List of Figures

1. Schematic drawing of a slit spectrograph with a reflection grating.
2. Schematic showing angles of incident angle $\alpha$, diffraction angle $\beta$, and out-of-plane angle $\gamma$.
3. An echellogram of IRCS. The image is a $L$-band frame.
4. Variation of inclination and curvature with the out-of-plane angle of a cross-disperser.
5. Tilt and curvature of a slit image.
6. Variation of the tilt angle of slit images with diffraction angle for the R2.00 (blaze angle = 63$.^{\circ }$5) echelle grating.
7. Effective groove widths with incident and diffraction angles.
8. The effective blaze functions and locations of the interference mazima when (a) $\theta =$ 0 degrees and (b) $\theta =$4 degrees for m $=$ 30 with R2.00 echelle grating . The thin solid lines indicate effective blaze function considered the shadowing effect, which is represented by Eq. 33. The dotted lines indicate blaze functions without shadowing effect. The thick solid vertical lines indicate the interference pattern.The dashed lines indicate the angles when $\alpha = \beta$.
9. Variation of the blaze peak efficiency with $\theta$ ($=$ $\alpha$ $-$ $\theta _{B}$) for an R2.00 echelle.
10. Variation of the blaze peak efficiency with $\theta$ ($=$ $\alpha$ $-$ $\theta _{B}$) for an R2.75 echelle. $\bar{m} = {m}$.
11. $I_m/I_0$ for an R2.00 echelle.
12. $I_m/I_0$ for an R2.75 echelle
13. Variation of the blaze peak efficiency with out-of-plane angle $\gamma$ for an R2.00 echelle.
14. Variation of the blaze efficiency with out-of-plane angle $\gamma$ for an R2.75 echelle.
15. Variation of the blaze peak efficiency with order number for an R2.00 echelle.
16. Variation of the blaze peak efficiency with order number for an R2.75 echelle.
17. Locations of Wood's anomallies for an R2.00 echelle. Arrows indicate their positions.
18. Locations of Wood's anomallies for an R2.75 echelle. Arrows indicate their positions.
19. Layout of (a) the fore-optics and camera sections and (b) the spectrograph section (Tokunaga et al., 1998).
20. Variation of the blaze efficiency with the difference between the incident and blaze angles, $\alpha - {\theta }_{B}$, or the deviant angle from the Littrow Configuration. The solid line is for the echelle grating ( $\theta _{B} =$ 63$.^{\circ }$5) and the dashed line is for the cross-disperser grating ( $\theta _{B} =$ 8$.^{\circ }$016) of IRCS. The dotted and dashed-dotted lines indicate the initial reference angle between the incident and blaze angles for the echelle grating, 4$^\circ$, and for the cross-disperser, 15$.^{\circ }$984, respectively.
21. Echelle simulator example for IRCS. An $H-$band spectral frame of the L1551 IRS 5 jet and OH lines, [Fe II] lines, and atomic hydrogen lines on it.
22. Response functions of apertures in Figure 22. Solid lines represent product of the blaze functions of the gratings, atmospheric transmittance, and filter transmittance. Red, blue, and green dashed lines indicate the positions of OH emission lines, [Fe II] lines, and atomic hydrogen lines, respectively.
23. Relation between the echelle setting parameters (ESP) and offset angles from the nominal incident angle ($\alpha =$ 67$.^{\circ }$5). The lower panel shows the residuals after subtracting the offset angles of Eq. 42 obtainded by a least square fitting from measured offset angles.
24. Relation between the cross-disperser setting parameters (XSP) and offset angles from the nominal incident angle ($\alpha =$ 24$.^{\circ }$0). The lower panel shows the residuals after subtracting the offset angles of Eq. 43 obtainded by a least square fitting from measured offset angles.
25. Atmospheric transmittance, response function of the order sort filters, and blaze functions of the echelle and cross-disperser gratings.
26. Setting basic parameters for IRCS echelle spectra when the slit length is 3$.^{''}$89. The pixel scale of the echelle spectra along the slit length is about 0$.^{''}$060.
27. A reference dark frame made of combining several dark frames with median filtering. The integration time is 300 s.
28. Frames for making $H-$band flat frame. (left) OFF flat frame and (right) ON flat frame.
29. Frames for making $K-$band flat frame. (left) OFF flat frame and (right) ON flat frame.
30. Several main parameters of the APALL task to make the aperture data from point source spectra of Traceref.imh. The paremeters with itelic are critical.
31. Several main parameters of the APALL task to adjust the widths of apertures which are determined by llimit and ulimit. These limit parameters are adjusted to show all spectrum area along the slit length.
32. A parameter set for the APNORMALIZE task. The parameters with italic are critical.
33. Part of the normalized flat frames of $H$-band made by (a) APNORMALIZE task (b) APFLATTEN.
34. Part of the normalized flat frames of $K$-band made by (a) APNORMALIZE (b) APFLATTEN.
35. An example procedure for making a bad pixel mask and correcting bad pixels on an object.imh.
36. Bad pixels on the detector of the echelle section of IRCS. Black dots and lines are the bad pixels.
37. An example procedure to correct cosmic ray events for an object frame.
38. Main parameters to extract apertures for all frames with a reference frame.
39. A conceptional diagram of transformation from the image coordinates to the user coordinates during wavelength calibration and distortion correction. This diagram shows before and after the application of transformation of coordintes. Two images of a comparison line at the upper part show difference between before and after the distortion correction. Two aperture images at lower part show difference between before and after the wavelength calibration.
40. An example of the parameter setting and execution of the REIDENTIFY task. The parameters in italic are critical.
41. An example of the parameter setting and execution results of the FITCOORDS task.
42. An example of the parameter setting and execution results of the TRANSFORM task.
43. Sky subtraction with the BACKGROUND task.
44. Expanding a standard star spectrum along the spatial direction
45. A CL script to make one-dimensional spectrum and its usage.
46. A CL script to expand one-dimensionl spectrum along the spatial direction and its usage.
47. (a) Spectrum of an aperture including the Br12 absorption line. (b) Spectrum after the Br12 absorption line was removed by the SPLOT task.
48. A CL script to make a blackbody spectrum with the same width as the aperture.
49. Calibrated apertures. These show the calibrated apertures of the L1551 IRS 5.