Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects

Dae-Sik MoonDepartment of Astronomy & AstrophysicsUniversity of Toronto

Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects

Most frequent question by Korean astronomers on me:


“How is your research going?”


“How is your research going?” Not much interested in my research.



“Have you seen Yu Na Kim in Toronto?”

http://en.wikipedia.org/wiki/File:Yunakimedal2.jpg



“Have you seen Yu Na Kim in Toronto?” For the record: “No, I’ve not seen her in Toronto/Canada. I’ve seen her at other places.”

http://en.wikipedia.org/wiki/File:Yunakimedal2.jpg

Three Key Elements of Spectrographs


Field of View


Field of View(Long Slit)Integral FieldMulti-Object



Spectral Resolution



Spectral Resolution

ImmersionDouble PassFringe Interference



Spectral Resolution


Spectral Coverage



Spectral Resolution


Spectral Coverage

Cross DispersionMultiple Gratings


Field of View

Spectral Coverage

They are incompatible and competing!It’s very difficult to satisfy all together.

Spectral Resolution

I Want Them All


Field of View

Spectral Coverage

They are incompatible and competing!It’s very difficult to satisfy all together.

Spectral Resolution

(General) Current Near-Infrared Spectrographs of Large Telescopes Integral-field spectroscopy is (almost) standard; Multi-object spectroscopy is becoming a reality (MOSFIRE, FLAMINGOS-2, KMOS); Most cases R 5,000 (medium or low resolutions); R 10,000 (high resolutions) is (near) reality and is booming , especially immersion gratings (~10 SPIE papers in 2010 July; e.g., IGRINS); Usually J, H, K separately; Cross-dispersion (= multi-order) for broad spectral coverage.

Typtical Case: Spectral Resolution, Coverage, and Field of View● 0.5 seeing = slit width ( resolution element);● Nyquist sampling: 2 detector pixels per resolution element;● Single band spectral coverage: 0.3 micron of H band;● 2K 2K detector array; 18 micron pitch;● 10-m, f/15 telescope.

Typtical Case: Spectral Resolution, Coverage, and Field of View● 0.5 seeing = slit width ( resolution element);● Nyquist sampling: 2 detector pixels per resolution element;● Single band spectral coverage: 0.3 micron of H band;● 2K 2K detector array; 18 micron pitch;● 10-m, f/15 telescope.

= 0.3/1024, spectral coverage per resolution element; R = / 5600, maximum spectral resolving power for a single band with linear dispersion; FoV = 0.5 (0.5 1024) = 0.5 8.5 f/#cam (projected slit / slit) f/15 2, very fast! Extremely difficult (although possible)!

Typtical Case: Spectral Resolution, Coverage, and Field of View● For integral field spectroscopy, slit width can be smaller than the seeing ( no loss of the light)● Slit width: 0.5 0.3


FoV = 0.3 5.1 6 12 integral field on 10-m telescope; f/#cam 3, challenging, but benign system (it’s not a cancer!)


FoV = 0.3 5.1 6 12 integral field on 10-m telescope; f/#cam 3, challenging, but benign system (it’s not a cancer!)

Designing a spectrograph camera of R 5000 and an integral field of 6 12 for an integral-field spectrograph of a 10-m telescope covering a single broadband can be a good PhD project for a challenging/ambitious graduate student.

Image slicer-based Integral-Field Spectrograph

Image Slicer:

The input image is formed at a segmented in thin horizontal sections which are then sent in slightly different directions; Usually three mirror arrays to form a pseudo long slit: slicer array (tilted spherical mirrors forming pupil images of each slicer) + pupil array (or capture mirrors, recombines the separate beams into the desired linear image) + field array (forms a common virtual pupil, its aperture serves as the entrance slit to the spectrograph). Contiguous sampling of the sky while retaining spatial information. Challenging optical design, fabrication, and implementation.



Current Integral-Field Spectrographs

Integral-field Infrared Spectrographs on Large Telescopes

Most of them are medium resolution, narrow integral-field spectrographs.

(VLT)

(Palomar) (Keck)) NIFS(VLT)




(VLT)


According to David Lambert’s definition yesterday, they are bunch of overly complicated “photometers!”




(VLT)





Empty parameter space

(VLT)


Wider, higher




(VLT)


(2012?)


(VLT)


(2012?)

Wide Integral Field Infrared Spectrograph

FoVs: 15 30 on 4-m telescope; 6 12 on 10-m telescope


WIFIS Optical Design by R. Chou (UofT graduate student)

Optical Layout

Offner Relay

FISICA Integral Field Unit

Collimator System

Grating Turret

Spectrograph Camera

Detector

~ 1.5 m

~ 1 m


WIFIS Optical Design by R. Chou (UofT graduate student)

Optical Layout

Offner Relay

FISICA Integral Field Unit

Collimator System

Grating Turret

Spectrograph Camera

Detector

~ 1.5 m

~ 1 m

Optical Components:● Offner Relay;● FISICA Integral Field Unit;● Collimator System;● Gratings (J, H, K);● Spectrograph Camera.

Wide Integral Field Infrared Spectrograph● R 5000, 6 12 on 10-m (= 15 30 on 4-m) IFS; ● Offner Relay 3 spherical mirrors, cold stop and filter wheel location;● FISICA Integral Field Unit Image slicer (see next slides); ● Collimator System Off-axis parabola + 2 aspherical lenses;● Gratings (J, H, K) Grating turret; m = 1 mechanical gratings (from Richardson Gratings);● Spectrograph Camera 6 lenses (CaF2 + SFTM16; chromatic pair), one aspherical doublet, 15-cm diameter, ~f/3;● Detector Hawaii II RG 2K 2K array, active focusing mechanism (including tip-tilt); ● Pupil imaging system(?) For alignment;● Univ. Toronto + Univ. Florida + KASI (+ Caltech).● PI, Visiting Instrument (D.-S. Moon)




Huygens (not FFT) EED


WIFIS Image Slicer

FISICA: Florida Image Slicer for Infrared Cosmology and Astrophysics (From University of Florida)

WIFIS BasicsWIFIS Image Slicer

WIFIS BasicsWIFIS Image Slicer

WIFIS Image Slicer: FISICA

FISICA Internal Optical Path:Mirror Arrays + Flat Fold Mirrors

FISICA Package

FISICA test observations with FLAMINGOS spectrograph on the KPNO 4 m of SNR G11.2-0.3

[Fe II] 1.644 micron emission of the young core-collapse supernova remnant G11.2-0.3 obtained with WIRC imaging camera on Palomar 5-m telescope (Koo et al. 2007; Moon et al. 2009).

Radio continuum contours

Line integrated FISICA maps of [Fe II] 1.644 micron transition (Lee, Moon, Rahman, Koo et al. in preparation)

Clump 3

FISICA test observations with FLAMINGOS spectrograph on the KPNO 4 m of SNR G11.2-0.3

FISICA + Flamingos J+H Grating:FoV: 15 30, R 1000

> 10 [Fe II] lines

FISICA test observations with FLAMINGOS spectrograph on the KPNO 4 m of SNR G11.2-0.3FISICA + Flamingos J+H Grating:FoV: 15 30, R 1000

Av map

NH map

FISICA: from NOAO to U.of.Toronto (2010 March)

FISICA Dewar


FISICA Dewar

Just Photo,Not Food in Cold Dewar


FISICA Dewar


FISICA Dewar


FISICA Assembly

WIFIS Sciences and Schedule

● Dynamics and Chemistry of “Something 2-D Extended” Supernova Remnants, Star-Forming Regions, Galaxies, etc.

● Supernova Ejecta and Circumstellar Knots (e.g., G11.2-0.3);

● Extended Nebulae around Ultra-luminous X-ray Sources;

● Wet Merging Galaxies at Z 1;

● Circumnuclear Regions of Nearby Galaxies;

● And more ....

● Unofficial personal review in 2010 October at Toronto by Keith Matthews (Caltech) & James Graham (Berkeley Toronto);

● Dewar Design in 2011 Summer;

● Assembly and First Observations in late 2012(?)

WIFIS Sciences: Ultra-luminous X-ray Sources

Keck LRIS (7-h) spectrum of ULX Ho IX X-1 (Moon & Harrison 2010)

Extended, X-ray photo-ionized (and shocked) nebulae

WIFIS Sciences and Schedule

● Dynamics and Chemistry of “Something 2-D Extended” Supernova Remnants, Star-Forming Regions, Galaxies, etc.

● Supernova Ejecta and Circumstellar Knots (e.g., G11.2-0.3);

● Extended Nebulae around Ultra-luminous X-ray Sources;

● Wet Merging Galaxies at Z 1;

● Circumnuclear Regions of Nearby Galaxies;

● And more ....

● Unofficial personal review in 2010 October at Toronto by Keith Matthews (Caltech) & James Graham (Berkeley Toronto);

● Dewar Design in 2011 Summer;

● Assembly and First Observations in late 2012(?)

WIFIS Observations (Current Plan)

Palomar 5-m Hale Telescope


IRTF 3-m Telescope


GTC 10.4-m Telescope in La Palma

Current & Future Integral-Field Spectrographs



(VLT)


(2012?)Future

Wide-field ( 10 5 on 10-m Telescope), medium-resolution (R 5000) integral-field spectrograph (IFS) in the near future

How about medium-field, high-resolution IFS with a single 2K 2K array, or wide-field, high-resolution IFS with a 4K 4K array (e.g., Immersion grating + Wide Image Slicer + Fast Spectrograph Camera)?

(General) Current Near-Infrared Spectrographs of Large Telescopes Integral-field spectroscopy is (almost) standard; Multi-object spectroscopy is becoming a reality (MOSFIRE, FLAMINGOS-2, KMOS); Most cases R 5,000 (medium or low resolutions); R 10,000 (high resolutions) is (near) reality and is booming , especially emersion gratings (~10 SPIE papers in 2010 July); Usually J, H, K separately; Cross-dispersion (= multi-order) for broad spectral coverage.

Two key words for near-future integral-field, near-infrared spectrgraphs:

“Wide” & “High Resolution”

Currently available integral-field spectrographs are narrow-field, low-resolution integral-field spectrographs

Documents

Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects