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

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

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 Three Key Elements of Spectrographs

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

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

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

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

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

14. Spectral Coverage Spectral Resolution Field of View Three Key Elements of Spectrographs They are incompatible and competing! It’s very difficult to satisfy all together.

15. Spectral Coverage Spectral Resolution Field of View I Want Them All Three Key Elements of Spectrographs They are incompatible and competing! It’s very difficult to satisfy all together.

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-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.

24. Image slicer-based Integral-Field Spectrograph

25. Current Integral-Field Spectrographs (VLT) (Palomar) NIFS (VLT) (Keck)) Integral-field Infrared Spectrographs on Large Telescopes Most of them are medium resolution, narrow integral-field spectrographs.

26. Current Integral-Field Spectrographs According to David Lambert’s definition yesterday, they are bunch of overly complicated “photometers!” (VLT) (Palomar) NIFS (VLT) (Keck)) Integral-field Infrared Spectrographs on Large Telescopes Most of them are medium resolution, narrow integral-field spectrographs.

27. Current Integral-Field Spectrographs (VLT) (Palomar) NIFS (VLT) (Keck)) Integral-field Infrared Spectrographs on Large Telescopes Most of them are medium resolution, narrow integral-field spectrographs.

28. Current Integral-Field Spectrographs Empty parameter space Wider, higher (VLT) (Palomar) NIFS (VLT) (Keck)) Integral-field Infrared Spectrographs on Large Telescopes Most of them are medium resolution, narrow integral-field spectrographs.

29. Current Integral-Field Spectrographs (2012?) (VLT) (Palomar) NIFS (VLT) (Keck)) Integral-field Infrared Spectrographs on Large Telescopes Most of them are medium resolution, narrow integral-field spectrographs.

30. Current Integral-Field Spectrographs Wide Integral Field Infrared Spectrograph FoVs:  15  30 on 4-m telescope;  6 12 on 10-m telescope (2012?) (VLT) (Palomar) NIFS (VLT) (Keck))

31. Wide Integral Field Infrared Spectrograph ~ 1.5 m Optical Layout Grating Turret FISICA Integral Field Unit Spectrograph Camera Offner Relay Collimator System Detector ~ 1 m WIFIS Optical Design by R. Chou (UofT graduate student)

32. Wide Integral Field Infrared Spectrograph ~ 1.5 m Optical Layout Grating Turret FISICA Integral Field Unit Spectrograph Camera Offner Relay Optical Components: ● Offner Relay; ● FISICA Integral Field Unit; ● Collimator System; ● Gratings (J, H, K); ● Spectrograph Camera. Collimator System Detector ~ 1 m WIFIS Optical Design by R. Chou (UofT graduate student)

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

35. Wide Integral Field Infrared Spectrograph

36. Wide Integral Field Infrared Spectrograph 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 Image Slicer WIFIS Basics

40. WIFIS Image Slicer WIFIS Basics

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). Clump 3 Radio continuum contours Line integrated FISICA maps of [Fe II] 1.644 micron transition (Lee, Moon, Rahman, Koo et al. in preparation)

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 Av map FISICA + Flamingos J+H Grating: FoV: 15  30, R  1000 NH map

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

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