Visible MCAO supported spectro-imager: the BATMAN …€¦ · + BATMAN French-Italian team 1 Laboratoire d'Astrophysique de Marseille, France 2 INAF Osservatorio Astronomico di Brera,

VLT AO community days, 20-21 Sept. 2016

Frederic Zamkotsian, Romain Thomas, Julien Zoubian, Carlo Schimd, Sylvain de la Torre, Eric Jullo, Olivier Ilbert, Samuel Boissier, George s Comte, Jean-Claude Bouret,

Delphine Russeil, Audrey Delsanti, Pierre Vernazza, B enoit Neichel

+ BATMAN French-Italian team

1 Laboratoire d'Astrophysique de Marseille, France2 INAF Osservatorio Astronomico di Brera, Italy

3 INAF/IASF Bologna, Italy4 INAF - Telescopio Nazionale Galileo, Spain

5 INAF-OAT, Osservatorio Astronomico di Trieste, Italy

Visible MCAO supported spectro -imager: the BATMAN family


Extragalactic physics and cosmology

�Dynamical model reconstruction of local structure g rowth� Velocity survey of large galaxies FOV� zspectro = zcosmo + vp / c� By Tully-Fischer, Vmax gives the intrinsic luminosity and then zc

� Determination of the dynamical model / structure growth

�Instrument parameters� Complete multiplexing of the FOV� Optical spectroscopy (R 1500)

7 velocity meas. across the gal.(0.2-0.4” slits)

� Study at z=0.5 (z=1)� Flux calibration


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 vsstarburst), 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 1000-1500)


Stellar physics

�Open clusters: characterization of the stellar conte nt, 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)


Stellar physics

�Instrument parameters� Complete multiplexing of stars in the FOV� Requires flux calibration� Spatial resolution 0.15” – 0.2”� Optical spectroscopy, R 1500 (5000)

NGC6334 NGC6357


Stellar physics

�The EHB (Extreme Horizontal Branch) stars in globula r 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

�Instrument parameters� Multiplexing of stars in the FOV� Optical spectroscopy, R 1500 � Spatial resolution 0.2”� Imagery for selection of objects

(color-magnitude diagram det.by imagery in different bands)

H B

NGC 1808

EHB


Stellar physics

�Binaries: what is the fraction of Mdwarf – WhiteDwar f binaries? Is there a clue to the apparent deficit of isolated WD in cluster populations ?

� Search of WD binaries� Simultaneously check on normal

main sequence binary pop.

�Instrument parameters� Multiplexing of stars

in the FOV� Optical spectroscopy

R 500 � Spatial resolution 0.2”� Very good photometry

M67

Locus ofms-ms binaries

Expected locus of ms+WD binaries


Solar system objects

�Near Earth Objects detection and characterization� V = 1.5 arcmin / hour� magvis = 16 – 19� Simultaneous spectro of G2 stars� Extension to asteroïds

�Instrument parameters� Imagery: detection

and trajectory determination� Optical spectroscopy

R 300 - 500 � Adjustable integration time� Follow the object Itokawa (Hayabusa)


BATMAN concept:a MOEMS-based spectro-imager

Measured spectra

Field of view

TNG Micro-mirror array in the

telescope focal plane

CCD camera

Spectrograph arm

Imaging arm


Hub

ble

ultr

a de

ep fi

eld

(HU

DF

),

NA

SA

, 3/

9/20

04

Reflective surface

Telescope(ground or space)

Spectrometer

CCD Camera

Measured spectraTelescope’s field of view�� Thousands of galaxies

Overlapping Spectra

Multi-object spectroscopy


2D Micromirror array in the telescope focal plane

Telescope(ground or space)

CCD Camera

Spectrometer

Measured spectraTelescope’s field of view�� Thousands of galaxies

Hub

ble

ultr

a de

ep fi

eld

(HU

DF

),

NA

SA

, 3/

9/20

04

Multi-object spectroscopy


�Most popular MOEMS devices available�Micro-mirrors

�2048x1080 individually tiltable�13.68µm pixel pitch, �Tilt angle of 12°

� Numerous applications �Prime use displaying images �No customization possible

�Space qualification tests (ESA contract)� -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

Texas Instruments DMD

Zamkotsian et al., SPIE 6884, 2008


Parameters (BATMAN at TNG)

Field of view 6.8 arcmin x 3.6 arcmin

Focal ratio F/4 on DMD (scale = 0.2 arcsec per micromirror)

Beams on DMD incoming light at normal incidence out-coming light at 24°DMD orientation at 45°

Wavelength range 400 - 800 nm

Spectral resolution R = 560 for 1 arcsec object (typical slit size)

Two arms instrument one spectroscopic channelone imaging channel

Detectors Two 2k x 4k CCDs


Optical design


� Simulated spectra (400 – 800 nm)

Simulated spectra


�General design

BATMAN: the opto-mechanics

Zamkotsian et al.,

SPIE 9908, 2016


�General design



�General design



Detector

Instrument software

Mirrors / grating Fore-optics Hexapods Calibration unit

Mirrors mount

Detector

On-sky by end 2017


ROBIN


ROBIN: imagery

Pixels Camera

Pix

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1440

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z00 pattern2 z09 pattern2 z20 pattern1

z25 pattern1 z40 pattern1 z49 pattern2


ROBIN: slits

Pixels Camera

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era

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50

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Slit: 1 µM (13.68 µm)Spectrum on 1.5 detector pixel (8,3µm) in 450-650nm wavelength range

ROBIN: spectra


Pixels Camera

Pix

els

Cam

era

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50

100

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Pixels Camera

Pix

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Slit: 1 µM (13.68 µm)Spectrum on 1.5 detector pixel (8,3µm) in 450-650nm wavelength range

ROBIN: spectra


BATMAN: the simulator







BATMAN for TNG

Spectrograph Imager

MOEMS-DMD/MIRA

Pupil planeFocal plane

Focal plane

Telescope

FOV = 6.8 x 3.6 arcmin2

BATMAN for VLT

Spectrograph Imager

MOEMS-DMD/MIRA


Focal plane

VLT + visible MCAO

FOV = 1 x 1 arcmin2

BATMAN for VLT

Spectrograph Imager

MOEMS-DMD/MIRA


Focal plane

VLT + AOF

DM 2 / DM 3

FOV = 1 x 1 arcmin2

BATMAN for VLT

VLT + AOF

FOV = 12 x [1 x 1 arcmin2] or any combination in wa velength bands

Focal plane


BATMAN unique abilities

�Large FOV� Single large FOV� Segmented FOV

�SNR-limited observation� New observational mode� Optimize scientific return� Homogeneous samples, easier to reduce

�Versatility IN the FOV� MOS + IFU + Imagery� Photometric calibration quasi-simultaneous � Photometric selection / z selection with the imagery� Transients live detection and characterization

� Spatial and spectral resolution diversity in the FO V

Visible+ IR ?


Parameters BATMAN for VLT3: TBD

Field of view 1 x 1 arcmin2 ++ ?

Focal ratio F/4 on DMD (scale = 0.2 arcsec per micromirror)

Beams on DMD incoming light at normal incidence out-coming light at 24°DMD orientation at 45°

Wavelength range 400 - 800 nm + IR ?

Spectral resolution R = 500 – 1500 up to 5000 ?

Two arms instrument one spectroscopic channelone imaging channel

Detectors Two 2k x 4k CCDs


Frederic Zamkotsian, Romain Thomas, Julien Zoubian, Carlo Schimd, Sylvain de la Torre, Eric Jullo, Olivier Ilbert, Samuel Boissier, George s Comte, Jean-Claude Bouret,

Delphine Russeil, Audrey Delsanti, Pierre Vernazza, B enoit Neichel

+ BATMAN French-Italian team

1 Laboratoire d'Astrophysique de Marseille, France2 INAF Osservatorio Astronomico di Brera, Italy

3 INAF/IASF Bologna, Italy4 INAF - Telescopio Nazionale Galileo, Spain

5 INAF-OAT, Osservatorio Astronomico di Trieste, Italy

Visible MCAO supported spectro -imager: the BATMAN family


Extra-slide, MIRA : the European Micro-Mirror Array

Waldis et al., SPIE 6887, 2008

Canonica et al., JMM, 2013

Documents

Visible MCAO supported spectro-imager: the BATMAN …€¦ · + BATMAN French-Italian team 1 Laboratoire d'Astrophysique de Marseille, France 2 INAF Osservatorio Astronomico di Brera,