the 3d-ntt c. balkowski gepi, observatoire de paris lijiang, november 2010

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