Daystar SR-127 SolaREDi 0.4Å PE H-alpha Telescope ( .4SR127PE)

Daystar SR-127 SolaREDi 0.4Å PE H-alpha Telescope

The Daystar SR-127 SolaREDi 0.4Å PE H-alpha Telescope is now in carbon fiber. This dedicated design offers Quantum control completely built-in for easy set-up and operation.

Filters with 0.4 ångström bandwidths will reveal excellent surface contrast as well as fine chromosphere detail.

• Quality 127mm doublet objective by ISTAR Optical.
• Focal Length: 4064mm
• Digital readout and precision tuning control.
• Accurate to 0.01Å in center wavelength.  12VDC
• Uses 12VDC power can run off batteries.
• Same Quantum Control software capable.
• Robust, 2 inch steeltrack and rack and pinion focuser for added strength.
• Fully integrated DayStar filtration with classic DayStar Quantum control.
• 100% safe and fully blocked directly through the OTA
• 100% safe and fully blocked directly through white light solar finder scope

Recommended:  Tele Vue 55mm Plossl eyepiece for full disk or Tele Vue 32mm or 40mm plossl eyepieces for higher power views with the SR-127 Solar Telescope

Half-Bandwidth (Maximum @ f/30)	Views to Expect
0.8 ångström	Filters with 0.8 ångström bandwidths will reveal prominences in high contrast.
0.7 ångström	Filters with 0.7 ångström bandwidths will reveal prominences in high contrast and occasionally, surface texture. Prominences are generally larger with .7Å filters than in narrower bandwidths.
0.6 ångström	Filters with 0.6 ångström bandwidths will reveal some surface contrast as well as prominences.  A .6Å filter can be a good compromise for those having a difficult decision.
0.5 ångström	Filters with 0.5 ångström bandwidths will reveal better surface contrast as well as great prominences.
0.4 ångström	Filters with 0.4 ångström bandwidths will reveal excellent surface contrast as well as fine chromosphere detail.
0.3 ångström	Filters with 0.3Å ångström bandwidths will reveal superior surface contrast above any other filter. Views are generally somewhat dimmer.  Expect “Pencil-Thin” details on surface and prominence features.

Quantum PE Grade Series

Our Quantum PE grade series is designed for professional research studies and applications in which precision homogeneity and onband transmitance values across the substrate surface are required. These filters require additional quality control steps and additional fabrication and testing time.

Our precision Quantum housing incorporates ALL of the desired features for today’s professional solar astronomer.

Daystar Filters is pleased to offer new, high resolution spectrographic scanning services for all our Quantum PE clients. Our new, specially engineered spectroscopic testing equipment provides high resolution mapping of all new DayStar Filters we manufacture.

PE grade filters are manufactured and qualified to a spectral uniformity in CWL (Central Wavelength) accuracy of ± 0.05 ångström*. Our high resolution etalon mapping equipment offers qualification certified accurate by independent testing with etalon transmission sample sizes of 5mm, 2mm or 1mm sample sizes with certification printouts available on new PE filter purchases.

*The mean peak wavelength of all 12 mm. dia. areas shall be within ± 0.05 ångström of the full aperture wavelength measurement.

H-alpha Wavelength

Various wavelengths are typically isolated as they relate to Fraunhofer lines. A majority of Quantum filters are applied in direct observation of the solar disk. Absorption lines of Hydrogen are extensively used for observation of the chromosphere and prominences. The Hydrogen Alpha (Hα) absorption line as observed from within the Earth’s atmosphere has a width of approximately 0.8 Å. Due to the presence of other absorption and emission lines near Hα, a filter of less than 1.0 Å width is required in order to isolate Hα light from the solar continuum. The narrower the FWHM, the greater isolation of desired wavelength and the greater the effective contrast in the observable image through exclusion of continuum and Doppler shifted light.

A filter of FWHM 1.0 Å or narrower is required to observe prominence detail. A filter of FWHM 0.7 Å or narrower is preferred to observe prominence detail and spicule. Light emitted from prominences typically travels at such velocity as to exhibit wing shift in red or blue wing. As filter bandpass is reduced, less wing shifted light emitted from prominences is allowed to pass and detail becomes finer in structure. Filters below 0.5 Å FWHM typically do not reveal as significant prominence structure.

A filter of FWHM 0.5 Å or narrower is suggested to observe surface structure of the chromosphere, while still revealing prominences. A filter of FWHM 0.4 Å or narrower is required to observe the chromospheric network. A filter of FWHM 0.3 Å is typically used only in research applications, for examination of surface and prominence structure with wing shift effects eliminated.