Using a laboratory set-up comprising i/ a 16 bits CCD camera ii/ a Littrow Further calibrations have been done with photometric accuracy Wavelength variations when using a quasi-parallel beam from a point-like sourceĪre presented. Polynomial curves precisely fitting the transmitted central Incidence the maximum transmission wavelength as well as the finesse wereĮvaluated. ThreeĮtalons of 40, 60 and 90 mm diameter were accurately analysed. We consider the use of the commercially available Fabry-Perot etalons (FP)įor the imaging of the solar chromosphere in the H alpha line of HI. The proposed NBI is also compared with similar instruments used around The theoretically estimated performance of Wavelength coverage, optimum spacing ratio, parasitic lightĬontribution, field-of-view, spectral and spatial resolution, Present the important design parameters of the instrument such as Several simulations and numerical studies have been carried out toĪrrive at the optimal design of the instrument. Solar atmosphere (one or more levels) with good temporal cadence. High precision polarimeter to obtain the vector magnetic fields of the Instrument will also have the additional capability of makingĭopplergrams at very high cadence.The instrument can be combined with a The instrument will be capable of observing the solarĪtmosphere at various wavelength positions of the spectral line with theĮxpected temporal cadence of about one spectral image per second. The NBI comprised of two Fabry-Perot interferometers The narrow band imager (NBI) is proposed to be one of theīack-end instrument for NLST to provide a spectral resolution of 40 m Proposed to build a 2-m class National Large Solar Telescope (NLST) toīe located at a site which is suitable for high resolution observations Indian Institute of Astrophysics (IIA) has Instruments deployed to study the dynamics of the solar features atĭifferent wavelengths. Besides, we give examples of solar chromospheric images in the Ha line core and wing.Ī large solar telescope is usually equipped with several post-focus The BF and pre-filter spectral parameters provide high-contrast monochromatic images.
The wavefront interferograms of optical elements and telescope as a whole show that the wavefront distortion of the optical path is within 0.25 λ. We describe for the first time the design features and their related BF passband tuning. All telescope optics was cleaned and adjusted. The optical immersion in the filter was changed. A contrast interference blocking filter and a new Iceland spar and quartz crystal plates instead of damaged ones were made and installed in the Hα birefringent filter (BF), manufactured by Bernhard Hallе Nachfl. A new reimaging lens to produce full-disk solar images 18 mm in diameter at the CCD camera Hamamatsu C-124 with a detector 36×24 mm (4000×2672 pixels) was designed and manufactured to replace the out-of-operation 50×50 mm Princeton Instruments camera. After several decades of observations with the chromospheric telescope at Baikal Astrophysical Observatory, a need arose to improve the characteristics of this telescope and filter. Besides, we give examples of solar chromospheric images in the Hα line core and wing.Ī chromospheric telescope is an important instrument for synoptic observations and solar research.
The BF and prefilter spectral parameters provide high-contrast monochromatic images. A contrast interference blocking filter and new calcite and quartz crystal plates were made and installed instead of damaged ones in the Hα birefringent filter (BF), manufactured by Bernhard Hallе Nachfl. A new reimaging lens to produce full-disk solar images 18 mm in diameter at the CCD camera Hamamatsu C-124 with a 36×24 mm detector (4000×2672 pixels) was designed and manufactured to replace the out-of-operation 50×50 mm Princeton Instruments camera. After several decades of observations with the chromospheric telescope at the Baikal Astrophysical Observatory, a need arose to improve the characteristics of this telescope and filter. A chromospheric telescope is an important instrument for synoptic observations and solar research.
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