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- Map of the Canary Islands
- Map of the island of La Palma
- Plan of the observatory site
- Distribution of clear (spectroscopic) hours by month
- Flux calibrated night sky spectrum, La Palma
- Time allocation on the Isaac Newton Group of Telescopes
- Schematic views of the WHT
(a) in perspective (b) looking orthogonally to the altitude and azimuth axes
- The area of sky
accessible to the WHT. Lines of equal zenith
distance are given on a plot of declination against hour angle.
The limits corresponding to partial obscuration of the telescope
by the dome rail (Zenith distance <78 degrees) and the zenith blind
spot (Zenith distance > 0.21 degrees; see text) are shown.
- Optical layout of the WHT
- Layout of the WHT Prime Focus Corrector and Atmospheric
Dispersion Compensator
- Spot diagrams for the f/11
Cassegrain and Nasmyth foci of the
WHT. (a) Aberrations on a flat focal surface passing though the
nominal focus on-axis. (b) Aberrations on a concave surface with radius
of curvature 2.2 m. This illustrates the image quality available at
the edge of the field for a suitably focused autoguider. (c) Aberrations
on a flat surface which is focused for a compromise over the field.
- Spot
diagrams in a single plane for the Nasmyth foci of the
WHT when used with the image derotation optics. Images for
wavelengths from 330 - 1000 nm and distances of up to 2.5 arcmin
from the axis are shown.
- Vignetting at various foci of the WHT. The curves show the
percentage transmission as a function of field radius. For
accurate photometry, they should be interpreted with caution.
The diagram refers to the area outside the constant central
obstruction (8.4%) and secondary vane obstruction (0.6%). (a) f/11 Cassegrain
and Nasmyth foci (b) prime focus.
- Three
views of the Cassegrain acquisition and guider unit
for the WHT. (a) Plan, showing the autoguider, cable wrap and filter slides.
(b) Elevation, showing TV, autoguider and comparison system. (c) Elevation,
showing the large and small feed mirrors and
the auxiliary port.
- The
acquisition and guider unit for the Utrecht Echelle
Spectrograph at the Nasmyth focus of the WHT. (a) Side view (b) Plan view
- The
Prime Focus Instrument Platform plan view (above), and side view (below)
- Schematic views of the INT from the east and north.
- The
area of sky accessible to the INT. Lines of equal
zenith distance are drawn on a plot of declination against hour angle.
- Spot
diagrams for images at the f/15 Cassegrain focus of the
INT, showing the dependence on field radius and the effects of defocussing.
- Spot
diagrams for the prime focus of the INT with the three-element
corrector at different wavelengths and field radii.
The scale is shown by a circle of radius 1.0 arcsec.
- Three
views of the Cassegrain acquisition and guider unit of the
INT, showing the autoguider, TV camera, comparison system and
filters. (a) and (b) Elevation, (c) Plan
- The
optical system for viewing the acquisition field at the
Cassegrain focus of the INT.
- The
area within which guide stars may be chosen for use with
the autoguider at the Cassegrain focus of the INT. Stars
may be selected in the shaded area. If the autoguider probe
is moved closer to the centre of the field, then the slit is
obscured. Partial obscuration occurs in the area shaded with
dashed lines. The field outside the circle
is heavily vignetted, but bright stars may
be usable. The orientation of the diagram on the sky is
given for the instrument rotator in PA = 0. At other PA's,
the diagram must be rotated anticlockwise by the PA.
- The
area within which guide stars may be selected for use with
the autoguider at the prime focus of the INT.
(a) Scale drawing of the locations of chip, rotator axis and
guide-star acquisition field, showing probe-coordinate limits.
(b) A sketch showing the general
relation between guide probe and sky coordinates for any PA.
- Schematic views of the JKT. (a) From
the north (b) From the west
- The
area of sky accessible to the JKT. Lines of constant
zenith distance are drawn on a plot of declination against
hour angle. The horizon and hour-angle limits are shown
for the two possible cases: (a) Telescope west of the pier
(b) Telescope east of the pier
- Optical
layout of the JKT, showing the f/8.06 Harmer-Wynne and
f/15 Cassegrain configurations.
- (a)
Spot diagrams for images at the f/8.06 focus of the JKT for
various wavelengths and field radii. The diameter of the
circle is 1.0 arcsec.
(b) Spot diagrams for a flat surface at the f/15 Cassegrain
focus of the JKT.
- The
acquisition and guider unit used with the CCD camera
at the f/15 Cassegrain focus of the JKT, showing grisms,
filters, shutter assembly, TV camera, autoguider, drift-
scan table and CCD cryostat.
- The
acquisition unit used with the photometers and
spectrographs at the f/15 Cassegrain focus of the JKT,
showing the acquisition mirror, TV camera and comparison system.
- FOS
- The efficiency of FOS-1
- The efficiency of FOS-2
- Format of a FOS-1 mode D spectrum
- The JKT Richardson-Brealey Spectrograph
- Efficiency curves for the JKT CCD camera grisms
- The INT Intermediate Dispersion Spectrograph
- Efficiency curves for the IDS collimators
- Efficiency curves for the IDS gratings
- Exploded
view of the optical components of ISIS and FOS-2, showing
the light paths through the components.
- The
Polarimetry optics, slit area components, folds, and below slit
filters of ISIS and FOS-2.
- The ISIS Collimator Assembly
- The ISIS Grating Cells
- Format
of the output of the blue cross-disperser, with IPCS (solid lines)
and EEV P88300 CCD (dashed lines) outlines superimposed. The solid lines
represent the outline of the IPCS field in a typical format, and the dashed
lines a TEK 1024 chip. The
crosses mark the points at which the grating efficiency drops to half of its
peak value in that order. The central wavelength of each order is marked.
- Efficiency curves for the ISIS gratings
- Schematic of LDSS-2
- Laboratory measurements of the efficiency of, (a) the main optics
(camera and collimator), (b) the grisms
- Schematic
of the Utrecht Echelle Spectrograph (UES).
- TAURUS-2
- The efficiency of the TAURUS-2 focal reducer (i.e. camera
plus collimator)
- Responsive
Quantum Efficiency (RQE) as a function of wavelength for the
Tektronix and EEV CCD detectors most commonly used on the La Palma Telescopes
- A schematic representation of how photons are counted
by the IPCS
- Responsive Quantum Efficiency as a function of wavelength for the
S-20 photocathode used in the IPCS. The overall efficiency of the IPCS is equal to the efficiency
of the photocathode multiplied by the counting efficiency, which
is probably about 60 %
- Optical
layout of the Peoples' Photometer. The top eyepiece
is the old TV position (not now used) and the lower eyepiece is the
present TV position.
- The
ISIS Spectrograph and the A&G box with the fibre system
- Attenuation
curves for Polymicro high OF (FH series) optical fibre
- The Multi-Purpose Fotometer
- Plot of declination against
hour angle for the latitude of
La Palma, showing lines of equal zenith distance. This plot shows the
region within which observations are possible with the WHT.
- Plot
of declination against hour angle for the latitude of
La Palma, showing lines of equal zenith distance. This plot shows the
region within which observations are possible with the INT.
- Plot
of declination against hour angle for the latitude of
La Palma, showing lines of equal zenith distance. This plot shows the
region within which observations are possible with the JKT, with the
telescope both east of the pier (a) and west of the pier (b).
- Plot
showing how the magnitude of atmospheric refraction varies
with wavelength and airmass.
- Plot
of parallactic angle against hour angle, showing lines
of constant declination. Note the discontinuity at transit (hour angle
equal to zero) for objects with a declination equal to the latitude
of La Palma.
- Theoretical
atmospheric extinction on La Palma as a function
of wavelength and airmass
- The light path of INT or WHT prime focus near the filter
Tue Aug 15 16:42:46 BST 1995