U.S. patent application number 11/296822 was filed with the patent office on 2006-05-04 for systems and methods for aligning a telescope.
Invention is credited to Kenneth W. Baun, John E. Hoot.
Application Number | 20060092508 11/296822 |
Document ID | / |
Family ID | 26802764 |
Filed Date | 2006-05-04 |
United States Patent
Application |
20060092508 |
Kind Code |
A1 |
Baun; Kenneth W. ; et
al. |
May 4, 2006 |
Systems and methods for aligning a telescope
Abstract
Embodiments of a telescope system include methods for alignment
with a spherical coordinate system. For example, embodiments may
include determining data for date, time, location, level and North
(true or magnetic). Upon acquisition of this data, the telescope
system can determine and first alignment. To the extent needed or
desired, further alignment methods can improve the accuracy of the
first alignment; however, in many cases, the first alignment is
sufficient to align a field of view of the telescope with a
selected and/or desired astronomical object.
Inventors: |
Baun; Kenneth W.; (Trabuco
Canyon, CA) ; Hoot; John E.; (San Clemente,
CA) |
Correspondence
Address: |
KNOBBE MARTENS OLSON & BEAR LLP
2040 MAIN STREET
FOURTEENTH FLOOR
IRVINE
CA
92614
US
|
Family ID: |
26802764 |
Appl. No.: |
11/296822 |
Filed: |
December 7, 2005 |
Related U.S. Patent Documents
|
|
|
|
|
|
Application
Number |
Filing Date |
Patent Number |
|
|
10357912 |
Feb 4, 2003 |
|
|
|
11296822 |
Dec 7, 2005 |
|
|
|
09428865 |
Oct 26, 1999 |
|
|
|
10357912 |
Feb 4, 2003 |
|
|
|
10358754 |
Feb 5, 2003 |
|
|
|
11296822 |
Dec 7, 2005 |
|
|
|
60105626 |
Oct 26, 1998 |
|
|
|
60143637 |
Jul 14, 1999 |
|
|
|
Current U.S.
Class: |
359/429 ;
359/399; 359/430 |
Current CPC
Class: |
G02B 23/165 20130101;
F16M 11/10 20130101; G02B 23/16 20130101; G02B 23/00 20130101; F16M
11/18 20130101; F16M 11/32 20130101; F16M 11/2014 20130101 |
Class at
Publication: |
359/429 ;
359/430; 359/399 |
International
Class: |
G02B 23/00 20060101
G02B023/00 |
Claims
1. A method of aligning a field of view of a telescope tube with a
system of locating celestial objects, the method comprising:
receiving date data indicative of an approximate current date;
receiving time data indicative of an approximate current time;
receiving location data indicative of an approximate current
location of a telescope system including a telescope tube and motor
control electronics capable of positioning a field of view of the
telescope tube; receiving first data indicative of the telescope
tube being approximately positioned at a terrestrial direction or a
determinable angle with respect to the terrestrial direction;
receiving second data indicative of the telescope tube being
approximately positioned at horizontal or a determinable angle with
respect to horizontal; and electronically determining an alignment
of the field of view of the telescope tube with respect to a system
of locating celestial objects.
2. The method of claim 1, wherein the system of locating celestial
objects comprises a celestial coordinate system.
3. The method of claim 1, wherein the receiving first data
comprises receiving an indication from a user that the telescope
tube is appropriately positioned.
4. The method of claim 3, wherein the first data comprises data
received from an incremental encoder system.
5. The method of claim 4, comprising zeroing a count based on
output from the incremental encoder system upon receipt of the
indication.
6. The method of claim 4, comprising storing a count based on
output from the incremental encoder system upon receipt of the
indication.
7. The method of claim 3, wherein the first data comprises data
received from an absolute encoder system.
8. The method of claim 1, wherein the receiving second data
comprises receiving an indication from a user that the telescope
tube is appropriately positioned.
9. The method of claim 8, wherein the second data comprises data
received from an incremental encoder system.
10. The method of claim 8, wherein the second data comprises data
received from an absolute encoder system.
11. The method of claim 1, wherein at least one of the date data
and time data is acquired from an electronic device capable of
measuring time or date.
12. The method of claim 1, wherein the location data is acquired
from an electronic device capable of measuring location of the
telescope system.
13. The method of claim 1, wherein the terrestrial direction
comprises approximately true North.
14. The method of claim 1, wherein the terrestrial direction
comprises approximately magnetic North.
15. The method of claim 1, comprising: electronically determining a
plurality of celestial objects potentially available to the field
of view of the telescope tube based at least in part on the date
data, the time data, and the location data; receiving a user
selection of one of the plurality of celestial objects; and using
said alignment, moving the field of view of the telescope tube to
include a vicinity of the one celestial object.
16. The method of claim 1, comprising correcting the alignment of
the telescope tube through acquisition of additional alignment
data.
17. The method of claim 16, wherein the acquisition of additional
alignment data comprises: selecting an alignment celestial object
from a database of celestial objects, the alignment celestial
object selected based at least in part on the date data, the time
data, and the location data; using said alignment, moving the field
of view of the telescope tube to include a vicinity of the
alignment celestial object; receiving data indicative of the
alignment celestial object being identified through the telescope
tube; and electronically correcting said alignment of the telescope
tube with respect to the system of locating celestial objects.
18. The method of claim 17, wherein the acquisition of additional
alignment data comprises: selecting a second celestial object from
a database of celestial objects, the second alignment celestial
object selected based at least in part on the date data, the time
data, and the location data; using said corrected alignment, moving
the field of view of the telescope tube to include a vicinity of
the second alignment celestial object; receiving data indicative of
the second alignment celestial object being identified through the
telescope tube; and electronically correcting the corrected
alignment of the telescope tube with respect to the system of
locating celestial objects.
19. The method of claim 16, wherein the acquisition of additional
alignment data comprises: receiving data indicative of a selection
of an alignment celestial object, wherein data regarding the
alignment celestial object is stored in a database of celestial
objects and is selected based at least in part on the date data,
the time data, and the location data; using said alignment, moving
the field of view of the telescope tube to include a vicinity of
the alignment celestial object; receiving data indicative of the
alignment celestial object being identified through the telescope
tube; and electronically correcting said alignment of the telescope
tube with respect to the system of locating celestial objects.
20. An article of manufacture comprising software instructions
stored in a processor accessible storage medium and executable by a
processing device capable of providing instructions to a telescope
positioning system to accurately position a telescope tube with
respect to a sky, the software instructions configured to cause the
processor to receive or calculate data indicative of an approximate
current time, an approximate current date, an approximate current
location, a terrestrial direction or a determinable angle with
respect to the terrestrial direction, and horizontal or a
determinable angle with respect to horizontal, and to cause the
processor to determine an alignment of the telescope tube with
respect to a celestial coordinate system.
21. The article of manufacture of claim 20, wherein the software
instructions are capable of causing the processor to use the
alignment to move the telescope tube to view a desired celestial
object.
22. The article of manufacture of claim 20, wherein the terrestrial
direction comprises approximately true North.
23. The article of manufacture of claim 20, wherein at least one of
the data indicative of current time, current date, current
location, terrestrial direction, and horizontal is automatically
acquired from an electronic device capable of measuring the
same.
24. The article of manufacture of claim 20, wherein the software
instructions are capable of causing the processor to correct the
alignment of the telescope tube through acquisition of additional
alignment data.
25. A telescope system comprising: an optical system usable in
resolving distant objects; an electronic positioning system capable
of positioning the optical system, wherein the electronic
positioning system includes positional reference indicators capable
of identifying a change in position of the optical system; computer
accessible memory configured to store alignment data at least
generally indicative of time, date, location, output from the
positional reference indicators with respect to a terrestrial
direction, and output from the positional reference indicators with
respect to horizontal; and a processor configured to determine an
alignment of the optical system with respect to a system of
locating celestial objects.
26. The method of claim 25, wherein the system of locating
celestial objects comprises a celestial coordinate system.
27. The telescope system of claim 26, comprising computer
accessible memory configured to store positional information for at
least a plurality of celestial objects with respect to the
celestial coordinate system, wherein said processor is also
configured to determine at least one viewable celestial object from
the plurality of celestial objects, the processor also configured
to position the optical system to view a vicinity of the viewable
celestial object based on the alignment data and the corresponding
positional information of the viewable celestial object.
28. The telescope system of claim 25, wherein the positional
reference indicators comprise optical encoders.
29. The telescope system of claim 25, wherein the positional
reference indicators comprise incremental encoders.
30. The telescope system of claim 25, wherein the positional
reference indicators comprise absolute encoders.
31. The telescope system of claim 25, wherein the terrestrial
direction comprises approximately true North.
32. The telescope system of claim 25, comprising one or more
devices capable of measuring at least one of time and date.
33. The telescope system of claim 25, comprising one or more
devices capable of measuring at least one of terrestrial direction
and horizontal.
34. The telescope system of claim 25, comprising one or more
devices capable of determining location of the optical system.
35. A telescope system capable of using input data to determine at
least a first approximated alignment, the telescope system
comprising: a telescope tube; means for positioning the telescope
tube; means for acquiring an approximate current date; means for
acquiring an approximate current time; means for acquiring an
approximate current location; means for acquiring an approximate
positional information with respect to a terrestrial direction;
means for acquiring an approximate positional information with
respect to horizontal; and electronic means for aligning the
telescope tube with the sky.
36. The telescope system of claim 35, wherein the means for
acquiring the approximate positional information with respect to a
terrestrial direction comprises means for receiving user input.
37. The telescope system of claim 35, wherein the means for
acquiring the approximate positional information with respect to
horizontal comprises means for receiving user input.
38. The telescope system of claim 35, comprising means for using
the alignment of the telescope tube to view a celestial object.
39. The telescope system of claim 35, comprising means for
correcting the alignment of the telescope tube.
40. A method of determining a first approximation of an alignment
of a field of view of a telescope tube, the method comprising:
acquiring an indication of current time; acquiring an indication of
current date; acquiring an indication of current location;
acquiring an indication that a telescope tube is approximately
level; acquiring an indication of a terrestrial orientation of the
telescope tube, wherein the terrestrial orientation comprises one
of North, South, or an identifiable terrestrial orientation; and
determining a first approximation of an alignment of a field of
view of the telescope tube.
41. The method of claim 40, comprising using the first
approximation to electronically move the telescope tube to until a
desired celestial object is within the field of view.
Description
PRIORITY CLAIM
[0001] The present application is a continuation of U.S. patent
application Ser. No. 10/357,912, filed Feb. 4, 2003 entitled
"Automated Telescope Alignment and Orientation Method" (the '912
Application), which is a continuation of U.S. patent application
Ser. No. 09/428,865, filed Oct. 26, 1999 entitled "Automated
Telescope Alignment and Orientation Method" (the '865 Application),
which claims a priority benefit of U.S. Provisional Pat. App. Ser.
No. 60/105,626, filed Oct. 26, 1998 entitled "Fully Automated
Telescope System With Distributed Intelligence" and 60/143,637,
filed Jul. 14, 1999, entitled "Self Orienting, Self Aligning,
Intuitive Automated Telescope." The present application is also a
continuation of U.S. patent application Ser. No. 10/358,754, filed
Feb. 5, 2003 entitled "Automated Telescope With Distributed
Orientation and Operation Processing" (the '754 Application), which
is also a continuation of the '865 Application. Each of the
foregoing disclosures is expressly incorporated herein by
reference.
CROSS-REFERENCE TO RELATED APPLICATIONS
[0002] The present application is related to the following
co-pending applications, including any subsequently filed
continuations, continuations-in-part, or divisionals of the same:
The '912 Application, the '754 Application, and U.S. patent
application Ser. No. 11/189,005, filed Jul. 25, 2005 entitled
"Systems and Methods for Automated Telescope Alignment and
Orientation," the disclosures of which is expressly incorporated
herein by reference.
FIELD OF THE INVENTION
[0003] The present invention relates to telescopes or other
observation instruments and, more particularly, it relates to
telescope systems with distributed intelligence and control systems
for such telescopes.
SUMMARY OF THE INVENTION
[0004] The present invention relates to fully automatic telescope
systems which are capable of performing alignment and orientation
operations under program control with a minimum of intervention by
a user. The telescope system is able to perform its alignment and
orientation functions regardless of whether it might be configured
as an alt-azimuth telescope or as an equitorial telescope. In
accordance with the invention, the system is provided with
sufficient processing power and with a multiplicity of application
routines so that alignment and orientation is performed with regard
to a large number of different algorithms and with respect to a
variety of user definable data type inputs. All that is required is
that some location index be provided to the system and that the
system's motors are initialized to a horizontal and vertical
referant. Time might be included as an input parameter, whether
user provided, or by automatic extraction from a peripherally
coupled device. Location indices as well as horizontal and vertical
referants might be user provided, obtained under user direction, or
automatically obtained from various other peripherally coupled
devices.
[0005] The telescope system has a distributed intelligence in that
its motor control functions are independently developed by motor
modules including a microcontroller, operating on motor movement
commands received from a hand held command module, in combination
with position feedback information derived from optical encoders
coupled to each motor shaft. Alternatively, the encoders might be
coupled to each of a telescope's two generally orthogonal axes, and
encoder feedback signals directed to the motor module
microcontrollers.
[0006] Distributed intelligence is further characterized in that
the telescope system hand held command module might be provided in
two separate configurations. A first configuration is simplified,
and only provides direction and speed commands to the intelligent
motor modules. System intelligence thus resides in the motor
modules with the command module functioning more as a steering
wheel, or directional joy stick.
[0007] In a second configuration, the command module is a fully
functional microprocessor controlled command unit, capable of
executing high level application software routines and performing
numerous data processing tasks, such as numerical calculations,
coordinate system transformations, database manipulations, and
managing the functional performance of various different
peripherally coupled devices.
[0008] A central interface panel is provided on the telescope
system and supports interconnection between and among the
intelligent motor modules, the command module (of either form) and
peripheral devices. Communication between and among the component
parts is made over serial data and control communication channels
in accordance with a packet based serial communication protocol. An
RS-232 port is also provided such that a command module is able to
communicate with ancillary RS-232 capable devices like personal
computer systems and/or a command module belonging to another
intelligent telescope system according to the invention.
[0009] Use of the various communication channels allows the
telescope system according to the invention to communicate with
other devices in order to exchange stored information, exchange
created and stored operating routines, obtain updates to programs
and/or internal databases and the like. In this regard, the
telescope system includes a number of internal databases, including
at least one database of the celestial coordinates (RA and DEC) of
known celestial objects that might be of interest to an observer.
Further, the system includes a database of the geographical
coordinates (Latitude and Longitude) of a large body of
geographical landmarks. These landmarks might include the known
coordinates of cities and towns, cartographic features such as
mountains, and might include the coordinates of any definable point
on the earth's surface whose position is stable and geographically
determinable. Each of the databases are user accessible such that
additional entries, of particular interest to a user, might be
included.
[0010] The solution to any given problem in celestial trigonometry
depends on being able to convert measurements obtained in one
coordinate system (alt-az, for example) into a second coordinate
system (the celestial coordinate system). The present invention
relates to a system and method for orienting a computerized
telescope system of the type including a telescope coupled for
rotation about two orthogonal axes, with respect to a spherical
coordinate system. The telescope is provided with a pair of motors,
each motor coupled to rotate the telescope about a respective one
of the orthogonal axes. Each motor further includes a positional
reference indicator which defines an arcuate position of the
telescope with respect to its corresponding axis. Positional
reference information is taken from each positional reference
indicator and provided to a control processor which is programmed
to carry out the calculations necessary for effecting coordinate
system transformation.
[0011] In a first line of procedure, the computerized telescope
system is able to locate its own alignment stars based on date and
time entries provided by, a user during an initialization
procedure. Specifically, the telescope is moved about one of its
orthogonal axes until the telescope is pointed at a first
positional reference. In one aspect of the invention, the first
positional reference is North.
[0012] After the telescope system is pointed to the first
positional reference, the arcuate position of that positional
reference indicator is recorded and stored by the control processor
so as to define a first reference position. Next, the telescope is
moved about a second axis in order to position the telescope at a
second reference point. In a particular aspect of the invention,
the second reference point is the horizon, thus causing the
telescope to be leveled. The arcuate position of the respective
positional reference indicator is read and recorded to thereby
define a second reference point.
[0013] Particularly, the positional reference indicators are
position encoders of altitude and azimuth motor assemblies.
Pointing the telescope North and leveling the telescope, functions
to zero-in the position encoders of the altitude and azimuth motor
assemblies. Any subsequent motion of the telescope away from its
0,0 position allows the telescope system to directly calculate its
altitude and azimuth displacements from the 0,0 reference
point.
[0014] Using time and date entries provided by a user, the
telescope system consults a database of well known celestial
objects and selects a particular bright object which is currently
above the horizon. The entered time and date information allows the
system to calculate whether that particular bright object has
rotated sufficiently in right ascension to bring it above the
observer's horizon, while a virtual latitude and longitude entry
provided by an observer's entering a geographical indicia, provides
the system with sufficient information regarding an observer's
latitude such that it may calculate a declination value for the
desired viewing object.
[0015] The system automatically slews the telescope to the vicinity
of the desired viewing object by commanding the appropriate motion
from the altitude and azimuth motors. Once the telescope has slewed
to the vicinity of the desired star, the observer is prompted to
center the star in the field of view of the telescope eyepiece.
Once the star is centered in the field of view of the eyepiece, the
system calculates the position and orientation of the telescope
with respect to the night sky (the celestial sphere).
BRIEF DESCRIPTION OF THE DRAWINGS
[0016] These and other features, aspects and advantages of the
present invention will be more fully understood when considered
with respect to the following detailed description, appended claims
and accompanying drawings wherein:
[0017] FIG. 1 is a semi-schematic perspective view of one
embodiment of a telescope system in accordance with the present
invention, configured in an initial, un-automated manner;
[0018] FIG. 2 is a semi-schematic perspective view of the telescope
system of FIG. 1, including semi-intelligent drive motors coupled
to the telescope axes and illustrating alternative control
systems.
[0019] FIG. 3a is a semi-schematic partial perspective view of an
electrical interface panel in accordance with the present
invention;
[0020] FIG. 3b is a semi-schematic block diagram of the signal and
bus configuration of the electrical interface panel of FIG. 3a;
[0021] FIG. 4a is a semi-schematic exploded perspective view of a
semi-intelligent motor assembly in accordance with the present
invention;
[0022] FIG. 4b is a semi-schematic block diagram of the electrical
components of a semi-intelligent motor assembly in accordance with
the present invention;
[0023] FIG. 5a is a semi-schematic front view of an embodiment of a
semi-intelligent dual-axis drive motor motion control system
according to practice of principles of the present invention;
[0024] FIG. 5b is a semi-schematic block diagram of the electronic
components of the embodiment of the semi-intelligent dual-axis
drive motor motion control system of FIG. 5a;
[0025] FIG. 6a is a semi-schematic front view of an intelligent
dual-axis drive motor motion control system according to practice
of principles of the present invention;
[0026] FIG. 6b is a semi-schematic block diagram of the electronic
components of the embodiment of the intelligent dual-axis drive
motor motion control system of FIG. 6a;
[0027] FIG. 7a is a simplified waveform diagram of ideal
photodetector output characteristics, illustrating a quadrature
output pattern;
[0028] FIG. 7b is a simplified waveform diagram illustrating
photodetector "on" and "off" periods in accord with the
invention;
[0029] FIG. 7c is a simplified waveform diagram depicting
dynamically tuned photodetector output characteristics, exhibiting
an ideal quadrature output pattern;
[0030] FIG. 8 is a conceptual flow diagram of an initialization
procedure in accordance with the invention;
[0031] FIG. 9 is a database table illustrating an exemplary
location entry;
[0032] FIG. 10a is a conceptual flow diagram of a first, "easy"
alt-az alignment and orientation procedure in accord with the
invention;
[0033] FIG. 10b is a conceptual flow diagram of a second, single
star, alt-az alignment and orientation procedure in accord with the
invention;
[0034] FIG. 10c is a conceptual flow diagram of a third, two-star,
alt-az alignment and orientation procedure in accord with the
invention;
[0035] FIG. 11a is a conceptual flow diagram of a first, "easy"
polar alignment and orientation procedure in accord with the
invention;
[0036] FIG. 11b is a conceptual flow diagram of a second, single
star, polar alignment and orientation procedure in accord with the
invention;
[0037] FIG. 11c is a conceptual flow diagram of a third, two-star,
polar alignment and orientation procedure in accord with the
invention;
[0038] FIG. 12 is an exemplary line listing of a communication
packet in accordance with the interface protocol of the
invention;
[0039] FIG. 13 is a simplified partial perspective view of a
uniform illumination lightbox;
[0040] FIG. 14 is a perspective view of a second embodiment of a
telescope according to the invention, having integrated motor
assemblies;
[0041] FIG. 15 is a simplified, exploded, partial perspective view
of a declination (altitude) motor assembly integrated into a fork
arm of the telescope of FIG. 14;
[0042] FIG. 16 is a simplified, partial perspective view of a right
ascension (azimuth) motor assembly integrated into the base housing
of the telescope of FIG. 14;
[0043] FIG. 17 is a simplified schematic diagram of an MR sensor
useful in practice of the present invention;
DETAILED DESCRIPTION OF THE PREFERRED EMBODIMENT
[0044] The detailed descriptions of a fully automated telescope
system with distributed intelligence set forth below in connection
with the appended drawings are intended only as a description of
the presently preferred and illustrated embodiments of the
invention, and are not intended to represent the only form in which
the present invention may be constructed or utilized. The detailed
descriptions set forth the construction and function of the
invention as well as the sequence of steps utilized in the
operation of the invention in connection with the illustrated
embodiments. It is to be understood by those having skill in the
art, that the same or equivalent of functionality may be
accomplished by various modifications to the illustrated
embodiments without departing from the spirit and scope of the
invention.
[0045] A fully automatic telescope system with distributed
intelligence and a control system for operating such a telescope
will now be described with reference to the embodiments illustrated
in the Figures.
[0046] In FIG. 1, a telescope system 10 for observing celestial,
and terrestrial, objects is provided in accordance with the present
invention. The telescope system 10 suitably comprises a telescope
tube 12 which houses the optical system required for resolving
distant objects and including a focusing objective and eyepiece 14
coupled to the optical system in a manner to allow observation of
the optical system's focal plane. The telescope tube 12 is
supported by a mount 16 which facilitates movement to the telescope
tube 12 about two orthogonal axes, a substantially vertical axis,
termed an azimuth axis and a substantially horizontal axis, termed
an altitude axis. As those having skill in the art will appreciate,
the horizontal and vertical axes of the mount 16 in combination
define a gimbaled support for the telescope tube 12 enabling it to
pivot in a horizontal plane defined by the vertical (or azimuth)
axis and, independently, to pivot through a vertical plane defined
by the horizontal (altitude) axis.
[0047] It should be noted, at this point, that the telescope system
10 is illustrated as comprising a telescope tube 12 configured as a
refracting-type telescope. However, the form of the telescope's
optical system, per se, is not particularly relevant to practice of
principles of the present invention. Thus, even though depicted as
a refractor, the telescope system 10 of the present invention is
eminently suitable for use with reflector-type telescopes. The
specific optical systems used might be Newtonian,
Schmidt-Cassegrain, Maksutov-Cassegrain, and any other conventional
reflecting or refracting optical system configured for telescopic
use.
[0048] In the telescope system embodiment illustrated in FIG. 1, it
is convenient to support the telescope tube and mount combination
in such a manner that the vertical axis 18 is, indeed,
substantially vertical such that the telescope pivots (or rotates)
about the vertical axis in a plane which is substantially
horizontal. A tripod, indicated generally at 22, conventionally
functions to support the mount 16 such that the azimuth axis 18 is
substantially orthogonal to a horizontal plane, relative to a user
of a telescope system. The tripod 22 includes three legs 24a; b, c,
which are arranged in a triangular pattern. Each of the legs are
independently adjustable for leveling the mount 16 regardless of
the nature of the surface on which the telescope system 10 is
used.
[0049] The illustrated embodiment of the telescope system of FIG. 1
is a manual, non-automatic embodiment in that the telescope tube 12
is pivotally moved about the azimuth axis 18 and altitude axis 20
by a user's grasping and manually moving an axially mounted azimuth
control knob 26 and an axially mounted altitude control knob 28.
Each of the control knobs 26 and 28 are journaled to respective
axis pins through a conventional gearing system such that small and
precise movements of the telescope tube 12 may be made about the
azimuth and altitude axes 18 and 20 by relatively large rotations
of the control knobs 26 and 28. In this respect, the telescope
system 10 of FIG. 1 resembles a conventional, manually operated
telescope system.
[0050] In addition to supporting telescope motion about two
orthogonal axes, the mount 16 further comprises an electrical
interface junction panel 30 which, in a manner to be described in
greater detail below, is configured to support upgradeability of
the telescope system 10 into a fully automatic telescope system
with distributed intelligence, in a plurality of logically
consistent steps, each of which results in a fully functional
telescope system having greater or lessor degrees of intelligence
and functionality, depending on where, along the upgrade spectrum,
user achieves the most subjectively desirable ratio between system
complexity and functional benefit.
[0051] Turning now to FIG. 2, there is depicted a semi-schematic
perspective view of the telescope system 10 of FIG. 1, including
semi-intelligent motor means for pivotally moving the telescope
about the azimuth axis 18 and altitude axis 20. Semi-intelligent
motor means suitably comprises a semi-intelligent, self-contained
azimuth axis drive motor assembly 32 and a semi-intelligent,
self-contained altitude axis drive motor assembly 34. Each of the
drive motor assemblies 32 and 34 are self-contained motor packages
including a DC brush-type motor, an associated electronics package
hosted on a printed circuit board, a reduction gear assembly and an
optical encoder assembly, configured together in a housing in a
manner according to co-pending patent application entitled
INTELLIGENT MOTOR MODULE FOR TELESCOPE AXIAL ROTATION, filed on
instant date herewith and commonly owned by the Assignee of the
present invention, the entire disclosure of which is expressly
incorporated herein by reference. The semi-intelligent motor
assemblies 32 and 34 are each affixed to the telescope mount 16 and
coupled to the azimuth and altitude axes 18 and 20, respectively,
so as, to be able to pivotally move the telescope tube 12 about the
corresponding axis when the motor assembly is activated. Each of
the motor assemblies 32 and 34 are plugged into respective
corresponding receptacles in the electrical interface junction
panel 30 which, in a manner to be described in greater detail
below, functions as a signal interface for the motor assemblies as
well as providing power and ground thereto. The electrical
interface junction panel 30 allows motor control signals to be
directed to each of the motor assemblies 32 and 34, the motor
control signals providing speed and direction information to the
electronics package which, in turn, provides appropriate activation
signals to the respective DC motor comprising the assembly. The
electrical interface junction panel 30 further allows for signal
communication between each respective one of the motor assemblies
32 and 34 and a hand-held system control unit 36.
[0052] In operation, a user plugs the hand-held system control unit
36 into an appropriate receptacle of the electrical interface
junction panel 30 and further plugs the motor assemblies 32 and 34
into their respective receptacles, thus completing a signal path
between each of motor assemblies and the system control unit 36.
Motion commands are provided to the system by the user by accessing
the appropriate function provided on the system control unit 36.
Signals corresponding to the desired motion are directed by the
control unit 36 to the appropriate motor assembly through the
electrical interface junction panel 30. For example, if a user
desires to slew the telescope in a counter-clockwise direction, he
may enter a command into the control unit 36 telling the telescope
system to move "left". In response, the azimuth axis motor assembly
32 is commanded to activate its integral motor to rotate in a
particular direction, thus causing the telescope mount to pivot in
a counter-clockwise fashion about the azimuth axis 18. In like
manner, when a user desires to elevate the telescope tube 12 in an
upwardly direction, the user would enter the appropriate "up"
command into the control unit 36, thus activating the altitude
motor assembly 34, which, in turn, causes the telescope to pivot
upwardly about the altitude axis 20.
[0053] Turning briefly now to FIGS. 3a and 3b, the mechanical and
electrical configuration of the electrical interface junction panel
30 are illustrated. As can be understood from FIG. 3b, the
interface junction panel 30 suitably comprises four RJ11-type
connector receptacles, with three of the receptacles 38, 40 and 42,
comprising 4-pin RJ11 connectors and one of the receptacles 44,
comprising an 8-pin RJ11 connector. In addition to the RJ11
connections, the electrical interface junction panel includes a
"mini pin" type 12 volt power receptacle 46 and a visible "power
present" indicator comprising an LED 48 mounted to shine through a
recessed opening in the panel located proximate to the power pin
46.
[0054] FIG. 3a illustrates the electrical connections-made between
and among the 4-pin RJ11 connectors, the 8-pin RJ11 connector and
the 12 volt power pin 46. External power is supplied to the various
connectors comprising the electrical interface panel 30 by a
suitable 12 volt power source 48 which might comprise a dedicated
12 volt battery pack or, alternatively, an adaptor configured to
mate with a 12 volt automotive battery through, for example, an
accessory power plug or a cigarette lighter. The external power
source 48 is plugged into the 12 volt power pin 46 which takes the
12 volt potential from the pin's center post and distributes it to
pin 1 of the 8-pin RJ11 connector 44 and the No. 4 pin of each of
the 4-pin RJ11 connectors 38, 40 and 42. The 12 volt potential is
referenced to a return or ground potential, contacting a sleeve
surrounding the center post, in conventional fashion, and the
reference potential is directed to the No. 8 pin of the 8-pin RJ11
connector 44 and the No. 1 pin of the 4-pin RJ11 connectors 38, 40
and 42. In addition, the 12 volt supply is dropped across a
series-configured resistor 50 and LED diode 48 combination such
that the LED 48 emits when a power supply is present. Thus, a user
is able to determine if the system is powered-up by examining the
LED 48 disposed in the recessed opening 48 in the electrical
interface junction panel.
[0055] In addition to power and ground, each of the 4-pin RJ11
connectors 38, 40 and 42 further comprise a 2-conductor serial
signal path with pin No. 3 of each of the connectors identified to
a serial signal termed "CLK" and pin No. 2 of each of the
connectors identified to a serial signal termed "DATA". A first
4-pin RJ11 connector 38 is configured as a connector for supporting
various pieces of auxiliary equipment and its serial signal lines
are each identified as "AUX". The CLK and DATA signals comprising
pins 3 and 2, respectively, are identified as AUX CLK and AUX DATA
respectively. Likewise, the next 4-pin RJ11 connector 40 is
configured to provide serial CLK and DATA signals to the altitude
motor assembly 34 (alternatively a declination motor assembly) and
its CLK and DATA signal lines are thus denoted ALT CLK (Dec CLK)
and ALT DATA (Dec DATA) respectively. 4-pin RJ11 connector 42 is
configured to provide serial CLK and DATA signals to the azimuth
motor assembly 32 (alternatively a right ascension motor assembly)
and its CLK and DATA signals are referred to respectively as AZ CLK
(RA CLK) and AZ DATA (RA DATA).
[0056] Each of the respective CLK and DATA signals of each of the
respective 4-pin RJ11 connectors are electrically connected to a
corresponding CLK and DATA signal pin of the 8-pin RJ11 connector
44. Thus, the AZ CLK and AZ DATA signal pins of connector 42 are
coupled to pin 6 and 7, respectively of the 8-pin RJ11 connector.
ALT CLK and ALT DATA are connected to pins 4 and 5, respectively,
of connector 44 and AUX CLK and AUX DATA are connected,
respectively, to pins 2 and 3 of connector 44. The source of each
of these signals suitably comprises the hand-held control unit 36
which provides such signals over a flexible 8 conductor cable
terminating in a male 8-pin RJ11 connector suitable for mating with
the 8-pin connector 44 disposed on the electrical interface
junction panel 30.
[0057] Thus, it will be understood, that the electrical interface
junction panel 30 provides a means for routing power and control
signals between and among an external power source and a control
unit, a plurality of separately provided motor assemblies and
various optional auxiliary pieces of electronic equipment, such as
electronic focusers, electronic leveling means, a global
positioning system receiver, and the like, so long as the auxiliary
electronic equipment is configured to communicate over a 2
conductor signal bus supporting clock and data signals.
[0058] The interface panel 30 can be viewed as essential
distribution axis which enables interconnection between and among
the various components of the automated telescope system through
2-conductor serial bus connections. Each 2-conductor serial bus
carries packetized command and data signals on one wire and clock
signals on the other. Each serial bus is coupled between an
intelligent or semi-intelligent signal source, such as a system
control unit (36 of FIG. 2) and either an axial drive motor
assembly or an auxiliary apparatus. The 2-conductor serial cabling
between and among the different components of the system is an
important feature of the present invention, since it allows the
components to be interconnected using small, thin, flexible cabling
which is adapted for serial communication using a packet protocol.
Commands and data are passed from device-to-device in "bite sized"
packets which merely inform the receiving device of the commands
which the device is to execute. Large, thick, byte-wide cabling,
conventionally comprising a large number of conductors suitable for
both address and data bus requirements, are no longer required in
an intelligent telescope system according to the invention. Each of
the novel components are suitably sized and provided with a
suitable degree of intelligence so as to be quickly and simply
coupled together with flexible serial interface cables in order to
realize the benefits of the system as a whole.
[0059] It bears mentioning that the use of small, thin, flexible
serial interconnect cabling significantly reduces the inertial drag
on a system that would normally be present when using conventional
multiple conductor cabling. In addition, the use of small, thin,
flexible cables vastly reduces the spring tension that conventional
motor and cable systems would apply to a telescope mount.
[0060] Pertinent to practice of principles of the present invention
is the degree of intelligence which is provided to the motor
assembly comprising either the azimuth or altitude axis motor
assemblies 32 and 34 of FIG. 2. Referring now to FIGS. 4a and 4b,
the intelligence of either of the motor assemblies is implemented
in electronic circuitry 50 hosted on a printed circuit board which
is disposed within the motor assembly housing along with at least a
motor 52 and an optical encoder subsystem 54. The electronic
circuitry 50 communicates with the outside world over a serial
interface bus which is coupled to the circuitry through a 4-pin
connector 56. The connector 56 is adapted to be cable connected to
a control source through either the altitude motor RJ11 connector
40 or the azimuth motor RJ11 connector 42 as described in
connection with the interface panel 30 of FIGS. 3a and 3b. Power
and ground is taken from pins 1 and 4, respectively, of the
connector 56 and routed to a power supply distribution circuit 58
wherein battery power is filtered and regulated to a nominal
voltage level required by the circuitry, before being distributed
to the active components comprising the circuit package 50.
Additionally, the raw battery voltage is filtered and provided to
motor driver circuitry 51 as well as to the respective motor 52.
Power distribution circuit 58, thus is able to provide both
regulated low voltages appropriate for an electronic circuit, and
filtered high voltages suitable for motor applications. It should
be understood that while 12 Volts is preferred as a battery supply
voltage, the battery need not be limited thereto. So long as the
motor and its associated driver circuitry are capable of operating
at higher voltage levels, voltages as high as 16-18 Volts might be
used.
[0061] The CLK and DATA lines of the serial interface are connected
to respective inputs of a microprocessor 60 which functionally
controls operation of its associated motor 52 under firmware
program control. Microprocessor 60 is suitably implemented as an
8-bit microprocessor or controller, exemplified by the PIC16C54
microprocessor, manufactured and sold by Microchip Technology,
Inc., and functions to control both direction of motion and speed
of motion of its respective motor 52 by evaluating specific motor
motion commands against a feedback signal provided by an optical
encoder assembly 54.
[0062] Although the PIC16C54 is described as a microprocessor, it
is technically an 8-bit, fully static, EPROM/ROM-based CMOS
microcontroller employing a RISC architecture with 33 single
word/single cycle instructions. The PIC16C54 uses a Harvard
architecture in which program instructions and data are accessed on
separate buses, thus improving bandwidth over traditional von
Neumann architectures where program instructions and data are
fetched on the same bus. The PIC16C54 comprises a 512.times.12
instruction EPROM/ROM memory for hosting an operational program
instruction set and a 25 byte general purpose SRAM register file
memory. Separating the program and data memory allows instructions
to be sized differently than the 8-bit wide data byte. Instruction
opcodes are 12-bits wide making it possible to have all
instructions be single word-type instructions.
[0063] Conventionally, the PIC16C54 comprises three I/O ports, a
4-bit I/O register, termed port A and identified as pins A0 through
A3, an 8-bit I/O register termed port B and identified as pins B0
through B7, and an 8-bit I/O general purpose register termed port C
and identified as pins C0 through C7. All ports may be used for
both input and output operation. Each of the I/O pins are
tri-state, and can be programmed individually as either an input or
an output.
[0064] As depicted in FIG. 4b, serial CLK and DATA inputs are
directed to the bit-0 (A0) and bit-1 (A1) pins of the
microcontroller's A port, respectively. Further, the bit-2 (A2) and
bit-3 (A3) pins of the microcontroller 60 define the motor motion
control outputs and are directed to the motor driver circuit 51 and
thence to the circuit's associated motor 52 in order to define the
scope of motor movement and its direction. As will be described in
greater detail below, the I/O pins B0-B7 of port B of the
microcontroller 60 are programmed to receive feedback signals
provided by an optical encoder assembly 54 which are processed in
accordance with an application firmware program in order to define
encoder and, thus motor position. Clock input and output pins (OSC1
and OSC2, respectively) are connected to a crystal oscillator 61,
operating at four times the instruction cycle rate, or 20 MHz, and
which defines the timing reference signals for the microcontroller
60.
[0065] Commands are provided in serial fashion to the data input A1
of the microcontroller 60 in accordance with a packet communication
protocol, with each command packet comprising one or more bytes of
information and with each information byte being sequentially
clocked into the microprocessor 60, bit-by-bit, by a clock signal
provided to the microprocessor's CLK pin A0. As will be understood
by those familiar with the PIC16C45 I/O, data transmission is
bi-directional, while clock signals are commonly sourced by a bus
master device, such as a control unit, as will be described
presently.
[0066] Exemplary commands that are received and processed by the
microprocessor 60 include motor motion commands, more properly
termed "step rate" commands, by which the microcontroller is
instructed how fast, in which direction, and to what extent to move
its associated motor. Since each motor is feedback controlled,
feedback information, corresponding to actual motor movement, is
stored in an "error count" register, internal to the
microcontroller 60, whence it is available and may be read out to a
follow-on processor for evaluation. Further commands that may be
processed by the microcontroller 60 include commands for writing
error count data to the register and reading microcontroller status
information, including motor PWM count and the change in motor
position since the last status read operation.
[0067] Other commands that are supported by the particular
microcontroller 60 of the illustrated embodiment, include commands
related to various power saving features commonly implemented in
modern integrated circuits. In particular, a SLEEP command places
the microcontroller in a "sleep" mode that terminates when the
interface clock signal is next driven low. When in "sleep" mode,
the watchdog timer, if enabled, will be cleared and the device's
oscillator driver will be turned off. The I/O ports maintain the
status they were in before the SLEEP instruction was executed,
i.e., driving high, driving low, or hi-impedance (tri-state).
[0068] Upon receipt of a motor motion (or step rate) command,
indicating that the electronic circuitry 50 is to command motor
movement, operational firmware in the microcontroller 60 causes
appropriate PWM signals to be provided to its corresponding motor
driver circuitry and thence to the motor 52, at the appropriate
pulse rate and duty cycle. The motor 52 moves in response to its
motion command; the extent, direction and speed of which are
evaluated by an optical encoder system 54 which provides motor
positional feedback information in a closed-loop fashion.
[0069] In conventional, or classical, closed-loop control systems
used in connection with automated telescope control, one or more
position feedback sensors may be placed anywhere between the motor
shaft and the telescope focal plane. Once a position feedback
sensor is calibrated such that its output can be converted to an
apparent stellar position, the sensor will automatically correct,
through this calibration, for any systematic errors from the motor
shaft up to the position feedback sensor.
[0070] In the particular embodiment of the present invention, the
optical encoder assembly 54 comprises a disk 55 (best seen in FIG.
4a) about whose circumference a pattern of alternating transparent
and opaque slots are disposed which, when rotated through the path
of a light source and photodetector, are able to generate a series
of pulses. The optical encoder disk is coupled to the shaft of a
drive motor 52 in a manner as described in co-pending application
entitled INTELLIGENT MOTOR MODULE FOR TELESCOPE AXIAL ROTATION,
commonly owned by the Assignee of the present invention, the entire
disclosure of which is expressly incorporated herein by reference.
Since the motor 52 is coupled to its corresponding telescope axis
by means of gears (cog and worm) there is no need to take drive
train slippage into account as would be the case when using belts
or friction transfer clutches. Accordingly, the optical encoder
disk is able to be coupled directly to the motor shaft and still
provide position information with sufficient accuracy to enable
precise acquisition and tracking of stellar objects.
[0071] The optical encoder wheel 55 is disposed with respect to the
motor circuit's circuit board such that its alternating teeth (or
slots) are rotated through the path of a light source developed by
an LED diode 62 and a pair of bipolar photodetector transistors 63
and 64. A pair of photodetector transistors is used in the
illustrated embodiment of the invention in order to resolve
incremental motor shaft angular displacement in quadrature. Thus,
it will be understood that the encoder system according to the
present invention is an incremental encoder system, as opposed to
an absolute encoder system wherein the optical encoder disk
patterns are defined by either binary or Gray codes.
[0072] Pulses, for each incremental resolved motor shaft angle
step, are counted by the microcontroller 60 and the total encoder
count value, representing full motion of the telescope about the
axis, is evaluated against the movement extent command given to the
corresponding motor. Accordingly, it can be seen that if a
particular motor were commanded to rotate the telescope through
fifty one seconds of arc in a positive (upwardly) direction, the
microcontroller 60 is able to evaluate the optical encoder system
54 to determine that the motor did, indeed, move precisely that
amount, no more and no less. If the measured motor motion were
inconsistent with the commanded motor motion, the microcontroller
60 is able to calculate the direction and extent of a subsequent
motor command to move the motor (and thus the telescope) to its
desired position.
[0073] The operation of the encoder system 54 will now be described
in connection with the waveform diagrams of FIGS. 7a, 7b and 7c. In
addition, it will be evident to those having skill in the art that
the separation distance between the circumferentially disposed
teeth of the optical encoder wheel 55 is mapped to the linear
displacement distance separating the photodetector transistors 63
and 64, such that as the optical encoder wheel is rotated before
the photodetectors, each respective photodetector will define a
periodic output signal representing increasing and decreasing
brightness of a light source emitted by the LED diode 62. It should
be further noted that the periodic signals are 90 degrees
out-of-phase so as to define a signal in quadrature.
[0074] The most desirable signal characteristics, albeit not
realizable in the physical world, are depicted in the waveform
diagram of FIG. 7a. The output signal from each of the
photodetectors is illustrated as a squarewave with a 50% duty
cycle, with the output signal from photodetector No. 2 being 90
degrees behind the output signal from photodetector No. 1.
Evaluating both of the output signals in combination, it will be
evident that there are four separate combinations of values for the
signals, with the four combinations repeating in time in a periodic
fashion. The four possible combinations of signal values are:
on-off, on-on, off-on and off-off. Because the signal combinations
appear in a particular, predetermined pattern, the direction of
motion of the encoder wheel 55 and, thus, the motor, can be
determined by evaluating the development of the patterns. For
example, for a given on-off initial phase state, if the pattern
transitions to an on-on phase state, the motor is moving in a
forward direction. If the on-off phase state transitions to an
off-off phase state, the motor is moving in the opposite
(presumably) backward, direction. Further, each phase state
transition defines what is termed herein a "tick" and defines 1/4
of the angular rotation required to rotate the encoder wheel 55
from a first tooth to the next tooth (1 period).
[0075] The definition of "on" and "off" is predicated on a
photodetector output signal passing between two pre-set threshold
voltages. As seen in FIG. 7b, each photodetector output signal
defines a periodic waveform, which, in a manner to be described in
greater detail below, is adjusted to oscillate within a particular
voltage envelope. In accordance with practice of the invention,
each photodetector signal is defined to be in the "on" state when
its voltage excursion reaches and exceeds a 2.0 volt threshold
level. Each photodetector remains in the "on" state until its
signal level drops to a value of approximately 0.8 volts, whence
the photodetector output is deemed to switch from the "on" to the
"off" state. The photodetector remains in the "off" state until its
voltage value again reaches the 2.0 volt threshold level, whence it
switches to the "on" state. Accordingly, it can be seen that each
of the signals from the respective photodetectors define
alternating "on" periods and "off" periods so as to define
quadrature patterns.
[0076] In FIG. 7c, the periodic signals from the two photodetectors
of FIG. 7b, have been superposed, so as to define the quadrature
pattern: on-off, on-on, off-on and off-off.
[0077] Returning to FIG. 4b, the photodetector transistor 63 and 64
are preferably implemented as MPN transistors with their collector
terminals connected in common to V.sub.cc and their respective
emitter terminals coupled to I/O pins B0 and B1 of the
microcontroller 60. The microcontroller is thus able to count each
of the quadrature ticks and evaluate the quadrature pattern so as
to determine both motor speed and motor direction by evaluating
each photodetector's output. As regards motor movement commands,
the microcontroller 60 is configured to provide PWM signals to the
motor driver 51 which, in turn, supplies appropriate motor rotation
signals to its associated motor 52. The microcontroller 60 outputs
PWM signals (pulses) at a 150 pulse per second repetition rate and
determines actual motor speed by varying the duty cycle of each
pulse. For example, to run the motor at its maximum speed, the duty
cycle for each pulse would be set to approximately 99%, i.e.,
substantially always on, and the repetition rate set at the maximum
150 pulses per second rep rate. In contrast, were the
microcontroller 60 commanded to run the motor 52 at a sidereal
rate, the microcontroller 60 would issue PWM pulses to the motor
driver 51 having an approximately 2% duty cycle and at a
substantially slower repetition rate. In this regard, it should be
noted that when running at the sidereal rate, the PWM pulse rate
should equal or exceed approximately 45 pulses per second in order
that the resulting telescope motion not be apparently jerky to the
human eye. It has been established that step-wise motion at
repetition rates exceeding 45 repetitions per second appears smooth
and continuous to the human eye. Thus, PWM pulse rates should meet
or exceed this 45 pulse per second repetition rate and the motor
mechanical gearing system adjusted accordingly. Given the maximum
PWM pulse rate of 150 pulses per second, it will be understood that
the maximum pulse repetition rate defines a minimum time window
between like pulse transition edges of approximately 6
milliseconds. In order to determine motor speed, the
microcontroller 60 counts the number of "ticks" it receives from
the optical encoder system within the 6 millisecond timing window.
The microcontroller evaluates the number of ticks received in the
window against the number of ticks expected and, if the number of
ticks received is greater than or less than the number of ticks
expected, establishes an error count in an internal register. The
microcontroller then adjusts the motor pulse duty cycle in order to
slow-down or speed-up the motor in response to the magnitude and
sign of the error count. The resulting ticks are again compared to
a nominal established value, with excess ticks being added to the
error count register and the shortfall being subtracted therefrom.
The process continues until the error register is substantially
zeroed-out, meaning that the motor is now running at its expected
rate. In addition to evaluating motor speed, the microcontroller 60
further stores the number of "ticks" it has commanded the motor to
move during the entire motor movement operation in a separate
internal register. Thus, from the beginning of a motor movement
command to the end, the microcontroller maintains a record of the
total number of ticks the motor has moved through. This internal
register is available for periodic interrogation by a separate
control unit which, in a manner to be described further below, can
translate the tick count into telescope angular displacement about
an axis and, thus, the position vector of the telescope system.
[0078] In addition to commanding motor movement and evaluating
optical encoder feedback signals, the microcontroller 60 may
maintain the last-commanded motor motion in a data field defined in
RAM memory. This last-commanded motor motion (the delta from the
next-most previous motor motion command) is maintained in RAM and
is also available for access by a system controller by providing
the appropriate memory access command to the microcontroller 60.
Thus, the motor control electronics comprising the electronics
package 50 of the present invention can be seen to comprise means
for acquiring, storing and recalling motor position information of
its corresponding motor and, thus, the position of the telescope
with respect to the corresponding axis.
[0079] An additional feature of the motor control circuitry
comprising the electronics package 50 is its ability to
intelligently evaluate the correspondence between a motor movement
command and actual motor motion as read from the optical encoder
system 54. In particular, the microcontroller 60 includes firmware
that evaluates a motor PWM pulse against ticks received from the
optical encoder system 54 in order to determine that the motor is,
indeed, moving. A PWM threshold is set within the firmware such
that if the PWM threshold is reached without the microcontroller's
having received any corresponding motion ticks from the optical
encoder system, the motor is deemed "locked" or "burnt-out" and the
microcontroller ceases to issue any further motion commands until
reset. Thus, it will be seen that the circuitry comprising the
electronics package 50 includes means allowing for an intelligent
evaluation of motor PWM commands versus encoder movement response
metrics in order to determine possible motor lock or burn-out.
[0080] An additional feature implemented in the exemplary
electronics package 50 is an ability to adaptively tune the
brightness of the optical encoder LED diode 62 in order to provide
for optimal squareness and amplitude characteristics of the
photodetector signal received by the microcontroller 60.
Specifically, LED brightness is adaptively tuned by switching one
or more of five parallel-connected resistors into the LED current
path between V.sub.cc and a microcontroller input. Five resistors,
65a through 65f, are parallel-connected in common to the LED diode
62 at one end. The other end of each of the resistors, 65a-65f, are
connected to respective I/O pins (B2 through B7) comprising the B
port of the microcontroller 60. One or more of the resistors are
selectively incorporated into the LED circuit by selecting their
respective I/O pins as active.
[0081] LED brightness is considered optimized when a particular
photodetector output signal is evaluated as "on" approximately 50%
of the time and "off" approximately 50% of the time. This condition
is obtained when the amplitude of each photodetector signal is such
that it at least exceeds the 2.0 volt threshold and is not
sufficiently strong that it "bleeds" over the 0.8 volt "off"
threshold. In other words, if the signal amplitude is too low, the
photodetector is not able to "turn on". Conversely, if the signal
amplitude is too high, i.e., the signal is saturated, the
photodetector will not be able to "turn off".
[0082] LED brightness is optimized by a firmware routine that is
invoked during an initialization procedure when the telescope
system is started-up. Specifically, as depicted in the flow diagram
of FIG. 8, the microcontroller 60 first causes its associated motor
to spin-up and move at a pre-determined speed in a pre-determined
direction, for a pre-determined period of time. During this period,
the microcontroller 60 evaluates the output of a single one of the
photodetectors and determines the effective duty cycle of the
photodetector output signal.
[0083] If the perceived signal duty cycle was such that the
photodetector is "on" for a longer period of time than it is "off",
the microcontroller concludes that LED brightness is greater than a
desired, nominal value. In contrast, if the effective signal duty
cycle is such that the photodetector is "off" for a longer period
of time than it is "on", the microcontroller concludes that LED
brightness is lower than its desired, nominal value. In response,
resistors 65a through 65f are selectively enabled into the LED
circuit. Following each resistor reconfiguration, the
microcontroller again evaluates the effective duty cycle of
photodetector signal until the effective duty cycle reaches the
desired 50% point. Once the desired LED brightness characteristic
has been achieved, the microcontroller 60 reviews the register
state corresponding to the B2 through B7 inputs. The register state
for each pin will have a particular value depending on whether the
I/O for that pin is active, inactive or tri-state. The register
state defining the pin activation configurations required to return
the necessary detector output characteristics is passed, as an
initialization I/O configuration value to an external system
controller where it is stored in non-volatile memory for future
reference. Alternatively, the I/O configuration of the
microcontroller required to return the necessary detector output
characteristics might be saved into the microcontroller's REM
memory as an I/O configuration value from where it might be
retrieved upon interrogation by an external system controller.
Regardless of how saved and where it eventually resides, the I/O
configuration value is available to be passed to the motor
microcontroller each time the telescope system is initialized. The
I/O configuration value need only be obtained once, when the
telescope system is first set up for use. The I/O configuration
may, however, be reobtained and/or recalculated upon a user's
initiative, in order to account for the gradual roll-off in LED
output strength over long periods of time. This would be useful to
observers who use their telescope systems on an almost continuous
basis and who require the greatest precision in automatic motor
control performance.
[0084] Thus, it will be understood that the microcontroller 60, in
combination with resistors 65a through 65f, the LED diode 62 and
photodetector transistors 63 and 64, comprise means for adaptively
tunning LED brightness characteristics in order to obtain optimal
photodetector output signal squareness and amplitude
characteristics. Optimal output signal characteristics are an
important feature of the present invention since it enables motor
speed and direction evaluations to be made with a significantly
greater degree of precision and accuracy than with conventional
systems.
[0085] One particular embodiment of a hand-held control unit
suitable for use in combination with a semi-intelligent motor
assembly is depicted in FIGS. 5a and 5b. FIG. 5a is a front view of
the exterior portion of a semi-intelligent drive motor motion
control unit 70 illustrating the various function keys that might
be used by a user of the telescope system in order to command a
telescope to move through various evolutions. The motion control
unit 70 comprises a hand-held, self-contained, computer control
unit, enclosed within a functional housing. The motion control unit
is operational as a dual-axis motor drive corrector which enables
telescope axis motor motion, from the very small tracking
corrections necessary for long exposure astrophotography at
sidereal rates to the very fast slewing movements required for new
object acquisition. The motion control unit supports motor movement
commands for microslewing a telescope to, and for precision
centering of a telescope onto, selected celestial objects. In
addition, the motion control unit 70 is able to command certain
special movement functions such as selecting various drive rates
for the telescope motors, adjusting an optional electronic focuser,
and the like.
[0086] Direction keys 71, labeled with directional arrows
indicating movement directions (up, down, left and right) enable a
telescope system to move, or microslew, in the specified direction
at any one of a plurality of allowable, settable speeds. A speed
key 72 is used to change a speed at which the telescope system is
moved by depressing the key at the same time that one of the
direction keys is being depressed. As was described previously, the
number of allowable speeds which can be commanded to a
semi-intelligent motor assembly according to the invention, is
limited only by the number of speed bits comprising the speed and
direction command. In the particular embodiment being described,
the number of settable speeds that can be commanded to the
semi-intelligent motor assembly is arbitrarily limited to four. At
this juncture, it is important to mention that these settable
speeds refer to telescope movement commanded by an observer that
interrupts nominal telescope tracking motions, conducted at the
well understood sidereal rate.
[0087] The four speeds selected for implementation in the
illustrated embodiment range from the top speed of telescope
motion, to a speed slightly in excess of the sidereal rate. The top
speed corresponds to telescope displacement of from about 4 degrees
to about 9 degrees per second. Top speed is particularly useful for
stewing the telescope to the vicinity of new object which an
observer desires to acquire. A second speed corresponds to about
0.75 degrees per second of telescope motion and is useful for
centering a selected object in a wide-field eyepiece. A third speed
corresponds to about 32 multiplied by the sidereal rate (about 8'
of arc per second) and is useful for centering a selected object in
a high-power eyepiece. The slowest settable speed is about 4.times.
the sidereal rate (about 30' of arc per second and is typically
used for precision centering and for guiding the telescope system
during astrophotography.
[0088] Each of the individually selectable speeds are associated
with a corresponding speed indicator LED which illuminates when
that particular speed has been selected. For example, a first LED
74 illuminates when the selected speed is the top, a second LED 76
illuminates when the selected speed is the 0.75 degrees per second
rate, the third LED 78 illuminates when the selected speed is
32.times. the sidereal rate and the fourth LED 80 illuminates when
the selected speed is 4.times. the sidereal rate. Thus, the
currently selected speed is indicated by the speed indicator LED
proximate the speed key 72 and depressing the speed key 72
increments the selected speed to the next speed, illuminating the
appropriate speed indicator LED.
[0089] Focus control keys 82 and 84 are provided to enable the
motion control unit 70 to control the operation of an optional
electronic focuser which may be coupled to the focusing ring of a
telescope view finder. Images appearing in the view finder may be
focused by depressing the in 82 or out 84 focus keys, causing a
"DIRECTION AND MOVE" command to be issued to an auxiliary focusing
device over an auxiliary bus system, in a manner to be described in
greater detail below.
[0090] A "mode" key 86 may be used to define certain special
function operations, such as tracking rate changes, direction
reversal, mount configuration identification, and the like. For
each mode function capable of definition by the system, the LED
bank indicates which of the chosen mode functions are operative at
any given time. For example, when power is first applied to the
motor control unit, all four LEDs are caused to blink rapidly,
indicating the unit is ready for operation. Depressing any key on
the housing causes the first LED 74 to become steady, while the
remaining LEDs turn off.
[0091] In order to select mount configuration (Alt-Az or
equatorial), the user depresses and holds the mode key 86 until
both the first and second LEDs 74 and 76 burn steady, while the
third and fourth LEDs 78 and 80 return to blinking. This action
places the motor control unit in Alt-Az mode. To set the system
into equatorial mode, the speed key 72 is depressed -once for
Southern Hemisphere operation, and twice for Northern Hemisphere
operation. Depressing the speed key a third time returns the system
to Alt-Az mode. Following the mount configuration mode choice, the
user depresses the mode key 86 until only the first LED 74 is lit.
The unit then exits the mode function and activates the direction
keys. If equatorial mode was chosen, the drive motors are now set
to track objects at the sidereal rate.
[0092] The tracking rate of a telescope system may also be changed,
in 0.5% increments from the default sidereal rate, by accessing a
tracking speed mode function through the mode key 86. To do so, a
user depresses the mode key until the mode function shows active on
the LED bank (LEDs 74 and 76 "on" steady, LEDs 78 and 80 indicating
the tracking mode last chosen). Depressing the "in" key 82 causes
the tracking rate to increase by 0.5% and causes the fourth LED 80
to burn steady. Depressing the "out" key 84 causes the tracking
rate to decrease by 0.5%. The third LED 78 is caused to burn steady
to so indicate. In order to exit the tracking rate change mode, the
mode key 86 is again depressed, which returns the telescope to
normal operation.
[0093] The internal construction of the semi-intelligent drive
motor motion control unit 70 is illustrated in the schematic
diagram of FIG. 4b. As can be seen, the operational focus of the
motion control unit 70 is an EPROM/ROM based 8-bit microcontroller
88 exemplified by the PIC16C54, manufactured and sold by Microchip
Technology, Inc. The function keys described above in connection
with FIG. 5a, provide inputs to the microcontroller 88 which, in
response, develops control output signals which are directed to an
8-pin output header 90 having a pin configuration which corresponds
to the 8-pin RJ11 connector (44 of FIG. 3b) of the electrical
interface junction panel, to which the motion control unit 70 is
intended to be connected. In response to the various direction,
speed, focus and mode commands input to the microcontroller 88, the
microcontroller develops and outputs control signals for the
altitude motor (ALT CLK and ALT DATA), the azimuth motor (AZ CLK
and AZ DATA), and a control signal pair for the auxiliary bus (AUX
CLK and AUX DATA). Movement, speed, focus and mode commands are
received by the microcontroller 88 and appropriate output control
signals are developed thereby in accordance with a software or
firmware program hosted by the microcontroller 88 and
conventionally stored in an internal memory space such as a
programmable ROM memory.
[0094] In addition to direction, speed, focus and mode commands,
microcontroller 88 is adapted to differentiate between Northern and
Southern hemisphere operations and between equatorial/Alt-Az
tracking modes. A pair of jumpers are provided, with the first
jumper 92 differentiating between Northern and Southern hemisphere
operations by its presence or absence, respectively. Southern
hemisphere operation is defined by the presence of a jumper in the
first jumper position 92 which completes the electrical short and
asserts an I/O active state on both the RTCC and B6 inputs. For
Northern hemisphere operations, the jumper is absent from the first
jumper position 92 putting the RTCC input in an I/O inactive
state.
[0095] Likewise, equatorial and Alt-Az operational modes are
differentiated by the presence or absence of a jumper in the second
jumper position 94, respectively. Alt-Az mode is defined by
shorting the jumper position and thereby asserting an I/O active
state on the RTCC and RBC inputs. Equatorial mode is indicated by
an I/O inactive state on RTCC while the B7 input remains
active.
[0096] With regard to communication between microcontroller 88 of
the control unit and the microcontroller 60 of the semi-intelligent
motor assembly, commands are provided in serial -fashion to the
semi-intelligent motor assembly in accordance with a packet
communication protocol, wherein each command packet comprises one
or more bytes of information and with each information byte being
sequentially clocked into the receiving microcontroller,
bit-by-bit, by a serial clock signal. In accordance with practice
of principles of the invention, each semi-intelligent motor
assembly is directly coupled to the control unit's microcontroller
88 via a two-wire serial interface connection through the control
unit's header 90 and, thence to appropriate I/O pins of the
microcontroller 88. Thus, information being communicated between a
control unit and a motor assembly need not be preceded with header
information. However, since the auxiliary serial interface is able
to host a multiplicity of auxiliary apparatus, information being
communicated between a control unit's microcontroller 88 and a
particular piece of auxiliary apparatus needs to be preceded by an
address header in order to identify the information's intended
recipient.
[0097] With regard to motor motion commands, these commands are
issued directly to the motor assembly's microcontroller over the
corresponding two-wire serial interface. Motor motion commands,
more correctly termed step rate commands, are identified, in
hexadecimal, as (00 h) and comprise three bytes of information. The
step rate is defined as the number of steps or "ticks" that occur
approximately every 6 milliseconds. The format is a two's
compliment number with the first number representing the whole
steps or "ticks" and the next two bytes representing the fractional
portion thereof. Each step rate command includes a sign (..+-..)
which determines the direction of motor motion.
[0098] A second step rate command, denoted (01 h) in hexadecimal is
formatted substantially identically with the (00) command but is
used for step rates greater than the 2.times. the sidereal rate.
Additional information communicated between the control unit
microcontroller and the motor assembly microcontroller include a
"change error count" command (02 h) which commands a one time
change of the motor microcontroller error count register. A "set
LED position" (03 h) command sends out the I/O configuration byte
which has been stored for that particular motor assembly in order
to optimize its photodetector performance. A "find LED position"
(04 h) command is issued to the motor assembly when it is desired
that the motor assembly finds the best LED current in order to
optimize photo detector performance. A "get LED position" (09 h)
command instructs the motor assembly to write out the I/O
configuration byte that corresponds to optimized photo detector
performance.
[0099] Additional commands, such as "turn on motor in positive
direction" (06 h) and "turn on motor in negative direction" (07 h)
are also provided by the control unit to the motor assembly's
microcontroller. A "status" (08 h) command is read from the motor
assembly's microcontroller the "status" command is typically 3
bytes in length and further includes an additional flag bit. The
first two bytes of information comprise the determined change in
motor position since the last status read. The next byte comprises
the PWM pulse count which is used to determine whether or not the
motor is in a stall condition. The final bit, the flag bit, an
illegal encoder flag which indicates that an encoder "tick" was
missed during the current motor position change. This bit is
typically reset after a data read, as is the determined motor
position information.
[0100] Those familiar with the internal construction and
operational programming of a PIC16C5X series microcontroller will
be able to routinely develop additional applications and command
sets suitable for, for example, controlling LED operation,
developing a digital clock, or controlling a keypad. All that is
required in practice of principles of the invention, is that the
control unit microcontroller be able to communicate with one or
more motor assemblies so as to command, at least, motor speed and
direction changes which the motor assembly executes without further
intervention on the part of the control unit. This distribution of
intelligence allows both the motor assembly and the control unit to
be implemented using relatively simple components, with each
respective apparatus being responsible for a particular set of
functions; the control unit translating keypad input into motor
motion commands, the motor assembly receiving the motor motion
commands and causing the required amount of telescope motion about
its axis. Commands and status information are communicated between
the control unit and the motor assembly via a two-wire serial
interface in accordance with a packet communication protocol. The
control unit is able to determine that its commands have been
appropriately executed by evaluating returned status information
from the motor assembly. Appropriate telescope motion in response
to a motor movement command is ensured by evaluating feedback
signals developed by an optical encoder system mechanically coupled
to the motor and electronically evaluated by the motor assembly's
microcontroller unit.
[0101] Thus, in accordance with the invention, the hand-held
control unit and motor assembly, in combination, suitably provide
means for distributing motor control intelligence, with the
intelligence partitioned into first and second portions, the first
portion responsive to user input and for translating that input
into suitable command signals, the second portion responsive to the
command signals and translating the command signals into signals
suitable for use by a motor driver circuit in effecting motor
motion. The two portions of the system's distributed intelligence
are coupled together over a two-wire serial interface allowing
bidirectional communication of data and command signals between the
two portions over a thin, flexible cable.
[0102] An additional embodiment of a hand-held control unit
suitable for intelligent control of a telescope system according to
the invention, is illustrated in FIGS. 6a and 6b. FIG. 6a depicts
the exterior of an intelligent telescope system controller as it
would appear to a system user, while FIG. 6b illustrates, in
semi-schematic block diagram form, configuration of the electronic
system components which provide functionality to the controller
100.
[0103] FIG. 6a is a front view of the exterior portion of an
intelligent telescope system controller 100 illustrating the
various function keys that are used by a user of the telescope
system in order to command a telescope to move through various
evolutions. The intelligent controller 100 comprises a hand-held
package which functions as a full-spectrum control unit capable of
intelligently defining and commanding motor movements required for
astronomical observations, as well as for implementing various pre
and post processing features in a manner similar to a
microcomputer.
[0104] The intelligent controller 100 suitably comprises an LCD
display screen 102, capable of displaying text, numeric and graphic
output data that might be consulted by a user in operating the
telescope system. All prompts, user queries, confirmation messages,
and the like, are displayed on the LCD screen 102. Telescope motion
direction keys 112, labeled with directional arrows, indicating up,
down, right and left, provide the necessary inputs for enabling the
telescope system to move, or microslew, in the specified direction,
at any one of a number of allowable, settable speeds. As was
described previously, the number of allowable speeds which can be
commanded to the semi-intelligent motor assembly according to the
invention, is limited only by the number of speed bits comprising
the speed and direction command. In the particular embodiment being
described, the number of allowable speeds that can be commanded to
the semi-intelligent motor assembly is 8, with one of the 8
allowable speeds being reserved for the motor stop command. Motor
speed changes are effected by entering numerical values on a
numeric keypad 104. To change or define a particular motor speed, a
user presses and releases the desired numeric key corresponding to
the desired speed range (1 being the slowest, 9 being the fastest).
Once the desired speed is selected, the desired motion direction
key 112 is depressed and the system commands the corresponding
semi-intelligent motor assembly to move the telescope system at the
desired speed, in the desired direction.
[0105] Scroll keys 106 and 108 are provided in order that a user
may scroll through a data base listing or through available menu
options that might be shown on the LCD display screen 102. A "?"
key 110, disposed between the scroll keys 106 and 108, accesses an
internal "help" file and, when depressed, causes the LCD screen 102
to display a brief description of the selected menu item on the
first line of the display. An enter key 113 selects a file menu or
option, or is used to define the completion of an entry made in
response to a system prompt. A mode key 114 allows a user to exit a
current menu to return to a previous menu and a go-to key 115
commands the telescope system to slew the telescope to an object
chosen from an internal celestial object data base listing, for
example.
[0106] The internal construction of the intelligent telescope
system controller 100 is illustrated in the schematic diagram of
FIG. 6b. As can be seen from the figure, the intelligent
controller, indicated generally at 100, suitably comprises a dual
processor system, with the dual processing functions implemented by
a first, general purpose microprocessor 121 exemplified by the
68HC11, a member of 68HCxx family of microprocessors manufactured
and sold by Motorola, and a second, purpose configured
microprocessor or microcontroller 122, exemplified by the PIC16C57
microcontroller manufactured and sold by Microchip Technology,
Inc.
[0107] The general purpose microprocessor 121 is coupled to a
16-bit address and data bus (AD[0,15]) and an 8-bit data bus
(D[0,7]), which allow the microprocessor 121 to communicate with a
programmable read-only memory (ROM) memory circuit 124 and a random
access memory (RAM) 126. Further, the four most significant bits of
the data bus (D[4,7]) are coupled to the system's LCD display
driver circuit 127 to provide an interface between the
microprocessor 121 and the system's LCD display 120. As will be
described in greater detail below, the microprocessor 121 is
responsible for implementing the top-level firmware architecture of
the system according to the invention and for executing loadable
application software routines pertinent to the exemplary
intelligent telescope system.
[0108] Programmable read-only-memory circuit 124 is preferably
implemented as a FLASH programmable ROM and is provided in order to
host the instruction set for downloaded applications and software
routines, data tables such as a stellar object position data base,
the Messier object catalog list, an earth-based latitude/longitude
correspondence table, and the like. Although described as an FPROM,
the ROM memory may be implemented as an EEPROM, or any other type
of programmable non-volatile memory element. Indeed, the ROM 124
might be implemented as an external mass storage unit, such as a
hard disk drive, a programmable CD-ROM, and the like. All that is
required, is that the memory 124 be able to be written to, in order
that its hosted data bases and tables may be updated, and be
non-volatile, in order that its hosted data bases and tables be
available to the system upon boot-up or power-on-reset.
[0109] Microprocessor 121 is further coupled via a 2-bit
serial-type control bus 123 to the microcontroller 122 which, in
turn, is coupled via a multiplicity of interface signal lines to
the various function keys (indicated generally at 132) which
comprise the operator/system interface for this system. In this
respect, the microcontroller 122 functions as the system I/O and
interface controller which translates user input taken from the
keypad, and provides command and control signals, derived from the
user input, to the system microprocessor over the serial interface
123. The serial, interface bus 123 is further comprised of two
signal lines, CLK and DATA, which function much the same as the
2-wire serial interfaces between a motor assembly and the
particular embodiment of a control unit described in connection
with FIG. 5b. The interface bus 123 is bi-directional and command
and data signals are communicated in accordance with a packet
transmission protocol.
[0110] The system microprocessor 121 is further coupled to RS-232
interface port circuitry 128 via an additional 2-wire (supporting
conventional Tx and Rx signal lines) serial bi-directional
interface bus 133. The RS-232 port circuitry 128 is in turn coupled
to an RS-232 interface connector 129, through which bi-directional
communication between the microprocessor 121 and external
information sources such as a personal computer (PC), a World Wide
Web interface link, and the like, may be effected. Indeed, the
RS-232 port 128 may be configured to communicate with a similar
RS-232 port comprising another, separate intelligent controller
system operating in connection with another, separate telescope
system. It will be understood that, when operating under
appropriate I/O control application firmware, the microprocessor
121 in combination with the RS-232 port 128 provides means for
quickly and easily interfacing the system to an external source of
programming code, data or other information that a user might
desire to incorporate into the operating instructions or data
tables comprising the intelligent controller of the present
invention.
[0111] Likewise, the microcontroller 122 is coupled to a bundled
serial interface connector 130, suitably comprising an 8-pin
RJ11-type interface suitable for connection to the 8-pin receptacle
(44 of FIGS. 3a and 3b) of the electrical interface panel (30 of
FIGS. 3a and 3b). The serial interface connector is configured to
support communication between the microcontroller 122 and two
telescope axis drive motor assemblies along with a plurality of
auxiliary devices, over respective 2-wire serial interface busses.
So configured, the PIC16C57 microcontroller 122 will be understood
as interfacing between the user I/O interface keys 132 and the 68
HC 11 microprocessor 121, to generate command and control signals
suitable for use by a semi-intelligent motor assembly and/or an
auxiliary device, such as an electronic focusing system, and
provide such command and control signals to the serial electrical
interface panel (30 of FIGS. 3a and 3b) for routing to their
appropriate destination. A crystal oscillator circuit 135 is
further coupled between the microcontroller's clock inputs (OSC1
and OSC2) and provides an 8 Mhz operational clock signal to the
microcontroller 122.
[0112] Power is also received, from an external power supply,
through the serial interface connector 130. The power and ground
pins are coupled to a power supply circuit 134. The supply circuit
134 is preferably implemented as a voltage regulator and functions
to condition a 12 Volt (for example) supply input to the reduced
voltage levels required by modern integrated circuits. A pertinent
consideration given to the power supply circuit 134 is its need to
provide suitable supply voltages and currents for a plurality of
LEDs which populate the system 100. In particular, the LCD display
120 is backlit by an arrangement of LEDs which are configured in a
circuit 136 and disposed about the display screen in a novel
fashion to provide uniform illumination of the entire surface of
the display screen. Operation of the LED circuit 136 is controlled
by the microcontroller 122, and its configuration will be described
in detail below.
[0113] In accordance with the present invention, the 68 HC 11
microprocessor 121 performs the high level application software
execution tasks and the associated data handling and numerical
processing, in order to define the appropriate motion commands to
be provided to the PIC16C57 microcontroller 122. The
microcontroller 122 receives motion command inputs from either the
microprocessor 121 or the user interface keys over interface bus
123 and suitably processes the received motion commands into
command and control signals suitable for use by a motion control
processor.
[0114] To complete the system, and to give the microprocessor 121
some means of performing time calculations appropriate to celestial
motion, a real time clock 138 is provided and is coupled to a clock
input of the microprocessor 121, as well as being coupled to a
clock input of the microcontroller 122. The real time clock 138 is
preferably implemented as a precision timing reference clock signal
generator, such as a UTC clock, that is used by the microprocessor
121 to calculate sidereal time intervals and preferably resides as
an integral component of the control unit 100. Alternatively, the
clock 138 might be implemented as a separate, off-board integrated
circuit comprising a conventional UTC clock which communicates with
the system over the RS-232 interface, or an on-board UTC clock and
follow-on circuitry for converting UTC time intervals to sidereal
time intervals prior to providing a timing reference signal to the
microprocessor 121.
[0115] Thus, it should be understood that the intelligent telescope
system controller 100 suitably comprises a means for adding full
intelligence to a telescope system which includes semi-intelligent
motor assemblies in accordance with the present invention. The
intelligent telescope system controller performs this function by
bifurcating the system's processing and control functions into a
first, sub-system comprising a microprocessor operative for system
data processing, and a second, microcontroller system for
implementing I/O control. System intelligence is maintained
up-to-date, by allowing "new object" roadability through an RS-232
port. System software, updated celestial object catalog tables, and
the like, may be loaded into the system through the RS-232 port
from a PC, an attached disk or diskette drives, a web site, a
separate intelligent telescope system controller in accordance with
the invention, and the like.
[0116] In particular, a user may "clone" his system's application
programs and his system's database contents into another user's
system using the RS-232 port to effect bidirectional communication.
Alternatively, the user may receive program and data information
from a second intelligent telescope system controller, thus
"cloning" that controller into his own, over the RS-232 interface.
The "clone" function is implemented by accessing the various user
interface keys provided on the exterior of the controller 100. For
example, the user might depress the mode key 114 until a system I/O
menu appears in the controller's LCD display. The user might then
scroll through the menu using the scroll keys 106 and 108 until a
"clone" menu option appears in the screen. If suitable connections
are made between two intelligent system controllers according to
the invention, and if the appropriate input and output states are
set for each controller (the controller being cloned outputs data),
the user might depress the enter key 113, initiating the
process.
[0117] Several other system utilities are supported by the
microprocessor 121 of the intelligent telescope system controller
according to the invention. For example, the system may be placed
in a state of suspension by invoking one of two, reduced
functionality, modes termed "sleep mode" and "park mode". Since, as
was described above, the system and timing reference is preferably
a crystal controlled clock 130 coupled to the microprocessor 121,
an external time-of-day input is required in order that the system
can correctly calculate the system's local hour angle and, thus,
the celestial sphere's rotational state with respect to a specific
observer. When the system is placed in "park mode", all system
orientation parameters (to be described subsequently) are saved in
the buffer/scratch pad RAM 126, from whence they may be recalled
when a user desires to perform additional observations. Once the
system is oriented and has been placed in "park mode" all that is
required is that-the user input a time-of-day datum for the
telescope system to precisely know (or, more correctly, remember)
its orientation with respect to the sky.
[0118] In "sleep mode" the system again remembers its orientation
parameters, but maintains the clock 138 in an operative condition
while reducing power to the remaining system components to
maintenance levels. Thus, in "sleep mode", the system is ready to
"wake up" at any time the user gives it an operation command.
[0119] Beyond support of system utilities, the intelligent
telescope system controller is also able to support a multiplicity
of auxiliary devices that might be coupled to the telescope system
in order to enhance its capabilities. Pertinent such devices
include an automatic focusing unit, a clock and date module, a
speech recognition module and an associated audio output module, an
automatic alignment tool(tube leveler and/or axis planarizer), a
global positioning system (G.P.S.) module, a photometer, an
autoguider, a reticle illuminator, a cartridge reader station (for
courseware, new revisions, new languages, object libraries, data
storage) and the like. Each auxiliary device is coupled to the
system, in daisy-chain fashion, over the AUX DATA and AUX CLK
signal lines comprising a serial auxiliary bus system. As was the
case for the Alt (Dec) and Az (RA) serial busses coupled between
the controller and the motor assemblies, the auxiliary bus is a
2-wire serial communication interface and further includes a supply
voltage line, supplying 6-18 and preferably 12 Volts of power, and
a ground potential line.
[0120] The 2-wire interface comprises a bidirectional data line
which supports data communication using a packet transmission
protocol, and a clock line which supports a clock signal typically
sourced by the bus master, in this case, the system controller.
Because the auxiliary devices are daisy-chain configured, each
device is provided with a unique bus address so that commands can
be efficiently processed by the particular device being accessed.
In accordance with the present invention, bus addresses are
expressed as a binary numerical value defining an address byte.
Thus, the system is able to communicate with up to 256 separate
addresses and, therefore, 256 separate devices. However, as will be
explained below, one address, the "byte zero" address, is reserved
as a broadcast address, indicating that the following command or
commands are to be executed by all devices coupled to the bus.
[0121] All communication transactions over the auxiliary interface
bus are performed in accord with a packet transmission protocol.
All bus activity begins with a bus master (typically the system
controller) initiating a communication packet to a selected target
device. Once the master-to-target communication is completed, the
target device returns a message or status communication packet back
to the bus master. As illustrated in the simplified interface
protocol packet content diagram of FIG. 12, all packets begin with
"count byte" which defines the number of bytes comprising that
particular initiating or response packet. In the case of an
initiating packet, the second byte comprises the "address byte" for
the particular target device which will execute the command, and is
followed by a "command byte" which defines the operation to be
carried out. "Intermediate bytes", unique to each device, follow
the "command byte" in the case of an initiating packet, or the
"count byte" in the case of a response packet. A "last byte" is
also unique to each device and is the final byte of an initiating
packet transmitted by the master. Optionally, a target device may
be configured to transmit a "last byte" as the final byte of a
response packet.
[0122] The clock signal is driven by the bus master for all
information transfers, regardless of the direction of data flow. In
addition, the bus master may temporarily relinquish control of the
bus and designate a particular device to temporarily assume the bus
master role in third-party data transfer operations, such as
between a CCD imager and a disk drive. All auxiliary devices are
"I/O hot" in that all devices are constantly "snooping" the bus and
can evaluate all packets transmitted thereon. Once a device
determines that a packet header contains its address, the rest of
the packet is clocked into its I/O registers and the command is
then executed.
[0123] Certain broadcast commands are common to all auxiliary
devices and are identified by a "broadcast address", indicating
that all devices coupled to the bus are to execute the following
command. Exemplary broadcast commands include a "bus reset" command
which is used to perform a soft reset of the bus and the "sleep"
command which places each device in its own particular low-power
mode. An "inquiry" command is not specifically a broadcast command,
but is nevertheless directed to all devices on the bus; albeit
sequentially. The "inquiry" command is used to determine the
presence of a device on the bus. The initiating packets cycle
through the bus addresses, with devices populating the bus
returning a status byte identifying the device revision number or
module type, as their addresses are received.
[0124] The full spectrum of auxiliary device command sets can be
easily implemented in the intelligent system controller (100 of
FIGS. 6a and 6b) because of the capability range of its
microprocessor (121 of FIG. 6b). It will be understood, that the
full spectrum command set may be incorporated in the microprocessor
by a reasonably proficient programmer making the intelligent system
controller 100 capable of supporting the full spectrum of auxiliary
devices. A reduced set of auxiliary device command sets are
implemented in the semi-intelligent system controller (70 of FIGS.
5a and 5b) because of the relatively limited capabilities of its
microcontroller 88, with respect to the capabilities of the fully
intelligent system. Thus, only certain auxiliary devices are
supported, such as an electronic focusing unit, in the
semi-intelligent configuration, while the capacity for upgrading
the system to a fully intelligent configuration remains unimpaired.
Indeed, the serial auxiliary interface bus provides a particular
enabling feature for system upgrade capability by virtue of its
simplicity and the inherent expandability of the 2-wire serial bus
concept. Adding capability to the telescope system of the
invention, is as uncomplicated as merely coupling additional
devices to the bus. The bus, then, provides the framework within
which intelligence and capability are added, subtracted or modified
on a piece-by-piece basis.
[0125] Each component coupled to the system comprises its own
operational intelligence and requires only a serial command
interface with a controlling entity to perform its designated
function. Since each component comprises sufficient intelligence
(processing power) to execute its tasks without higher level
supervision, the controlling entity is free to execute application
programs, perform complex arithmetic calculations, maintain
database entries, and the like.
[0126] Primary control of an automated telescope system with
distributed intelligence, in accordance with the present invention,
is provided by a fully intelligent telescope system controller 100.
Substantially all functions of an automated telescope system can be
implemented through the keypad portion of the controller 100 by
depressing the various alpha, numeric and function keys provided
thereon. Once the automated telescope system has been appropriately
aligned, as will be described in greater detail below, an object
menu library, stored in a dedicated memory space provided in the
controller, is used to automatically slew the telescope system to
any particular celestial (or terrestrial) object an observer
desires to view or photograph. However, prior to beginning an
observation and, indeed, during initial setup of the system, a user
must first initialize the system by entering certain information in
accordance with an initialization, or setup, procedure which can be
best understood with reference to the initialization procedure flow
chart of FIG. 8.
[0127] After each of the individual components comprising the
telescope system are connected together through the electronic
interface junction panel (30 of FIG. 2), the intelligent system
controller 100 is plugged into the control unit port (44 of FIGS.
3a and 3b) and power is provided to the system. Following
"power-on-reset", a warning message is displayed on the LCD screen
102 of the system controller 100, warning the user not to look
directly at the sun through the telescope. The warning remains on
the LCD screen 102 for a period of a few seconds following which
the system controller prompts the user to enter the current date,
by entering the appropriate figures in a formatted date field. An
exemplary date field might appear as "Jan. 1, 1999". Numeric
values, such as the date and year are entered by pressing the
corresponding numeric keys of the numeric keypad 104 when prompted
to do so by the system. The current month is entered by scrolling
through a list of months using the up 106 and down 108 arrow keys
provided for that purpose. In particular, the date cursor
automatically jumps to the next space once a particular numeric
value is entered. If a mistake is made during entry, the right or
left directional keys may be depressed in order to move the cursor
backward or forward until it is positioned over the incorrect
entry. The correct entry may then be made by depressing the
appropriate numeric key on the numeric keypad 104.
[0128] The numeric keys are used to enter the current day. Then,
the up 106 and down 108 scroll keys are used to cycle through the
list of months. When the current month is displayed the right arrow
key causes the cursor to move to the year field into which the
current year is entered using the numeric keys 104. After all of
the date information has been correctly entered, a user depresses
the enter key 113 in order to inform the system that the current
date has been entered and the date setting procedure is now
concluded.
[0129] The system then prompts the user to enter the current time.
It should be noted that the system-is operative in a 24-hour mode
and, therefore, time should be entered using a 24-hour clock (i.e.,
9:00 pm is entered as 21:00). As was the case with the date entry,
a user depresses the enter key 113 in order to inform the system
that the time entry procedure has been concluded. It is worth
mentioning, at this point, that a user should enter a time just
slightly ahead of the current time prior to depressing the enter
key. The enter key is depressed at the exact moment the current
time matches the time the user entered. This procedure is very
useful in enhancing the precision of the positioning calculations
undertaken by the system, by giving the system a more precise
indication of the correct time. Needless to say, the more precise
the time indication provided to the system, the better the system
will be able to locate objects on the basis of their published
right ascensions and the better the system will be able to
accurately position the telescope to view them.
[0130] At this point, the positioning keys 112 of the system
controller 100 are activated such that they may be used to move the
telescope. A user is able to either immediately proceed to using
the telescope without further initialization data entry, or
continue with data entry in order to enable additional features of
the inventive system. If a user chooses to continue with
initialization, a next procedure displays the status of a daylight
savings time feature. Daylight savings time is in effect from the
first Sunday in April through the last Sunday in October in most
areas of the United States and Canada. Users are cautioned to
investigate as to whether their geographic local time conforms to
daylight savings time or not. The display status is in a "negative
default" condition indicating that the daylight savings time
feature is not enabled. If a user is currently in daylight savings
time, the enter 113 key is depressed once which causes the display
indication to change from NO to YES. When the desired setting is
displayed on the screen, the mode 114 key is depressed indicating
that the daylight savings time procedure is concluded.
[0131] A next sequence of data entry options enables a particularly
novel orientation feature of the present invention, wherein an
observer's latitude and longitude are approximated by the latitude
and longitude of the closest city or other geographical landmark
which a user may designate as reasonably approximating his
observation location. For example, the next procedural step causes
the LCD display 102 to request entry of the nation, state or
province, of the user's primary observation site. The UP 106 and
DOWN 108 scroll keys are used to scroll through a list of various
countries, states and provinces contained in the system's database
until the observer's nation, state or province appears on the
screen. Following selection of the observer's nation, state or
province, the observer is requested to select the closest city or
major geographical feature to their primary observation location by
using the UP and DOWN scroll keys to cycle through an alphabetical
list of cities and geographical features. When the desired city or
feature is displayed on the LCb screen, the user presses the enter
key 113 to inform the system that the virtual location procedure
has been concluded. The geographical coordinates (latitude and
longitude) of the selected site are then entered into system memory
as a first approximation observation location indicia which is used
in combination with the current time to orient and align the
telescope system for fully automated use.
[0132] This virtual location procedure is enabled by a database
table comprising a multiplicity of alphabetically listed geographic
locations with each associated to their known latitude and
longitude coordinates, as depicted in FIG. 9. FIG. 9 illustrates a
partial database listing of an exemplary top-level location table
and a sub-level database listing for locations contained within the
indicated California entry. The location database listing is
typically stored in the system's ROM memory 124, but might
alternatively be stored in an external disk drive, on floppy
diskette, or some other such mass storage device so long as the
location database listing is stored in some form of non-volatile
memory such that it may be accessed at need upon system
power-up.
[0133] The need for such a virtual location procedure is evident
when one considers that the location of a particular celestial
object in the night sky, at any given time, is solely a function of
the observer's latitude and the observer's local hour angle
displacement from the celestial meridian, in turn a function of the
observer's longitude and the observer's local time-of-day. Thus,
once an observer's latitude and longitude are known, and the
time-of-day (expressed in universal time coordinates) is known, the
observer has, all of the information necessary to compute the
relative bearing in either altitude and azimuth or declination and
right ascension of any celestial object whose absolute coordinates
are known. When an observer enters a reasonable approximation of
his latitude and longitude, and enters his local time, the system
is able to reasonably approximate the orientation of the night sky
with respect to that observer. As will be described in greater
detail below, further corrections may be made to this "first
approximation" orientation procedure in order to more precisely and
accurately define the night sky with respect to the telescope's
orientation.
[0134] Following the virtual location procedure, the system then
prompts a user to enter the configuration and alignment mode to be
used for the telescope system to which the system controller 100 is
coupled. The system has two configuration and alignment options;
Alt-Az and polar (equatorial). The choice between these two
configuration and alignment modes is made by scrolling through the
choices using the UP 106 and DOWN 108 arrow keys until the
appropriate configuration and alignment mode appears on the screen.
When the appropriate mode appears, the user depresses the mode 114
key thereby informing the system of the configuration and alignment
method most appropriate for the telescope system. Once system
configuration is determined, the controller commences a motor test,
slewing the telescope a short distance horizontally and vertically
(RA and Dec). After the motor test is completed, the system
initialization is complete and the telescope system is ready to be
aligned for observations.
[0135] System initialization is performed the first time that power
is applied to the system controller 100 or any time the system is
affirmatively RESET. During subsequent observation sessions, when
power is applied to the system controller 100, the controller
internally initializes and will only prompt a user to enter a
randomly selected number used in connection with the sun warning
and, subsequently to enter the time and date. From this point, the
system proceeds directly to telescope alignment and, in addition,
if the polar (equatorial) configuration and alignment model was
specified during the initialization procedure, the system
controller 100 automatically activates the right ascension (RA and
Dec) motor subassemblies.
[0136] Since the system controller is operable to define telescope
alignment with respect to both Alt-Az and polar (equatorial)
configuration and alignment models, it would be appropriate to
discuss the different alignment procedures associated with each of
the models seriatim, with the Alt-Az alignment models being
described first. In accordance with practice of principles of the
invention, the system enables the user to choose among four
different alignment procedures, three of which are concerned with
aligning the telescope to the celestial sphere and one of which is
used in connection with terrestrial alignment.
[0137] In a manner well understood by those having skill in the
art, a telescope configured to operate in an Alt-Az mode is unable
to "stop the sky" in hardware by maneuvering in equatorial
coordinates. Accordingly, Alt-Az telescope configurations must
"stop the sky" in software when tracking a celestial object. In
contrast to a polar or equatorial mounting, which may be driven in
one axis only, at a constant rate, both axes of an Alt-Az telescope
mount must be driven at rates that vary over a wide dynamic range.
Specifically, the drive rate equations for the altitude and azimuth
motors, respectively, of an Alt-Az telescope systems are as
follows: d Z d h = 15 .times. .times. sin .times. .times. A .times.
.times. cos .times. .times. .phi. Equation .times. .times. 1 d A d
h = - 15 .times. ( sin .times. .times. .phi. + cot .times. .times.
Z .times. .times. cos .times. .times. A .times. .times. cos .times.
.times. .phi. ) Equation .times. .times. 2 ##EQU1##
[0138] Where Z is the calculated zenith distance of an observer, h
is the observer's local hour angle (or LHA), A is azimuth (measured
Westward from the South) and (p is the observer's latitude. The
rate of change of an object's zenith distance Z with hour angle h
and the rate of change of an object's azimuth A with respect to
hour angle h is defined in units of (sidereal second).sup.-1. Thus,
in order for the telescope system to be able to adequately acquire
and track a given celestial object, it is necessary that the
telescope system understand its orientation with respect to the sky
such that such that an observer's latitude and local hour angle
(.phi., h) can be calculated.
[0139] Over the centuries, a great deal of thought and
consideration has been given to various methods for determining
latitude and longitude from an evaluation of the positions of
celestial objects with respect to the celestial coordinate system.
Specifically, the field of celestial navigation is directly
concerned with mathematical methods for determining an observer's
latitude and longitude from measurements taken of the positions of
the sun, moon, planets and various known stars. Although position
determination methodologies have evolved over the centuries, they
may all be conceptually viewed as defining various mathematical
means for observing and measuring the positions of celestial
references in an earth-based coordinate system (rectangular
coordinates or altitude-azimuth coordinates) and comparing the
measurements so obtained with the positions of such celestial
objects expressed in celestial coordinates (right ascension and
declination) as are tabulated in an ephemeris.
[0140] The solution to any given problem in celestial trigonometry
therefore depends on being able to convert measurements obtained in
one coordinate system (Alt-Az, for example) in the other coordinate
system (the celestial coordinate system). Coordinate system
conversions are well understood by those having skill in the art
and, indeed, have also undergone a conceptual evolution,
culminating in modern day, computer assisted, matrix transformation
and rotation mathematics. Nevertheless, regardless of the
coordinate systems used to express an observation and the
coordinate system used to define a universal reference,
observations made in one coordinate system may be rotated into the
reference coordinate system using simple mathematical principles,
so long as two points in one coordinate system correspond to the
same two points in the other coordinate system such that the
transformation boundaries with respect to displacement and rotation
are defined. Thus, in accordance with generally accepted
mathematical principles, two reference points expressed in an
Alt-Az coordinate system, for example, are a necessary and
sufficient condition for the Alt-Az coordinate system to be rotated
into a celestial coordinate system, so long as those same two
measurement points have a corresponding location metric in the
celestial coordinate system.
[0141] Proceeding now to the alignment methodologies in accordance
with practice of the invention, a first, "easy" alignment procedure
will be described in connection with the procedural flow chart of
FIG. 10a. After internal initialization and prior to beginning an
observation session, the LCD display 102 of the intelligent
telescope system controller 100 displays a prompt screen requesting
the user to select one of four alignment procedures, which a user
may select by scrolling through the various choices using the UP
106 and DOWN 108 scroll keys. A first alignment procedure, denoted
"easy" requires no knowledge of the night sky because the system
controller is able to locate its own alignment stars based on the
date and time entries provided by the user during
initialization.
[0142] Specifically, when the "easy" alignment procedure is
selected, the system next prompts the user to move the telescope
(using the motion keys 112) until the telescope is pointed North.
After the telescope tube is pointed North, a user depresses the
enter key 113 to inform the system that the telescope tube is in
its appropriate position. Next, the system prompts the user to
level the telescope tube by adjusting the telescope's altitude
position until the altitude (or declination) setting circle is set
to 0 degrees. Pointing the telescope North and leveling the
telescope tube functions to zero-in the position encoders of the
altitude and azimuth motor assemblies. Any subsequent motion of the
telescope away from its 0,0 position allows the telescope system to
directly calculate its altitude and azimuth displacements from the
0,0 terrestrial reference points. Using the time and date entries
presented by the user, the telescope system consults a database of
well known celestial objects and selects a particular bright object
which is currently above the horizon. The entered time and date
information allows the system to calculate whether that particular
bright object has rotated sufficiently in right ascension to bring
it above the observer's horizon, while the virtual latitude and
longitude entry provided by an observer's entering their closest
city or geographic feature, provides the system with sufficient
information regarding an observer's latitude so that it may
calculate an approximate declination value for that bright
object.
[0143] Once an object (star) is identified in the database, the
system automatically slews the telescope to the vicinity of that
star by commanding the appropriate motion from the altitude and
azimuth motors. Once the telescope has slewed to the vicinity of
the desired star, the observer is prompted to center the star in
the field of view of the telescope eyepiece, using all four
direction keys (112 of FIG. 6a) as required to center the star.
When the star is centered in the field of view of the eyepiece, the
observer presses the enter key 113 and the system then searches the
data base for a second bright object or star which is displaced at
least 30 degrees from the previous star in order to increase the
accuracy of alignment procedure. Once the second star is identified
from the data base, the system automatically slews the telescope to
the vicinity of that star and once again prompts the user to center
that star in the field of view of the eyepiece using the direction
keys 112 of the system controller 100. When the second star is
centered, the system calculates the position and orientation of the
telescope with respect to the night sky (the celestial sphere).
[0144] A further, truncated, alignment procedure is depicted in the
alignment flow chart of FIG. 10b, in which an Alt-Az configured
telescope is oriented to the night sky using only a single star
alignment procedure. As with the previous case, a user is prompted
to zero-in the motor position encoders by pointing the telescope to
the North and leveling the telescope such that the altitude setting
is at 0 degrees. The user then selects a particular star from an
alphabetized stellar object database list and presses the enter key
113, causing the telescope to automatically slew to the vicinity of
that star. The user centers the star in the,field of view of the
eyepiece by depressing the position keys 112 as required. Once the
chosen star is centered in the field of view of the eyepiece the
user again presses the enter key 113 the telescope is aligned for a
night of viewing.
[0145] Although the telescope might technically be considered
"aligned" after the user follows the above-described one star
alignment procedure, the accuracy of the one star telescope
alignment procedure should only be considered sufficient for
general astronomical observations. Because of certain pointing
errors that occur as the result of well known astronomical
perturbations, as will be described further below, additional
observations and alignment steps should be incorporated into the
procedure to refine the accuracy of the initialization
procedure.
[0146] Turning now to FIG. 10c, a user definable two star alignment
procedure will now be described in connection with the illustrated
procedural flow chart. As with the previous two alignment
procedures, the telescope undergoes an internal initialization
prior to beginning the observation session following which the LCD
display 102 of the intelligent telescope system controller 100
displays a prompt screen requesting the user to select an alignment
procedure. If the user desires to align the telescope with regard
to two user defined celestial objects, the user may scroll through
the alignment to the two star alignment option and press the enter
key 113.
[0147] The system next prompts the user to point the telescope to
the North, in order to zero the azimuth axis position encoders,
after which the user depresses the enter key 113 to inform, the
system the telescope tube is in its appropriate azimuth position.
Next, the system prompts user to level the telescope by adjusting
the telescope's altitude position until the altitude (or
declination) setting circle is set to 0 degrees, thus zeroing the
altitude motor position encoders. As was described previously, all
subsequent motion of the telescope away from this pre-set 0,0
position, allows a telescope system to directly calculate its
altitude and azimuth displacements from the 0,0 reference point.
The user is then prompted to scroll through an alphabetized stellar
object database listing and select a particular star from the list
by depressing the enter key 113. Again, once a particular user
defined star is identified, the system controller automatically
slews the telescope to the vicinity of that star. When slewing is
complete, the user is prompted to center that star in the field of
view of the eyepiece using the position keys and, when the star is
centered, the user depresses the enter key. The user is then
prompted to scroll through the alphabetized stellar object data
base listing and select a second particular star from the list.
Again, the enter key is depressed indicating that the user has
selected the second star. Once again, the system controller
automatically slews the telescope to the vicinity of the star after
which the user is again prompted to center that star in the field
of view of the eyepiece using the position keys. When the second
star is centered the user depresses the enter key and the system
controller calculates the absolute position of the telescope system
with respect to the night sky.
[0148] Once the absolute position of the telescope system with
respect to the night sky is determined, the system microprocessor
121 is easily able to calculate the path of any given celestial
object through the sky and to develop the appropriate motor motion
commands in accordance with the above-mentioned drive rate
equations, such that an Alt-Az telescope system can smoothly and
accurately track the object, i.e., "stops the sky" in software. A
celestial object's motion through the sky will, necessarily, be
calculated in terms of its rate of change in both altitude and
azimuth as a function of time. Thus, for a given time period, the
system microprocessor 121 is able to calculate the incremental
motor step or "tick" rates required to be executed by the motor
assembly so as to allow the telescope to track the object as it
moves through the sky.
[0149] With regard to the foregoing alignment systems described in
connection with the procedural flow charts of FIGS. 10a, 10b and
10c, it should be noted that the system controller calculates the
telescope's position by mapping the telescope's Alt-Az coordinate
system (Cartesian coordinate system) to the RA and Dec spherical
coordinate system defining the night sky (the celestial sphere). In
particular, the system controller reads the telescope's altitude
and azimuth angular positions, when pointed at the selected star or
stars, by reading the altitude and azimuth motor position encoder
values when the user depresses the enter key after each star has
been centered in the telescope eyepiece. From the telescope
pointing angles thus defined, the system controller calculates the
telescope's Cartesian position vectors and resolves each position
vector into a matrix of direction cosines. The Cartesian coordinate
matrix is mapped into a similarly defined matrix of the direction
cosines of the star or stars expressed in terms of the celestial
coordinate system, using well understood mathematical techniques
involving matrix manipulation and rotation. The matrix of celestial
direction cosines is generated by evaluating the RA and Dec
coordinates of the star or stars identified by the user during the
selection procedures.
[0150] It will be evident to those familiar with the mathematical
arts that once the same two points are identified in two different
coordinate systems, those two coordinate systems can be
mathematically mapped to one another such that any further
coordinates expressed in one coordinate system are easily expressed
in the other coordinate system through a mathematical transform.
Thus, once the telescope system is aligned with respect to the
celestial sphere, further observations may be made by merely
expressing the location of a desired object in terms of its
celestial coordinates. The system controller understands the
relationship between the celestial coordinate system and the
telescope's altitude and azimuth coordinates, makes the proper
mathematical transformation and drives the altitude and azimuth
motors appropriately to point the telescope at the desired
celestial position.
[0151] Once a telescope is "aligned" by use of one of the
above-described alignment procedures, the user might wish to
further refine the alignment accuracy of the telescope system by
refining the Cartesian coordinate matrix defining the telescope's
altitude and azimuth position vector. As is well known in the art,
certain corrections must be applied to a celestial object's mean
catalog of position in order to reduce it to the object's apparent
position in the night sky. When an observer plans an evening's
observations, the observer typically obtains an object's RA and Dec
coordinates from an ephemeris or catalog which defines the object's
position in terms of the coordinate system of a standard epoch.
This is the mean position of the object. However, the standard
epoch is generally different than the epoch at the time of
observation. In addition, the object's catalog position does not
include corrections for certain positional errors which depend upon
the observation time and the particular location of the observer.
Thus, the catalog position does not define precisely where the
observer would likely find the desired object. Since the
telescope's system controller operates on an object data base which
defines celestial objects according to their mean position taken
from a catalog, the mean coordinates must be converted to apparent
coordinates before commands are sent to the telescope's altitude
and azimuth motors, in order that an object may be precisely
acquired and tracked.
[0152] The corrections that must be applied to a catalog mean
position in order to reduce it to apparent position are listed in
the following table, in order of decreasing size. TABLE-US-00001
TABLE 1 Correction Approx. Magnitude Precession 40' of arc.
Refraction 30' of arc. Annual Aberration 20'' of arc. Nutation 17''
of arc. Solar Parallax 9'' of arc. Stellar Parallax 1'' of arc.
Orbital Motion 1'' of arc. Proper Motion 0.5'' of arc. Diurnal
Aberration 0.3'' of arc. Polar Motion 0.1'' of arc.
[0153] Not all of the listed corrections need be applied, only
those corrections larger than the required pointing accuracy of an
observation. Typically, only precession and refraction corrections
need be made.
[0154] Additional sources of systematic error come from certain
mechanical errors introduced by imperfections in the telescope
mount, the motor and drive train system, the servo feedback system
and imprecisions in leveling the telescope. Mechanical corrections
that should be considered when precisely aligning the telescope
system are listed in the following table. TABLE-US-00002 TABLE 2
Encoder Zero Offset Azimuth Axis Tilt (Alt-Az Mounts) Polar Axis
Misalignment (Equatorial Mounts) Axis Non-orthogonality Collimation
Error Tube Flexure Mount Flexure Gearing/Bearing Error Drive Train
Torsion Error
[0155] These corrections are computed in a manner that can be used
with any telescope of a particular mounting type, but the values of
the error parameters are unique to each individual telescope
system, since they are characteristics of that system. For example,
in closed loop systems, the position feedback encoders provide a
numerical value corresponding to the angular position of an axis.
This numerical value is converted to a meaningful coordinate, such
as RA, Dec, altitude or azimuth, by applying a calibration
algorithm to the raw encoder data. These encoder zero offset
corrections are incorporated into the calibration algorithm in
order to provide numerical values representing the true position of
the telescope. The system controller compares the apparent position
of the desired object with the position of the telescope
(determined from the position encoder readings) and generates
appropriate movement commands to the motors in order to minimize
the difference between the object and telescope positions.
[0156] Each of the astronomical and mechanical error sources are
dealt with in precisely the same manner as initial telescope
orientation. Once the telescope has been "aligned" the user may
slew to a next object in order to begin observation. If the next
object is not precisely centered in the telescope eyepiece, or if
the next object drifts from the center of the eyepiece during
tracking, the user may manually reposition the telescope using the
position keys and commands the system to re-sync to the object's
new position. The minor corrections, thus made, form the basis for
a refinement of the Alt-Az position matrix which is then mapped
into the celestial coordinate system. As further celestial objects
are evaluated, the matrix is further refined to account for finer
and finer error sources. Although capable of such further accuracy
definition, it will be understood that the system according to the
invention is able to account for, at least, the first two major
mechanical error sources during the initial orientation procedure.
Certain astronomical corrections are defined by well understood
mathematical algorithms and can be easily incorporated into the
orientation procedure. Thus, the pointing and tracking ability of
the telescope system according to the invention is deemed
sufficiently accurate for deep-sky observations and
astrophotography following the alignment procedures set forth in
connection with FIGS. 10a, 10b and 10c.
[0157] Since the system controller is operable to define telescope
alignment and movement with respect to a polar (equatorial) mount
configuration, it is now appropriate to discuss alignment
procedures associated with an equatorial mount in connection with
the procedural flow charts of FIGS. 11a, 11b and 11c. Each of the
polar alignment procedures first requires that the polar
configuration and alignment mode is chosen by a user during system
initialization as described in connection with the initialization
procedure flow chart of FIG. 12. Needless to say, it is also
necessary to that the telescope mount be configured as an
equatorial mount and that the user properly adjusts the telescope's
declination axis such that the declination axis is perpendicular to
the mount's declination plane and that the celestial pole (North or
South depending upon the observer's hemisphere) falls on the
mount's declination plane.
[0158] Turning now to FIG. 11a, an "easy" polar alignment procedure
is described. Specifically, when the "easy" alignment procedure is
selected from the menu, the system prompts the user to point the
telescope (using motion keys 112) along the RA axis until the
telescope is pointed to the horizon (RA home position). The user
then depresses the enter key 113 to inform the system that the
telescope tube is in its appropriate RA position. Next, the system
prompts the user to move the telescope until the declination
setting circle reads 90 degrees. Putting the telescope in a home
position with regard to both RA and Dec functions to zero-in the
position encoders of the declination and right ascension motors.
Any subsequent of the telescope away from its 0,0 position allows
the telescope system to directly calculate its right ascension and
declination displacement from the 0,0 reference point.
[0159] After the previous steps are completed, the remainder of the
"easy" polar alignment procedure is identical to the "easy" Alt-Az
alignment procedure described in connection with FIG. 10a. In
particular, using the time and data entries provided by the user,
the telescope system consults a data base of well known celestial
objects and selects a particular bright object which is currently
above the horizon; the system automatically slews the telescope to
the vicinity of that star by commanding the appropriate motion from
the right ascension and declination motors; prompts the user to
center the star in the field of view of the telescope eyepiece and
uses the observer's manual position adjustments to refine its
orientation algorithm. The process is repeated for a next star
which, when centered by the observer, allows the system to
calculate the precise position and orientation of the telescope
with respect to the night sky (the celestial sphere).
[0160] As was the case with the Alt-Az configuration, a truncated,
one-star, alignment procedure is provided to support an equatorial
mount configuration and is depicted in the procedural flow chart of
FIG. 11b. As with the previous case, a user is prompted to zero-in
the motor position encoders by commanding the telescope to move to
its RA and Dec home positions. The user then selects a particular
star from an alphabetized stellar object data base list and may
press the enter key 113, causing the telescope to automatically
slew to the vicinity of that star. The user then centers the star
on the field of view of the eyepiece by depressing the position
keys 112 as required. Once the chosen star is centered in the field
of view of the eyepiece, the user again presses the enter key 113
and the telescope is deemed aligned for a night of viewing.
[0161] A two-star alignment procedure is depicted in the procedural
flow chart of FIG. 11c, in which the user is again prompted to move
the telescope to the RA and Dec home positions and align the
telescope by sequentially selecting two stars from an alphabetized
stellar object data base list. As each star is selected, the
telescope system automatically slews to the vicinity of that star,
following which the user centers the star in the field of view of
the eyepiece using the position keys 112 as required, and depresses
the enter key 113 in order to inform the system that the desired
star is centered.
[0162] Following definition of the home position, and following
entry of either one or two stars in accordance with the above
procedures, the telescope system calculates the telescope's
position with relation to the night sky. Since the telescope mount
comprises an equatorial configuration, the computation algorithm is
simplified somewhat since the system need not convert coordinate
systems, from, for example, Alt-Az to equatorial. Since an
equatorial mount maneuvers in accordance with a spherical
coordinate system defined by RA and Dec, all that is required to
orient the telescope is a simple rotation of the telescope
spherical coordinate system into the celestial coordinate system.
The rotation is made about the telescope's RA and Dec axes in
accordance with well established mathematical principles which need
not be discussed further herein.
[0163] Following orientation, the equatorially configured telescope
system is now able to acquire and track selected celestial objects
by appropriate motion commands to its right ascension and
declination motor assemblies. Once a selected celestial object is
acquired, tracking is effected simply by commanding the right
ascension motor assembly to move the telescope about the
corresponding right ascension axis at the sidereal rate in the
desired direction. No further commands need be given the
declination motor assembly unless the user desires to acquire a
different celestial object or, alternatively, the user desires to
more precisely and accurately align the telescope system to
compensate for some slight originally unaccounted for error.
[0164] Returning now to FIG. 6b, the system microprocessor 121
receives user I/O information, as provided by the system I/O
microcontroller 122 and performs any needed data processing under
application software program control. Data processing typically
results in some form of desired telescope motion. The system
microprocessor 121 is able to calculate the direction and extent of
any required motor motion and is further able to direct the
appropriate motor assembly to take the required action by passing
the appropriate command through the system I/O microcontroller 122.
Motor motion commands are substantially the same as those described
in connection with the embodiment of FIGS. 5a and 5b and are
provided to the system I/O microcontroller 122 over a two-wire
serial clock and data bus 133. Certain commands are passed through
the microcontroller 122 and are issued directly to the motor by the
system microprocessor. Such commands typically include the step
rate commands, the error count commands, the set and find LED
position commands, and the like. Certain other information,
typically read data, is held and processed by the system I/O
microcontroller 122 for use by the microprocessor when it so
desires.
[0165] Notwithstanding the foregoing discussion of telescope
orientation and alignment, it will be evident to one having skill
in the art, that major simplifications can be made to a telescope
orientation and alignment procedure by incorporating additional
component devices that are able to automatically provide an
indication of the orientation of the telescope tube with respect to
the compass, i.e., north-south sensing, an automatic indication of
axial tilt, i.e., telescope level, and an automatic indication of
absolute position and time. Pertinent to alignment and orientation
simplification is the realization that electronic compasses, based
on magnitoresistive sensors are able to electrically resolve a
position orientation using the earth's magnetic field, to an
accuracy of approximately 1/2 degree and with a resolution of about
0.1 degrees. As is well understood by those having skill in the
art, the earth is surrounded by a magnetic field which has an
intensity of from about 0.5 to about 0.6 gauss and includes a
component parallel to the earth's surface that always points
towards magnetic north. This feature of the earth's magnetic field
forms the basis for all magnetic compasses and it is the components
of this field, parallel to the earth's surface, better used to
determine compass direction.
[0166] In particular, a type of magnetic sensor, termed a
magnitoresistive sensor (MR) is constructed of thin strips of a
nickel iron (NiFe) magnetic film, also termed permalloy, whose
electrical resistance properties vary with a change in an applied
magnetic field. MR sensors have a well defined axis of sensitivity,
respond to changes in an applied magnetic field as little as 0.1
milligauss, have a response time of less than 1 microsecond and are
generally commercially available as packaged integrated circuits.
MR sensors are thus particularly suitable for use in a north-south
sensing apparatus coupled to the telescope system of the exemplary
embodiments.
[0167] One such configuration is shown in FIG. 17 which is a
semi-schematic circuit diagram of a north-south sensor system, in
accordance with the invention, that incorporates an MR sensor,
implemented as an HMC 1021S, manufactured and sold by Honeywell,
Inc. of Plymouth, Minn. The MR sensor 200 is a magnitoresistive
sensing element constructed of NiFe thin films deposited onto a
silicon substrate in a manner to define a Wheatstone resistor
bridge. The MR sensor 200 further incorporates a current strap
which is used to electrically "set" or "reset" the polarity of the
device output and further allows a compensating offset field to be
applied to the sensing elements to compensate for ambient magnetic
films. A supply voltage is coupled to the MR sensor and causes a
current to flow through the magnitoresistors comprising the
Wheatsone bridge configuration. A crossed applied field causes
magnetization in two of the oppositely placed resistors to rotate
towards the current, resulting in an increase in the corresponding
resistance. In the remaining two oppositely-placed resistors,
magnitization rotates away from the current resulting in a decrease
in the resistance.
[0168] Current passing through two of the arms of the Wheatstone
bridge is taken from the MR sensor at two outputs, one of which is
applied to the non-inverting input of an operational amplifier 202
configured as a voltage follower. The second output is applied to
the non-inverting input of a second operational amplifier 204, the
inverting input of which is coupled to receive the output of the
voltage follower 202. The output of the second operational
amplifier 204 is directed to the non-inverting input of a gain
stage 206 which, in turn, drives an output pin 208 to give an
indication signal as to whether or not the MR sensor is aligned
with the earth's magnetic field. In operation, the gain stage 206
is configured so as to output a signal if the current from the MR
sensor's two outputs is unbalanced, i.e., indicating that the
sensor is not aligned with the earth's magnetic field. As the
center comes into alignment with the field, current through the
oppositely-placed resistor arms becomes balanced, resulting in the
second operational amplifier 204 having a null output. Gain stage
206, in turn, outputs a null signal indicating that the MR sensor
is aligned with the earth's magnetic field, i.e., pointing towards
magnetic north.
[0169] As a further indication of whether or not the MR sensor is
pointing towards magnetic north, two light emitting diodes 210 and
212 are coupled, in parallel fashion, to the output of the gain
stage 206. A first light emitting diode (LED) 210 is reverse
coupled to the output of the gain stage 206. By reverse coupled, it
is meant that the negative side of the diode is coupled to the
output, while the positive side is coupled to a reference
potential, such as ground. A second diode 212 is coupled in forward
fashion to the output of the gain stage 206. In combination, the
diodes function to give an indication as to the alignment of the MR
sensor with earth's magnetic field. When the sensor 200 is
mis-aligned in one direction, the gain stage output will be either
positive or negative, depending on whether the sensor is
mis-aligned to the "left" or "right" of a centerline indicating the
direction of magnetic north. When the sensor is mis-aligned to one
direction, the gain stage output might be negative, in which case
the first LED 210 (the negatively coupled LED) will conduct
current, thereby emitting light. If the MR sensor 200 is misaligned
in the opposite direction, the gain stage 206 will output a
positive signal, causing the positively coupled LED 212 to conduct,
lighting-up in turn. When the sensor is aligned to magnetic north,
the gain stage output is nulled and both LEDs are off.
[0170] It should be noted, that since these are diodes, there is a
forward voltage drop associated therewith which limits their
precision in indicating magnetic north precisely. Depending on the
value of the forward voltage drop of the LEDs 210 and 212, the MR
sensor has a slight range about true north during which time the
gain stage 206 will not develop a sufficient output signal to
activate either the forward or reverse biased LED. However, even
within this "uncertain" range, the gain stage 206 is outputting a
signal to the output pin 208 which is able to be evaluated by
either an intelligent system control unit (100 of FIGS. 6a and 6b)
or an integrally coupled PIC processor of the type described
above.
[0171] It bears mentioning further that the MR sensor system is
able to be calibrated by a zero adjustment circuit 214 which is
coupled to the inverting input of the second operational amplifier
204. Zero adjustment circuit 214 is provided in order to compensate
for the input offsets commonly exhibited by almost all operational
amplifiers, and suitably comprises an adjustable resistor coupled
between positive and negative supply voltages with a center tap
defining the zero adjustment connection to the inverting input of
the operational amplifier 204. In operation, the sensor is
precisely aligned with the earth's magnetic field in a
manufacturing jig and the variable resistor is adjusted until such
time as the gain stage 206 defines a null output signal. This
indicates that the overall circuit is now balanced with circuit
offsets compensated for.
[0172] Further, the sensor circuit suitably includes a set/reset
circuit, suitably configured as a current pulse generator, which is
used to eliminate the effects of past fail hysteresis and which can
electronically set or reset the polarity of the output by applying
an appropriate set or reset signal.
[0173] The MR sensor arrangement depicted in FIG. 17 has particular
utility when configured on a small printed circuit board and
mounted on a telescope tube in such a manner that the position axis
of the center is aligned with the long axis of the telescope.
Therefore, when the MR sensor is aligned with the earth's magnetic
field so as to indicate magnetic north, the telescope tube is also
positioned with its optical axis aligned towards magnetic north.
The sensor's output 208 is coupled to the auxiliary input of the
electrical interface (30 of FIGS. 3a and 3b) and is thereby made
available to system processing components as an automatic direction
indication signal. In this manner, there is no longer any need for
a user to manually align the telescope to point towards north. Once
the automated telescope system is turned on, an application routine
automatically slews the telescope back-and-forth in the horizontal
direction and examines the "sense" of the output of the sensor.
Once the automated system detects that the sensor is aligned
correctly with north, i.e., senses a null output, the automated
telescope system evaluates the position of the motors and
initializes the azimuth motor assembly.
[0174] While the discussion above has concerned itself with a
description of how an MR sensor system is configured to align its
self with the earth's magnetic field, i.e., give an indication of
magnetic north, it should be noted that the sensor can be
configured to give an indication of its alignment with respect to
true north. In this particular instance, the sensor system is
aligned with true north in a manufacturing jig and the zero
adjustment circuit 214 is adjusted such that the gain stage 206
outputs a null indication. It should be understood that the
currents in the oppositely-disposed arms of the Wheatsone bridge
will necessarily be unbalanced, but the zero adjustment circuit 214
is adapted to compensate for this misadjustment as well as
compensate for any offsets developed by the operational amplifiers
202 and 204.
[0175] It is also quite within the contemplation of the present
invention to use an MR sensor in a 3-axis mode in order to
eliminate axial tilt concerns by electronically dealing with any
axis non-orthogonality. In this implementation, an additional MR
sensor is provided which is aligned in a plane orthogonal to the
plane of the horizontally disposed MR sensor. The additional MR
sensor is configured to measure the vertical portion of the US
magnetic field, i.e., the angle of the magnetic field to the
surface of the earth. Errors introduced by axial tilt can be quite
large depending on the magnitude of the dip, or inclination,
angle.
[0176] An additional method that might be used to correct for axial
tilt is to incorporate an inclinometer, or tilt sensor, with the MR
sensor in order to electrically define any mount offsets due to
mount pitch. When an inclinometer, or tilt sensor, is incorporated
with the MR sensor, the telescope system is provided with a fully
automated, electronic methodology for 3-axis sensing. This allows
the telescope system to automatically adjust itself to a level
condition as well as automatically adjusting itself to align with
either true or magnetic north. Once these alignments are made, the
axis encoders of the motor systems are automatically initialized in
order to compensate for the mount alignment parameters. Therefore,
electronic sensors coupled to the telescope tube provide a very
repeatable position index when in proximity with the mount's axis
crossings. Electronic sensors are used as fixed point
high-resolution devices, with fine positioning being provided by
the motor encoders. Since pointing accuracy typically depends on
the flexure characteristics of a tube, the mechanical stability of
the tube and mount combination and the quality of the gearing
between the drive motor and a telescope mount, it will be
understood that pointing accuracy can be simply and easily added to
a inexpensive telescope system that might exhibit a certain
mechanical looseness.
[0177] As was developed above, in order to completely align a
telescope system, the user or an intelligent telescope system need
only know the direction of north, the inclination of the horizon
(level), the time and date and its position on the earth's surface.
If these quantities are known, there is no further information that
need be provided to any telescope system to allow it to thereafter
point to any designated object with a known ephemeris, other than
an command to do so. Time and date information are accessible by
receiving a broadcast signal, WWV, which is made available for such
purpose. The automated telescope system according to the invention
fully contemplates being able to couple a source of WWV information
into the intelligent system control unit so that the control unit
is able to continually update date and time information such that
the time and date variables of the alignment system are eliminated.
WWV is in Fort Collins, Colo. and broadcasts continuous time and
frequency signals on 2.5, 5, 10, 15 and 20 MHz. All frequencies
provide the same information, with frequencies above 10 MHz working
best during daylight hours, while lower frequencies working best at
night. The beginning of each hour is identified by a 0.8 second
long 1500 Hz tone, with the beginning of each minute identified by
a similar length 1000 Hz tone. Second pulses are given by a 440 Hz
tone the 29th and 59th second pulses of each minute being omitted.
Time signals may be input directly from a WWV receiver, with the
various frequency tones defining clock signals which can be
processed by the intelligent system control unit to update its date
and time information.
[0178] Alternatively, WWV information may be received via an
Internet connection by a laptop-type personal computer system.
Information processed by the laptop can be transferred to the
intelligent system control unit over the auxiliary input bus of the
interface panel in a manner as described above.
[0179] Accurate location information can be provided to the
intelligent system control unit by use of a global positioning
system (GPS) or differential global positioning system (DGPS)
receiver configured with an NMEA interface. The NMEA interface is a
well recognized interface protocol which can additionally be
coupled to the auxiliary interface to provide a source of location
information directly to the intelligent system control unit. Once
the intelligent system control unit has location, time and date
information available as well as the output of the "north" and
"level" sensors, the intelligent system control unit becomes fully
aware not only of its location but also of the spatial orientation
of the telescope system to which it is coupled.
[0180] The systems and methods associated with 3-axis sensing, as
described above, are equally applicable to additional "pointing" or
"acquisition" devices beyond the novel telescope system in
accordance with the invention. Indeed, 3-axis sensing systems are
adaptable to be mounted on a detachable viewfinder or telescope
eyepiece such that a user need only direct the eyepiece in
accordance with the signals received from the sensing devices in
order to orient themselves with both horizon and with north.
Binoculars and heads-up-display (HUD) goggles are also able to be
configured with 3-axis sensing devices in the above manner in order
to provide them with an orientation capability.
[0181] A further feature of the intelligent system control unit
(100 of FIGS. 6a and 6b) is the construction of the light source
for providing uniform illumination to the LCD display screen 102.
With reference, now, to FIG. 13, a cusped, curvilinear optical
light box 150 is disposed on the surface of the control unit's
electronic component circuit board, and positioned in the region
just beneath the LCD display screen, and having approximately the
same footprint. The light box defines a generally rectangular,
hollow enclosure, with its surface describing a pair of curvilinear
arcs 151 and 152, laterally symmetrical about a central, downward
projecting, cusp which bisects the surface. Illumination LEDs 153,
154, 155 and 156 are arranged, in pairs, along each of the short
sides of the light box and are configured to shine into the
enclosure, in the direction of the cusp.
[0182] Each of the curvilinear surfaces are rendered translucent,
by painting them white, for example, or by constructing the
reflector from a translucent material such as a suitable plastic.
The translucent property of the surface allows the light developed
by the LEDs to shine through the surface, but permits each arcuate
portion to diffuse the light and direct it (as a backlight source)
onto the LCD display in a diffusion pattern promoting uniform
illumination.
[0183] In a conventional, flat-surfaced light box, light energy,
from a non-coherent, uniform, source such as an LED, is scattered
through the translucent surface only when the scattering vector of
the light makes a relatively large angle with the surface in
question. As the surface element is farther and farther away from
the light source, the scattering angle becomes correspondingly
smaller, until the light is scattered along the surface underside
(perpendicular scatter vector) and very little is scattered through
the material and onto the display (Normal scatter vector). This
phenomenon results in a dark, or relatively unilluminated, region
in the center of the display, while the edges are over illuminated
(so called hot spots). This makes the display hard to read,
particularly at night.
[0184] The curvilinear arcuate surfaces of the light box 150
according to the invention, are shaped to insure a substantially
greater degree of normal scattering out of the light box at the
light path extremities, i.e., the portion of the surface farthest
from the light source (the center). Moreover, the gradual curvature
of each surface maintains the surface at a relatively constant
scattering angle with respect to the light source. Thus the light
energy diffused through the surface is relatively constant along
the surface in the direction from the light source towards the
cusp. In the region of the cusp itself, surface reflection adds an
additional component of illumination to the light directed onto the
display. Light scattered from a first arcuate surface 151 at a low
angle, is reflected from the second arcuate surface 152 at an equal
angle and thus towards the display. Low angle surface scattering is
therefore recovered to some degree and forms an additional
component of illumination in the central region.
[0185] It should be evident, from the foregoing discussion, that
the various components and elements of the present invention are
not limited to the particular telescope systems illustrated thus
far. Indeed, the telescope and motor systems described in
connection with the illustrated embodiments, were chosen because
the novel components of the invention appeared externally and
admitted of more direct identification. Turning now to FIG. 14,
there is depicted a further embodiment of a fully automated
telescope system, in which the motor assemblies are not configured
as add-on components, but rather are integrated into the telescope
system.
[0186] The telescope system of FIG. 14 is shown as configured to
operate in equatorial mode, with its legs 160a, 160b and 160c
positioned to equatorially align the telescope such that the top
surface 161 of the base housing 162 rotates to define the system's
RA plane. Right and left fork arms 163 and 164, respectively,
support the telescope tube 165 and provide its declination rotation
axis. The base housing 162 additionally supports an interface panel
substantially similar to the interface panel 30 of FIGS. 1, 2, 3a
and 3b, but without the serial interface connections to the Alt
(Dec) and Az (RA) motor assemblies. Rather, the interface panel 166
provides for plug-in connection of either of the previously
described control units, and for plug-in connection of a
multiplicity of auxiliary devices through an auxiliary bus.
[0187] Motor assembly coupling connections are not required for the
embodiment illustrated in FIG. 14, since the motor assemblies are
incorporated into the telescope structure. Thus, external
connections are not required. However, electrical connection to the
motor assemblies is made via an identical 2-wire serial interface
as with previous embodiments, except that the motor interface
busses are internalized into the telescope structure as well.
[0188] A first, declination (or altitude) motor assembly is
configured into a motor enclosure 168, formed by in the hollow
interior of one of the fork arms; the right fork arm 163 in the
illustrated embodiment. FIG. 15 depicts the internal configuration
of the fork arm 163 and illustrates the position of a declination
(Alt) motor assembly 170 and its associated gear train 172 within
the fork arm.
[0189] A second, right ascension (or azimuth) motor assembly is
configured to fit within the base housing 162 of the telescope
system, in a manner depicted in FIG. 16. The RA (Az) motor assembly
174 and its associated gear train 176 are disposed in a hollow
enclosure formed just beneath the RA surface 161 of the telescope.
Direct DATA, CLK, power and ground couplings are taken from
hardwired connections made between the control unit input of the
interface panel 166 and each respective motor assembly. Each motor
assembly 170 and 174 comprises the same electronic components as
those described in connection with previous embodiments and are,
therefore, endowed with the same degree of intelligence.
[0190] The telescope system embodiment of FIGS. 14,15 and 16 may be
controlled by either the semi-intelligent or fully intelligent
control units described previously, with the same degree of
functional performance. Moreover, the auxiliary bus supports the
same numbers and types of auxiliary devices.
[0191] It should be understood, therefore, that distributing
intelligence across various functional components of a telescope
system, is not limited to the particular configuration of the
telescope. Certain portions of the system may be integrated into
the telescope in the interest of compactness and design efficiency
without sacrificing any of the virtues of intelligence
distribution. All that these integrated systems lack is the ability
to be lobotomized to a purely mechanical system operated entirely
by manual manipulation.
* * * * *