The 3D-NTT
C. Balkowski
GEPI, Observatoire de Paris
Lijiang, november 2010
The 3D-NTT is a collaboration between LAM ( Marseille), GEPI (Paris) and LAE (Montréal)
• Constructing Team
P. Amram, P. Balard, C. Balkowski, O. Boissin, J. Boulesteix, C. Carignan, O. Daigle, M-M. de Denus, B. Epinat, J-L. Gach, O. Hernandez, F. Rigaud
• Private companies
SESO, Fogale, Cedrat, Immervision, Photon-etc, BMV Optical
• Science Team
P.Amram, A. Boselli, V. Buat, J-G Cuby (LAM) C. Carignan, O. Hernandez (LAE), C. Balkowski, M. Lehnert, S. Mei, T. van Driel (GEPI), J. Bland-Hawthorn (AAO), J. Cepa (IAC), R. Corradi (ING), R. Dettmar, D. Bomans (Bochum), P.A. Duc (CEA), G. Östlin (Stockholm), R. Rampazzo (Padova), L. Verdes Montenegro (Granada), W. Zeilinger (Wien)
1D 2D 3D … Spectroscopy
• 1D : I()
• 2D : I(,x)
• 3D : I(,x,y)
x
y
1D 2D 3D (3D½)
1940
1970
2020
1990
2050
1900
100 mor moon
25 m ?
8-10 m
5 m
2.5 m
1 m
date
s
dia
metr
of
téle
scop
es
Point source Spectroscopy(essentially stellar)
Long slit Spectroscopy(nebular and galactic)
Integral field Spectroscopy
Multi-objects Spectroscopy
Multi-objects & Multi-IF Spectroscopy
3D½
2D
1D
3D
Objective Prism Objective Prism then objective- grismthen objective- grism
3D
Some history about the Fabry-Perot interferometer
2 semi-reflecting plates of glass, parallel, producing an interference pattern
(Fabry and Perot, Marseille, 1892)
YX
Dynamics from 3D spectroscopy
Nearby galaxies:-HI, Halpha, CO- VLA, 4m - IFU, Fabry-Perot
Distant galaxies:-Ionized gas- VLT, IFU
FUTURE:- ELT- SKA
Velocity field
14/05/2009 - ThinkShop
SINS: 1.5<z<3
Genzel et al. 2006, 2008Forster-Schreiber et al.
2008BzK 15504, z=2.4
IMAGES: 0.4<z<0.8
Yang et al. 2008
J033249.53-274630.0, z=0.5
GHASP: local
Epinat et al. 2008M63, Local
galaxy
MASSIV: 1<z<1.8
Epinat et al. 2009
VVDS22001425, z=1.3
HST
Velocity Field
Hdistribution
WE NEED TO DISENTANGLE EVOLUTION EFFECTS FROM RESOLUTION EFFECTS ON KINEMATICAL DATA
USE OF A LOCAL KINEMATICAL REFERENCE SAMPLE
Z=2.4 Z=1.3 Z=0.5 Local
Epinat et al. 2008, 2009
Dw
arfs, Irre
gula
rs
Blu
e co
mp
act
Local reference sample GHASP (Gassendi H survey of SPirals)
Environment/Galaxy density
Early-type
Gaseous Disk
Intermediate
Barred & non-Barred Galaxies
HSB & LSB
Mass Luminosity
Field
Pairs
Compact Groups
Groups
Late-type
GHASP 203 nearby galaxies
-15<Mb<-22Sa to irregular
High quality 3D datacubes:• High spectral resolution ~10 km/s
• Seeing limited ~3''
Morphological Type
Observed at OHP
203 nearby galaxies
Simulation of high-z galaxies from GHASP data
• 153 GHASP galaxies projected at z=1.7• Lowest angular size: 8.5 kpc/"
• Seeing: 0.5"
• Pixel size: 0.125"
• No noise added
• How do galaxies form? • Are distant rotating disks well classified?
• What are the biases?
• Rotating disk misclassified
• Asymmetry in the H distribution
• Close pairs seen as RD?
Classification of the kinematics of distant galaxies
mapH VF
mapH VF
~70% of regular GHASP rotating disks are classified correctly
Results • Comparison of high-z data with projected local data
Possible to disentangle distance effect from evolutionary effects
70% of the high redshift rotating disks well classified
High-z disks show higher velocity dispersion than local galaxies
Sign of dynamical evolution with z
Need to check the spectral resolution effects on the data (R=15000-> R=3000)
3D-NTT
On the sky at the ESO NTT in 2012 as a visitor instrument
Collaboration between LAM (Marseille), GEPI (PARIS) and LAE (Montréal)
PI M. Marcelin
Design of the 3D-NTT
NTT derotator
The 3D-NTT is a visitor instrument to be put at the Nasmyth focus of the NTT
Optics
designed and made at LAE Montréal)
Mechanics
- Most made at GEPI (Pôle Instrumental)
- Some parts (e.g. filter wheels) made at LAE workshop
- Supports of CCD and cryostats made at LAM workshop
- Main structure made by a private company
The detectors
• L3CCD for high resolution mode (O. Daigle, LAE)
Chip purchased. Controler being made.
• 4k x 4k blue sensitive CCD for low resolution mode (J-L. Gach, LAM)
Chip purchased
The Fabry-Perot interferometers
Mechanics made at GEPI
Two sets of plates made by SESOPiezo-actuators and positioning capacitors purchased
Double Fabry-Perot Integral Field Spectrometer
• Same device – Tunable Filter – Scanning Fabry-Perot
• Develop our own coatings
• Develop our own controller to replace the CS100-type controller
What is new with our Tunable Filter ?• Long excursion piezo-actuators (200 µm) • Cover of a wide range of interference orders
Coating and controler of the interferometers
• Coating characteristics computed
Deposits in progress
• Controler developed at LAM
Tunable Source for the calibration
Manufactured by Photon-etc it will provide an absolute wavelength calibration
Narrow line tunable over a wide spectral range
(0.4 nm over 400 to 1000 nm or 0.1 nm over 600 to 1000 nm).
The two modes of the 3D-NTT
TUNABLE FILTER MODE (R ~ 500 à 1000) monochromatic images
Field of view ~ 17' x 17’ Wavelength range 350nm to 850nm Spectral resolution : tunable from 300 to 6 000 (@H) Detector CCD (4096 x 4096 with 12 µm pixels) scale: ~ 0.25"/pixel
HIGH RESOLUTION MODE (R ~ 10 000 à 20 000)Velocity fields
Field of view ~ 8.5' x 8.5' Wavelength range 350nm to 850nm Spectral resolution : from 10 000 to 40 000 (@ H) Detector : L3CCD (1600 x 1600 with 16µm pixels) scale: ~ 0.33"/pix
What is the principle of the Tunable Filter ?
It is a Fabry-Perot interferometer in which the plates are so close to one another (a few microns) that you do not see anymore interference rings through it when looking at a monochromatic source but a spot (Jacquinot spot)
Changing the spacing between the plates then enables to tune the transmitted wavelength, it can be used as a filter for the Fabry Perot at HR
High resolution mode observations
Low resolution mode
observations
Example of images produced by a Tunable Filter
NGC1365 observed with the TTF on the AAT for measuring abundances from line-ratios
(Veilleux et al. 2003)
H
[NII] / H [NII]
Red continuum
Two large programmes
• Characterizing the interstellar medium of nearby galaxies with 2D maps of extinction and abundances
• Gas Accretion & Radiative Feedback in the Early Universe
Large Programme « Galaxies »
Observation of the ionized gas in SINGS galaxies with the Tunable Filter to map :
• star formation
• dust extinction and metal abundance (from line ratios maps)
• observed lines : [OII] 372.7 nm
H beta 486.1 nm
[OIII] 495.9 - 500.7 nm
[NII] 654.8 - 658.4 nm
H alpha 656.3 nm
Goal :
- Understand the nature, origin and evolution of these galaxies, comparing the 3DNTT maps with maps obtained in FIR (MIPS/Spitzer) and UV (Galex) for a detailed analysis of extinction and its relation with other physical quantities such as metal abundance.
- Reference sample for studies at larger redshift.
Large Programme « QSOs »Observation of 30 quasars at z ~2 in the Lyman alpha line (redshifted at 380 to 400 nm for z ~ 2.2 to 2.3) with the Tunable Filter, with 5 deep images for each target (one at the quasar redshift, two blueshifted and two redshifted).
Goal :
The aim is to detect galaxies with a high stellar formation rate around quasars, in order to check if quasars with a high UV luminosity suppress the stellar formation around them as suggested by recent observations with the TTF on the AAT (Barr et al. 2004 et Francis & Bland-Hawthorn 2005).
If such an observation is confirmed, it will put strong constraints on the cosmological models.
Other possible programmes
• A Search for Planetary Nebulae around nearby elliptical galaxies. Tracing the large scale velocity field of galaxies
• Ionized Gas in Star-forming and luminous infrared galaxies
• The origin and fate of faint ionized gas in the halos of irregular dwarf galaxies
• On the lifetime of grand design spiral patterns
• The Mystery of the Interacting Galaxy Pair NGC 4410a/b
• Ionization Cones: Probing the Accretion Mode of Obscured Active Galactic Nuclei
• Tracing the eventful life of galaxies in low density environments
• The origin of asymmetries in isolated galaxies
• Integration of the raw data files (different cycles) into an interferogram data cube
• Phase correction to create wavelength sorted data cubes
• Hanning spectral smoothing• Sky emission removal• Spatial binning/smoothing (adaptive smoothing)• Radial velocity maps extraction• Addition of the astrometric information (WCS)• Kinematical information extraction (RCs)
FP data reduction pipeline
Get the data available quickly
common database (LAM, LAE, GEPI)
FP data reduction
Near future
3D-NTT
- Observations of more nearby samples (Barred, Compact Groups, Mergers, Blue Compact Galaxies, LIRG, LSB, …)
- Comparison with high redshift galaxies
• FP database www.fabryperot.oamp.fr
Double Fabry-Perot Integral Field Spectrometer
Comparison with other TF instrumentsMerit factor X = ΩNA where A =telescope area, Ω= instrument solid angle, N = number of nights per year
• The Taurus Tunable Filter (TTF; 370-950nm) operated during the years 1996-2000 at the WHT and 1996-2003 at the AAT. X = 50(3.9x3.9)(9x9) = 65,000.
• The Maryland Magellan Tunable Filter on Magellan (MMTF; 470-900nm) had First Light in Dec 2006. X = 7(6.5x6.5)(27x27) = 220,000.
• The Osiris Tunable Filter on Grantecan (OTF; 430-970nm) is due to see First Light in June 2008. X = 100(10x10)(6.7x6.7) = 450,000.
• The PFIS on SALT (430-860nm) will have a merit function of X = 10 ? (11x11)(8’x8’)= 77 000
• The 3D-NTT (370-900nm) would have a merit function of X = 50(3.5x3.5)(17x17)= 175,000.
The 3DNTT would be a powerful TF survey facility once commissioned.
BTFi Brazilian Tunable Filter
• Field of View (assuming EMCCD – 16002 ; 16m pixel)– GLAO-fed - FoV ~3’ ; Spatial sampling ~0.12”
(f/6.7 camera)– SL-fed - FoV ~6’ ; Spatial sampling
~0.24” (f/3.3 camera)• Spectral Resolution:
– iBTF: 5 < R < 5,500– FP: 250 < R < 40,000
• LAE to provide: EMCCD controllers (CCCP)
• LAM to provide: FP controller + etalon ?
3D spectroscopy : an essential tool for 4m, VLT, ELTs and
LST
VLT Keck Gemini GTCVLT Keck Gemini GTC
E-ELT TMT JWST E-ELT TMT JWST
FORS 1FORS 1FOcal Reducer low resolution SpectrographFOV 6.8'x6.8'movable slitsλ 0.33 - 1.1 µ100<R<1500
FORS 2FORS 2FOV 6.8'x6.8'movable slitsmulti-objects masksλ 0.33 - 1.1 µ100<R<1500
FLAMESFLAMESFiber Large Array Multi Element Spectrograph
FLAMES/UVESFLAMES/UVES8 objectsλ 0.37 - 0.9 µR=47000
FLAMES/GIRAFFEFLAMES/GIRAFFE130 objectsλ 0.37 - 0.9 µR=20000
VIMOSVIMOSVisible Imaging Multi Object SpectrographFOV 54"x54" (IFU) or4 x 7' x 8' discontinuous80x80 fibersλ 0.37 - 1 µ180<R<5000
SINFONISINFONISPectrograph for Infrared Faint Field ImagingFOV 0.8" to 8"image slicerλ 1.05 - 2.45 µR=4000
VISIRVISIRSPectrograph for Infrared Faint Field ImagingFOV up to 51"x51"slitlessλ 8-13 ; 18-24 µR=25000
VLT
GMOS NGMOS NGemini Multi Object SpectrographFOV 5.5'x5.5' discontinuous35 arcsec suare for IFUλ 0.36 - 1.1 µ670<R<4400
GMOS SGMOS SGemini Multi Object SpectrographFOV 5.5'x5.5' discontinuous35 arcsec suare for IFUλ 0.36 - 1.1 µ670<R<4400
NIFS NNIFS NNear Infrared Integral Field Spectrograph3"x3" IFUλ 1 - 2.5 µR=5000
GNIRSGNIRSNear Infrared Integral Field SpectrographIFUλ 1.5 - 5 µR=800-18000
Gemini
CIRPASSCIRPASSNear Infrared Integral Field SpectrographFOV 13"x4.7" IFUλ 0.9 - 1.8 µR=3000en construction
North South
LRISLRISLow Resolution Imaging SpectrographFOV 4'x8' discontinuousslit masks 30 objectsλ 0.39 - 1.05 µ300<R<5000
NIRSPECNIRSPECNear InfraRed SPECtrometerFOV 46"x46"λ 0.96 - 5.5 µ2000<R<25000
DEIMOSDEIMOSDeep Extragalactic Imaging Multi Object SpectrographFOV 16'x16' discontinuousslit masks 130 objectsλ 0.41 - 1.1 µ200<R<5000
Keck
OSIRISOSIRISOH Suppression Infra Red Imaging SpectrographFOV 6.4"x1.6" OA1000 continuous spectraλ 1 - 2.5 µR=3800AO corrected
JWST
NIRSPECNIRSPECNear InfraRed SPECtrograph100 objects within a 3'x3' FOV MEMS (shutter masks)λ 0.6 - 5 µ100<R<1000ESA : spectrographNASA : InSb or HgCdRe detectors
MIRIMIRIMid InfraRed InstrumentFOV 2'x2'λ 5 - 28 µR=1500JPL
NIRCAMNIRCAMNear InfraRed CAMeraFOV 2.3'x2.3' slitlesstunable filter λ 0.6 - 5 µR=100Univerity Arizona
FGS-TFI FGS-TFI Find Guider Sensor – Tunable Filter ImagerFOV 2'x2'λ 1.5 - 5 µPI: R. Doyon (LAE) 2048x2048 HgCdTe array
CSA - Canada
Conclusion
• 3D spectroscopy is an unique tool for many fields in astronomy
• Any telescope should be equipped with 3D spectrometer
• 3D-NTT should be available in about one year