Gemini: A Visiting DMD-based spectro-imager
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1 Gemini: A Visiting DMD-based spectro-imager Frederic Zamkotsian, Julien Zoubian, Romain Thomas, Carlo Schimd, Sylvain de la Torre, Eric Jullo, Olivier Ilbert, Samuel Boissier, Georges Comte, Jean-Claude Bouret, Delphine Russeil, Audrey Delsanti, Pierre Vernazza, Benoit Neichel, Alessandro Boselli, Benoit Epinat, Philippe Amram, Walter Boshin, Luigi Guzzo + BATMAN French-Italian team frederic.zamkotsian@lam.fr
2 BATMAN concept Field of view Measured spectra TNG CCD camera Spectrograph arm Micro-mirror array in the telescope focal plane Imaging arm
3 Multi-object spectroscopy Hubble ultra deep field (HUDF), NASA, 3/9/2004 Telescope s field of view Thousands of galaxies Overlapping Spectra Measured spectra Telescope (ground or space) CCD Camera Reflective surface Spectrometer
4 Multi-object spectroscopy Hubble ultra deep field (HUDF), NASA, 3/9/2004 Telescope s field of view Thousands of galaxies Measured spectra Telescope (ground or space) CCD Camera Spectrometer 2D Micromirror array in the telescope focal plane
5 Texas Instruments DMD Most popular MOEMS devices available on the market. Micro-mirrors 2048x1080 individually tiltable (> 2 millions mirrors) 13.68µm pixel pitch, Tilt angle of 12 Numerous applications Prime use displaying images No customization possible Space qualification tests (ESA contract, EUCLID) -40 C in 10-5 mbar vacuum Micro-mirrors in position for > 1500s DMD fully operational 1038 hours life test, radiations, vibrations No show-stopper for space application
6 Parameters: Field of view Focal ratio Beams on DMD Wavelength range Spectral resolution Two arms instrument Detectors 6.8 arcmin x 3.6 arcmin F/4 on DMD (scale = 0.2 arcsec per micromirror) incoming light at normal incidence out-coming light at 24 DMD orientation at nm R = 560 for 1 arcsec slit to 2000 for 0.2 arcsec slit one spectroscopic channel one imaging channel Two 2k x 4k CCDs
7 Optical design
8 Optical design
9 Simulated spectra Simulated spectra ( nm)
10 BATMAN: the opto-mechanics
11 BATMAN
12 BATMAN is under construction
13 BATMAN is under construction
14 BATMAN is under construction
15 BATMAN is under construction
16 BATMAN is under construction
17 BATMAN is under construction
18 BATMAN is under construction
19 BATMAN is under construction
20 BATMAN is under construction Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera Pixels Camera
21 BATMAN is under construction Pixels Camera Pixels Camera Slit: 1 µm (13.68 µm) Spectrum on 1.5 detector pixel (8,3µm) in nm wavelength range
22 BATMAN is under construction Pixels Camera Pixels Camera Pixels Camera Pixels Camera Slit: 1 µm (13.68 µm) Spectrum on 1.5 detector pixel (8,3µm) in nm wavelength range
23 Simu BATMAN : limiting magnitude
24 TNG ( ) Italian telescope 3,6m Seeing-limited First Science Cases Gemini ( ) US telescope 8,2m MCAO (GeMS) 90 mas resolution VLT ( ) European telescope 8,2m Visible MCAO (MAVIS) 20 mas resolution
25 TNG MOEMS-DMD/MIRA Focal plane Spectrograph Imager Telescope Focal plane Pupil plane FOV = 6.8 x 3.6 arcmin2
26 Gemini MOEMS-DMD Focal plane Spectrograph Imager Gemini + visible GeMs Focal plane Pupil plane FOV = 1.5 x 1.5 arcmin2
27 Parameters (TNG / Gemini) TNG (F/4) 3.6m Gemini + GeMS (F/4) 8.2m Gemini + GeMS (F/8) 8.2m Spatial resolution Field of view x 3.6 arcmin x 1.5 arcmin x 0.8 arcmin2
28 Nearby galaxies physics Nearby galaxies characterization (ex: XUV galaxies) Short time-scale star formation rate (Halpha), the dust distribution (Balmer ratio), the kinematics, the nucleus physics (AGN vs starburst), abundances) For instance, study of NGC772 - central part of gal. / nucleus - kinematics of the elongated spiral arms - star forming regions in the disk - star forming region in the XUV part of gal. - comparison with regular part of disk (metallicity, IMF, star forming history) Instrument parameters Complete multiplexing of all regions in the FOV Optical spectroscopy (R )
29 Nearby galaxies physics IFU Adaptable slit: following star formation regions
30 Nearby galaxies physics IFU Sliding slit: 3D galaxy arm reconstruction
31 Nearby galaxies physics IFU Sliding slit: 3D galaxy arm reconstruction Gemini + GeMS + BATMAN = from nearby to remote galaxies
32 Stellar physics Open clusters: characterization of the stellar content, especially the PDMF (present day mass function) Stellar physics and star formation in the Galactic center Clusters in the local group (Magellan clouds) Spectroscopic analysis of stars - distribution of stellar classes/types within the cluster (e.g. does the cluster core harbors the most massive stars?) constraints on IMF scenarios - physical distance of the cluster and location with respect to galactic arms (requires flux calibration) constraints on star formation - establish the evolutionary status of stars in the cluster (HR diagram) pinpoint empirical evolutionary links between different types of stars (e.g. massive dwarfs vs masive giants/supergiants, WRs) test whether single star evolutionary tracks can account for the observed stellar population Spectroscopic analysis of the diffuse matter in the cluster - derive ionization parameters, abundances, kinematics, selective extinction physics of HII regions etc)
33 Stellar physics MOS NGC6334 NGC6357 Instrument parameters Complete multiplexing of stars in the FOV: MOS with 100s objects Requires flux calibration Spatial resolution 0.6 down to 0.08 with Gemini+GeMS (access to the core of the clusters) Optical spectroscopy, R 1500 (5000)
34 Stellar physics MOS The EHB (Extreme Horizontal Branch) stars in globular clusters Faint blue stars (high Teff, lower luminosity, higher gravities) Physics of these objects - Variable surface abondance of He - Surface gravity - Fitting of Balmer lines profiles to Stark effect models NGC 1808 Instrument parameters Multiplexing of stars in the FOV Optical spectroscopy, R 1500 Spatial resolution 0.6 to 0.08 Imagery for selection of objects (color-magnitude diagram det. by imagery in different bands) EHB H B
35 Stellar physics MOS Binaries: what is the fraction of Mdwarf WhiteDwarf binaries? Is there a clue to the apparent deficit of isolated WD in cluster populations? M67 Search of WD binaries Simultaneously check on normal main sequence binary pop. Locus of ms-ms binaries Instrument parameters Multiplexing of stars in the FOV Optical spectroscopy R 500 Spatial resolution 0.08 Very good photometry Expected locus of ms+wd binaries
36 Solar system objects Transients Near Earth Objects detection and characterization V = 1.5 arcmin / hour mag vis = Simultaneous spectro of G2 stars Extension to asteroïds Instrument parameters Imagery: detection and trajectory determination Optical spectroscopy R Adjustable integration time Itokawa (Hayabusa) Follow the object (imagery to spectroscopy in 1ms after alert)
37 BATMAN: the simulator
38 BATMAN: the simulator
39 BATMAN: the simulator
40 on Key numbers FOV 1.5 x 0.75 arcmin 2 (+) Spatial sampling 45mas / µm / detector pixel Imagery: multi-band filters Spectro: spectral resolution (+) Spectro MOS: 1 several 100s objects Spectro IFU: FOV 1 up to 90 (sequential) Unique abilities Imagery and spectroscopy in parallel (high accuracy photometry) Highly flexible (any combination of MOS, IFU, spectral resolution ) Transients (spatial, temporal), like SNe, NEO, AGN Schedule BATMAN on Gemini in MOS IFU Transients
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