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The Cherenkov Telescope Array Observatory (CTAO) consists of three types of telescopes: large-sized (LST), mediumsized (MST), and small-sized (SST), distributed in two observing sites (North and South). For the CTA South "Alpha Configuration" the construction and installation of 37 (+5) SST telescopes (a number that could increase up to 70 in future upgrades) are planned. The SSTs are developed by an international consortium of institutes that will provide them as an in-kind contribution to CTAO. The SSTs rely on a Schwarzschild-Couder-like dual-mirror polynomial optical design, with a primary mirror of 4 m diameter, and are equipped with a focal plane camera based on SiPM detectors covering a field of view of ~9°. The current SST concept was validated by developing the prototype dual-mirror ASTRI-Horn Cherenkov telescope and the CHEC-S SiPM focal plane camera. In this contribution, we will present an overview of the SST key technologies, the current status of the SST project, and the planned schedule.

We present the preliminary design of Cerberus, a new scientific instrument for the alt-az, 80cm OARPAF telescope in the Ligurian mountains above Genoa, Italy. Cerberus will provide three focal stations at the Nasmyth focus, allowing: imaging and photometry with standard Johnson-Cousins UBVRI+Ha+Free filters, an on-axis guiding camera, and a tip-tilt lens for image stabilization up to 10Hz; long slit spectroscopy at R 5900 thanks to a LHIRES III spectrograph provided with a 1200l/mm grism; \'echelle spectroscopy at R 9300 using a FLECHAS spectrograph with optical fiber., Comment: 6 pages, 4 figures. Submitted to Proceedings of SPIE Astronomical Telescopes + Instrumentation 2020

Specific astronomical science cases could take advantage of VPHG devices with design and features tailored for achieving the best performances. The manufacturing process require materials where it is possible to precisely control the efficiency response, specially in complex optical designs, where the realization tolerances have to be strictly fulfilled. In this paper, we present an innovative design for the DOLORES spectrograph @ TNG as an example of complex VPHG (in GRISM mode) based on photopolymers. This dispersing element and its prisms were designed to cover, with low R, more than one octave and to disentangle 1st and 2nd diffraction orders avoiding the typical contamination. The ok-sky results are finally presented.

Volume Phase Holographic Gratings (VPHGs) are diffractive elements widely employed in the field of astronomical spectrographs. Photosensitive materials are used for the production of such elements and photopolymers represent a very interesting possibility. In particular, Bayfol ® HX solid photopolymers are high performance holographic materials that have been already used for the realization of VPHGs working in the visible for small spectrographs. Recently, a new set of GRISMs have been commissioned at BFOSC spectrograph in order to replace worn or outperforming ones and improve the instrument throughput. The first dispersing element covers the Hα band, while the second one is designed to work in the UV down to 330 nm. Issues related to the material absorption and to the light scattering were faced at short wavelengths. A step forward in the implementation of this class of holographic materials is the design of VPHGs working in the infrared. Two gratings were designed, covering the ZJ band (0.8 – 1.35 μm) and the JH band (1.05 – 1.9 μm). RCWA simulations were performed to find the parameters (refractive index modulation and thickness) required to obtain high efficiency in the target spectral ranges. Material absorptions are not negligible in the NIR and have to be taken into account during the design phase. Preliminary writing tests were performed giving interesting results. In order to make the design phase more reliable, a study of the dependence of the refractive index modulation on wavelength was performed.

In the astronomical field, the progressive increase in telescope size and in the complexity of the spectroscopic instrumentation has highlighted how the current technologies and traditional materials for dispersing elements do not completely meet the present and future requirements. Therefore, new materials and solutions have to be developed, not only to realize future astronomical facilities, but also to improve the performances of already available instruments and devices. In this context, the use of photopolymeric materials for the production of Volume Phase Holographic Gratings (VPHGs) is becoming an interesting approach thanks to their key properties, in particular the self-developing, high sensitivity and the simple manufacturing process. Here, the main design parameters and the strategy to address them will be presented considering the whole UV-NIR spectral range showing the actual capabilities together with the results obtained on real observing astronomical facilities.