wide field, high resolution integral-field near-infrared spectroscopy of extended objects
DESCRIPTION
Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects. Dae-Sik Moon Department of Astronomy & Astrophysics University of Toronto. Most frequent question by Korean astronomers on me :. - PowerPoint PPT PresentationTRANSCRIPT
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Dae-Sik MoonDepartment of Astronomy & AstrophysicsUniversity of Toronto
Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects
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Most frequent question by Korean astronomers on me:
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Most frequent question by Korean astronomers on me:
“How is your research going?”
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Most frequent question by Korean astronomers on me:
“How is your research going?” Not much interested in my research.
![Page 5: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/5.jpg)
Most frequent question by Korean astronomers on me:
“How is your research going?” Not much interested in my research.
“Have you seen Yu Na Kim in Toronto?”
![Page 6: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/6.jpg)
Most frequent question by Korean astronomers on me:
“How is your research going?” Not much interested in my research.
“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.”
![Page 7: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/7.jpg)
Three Key Elements of Spectrographs
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Three Key Elements of Spectrographs
Field of View
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Three Key Elements of Spectrographs
Field of View(Long Slit)Integral FieldMulti-Object
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Three Key Elements of Spectrographs
Field of View(Long Slit)Integral FieldMulti-Object
Spectral Resolution
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Three Key Elements of Spectrographs
Field of View(Long Slit)Integral FieldMulti-Object
Spectral Resolution
ImmersionDouble PassFringe Interference
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Three Key Elements of Spectrographs
Field of View(Long Slit)Integral FieldMulti-Object
Spectral Resolution
ImmersionDouble PassFringe Interference
Spectral Coverage
![Page 13: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/13.jpg)
Three Key Elements of Spectrographs
Field of View(Long Slit)Integral FieldMulti-Object
Spectral Resolution
ImmersionDouble PassFringe Interference
Spectral Coverage
Cross DispersionMultiple Gratings
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Three Key Elements of Spectrographs
Field of View
Spectral Coverage
They are incompatible and competing!It’s very difficult to satisfy all together.
Spectral Resolution
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I Want Them All
Three Key Elements of Spectrographs
Field of View
Spectral Coverage
They are incompatible and competing!It’s very difficult to satisfy all together.
Spectral Resolution
![Page 16: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/16.jpg)
(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.
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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.
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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)!
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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
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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!)
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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!)
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.
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Image slicer-based Integral-Field Spectrograph
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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.
Image slicer-based Integral-Field Spectrograph
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Image slicer-based Integral-Field Spectrograph
![Page 25: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/25.jpg)
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)
![Page 26: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/26.jpg)
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)
According to David Lambert’s definition yesterday, they are bunch of overly complicated “photometers!”
![Page 27: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/27.jpg)
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)
![Page 28: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/28.jpg)
Current Integral-Field Spectrographs
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Empty parameter space
(VLT)
(Palomar) (Keck)) NIFS(VLT)
Wider, higher
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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)
(2012?)
![Page 30: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/30.jpg)
Current Integral-Field Spectrographs
(VLT)
(Palomar) (Keck)) NIFS(VLT)
(2012?)
Wide Integral Field Infrared Spectrograph
FoVs: 15 30 on 4-m telescope; 6 12 on 10-m telescope
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Wide Integral Field Infrared Spectrograph
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
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Wide Integral Field Infrared Spectrograph
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.
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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)
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Wide Integral Field Infrared Spectrograph
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Wide Integral Field Infrared Spectrograph
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Wide Integral Field Infrared Spectrograph
Huygens (not FFT) EED
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Wide Integral Field Infrared Spectrograph
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WIFIS Image Slicer
FISICA: Florida Image Slicer for Infrared Cosmology and Astrophysics (From University of Florida)
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WIFIS BasicsWIFIS Image Slicer
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WIFIS BasicsWIFIS Image Slicer
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WIFIS Image Slicer: FISICA
FISICA Internal Optical Path:Mirror Arrays + Flat Fold Mirrors
FISICA Package
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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
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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
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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
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FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
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FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
Just Photo,Not Food in Cold Dewar
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FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
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FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
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FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Assembly
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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(?)
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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
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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(?)
![Page 53: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/53.jpg)
WIFIS Observations (Current Plan)
Palomar 5-m Hale Telescope
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WIFIS Observations (Current Plan)
IRTF 3-m Telescope
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WIFIS Observations (Current Plan)
GTC 10.4-m Telescope in La Palma
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Current & Future 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)
(2012?)Future
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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)?
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(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.
![Page 59: Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects](https://reader035.vdocument.in/reader035/viewer/2022062502/56814c80550346895db99c9d/html5/thumbnails/59.jpg)
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