DayStar Filters QUARK User manual

DAYSTAR FILTERS QUARK
Congratulations on your purcha se of a Quark Hydrog en Alpha
“Eyepiece” solar filter. Please read this manual before using the product.
To use the filter, plug in the included power supply, then place the
Quark after your telescope’s diagonal and insert an eyepiece or
camera in the rear of the filter. Turn the knob to point straight away
from the light. When the light turns green in about 5-10 minutes
your viewing experience can begin.
To prevent damage, we recommend using an Energy Rejection Filter on
telescopes of 80mm aperture or more, or when tracking the Sun for long
periods. This can be a UV/IR cut filter mounted before the diagonal, or a
full aperture red or yellow glass ERF mounted in front of the telescope.
Warnings:
Do not disassemble the filter, the bl ocking element is separated from the
etalon and the complete ssembly must be used together for safe viewing.
Do n ot po wer the filter from a computer or cell phone charger as the
Quark requires a high current power supply (> 1.5A) for operation.
For assistance:
Call: 1 [phone]
Email: servi [email protected]
Visit: http://www.da ystarfilters.com

Cautions & Warnings:
There are n o use r se rviceable pa rts inside the Quark. Do not
diassemble t he unit. Certain components are under p ressure a nd
disassembly can ca use permanent damage. All el ements 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 telescop e and filter is advised in
assembly, use and dismantling at all times.
 Telescope owners must use caution when affixing the filter to the
telescope ne ver to poi nt any telesco pe at the sun without th e
solar filter safely installed first.
 While ob serving, owners must take care and ca ution that all
parts of the filter and telescope a ssembly are pro perly affixed
and th at no pie ces h ave be en opened, tam pered with or
removed.
 Owners must also use caution when the telescope is being
assembled and dismantled to assure the telescope is never
pointing at the sun without the solar filter properly installed.
 Responsible owners will be prud ent to inform guest or novice
observers of the special nature of the telescope configuration so
not to imply that telescopi c observing of the sun is safe without
proper filtration.
A few very important points that owners and operators must
understand:
• DayStar filters are rear-mounted and can be applied to a
choice of telescopes if applie d p roperly. If app lication i s
incorrect, the filter will not perform as specified.
• DayStar Filters a re interferen ce filters. If light reaches a
DayStar Filter at an angle, it will cause wavelength
wingshift. For our application on a telescope, DayStar owners
need F/1 5 to F/30 light, so we need to alter you r telescope’s
F/ratio in order to reach F/15 to F/30 where your DayStar will
operate correctly. Best performance is at F/27-F/32.
• DayStar filters are temperature sensitive. Changi ng the
temperature will change the wavelength (CWL) that the filter will
transmit. Users need to be aware of temperature tuning issues.

USAGE:
The Quark is de signed for use o n F/4 to F/9 refractors. Combined with
an integrated 4.3x telecen tric barlow, this results in a F/17 to F/38 final
image respectively, to provide the best performance from your filter.
Because of the incl uded barlo w, ima ges will a ppear 4x larg er than
without the Quark, and ample additional backfocus is available.
The filter mu st be plu gged in usi ng th e su pplied power supply. The
etalon cavity is precision heated to regulate the wavelength of the filter
output.
Any other US B power source you wi sh to use m ust be rated fo r at least
1.5 amps at 5 volts. Co mputer USB ports and cell phone chargers d o
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.
Knob tuning:
If the imag e la cks contrast, you may nee d t o adj ust th e ce nter
wavelength of the filter.
A knob is provided to adjust the center wavelength of the filter. Turn th e
knob counter clockwise to lower the wavelength towards the blue by u p
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.
Tuning i s required on tele scopes with “droop” of th e focu ser, be cause
even very sli ght tilts will effectivel y lower th e ce nter wavelengt h of the
filter. Turn the kno b clockwise 2-3 clicks and wait 5-10 minutes to see if
the view is improved.
Additional tu ning can be performed, j ust ke ep in mi nd that after every
adjustment of the knob the filter must settle in tempera ture for
approximately 5-10 minutes before your change becomes effective.
Tuning can also b e use d to observe Doppler shifted feature s 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 sunli ght can create ve ry high tem peratures where i t falls,
so care must be taken to prevent melted components or fire.
For brief observing sessio ns with le ss than 80m m of apertu re when not
using a tracking mount, it can be OK to use no energy rejection at all. Be
alert for any rise in temperature of your telescope, diagonal, or Quark.
For tele scopes un der approximately 120mm of
aperture, a scre w in UV /IR cut filter can be
employed in front of the telescope diagonal. The
UV/IR cut filter reflects UV and IR light back out
the front of the telescope, reducing temperatures
inside. Do not use a UV/IR cut filter with oil
spaced o bjective tele scopes, or any telescope
with an integrated rear field flattener or Petzval lens. The UV/IR cut filter
must be the first optical element to receive concentrated light.
For b est pe rformance, a red o r
yellow gla ss front mount Energy
Rejection Fil ter sh ould b e use d.
This prevents almost all heat from
entering the telescope, an d is the
safest opti on. Mo dels are
available fo r up to 1 0 i nches of
aperture an d are cu stom built for
each DayStar filter owner. Please
measure the outside di ameter of
the front of your tele scope’s d ew
shield. T his tube OD measurement is critical to e nsuring a good fit for
your ERF.
Please note, a Herschel Wedge or white light filter cannot be used with
the Quark. These filters pass very little light by design and so will result
in an extremely dark image if used with the Quark.

How it works:
Light fro m t he tele scope enters th e blo cking filter (at left), where
wavelengths near H alph a are tran smitted whil e the re st are reflected
back out. Red H alpha light then p asses through the tele centric barlow
lens elements to achieve a slower focal ratio, m ore parallel light beam.
The Etalon p asses a very narrow rang e of light wavelength s, but it is
sensitive to t emperature and lig ht an gle. In the Quark, the Etalon is
heated to a pproximately 100-150°F to co ntrol the wavelength passed,
and the telecentric barlow controls the angle of light entering the Etalon.
Care and cleaning:
While not in use, we re commend that users store the Quark with its end
caps on, in a climate controlled e nvironment. 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 a ssembly. While
the exterio r glass surface coatings a re d urable, they are ea sily
scratched. A few specks of dust will have no effect on the quality of th e
image, and may be g ently blown off with a sque eze bulb. Do NOT use
compressed air can s to blow dust off any optical surfa ces. S mall
amounts of residual 'film' will not affect visual performance. Fingerprints,
smudges and smears must be cleaned off. Preferred cleaning met hod is
to return the Quark to the DayStar Filters la boratory for prope r factory
cleaning.
Do not unscrew, open or separate your Quark filter assembly. The optical
elements are held under pressure by design and will become damaged if
opened. Opening the opti cal filter asse mbly will void your wa rranty. The
safest cleaning method is to moisten a very soft, lint-free tissue, cloth or
"Qtip" with a pure acetone, methan ol, or Iso propyl Alcohol (reagent
grade) and gently whisk away the stain. Do not apply solutions directly to
the glass surface. Stroke from the center of the ape rture outward only.
After each cleaning stroke, use a fresh applicator. The fewer strokes, the
better! The metal hou sing and othe r non optical parts are a nodized
surfaces and can be cleaned with Windex.

Eyepiece Selection:
Daystar Recommends Tele Vue Plossl series
eyepieces of 25mm, 32mm, and 40mm.
Remember t hat at F/30, a high powered eyepi ece
can exceed Dawes' limit. Observers will find best
results with an eyepiece which is 32mm or g reater
to avoid this. Eyepieces of higher power will result
in a 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 an d oth er "fa st" eye pieces
typically perform very badly on DayStar applications.
Other brands do offer Plossl eye pieces in 32-40mm and they can give a
respectable performance in lieu of a Tele Vue. We have al so found
some of the very old wide field "Erfle" eyepieces aren't ba d for a n
experienced observer. I t sho uld be noted th at re peatedly i n side-by-
side tests, we found Tele Vue brand Plossl eyepieces to offer the highest
contrast, m ost even view and wid est exit pupil. In Solar Observing,
contrast is achieved by co ntrol of scattering. Tele Vue Plossl s 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 re sults 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 ove r your he ad t o limit the stray light tha t enters yo ur 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 l onger periods so a s to pi ck out mo re subtle detail s on the
surface of the Sun.

About Seeing Limitations and Resolution:
Solar observing seeing conditions vary greatly from nighttime conditions.
During th e daytime, ra diant he ating from th e sun affect s seeing
significantly. Characterized by turbulence or shimmering as seen over a
hot street, seeing can cause significant impa ct on quality o f solar
observations.
- Bad seei ng is cau sed b y air of diffe rent tempe ratures mixing. This
typically hap pens within t he lowest 10 f eet of air. It occu rs mo st often
over pavem ent, dark obje cts, roo ftops and sometimes trees.
- High cirrus clouds or “scuzz” will cause scattering of sunlight in the high
atmosphere which often makes for b ad viewing conditions. A classi c
sign of high cirrus clouds is the inability to achieve fo cus, or th e 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 b e su sceptible to seei ng issu es. Solar Ob servers usi ng high
powered, hig h resolution telescopes a nd DayStar f ilters should hee d
daytime seeing. While many of these conditions are beyond our control,
observing in an are a wit h ideal c onditions, witho ut 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 lo cations benefit f rom best seeing in
the morni ng, while ma ny have best see ing in the afterno on. Because
most heat va riation between air and g round surfaces occu rs within the
first 10 feet above the gro und, often a high observing platform wil l 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 came ras and DSLR
cameras has o ffered a
simple op portunity for
solar ob servers t o imag e
the Sun in Hydroge n
Alpha with a Digital SL R
camera. Ple ase b e advi sed, ho wever, that due to the nature of
monochromatic light and its effects on a CCD came ra, certain negative
effects are likely to occur.
The DSLR i mager mu st be a ware t hat mo st ca mera manufacturers
(Canon a nd Nikon) u se a n IR blocking filter which greatly re duces the
transmission of Hyd rogen Alpha light. DSL R cameras without this IR
blocking filter will have better sensitivity imaging in Hydrogen Alpha.
The imag er shoul d also app reciate that even after co nsidering IR
blocking filters, that the COLOR CCD chip is constructed in a way that
only 1 in 4 pi xels detect red light. The other 3 sensors only detect blue
and green b ecause the p ixels are a ctually perm anently covere d with a
colored dye for each corresponding color. So a co lor CCD chip (in a
DSLR o r a CCD camera) will only offer 1/4 the sensitivity and 1/2 the
resolution of a monochrome chip.
Another eff ect pre sent in CCD i maging of
monochrome light of Hydroge n Alp ha is the
interference pattern - or Ne wton's Rings. The
effect is similar to interference testing of an optical
surface b etween two flat surfa ces. The sen sor
and cover slip cause a small interferometer inside
the came ra and cau se a Newto n's Ring moire'
pattern. The CCD chip m ust be tilted to a mino r
degree to p revent this pa ttern. Recent advances
in afterm arket adapte rs of fer a si mplified solution f or th e i ssue. 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 Quark to adjust the lig ht angle and extinct
the interference pattern.

Exposure time:
Imaging solar vs. nighttime astrophotography is very different. Dark sky
imaging requ ires lo ng exp osure time s to capture e nough light. Solar
imaging offers a mple light , so expo sures 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 l ong exposure
CCD cameras when imaging the sun.
 Because the sun ha s a range of brightnesses, automatic
exposure doesn’t work well. A softwa re interface that allows the
user to control the exposure settings manually is very important.
Exposures for promi nences taken th rough a DayStar with a we bcam
style camera might be ab out 1/15 – 1/ 100th of a se cond. Exposures for
surface detai l woul d be even shorte r exposure with about 1/ 300 to
1/500th 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 came ras can be u sed, but
will typically only be able to image ei ther the surface or prominences,
necessitating multiple bracke ted expo sures and su bsequent
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 outp ut of the Quark, the
image scale will be quite l arge and small (1/2” o r below) image sensors
will only ca pture a fractio n of the whole solar disk in one fram e. Larg e
pixel sizes (9 microns and above) will enable a larger field of view.
Alternatively, a focal re ducer can be em ployed
between th e Quark an d th e came ra. Simple 1.2 5”
screw in focal redu cers can be atta ched to the
camera nosepiece to allo w a wider field of view wit h
small (1/2”, 1/3”, ¼” ) sensor cameras. Mo re
distance b etween the focal re ducer and came ra
surface will result in more focal r eduction and l arger fiel d of view.

Features of the Sun in Hydrogen Alpha:
By observin g the sun
with a narro w
bandpass filter tun ed
to 6562.8Å, we ca n
observe the behavior
of the Sun' s
Chromosphere. The
chromosphere is like a shell of g as aro und the Sun' s p hotosphere,
always movi ng a nd changing. Th e chromosphere's stru cture behaves
differently in active regions than quiet areas, where magnetic field
lines are stronger. T hought to be tied to the photo sphere, 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 ag ainst th e
dark black contrast of
space. To observe the details of chromosphere on the fa ce of the sun,
we ne ed a narrower fil ter to elimin ate more off-band li ght of the
photosphere and continuum. We need a filter l ess tha n 1.0Å. Th e
narrower the filter's bandpass, the mo re contrast we w ill see - down to
0.4Å, where promi nence stru cture is reduced due t o high vel ocity and
subsequent wing shift.
Filaments appear a s
large, dark eyebrows
across the surface of
the Sun.
With a b rightness of
about 10% of the disk
due to scatterin g,
they appear
dark on the surfa ce, but on the limb, sho w as a prominence. Active
Region Filaments (ARF) di ffer from Qui escent Region Filaments (QRF ).
ARF are da rker, smaller and have m ore cohe rent f ibril structu re 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 re gions
and h ave been
studied exh austively.
They are barely
visible, last only about
15 minutes, and resemble a "burning prarie". Some jets
can be seen shooting 10,000 km up fro m the Sun' s limb at velo cities of
about 30 km/sec. Studied exhaustivel y, they pre sent a num ber of
observing ch allenges, a s they are to o small to re solve and move so
quickly as to present wing-shift challenges.
Active Regions are a
concentration o f
magnetic acitivity with
several ty pes of
features co ntained in
a close area.
Field Transition
Arches (FTA's)
connect P and F
spots – ele ments of
opposite polarity.
Inside a n active
region, w here
sunspots a re
originally linked by a
FTA, a shea r boundary forms. Field Transition Arches are differen t 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 re gion area i s
occupied by plage.
Considerable
atmospheric heating
takes p lace in th e
plage. It is bright in
everything from Halp ha to the Calci um H and K lines. Thi s he ating is
thought to account for an absen ce of spicule. While absent over plage,
spicule are prominent around its edges.

Ellerman Bomb: A
remarkable f eature of
Emerging Flux
Regions is the
Ellerman bomb.
Bright points with very
broad H-alp ha wings (±5Å) that are low in the atmosphere so they are
not visible on H al pha cente rline. Called ' moustaches' fo r their
appearance on spe ctrograph, they ap pear spectroscopically li ke wi de
moustaches with a gap i n the mi ddle. This strange and tiny feature
typically occurs at the center of the EFR or in the edg es 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 chan ging by flux e mergence or sunspot
motion. Stre sses in line s of force b uild up slowly a nd a re released in
flares. They occur mo st freque ntly at n eutral li nes where a fila ment is
supported by hori zontal sheared field lines. Thi s e vent can o nly 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 di pole, or
"flux tube" is
surfacing on the disk,
eventually p roducing
a bipolar sunspot group. Each p ole of an EFR is often marked by pore s
or small d eveloping su nspots. Surge s or even small sol ar fla res can
sometimes occur in EFRs. An EFR emerges with small bright H region
with little surges, then weak a rch filaments (AFS ) over brig ht 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 by 1-2 inches (2-5cm).
Ensure Quark is installed AFTER diagonal.
Make sure a 25 to 40mm eyepiece (not included) is installed.
Ensure knob is pointing straight away from the power jack.
Check for focuser droop, all connections between telescope and
Quark must be tight and square.
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 kn ob up 3-4 clicks clockwise past center
and wait 5-1 0 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 p oor seeing. Poo r seeing can
be caused b y the p resence of he at waves f rom concrete, a sphalt, o r
machinery. Weather effects like the je t stream ca n also cau se blurring.
Try moving to a different location or else observe on a day when weather
conditions are improved.
Yellow LED indication:
Your filter i s adjusting to t he wavelen gth ch osen by the kn ob.
Wait approximately 5-10 minutes for the tempe rature to adju st 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 for
the Quark to regulate the temperature. However, the filter may still be
usable while slightly mistuned and performance may not be affected.
Red LED indication:
This u sually indicates that the Q uark i s n ot receiving e nough
voltage. If powe red by battery, recharge the batte ry. Make su re to use
the supplied AC/DC wall adapter, as cell phone chargers and P C USB
ports do not have enough current capability for the Quark.
Red indi cation can also mean an electrical fault i n the Quark
electronics. I f power source changes do not resolve the red indi cation,
please return the Quark 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.
Compatibility: F/4 to F/9 refractor telescopes.
Not suited for off-axis (SCT or dob) application.
Barlow: Integrated, fully baffled 2 element telecentric 4.3X barlow
optimized for 656nm
Blocking filter: Integrated 12mm blocking filter
Clear aperture: 20mm clear etalon aperture
Full disk: Passes full solar disk for focal lengths under ~450mm.
Aperture limit: None, usable on large telescopes for high magnification.
For apertures over 80mm*, suggest UV/IR application
before diagonal for Energy Rejection.
Sun side: 1.25” and 2.0” combo male snouts with safety indent.
Focal point: 1.25” snout requires approx. 8mm in-focus.
2” requires approx. 10mm out-focus.
Eyepiece side: 1.25” female drawtube.
Brass compression ring to protect eyepiece.
Optional 2" and SCT accessories available.
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 5-6 minutes after power up or change
of wing shift.
Temperature: Ambient temperature range 0°-100°F
Dimensions: 55mm diameter x 71mm x 146mm long.
Includes: Quark filter, power supply, user manual.
Warranty: 5 years
*All dedicated solar tracking applications should employ energy rejection

FCC N
o
This equ
Class B
d
are d e
s
interfere
n
and can
accorda
n
commun
not occu
interfere
n
turning t
h
the inter
f
Reorient
between
outlet o
n
Consult
t
Corre
c
the end
or huma
from ot
h
sustaina
b
mixed
w
local go
v
for envir
supplier
Househ
o
disposal
.
Copyri
This ma
n
o
tice:
ipment has bee
n
d
igital device, pu
s
igned to pro
v
n
ce in a re siden
t
radiate radio fre
q
n
ce with the instr
u
ications. Ho wev
e
r in a particular i
n
n
ce to radio or t
e
h
e equipment off
f
erence by one o
r
or reloc ate th
e
the equipme nt
n
a ci rcuit differe
n
t
he dealer or an
e
c
t Disposal of
(Waste Electric
a
(Applicable i n
countries with
s
This m arking
s
that it sh ould n
of its working lif
e
n health from u
n
h
er types of wa
s
b
le reuse of m
a
w
ith o ther comm
e
v
ernment office,
f
onmentally safe
and che ck the
t
o
ld u sers shoul
d
.
ght:
n
ual copyright ©
D
n
tested and foun
rsuant to part 15
v
ide rea sonable
t
ial installation. T
q
uency energy
a
u
ctions, may cau
e
r, there i s no
g
n
stallation. If this
e
levision receptio
and on, the use
r
r
more of the foll
o
e
receiving ant
e
and re ceiver. C
n
t from that to w
ex
perienced radi
o
This Produc
t
a
l & Electronic E
q
the Eu ropean
s
eparate collectio
s
hown o n the pr
o
ot be disposed
w
e
. To preve nt po
s
n
controlled waste
s
tes and recy cle
a
terial re sources
e
rcial wastes p
u
f
or details of wh
e
recycling. Bus in
e
t
erms an d co ndi
t
d
conta ct eithe
r
D
ayStar Filters 2
0
d to comply with
of the FCC Rule
protection ag
his equipment g
e
a
nd, if not install
e
se harmful interf
e
g
uarantee t hat in
equipment does
n, which can be
r
is encouraged t
o
o
wing measures:
e
nna. In crease
t
onnect the equi
p
hich the receive
r
o
/TV technician f
o
t
:
q
uipment)
Union and ot
h
n systems)
o
duct or its liter
a
w
ith other house
h
s
sible harm to th
disposal, pleas
e
it respo nsibly t
o
. T his pro duct
s
u
rchased th is p r
o
e
re and how the
y
e
ss us ers shoul
d
t
ions of the purc
r
the reta iler w
0
14, all rights re
s
the limits for a
s. These limits
ainst ha rmful
e
nerates, uses
e
d and used in
e
rence to radio
terference will
cause harmful
determined by
o
try to correct
t
he se paration
p
ment into an
r
is connected.
o
r help.
h
er Europ ean
a
ture, indicate
h
old wastes at
e environment
e
separate this
o
promo te the
s
hould not be
o
duct, o r thei r
y
can take item
d
conta ct their
hase co ntract.
here they for
s
erved.

Warranty:
Blockers and trimmers are considered a wear item and only warrantee d
on a pro-rated five year term.
Warrantor: DayStar Filters LLC
Elements of Warranty: DayStar warrants, for five years of the original
retail purchase o wner, this Prod uct to b e free from defects in materials
and workmanship with only the limitations or exclusions set out below.
Warranty Duration: This warranty to t he original user shall last for one
year of the original u ser. The warrant y is i nvalid if the P roduct is (A)
damaged o r not maintain ed a s detail ed in Op erating and M aintenance
Manual (B) modified, altered, o r use d as pa rt of any conversion kits,
subassemblies, or any configuratio ns not sold by DayStar, or (C)
serviced or repaired by someon e other than the DayStar Filters Service
Center fo r a defe ct or manlfunction cove red by this warranty. This
warrantee in cludes shipping to a nd 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 thi s warranty is in effect, warrantor will
repair the defect and return it to you without charge for pa rts, service or
any cost incurred by the warrantor in connection with the performance of
this warranty. THE FIVE YEAR WARRANTY SET FORTH ABOVE I S
THE SOLE AND ENTIRE WA RRANTY PERTAINING TO THE
PRODUCT AND IS IN LIEU OF AND EX CLUDES AL L OTHER
WARRANTIES OF ANY NATURE WHATSOEVER, WHETHE R
EXPRESS, IMPLIED OR ARISIN G BY OPERATION OF LAW,
INCLUDING BUT NOT LIMITED TO ANY IMPLIED WARRA NTIES OF
MERCHANTABILITY OR FITNESS FOR A PARTI CULAR P URPOSE.
THIS W ARRANTY DOES N OT COVER OR PR OVIDE FOR TH E
REIMBURSEMENT OR PAYMENT OF I NCIDENTAL 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 repo rt the fa ilure of e quipment.
Should te chnical support be una ble to resolve the co nflicts of the
product, it should be packaged in its original packaging and returned with
evidence of original p urchase a nd n ote de scribing defe ct to in clude
owner contact information. The produ ct sho uld be shipped freig ht 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]