ALPY product line has been designed around standard mechanical threads (M42x075, SM1, SM05) to facilitate the integration with your existing instrumentation.
ALPY product line also includes a separate guiding module (mirror slit 23µm) and a calibration module with neon/argon and tungsten lamps. ALPY offers a complete solution for astronomical spectroscopy. Each ALPY module is independant, making ALPY unique and revolutionnary.
Beyond modularity between the Alpy 600 spectrograph, guiding module and calibration module, the spectrograph itself is versatile and multi-purpose.
It's versatility allows interface with most CCD cameras with a standard M42x0.75mm thread. A C-mount adapter is available as well as a barlow lens element extending the backfocus and enlarging the spectrum, specially designed for Digital SLRs.
The removable standard slit includes multiple positions (25µm hole; 25µm, 50µm, 100µm or 300µm slits; 5µm tolerance) with a clear position (3mm hole) for a slitless mode.
A fiber connector mounting is also available making the Alpy 600 compatible with our optical fiber eShel solution.
Last but not least, the Alpy 600 is also a visual spectroscope (with or without slit) with an optional widening lens element. Watch for solar spectrum with Alpy 600 alone, or look for stars or nebulae spectra using Alpy 600 as an eyepiece on your telescope (diamètre 31.75mm).
ALPY product line benefits from Shelyak's experience and expertise in the area of astronomical spectroscopy. For exemple, Alpy 600 optics have been specially designed for this spectrrograph, allowing an excellent quality spectrum through all the visible domain from near-UV to near-IR (calcium triplet).
The ALPY product line benefits from our experience and expertise in the area of astronomical spectroscopy. For example, the Alpy 600 optics have been specially designed for this spectrograph, giving an excellent quality spectrum through all the visible domain from near-UV (Balmer serie, astonishing H&K lines) to near-IR (calcium triplet).
Lambda max is the wavelength at which the maximum fraction of light is absorbed by a solution. Lambda (λ) is a Greek letter that scientists use as the symbol for wavelength.
Lambda max is the wavelength at which the maximum fraction of light is absorbed by a solution(in this case by Alpy600). Lambda (λ) is a Greek letter, that scientists use as the symbol of wavelength.
multi-position non reflective slit: 25µm hole, 25µm/50µm/100µm/300µm slits, 3mm hole
- spectrograph core with 600gr/mm grism, second order filter (cuts around 720nm and above) and collimator lens
- M42x0.75 camera adapter with objective lens (focus adjustable for CCD back focus: 10.5-21mm)
- 1.25inch telescope adapter
- Alpy 600 mechanical body
Below are first spectra with the Alpy 600 using a Stellarvue SV80S APO and The Imaging Source DMK41 video camera, or, Atik ATK16 CCD camera. Results with the DMK41 camera have been outstanding. However, the Atik ATK16 CCD camera 8um pixels with the SV80S 480mm FL produces images that are considerably under-sampled. The resulting spectra contain distorted continuum, primarily on the blue end - in part this is due to the slight curvature ('smile') of the 2D spectra produced by the grating-prism (grism). The curved spectra traverses several horizontal rows of pixels, but because of under-sampling, the transition is in rough gradient steps. It may be possible to reduce the under-sampling distortions by slightly defocusing the telescope to enlarge the star on the slit. Some experimenting is in order.
I did not purchase the Alpy 600 with its guiding module (...eventually). So far I have been able to center a bright star on the spectrograph slit, then carefully align the 80mm guide scope utilizing the cross-hair reticule function in the PHD guiding software and TIS DMK21 video camera. Once the guide scope is aligned and locked in I can center fainter stars on the slit, then switch to guiding mode. Still lots to try and learn.
So far the Alpy 600 is a winner. Initial setup is pretty straight forward, and well explained in the introduction / instructions on the included CD. From what I have seen so far, it is a VERY well thought out instrument, the results speak for themselves.
I purchased the Alpy 600 from Woodland Hills Telescopes @ telescope.net -- helpful, informative service.
Stellarvue SV80S f/6, 80mm guidescope, Losmandy GM8 mount
|Flip-mirror, Alpy 600 spectrograph, Atik ATK16 CCD camera|
The following are spectroscopy graphs of different stars using the Alpy 600 from Shelyak. The X Axis is the measurement of wavelengths (measured in Angstroms in this case) while the Y Axis represents the number of times the spectrograph instrument detected that wavelength. For example, take a look at the graph below of EZ Cma Wolf Rayet Star. Since these types of stars are losing mass extremely rapidy, these stars tend to have less hydrogen and more helium and nitrogen. In the case of EZ Cma, helium is abudant. If you would rather get the results in nanometers, simply divide the Angstroms number by 10. So therefore He II below would be at 656 nm.
Above, spectra of Wolf-Rayet star EZ Cma with Alpy 600 spectrograph using a SV80S and Atik ATK16 CCD camera. Below is a similar Wolf-Rayet star, WR141, recorded with a Star Analyzer SA100, 100 lines/mm grating, using same scope and camera. The increase in spectral resolution is clearly apparent in the Alpy 600 spectra above.
Alpha Orionis "Betelgeuse", Alpy 600, SV80S, DMK41 video
Beta Auriga, Alpy 600, SV80S, DMK41 video
Spectra of Orion Nebula core next to Trapezium star groug, Alpy 600, SV80S, DMK41 video
Solar spectra, Alpy 600, SV80S, DMK41 video
Be star Zeta Tauri, Alpy 600, SV80S, DMK41 video
|Name||Shelyak - Alpy 600 Base Module Spectrograph|
|Custom Stock Status||Ships in 3-5 Days|
|Camera Adaptable||T2 camera interface|
|CCD||M42X0.75mm (C- mount adapter optional)|
|Lo-Res Images||resolving power R~600 @ 6563Å|
|Prisms||grism (grating + prism) dispersive element|
|Spectral Response||3750Å - 7200Å|
|Telescope Interface||as eyepiece (31.75mm dia.)|
The ISIS software had a steep learning curve. There is no manual or help files - only a tutorial that refers to another tutorial that in turn refers to a third one. It is made slightly more confusing in that even though the tutorials are in English and the screen displays are in English, the figures in the instructions are in French. Many of the included files are in French with no English translations. Eventually I got most of it figured out.
The software would also be more useful if it had a way to print the displays. The only thing that can be printed is the final dispersion figure and this is a three step process. And there was a problem with this. ISIS was designed to interface with gruplot via the pgruplot function. The included CD includes version gnuplot 5.03. Unfortunately the pgruplot was deprecated starting with version 5.0 and I have not been able to change the calling routine in ISIS. After much hair pulling, I gave up and downloaded an older version and it works properly.
So far I only have the basic unit so aligning with a star in slit mode takes so work. I have a separate guide scope piggybacked on my main scope and have had no issues with 10 minute exposures. I do plan to get the guide module in the near future. (Posted on 3/15/2016)
As a low resolution spectroscope, it will not show the detailed features in emission lines as will be seen with a high resolution unit like the LHires III. But the advantages include a wider range of wavelengths so that more emission lines can be shown in a single image. There are many uses for low resolution spectroscopy, and this unit is very capable of producing high quality spectra suitable for scientific purposes.
(Posted on 2/7/2015)