The decker is a long reflective plate which overlies the slit. The observer may select a variety of options including slits of varying length, rectangular blockers of varying widths, circular blockers of various diameters, a set of non-symmetric slots for bizarre sky subtraction schemes, or the decker may be withdrawn completely for unobstructed direct imaging. One positon called "the finger" places the end of the rectangular blocker just off of the slit (for slits 1" or less wide) for use as a reference for positioning objects at the center of the slit length (it's usually a convenience in the reduction if everything falls along the same rows).

Notice that there are two full length positions (1 and 10). Position 1 may be used for either spectroscopic or direct. Position 10 will allow a full length slit for "normal" slit sizes, but will be paritally obstructed by adjacent portions of the decker if the slit is fully open, as for a direct window. Position 10 is closer physically to the normally used finger (position 11), so if you are switching between large and small spectroscopic slits, you may wish to use these adjacent positions. In fact the decker moves very rapidly, so 1 will work just as well. But don't use 10 for directs. A full-length decker is 145 arcseconds, which is 333 pixels on either the red or blue side detector (both have 15 micron pixels). This corresponds, of course, to the full length of the slit itself.

The decker slide is presently configured as follows:

Position	Name	Encoder number	Notes
0	Home	0
1	Open	-4375	For direct imaging
2	Asymmetric slots 1	-2942
3	Asymmetric slots 2	-2601
4	Asymmetric slots 3	-2259
5	Asymmetric slots 4	-1918
6	1 arcsec long	-1398	For slits up to 14" wide
7	2 arcsec long	-1228	For slits up to 14" wide
8	15 arcsec long	-1058	For slits up to 14" wide
9	30 arcsec long	-885	For slits up to 14" wide
10	60 arcsec long	-712	For slits up to 14" wide
11	Spect	-170	Full length, not for directs
12	Finger	-75	End of blocker in slit for slits larger than 1" wide
13	2 arcsec rectangular blocker	-29	For slits up to 9.5" wide
14	4 arcsec rectangular blocker	108	For slits up to 9.5" wide
15	6 arcsec rectangular blocker	217	For slits up to 9.5" wide
16	8 arcsec rectangular blocker	335	For slits up to 9.5" wide
17	9 arcsec circular blocker	1154	*
18	6 arcsec circular blocker	2348	*
19	3 arcsec circular blocker	3522	*
*The occulting disks are alumininized spots on a quartz plate which is not AR coated. Occulting disks are designed for use in direct imaging mode and do not line up with the slit. To occult objects in spectroscopy mode, use the rectangular blocker.

Figure 1: Decker Occulting Spots (for Direct Imaging, not Spectroscopy), 3, 6, and 9 arcsec diameters.

Figure 2: Slit Length Settings (left) of Spect, 60, 30, 15, 2, and 1 arcsec long, and Assymetric Slots (right).

Figure 3: Finger (Rectangular Blocker) on left, Slit Length Settings (right).

The aluminized slit opens bilaterally, and the smallest available step is a tiny fraction of a pixel. For convenience, the most commonly used slit sizes may be selected from the spectrograph controller simply by selecting the size in arcsecs according to the table below. Alternatively, you may enter the desired slit width in arcseconds from the 'Other...' option in the Slit selection menu.

Minimum slit size is set to 0.4 arcsec. Remember that you need at least a two pixel slit to minimize aliasing problems with narrow emission lines.

Scales and Conversions
scale at slit = 3.86 arcsec/mm
1mm = 3.86 arcsec = 8.885 pixels (for 15 micron pixel size)
1 pixel = 0.43 arcsec = 0.1126 mm (for 15 micron pixel size)

Position	Name	Encoder Number
0	Home	0
1	Open	-34344
2	0.5 arcsec	3989
3	1.0 arcsec	3857
4	1.5 arcsec	3724
5	2.0 arcsec	3591
6	2.5 arcsec	3459
7	3.0 arcsec	3326
8	4.0 arcsec	3061
9	5.0 arcsec	2796
10	9.0 arcsec	1734
	Other...	User enters desired slit size in arcsec

There are three stacked filter wheels called, from top to bottom, the upper, lower, and user wheels. One position of each wheel (position 0) is always empty.

Filters in the top three wheels will affect both beams of the spectrograph. If you want to use different filters on the two sides, they must be installed in the holders in front of the cameras. Since these later filters are in the collimated beam they must be bigger than 3.5 inches in diameter in order to avoid vignetting for direct imaging (a 2" square filter will reduce the effective aperture to about 1-meter; if this is your plan, it would surely be more politic to ask for one-meter time in the first place).

Order separating filters should not be necessary in typical double-beam use, except in the far red.

Upper Filter Wheel
Position	Name*	Encoder number
0	Home	0
11	Open	1275
12	None	2299
13	Spinrad NS**	3323
14	ND5.0	4347
15	ND1.25	5371
16	ND7.5	6395
17	ND2.5	7419
18	calcite prism	251
*ND values are in magnitudes. **Spinrad night sky filter pass band is ~6100 - 7600 A

Lower Filter Wheel
Position	Name	Encoder number
0	Home	0
11	Open	1435
12	BG14++	2459
13	OG570	3483
14	ND6.25	4507
15	GG455	5531
16	CuSO4*	6555
17	GG385	7569
18	GG495	411
*This is a good quality, full slit length crystal.

The user filter wheel accepts up to four filters of your choice mounted in our 2" square holders. Filter may be up to 8mm deep. Someone will definitely need to show you how to mount the filters on the first occasion. Please have a staff member (telescope technician or support astronomer) update the Kast motor control software with the current filters. Please remove your filters at the conclusion of your run (and have a staff member update the motor software accordingly). It's definitely safest not to assume that if the motor control software says the wheel is empty that there are no filters in place. We suggest always setting this wheel to the open position if you're not using it, just in case.

We have a fairly large library of narrow and intermediate band interference filters available, mostly on loan from astronomers within the UC system. It's clearly best not to assume that any specific filter will be here when you need it, as the owners are certainly free to remove them at will, and they may on occasion be loaned out. Since they're not really ours, we don't really control them. Any arrangement to take them elsewhere should be made with the owners, and duly recorded on the mountain as well.

User Filter Wheel
Position	Name	Contents	Encoder number
0	Home	N/A	0
0	Open	Empty	1178
1		(user determined)	2816
2		(user determined)	4454
3		(user determined)	6093
4		(user determined)	7731

Instead of the User Filter Assembly (described above) a Polarimeter Module can be installed (the current default Kast setup has the polarimeter installed instead of the user filter assembly). The polarimeter module contains two filter wheels and a waveplate. The polarimeter module will affect both beams of the spectrograph.

The upper and lower filter wheels accept up to four filters mounted in our 2" square holders. Filters may be up to 8mm deep. The lower filter wheel usually has B, V, R, and I filters installed, though this may not always be the case. If you install other filters, please remove them at the conclusion of your run. We suggest always setting these wheels to the open position if you're not using them. The tables below list the usual contents of the two wheels, though if wish to use them you should double check the contents.

Polarimeter Upper Filter Wheel
Position	Name	Encoder number
0	Home	0
1	Open	2319
2	Filter	681
3	Polaroid	7234
4	None	5596
5	Empty	3957

Polarimeter Lower Filter Wheel
Position	Contents	Step number
0	Home	0
1	Open	5914
2	B	4275
3	V	2637
4	R	998
5	I	7552

The waveplate can be moved in and out of the light path and rotated via the Kast motor control software.

Waveplate Insertion and Rotation
Position	Name	Encoder number	Notes
Out	Out	N/A	Waveplate out position
0	Home	0
1	0.0 deg	485
2	22.5 deg	673
3	45.0 deg	860
4	67.5 deg	1084
5	90.0 deg	1235
6	112.5 deg	1423
7	135.0 deg	1610
8	157.5 deg	1798
9	180.0 deg	1985
10	202.5 deg	2173
11	225.0 deg	2360
12	247.5.0 deg	2548
13	270.0 deg	2735
14	292.5 deg	2923
15	315.0 deg	110
16	337.5 deg	298

There are two separate carriers, either one of which (or neither, but not both) may be in the beam. Either carrier may contain one of the overcoated dichroics, or an aluminized flat mirror. The carrier called 1 (or X) is the one farthest away from the access door, and moves in an E-W sense with the TUB at its standard (90 degree) position angle (or left-right as seen from the access door); number 2 (or Y) is closer to the door and moves N-S (or toward and away from the door). Crossover for the blue dichroic (D46) is about 4650 A, and for the red dichroic (D55) it is about 5500 A. The crossover for the new D46 is about 4600 A and for the D57 at 5700 A. About 200 angstroms of the spectrum are affected by the crossover of the dichroic. The new D46 will replace the original D46 in the 2017A semester. The old D46 will remain available by special request for observers with long term programs that desire no changes in hardware. The new dichroics have superior transmittance/reflectance and more distinct crossovers than the original D46 and D55. However, the new dichroics have brighter ghost images 45 pixels (and additional fainter ghosts about 90 and 135 pixels away) from the main trace than the old dichroics. Insertion or removal of the D46 dichroic shifts the red spectrum by less than one pixel, but the D55 dichroic shifts the spectrum by about 10 pixels, compared to when no dichroic is in place. If you're only using one side at a time, in order to switch sides move the mirror in for blue or out for red. To get Select Side illuminated clear Clear red dichroic D46 or D55 or D57 both mirror Mirror blue

Dichroic Transmittance and Reflectance Plots Figure 1: New D4600 Reflectance-Transmittance Plot. Note that the reflectance greater than 1 is because it is a relative measurement compared to the flat mirror's aluminum coating. Figure 2: D5700 Reflectance-Transmittance Plot. Note that the reflectance greater than 1 is because it is a relative measurement compared to the flat mirror's aluminum coating. Figure 3: D5500 Reflectance-Transmittance Plot. Figure 4: Old D4600 Reflectance-Transmittance Plot. Scheduled to be retired 2017A semester.