Transcript Wide-field and High-resolution Integral

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:
Most frequent question by Korean
astronomers on me:
“How is your research going?”
Most frequent question by Korean
astronomers on me:
“How is your research going?”
 Not much interested in my research.
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?”
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.”
Three Key Elements of Spectrographs
Three Key Elements of Spectrographs
Field of View
Three Key Elements of Spectrographs
Field of View
(Long Slit)
Integral Field
Multi-Object
Three Key Elements of Spectrographs
Field of View
Spectral
Resolution
(Long Slit)
Integral Field
Multi-Object
Three Key Elements of Spectrographs
Field of View
Spectral
Resolution
(Long Slit)
Integral Field
Multi-Object
Immersion
Double Pass
Fringe Interference
Three Key Elements of Spectrographs
Field of View
Spectral
Resolution
(Long Slit)
Integral Field
Multi-Object
Immersion
Double Pass
Fringe Interference
Spectral
Coverage
Three Key Elements of Spectrographs
Field of View
Spectral
Resolution
(Long Slit)
Integral Field
Multi-Object
Immersion
Double Pass
Fringe Interference
Spectral
Coverage
Cross Dispersion
Multiple Gratings
Three Key Elements of Spectrographs
Field of View
Spectral
Resolution
Spectral
Coverage
They are incompatible and competing!
It’s very difficult to satisfy all together.
Three Key Elements of Spectrographs
Field of View
I Want Them All
Spectral
Resolution
Spectral
Coverage
They are incompatible and competing!
It’s very difficult to satisfy all together.
(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);
 10,000 (high resolutions) is (near) reality and is
booming , especially immersion gratings (~10 SPIE
papers in 2010 July; e.g., IGRINS);
R
 Usually
J, H, K separately;
 Cross-dispersion (=
coverage.
multi-order) for broad spectral
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
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!)
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.
Image slicer-based Integral-Field Spectrograph
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.
Image slicer-based Integral-Field Spectrograph
Current Integral-Field Spectrographs
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Current Integral-Field Spectrographs
According to David Lambert’s
definition yesterday, they are
bunch of overly complicated
(VLT)
“photometers!”
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Current Integral-Field Spectrographs
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Current Integral-Field Spectrographs
Empty
parameter
space
Wider, higher
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Current Integral-Field Spectrographs
(2012?)
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
Current Integral-Field Spectrographs
Wide Integral Field
Infrared Spectrograph
(2012?)
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
FoVs:
 15  30 on
4-m telescope;
 6  12 on 10-m telescope
Wide Integral Field Infrared Spectrograph
~ 1.5 m
Grating
Turret
Optical Layout
FISICA
Integral
Field
Unit
Spectrograph
Camera
Offner
Relay
Collimator
System
~1m
Detector
WIFIS Optical Design by R. Chou (UofT graduate student)
Wide Integral Field Infrared Spectrograph
~ 1.5 m
Grating
Turret
Optical Layout
FISICA
Integral
Field
Unit
Spectrograph
Camera
Offner
Relay
Optical Components:
● Offner Relay;
● FISICA Integral Field Unit;
● Collimator System;
● Gratings (J, H, K);
● Spectrograph Camera.
~1m
Collimator
System
Detector
WIFIS Optical Design by R. Chou (UofT graduate student)
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)
Wide Integral Field Infrared Spectrograph
Wide Integral Field Infrared Spectrograph
Wide Integral Field Infrared Spectrograph
Huygens (not FFT) EED
Wide Integral Field Infrared Spectrograph
WIFIS Image Slicer
FISICA: Florida Image Slicer for
Infrared Cosmology and Astrophysics
(From University of Florida)
WIFIS Image Slicer
WIFIS
Basics
WIFIS Image Slicer
WIFIS
Basics
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).
Clump 3
Radio continuum contours
Line integrated FISICA maps of [Fe II] 1.644
micron transition
(Lee, Moon, Rahman, Koo et al. in preparation)
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 G11.2-0.3
FISICA + 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: from NOAO to U.of.Toronto (2010 March)
Just Photo,
Not Food in Cold Dewar
FISICA Dewar
FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
FISICA: from NOAO to U.of.Toronto (2010 March)
FISICA Dewar
FISICA: from NOAO to U.of.Toronto (2010 March)
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
Extended, X-ray photo-ionized (and shocked) nebulae
Keck LRIS (7-h) spectrum of ULX Ho IX X-1 (Moon & Harrison 2010)
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
WIFIS Observations (Current Plan)
IRTF 3-m
Telescope
WIFIS Observations (Current Plan)
GTC 10.4-m
Telescope in La Palma
Current & Future Integral-Field Spectrographs
(2012?)
Future
(VLT)
(Palomar)
(Keck))
NIFS
(VLT)
Integral-field Infrared Spectrographs on Large Telescopes
Most of them are medium resolution, narrow integral-field spectrographs.
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, highresolution 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);
 10,000 (high resolutions) is (near) reality and is
booming , especially emersion gratings (~10 SPIE
papers in 2010 July);
R
 Usually
J, H, K separately;
 Cross-dispersion (=
coverage.
multi-order) for broad spectral
Currently available integral-field
spectrographs are narrow-field, low-resolution
integral-field spectrographs
Two key words for near-future
integral-field, near-infrared
spectrgraphs:
“Wide” & “High Resolution”