DAYSTAR FILTERS Quark Hydrogen Alpha Eyepiece Solar filter User Guide

DAYSTAR FILTERS Quark Hydrogen Alpha Eyepiece Solar filter

Product Information

The Daystar Filters Quark is a solar observing filter designed for use on refractors with an aperture of F/4 to F/9. It is equipped with an integrated 4.3x telecentric barlow, resulting in a final image of F/17 to F/38. The filter is designed to provide the best performance and enhance the viewing experience. The Quark filter consists of multiple components, including an etalon and a blocking element. These components must be used together for safe viewing. Disassembling the filter or removing any internal component can cause permanent damage and result in unfiltered light, which can be harmful to the eyes or equipment. The filter requires a high current power supply (> 1.5A) for operation. It is important to use the supplied power supply or a USB power source rated for at least 1.5 amps at 5 volts. Computer USB ports and cell phone chargers may not provide sufficient power.

Product Usage Instructions

1. Affixing the Filter: When attaching the filter to your telescope, ensure that the solar filter is safely installed first. Never point the telescope at the sun without the proper solar filter in place.
2. Powering the Filter: Plug the filter into the supplied power supply or a USB power source rated for at least 1.5 amps at 5 volts. Allow the filter to come up to temperature and settle. When the light turns green, you can begin viewing.
3. Knob Tuning: If the image lacks contrast, you may need to adjust the center wavelength of the filter. Turn the knob clockwise 2-3 clicks and wait 5-10 minutes to see if the view improves. Additional tuning may be necessary, but remember to allow the filter to settle in temperature for approximately 5-10 minutes after each adjustment.
4. Caution and Care: Always exercise caution and care when assembling, using, and dismantling the telescope and filter. Ensure that all parts are properly affixed and that no pieces have been opened, tampered with, or removed. It is essential to inform guests or novice observers about the special nature of solar observing and the need for proper filtration.

For further assistance, you can contact Daystar Filters through the following channels:

• Call: 1 866-680-6563
• Email: service@daystarfilters.com
• Visit: http://www.daystarfilters.com

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 tra cking 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 blocking 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: 1 866-680-6563
• Email: service@daystarfilters.com
• Visit: http://www.daystarfilters.com

Cautions & Warnings:
There are n o user se serviceable pa rts inside the Quark. Do not diassemble t he 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.
• Telescope owners must use caution when affixing the filter to the telescope never to point any telescope at the sun without th e solar filter safely installed first.
• 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.
• 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 prudent ent informing guest or novice observers of the special nature of the telescope configuration so as 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 rear-mounted and can be applied to a choice of telescopes if applied properly. If the application i s incorrect, the filter will not perform as specified.
• DayStar Filters are interference filters. If light reaches a DayStar Filter at an angle, it will cause a wavelength wing shift. 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. The 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 designed for use on F/4 to F/9 refractors. Combined with an integrated 4.3x telecentric Barlow, this results in a F/17 to F/38 final image respectively, to provide the best performance from your filter. Because of the included Carlo w, ima ges will appear 4x larger than without the Quark, and ample additional back focus is available. The filter must be plugged in using the su pplied 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 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 image lacks contrasts, 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 counterclockwise 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 telescopes with “droop” of the focus ser, because even very slight tilts will effectively lower the center wavelength 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, 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, and away from you will be reddened (clockwise knob tuning).

Energy Rejection:
Concentrated sunlight 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 sessions with less than 80m m of aperture 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 best performance, a red o r yellow glass front mount Energy Rejection Filter should be used. This prevents almost all heat from entering the telescope, and is the safest option. Mo dels are available for up to 10 inches of aperture and are custom built for each DayStar filter owner. Please measure the outside diameter of the front of your tele scope’s dew

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 from the tele scope enters the blocking filter (at left), where wavelengths near H alph a are tran smitted 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 lig ht angle. In the Quark, 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 Quark 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 a re d urable, they are ea sily 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 a compressed air can s 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. The preferred cleaning method is to return the Quark to the DayStar Filters la laboratory 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 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, 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 aperture outward only. After each cleaning stroke, use a fresh applicator. The fewer strokes, the better! The metal housing and other nonoptical parts are anodized surfaces and can be cleaned with Windex.

Eyepiece Selection:
Daystar Recommends Tele Vue Plossl series eyepieces of 25mm, 32mm, and 40mm. Remember that at F/30, a high-powered eyepiece ece can exceed Dawes’ limit. Observers will find the 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 “fast” eyepieces 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 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 Plossl s stand out in superior design. Furthermore, the adjustable eyecup 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 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 a s to pick out more subtle details 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 the sun affects seeing significantly. Characterized by turbulence or shimmering as seen over a hot street, seeing can cause a significant impact on quality o f solar observations.

• Bad seeing is caused b y air of different temperatures mixing. This typically happens within the lowest 10 feet of air. It occurs most often over pavement, dark objects, roo stops 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 b e su sceptible to seeing issues. Solar Ob servers usi ng high-powered, high- resolution telescopes nd DayStar filters should hee d daytime seeing. While many of these conditions are beyond our control, observing in an area wit h ideal conditions, without pavement in the direction of viewing, and on days with no high cirrus will offer the best results. The 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 the movement of the sun. Some locations benefit from best seeing in the morning, while many have best seeing in the afterno on. 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 that 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 a n IR-blocking filters which greatly reduce the transmission of Hydrogen Alpha light. DSL R 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, 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 pre-sent in CCD i maging of monochrome light of Hydrogen Alp ha is the interference pattern – or Newton’s Rings. The effect is similar to interference testing of an optical surface between two flat surfaces. The sen sor and cover slip cause a small interferometer inside the came ra and cause a Newton’s Ring moire’ pattern. The CCD chip m ust be tilted to a mino r degree to o revent 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 DSL and Quark 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 a mple 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 th rough a DayStar with a we bam style camera might be ab out 1/15 – 1/ 100* of a second. Exposures for surface detai I would be even shorter exposure with about 1/ 300 to 1/500 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 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 output of the Quark, the image scale will be quite I arge and small (1/2″ 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 Quark and the camera. Simple 1.25″ screw-in focal reducers can be atta ched to the camera nosepiece to allow a wider field of view with small (1/2″, 1/3″, ¼” ) sensor cameras. Mo re distance between the focal reducer and came ra surface will result in more focal reduction and I arger field of view.

Features of the Sun in Hydrogen Alpha:

By observing the sun with anarro w bandpass filter tuned 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 photosphere, always moving and changing. The chromosphere’s structure behaves differently in active regions than in 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 1A or more will show prominences, a detail of the chromosphere projected against the dark black contrast of space. To observe the details of the 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 I ess than 1.0A. Th € narrower the filter’s bandpass, the more contrast we will see – down tc 0.4A, 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) are low in the atmosphere so they are not visible on Halpha 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 that 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 e vent 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 di pole, or “flux tube” is surfacing on the disk, eventually p producing 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 the 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 40-mm eyepiece (not included) is installed. Ensure the knob is pointing straight away from the power jack. Check for focuser droop, all connections between the 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 the wing shift knob up 3-4 clicks clockwise past the center and wait 5-1 0 minute. If that does not improve the view, try down 3 -4 clicks below the 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. Poo r seeing can be caused by the presence of he at waves f rom concrete, a sphalt, o r machinery. Weather effects like the je t stream can 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 is adjusting to the wavelength chosen by the kn ob. Wait approximately 5-10 minutes for the temperature 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 go 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 usually indicates that the Quark is not receiving enough voltage. If powered by a battery, recharge the battery. 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.
The red indication can also mean an electrical fault i n the Quark electronics. If power source changes do not resolve the red indication, 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

FCC statement

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 residential 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 interference 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 the interference by one or more of the following measures: Reorient or relocate the receiving antenna. Increase the separation between the equipment and the receiver. Connect the equipment to an outlet on a circuit different from that to which the receiver is connected. Consult 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 1 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 separate this from other types of wastes and recycle it responsibly to promote the sustainable reuse of material re sources. This pro duct should not be mixed with other commercial wastes 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 theirsupplier and check the terms and conditions of the purchase contract. Household u sers should contact either the retailer where they are for disposal.

Copyright:
This manual copyright © DayStar Filters 2014, all rights reserved.

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 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 the Operating and Maintenance Manual (B) modified, altered, o r 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 defe ct or malfunction cove red by this warranty. This warrantee in cludes 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 responsibility 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, the 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 EX CLUDES AL L 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 FORTH E REIMBURSEMENT OR PAYMENT OF INCIDENTAL OR CONSEQUENTIAL DAMAGES.
• Procedure for obtaining performance of warranty: Upon discovery of a 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 a note describing the defect including owner contact information. The product should be shipped freight pre-paid by traceable means or delivered to the warrantor at:

DayStar Filters LLC 149 Northwest 0O Highway, Warrensburg, MO 64093 USA www.DayStarFilters.com – 1 866-680-6563

References

• DayStar Filters - Ultra narrow Bandpass filters

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