Celestron CPC DELUXE 1100 HD, Instruction Manual

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Celestial pole
Š‡‹ƒ‰‹ƒ”›’”‘Œ‡ –‹‘‘ˆƒ”–Šǯ•”‘–ƒ–‹‘ƒŽƒš‹•
north or south pole onto the
celestial sphere.
Celestial An imaginary sphere surrounding the Earth,
Sphere concentric with the Earth’s center.
Collimation The act of putting a telescope’s optics into perfect
alignment.
D –
Declination The angular distance of a celestial body
(DEC)
‘”–Š‘”•‘—–Š‘ˆ–Š‡ ‡Ž‡•–‹ƒŽ‡“—ƒ–‘”Ǥ–ƒ›
be said to correspond to latitude on the
surface of the Earth.
E –
Ecliptic
Š‡’”‘Œ‡ –‹‘‘ˆ–Š‡ƒ”–Šǯ•‘”„‹–‘–‘–Š‡ ‡Ž‡•–‹ƒŽ
•’Š‡”‡Ǥ–ƒ›ƒŽ•‘„‡†‡Ƥ‡†ƒ•Dz–Š‡ƒ’’ƒ”‡–
yearly path of the Sun against the stars.”
Equatoria l A telescope mounting in which the instrument
mount is set upon an axis which is parallel to the
ƒš‹•‘ˆ–Š‡ƒ”–ŠǢ–Š‡ƒ‰Ž‡‘ˆ–Š‡ƒš‹•—•–„‡
equal to the observer’s latitude.
F –
Focal length The distance between a lens (or mirror) and the point
ƒ–™Š‹ Š–Š‡‹ƒ‰‡‘ˆƒ‘„Œ‡ –ƒ–‹Ƥ‹–›‹•„”‘—‰Š–
to focus. The focal length divided by the aperture of
the mirror or lens is termed the focal ratio.
G –
GoTo Term used to refer to a computerized telescope
or to the act of slewing (moving) a computerized
telescope.
J –
Jovian Planets Any of the four gas giant planets that are at a greater
distance form the Sun than the terrestrial planets.
K –
Kuiper Belt A region beyond the orbit of Neptune extending
to about 1000 AU which is a source of many short
period comets.
L –
Light–Year (ly) Ž‹‰Š–Ȃ›‡ƒ”‹•–Š‡†‹•–ƒ ‡Ž‹‰Š––”ƒ˜‡”•‡•‹ƒ
˜ƒ ——‹‘‡›‡ƒ”ƒ––Š‡•’‡‡†‘ˆ͙͠͞ǡ͘͘͘‹Ȁ•‡ Ǥ
ȋ͚͡͡ǡ͚͟͡Ȁ•‡ ǤȌ‹–Š͙͛ǡ͟͝͝ǡ͘͘͞•‡ ‘†•‹ƒ›‡ƒ”ǡ
–Š‡Ž‹‰Š–Ȃ›‡ƒ”‡“—ƒŽ•ƒ†‹•–ƒ ‡‘ˆ͝Ǥ͠͠–”‹ŽŽ‹‘‹Ž‡•
ȋ͡Ǥ͜͞–”‹ŽŽ‹‘ȌǤ
M Ȃ
Magnitude Magnitude is a measure of the brightness of a
celestial body. The brightest stars are assigned
magnitude 1 and those increasingly fainter from
2 down to magnitude 5. The faintest star that can
„‡•‡‡™‹–Š‘—–ƒ–‡Ž‡• ‘’‡‹•ƒ„‘—–ƒ‰‹–—†‡͞Ǥ
Each magnitude step corresponds to a ratio of 2.5 in
brightness. Thus a star of magnitude 1 is 2.5 times
brighter than a star of magnitude 2, and 100 times
brighter than a magnitude 5 star. The brightest star,
‹”‹—•ǡŠƒ•ƒƒ’’ƒ”‡–ƒ‰‹–—†‡‘ˆȂ͙Ǥ͞ǡ–Š‡ˆ—ŽŽ
‘‘‹•Ȃ͙͚Ǥ͟ǡƒ†–Š‡—ǯ•„”‹‰Š–‡••ǡ‡š’”‡••‡†
‘ƒƒ‰‹–—†‡• ƒŽ‡ǡ‹•Ȃ͚͞Ǥ͟͠ǤŠ‡œ‡”‘’‘‹–‘ˆ–Š‡
apparent magnitude scale is arbitrary.
Meridian A reference line in the sky that starts at the North
celestial pole and ends at the South celestial pole and
’ƒ••‡•–Š”‘—‰Š–Š‡œ‡‹–ŠǤˆ›‘—ƒ”‡ˆƒ ‹‰‘—–Šǡ
the meridian starts from your Southern horizon and
passes directly overhead to the North celestial pole.
Messier ”‡ Šƒ•–”‘‘‡”‹–Š‡Žƒ–‡͙͘͘͟•™Š‘™ƒ•
primarily looking for comets. Comets are hazy
†‹ơ—•‡‘„Œ‡ –•ƒ†•‘‡••‹‡” ƒ–ƒŽ‘‰‡†‘„Œ‡ –•
that were not comets to help his search. This catalog
became the Messier Catalog, M1 through M110.
N –
Nebula –‡”•–‡ŽŽƒ” Ž‘—†‘ˆ‰ƒ•ƒ††—•–ǤŽ•‘
”‡ˆ‡”•–‘ƒ› ‡Ž‡•–‹ƒŽ‘„Œ‡ ––Šƒ–Šƒ•ƒ
cloudy appearance.
North Celestial The point in the Northern hemisphere around
Pole which all the stars appear to rotate. This is
caused by the fact that the Earth is rotating on
an axis that passes through the North and
South celestial poles. The star Polaris lies less
than a degree from this point and is therefore
referred to as the “Pole Star”.
Nova Although Latin for “new” it denotes a star that
suddenly becomes explosively bright at the end of its
life cycle.
O –
Open Cluster ‡‘ˆ–Š‡‰”‘—’‹‰•‘ˆ•–ƒ”•–Šƒ–ƒ”‡ ‘ ‡–”ƒ–‡†
along the plane of the Milky Way. Most have
an asymmetrical appearance and are loosely
assembled. They contain from a dozen to many
hundreds of stars.
P –
Parallax ƒ”ƒŽŽƒš‹•–Š‡†‹ơ‡”‡ ‡‹–Š‡ƒ’’ƒ”‡–’‘•‹–‹‘
‘ˆƒ‘„Œ‡ –ƒ‰ƒ‹•–ƒ„ƒ ‰”‘—†™Š‡˜‹‡™‡†
„›ƒ‘„•‡”˜‡”ˆ”‘–™‘†‹ơ‡”‡–Ž‘ ƒ–‹‘•ǤŠ‡•‡
’‘•‹–‹‘•ƒ†–Š‡ƒ –—ƒŽ’‘•‹–‹‘‘ˆ–Š‡‘„Œ‡ –ˆ‘”
a triangle from which the apex angle (the parallax)
ƒ†–Š‡†‹•–ƒ ‡‘ˆ–Š‡‘„Œ‡ – ƒ„‡†‡–‡”‹‡†
if the length of the baseline between the observing
positions is known and the angular direction of the
‘„Œ‡ –ˆ”‘‡ƒ Š’‘•‹–‹‘ƒ––Š‡‡†•‘ˆ–Š‡„ƒ•‡Ž‹‡
has been measured. The traditional method in
astronomy of determining the distance to a celestial
‘„Œ‡ –‹•–‘‡ƒ•—”‡‹–•’ƒ”ƒŽŽƒšǤ
Parfocal Refers to a group of eyepieces that all require the
same distance from the focal plane of the telescope
to be in focus. This means when you focus one
parfocal eyepiece all the other parfocal eyepieces, in
a particular line of eyepieces, will be in focus.
Parsec The distance at which a star would show parallax
‘ˆ‘‡•‡ ‘†‘ˆƒ” Ǥ–‹•‡“—ƒŽ–‘͛Ǥ͚͞Ž‹‰Š–Ȃ›‡ƒ”•ǡ
͚͘͞ǡ͚͞͝ƒ•–”‘‘‹ ƒŽ—‹–•ǡ‘”͛͘ǡ͘͘͠ǡ͘͘͘ǡ͘͘͘ǡ͘͘͘
km. (Apart from the Sun, no star lies within one
parsec of us.)
Point Source
‘„Œ‡ –™Š‹ Š ƒ‘–„‡”‡•‘Ž˜‡†‹–‘ƒ‹ƒ‰‡
because it to too far away or too small is considered
a point source. A planet is far away but it can be
resolved as a disk. Most stars cannot be resolved as
disks, they are too far away.