Some things cannot be improved. You can only make them better.
Filters for astrophotography are constantly being improved to adapt them to modern imaging systems and changing environmental conditions. Our CMOS-optimized narrowband filters are the best example for this development and research process. There are other demands for those filters which are used for science instead of pretty pictures: they must deliver data that are comparable even with decades-old data sets. New developments must therefore only improve production and handling without changing the filter characteristics themselves.
The filters used today for scientific photometry with digital sensors go back to the filter sets introduced by Johnson and Cousins, which were developed in the 1950s-1970s and which were adapted in the 1990s by M. Bessel for CCD cameras - in each case using the techniques available at the time.
The original UBV filters consisted of coloured glass, partly even without protective coating. Therefore, the V filter, for example, worked wonderfully in dry observing sites. However, because its BGT39 material was exposed to the environment without protection and had hygroscopic properties, it aged if there was high huminity: so, under less favourable conditions, it quickly got hazy.
Another feature of the original filters was that the Cousins Ic bandpass filter, for example, was open at the red end, so the sensor or film - instead of the filter itself - limited the sensitivity at the red edge of the spectrum. At the blue end of the spectrum, on the other hand, it was the atmosphere (humidity, altitude of the observing site) rather than the filter that set a limit. Despite these disadvantages, thousands of observations were made with UBV filters and the filter systems based on them.
Whoever develops filters today has many more possibilities to influence the spectral transmission characteristics. While the original filters consisted of coloured glasses and protective glasses of different thickness and transmission, which on top of that were not resistant to ageing, we can now manufacture dielectric filters whose characteristics allow very well-defined transmission windows - but they are steeper than the original transmission windows, and depend on the focal ratio. On fast telescopes with f/2-f/4 they work somewhat differently than on slow telescopes with f/8, and since the angle of incidence of the light distributed over the field of view also changes, there are now some new problems on modern telescopes with large CCD sensors that were unknown on old, slow telescopes with film cameras. A modern photometric filter therefore does not have to provide perfectly delineated transmission windows with steep edges, but data that are comparable to the old data sets (even if only by using reliable conversion algorithms).
The UBVRI system was developed in the 1950s for the 0.9m McDonald Observatory telescope and initially consisted of a Johnson UBV filter set, later extended by Cousins to include the R and I filters for the red region of the spectrum. The filters of the extended UBVRI system according to Johnson and Cousins include:
- U – Ultraviolet, with a transmission window between about 320 and 400 nm
- B – Blue, with a transmission window between about 400 and 500 nm
- V – Visible, with a transmission window between about 500 and 700 nm
- R – Red, with a transmission window between about 550 and 800 nm
- I – Infrared, with a transmission window between about 700 nm and 900 nm.
According to the state of the art at that time, the filters had different thicknesses and transmittance values as well as no sharply defined edges (if any). Their spectrum therefore corresponds to a curve instead of a plateau.
Bessel filters for the digital age
In 1990, M. S. Bessel looked into the subject in order to find a filter combination for the new CCD cameras that were becoming increasingly widespread at the time. These Bessel-UBVRI filters are still standard today and are also the most widely used in amateur circles such as the AAVSO. The V-filter in particular has proved to be an inexpensive introduction to photometry: It corresponds approximately to the visual brightness; since only one measured value is used, this is optimal for getting to know the techniques.
Since 2010, Baader Planetarium has offered photometric UBVRI filters according to Bessel, which protected the coloured glasses from ageing with a dielectric coating and at the same time provided the desired transmission properties. This is not at all a matter of course: unfortunately, comparisons by the AAVSO have shown that not every modern "Bessel filter" actually shows the irregular flanks of genuine Bessel filters, but instead there are often plateaus with steep flanks. These steep slopes are easily achievable with dielectric filters, but the data obtained with them are simply not comparable, or only with difficulty, with the old data sets. Compare for yourself: You can find the transmission spectra in the product description.
New generation of Baader Planetarium UBVRI filters
[br]
[br]
Die We could not further improve the characteristics of our previous, Bessel-compatible UBVRI filters - but we could make the filters better. The new generation of Baader Planetarium UBVRI filters, introduced at the end of 2021, is a modern filter set that is both fully compatible with the characteristics of the original Bessel filters and at the same time meets modern demands for contemporary filters:
- The photometric filters now have the same thicknesses as all other Baader filters:
- 2 mm filter thickness for all filters up to size 2" mounted (1.25", 31 mm, 36 mm, 2")
- 3 mm filter thickness for all sizes above (50.4 mm, 50 x 50 mm, 65 x 65 mm)
- This means that they fit into any commercially available filter wheel, for which the original filters were often simply too thick and could not be fixed securely.
- They are parfocal with all other Baader filters of the same size and now also available in sizes up to 100x100mm - large enough even for modern, professional sensors, or optimal for easy handling in the common filter mounts for amateur telescopes.
- The coating of all photometric filters is manufactured in the same technology as the CMOS-optimized narrowband and LRGB filters. The lifetime also applies here.
Transmission curves of the CMOS-optimized Baader UBVRI Bessel Photometric Filters
The next generation: SLOAN filters
In 2000, a new era in photometry began: with the Sloan Digital Sky Survey (SDSS), a 2.5 m telescope at Apache Point Observatory (New Mexico, USA) surveyed one third of the sky in five wavelengths. A camera with a total of thirty large CCD sensors with 2048×2048 pixels each was used, each in five rows of six sensors. In front of the sensors was a u'g'r'i'z' filter set for five non-overlapping wavelength windows around 355.1, 468.6, 616.6, 748.0 and 893.2 nm; light pollution such as the airglow at 558nm and the mercury line at 546 nm were masked out. This system was also used for the Pan-STARRS project; the broad data base of these two surveys makes them very well suited for calibrating images. Another advantage are the wider transmission windows, which allow fainter objects to be measured in a shorter time.
Transmission curves of the new Baader SLOAN/SDSS (ugriz') Photometric Filters
Even though the six Sloan filters have a different characteristic than the UBVRI filters, there are now the appropriate algorithms to compare the data with each other or to convert them into each other. Therefore, the Sloan photometry system is gaining more and more importance. At present, UBVRI filters still dominate in amateur circles, but we not only offer unmounted Sloan filters for professional telescopes, but also in the sizes and mounts commonly used by amateurs. In the coming decades, it is expected that the Sloan system will also become more widespread in amateur circles, which is why Baader Planetarium's SLOAN filters are also available in the common filter sizes for amateur telescopes as well as in the large format 100x100 mm. The SLOAN z' filter is currently not included in the scope of delivery, as its function can usually also be taken over by the UBVRI -I- filter.
The same technology is used for the Sloan filters as for the CMOS-optimized narrowband and LRGB filters. Here, too, the lifetime applies.
Ready for the future
At a time when common filter types often disappear from the market without warning, with these filters we want to offer all users a way to build on previous data obtained with UBVRI or Sloan filters. Long-term availability makes it possible for amateurs to enter with a limited budget and a small set of filters to expand in the long term. Therefore, we have resisted the temptation to improve the filter lines and have done our utmost to improve the filters in durability and applicability.
[product sku="qhySWIRcameras"]
Two new cooled CMOS cameras QHY 990 and QHY 991 for the near infrared spectrum.
In September 2021, QHY began shipping 2 new camera models, the QHY990 and the QHY991. Both are cooled cameras with CMOS sensors covering the near infrared wavelength range.
Both models use Sony InGaAs sensors with square pixels measuring 5µm x 5µm. The IMX990 is a 1.3-megapixel sensor and the IMX991 has a 0.4-megapixel array. The spectral response starts at 400. and ends at 1700 nanometres. The maximum quantum efficiency is 77 % at a wavelength of 1200 nanometres.
More details about SWIR QHY990 and QHY991 can be found on our product page
Important addition to the Baader UFC and M68 system
- UFC tilter for an optimally flattened field of view
- Compatible with the entire Baader UFC system
- 0-1° tilt – allows a shift of up to 1° to compensate for misalignments in the image field
- 9.75 - 10.50 mm optical length
On our overview page for the Baader UFC system, we have published some blog posts that explain the system clearly for a better understanding of the system.[br]
- M68 titlter for an optimally flattened field of view
- Compatible with the entire Baader M68 system
- 0-1° tilt – allows a shift of up to 1° to compensate for misalignments in the image field
- 9.50 - 10.25 mm optical length[br]
Accessories for the M68 System
- Reducing piece: M68a to M62a for direct connection of M62 accessories (e.g. QHY Color Filter Wheel (CFW 3) to the M68 system
- Chonverts the M68 (Zeiss) female into a M62 male thread
- Telescope side M68 male thread, eyepiece side M62 male thread
- Optical length: 5 mm
- Inner diameter: 59 mm, outer diameter: 76 mm[br]
- Reducing piece: M68a to M54a for direct connection of M54 accessories (e.g. QHY Color Filter Wheel (CFW 3) to the M68 system
- Converts the M68 (Zeiss) female into a M54 male thread
- Telescope side M68 male thread, eyepiece side M54male thread
- Optical length: 5 mm
- Inner diameter: 51 mm, outer diameter: 76 mm[br]
Baader Large Devices
- Compact, mobile rotary stage for adjustment of 3" or 8" PAN EQ clamps on double mounting plates or mounts of the L-Mount series.
- Makes it possible to adjust the optical axes of parallel mounted telescopes to each other.
- Mounts parallel to the main telescope on the side of the dual mount or on the side port of a PlaneWave L-mount to align and simultaneously operate secondary telescopes such as RASA-, or Newtonian telescopes parallel to the main telescope in the azimuthal or equatorial configuration. To connect the PAN adjuster to the L-350 mount, the [product sku="2451516"] is required.
- Push pull screws allow to adjust the angle of the installation plate to the rotation plate.
- Adjustment screws allow to adjust the rotational angle between the attachment plate and the rotation plate
- Cutouts and hole in the middle allows for cabeling
- Made of solid Dural Aluminum and connected with stainless steel clamping rings.
- Developed and manufactured at Baader Planetarium in Germany.[br]
- is needed to connect the [product sku="2451515"] to the L-350 mount from PlaneWave Instruments
- PAN-Adjuster with the corresponding adapter for L-350 is attached to the side port of the mount in order to be able to align second instruments, e.g. a RASA or Newtonian telescope, parallel to the main instrument and operate them simultaneously.[br]
- Enables the use of up to three instruments at the focal plane of a telescope.
- Designed, manufactured and assembled in Germany
- IMP85 (Instrument Multi Port) with 85mm clear aperture, in order to have one large straight Port 1 for unobstructed, unreflected light beam for the main camera.
- Two automated with 67mm clear diameter mirrors with 40 x 40 mm and BBHS coating can be set to deflect the light either left, right or to let it pass through undeflected.
- These ports can be used for various other optical instruments like spectrographs, video cameras, planetary cameras or a simple eyepiece.
- Can be controlled by a keypad or remotely via a webinterface.
- Massive CNC machined housing made of dural aluminium carries even the heaviest loads fo large cameras
- Power-over-Ethernet via the RJ45 ethernet port. In addition the device can also be powered by a standard 12V hollow plug 5.5/2.1. 12V power supply is included in the scope of delivery
- Connections telescope-side: 120 x 7.5 mm dovetail mount
- Connection Port 1 camera-side: 120 x 7.5 mm dovetail mount
- Connestion Port 2 and Port 3 camera-side: M68x1 female[br]
Accessories for IMP85
[product sku="2451310"]
- Telescope adapter for Hedrick focuser 3.5" for PlaneWave CDK 14/17/20/24" to the [product sku="2451300"]
- Designed and manufactured in Germany
- Connections on camera side: 120 x 7.5 mm dovetail
- Black anodized
- Optical ength: 0.5 mm
- Internal and external diameter: D120a/ D82,5i[br]
[product sku="2451311"]
- Telescope adapter for telescopes with IR90 - integrated Rotating Focuser to the [product sku="2451300"]
- Designed and manufactured in Germany
- Connections on camera side: 120 x 7.5 mm dovetail
- Black anodized
- Optical length: 40.9 mm
- Inner and outer diameter: D120a/ D85[br]
[product sku="2451312"]
- Telescope adapter for Alluna Optics M100a (male thread) to the [product sku="2451300"]
- Designed and manufactured in Germany
- Connection on camera side: 120 x 7.5 mm dovetail
- Black anodized
- Optical length: 0.5 mm
- Inner and outer diameter: D120a/ D90i[br]
[prodcut sku="2451313"]
- Fits to Port 1 of the [product sku="2451300"], provides an M100x1 female thread for Alluna Optics on the camera side
- Designed and manufactured in Germany
- Connection on telescope side: 120 x 7.5 mm dovetail
- Black anodized
- Optical length: 0.5 mm
- Inner and outer diameter: M100x1i / D120[br]
[product sku="2451314"]
- Telescope adapter for telescopes with Starlight Instruments FeatherTouch 3.5" focuser to the [product sku="2451300"]
- Developed and manufactured in Germany
- Connection on camera side: 120 x 7.5 mm dovetail
- Black anodized
- Optical length: -2.5 mm
- Inner and outer diameter: D120a/ D92i[br]
[product sku="2451315"]
- Connection camera side to M68x1 female thread on the Port 1 of the [product sku="2451300"]
- Designed and manufactured in Germany
- Connection on telescope side: 120 x 7.5 mm dovetail
- Black anodized
- Optical length: 0.5 mm
- Inner and outer diameter: M68x1i / D120 x 7,5 mm[br]
Further Baader accesories
- System M54 – spacer (Fine-Adjustment) rings, available in thickness 0,3mm (black), 0,5mm (red), 1mm (gold)
- Very thin ring for finetuning in the M54-system
- Ring in M48 diameter without threads
- Fits between all M54 threads, equals approx. 2/5 (0,3mm), 2/3 (0,5mm) respectively 1 1/3 (1mm) turn of rotation. Rotation may differ slightly.
- Prevents binding between two M54 threaded parts[br]
- Adapter to connect the [product sku="2957220"] onto M48-threads
- only suitable for BDS-SC Diamond Steeltrack® focuser
- optical length: 35 mm[br]
In just under a month, an annular Solar eclipse will take place on the morning of Thursday June 10th. An annular eclipse occurs when the Moon passes between the Earth and the Sun but the Moon's apparent diameter is smaller than that of the Sun's due to the Moon's orbit being elliptical and it being further away from our Earth (at/near apogee) at that time. This leads to the outer parts of the Solar disc being "exposed" in an annulus or ring - often called "ring of fire".
For those lucky enough to live in north-east Canada, western Greenland and far eastern Russia, will get to see the annular phase event which will last for a maximum of 3m 51s over north west Greenland. For people living in northern Europe including, Germany, UK, Portugal and Spain a partial eclipse will be visible. The amount of obscured Sun will vary depending on your location and below are some approximate values of this amount for a selection of locations:
- Germany (north / south): ~17% / ~6%
- Austria: ~4%
- Czech Republic: ~8%
- France (north / south): ~17% / ~3%
- Iceland: ~60%
- Norway (Oslo): ~31%
- Spain (north / south): ~8% / ~1%
- Sweden (Stockholm / Tromso): ~26% / ~51%
- Switzerland: ~6%
- UK (north / south) ~36% / ~20%
The image above right shows the path of the eclipse. The dark orange shows the land regions that will see the annular eclipse with the light-orange and yellow shading being the land areas experiencing the partial eclipse. For more details including an animation of the eclipse path see timeanddate.com website. Also visit NASA's Solar Eclipse website for an interactive map where you can see locations, times of the eclipse and amount of the Sun obscured.
It is most important to mention that when it comes to the Sun safety is paramount: Never directly look at an annular or partially eclipsed Sun as such an event still requires the use of appropriate safety equipment such as our AstroSolar® OD5.0 film or our Safety Herschel Prism.
White light intensity view of the Sun from the GONG website
At the moment the Sun is coming out of Solar minimum so hopefully when its "eclipse time" it's surface will have some activity in the form of Sunspots or Sunspot groups and faculae too. To see how active the Sun is at the moment there is a very useful resource in the form of the National Solar Observatory's GONG website. GONG stands for Global Oscillation Network Group and it is a network of six sensitive imaging systems located around the Earth to obtain nearly continuous observations of the Sun's "five-minute" oscillations, or pulsations. You can see the range of near real-time Solar images here with the white-light views on this page from the different sites.
Pin hole camera obscura image showing the partially eclipsed Sun
A simple and no-cost way of seeing the eclipse is by using a simple camera obscura. This simply consists of two pieces of card, or a cardboard box (e.g. shoe box), with the skyward end of the unit having a pin-hole (or holes) punched into it and the Sun's image is projected onto the card opposite. A simple guide of how to make one easily can be found on our website. The image to the right shows the result of such a set up using two A4 pieces of card from the total Solar eclipse in the USA in 2017 where holes were made in the skyward "shadow maker" cardboard sheet to show the location and date of the event. A crescent partially eclipsed Sun is easily seen.
To view and image the eclipse filters are most often used and we offer a range for different applications.
[br]
Baader AstroSolar Eclipse Glasses
Solar Viewer AstroSolar® Silver/Gold: Sometimes referred to as "Eclipse Glasses", these are the simplest and easiest way to observe a Solar eclipse. These viewers use our (made in Germany) AstroSolar® Silver/Gold Safe film which reduce the sun light intensity by 99,999% and give 100% UV- and IR-protection to safely protect your eyes for visual solar observation. The Solar film is mounted in a strong card sunglasses-type frame – so these are solar viewers that you wear like sunglasses. Apart from an eclipse they can also be used for viewing very large sunspots or sunspot groups should they develop.
[br]
Baader AstroSolar film
Baader Digital OD 3.8 Solar film - for imaging use ONLY
Baader OD 5.0 Astrosolar film for safe visual and photographic use
One of our most popular products, these very high quality front end/objective end film filters are available in two optical densities and various sizes:
- AstroSolar® OD 3.8 Photo Film: is for imaging use only and currently available in 20cmx30cm sheets.
- AstroSolar® Safety Film OD 5.0: Can be used for both safe visual and imaging purposes. These are currently available in sheets of 14x15.5cm, 20x29cm (~A4 size - our most popular size) and 117cm x 117cm giant sizes.
With these Solar filters it is up to you to make your own filter holder. However this is not complicated and you can find a useful guide here and some additional information on our AstroSolar website.
[br]
Baader ready-made AstroSolar® filters
Ready-made AstroSolar filters
These ready-to-use filters use our high quality OD 5.0 AstroSolar® Safety Film (OD 3.8 for the Digital Solar filter - see below) for the but are pre-mounted stress-free in a unique aluminium cell which have elongated slots and rubber-coated bolts so the filter unit can be fitted and securely clamped onto a range of different telescope tube sizes. Three safety Velcro safety straps and full instructions are included.
For any of these ready-made filters, the correct filter size for your optical equipment will depend on the outside and/or inside diameter of your telescope tube wall and for more information:
Clamping range of our ready-made Solar filters
- Click here to download Baader's information sheet for the clamping range for these filters (seeimage opposite too) for newtonians, refractors/camera lenses and compound instruments.
- Use our useful Solar Filter Finder Tool which allows you to simply select what telescope/lens etc you have and the appropriate filter model will be displayed: see here to use the Filter tool.
Our ready-made filters are available in four versions:
ASTF: AstroSolar Telescope Filter - for use with telescopes and large telephoto lenses from 80mm up to 280mm.
ASSF: AstroSolar Spottingscope Filter - for small telescopes, spotting scopes and camera lenses with apertures from 50mm to 150mm. The image below left shows a test set up for the 2017 American eclipse with a small refractor telescope (left-side) having an ASSF on its objective end and an ASBF attached to a DSLR telephoto lens (right-side).
ASSF (left) and ASBG (right) on a pre-eclipse trip test run
Below is an image of a partially eclipsed Sun taken through an ASSF filter with a DSLR and a telephoto lens. Sunspots and faculae can be seen. The image to its right is the same image but simply colorised.
Partially eclipsed Sun through an ASSF filter
Simple colorized image of the image
[br]
Baader ASBF filters attached to binoculars mounted on a 10Micron BM-100 binocular mount
ASBF: AstroSolar Binocular Filter - for use with binoculars (or small telescopes and camera lenses) from 50mm to 100mm in aperture. The filter holders are "D" shaped so that the two binocular objectives can be moved close together for comfortable viewing. The ASBF filters can also be used on their own on a small telescope or with e.g. two camera lenses or a small telescope and camera lens mounted side-by-side and positioned close together. The filters are supplied as one unit only, so for binocular use you will need to purcahse two of the ASBF filters. The image to the right shows a pair of ASBF models attached to a large pair of binoculars that are mounted on a 10Micron Leonardo BM-100 Bino Mount.
With the above OD 5.0 ASTF, ASSF, ASBF ready-made filters and OD 5.0 AstroSolar film you can use our Solar Continuum filter and [product sku="2458392"] which enhances contrast and reduces the effect of atmospheric turbulence. Our 2" Cool-Ceramic Safety Herschel Prism which is available in a visual and photographic version, also allows for safe white light Solar observation and imaging with refactors up to ~150mm.
[br]
Baader Digital Solar Filter (BDSF) showing the prominent warning sign that it is for imaging use only
BDSF: Baader Digital Solar Filter - for telescopes and lenses from 80mm to 280mm in aperture. As with the OD 3.8 AstroSolar film this is for high speed digital imaging only and NOT suitable for visual solar observation. A warning label on the front of the filter warns the user that the filter is not for visual use.
Eclipse Imaging
Please remember that appropriate safety filters must be used when imaging the eclipse (as we have outlined above).
For those that want to image the eclipse there are many ways to do this. The exact settings on your camera will depend on your particular equipment and set up, and it is best to do some practice runs prior to the event. However low ISO and fast shutter speeds are usually used. You can take photos simply and easily with your mobile phone or a camera of the pin-hole camera obscura projected Solar image mentioned earlier.
If you want to image the eclipse through a telescope and capture some fine Solar surface detail and granulation you can use our [product sku="2458392"] which also comes with a A4-sized AstroSolar® Photo Film OD 3.8. For those wanting something a little different when imaging, our [product sku="2458355"] will let you image in blue Calcium-K light showing the Sun's chromospheric details.
Afocal photography can be done with binoculars, spotting scopes or telescopes using our [product sku="2450330"] which accommodates cameras up to ~1.5kg and features a swivel arm that allows you to easily swap between a "photo mode" and then go back to visual observing. If you want to use your mobile phone, there is the Celestron NexYZ Universal 3 axis Smartphone Adapter for easy smartphone camera placement over your eyepiece.
Morpheus range of eyepieces. Can also be used for projection imaging too.
Our Hyperion and Morpheus range of eyepieces allow you to observe the event with your telescope (with an appropriate safety filter) and with the many adapters that are available for them, allow afocal and/or eyepiece projection imaging using DSLR, Mirrorless/MILC, camcorders and astronomical Solar system imagers too. You can find out more on how you can use these eyepieces for imaging in our Hyperion application example brochure, Morpheus Visual and Photography guide and our digiscoping guide.
Please always remember that a suitable safety solar filter must always be used if observing or imaging our Sun!
We wish you clear skies for this event and we look forward to seeing your results!
Its hard to believe that a year has gone by since our Solar System neighbour Venus seemed to be around for ages and riding high in our evening sky during the late winter and spring months. This year, after its superior conjunction on March 25th 2021, Venus will once again start to become part of our evening sky (which makes observation of the planet more "convenient" for many than when it is an early morning object) until towards the end of the year. Unlike last year's evening appearance, for many locations this coming "visit" the planet will not be as high in the sky and having a low and or flat western horizon would be beneficial. However Venus, which is similar in size to our Earth but has a temperature of ~450 degrees and a crushing atmospheric pressure ~90 times that of our own planet, is always worth pursuing visually or photographically if you can.
Venus and Mercury on the evening of 25th April
As April progresses, Venus becomes more visible in the evening sky and where it appears in your sky will depend on your location. One upcoming event to keep an eye occurs on 25th April. After sunset low in the north west horizon -1.5 magnitude innermost planet Mercury will be ~1.2 degrees away from its Solar System neighbour Venus which will be shining at -3.8. This encounter will be a nice sight in binoculars and low power short focal length telescopes. This also an ideal photo opportunity too a good opportunity to see Mercury if you have not seen it before.[br]
Venus with the Crescent Moon and Mercury on 13th May
On the evening of 13th May Venus will make a nice pairing with a thin crescent Moon which will be to the upper left of Venus. Mercury will be close by (~2.5 degrees) being to the upper right of the Moon. This will make a nice photogenic triangle. [br]
Moon and Venus on 11th June
Venus and Moon on the evening of 12th June
There will also be crescent Moon-Venus encounters on the evenings of 11th and 12th June when the Moon will be below right and then above left of Venus respectively by ~6 degrees.
Venus and Mars near each other with Moon close by on July 12.
On the evening of July 12th shortly after sunset our other Solar system neighbour Mars will be close-by (~1 degree) and below left of Venus with the slim crescent Moon nearby.[br]
If you want to capture these "wide-field" events mentioned above, a DSLR or Mirrorless camera with lens mounted on a tripod is all you need. The focal length of lens you use depends on how much of the foreground landscape scenery you want to capture and how "up close" you want to get. However anything from a medium to a zoom telephoto focal length lens can be used.
You will need to set the lens at infinity and experiment with exposure times for the sky brightness, lens aperture and camera ISO being used. A tripod to support your camera gear while photographing these events is highly recommended. The [product sku="2451020"] is an ideal sturdy tripod to carry your camera (or spotting scope) gear up to a total of 3kg. It features quick easy removable mounting plate, a fluid head with locking handles for smooth altitude and azimuth movements and extending legs with rising central column for tripod height adjustment up to a maximum of 1.89m.
This time around Venus apparent size will go from just under ~10" near the end of April where it will be ~99% illuminated, to just over 12" near end of July with ~82% illumination. During August its apparent size will increase slightly to ~14.5" and 75% illuminated, but by this time the gibbous phased Venus will be heading towards the horizon making viewing a little more difficult.
View of the crescent Venus in early December through a Celestron 8" SCT and with a [product sku="2954106"]
Venus will exhibit a crescent phase as the year draws to a close and it will appear larger in a telescope than earlier in the year but will be lower in the sky. The image to the left shows Venus very early in December when it will be only ~28% illuminated but being ~40" in size (~4x larger in apparent size than it was in April). However Venus will be very low down in the SW sky and as mentioned before a low and flat horizon would be ideal at this time depending on your location.
Observing Venus:
Classic Ortho eyepieces are ideal for planetary observation
Orthoscopic eyepieces are a favourite with planetary observers and our [product sku="2954106" template="wordpress/shortcode/productlink.phtml"], [product sku="2954110" template="wordpress/shortcode/productlink.phtml"], [product sku="2954118" template="wordpress/shortcode/productlink.phtml"] are ideal for viewing Venus (as well as other planets too). These parfocal eyepieces, which are the same optical design as the old Zeiss Jena Orthoscopic models, have a 52° apparent field of view and have high-transmission multi-coatings on all the glass-to-air surfaces to give very sharp and high contrast views. The apparent size of Venus will not be large during the months of April to August so if you want to get more magnification the [product sku="2956185"] will give a useful (but rare) 2.25x image amplification.
If you are using multiple eyepieces at the telescope, the [product sku="2957010"] which is available as an accessory on its own or [product sku="2957000"], makes simple work of swapping between different eyepieces (and magnifications) simply by rotating the turret to bring another eyepiece into the light path.
Double polarizer can help reduce the glare from Venus
Venus is very bright in our sky and to cut down its glare you can use our Double Polarizing filter to vary the brightness of the planet through the eyepiece which may allow you see some cloud detail. This filter can also be used with a planetary imaging camera too. The filter is simply screwed into the barrel of an eyepiece, Q-turret nosepiece mentioned above or a nosepiece of an imaging camera. It is also possible to screw the filter into the nosepiece of a diagonal so it is not necessary to remove the filter when swapping between eyepieces. Our colored planetary filters can also help with observations with red, yellow and blue versions being useful to increase contrast. If you want to swap between different filters our Universal Filter Changer makes this job easy and we provide many different telescope-side and eyepiece-side adapters to suit.
Imaging Venus:
QHY 5-III-462C Photo-Bundle with Baader FlipMirror II
For those who want to image the planet, there are a number of accessories you can help. Centering Venus (or other planet or Lunar feature) on a small sized sensor can be difficult and frustrating and this is where our [product sku="2458055"] (BFM II) can be of benefit. There many different telescope side, eyepiece port and camera port adapters for this that are available to suit your equipment. In use, centre Venus in your eyepiece, flip the BFM II diagonal mirror up and the planet should be visible in your camera's field of view.
The BFM II is also available as part of a complete photo bundle which includes 2" telescope side nosepiece, two 1.25" eyepiece holders, 10mm orthoscopic eyepiece for viewing and centering and a QHY-5-III-462C colour high speed low noise planetary imaging camera. This is an ideal package with everything you need to get into Solar system planetary imaging.
QHY-5-III-462C Planetary-Bundle (VIS/NIR) with complete Q-Turret Eyepiece Set
The Q-turret mentioned previously is not just limited to eyepiece use only. You can use a planetary imaging camera alongside your eyepieces so you can easily swap between your visual and imaging configurations. The Q-Turret eyepiece and barlow set is also available combined with the QHY-5-III-462C planetary camera for those who want such a visual and imaging combination package.
With Venus being smaller in apparent size you may want an increase in image amplification and the versatile [product sku="2956185"] can be used for imaging. Also our Classic Ortho eyepieces are ideal for doing eyepiece projection imaging with the OPFA Eyepiece Projection Adapters too.
Image of Venus taken with our U Venus filter
The Baader U Venus Filter, with a bandwidth of 60nm from 320nm-380nm with an 80% peak transmission, will allow you to record the Venus in the UV spectral region to capture cloud structures in the Venusian atmosphere with telescopes 5-6" aperture and above (ideally recommended).
We wish you good luck and clear skies in chasing Venus over the coming months and we look forward to seeing the results of your visual and imaging work.
New adapters for our UFC-System
- Baader UFC Fitting / T-2 (f) Thread Adapter
- telescope-side: mounting plate for UFC-Base
- camera-side: with T-2 female thread, especially for ASI cameras with T-2 (m) thread and 6.5mm back focus (ASI T-2 inner thread ring removed)
- can be adapted via the included screws and the mounting plate to the [product sku="2459110"]
- Optical height: 8.5 mm[br]
New Baader T-2 and M48 parts with omly 3 mm thread length
Modern cameras are usually characterised by extremely short optical heights, in order to be able to be mounted on various telescope constructions. To take care of this new development, all new Baader T-2 and M48 parts are delivered with the new 3 mm standard.
These two new nose pieces with Safety Kerfs are further developments of our 1¼" or 2" / T-2 nose pieces #2458105 and #2408150 with 5 mm T-2 thread. We currently have no plans to remove the two previous nosepieces from our product range.
- Nosepiece with Baader proprietory Safety Kerfs grooves so that even the heaviest accessories cannot fall to the ground
- Equipped with only 3 mm long T-2 thread
- Eyepiece-/camera side with male T-2 and M48 threads
- Telescope side with 2" outer diameter and 48mm filter thread for 2" filters
- Effective optical length 3 mm
[br]
- Nosepiece with 28mm insertion length, with Baader proprietory Safety Kerfs
- With only 3 mm long T-2 thread for modern CMOS cameras
- Eyepiece side with T-2 malel thread, telescope side with 1¼" outer diameter
- Incl. filter thread M28.5 for all 1¼" filters
- Optical path length: 1.5 mm
[br]
Quick Changing Rings to our Baader M48 System with only 3 mm long M48 thread for modern CMOS Cameras
- M48 female thread Heavy Duty Quick Changer
- Creates with the [product sku="2958595"] a quick-change and rotating device with the highest load capacity
- Optical path length 11 mm
- Quick release clamping for heavy accessories - with brass-clamping
- The changing system fits between any M48 connection[br]
- M48 male thread quick coupler with 50 mm dovetail
- Creates a quick change and rotating device with standard load capacity when coupled with [product sku="2958590"], part of [product sku="2958593"]
- Quick Changing Ring made from high performance steel
- The changing system fits between any M48 connection
- Optical length: 4mm[br]
- Heavy Duty M48 Quick Changing System enables lightning-fast changes between cameras, filter wheels or ClickLock eyepiece clamps, for example.
- Optical path length 15mm
- Consists of [product sku="2958590"] and [product sku="2958595"] with 50mm dovetail
- Quick-change and rotating device with maximum load capacity[br]
New ext
ension tubes for our
Baader M48 System: with only 3 mm long M48 thread for modern CMOS Cameras
All adapters to the M48 system can be found here
- Used to adjust the working distance of larger cameras and similar accessories with M48 thread
- Telescope side M48 internal thread, 3.5 mm depth
- Eyepiece-/camera side M48 external thread, 3 mm depth
- Baader M48 extension rings available in the sizes 5mm, 7.5mm, 10mm, 15mm , 30 and 40mm
- The Baader M48 extension rings 30mm and 40mm also serve as 2" nosepiece with Safety Kerfs.
- Aluminium[br]
[br]
StarAid Revolution Standalone Autoguiding – Revision B
[product sku="1485001"]
Due to high demand, there are no more large quantities in stock, but we expect another delivery by the end of March 2021.
- Stand-alone lightweight autoguider with AI-powered automatic polar alignment and built-in plate solving, now available in Revision B with new features
- camera control with dithering
- comet tracking
- USB-C Port with USB (5.0 V) instead of a DC Port (12V). The USB-C Port is both on the splitter, and on the StarAid
- Shorter housing, only 6,3 cm long
- StarAid automatically monitors the seeing conditions and the mount response
- No laptop is needed – control and troubleshoot with your smartphone
- Focusing via Live View function
- Starts guiding your mobile setup immediately when powered up - no user interaction is needed
- With built-in WiFi
- Multi-Star Guiding
- High Quality – improves image quality by up to 30% due to faster and multi-star guiding
- Polar alignment in 30 seconds – High accuracy: typically ~30” within about 2 minutes
- 2 LED lights indicate status of guiding
- Automatic platesolving within 2 seconds
- Powered via USB or a USB power bank
- Only one cable for easier set-up and less flexure
- 1¼ fitting, optional CS mount
- Antidust, no-fingerprint housing
- All mounts with an ST-4 compatible guide port and adjustable screws or knobs are supported (even single-axis tracking platforms)
The long awaited and much requested cameras - QHY294M-Pro and the QHY268M - have been pre-ordered and are expected to be available at Baader Planetarium from December 15th.
QHY294M Pro – Expanded Pixel Mode from 11.7 MP to 46.8 Megapixel!
The QHY294M Pro will soon be delivered to us in larger quantities and is expected to be available from Baader Planetarium.
The new QHY 294 Pro Series is a 4/3-inch camera equipped with the Sony IMX 294 (color) and IMX 492 (mono) sensor. The 294 Pro has 11.7 megapixels at 4.63 µm and 14 bit data depth. Both sensors are Back Side Illuminated.
The IMX 294 and IMX 492 chips have 46.8 million 2.315µm pixels, which Sony 2x2 bins on-chip to create the sensor's advertised 11.7 million 4.63 µm pixel array. The QHY 294 Pro series camera is capable of locking and unlocking the on-chip binning to provide two readout modes. The first mode reads the sensor in "locked" mode to produce 11.7 MP images with 4.63 µm pixel size and 14 bits per pixel. The second mode unlocks the binning to produce 46.8 MP images with 2.315 µm pixel size at 12 bits per pixel.
With the ability to use the 294 PRO with two different pixel sizes, it can also be used for two different focal lengths, matching the optimum resolution of the telescope.
- Mode 1 for telephoto lenses and Mode 0 for longer focal length systems.
- For narrow-band photographers, the 296 M-PRO can be combined with the [product sku="QHYCFW"] with or without [product sku="QHYOffAxisGuider"] with adapters that provide the 55 mm back focus required by many optical systems.
QHY268M – IMX571 Back Illuminated Sensor in Monoversion
The QHY268M is the first monochrome CMOS camera with an APS-C sensor. The chip has the same functions as the flagship QHY600M:
- USB Re-connection with 12V ON/OFF
- Extended Full Well and Multiple Read Modes
- Random thermal noise suppression
- 20Gb optical fiber transmission (PRO-Version)
- 1GB / 2GB oversized DDR3 memory
- Large programmable FPGA (only PRO)-Version
- Water-cooling option
By using the Sony IMX571 Back Illuminated Sensor, the price will be significantly lower. The high-resolution cooled, monochrome APS-C Camera uses a 26 Megapixel Sony IMX571 Back Iluminated Sensor with 16-bit A/D and 3.76um pixels. The QHY268 will be available as photo version and pro version. Image quality is identical between the two models.
Photgraphic Model QHY268 PHOTO: |
Professional Model QHY268 PRO: |
- USB3.0
- 6 FPS, full frame, 16-bit images
- 6.8 FPS, full frame, 8-bit image
- Support for ROI at higher frame rates
|
- USB3.0
- 2×10Gigabit optical fiber interface
- Programmable trigger in/out
- Advanced timing interface for GPS
- 6,9 FPS, full frame, 16-bit images
- Support for ROI at higher frame rates
- Customizable FPGA
Two 5m double fibre optic cables and two optical fibre modules are included with the camera. |
QHY-5-III-485C – Color Planetary and All Sky Camera
We are pleased to announce a new addition to QHYCCDs line of high speed, high QE, low noise, planetary cameras: the QHY-5-III-485C.
- Uses Sony's new IMX485 Color CMOS sensor
- Back-Side-Illuminated (BSI) sensor with high QE and very low noise
- 8.4 megapixel color CMOS sensor with an array of 3864 x 2176 pixels at 2.9um.
- With USB 3.0 interface, the full frame rate of 18.5 FPS at 16-bits or 44 FPS at 8-bits. Smaller regions of interest will yield even faster frame rates.
- This new camera makes a great planetary combo with the other newly released [product sku="QHY5III462C"] to photograph all objects of the solar system
- Includes a high resolution 8.3 MP All-Sky camera
While the QHY-5-III-485C does not have the extended near IR response of the QHY5III462C, it does have sHGC (Super High Cain Conversion) for exceptionally low (less than 1e-) read noise. For solar and lunar imaging, the NIR response is not required but the ability to take multiple short exposures in H-alpha light is ideal for solar use and making movies of solar prominences, arcs and eruptions.
The QHY-5-III-485C has 4 times the area of the smaller QHY-5-III-462C and 4 times the number of pixels. In area it is the same size as the popular IMX174 sensor but with back-illumination and higher resolution. The generous field of view provided by this larger sensor makes it ideal for solar and lunar imaging whereas the smaller, faster QHY 5-III-462C CMOS Camera (various versions available) with its enhanced IR response is superior for imaging planets like Jupiter, Saturn and Mars.
The QHY-5-III-485C standard package includes a 2.5mm Fisheye lens that converts the planetary camera into a high-resolution, 8.3 Megapixel All Sky camera with 180-degree field of view.
Cameras for Astronomy: from high time resolution sCMOS and EMCCD cameras to slow scan CCDs
We are pleased to announce our partnership with Oxford Instruments to offer the high end camera brand ANDOR Technology. This is primarily in response to requests from scientific institutes to integrate these high-quality special cameras into telescope systems and observation stations.
Andor Technology - an Oxford Instruments company - has achieved a special position in the development of cameras for very special applications in science and research in recent years. The performance of the models offered under the ANDOR brand name goes well beyond conventional limits. Exceptional quantum efficiencies of over 90% over a wide wavelength range are standard here. The sensors are in vacuum housings, which allows thermoelectric cooling down to -100°C (absolute sensor temperature). In combination with the special readout electronics of the cameras an extremely low readout noise is achieved.
The CCD models are particularly suitable for low-light applications and are also ideal for measurements requiring long exposure times. Such measurements also benefit from the extremely low dark current of this camera series.
sCMOS range: Balor, Marana, ZL41 Cameras
Andor's scientific CMOS cameras (sCMOS) represent a breakthrough technology based on the design and manufacturing techniques of the next generation of CMOS image sensors (CIS). Their unique characteristics make them ideal camera solutions for various applications in physics and astronomy.
Andor cameras are already used in many well-known observatories, e.g. in the flying observatory SOFIA, to discover and characterize e.g. exoplanets with highest efficiency, or to produce images with highest detail sharpness with Lucky Imaging.
Despite the comparably high prices, it certainly makes sense for some smaller research projects or even amateur astronomers to take a closer look at the ANDOR camera range. Finally, the special features of these cameras (e.g.: high QE, low readout noise, low dark current, sensor in vacuum housing) allow to further exploit the performance of existing instruments. Thus, the time needed to perform astronomical observations can be used more efficiently.
Case Study: Testing an ANDOR Marana sCMOS Camera on an High End amateur telescope on La Palma
Setup: 10micron GM 2000 HPS Mount, PlaneWave CDK 12,5 f/8 with Fused Silicia Mirror + Andor Marana 4.2B-6 sCMOS Camera
A first experiment with an ANDOR camera on a high end amateur telescope took place in July 2020 on La Palma, in cooperation with the well-known astrophotographer Christoph Kaltseis. It turned out that due to the sensitivity and the clean signal of the ANDOR cameras, excellent images can be obtained in a significantly reduced time. Surely the potential of the ANDOR Marana was used only rudimentarily in this test. Resourceful amateurs will in future explore the interaction of smaller telescopes and ANDOR cameras even further and achieve previously unattained results.
Read more on Andor Technology's website
[br]
You can find detailed information about the Andor cameras and technical details on our product pages:
We are glad that QHY has decided to offer the extremely promising IMX 455 SONY sensor in the consumer version after all, as all competitors do (but hiding the chip grade). So our customers now have more choice between 4 models of the QHY 600.
By using the IMX 455 in the new QHY600 L with a sensor of the consumer series, the price of the camera is reduced considerably. Compared to the other 3 models, the QHY-600-L is only available with a monochrome sensor. All Mono version of QHY600 PH & QHY600 PRO use IMX455 industry grade sensor (Grade-K) – except the QHY600-L
The QHY600-L is a new version of the QHY 600 camera series. It is similar to the QHY600 PH and the QHY600 PRO with a few exceptions (see table below) that make it the most competitive Sony IMX455 based camera on the market. Like the cameras of other manufacturers, the heart of the camera is equipped with a standard quality (C consumer) IMX455 sensor.
Like others in this price range, it uses the standard (consumer) grade, full frame 35mm format IMX455 sensor, two-stage cooling and fast USB3.0 interface. Unlike the competition, it has a large 1GB DDR3 image buffer, QHYCCD proprietary noise reduction technology, a humidity/pressure sensor in the sensor chamber and multiple read noise modes that are user selectable for lowest possible read noise or highest possible full well capacity. Also, the body has been reduced in length and is shorter than either the PH or PRO versions of the 600 series.
QHY 600 comparison table:
|
QHY600 L
|
QHY600 PH, Photographic Model |
QHY 600 PRO-L(ight)*
|
QHY600 PRO, Professional Model |
IMX 455 Sensorgrade |
-C (Consumer) |
-K (Industry): M-Version
-C (Consumer): C-Version |
-K (Industry) |
-K (Industry): M-Version
-C (Consumer): C-Version |
Mono/Color |
only Mono |
M/C |
only Mono |
M/C |
Length (w/dovetail ring) |
112 mm |
132 mm |
191 mm |
191 mm |
Diameter |
90 mm |
90 mm |
90 mm |
90 mm |
DDR 3 Image Buffer |
1GB |
1GB |
2GB |
2GB |
QHY filter wheel socket |
Yes |
Yes |
Yes |
Yes |
USB3.0
|
Yes |
Yes |
Yes |
Yes |
Humidity/Pressure Sensor |
Yes |
Yes |
Yes |
Yes |
Short back focus option |
No |
Yes |
Yes |
Yes |
Water cooling option |
No |
Yes |
Yes |
Yes |
ACC Socket |
No |
No |
Yes |
Yes |
GPS Box Option |
No |
No |
Yes |
Yes |
2 x 10 GB Ethernet |
No |
No |
No |
Yes |
Upgrade to full PRO Option |
No |
No |
Yes |
- |
All other technical data (also the readout modes) of the QHY-600-L are identical with the other models.
* formerly QHY-600-EB
A note in our own behalf on the topic of chip quality: We have at https://www.baader-planetarium.com/en/blog/why-is-the-qhy600-cmos-camera-more-expensive-than-models-from-other-manufacturers/ done a lot of effort into describing the differences of a CMOS image sensor between a consumer and an industrial version. There we state among other
the industry grade sensor is designed for longer life under normal use and can therefore withstand repeated cooling/heating cycles with less thermal stress, resulting in a longer life for a cooled camera. AND industrial sensors have a significantly lower number of pixel defects.""
If you decide to buy a QHY-600-L with the sensor in consumer quality, we strongly recommend to cool down the camera/sensor slowly, to cool down only so deep that the raw images are as low-noise as possible and especially not to switch off the cooled camera "hard", but to slowly increase the sensor temperature up to the outside temperature before switching off the power supply.
The GM 2000 HPS II COMBI combines the solid stability of the GM2000 HPS II Monolith with the portability of the GM 2000 HPS II Ultraport. These two mounts are no longer produced and will be replaced by this successor model.
This mount is basically a GM2000 HPS II Ultraport (“splittable” in two parts) with an additional lockingsystem; next to the quick locking system,which is very useful to carry and assemble the mount in the field, a further locking system was added for customers who have the mount permanently installed in an observatory. This will ensure agreat long-term stability, comparable to a GM2000 HPS II Monolith.
You can easily revert themount into a portable (“splittable”) version simply by removing the lockingscrews. This way the new GM2000 HPS II COMBI combines both advantages of the previous models in one single mount!
The technical specifications, sizes and weight of the new GM2000 HPS II COMBI are exactly the same as of the GM2000 HPS II Ultraport.
The GM2000 HPS II COMBI is now available.
Learn more about the GM 2000 HPS II COMBI on our 10micron product pages