1. Dae-Sik Moon Department of Astronomy & Astrophysics University of Toronto Wide Field, High Resolution Integral-Field Near-Infrared Spectroscopy of Extended Objects

2. Most frequent question by Korean astronomers on me :

3. Most frequent question by Korean astronomers on me : “How is your research going?”

4. Most frequent question by Korean astronomers on me : “How is your research going?”  Not much interested in my research.

5. 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?”

6. 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.”

7. Three Key Elements of Spectrographs

8. Field of View

9. Three Key Elements of Spectrographs Field of View (Long Slit) Integral Field Multi-Object

10. Three Key Elements of Spectrographs Field of View (Long Slit) Integral Field Multi-Object Spectral Resolution

11. Three Key Elements of Spectrographs Field of View (Long Slit) Integral Field Multi-Object Spectral Resolution Immersion Double Pass Fringe Interference

12. Three Key Elements of Spectrographs Field of View (Long Slit) Integral Field Multi-Object Spectral Resolution Immersion Double Pass Fringe Interference Spectral Coverage

13. Three Key Elements of Spectrographs Field of View (Long Slit) Integral Field Multi-Object Spectral Resolution Immersion Double Pass Fringe Interference Spectral Coverage Cross Dispersion Multiple Gratings

14. 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

15. 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

16. (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.

17. 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.

18. 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)!

19. 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 

20. 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!)

21. 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.

22. Image slicer-based Integral-Field Spectrograph

23. 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

25. 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)

26. 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!”

27. 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)

28. 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

29. 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?)

30. 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

31. 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

32. 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.

33. 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)

34. Wide Integral Field Infrared Spectrograph

36. Huygens (not FFT) EED

37. Wide Integral Field Infrared Spectrograph

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

39. WIFIS Basics WIFIS Image Slicer

40. WIFIS Basics WIFIS Image Slicer

41. WIFIS Image Slicer: FISICA FISICA Internal Optical Path: Mirror Arrays + Flat Fold Mirrors FISICA Package

42. 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

43. 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

44. 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 N H map

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

46. FISICA: from NOAO to U.of.Toronto (2010 March) FISICA Dewar Just Photo, Not Food in Cold Dewar

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

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

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

50. 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(?)

51. 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

52. 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(?)

53. WIFIS Observations (Current Plan) Palomar 5-m Hale Telescope

54. WIFIS Observations (Current Plan) IRTF 3-m Telescope

55. WIFIS Observations (Current Plan) GTC 10.4-m Telescope in La Palma

56. 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

57. 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) ?

58. (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.

59. 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