GMT’s Near IR Multiple Object Spectrograph - NIRMOS

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GMT’s Near IR Multiple Object Spectrograph - NIRMOS Daniel Fabricant Center for Astrophysics

description

GMT’s Near IR Multiple Object Spectrograph - NIRMOS. Daniel Fabricant Center for Astrophysics. NIRMOS Scientific Drivers. Discovery and characterization of the first galaxies Assembly and evolution of galaxies at z=2 to 3 Chemical evolution of galaxies. - PowerPoint PPT Presentation

Transcript of GMT’s Near IR Multiple Object Spectrograph - NIRMOS

Page 1: GMT’s Near IR Multiple Object Spectrograph - NIRMOS

GMT’s Near IR Multiple Object Spectrograph - NIRMOS

Daniel FabricantCenter for Astrophysics

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NIRMOS Scientific Drivers

• Discovery and characterization of the first galaxies

• Assembly and evolution of galaxies at z=2 to 3

• Chemical evolution of galaxies

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GMT and NIRMOS probe galaxy evolution from first light

Tentative IR detection of Ly α emission looking back 13 Gyr (Stark et al. 2007) ~10 hrs with Keck.

“At the faint limits now being probed, we have found the reliable identification and verification of distant Ly α emitters to be a very challenging endeavor, even with the most powerful facilities available to us.”

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Galaxies in formation 11 Gyr ago

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Galaxies are different at z=2

Kriek et al. 2009

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Compact red sequence galaxy 11 Gyr ago

Van Dokkum, Kriek & Franx 2009

This galaxy has a stellar mass of3 x 1011 Mּס despite its tiny size!

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Evolution of massive galaxies

van Dokkum et al. 2010

Re = 3 kpc10 Gyr ago

Re = 8 kpc6 Gyr ago

Galaxies selected from mass-number density relation at constant number density

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29 hr spectrum of H=20 Galaxy with Gemini 8 m

GMT will attain S/N of 10 for H=22.5 in 10,000 sec in natural seeing

Van Dokkum, Kriek & Franx 2009Kriek et al. 2009

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JWST and GMT: natural partners

James Webb Space Telescope

2014

Giant Magellan Telescope

2018

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JWST NIRCam imaging

2 arcminutes

10 square arcminutes in two bands

0.07″ images at 2.2 µm

Superb photometry and galaxy stucture

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JWST’s NIRSpec

At R=100 with very low background, JWST is a superb tool for rapid redshift measurements and selection of galaxy samples

At the resolution needed for dynamical mass measurements, a GMT instrument can provide greater sensitivity and larger fields of view than NIRSpec

• Multiple object spectrographat R=100 and R=1000 with 9 square arcminute FOV

• IFU and long slit at R=3000

•0.2″ nominal slit width

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GMT IR spectroscopy of distant galaxies

• Go faint: Observe galaxies 11 Gyr ago with ~3 x 1010 Mּס HVega=22.5 or HAB=24

• Infrared: Distant quiescent galaxies are bright at λ > 1.4 µm

• Wide-field: ~3 galaxies arcmin-2 at z > 2

• Spectral resolution: λ/Δλ~3000 for 100 km s-1 resolution and to reduce OH contamination

• Angular resolution: 3 kpc ~0.36 arcsec (LCO median at H), GLAO assist helpful

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GMT’s NIRMOS

NIRMOS Field of View35 square arcminutes

~105 z>2 galaxies!

• 0.9 to 2.5 μm imaging spectrograph

• Natural seeing or GLAO

• R~3000 with 0.5″ slit and full J, H, or K coverage – higher resolution possible

• Superb image quality: worst 80% EE better than 0.15″

•Volume Phase Holographic gratings reduce scattering (and OH background) by order of magnitude

NNNIRSpec

GMT/NIRMOS at R=3000 is twice as sensitive as JWST/NIRSpec at R=1000, with 4x the field of view

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Ground Layer Adaptive Optics

GLAO will improve spatial resolution by ~2

1.5 kpc resolution at z=2.5, same as JWST NIRSpec

Ground layer wavefront errors are weakly dependent on field angle

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NIRMOS optical layoutFused Quartz

CaF2 (foursegments)

CaF2CaF2

aspheric

S-TIM28

Fused Quartz

• 275 mm collimated beam diameter

•CaF2 lens blanks < 390 mm diameter available from current production

• Volume Phase Holographic gratings for dispersers

4 meters

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Critical technologies for NIRMOSTechnology Status

Large calcium fluoride lens blanks Canon/Optron quote in hand

Large S-TIM28 lens blanks Ohara quote in hand

Detector array Teledyne will produce, estimate in hand

Large cryogenic VPH gratings - Kaiser Optical could produce, K band performance the major open item

Ground layer adaptive optics $ Dependent on adaptive secondary mirror – soft fallback to seeing limited operation

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NIRMOS at GMT’s Gregorian Focus

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NIRMOS mechanical layout

Optics and mechanics cooled to 120 K

Collimator optics

Camera Optics

Filter and gratingwheels

Slit mask cassette

ImagingSpectroscopy

5m

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NIRMOS focal plane area

Manifest fibers

Tip/tilt guiders

Slit mask cassette

Cryocoolers

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Conclusions

• We believe that NIRMOS has great scientific potential, is technically feasible and affordable

• We invite our GMT partners to explore NIRMOS science with us

• We look forward to exploiting the potential of IR fiber technology with the MANIFEST team

• We are interested in collaborations in IR technology with GMT partners

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The End

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High Altitude Turbulence Restricts the Diffraction-limited Field of View

*

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NIRMOS in the JWST era

• NIRMOS at R=3000 is 2x as sensitive than NIRSpec at R=1000, with 4x the field of view

• NIRMOS at R=3000 is ~10x more sensitive than NIRSpec at R=3000 and retains MOS

• In natural seeing, NIRMOS attains S/N of 10 in 10,000 s at H=22.5 (0.5 x 0.5 arcsec)

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NIRMOS at GMT’s Gregorian focus

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NIRMOS mechanical layout

Optics and mechanics cooled to < 100 K