Meade - RCX400 14 inch Advanced Ritchey-Cretien with UHTC condition ( Refurbished )

The “advanced” in Advanced Coma-Free.

A traditional Ritchey-Chrétien (RC) is a type of reflector that delivers a coma-free, flat field
of view via hyperbolic primary and secondary mirrors. RC telescopes (from a variety of
manufacturers) are found in most of the world’s top observatories and NASA’s Hubble Space
Telescope. Because the mirrors in these telescopes have always been very expensive to make, few
amateur astronomers could enjoy them. Fortunately, Meade engineers developed a radical new
Advanced Coma-Free design by combining a hyperbolic secondary mirror with a
corrector-lens-and-spherical-primary-mirror combination that performs as one hyperbolic element.
This Advanced version of the traditional RC design produces a coma-free, flat field of view that
rivals traditional RC telescopes at a fraction of the cost. The design even eliminates
diffraction spikes and improves astigmatism, both of which are inherent in the traditional RC
design. When reviewing Meade’s LX400-ACF Advanced Coma-Free, Sky and Telescope magazine said, “
[It] does indeed perform like a Ritchey-Chrétien. The difference between the off-axis images
(compared to a Schmidt-Cassegrain) was dramatic to say the least.”
f/8 Advanced Coma-Free Optics: The Ritchey-Chrétien or RC optical design is well known to
discerning astrophotographers and is the telescope optical design in many of the leading
professional observatories of the world. By creating the Advanced Coma-Free design, Meade has
taken the f/8 RC optical design to another level by adding a corrector plate to reduce residual
astigmatism that is inherent in the traditional optical design. In addition many more design
features were added to the LX400-ACF for the demanding researcher and imaging enthusiast with
telescopes available in apertures of 10 inches, 12 inches, 14 inches, and 16 inches.
	  	
Series 5000 24mm 2” O.D. Ultra Wide Angle Eyepiece:
Standard equipment on all LX400 telescopes, the Series 5000 24mm 2” O.D. Ultra Wide Angle
Eyepiece represents the ultimate in eyepiece design and technology delivering extremely high
resolution, contrast and full-field sharpness over an astounding 82° apparent field-of-view. Only
the highest quality materials were selected to create this extraordinary eyepiece. The designs
required several different types of exotic glass in order to achieve the highest level of optical
performance.
	  	
New Carbon Graphite & Kevlar Tube:
The carbon graphite and Kevlar tube is a unique light-weight, high strength material with
ultra-low expansion characteristics that will maintain the spacing between the optics, so that
focus settings do not change with outside temperature changes. This is a critical feature to
astrophotographers. Instead of forcing a perfectly round shaped tube assembly, the tube is shaped
around the mechanisms and drive system of the front focus and collimation assembly, giving the
LX400-ACF its unique look and style.

New Rear and Front Cell Architecture:
The front and back cells of the LX400-ACF are designed to allow the maximum amount of air-flow
around the optics, in order to achieve the quickest ”cool down” times. To accelerate cool-down
time, a built-in fan on the rear cell can be turned on and off through the AutoStar II handbox.
The rear cell additionally incorporates a multi-port panel with 3 USB ports, a port for an
autoguider, AutoStar II handbox, illuminated reticle, RS232, and one for future ”Smart”
accessories.
	  	
LX400 Drive Base:
The multi-port panel of the LX400 drive base includes a special single High-Speed USB 2.0 input
port allowing simultaneous control over the telescope and either the Meade LPI or Deep Sky Imager
camera through Meade’s AutoStar Suite software. Additionally there are ports for a power cord
input, the AutoStar II handbox, a DB-9 auxiliary port, 12v out power port, and RS-232.
Additionally the LX400 includes the familiar on/off switch and LED power light indicator.
	  	
New Ultra-Stable Tripod:
Standard equipment for LX400 10”, 12”, and 14” telescopes, the patent pending trigger release leg
locks of the Ultra-Stable tripod are positioned at the top of the tripod legs for easy access.
 
ALL - NEW OPTICAL SYSTEM
The LX400 Advanced Coma-Free Optical System
It is generally accepted that the Ritchey-Chrétien or Classical RC system is the premiere optical
design for medium to large aperture astronomical telescopes. The primary benefit of a Classical RC
is the fact that it is an aplanatic design which means it is coma-free. Coma is an optical
aberration that causes star images to appear comet like with tails that point away from the
center of the field of view. The further from the center, the larger the effect. Fast Newtonians
suffer from this aberration the most, followed by other reflecting optical systems of various
designs. The Schmidt-Cassegrain or Schmidt-Newtonian design typically has ½ the coma of a
Newtonian of the same focal length. The Classical RC design uses a hyperbolic primary mirror and
a hyperbolic secondary mirror to create an aplanatic optical system which has no coma. This
system produces small round star images all the way to the edge of the field of view.

Meade’s engineering team recognized the advantages of the Classical RC design but explored the
possibility of using Meade’s unique engineering and manufacturing expertise to improve on the
basic design. The result is the LX400 optical system which is also an aplanatic, coma-free design
with small round star images to the edge of the field. The LX400 design is very similar to the
Classical RC and achieves the same benefits by using a hyperbolic secondary with a new advanced
front corrector plate and primary mirror that together perform as a hyperbolic primary. This
design has several advantages over the Classical RC design.

    * The LX400 eliminates the secondary mirror holder support vanes (spider) that cause
diffraction spikes. Because almost all reflecting telescopes produce diffraction spikes, many
people are used to seeing them and don’t consider them an aberration. But in reality, they are a
large distortion that reduces image contrast, lowers resolution and presents an unrealistic view
of the sky to the eye or the astro-imager.
    * The LX400 design reduces the amount of astigmatism that is inherent in the Classical RC
design.
    * The LX400, due to the front corrector plate, is a closed tube design. This keeps the
primary optical components protected from dust, moisture and other contaminates that might fall
on the optical surfaces of the primary and secondary mirrors.

While the LX400 optical system is as difficult to manufacture as a Classical RC, it was chosen
because of its superior performance (i.e., no diffractions spikes, reduced astigmatism and closed
tube). Due to Meade’s years of experience in designing and manufacturing sophisticated corrector
plates and optical systems, we are in a position that very few, if any, other companies enjoy.
Applying this expertise and Meade’s resources, we are able to produce this advanced optical
system at a fraction of the price that other companies would have to charge, if they could
produce it at all.
 

Precision GPS Alignment:
Telescope alignment is accomplished automatically using signals from the Global Positioning
System (GPS), a satellite system that enables extremely precise communication to the telescope of
the observer’s latitude and longitude, as well as local time. Integrated True-Level and North
electronic sensors in combination with a high-sensitivity Sony GPS receiver located in the
left-hand fork arm result in accurate telescope alignment to the sky at the touch of a button:
Just press the ENTER button on the Autostar II hand controller and watch as the telescope
measures level, points North, and slews at 8°/sec. to its first alignment star. Magnetic
declination compensation designed into the telescope software automatically engages during the
alignment process.

Software Downloads and Satellite Tracking:
The software included in Meade LX400 telescopes is under continuous factory review; updates to
this software are published at regular intervals on Meade’s website. Importantly, the latest
software version, as well as custom and updated guided tours, comet and asteroid positions, may
be downloaded in minutes from Meade’s website. Additionally, current Earth satellite orbital data
(including the International Space Station, Space Shuttle, etc.) may be downloaded; the telescope
then automatically acquires and tracks the satellite at the correct tracking rate. The
telescope’s flash memory may be upgraded through one of the RS-232 ports with new software or
data as they become available on Meade’s website.

Expanded Database and Larger User Memory:
The LX400 database has been expanded over the standard library of the LX200GPS to include 180,000
objects. In addition to more stars from the Hipparchos/Tycho catalog, we have added::

• The popular ”Lunar 100” with the finest features to see and image on the Moon
• A subset of the finest visual doubles from the Washington Double Star Catalog
• The PK Catalog of Planetary Nebulae
• The Hickson Catalog of Dense Galaxy Clusters
• The Gleason Catalog of Nearby Stars
• The Landolt Catalog of Photometric Standard Stars
• The Sharpless Catalog of HII Regions

Laser Aligned, Fixed Primary Mirror:
The primary mirror is laser aligned to the true optical path, then float bonded in place. It is
fixed, but literally floats on a layer of adhesive that results in zero stress to the glass and
no distortion to the optics (unlike mirror cells or floating point pads). There is no mirror
movement.

Field Operation:
LX400 scopes operate from eight C-cells neatly stored inside the fork arms. Alternately,
telescope powering may be effected from an automobile cigarette lighter plug (using the optional
#607 Power Cord) or from a standard home outlet (using the new optional AC Adapter).

#929 2” Diagonal with UHTC:
Standard equipment on all LX400 telescopes, attaches to the rear cell of and permits the use of
wide-field 2” O.D. eyepieces. Each diagonal includes a Meade optical-flat mirror of Pyrex glass,
UHTC-coated for maximum reflectivity.

Built-In Dew Heater:
Instead of wrapping a heating element around the telescope’s optical tube assembly to send heat
through the telescope’s front cell to prevent dew from forming on the corrector plate, the LX400
incorporates a nickel-chromium wire heating element that is in contact with the glass of the
corrector plate that quickly, efficiently, and safely sends heat through lens using the lowest
power drain possible. With two onboard temperature sensors, one to measure ambient temperature
(placed inside the fork arm) and one to measure the temperature of the corrector plate, the LX400
can be set to have the built-in dew heater keep the corrector plate warmed to a user-defined
setting above ambient temperature. By only using the dew heater precisely when needed, battery
usage is managed to its optimum. All functions to operate the dew heater are controlled by the
AutoStar II handbox.

Precision Encoder-Measured Digital Focusing:
With a laser aligned primary mirror fixed in position, focusing is performed electronically and
digitally by precisely moving the entire front cell in increments as fine as 1/100 of a
millimeter. Digital readout of the focus position can be read on the telescope’s AutoStar II
handbox. There are 4 different focusing speeds from fine to fast. Since the process is
accomplished without moving the primary mirror, the entire assembly is virtually free from image
shift.

High-Precision Pointing (HP) Capability:
Meade LX400 models permit the most accurate pointing capability ever offered in a commercial
telescope. Now you can command the telescope to GO TO an object located on the opposite side of
the sky (for example, a distance of 120 degrees in sky-angle) and, in conjunction with the
telescope’s unique SYNC command, the LX400 locates and centers the desired object. HP capability
is accessible in either the altazimuth or equatorial orientations.

Precision Electronic Optical Collimation:
Collimating a Cassegrain telescope has never been easier. LX400 owners will make precision
collimation adjustments to the secondary mirror of the telescope by using the arrow keys of
AutoStar II handbox, allowing a single person to simultaneously make adjustments and see the
results. In addition, Meade precision collimates the optics at the factory and then sets that
position as the default setting. So in the case where one may make a mistake in making a
collimation adjustment, the default setting can always be used.

Smart Drive Permanent Periodic Error Correction (PPEC):
Included as standard equipment, the Smart Drive permits a professional level of drive-rate
precision. No longer are large systems required, worm gear when smaller gears coupled to Smart
Drive software can achieve periodic errors of 5 arc secs or less-an observatory standard of
precision. All worm/worm-gear combinations, no matter how well made, have minor inaccuracies that
manifest themselves as periodic errors in the telescope tracking rate, with the period dependent
on the worm’s rate of rotation. To program the Smart Drive the observer guides on an object
visually, making corrections with the handbox controller. The software then remembers these
corrections, stores them in memory, and in the future automatically compensates for the periodic
errors of the gear system. Smart Drive user programming is stored in the telescope’s computer
memory forever, independently of any power source, unlike other periodic error correctors that
must be reprogrammed each time you use the system. The Smart Drive can be erased, updated, or
even averaged with future programming at the user’s option. The significant value of the Smart
Drive is immediately appreciated during long-exposure astrophotography, where the resulting low
periodic error of the system enables relaxed guiding with a minimum of handbox corrections. In
CCD imaging, where short exposures of deep-space objects are often all that is required for
stunning results, the Smart Drive often permits imaging without any guiding requirements at all.

Heavy-Duty Fork Mounts:
LX400 fork mounts are the strongest, most rigid mountings ever made available for telescopes of
these apertures. Fork arms, are both longer and stronger. This allows the 10”, 12” and 14” scopes
to go all the way to 90 degrees declination on a wedge, allowing you to reach the horizon. The
increased fork size also gives more back clearance to allow imaging all the way to the pole with
most cameras. DC-servo-motor-controlled (12v DC) worm gear drives with almost two hundred
selectable drive speeds, combined with the Meade Smart Drive on both telescope axes, permit
observatory-level precision in tracking, guiding, and slewing. Photo-guide speeds are selectable
from 0.01x to 1.0x sidereal, in increments of 0.01x; fast-slew speeds are selectable from 1°/sec.
to 8°/sec. in 0.1°/sec. increments. Use the 8°/sec. speed for rapid motion of the telescope across
the skies; once near the target, switch instantly to a speed of 1.5°/sec. or 3°/sec. for centering
in the viewfinder. Observing in the main telescope, use the 16x or 64x sidereal speed to place the
object in the center of the field.
	  	
Computer Optimized Internal Baffling: Unlike traditional Schmidt-Cassegrain designs, the
primary mirror moves along a baffle tube in order to achieve focus, Meade’s LX400 primary mirror
is mounted independent of the baffle tube. This allowed Meade’s engineers to take full advantage
of the baffle design to create full stray light cut-off performance, in order to produce the
maximum contrast. Additionally the secondary baffle, machined of aluminum with its distinctive
outer knife-edges further minimizes stray light in the optical path.

Focus Position Presets:
By setting up to 9 focus positions, LX400 owners can customize perfect focus from observer to
observer with different eyesight (similar to the custom settings in luxury cars to change the
mirror, seat, and steering wheel settings from one driver to another). The feature is also very
useful when using switching to various eyepiece and Barlow lens combinations or from a visual
setup to a camera setup.

UHTC Coatings:
Standard on all LX400 telescopes, the importance of Meade’s proprietary UHTC group becomes
apparent when comparing total telescope light transmission, or throughput, caused by the
multiplier, or compounding, effect of the four optical surfaces. With each optical surface
contributing significantly to telescope light throughput, the effect of all four surfaces
combined is indeed dramatic. At the H-a wavelength of 656nm., total transmission increases from
76.7% to 88.5%, an increase of 15.4%; at the helium wavelengths of 588nm. and 469nm. - strong
emission lines in hot planetary nebulae - total telescope transmission increases by 13.8% and
16.8%, respectively; at the two nitrogen II lines of 655nm. and 658nm. and at the sulfur II line
of 673nm., transmission is increased by 16%. Averaged over the entire visible spectrum (450nm. to
700nm.), total light transmission to the telescope focus increases by about 15%.
More Info about UHTC

Smart Mount:
Revolutionary Smart Mount technology is standard equipment on all LX400 telescopes. Smart Mount
improves the pointing accuracy of your LX400’s telescope’s ”Go To” system with the following
features:

• Constantly improved pointing accuracy with every object centered and sync’ed.
• Works with both equatorial and altazimuth configurations.
• Simple routine to refine pointing accuracy for the entire sky with your equipment configuration
and alignment.
• Refined pointing data can be saved and reused for permanent and portable setups.

Altazimuth and Equatorial Operation:
For all visual observing applications, for lunar and planetary photography, and for many CCD
imaging applications, Meade LX400 may be set up in the altazimuth mode - just attach the
telescope’s drive base directly to the tripod, use the GPS alignment procedure, and the
telescope’s computer actuates 2-axis tracking that keeps objects precisely centered in the field,
even at high powers, during the entire observing session. For long-exposure astrophotography
altazimuth-induced field rotation requires the new Ultrawedge or the #1220 (for 10”, 12”, 14”,
and 14” models) Field De-rotater, either of which may be purchased separately.

	

Specifications:
  LX400 14” Telescopes

    * Includes 14” Advanced Coma-Free (D=356mm, F=2845mm, f/8) optical tube assembly with
Ultra-High Transmission Coatings (UHTC) standard;
    * 4 speed front focusing mechanism;
    * Heavy-duty fork mount with 4”-diameter polar ball bearing, dual-axis 5.75” worm gears, and
2 multi-function, multi-port control panels;
    * Manual and electric slow-motion controls on both axes;
    * Thermal stabilization fan
    * Setting circles in RA and Dec;
    * Autostar II control system, 4-Megabyte flash memory, digital readout display,
permanently-programmable Smart Drive and 185-speed drive controls on both axes, High-Precision
Pointing, and 180,000-object onboard celestial software library;
    * GSP alignment system with extended sensitivity Sony GPS receiver, magnetic declination
compensation, and true-level and North electronic sensors;
    * Smart Mount which improves the pointing accuracy of your LX400 telescope’s ”Go-To” system;
    * 12v DC telescope power supplied from internal battery compartments accepting 8
(user-supplied) C-cells (optional 25ft. cords are available for powering from auto cigarette
lighter plug or form 115v AC);
    * 8 x 50mm viewfinder;
    * 2” diagonal mirror with UHTC and 1.25” adapter;
    * Series 5000 Ultra Wide Angle 2” O.D. 24mm eyepiece;
    * LX400 Ultra-Stable variable-height tripod;
    * Operating instructions

Aperture
14”
Focal Length
2845mm
Focal Ratio
f/8
Weight w/o Tripod
121 lbs.
Length (OTA + mount)
23.5”
Width (OTA + mount)
19”
Height (OTA + mount)
38.75”
Series 5000™ Eyepiece
24mm UWA
UHTC™
Included

UHTC



An important optional feature to optimize the performance of your Meade
telescope.

Image brightness in a telescope is crucially dependent on the reflectivity of
the telescope’s mirrors and on the transmission of its lenses. Neither of
these processes, mirror-reflectivity or lens-transmission, is, however,
perfect; light loss occurs in each instance where light is reflected or
transmitted. Uncoated glass, for example, reflects about 4% of the light
impacting it; in the case of an uncoated lens 4% of the light is lost at
entrance to and at exit from the lens, for a total light loss of about 8%. 
Early reflecting telescopes of the 1700’s and 1800’s suffered greatly from mirrors of poor
reflectivity- reflection losses of 50% or more were not uncommon. Later, silvered mirrors
improved reflectivity, but at high cost and with poor durability. Modern optical coatings have
succeeded in reducing mirror-reflection and lens-transmission losses to acceptable levels at
reasonable cost.

Meade Standard Coatings: The optical surfaces of all Meade telescopes include high-grade optical
coatings fully consistent in quality with the precision of the optical surfaces themselves. These
standard-equipment coatings include mirror surfaces of highly purified aluminum, vacuum-deposited
at high temperature and overcoated with silicon monoxide (SiO), and correcting lenses coated on
both sides for high light transmission with magnesium fluoride (MgF2). Meade standard mirror and
lens coatings equal or exceed the reflectivity and transmission, respectively, of virtually any
optical coatings currently offered in the commercial telescope industry.

The Meade UHTC Group: Technologies recently developed at the Meade Irvine coatings facility,
however, including installation of some of the largest and most advanced vacuum coating
instrumentation currently available, have permitted the vacuum-deposition of a series of exotic
optical coatings precisely tuned to optimize the visual, photographic, and CCD imaging
performance of Meade telescopes. These specialized, and extremely advantageous, coatings are
offered here as the Meade Ultra-High Transmission Coatings (UHTC) group, a coatings group
available optionally on many Meade telescope models.

In Meade catadioptric, or mirror-lens, telescopes (including the ETX-90EC, ETX-105EC and
ETX-125EC; LX10, LX90, and LX200GPS Schmidt-Cassegrains; and LXD55-Series Schmidt-Newtonians)
before incoming light is brought to a focus, it passes through, or is reflected by, four optical
surfaces: the front surface of the correcting lens, the rear surface of the correcting lens, the
primary mirror, and the secondary mirror. Each of these four surfaces results in some loss of
light, with the level of loss being dependent on the chemistry of each surface’s optical coatings
and on the wavelength of light. (Standard aluminum mirror coatings, for example, typically have
their highest reflectivity in the yellow region of the visual spectrum, at a wavelength of about
580nm.)

Mirror Coatings: Meade ETX, Schmidt-Cassegrain, and Schmidt-Newtonian telescopes equipped with
the Ultra-High Transmission Coatings group include primary and secondary mirrors coated with
aluminum enhanced with a complex stack of multi-layer coatings of titanium dioxide (TiO2) and
silicon dioxide (SiO2). The thickness of each coating layer precisely controlled to within +/-1%
of optimal thickness. The result is a dramatic increase in mirror reflectivity across the entire
visible spectrum; at the important hydrogen-alpha wavelength of 656nm. - the predominant
wavelength of emission nebulae - reflectivity is increased from 89% to over 97%. 

Correcting Lens Coatings: Meade telescopes ordered with the UHTC group include, in addition, an
exotic and tightly-controlled series of coatings on both sides of the correcting lens or
correcting plate, coatings which include multiple layers of aluminum oxide (Al2O3), titanium
dioxide (TiO2), and magnesium fluoride (MgF2). Per-surface light transmission of the correcting
lens is thereby increased at the yellow wavelength of 580nm., for example, to 99.8%, versus a
per-surface transmission of 98.7% for the standard coating.

The importance of the UHTC group becomes apparent when comparing total telescope light
transmission, or throughput, caused by the multiplier, or compounding, effect of the four optical
surfaces. With each optical surface contributing significantly to telescope light throughput, the
effect of all four surfaces combined is indeed dramatic, as demonstrated by the graphs on the
facing page, as well as by the table of the brightest nebular emission lines. At the H-alpha
wavelength of 656nm., total transmission increases from 77% to 93%, an increase of 93/77 or 21%
at all three nitrogen-III and sulfur-II wavelengths of 655nm. and 673nm.- prominent lines in
certain galactic nuclei and in supernova remnanats such as the Crab Nebula- transmission
increases by 21%; ; at the helium wavelengths of 588nm. and 469nm. - strong emission lines in hot
planetary nebulae - total telescope transmission increases by 18% and 19%, respectively; at the
two nitrogen II lines of 655nm. and 658nm. and at the sulfur II line of 673nm., transmission is
increased by 21%. Averaged over the entire visible spectrum (450nm. to 700nm.), total light
transmission to the telescope focus increases by about 20%.

Observing with the UHTC: Meade ETX, Schmidt-Cassegrain, and Schmidt-Newtonian telescopes equipped
with the UHTC present dramatically enhanced detail on the full range of celestial objects - from
emission and planetary nebulae such as M8, M20, and M57 to star clusters and galaxies such as M3,
M13, and M101. Observations of the Moon and planets, since they are observed in reflected (white)
sunlight, benefit in image brightness from the full spectrum of increased transmission. The
overall effect of the UHTC is, as it relates to image brightness, to increase the telescope’s
effective aperture. Image brightness (i.e., the ability to see faint detail) of the Meade 10”
LX200GPS is, for example, effectively increased by about one full inch of aperture.


Emission Line
Wavelength (nm.)
Transmission: Standard Coatings
(%)
Transmission: UHTC Group (%)
Increase*
Hydrogen-alpha (Ha)
656
76.9
93.1
21%
Hydrogen-beta (Hß)
486
75.3
85.8
14%
Oxygen III
496
76.5
85.4
12%
Oxygen III
501
77
85.4
11%
Helium II
496
72.5
86.1
19%
Helium I
588
79.5
93.5
18%
Nitrogen II
655
77
93.2
21%
Nitrogen II
658
76.7
92.8
21%
Sulfer II
673
75.7
91.8
21%

* The % increase is obtained by dividing the UHTC-transmission (column 4) by the
standard coatings transmission (column 3).

Effects on CCD Imaging: While the human eye loses sensitivity to light beyond wavelengths of
about 700nm., CCD imaging chips remain sensitive to about 750nm. and longer, wavelengths at which
the reflectivity of an aluminum coating is near its lowpoint. Importantly, however, the UHTC’s
total light transmission at 750nm. is 83%, vs. 72% for standard coatings, an increase of 83/72,
or 15%.