DayStar Filters Combo Quark Hydrogen Alpha Eyepiece User manual

DAYSTAR FILTERS COMBO QUARK
Congratulations on your purchase of a Quark Hydrogen Alpha “Eyepiece”
solar filter, designed specifically for compatibility with Schmidt Cassegrain,
Maksutov, and F/15 or greater Refractor telescopes. Please read this
manual before using the product.
To use the filter, plug in the included power supply. For SCT or Maks,
place a red or yellow glass off axis ERF (not included) over the front of
the telescope, and the included wedge adapter between the telescope
and the Quark, with the set screw on the wedge adapter pointing on the
same side as the off axis hole. For F/15 or greater refractors, do not
use the wedge adapter. Then insert the Quark and insert an eyepiece
or camera in the rear of the Quark. Turn the knob to point straight
away from the light. When the light turns green in about 5-15 minutes
your viewing experience can begin.
To prevent damage, we strongly recommend using an Energy Rejection
Filter. This can be a 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 assembly must be used together for safe viewing.
Do not power 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: [email protected]
Visit: http://www.daystarfilters.com

Cautions & Warnings:
There are no user serviceable parts inside the Quark. 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.
WARNING: When installing via the rear port, unfiltered
sunlight can be directed out the Questar right angle
eyepiece port; a metal plug or strict precaution must be
used to prevent injury.
Telescope owners must use caution when affixing the filter to the
telescope never to point any telescope at the sun without the
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 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 interference filters. If light reaches a
DayStar Filter at an angle, it will cause wavelength wing
shift. For our application on a telescope, DayStar owners need
F/15 to F/30 light. This model of Quark is designed only for use
on F/15 or slower refractor telescopes, or SCTs with an off axis
ERF. SCTs must not be used in full aperture with this unit.
•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.

USAGE:
The Combo Quark has a standard eyepiece snout so that it can be
inserted directly into the eyepiece drawtube.
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.
Because the Quark requires about 67mm of additional backfocus (99mm
when used with the wedge adapter), you will need to dial the focus knob
quite significantly.
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:
Energy Rejection Filters reduce the heat load on your filter assembly by
absorbing or reflecting UV and/or IR light and transmitting light in the
visual spectrum. These filters are Red, Yellow, or clear glass with an IR
and UV reflective coating. The ERF can also serve as an aperture mask
to accomplish a straight angle of incidence for light entering the filter.
Please note, a Herschel Wedge or white light filter cannot be used with
the Quark. Those filters block 99.999% of all light, including the desired
H alpha light.
REFRACTORS:
For brief observing sessions using refractors with less than 80mm of
aperture when not using a tracking mount. Be alert for any rise in
temperature of your telescope, diagonal, or Quark.
For telescopes under approximately 150mm of
aperture, a screw 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 a telescope with an integrated rear
field flattener or Petzval lens. The UV/IR cut filter must be the first optical
element to encounter concentrated light.
For highest safety, a red or yellow
glass front mount Energy
Rejection Filter should be used.
This prevents almost all heat from
entering the telescope. Please
measure the outside diameter of
the front of your telescope’s dew
shield. This tube OD
measurement is critical to
ensuring a good fit for your ERF.
MAKSUTOV TELESCOPES:
Maksutov telescopes usually use a full aperture colored glass ERF.

SCHMIDT CASSEGRAIN TELESCOPES:
SCT telescopes typically employ
a front mounted Energy
Rejection Filter (ERF) with an
off-axis opening of reduced
aperture. Full aperture glass
ERF’s are prohibitively
expensive and daytime seeing
quality limits resolution.
By reducing the aperture, the
focal ratio of your SCT will be
increased from the native focal ratio to the preferred ~F/30 beam.
Because the SCT has a central obstruction, we need to move the
opening off-axis. Now the beam that exits the SCT telescope is parallel
when it reaches the rear mounted DayStar Filter, but the light cone exits
the SCT off-axis. We must compensate for this angle with a wedge
adapter or the resulting transmission will be OFF-BAND. The wedge
adapter has a machined internal angle which counteracts the off-axis
light. THE WEDGE ADAPTER MUST BE ORIENTED TO MATCH THE
ERF in order to achieve on-band performance of the Quark.
The SET SCREW orientation must MATCH the ERF HOLE
orientation.
How it works:
Light from the telescope enters the blocking filter, where wavelengths
near H alpha are transmitted while the rest are reflected back out. Red
H alpha light then passes through the Etalon. The Etalon passes a very
narrow range of light wavelengths, but it is sensitive to temperature and
light angle. In the Quark, the Etalon is heated to approximately 100-
150°F to control the wavelength passed, and the slow focal ratio of the
Questar telescope 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 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 Quark to the DayStar Filters laboratory for proper 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, 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.
Eyepiece Selection:
Daystar Recommends Tele Vue Plossl series
eyepieces of 25mm, 32mm, and 40mm.
Remember that at F/14-30, a high powered
eyepiece can exceed Dawes' limit. Observers will
find best results with an eyepiece which is 32mm or
greater 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 and other "fast" eyepieces
typically perform very badly on DayStar applications.
Other brands do offer Plossl eyepieces in 32-40mm 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.
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 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 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 – 1/100th of a second. Exposures for
surface detail would be even shorter 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 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 Quark, the
image scale will be quite large 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 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.
If using off axis ERF, make sure ERF hole is on same side as wedge
adapter set screw.
Make sure a 25 to 40mm eyepiece (not included) is installed.
Ensure knob is pointing straight away from the power jack.
Check for 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 knob up 3-4 clicks clockwise past center and
wait 5-15 minutes. If that does not improve the view, try down 3-4 clicks below
center and wait 5-15minutes.
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 for the Quark
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 Quark 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 Quark.
Red indication can also mean an electrical fault in 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/14 to F/30 Refractor telescopes in full aperture.
SCT or Mak telescopes when used with Off Axis ERF
(not included)
Backfocus: Requires refocusing 67mm rearwards, 99mm with
wedge adapter.
Blocking filter: Integrated 25mm blocking filter
Clear aperture: 19mm clear etalon aperture
Full disk: Passes full solar disk for focal lengths under ~1800mm.
Aperture limit: None, usable on large telescopes for high magnification.
For apertures over 80mm, suggest Energy Rejection
Filter.
Sun side: 1.25” snout.
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.

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sustainable reuse of material resources. Household users should contact
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Copyright:
This manual copyright © DayStar Filters 2015, 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]