DayStar Filters Magnesium Quark Eyepiece User manual

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MAG"'-IESIUM QUARK
Congratulations on your purchase of a Quark Magnesium "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 LED 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.
Daystar Quark Configuration on Refractor
with Rear Mount UV fIR Cut ERF
-Eyepiece
(25-40mm
Plossl)
-D/WSTI\a
QUARK
-Diagonal
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: [e-mail]
Visit: http://www.daystarfilters.com

Cautions & Warnings:
There are no user serviceable parts inside the Quark. Do not
diassemble the unit. Certain components are under pressure and
disassembly
can cause permanent damage. All elements are required
for proper 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
use and dismantling at all times.
.. Telescope owners must use caution when affixing the filter to the
telescope never
to paint any at the sun without the
solar filter 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 is never
pointing at the sun without the solar filter properly installed.
.. owners will be prudent to inform or novice
observers of the nature of the telescope configuration so
not
to imply that 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 if properly. If application is
nf"ol.rr,:>f"t the filter will not as specified.
.. DayStar Filters are interference filters. If light reaches a
DayStar
Filter at an angle, it will cause wavelength
wingshift. The Quark contains a 4x telecentric barlow, for use
with telescopes with focal ratios from roughly F/4
to FIg.
.. DayStar filters are temperature sensitive. Changing the
temperature will change the wavelength (CWL) that the filter will
transmit. Users need to
be aware of tuning issues.

USAGE:
The Quark is rlO""-"\"",, for use on F/4 to FIg refractors. Combined with
an integrated 4.3x telecentric barlow, this results in a F/17 to F/38 final
respectively,
to provide the best performance from your filter.
Because of the included barlow, images will appear 4x larger than
without the and ample additional backfocus is available.
The filter must
be plugged in using the power supply. The
eta
Ion cavity is 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. USB and cell phone do
not normally this much power.
After letting the filter come
up to and the will turn
green and viewing can begin.
Knob tuning:
You may desire 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 0.5A. Turn clockwise to raise the towards the red by up to
Each click of the knob is
0.1 A.
Tuning is required on telescopes with "droop" of the because
even very slight tilts will lower the center wavelength of the
filter. Turn the knob clockwise 2-3 clicks and wait 5-10 minutes
to see if
the view
is improved.
Additional tuning can be just
in mind that after every
of the knob the filter must settle
in for
approximately 5-10 minutes before your change becomes effective.
Note: To be sure you are
on Magnesium, the best method is to observe
(or image at the same exposure time and gain) for several knob
The tuning is
on band when the surface is DARKEST and has
the most contrast.

Energy Rejection:
Concentrated sunlight can create very high temperatures where it falls,
so care must
be taken to prevent melted components or fire.
For brief observing sessions with less than 80mm of aperture 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 telescopes under approximately 120mm of
aperture, a screw
in UVIIR cut filter can be
employed
in front of the telescope diagonal. The
UVIIR cut filter reflects UV and IR light back out
the front of the telescope, reducing temperatures
inside. Do not use a UVIIR cut filter with oil
spaced objective telescopes, 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.
Yellow or
red glass front mount
Energy Rejection Filters (ERFs),
as shown at right, do not pass the
green Magnesium wavelength and
cannot
be used with the
Magnesium Quark.
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.

DayStar Quark Optical Configuration
Sitown wtth eemm FJI& ...-npl. obfect1v., ffW 0.' · field
.Iock ....
Tetecentrlc Bartow ........
Etllion
Flltwr
How it works:
Light from the telescope enters the blocking filter (at left), where
wavelengths near Magnesium are transmitted while the rest are reflected
back out. Yellow Magnesium 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 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 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 Piossl series
eyepieces of 25mm, 32mm, and 40mm.
Remember that at
F/30, a high powered eyepiece
can exceed Dawes'
lim i t. 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 Piossl 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 Piossl 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 from nighttime conditions.
During the daytime, radiant heating from the sun affects
significantly. Characterized
by turbulence or shimmering as seen over a
hot seeing can cause significant
on quality of solar
observations.
-Bad seeing is caused
by air of different temperatures mixing. This
typically within the lowest"
10 feet of air. It occurs most often
pavement, dark rooftops and sometimes trees.
-High cirrus clouds or "scuzz" will cause scattering of sunlight
in the high
which often makes for bad viewing conditions. A classic
of high cirrus clouds is the inability to achieve or the need
to
"chase focus", or a lack of contrast.
moving overhead
can also hurt conditions even on
DayStar Filters are high power viewing platforms and this high resolution
can be
to issues. Solar Observers using high
powered, high resolution and filters should heed
seeing. While many of these conditions are beyond our control,
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 stability.
Each observing location offers different behavior for 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
in
the morning, while many have best seeing in the aftemoon. Because
most heat variation between air and ground surfaces occurs within the
first 10 feet above the often a observing will offer
This might include a second story deck which overlooks
grass.

Solar Imaging Tips: RGB Inside the Camera
Oaystar recommends
Inaming V isib~
MONOCHROME CCO
ight
imaging whenever
possible for best results. VlSble
Llgtt Pi:6S8S
_ ,l m"",h lR·Bbcldng
The recent availability of
CCD cameras and DSLR
cameras has offered a
simple opportunity for
solar observers
to image CoIorb.,d senson;
the Sun with a Digital SLR =e~~~Ch
camera. Please be sensorlnoeleCUictly
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 Magnesium
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
'.
. II . \; 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 accessory is available from DayStar which can be used between the
DSLR and Quark
to adjust the light angle and extinct the interference
pattern,
is available in T (MG-040B) and C (IECC) mount versions.

Lucky Imaging:
Virtually all solar imaging can benefit from the technique of Lucky
Imaging, where a high speed camera is used
to capture hundreds or
thousands of frames
in a short time span. Then software can be
used to select and stack just the frames least affected atmospheric
this function include
Exposure time:
Imaging solar vs. nighttime astrophotography is very different. Dark sky
long exposure times
to capture light. Solar
offers ample light, so exposures should
be very short. Plus,
fluctuations
in 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 are beUer than long exposure
CCD cameras when imaging sun.
• Because the sun has a range
of automatic
exposure doesn't work well. A software interface that allows the
user
to control the exposure settings manually is very important.
Exposures in Magnesium should be kept to 1/30 second or less in order
to capture the fleeting moments of good seeing. Increasing camera gain
or addition
of a focal reducer AFTER the Quark can improve exposure
times.
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 Hydrogen Alpha).
In order to all these
we recommend the use
of 12 bit or 16 bit cameras. Normal 8 bit
cameras can be but will typically only be able to image either the
surface or
in Hydrogen 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", 113", y.,") sensor cameras. More
distance between the focal reducer and camera
surface will result
in more focal reduction and larger field of view.