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GMT’s Near IR Multiple Object Spectrograph - NIRMOS

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.

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GMT’s Near IR Multiple Object Spectrograph - NIRMOS

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

  2. NIRMOS Scientific Drivers • Discovery and characterization of the first galaxies • Assembly and evolution of galaxies at z=2 to 3 • Chemical evolution of galaxies

  3. 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.”

  4. Galaxies in formation 11 Gyr ago

  5. Galaxies are different at z=2 Kriek et al. 2009

  6. Compact red sequence galaxy 11 Gyr ago This galaxy has a stellar mass of 3 x 1011 Mסּ despite its tiny size! Van Dokkum, Kriek & Franx 2009

  7. Evolution of massive galaxies Re = 8 kpc 6 Gyr ago Re = 3 kpc 10 Gyr ago Galaxies selected from mass-number density relation at constant number density van Dokkum et al. 2010

  8. 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 2009 Kriek et al. 2009

  9. JWST and GMT: natural partners James Webb Space Telescope 2014 Giant Magellan Telescope 2018

  10. JWST NIRCam imaging 10 square arcminutes in two bands 0.07″ images at 2.2 µm Superb photometry and galaxy stucture 2 arcminutes

  11. JWST’s NIRSpec • Multiple object spectrograph • at R=100 and R=1000 with 9 square arcminute FOV • IFU and long slit at R=3000 • 0.2″ nominal slit width At R=100 with very low background, JWST is a superb tool for rapid redshiftmeasurements 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

  12. GMT IR spectroscopy of distant galaxies • Go faint: Observe galaxies 11 Gyr ago with ~3 x 1010 Mסּ 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

  13. GMT’s NIRMOS NN • 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 NIRSpec NIRMOS Field of View 35 square arcminutes ~105 z>2 galaxies! GMT/NIRMOS at R=3000 is twice as sensitive as JWST/NIRSpec at R=1000, with 4x the field of view

  14. Ground Layer Adaptive Optics Ground layer wavefront errors are weakly dependent on field angle GLAO will improve spatial resolution by ~2 1.5 kpc resolution at z=2.5, same as JWST NIRSpec

  15. NIRMOS optical layout Fused Quartz CaF2 CaF2 S-TIM28 CaF2 (four segments) Fused Quartz aspheric 4 meters • 275 mm collimated beam diameter • CaF2 lens blanks < 390 mm diameter available from current production • Volume Phase Holographic gratings for dispersers

  16. Criticaltechnologies for NIRMOS

  17. NIRMOS at GMT’s Gregorian Focus

  18. NIRMOS mechanical layout Spectroscopy Imaging Slit mask cassette Collimator optics 5m Filter and grating wheels Camera Optics Optics and mechanics cooled to 120 K

  19. NIRMOS focal plane area Cryocoolers Slit mask cassette Manifest fibers Tip/tilt guiders

  20. 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

  21. The End

  22. High Altitude Turbulence Restricts the Diffraction-limited Field of View *

  23. 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)

  24. NIRMOS at GMT’s Gregorian focus

  25. NIRMOS mechanical layout Optics and mechanics cooled to < 100 K

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