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The next Venus transit will be in December 2117… I took these pictures with my Coronado 90mm H-Alpha telescope in June 2012. You can get more information on this historical Venus 2012 transit on the Nasa web site.
Below is a picture of the first contact on the 5th of June 2012, at 3:07 PM PDT at San Bruno CA. The disk of Venus can be guessed in the mid-section.
A non-processed movie of the entry of Venus can be see below. It shows the first minute of the entry of the disc in front of the Sun.
The next picture was taken at 3:22 PM PDT. The Venus’ disk is clearly visible at this time. There is a large solar filament on the top of the image.
Later at 5:59PM PDT Venus is making its progression on the Solar disc. Solar spots can be seen on the left side of the Venus’ disc.
Mars is coming closer to opposition (first week of March). Its disc increased to over 12″, making it an easier astrophotography target.
On the 4th of February, the seeing was pretty good. Visually, at 400x or so, Mars disc was quite stable and full of details.
With a focal length of 7,000mm (using a barlow 2.5x), each pixel on the DMK covers about 0.15″.
On the right you can compare with a simulation of Mars disc captured on Calsky.org.
Location: San Bruno, CA
Seeing: 3/10, Transparency: 3/6, No Wind.
Celestron 11″ EdgeHD with DMK AS41 camera at F/D 10 (resolution: 1280×960)
Software: Avi Stack (stacking of about 800 frames each), Photoshop CS4, Astraimage Wavelet filter
Both pictures were taken using a Baader Infrared pass band filter IR742. Not only this filter improve images degraded by bad seeing, but it helps taking pictures of the moon by reducing the (sometime too) high contrast between different parts of the lunar landscape.
In the “virtual atlas of the moon” I can read the following:
Geological period: Nectarian (From -3.92 billions years to -3.85 billions years)
Size: Dimension: 638.0×638.0Km / 375.0×345.0Mi
Description:Formation with crater shape lengthened West East.
Very flat floor with ring of wrinkle ridge to the periphery and ghost craters to the South.
176 000 km2. 3.85 billion years old.
Langrenus (Top left) and Petavius (Bottom right)
The Petavius rille (or narrow valley) is easily visible from the mountains at the center of the crater, to the south rim. It said to have a dimension of 48Mi x 1.0Mi.
An smaller network of rilles is visible on the north west side of the crater.
On the cropped image below of the Petavius Crater, Petavius C (6.0Mi x 6.0Mi) and Petavius A (3.0Mi x 3.0 Mi) are highlighted. Petavius Rimae is 48Mi x 1Mi.
Location: San Bruno, California – Transparency 2/6 – Seeing 3/10
Telescope: Stellarvue 90mm Triplet with Flat field corrector
Camera: CCD Camera Qhy9 at 1×1 binning with Astronomik 12nm H-Alpha filter
This image is a detail of the Heart nebula (IC 1805) with my 90mm Stellarvue Triplet. I had to crop the image at the bottom of the frame, having some frosting issue with my CCD camera …
This is a composite image based on 20 images of 6min – totaling 2h of exposure.
The heart nebula is a great target for astrophotography, whether it is for wide field (picture I took in new mexico with 200mm tele) or a longer focal length such as below.
At 600mm of focal length (with the stellarvue 90mm), the nebula reveals complex details between the darker dusk lanes and bright parts of the emission nebula.
I took a couple of pictures when Jupiter was pretty close to opposition – here are some of these,
All pictures where shot from my observing site at San Bruno, CA.
I used my usual set up for this set of pictures. Seeing was above average, almost as good as on the 10/23/2011.
Processing was done using registax v6, photoshop cs4, and Astra image wavelet filter.
Date: 10/31/2011 at 7.11AM UTC
I used for this picture an athmospheric dispersion corrector, commercialized by Astro Electronic in Germany. I have been experimenting with this for a couple of months, and I concluded it significantly reduce the athmospheric dispersion for objects by or below 60 degree of altitude.
The effect is visible not only in the blue channel, but also in the luminance channel, enhancing the contrast of it. One of the main advantage is to be able to use a luminance channel even when the object is low in the horizon (below 50 degree).
Location: San Bruno, CA
Seeing was definitely above average this night.
The pictures below were taken with a 11″ Celestron EdgeHD, a 2.5x Barlow, and an imaging source DMK black and white camera.
Processing: Registax v6, astra image wavelet filter, photoshop cs4
This night not only the seeing was pretty good, but I could also enjoy a red spot transit. I was so busy taking snapshots this night I did not get a chance to observe Jupiter visually.
Last week ‘s seeing has been pretty good too. I can remember a great night last week where I clearly saw the disk or each of the four main Jovian satellite. I was visually able to compare at 600x magnification their relative disk sizes, and elusively saw some Albedo feature on Ganymede’s disk (optical illusion?).
This picture below is one of the best LRGB shot I was able to get this night. This is a composite picture of about 2,500 individual frames (1,000 for luminance, and 500 for each color channel).
The pictures below have been taken using the baader IR Pro 742nm filter.
Infrared imaging not only capture different features of Jupiter’s disk (methane absorbs IR wavelength),
but also minimizes the effect of bad seeing when imaging.
Images below are a composite of about 700 frames each.
Date: 9/4/2011 – 21H45 – 20 minute elapsed.
Coronado Solar Max II 90 mm and Imaging Source camera DMK 41AU02.as
This is a sequence of about 5,000 frames taken in 20min and combined into this short MPEG video. This prominence was extremely active, with changes happening visually in question of minutes.
Below is Sunspot group 1287, taken at 19H36min UTC
Next are the groups 1286, and 1277 taken at 20h57min UTC
Last, sunspot group 1283 taken at 20H49min UTC. The Sunspot group was close to the center of the sun .