OSIRIS: The Latest Keck Instrument and its Science
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1 OSIRIS: The Latest Keck Instrument and its Science James Larkin UCLA April 5, 2007 Photo John MacDonald CFHT
2 Outline How is OSIRIS different? Early Science Future Directions April 5, 2007 OSIRIS 2
3 How is OSIRIS Different? First it works with the Keck Adaptive Optics (AO) System So it dissects very small (~1 arcsecond) patches of the sky. Keck AO installed in 1999 High order Laser AO Just upgraded with new wfs and controller. Great performance April 5, 2007 OSIRIS 3
4 How Small is an arcsecond? Hold your thumb out at arm s length. Your thumbnail is about the same angular size as the moon, about 30 arcmin. An arcsecond is the width of your thumb held at a distance of 2km (1.3 miles) This is about 60 times smaller than the human eye can resolve. April 5, 2007 OSIRIS 4
5 The atmosphere limits angular resolution. Light from science target Perfect Plane Wave Atmosphere corrugates the wavefront Creates blurred images Seeing disk ~ 1 arcsecond Telescope System Science Camera Atmospheric cell sizes are ~20 cm They set the resolution regardless Telescope diameter. April 5, 2007 OSIRIS 5
6 Light from science target AO measures and corrects for the atmospheric turbulence. Light from reference star Creates partially sharpened images FWHM ~ arcsecond Strehl Ratio ~ Percentage of power restored to core. Deformable Mirror Science Camera Beam Splitter Computer Wavefront Sensor April 5, 2007 OSIRIS 6
7 Na Laser Guide Star AO Sodium Layer Altitude of 90km (mesosphere) 5-10 km thick. From ablation of meteorites High Power Laser Tuned to 589 nm Resonant scattering Claire Max, LLNL April 5, 2007 OSIRIS 7
8 Laser Guide Star Produces star at high altitude Can be placed directly on the target. Sodium Beacon Rayleigh Back Scatter April 5, 2007 OSIRIS 8 From Claire Max
9 AO on real objects Neptune Redshift 0.5 Disk Galaxy April 5, 2007 OSIRIS 9
10 Spectrographs April 5, 2007 OSIRIS 10
11 Spectrographs April 5, 2007 OSIRIS 11
12 Slit Spectroscopy Deimos, LRIS April 5, 2007 OSIRIS 12
13 AO Focus Pupil Plane Lenslet Array 1mm MEMs Optical - Infrasil, biconvex elements. Thickness is 1.0 mm with EFL of 0.8 mm. Pitch is 250 microns. 72x72 lenslet square area centered in 1.5 diameter circular substrate. ~98% fill factor April 5, 2007 OSIRIS 13
14 Dispersing Lenslet Spots April 5, 2007 OSIRIS 14
15 Dispersing Lenslet Spots April 5, 2007 OSIRIS 15
16 Dispersing Lenslet Spots April 5, 2007 OSIRIS 16
17 5% Bandpass OSIRIS Spectra White Light (3072 spectra) Arc Lines (3072 spectra) April 5, 2007 OSIRIS 17
18 Hn3 Diffraction-limited pinholes FWHM = 1.78 lenslets = 36 mas. April 5, 2007 OSIRIS 18
19 UCLA Infrared Lab Founded in 1989 Part of UCO Professors: Ian McLean and James Larkin Graduate Students: Matthew Barczys, Michael McElwain, Emily Rice, Sara Salha, Erin Smith, Shelley Wright Engineering Staff: Ted Aliado, George Brims, John Canfield, Chris Johnson, Evan Kress, Ken Magnone, John Milburn, Eric Wang, Jason Weiss. Major Instruments: GEMINI, NAVYCAM, KCAM*, NIRSPEC*, FLITECAM, NIRC2*, OSIRIS*, SHARC* Future Instruments: GPI IFU*, MOSFIRE, IRIS* *Optimized for AO April 5, 2007 OSIRIS 19
20 New Technologies made OSIRIS possible Hawaii-2 Detector (2048x2048) Rockwell R=3900 broadband spectrum requires >1700 pixels Extremely low dark currents (0.025 e/sec) which is still above background between OH-lines at AO platescales. 32 channels of cryogenic preamplifiers built at UCLA. Operates at about 60K or -350 F. April 5, 2007 OSIRIS 20
21 Small pupils require fast lenslets, which require a fast spectrograph. Large all metal off-axis optics - SSG Inc. April 5, 2007 OSIRIS 21
22 Fixed Grating Diffraction Products ruled directly on gold coating. The desire for high repeatibility, ease of reduction and calibration favor a fixed grating. Large format detector allows us to fit full broad band in one shot. Blazing the grating at 6.5 microns places each order within different bands. Order: 3 rd 4 th 5 th 6th Range: cm ~Band: K H J z April 5, 2007 OSIRIS 22
23 Six internal cryogenic mechanisms Designed and built at UCLA Each mechanism must run many thousands of times at -350 F. Special dry lubricants. Great care is used in selecting materials. April 5, 2007 OSIRIS 23
24 April 5, 2007 OSIRIS 24
25 April 5, 2007 OSIRIS 25
26 April 5, 2007 OSIRIS 26
27 April 5, 2007 OSIRIS 27
28 April 5, 2007 OSIRIS 28
29 First light Feb 22, 2005 clear with about 1 seeing FWHM=0.043 at K 40% Strehl at K First target was within 0.15 of field center. 0.2 April 5, 2007 OSIRIS 29
30 NGC 4151 Nearby Galaxy with a central active blackhole. April 5, 2007 OSIRIS 30
31 nucleus Flux [a.u.] H2 HeI H2 Brγ H2 [Ca VIII] off-nucleus [Fe II] CO λ [micron] April 5, 2007 OSIRIS 31
32 nucleus Flux [a.u.] H2 HeI H2 Brγ H2 [Ca VIII] off-nucleus [Fe II] CO λ [micron] April 5, 2007 OSIRIS 32
33 NGC Maps April 5, 2007 OSIRIS 33
34 Each pixel=129 km 0.8 Stratosphere Surface April 5, 2007 OSIRIS 34 Bouchez and OSIRIS Team
35 LGS Observations of V723 Cas (Nova Cas 1995) Campbell, Lyke, Team Keck Resolve Novae Shells Observe morphology & kinematics Directly determine distance Spatially distinct emission regions? [Si VI] μm [Al IX] μm Brγ μm April 5, 2007 OSIRIS 35
36 3D Visualization Red: [Al IX] Blue: [Si VI] Green: Brγ April 5, 2007 OSIRIS 36
37 How old is our Milky Way Galaxy? NGC 1232 Galaxies are a massive collection of stars, gas, dust, and dark matter Ages of oldest stars (white dwarfs) show a Milky Way age of 7.3 Billion Years Old Clusters of stars in the Milky Way implies an age between 7.5 to 10 Billion Years Old Unknown Birthdate for Spiral Galaxies??? Shelley Wright April 5, 2007 OSIRIS 37
38 Spiral Galaxy s Unique Rotation April 5, 2007 OSIRIS 38
39 OSIRIS LGS-AO Observations of Galaxies 9.5 Billion Years Ago 9.6 Gyr 9.7 Gyr 9.5 Gyr Gyr 9.6 Gyr Hα emission redshifted into the near infrared April 5, 2007 OSIRIS 39
40 Candidate Disk Galaxy 9.3 Billion Years Ago Wright et al 2007 April 5, 2007 OSIRIS 40
41 OSIRIS: Galaxies in the Early Universe Observe spectral shifts of hydrogen emission lines due to velocity offsets. Velocity maps (center column) show unexpected patternssome rotate, some don t! Suggests a complex fragmentation view of galaxy formation. (L to R) Line emission, velocity, and velocity dispersion maps for 3 target galaxies. April 5, 2007 OSIRIS 41 Results in preparation: D. Law, C. Steidel, D. Erb, J. Larkin, S. Wright, et al. These data obtainable only with Keck LGS + OSIRIS.
42 4c48.48:Radio Galaxy OSIRIS (z=2.343, 11.1 Billion light years) 1 [OIII] (500.7nm) Steps=27 km/s H+K image Carson et al kpc Weiss and OSIRIS Team April 5, 2007 OSIRIS 42
43 Last night New OSIRIS redshift record of z=6.42 ~10 9 solar mass blackhole (Quasar) Capak, Scoville, Larkin & Wright Light from 12.9 Billion years ago Seen only 800 Million years after the Big Bang. April 5, 2007 OSIRIS 43
44 Variability of Sgr A* K-band 0.02 /lenslet 15 minutes per slice With Ghez et al. Laser Shuttered by Telescope Crossing SGR A * AU Time April 5, 2007 OSIRIS 44
45 HD G1 Primary Binary L Dwarf companions April 5, 2007 OSIRIS 45
46 High Contrast Imaging Mike McElwain s Thesis At moderate Strehl ratios (< 0.95) and small separations (< 1 ), speckle noise produced by atmospheric wavefront distortion and imperfect optics are the dominate noise source. Typical speckle pattern for Keck II + OSIRIS Imager Innovative techniques for enhancing contrast Simultaneous Differential Imaging Spectral Suppression Speckles are wavelength dependent and can be modeled for each wavelength. Keck II + OSIRIS Spec in the Kbb filter April 5, 2007 OSIRIS 46
47 GQ Lup Possible planetary companion (J=13mag). Companion is 250 times fainter and only 0.73 away. 10 Minute exposure with Keck. McElwain, Metchev and OSIRIS Team April 5, 2007 OSIRIS 47
48 Future IFS: GPI: Gemini Planet Imager Instrument for the Gemini Telescopes PI: Bruce Macintosh (LLNL) PS: James Graham (UCB) Colloborations at LLNL, HIA, AMNH, JPL, U.of Montreal, and UCSC. UCLA will be responsible for the infrared integral field spectrograph. April 5, 2007 OSIRIS 48
49 GPI Main Mission Goal of GPI is to look at nearby young stars (about 100 stars) and try and find Jovian planets that are still self-luminous. Problem remains, the star is still much brighter (>1,000,000) and within 1 arcsecond of the planet. GPI is an extreme AO system with special coronagraph and interferometric calibration system. April 5, 2007 OSIRIS 49
50 Why an IFU? It takes a spectrum! At Strehl ratios of ~95%, dominant background is in speckles. A Planet will be fainter than many of these speckles. But the speckles are really little rainbows! So an IFU will see a different speckle pattern at each wavelength. April 5, 2007 OSIRIS 50
51 Speckles In Standard Image April 5, 2007 OSIRIS 51
52 Speckles with IFU April 5, 2007 OSIRIS 52
53 IRIS: Super OSIRIS for TMT April 5, 2007 OSIRIS 53
54 IRIS Optics Expandable with dithered lenslets. Lenslet Array 4.3 m Common reimager camera lens Alternate Gratings On Turret Imager Filter Wheels April 5, 2007 OSIRIS F/15 AO 54 Focus
55 Scientific Justifications Star and planet formation (YSO s) Probably only one per field. Stellar Clusters / population studies Single Field many objects Proportional to field size Galactic Center Single Field many objects. Requires precision astrometry Planets & Moons One per field AGN Quasars Radio Galaxies One per field Strong Gravitational Lenses Typically 1 or less in separation or extent Spatially resolved kinematics and chemistry within high z galaxies. Core sizes 0.2, scale 1 =9 kpc Res~4000 K~22-23mag April 5, 2007 OSIRIS 55
56 Summary OSIRIS is now in regular use at Keck. IFSs are becoming the instrument of choice for AO systems. TPF-C had an IFS as its baseline. At UCLA we re working to lead diffraction-limited IFS development. OSIRIS: 2005 GPI: 2010 IRIS: 2015 April 5, 2007 OSIRIS 56
57 Happy Birthday Debbie! April 5, 2007 OSIRIS 57
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