected patterns-unexpected patterns-

some rotate, somesome rotate, some

dondon’’t!t!

Suggests a complexSuggests a complex

fragmentation view offragmentation view of

galaxy formation.galaxy formation.

(L to R) Line emission, velocity, and velocity dispersion maps(L to R) Line emission, velocity, and velocity dispersion mapsfor 3 target galaxies.for 3 target galaxies.

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NIRC~1 hour

Scam – NIRSPEC~1 hour

NIRC2~1 hour

1”

OSIRISH-BandOH-suppressedCollapsed Spectrum0.100” scale15 minutes

OH-SuppressionOH-SuppressionPPM114182+6+27 imagePPM114182+6+27 image

Companion: H>22 Companion: H>22 mag mag @ 0.6@ 0.6”” separation separation

R=20 Spectrum

R=20 Background

Spectrum of Companion

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GQ GQ LupLup

•• Possible planetaryPossible planetary

companion (J=13mag).companion (J=13mag).

•• J band contrast is 6 J band contrast is 6 magmag

at 0.73at 0.73”” separation. separation.

•• 10 Minute exposure.10 Minute exposure.

•• Really Brown DwarfReally Brown Dwarf

McElwain, Metchev and OSIRIS Team (2006)

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HD 130948HD 130948

•• G1 PrimaryG1 Primary

•• Binary L DwarfBinary L Dwarf

companionscompanions

1.31.3””0.10.1””

6.46.4””

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OSIRIS OSIRIS Redshift Redshift Record Record z=6z=6.42.42

•• Quasar ~10Quasar ~1099 solar mass solar mass blackholeblackhole

•• CapakCapak, , ScovilleScoville, Larkin & Wright (April, Larkin & Wright (April

2007)2007)

•• Light from 12.9 Billion years agoLight from 12.9 Billion years ago

•• Seen only 800 Million years after the BigSeen only 800 Million years after the Big

Bang.Bang.

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OSIRIS caveats/summaryOSIRIS caveats/summary

•• OSIRIS works well with compact objects,OSIRIS works well with compact objects,meaning ~1meaning ~1””–– Extended objects quickly get split into hundreds ofExtended objects quickly get split into hundreds of

lensletslenslets..

•• Detector limited in many modesDetector limited in many modes

•• Background limited in the K-band with increasedBackground limited in the K-band with increasedbackgrounds due to AO and oversized pupils.backgrounds due to AO and oversized pupils.

•• AO with Laser is still not AO with Laser is still not ““routineroutine””, and requires, and requireslots of preparation and some patience.lots of preparation and some patience.

•• ButBut on good nights,on good nights, laser operations are verylaser operations are veryefficient.efficient.

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GPI:GPI:Gemini Planet ImagerGemini Planet Imager

•• Instrument for the Gemini TelescopesInstrument for the Gemini Telescopes

–– PI: Bruce Macintosh (LLNL)PI: Bruce Macintosh (LLNL)

–– PS: James Graham (UCB)PS: James Graham (UCB)

–– Colloborations Colloborations at LLNL, HIA, AMNH, JPL, U.ofat LLNL, HIA, AMNH, JPL, U.ofMontreal, and UCSC.Montreal, and UCSC.

•• UCLA will be responsible for the infraredUCLA will be responsible for the infraredintegral field spectrograph.integral field spectrograph.

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GPI Main MissionGPI Main Mission

•• Goal of GPI is to look at nearby young starsGoal of GPI is to look at nearby young stars

(about 100 stars) and try and find (about 100 stars) and try and find Jovian Jovian planetsplanets

that are still that are still ““self-luminousself-luminous””..

•• Problem remains, the star is still much brighterProblem remains, the star is still much brighter

(>1,000,000) and within 1 arcsecond of the(>1,000,000) and within 1 arcsecond of the

planet.planet.

•• GPI is an extreme AO system with specialGPI is an extreme AO system with special

coronagraph and coronagraph and interferometric interferometric calibrationcalibration

system.system.

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Why an IFU?Why an IFU?

•• It takes a spectrum!It takes a spectrum!•• At At Strehl Strehl ratios of ~95%,ratios of ~95%,

dominant background isdominant background isin speckles.in speckles.

•• A Planet will be fainterA Planet will be fainterthan many of thesethan many of thesespeckles.speckles.

•• But the speckles areBut the speckles arereally little rainbows!really little rainbows!

•• So an IFU will see aSo an IFU will see adifferent speckle patterndifferent speckle patternat each wavelength.at each wavelength.

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Star

Companion

Speckles

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Dispersion and SpecklesDispersion and Speckles

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Simulated Raw DataSimulated Raw Data•• Each spectrum is 16 pixels long.Each spectrum is 16 pixels long.

•• 68,000 spectra on a 2048x2048 detector.68,000 spectra on a 2048x2048 detector.

•• Spectra are separated by 4.5 pixels from their nearestSpectra are separated by 4.5 pixels from their nearestneighbors.neighbors.

Single Spectrum

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Speckles In Standard ImageSpeckles In Standard Image

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Speckles with IFUSpeckles with IFU

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GPI ScheduleGPI Schedule

•• Competition with Arizona.Competition with Arizona.

–– March 10-11, 2005March 10-11, 2005

•• We were selected in August, 2005.We were selected in August, 2005.

•• Contract started in June, 2006Contract started in June, 2006

•• Successful PDR in May 2007.Successful PDR in May 2007.

•• IFU will be complete in mid-2009.IFU will be complete in mid-2009.

•• On sky in 2010.On sky in 2010.

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IRIS: Super OSIRIS for TMTIRIS: Super OSIRIS for TMT

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Scientific JustificationsScientific Justifications

•• Star and planet formation (Star and planet formation (YSOYSO’’ss))–– Probably only one per field.Probably only one per field.

•• Stellar Clusters / population studiesStellar Clusters / population studies–– Single Field Single Field –– many objects many objects

–– Proportional to field sizeProportional to field size

•• Galactic CenterGalactic Center–– Single Field Single Field –– many objects. many objects.

–– Requires precision astrometryRequires precision astrometry

•• Planets & MoonsPlanets & Moons–– One per fieldOne per field

•• AGN AGN –– Quasars Quasars –– Radio Galaxies Radio Galaxies–– One per fieldOne per field

•• Strong Gravitational LensesStrong Gravitational Lenses–– Typically 1Typically 1”” or less in separation or extent or less in separation or extent

•• Spatially resolved kinematics and chemistry within highSpatially resolved kinematics and chemistry within highz galaxies.z galaxies.

–– Core sizes 0.2Core sizes 0.2’’’’, scale 1, scale 1””=9 kpc=9 kpc

–– Res~4000Res~4000

–– K~22-23magK~22-23mag

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IRIS RequirementsIRIS Requirements

•• Wavelength Range: 0.8-2.5 microns. Goal 0.6-5 micronsWavelength Range: 0.8-2.5 microns. Goal 0.6-5 microns

•• Field of View:Field of View:

–– Fields of view up to 2Fields of view up to 2””

–– Nyquist Nyquist Sampled (Sampled ( /2D) over 64x64 pixels for IFU/2D) over 64x64 pixels for IFU

•• At 1 micron, Nyquist~0.004At 1 micron, Nyquist~0.004””, this is only 0.256, this is only 0.256””x0.256x0.256””

•• Spectral Resolution of R=4000 over 20% Spectral Resolution of R=4000 over 20% bandpassbandpass

•• Excellent Image Quality (WFE < 25 nm)Excellent Image Quality (WFE < 25 nm)

•• High ThroughputHigh Throughput

•• Instrument background not more than 15% greater thanInstrument background not more than 15% greater than

Telescope+AO.Telescope+AO.

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SummarySummary

•• OSIRIS is now in regular use at Keck.OSIRIS is now in regular use at Keck.

•• IFUs IFUs are becoming the instrument of choice forare becoming the instrument of choice forAO systems.AO systems.–– TPF-C had an IFU as baseline.TPF-C had an IFU as baseline.

•• At UCLA weAt UCLA we’’re working to develop advancedre working to develop advanceddiffraction limited diffraction limited IFUIFU’’ss..–– OSIRIS: 2005OSIRIS: 2005

–– GPI: 2010GPI: 2010

–– IRIS: 2015IRIS: 2015