DayStar Filters SolaREDi 66 User manual

DAYSTAR FILTERS SOLAREDI 66
Congratulations on your purchase of a SolaREDi 66 Hydrogen Alpha
solar telescope. Please read this manual before using the product.
To use the telescope, plug in the included power supply, then insert
a diagonal and eyepiece (not included) in the rear of the telescope
and set the focus to about 5½. Turn the tuning knob to point
straight away from the indicator light. When the light turns green in
about 5-15 minutes your viewing experience can begin.
Warnings:
Do not disassemble the filter, the blocking element is separated from the
etalon and the complete assembly must be used together for safe
viewing.
Do not power the filter from a computer or cell phone charger as the
SolaREDi 66 requires a high current power supply (> 1.5A) for operation.
For assistance:
Call: 1 [phone]
Email: [e-mail]
Visit: http://www.daystarfilters.com

Cautions & Warnings:
There are no user serviceable parts inside the SolaREDi 66. Do not
disassemble the unit. Certain components are under pressure and
disassembly can cause permanent damage. All elements are required
for proper operation and removal of any internal component will cause a
malfunction that could result in unfiltered light which can cause blindness
or damage to equipment.
Solar Observing with a telescope is sensitive to certain risks.
•Caution and care of the telescope and filter is advised in
assembly, use and dismantling at all times.
•We recommend leaving the front cover on the telescope until the
diagonal and eyepiece are installed, and the telescope is pointed
at the Sun.
•While observing, owners must take care and caution that all
parts of the filter and telescope assembly are properly affixed
and that no pieces have been opened, tampered with or
removed.
•Responsible owners will be prudent to inform guest or novice
observers of the special nature of the telescope configuration so
not to imply that telescopic observing of the sun is safe without
proper filtration.
A few very important points that owners and operators must
understand:
•DayStar filters are temperature sensitive. Changing the
temperature will change the wavelength (CWL) that the filter will
transmit. Users need to be aware of temperature tuning issues.
•Because of the need for temperature regulation, a power
supply is required.
•The F/14 focal ratio of this telescope is longer than common
nighttime telescopes, and as such, consideration must be
given to using longer focal length eyepieces and larger format
image sensors for satisfactory viewing of the Sun. Eyepieces
shorter than approximately 12mm will outresolve the diffraction
limit and not add additional detail.
•Do not twist the red filter housing relative to the focuser or the
heater wire connections may pull out.

USAGE:
The SolaREDi 66 is a 66mm F/14 refractor with an integrated telecentric
baffled barlow and Hydrogen Alpha narrowband filter for dedicated solar
observing.
The filter must be plugged in using the supplied power supply. The
etalon cavity is precision heated to regulate the wavelength of the filter
output.
Any other USB power source you wish to use must be rated for at least
1.5 amps at 5 volts. Computer USB ports and cell phone chargers do
not normally support this much power.
After letting the filter come up to temperature and settle, the light will turn
green and viewing can begin.
Finder Usage:
The included zero power finder allows you to find the sun. With your
back to the Sun, observe the dot of light that passed through the front of
the finder on the target. Move the telescope pointing until the dot of light
is in the center of the target. Then, using a low power (long focal length)
eyepiece such as a 25mm-40mm, locate the sun through the telescope
eyepiece and center it.
Due to normal manufacturing variations in the finder, telescope, and
eyepiece, the dot may not land in the middle of the target when the Sun
is centered through the eyepiece. In this instance, center the Sun in the
eyepiece, then use a 3/32” hex L wrench (not included) to loosen the
screw holding the target and move the target plate so that the dot aligns
with the target. Then carefully tighten the screw.

Eyepiece Selection:
Daystar Recommends Tele Vue Plossl series
eyepieces of 15 to 32mm focal length.
Remember that at F/14, a high powered eyepiece
can exceed Dawes' limit. Observers will find best
results with an eyepiece which is 15mm or greater.
Eyepieces of higher power will result in a dim, fuzzy
disk without the ability to focus well.
We have tested a number of eyepieces over the years. We performed a
comprehensive eyepiece comparison between various brand names and
eyepiece styles. Naglers, zooms, radians and other "fast" eyepieces
typically perform very badly on DayStar applications.
Other brands do offer Plossl eyepieces and they can give a respectable
performance in lieu of a Tele Vue. We have also found some of the very
old wide field "Erfle" eyepieces aren't bad for an experienced observer.
It should be noted that repeatedly in side-by-side tests, we found Tele
Vue brand Plossl eyepieces to offer the highest contrast, most even view
and widest exit pupil. In Solar Observing, contrast is achieved by control
of scattering. Tele Vue Plossls stand out in superior design.
Furthermore, the adjustable eye cup offers additional contrast by
allowing the user to dark adapt during sunny days.
Eyepiece features we found to increase performance include:
- "Fully Multicoated" - Of those eyepieces which did better than others,
those marked "fully multicoated" offered better views from less internal
scattering.
- Blackened optical edges - Tele Vue and other eyepieces which
performed better all had blackened edges of their optical elements. This
also reduces internal scattering within the eyepiece.
Maximizing the viewing experience:
Daytime viewing results in stray light entering your eye that can make it
hard to see through the filter. We recommend a viewing hood or cloth be
placed over your head to limit the stray light that enters your eye,
allowing fainter prominences and more surface detail to be observed. A
comfortable chair also improves the experience, allowing the eye to stay
steady for longer periods so as to pick out more subtle details on the
surface of the Sun.

Knob tuning:
If the image lacks contrast, you may need to adjust the center
wavelength of the filter.
A knob is provided to adjust the center wavelength of the filter. Turn the
knob counter clockwise to lower the wavelength towards the blue by up
to 0.5Å. Turn clockwise to raise the wavelength towards the red by up to
0.5Å. Each click of the knob is 0.1Å.
Additional tuning can be performed, just keep in mind that after every
adjustment of the knob the filter must settle in temperature for
approximately 5-10 minutes before your change becomes effective.
Tuning can also be used to observe Doppler shifted features moving
towards or away from you. A feature moving towards you will be brighter
in blue (counterclockwise) wing shift, away from you will be reddened
(clockwise knob tuning).
Energy Rejection:
Concentrated sunlight can create very high temperatures where it falls,
so care must be taken to prevent melted components or fire.
The SolaREDi 66 includes a blocking filter as the first element to receive
concentrated light. It reflects all but red Hydrogen Alpha light back out of
the front of the telescope, preventing heat from building up inside the
unit.
However, if the telescope is pointed off of the Sun by more than about 1
degree, for example when first setting up the telescope or mount, then
concentrated light can fall on the black metal portions of the inside of the
tube and cause localized heating. We do not recommend leaving the
telescope in this situation for more than a minute. We recommend
leaving the front cover on the telescope until you are ready to observe.
Please note, a Herschel Wedge or white light filter cannot be used with
the SolaREDi 66. These filters pass very little light by design and so will
result in an extremely dark image if used with the SolaREDi 66.

How it works:
Light from the objective enters the blocking filter (at left), where
wavelengths near H alpha are transmitted while the rest are reflected
back out. Red H alpha light then passes through the telecentric barlow
lens elements to achieve a slower focal ratio, more parallel light beam.
The Etalon passes a very narrow range of light wavelengths, but it is
sensitive to temperature and light angle. In the SolaREDi 66, the Etalon
is heated to approximately 100-150°F to control the wavelength passed,
and the telecentric barlow controls the angle of light entering the Etalon.
Care and cleaning:
While not in use, we recommend that users store the SolaREDi 66 with
its end caps on, in a climate controlled environment. The optical filter life
expectancy is extended up to 2-3 times by climate controlled storage.
Do not touch the internal, optical elements of the filter assembly. While
the exterior glass surface coatings are durable, they are easily
scratched. A few specks of dust will have no effect on the quality of the
image, and may be gently blown off with a squeeze bulb. Do NOT use
compressed air cans to blow dust off any optical surfaces. Small
amounts of residual 'film' will not affect visual performance. Fingerprints,
smudges and smears must be cleaned off. Preferred cleaning method is
to return the SolaREDi 66 to the DayStar Filters laboratory for proper
factory cleaning.
Do not unscrew, open or separate your SolaREDi 66 filter assembly. The
optical elements are held under pressure by design and will become
damaged if opened. Opening the optical filter assembly will void your
warranty. The safest cleaning method is to moisten a very soft, lint-free
tissue, cloth or "Qtip" with a pure acetone, methanol, or Isopropyl Alcohol
(reagent grade) and gently whisk away the stain. Do not apply solutions
directly to the glass surface. Stroke from the center of the aperture
outward only. After each cleaning stroke, use a fresh applicator. The
fewer strokes, the better! The metal housing and other non optical parts
are anodized surfaces and can be cleaned with Windex.

About Seeing Limitations and Resolution:
Solar observing seeing conditions vary greatly from nighttime conditions.
During the daytime, radiant heating from the sun affects seeing
significantly. Characterized by turbulence or shimmering as seen over a
hot street, seeing can cause significant impact on quality of solar
observations.
- Bad seeing is caused by air of different temperatures mixing. This
typically happens within the lowest 10 feet of air. It occurs most often
over pavement, dark objects, rooftops and sometimes trees.
- High cirrus clouds or “scuzz” will cause scattering of sunlight in the high
atmosphere which often makes for bad viewing conditions. A classic
sign of high cirrus clouds is the inability to achieve focus, or the need to
“chase focus”, or a lack of contrast.
- A jet-stream moving overhead can also hurt seeing conditions even on
a clear day.
DayStar Filters are high power viewing platforms and this high resolution
can be susceptible to seeing issues. Solar Observers using high
powered, high resolution telescopes and DayStar filters should heed
daytime seeing. While many of these conditions are beyond our control,
observing in an area with ideal conditions, without pavement in the
direction of viewing, and on days with no high cirrus will offer best
results. Grass is the best environment for daytime seeing stability.
Each observing location offers different behavior for daytime seeing cells
at different times of the day, as the air through which one views changes
with movement of the sun. Some locations benefit from best seeing in
the morning, while many have best seeing in the afternoon. Because
most heat variation between air and ground surfaces occurs within the
first 10 feet above the ground, often a high observing platform will offer
superior seeing. This might include a second story deck which overlooks
grass.

Solar Imaging Tips:
Daystar recommends
MONOCHROME CCD
imaging whenever
possible for best results.
The recent availability of
CCD cameras and DSLR
cameras has offered a
simple opportunity for
solar observers to image
the Sun in Hydrogen
Alpha with a Digital SLR
camera. Please be advised, however, that due to the nature of
monochromatic light and its effects on a CCD camera, certain negative
effects are likely to occur.
The DSLR imager must be aware that most camera manufacturers
(Canon and Nikon) use an IR blocking filter which greatly reduces the
transmission of Hydrogen Alpha light. DSLR cameras without this IR
blocking filter will have better sensitivity imaging in Hydrogen Alpha.
The imager should also appreciate that even after considering IR
blocking filters, that the COLOR CCD chip is constructed in a way that
only 1 in 4 pixels detect red light. The other 3 sensors only detect blue
and green because the pixels are actually permanently covered with a
colored dye for each corresponding color. So a color CCD chip (in a
DSLR or a CCD camera) will only offer 1/4 the sensitivity and 1/2 the
resolution of a monochrome chip.
Another effect present in CCD imaging of
monochrome light of Hydrogen Alpha is the
interference pattern - or Newton's Rings. The
effect is similar to interference testing of an optical
surface between two flat surfaces. The sensor
and cover slip cause a small interferometer inside
the camera and cause a Newton's Ring moire'
pattern. The CCD chip must be tilted to a minor
degree to prevent this pattern. Recent advances
in aftermarket adapters offer a simplified solution for the issue. This
effect is a concern for both color and monochrome sensors.
An optional accessory is available from DayStar (MG-0408) which can be
used between the DSLR and SolaREDi 66 to adjust the light angle and
extinct the interference pattern.

Exposure time:
Imaging solar vs. nighttime astrophotography is very different. Dark sky
imaging requires long exposure times to capture enough light. Solar
imaging offers ample light, so exposures should be very short. Plus,
fluctuations in seeing dictate that short <1/10 second frame rates will be
better, as seeing cells move quickly to distort the image and can come
and go during a long exposure.
•Short exposure webcam imagers are better than long exposure
CCD cameras when imaging the sun.
•Because the sun has a range of brightnesses, automatic
exposure doesn’t work well. A software interface that allows the
user to control the exposure settings manually is very important.
Exposures for prominences taken through a DayStar with a webcam
style camera might be about 1/15 – 1/100
th
of a second. Exposures for
surface detail would be even shorter exposure with about 1/300 to
1/500
th
of a second.
Bit depth:
Solar activity encompasses a wide dynamic brightness range from bright
solar flares to faint eruptive or floating prominences quite a distance from
the solar limb. In order to capture all these features, we recommend the
use of 12 bit or 16 bit cameras. Normal 8 bit cameras can be used, but
will typically only be able to image either the surface or prominences,
necessitating multiple bracketed exposures and subsequent
recombination in a computer. 12 bit or 16 bit cameras enable capturing
these features in the same exposure, simplifying the image processing.
Focal reducers:
Because of the long effective focal length at the output of the SolaREDi
66, the image scale will be quite large and small (2/3” or below) image
sensors will only capture a fraction of the whole solar disk in one frame.
Large pixel sizes (9 microns and above) will enable a larger field of view.
Alternatively, a focal reducer can be employed
between the SolaREDi 66 and the camera. Simple
1.25” screw in focal reducers can be attached to the
camera nosepiece to allow a wider field of view with
small (1/2”, 1/3”, ¼”) sensor cameras. More
distance between the focal reducer and camera
surface will result in more focal reduction and larger field of view.

Features of the Sun in Hydrogen Alpha:
By observing the sun
with a narrow
bandpass filter tuned
to 6562.8Å, we can
observe the behavior
of the Sun's
Chromosphere. The
chromosphere is like a shell of gas around the Sun's photosphere,
always moving and changing. The chromosphere's structure behaves
differently in active regions than quiet areas, where magnetic field
lines are stronger. Thought to be tied to the photosphere, the
chromosphere is governed by magnetic forces and, yet it still has its own
IntraNetwork (IN) of material oscillating every 5 minutes.
On the limb, even a
rather wide filter of 1Å
or more will show
prominences, a
detail of the
chromosphere
projected against the
dark black contrast of
space. To observe the details of chromosphere on the face of the sun,
we need a narrower filter to eliminate more off-band light of the
photosphere and continuum. We need a filter less than 1.0Å. The
narrower the filter's bandpass, the more contrast we will see - down to
0.4Å, where prominence structure is reduced due to high velocity and
subsequent wing shift.
Filaments appear as
large, dark eyebrows
across the surface of
the Sun.
With a brightness of
about 10% of the disk
due to scattering,
they appear
dark on the surface, but on the limb, show as a prominence. Active
Region Filaments (ARF) differ from Quiescent Region Filaments (QRF).
ARF are darker, smaller and have more coherent fibril structure along
their axis. A sheared magnetic field runs parallel to this axis, permitting a
sizeable flare. QRF may produce a big Coronal Mass Ejection (CME). An
ARF may erupt and reform several times.

Spicules dominate
the chromospheres in
non-active regions
and have been
studied exhaustively.
They are barely
visible, last only about
15 minutes, and resemble a "burning prarie". Some jets
can be seen shooting 10,000 km up from the Sun's limb at velocities of
about 30km/sec. Studied exhaustively, they present a number of
observing challenges, as they are too small to resolve and move so
quickly as to present wing-shift challenges.
Active Regions are a
concentration of
magnetic acitivity with
several types of
features contained in
a close area.
Field Transition
Arches (FTA's)
connect P and F
spots – elements of
opposite polarity.
Inside an active
region, where
sunspots are
originally linked by a
FTA, a shear boundary forms. Field Transition Arches are different from
filaments in that they are thin and not very dark. The
FTA usually has plage or granular structure underneath.
Plages: Most of the
active region area is
occupied by plage.
Considerable
atmospheric heating
takes place in the
plage. It is bright in
everything from Halpha to the Calcium H and K lines. This heating is
thought to account for an absence of spicule. While absent over plage,
spicule are prominent around its edges.

Ellerman Bomb: A
remarkable feature of
Emerging Flux
Regions is the
Ellerman bomb.
Bright points with very
broad H-alpha wings (±5Å) that are low in the atmosphere so they are
not visible on H alpha centerline. Called 'moustaches' for their
appearance on spectrograph, they appear spectroscopically like wide
moustaches with a gap in the middle. This strange and tiny feature
typically occurs at the center of the EFR or in the edges of spots - where
the field is breaking the surface.
Solar Flares are intense, abrupt releases of energy which occur in areas
where the magnetic field is changing by flux emergence or sunspot
motion. Stresses in lines of force build up slowly and are released in
flares. They occur most frequently at neutral lines where a filament is
supported by horizontal sheared field lines. This event can only take
place along a magnetic inversion line. When many lines of force are
involved, two ribbons of emission appear, brightening simultaneously.
Emerging Flux
Regions: An area on
the Sun where a
magnetic dipole, or
"flux tube" is
surfacing on the disk,
eventually producing
a bipolar sunspot group. Each pole of an EFR is often marked by pores
or small developing sunspots. Surges or even small solar flares can
sometimes occur in EFRs. An EFR emerges with small bright H region
with little surges, then weak arch filaments (AFS) over bright plage
connect small spots on each dipole. Growth is rapid, forming in just a few
hours.

Troubleshooting:
Blank, featureless disk:
Ensure power is applied and LED is green.
Try moving focus in and out significantly, around the 5.5 position.
Make sure a 15 to 40mm eyepiece (not included) is installed, and
the 1.25” diagonal is installed between the focuser and eyepiece.
Ensure knob is pointing straight away from the power jack.
Poor contrast:
Check that optical surfaces are clean. Dust specks do not affect the
view, check for smudges such as oil from fingerprints.
Try adjusting wing shift knob up 3-4 clicks clockwise past center and
wait 5-10 minutes. If that does not improve the view, try down 3-4 clicks
below center and wait 5-10 minutes.
Atmospheric seeing or transparency may be poor, try again later.
Blurry image:
Blurry views are typically due to poor seeing. Poor seeing can be
caused by the presence of heat waves from concrete, asphalt, or machinery.
Weather effects like the jet stream can also cause blurring. Try moving to a
different location or else observe on a day when weather conditions are
improved.
Yellow LED indication:
Your filter is adjusting to the wavelength chosen by the knob. Wait
approximately 5-15 minutes for the temperature to adjust and then light
should turn green, indicating that the filter has settled to its required
temperature and is on band for viewing.
Yellow, never goes green LED indication:
If after 20 minutes of the same knob position setting the LED has
not turned green, the ambient temperature may be too hot or too cold to
regulate the temperature. However, the filter may still be usable while
slightly mistuned and performance may not be affected.
This can also occur if plugged into a computer USB port, which
causes the filter heater to reduce its current draw. Use the supplied power
adapter or a source rated for 1.5 amps, not a data USB port.
Red LED indication:
This usually indicates that the SolaREDi 66 is not receiving enough
voltage. If powered by battery, recharge the battery. Make sure to use the
supplied AC/DC wall adapter, as cell phone chargers and PC USB ports do
not have enough current capability for the SolaREDi 66.
Red indication can also mean an electrical fault in the SolaREDi 66
electronics. If power source changes do not resolve the red indication,
please return the SolaREDi 66 to DayStar for inspection and repair.

Specifications:
Wavelength: 6562.8Å
Tuning knob: Wing shift +/- 0.5Å in 0.1Å increments.
FWHM: Not specified. Prominence units are generally 0.6Å or
above, Chromosphere units generally 0.5Å or below.
Objective: Air spaced two element ED Apo, fully multicoated.
Aperture: 66mm
Focal Length: 936mm with focal point 94mm behind 1.25” flange.
Barlow: Integrated, fully baffled 2 element telecentric 2.4X barlow
optimized for 656nm
Blocking filter: Integrated 18mm blocking filter
Clear aperture: 19mm clear etalon aperture
Full disk: Full disk visible for eyepieces more than 18mm FL or
image sensors more than 9mm tall (1” format or larger).
Full disk in smaller sensors requires focal reducer.
Focuser: Dual speed crayford style, with 10:1 reduction and lock.
Eyepiece side: 2”-24 UNS “SCT” thread
1.25” female drawtube via included adapter with
brass compression ring to protect eyepiece.
Mounting foot: Vixen style dovetail with two ¼-20 holes.
Power: USB power, 5v 1.5amp, female Micro-B connector.
Power is required for proper operation.
Wall adapter: 90-240VAC wall adapter, includes US, UK, Euro and
Australian plugs.
Opt. battery: Optional 8-hour battery pack available.
LED indicator: Yellow: temperature settling.
Green: ready to observe, filter on band.
Red: fault such as low voltage.
Settling time: Approximately 5-15 minutes after power up or change
of wing shift.
Temperature: Ambient temperature range 40°-100°F
Dimensions: 126mm wide x 110mm tall x 446mm long
Weight: 2.3kg (4lb 15.5oz)
Includes: SolaREDi 66 telescope, power supply, user manual.
Warranty: 5 years

FCC Notice:
This equipment has been tested and found to comply with the limits for a
Class B digital device, pursuant to part 15 of the FCC Rules. These limits
are designed to provide reasonable protection against harmful
interference in a residen
tial installation. This equipment generates, uses
and can radiate radio frequency energy and, if not installed and used in
accordance with the instructions, may cause harmful interference to radio
communications. However, there is no guarantee that interfe
not occur in a particular installation. If this equipment does cause harmful
interference to radio or television reception, which can be determined by
turning the equipment off and on, the user is encouraged to try to correct
the interference by one or more of the following measures:
Reorient or relocate the receiving antenna. Increase the separation
between the equipment and receiver. Connect the equipment into an
outlet on a circuit different from that to which the receiver is connected.
Consul
t the dealer or an experienced radio/TV technician for help.
Correct Disposal of This Product:
(Waste Electrical & Electronic Equipment)
(Applicable in the European Union and other European
countries with separate collection systems)
This marking shown on the product or its literature, indicate
that it should not be disposed with other household wastes at
the end of its working life. To prevent possible harm to the environment
or human health from uncontrolled waste disposal, please se
from other types of wastes and recycle it responsibly to promote the
sustainable reuse of material resources. Household users should contact
either the retailer where they
purchased this product, or their local
government office, for details of
where and how they can take item for
environmentally safe recycling. Business users should contact their
supplier and check the terms and conditions of the purchase contract
This product should not be mixed with other commercial wastes
disposal.
Copyright:
This manual copyright © DayStar Filters 2015
, all rights reserved.
This equipment has been tested and found to comply with the limits for a
Class B digital device, pursuant to part 15 of the FCC Rules. These limits
are designed to provide reasonable protection against harmful
tial installation. This equipment generates, uses
and can radiate radio frequency energy and, if not installed and used in
accordance with the instructions, may cause harmful interference to radio
communications. However, there is no guarantee that interfe
rence will
not occur in a particular installation. If this equipment does cause harmful
interference to radio or television reception, which can be determined by
turning the equipment off and on, the user is encouraged to try to correct
Reorient or relocate the receiving antenna. Increase the separation
between the equipment and receiver. Connect the equipment into an
outlet on a circuit different from that to which the receiver is connected.
t the dealer or an experienced radio/TV technician for help.
(Applicable in the European Union and other European
This marking shown on the product or its literature, indicate
that it should not be disposed with other household wastes at
the end of its working life. To prevent possible harm to the environment
or human health from uncontrolled waste disposal, please se
parate this
from other types of wastes and recycle it responsibly to promote the
sustainable reuse of material resources. Household users should contact
purchased this product, or their local
where and how they can take item for
environmentally safe recycling. Business users should contact their
supplier and check the terms and conditions of the purchase contract
.
This product should not be mixed with other commercial wastes
for
, all rights reserved.

Warranty:
Blockers and trimmers are considered a wear item and only warranteed
on a pro-rated five year term.
Warrantor: DayStar Filters LLC
Elements of Warranty: DayStar warrants, for five years of the original
retail purchase owner, this Product to be free from defects in materials
and workmanship with only the limitations or exclusions set out below.
Warranty Duration: This warranty to the original user shall last for one
year of the original user. The warranty is invalid if the Product is (A)
damaged or not maintained as detailed in Operating and Maintenance
Manual (B) modified, altered, or used as part of any conversion kits,
subassemblies, or any configurations not sold by DayStar, or (C)
serviced or repaired by someone other than the DayStar Filters Service
Center for a defect or manlfunction covered by this warranty. This
warrantee includes shipping to and from any point inside the United
States. Insurance upon that shipping and/or international shipping and/or
any customs and/or import duties attached are the sole responsibiltiy
of the owner.
Statement of Remedy: In the event that the product does not conform to
this warranty at any time while this warranty is in effect, warrantor will
repair the defect and return it to you without charge for parts, service or
any cost incurred by the warrantor in connection with the performance of
this warranty. THE FIVE YEAR WARRANTY SET FORTH ABOVE IS
THE SOLE AND ENTIRE WARRANTY PERTAINING TO THE
PRODUCT AND IS IN LIEU OF AND EXCLUDES ALL OTHER
WARRANTIES OF ANY NATURE WHATSOEVER, WHETHER
EXPRESS, IMPLIED OR ARISING BY OPERATION OF LAW,
INCLUDING BUT NOT LIMITED TO ANY IMPLIED WARRANTIES OF
MERCHANTABILITY OR FITNESS FOR A PARTICULAR PURPOSE.
THIS WARRANTY DOES NOT COVER OR PROVIDE FOR THE
REIMBURSEMENT OR PAYMENT OF INCIDENTAL OR
CONSEQUENTIAL DAMAGES.
Procedure for obtaining performance of warranty: Upon discovery of
flaw, we require that the user communicate by telephone and/or email to
the DayStar Service department to report the failure of equipment.
Should technical support be unable to resolve the conflicts of the
product, it should be packaged in its original packaging and returned with
evidence of original purchase and note describing defect to include
owner contact information. The product should be shipped freight pre-
paid by traceable means or delivered to warrantor at:
DayStar Filters LLC
149 Northwest OO Highway, Warrensburg, MO 64093 USA
www.DayStarFilters.com - 1 [phone]