Examinando por Autor "Cappellaro, Enrico"

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    Architecture of the SOXS instrument control software
    (SPIE, 2018-06) Ricci, Davide; Baruffolo, Andrea; Salasnich, Bernardo; Fantinel, Daniela; Urrutia, Josefinab; Campana, Sergio; Claudi, Riccardo; Schipani, Pietro; Aliverti, Matteo; Ben-Ami, Sagi; Biondi, Federico; Brucalassi, Anna; Capasso, Giulio; Cosentino, Rosario; D'Alessio, Francesco; D'Avanzo, Paolo; Diner, Oz; Kuncarayakti, Hanindyo; Munari, Matteo; Rubin, Adam; Scuderi, Salvo; Vitali, Fabrizio; Achrén, Jani; Araiza-Durán, José A.; Arcavi, Iair; Bianco, Andrea; Cappellaro, Enrico; Colapietro, Mirko; Della Valle, Massimo; D'Orsi, Sergio; Fynbo, Johan; Gal-Yam, Avishay; Genoni, Matteo; Hirvonen, Mika; Kotilainen, Jari; Kumar, Tarun; Landoni, Marco; Lehti, Jussi; Li Causi, Gianluca; Marafatto, Luca; Mattila, Seppo; Pariani, Giorgio; Pignata, Giuliano; Rappaport, Michael; Tarunp, Landon; Landoni, Marco; Lehti, Jussi; Li Causi, Gianluca; Marafatto, Luca; Mattila, Seppo; Pariani, Giorgio; Pignata, Giuliano; Rappaport, Michael; Riva, Marco; Smartt, Stephen; Turatto, Massimo; Zánmar Sánchez, Ricardo
    SOXS (Son Of X-Shooter) is a new spectrograph for the ESO NTT telescope, currently in the final design phase. The main instrument goal is to allow the characterization of transient sources based on alerts. It will cover from near-infrared to visible bands with a spectral resolution of R 1/4 4500 using two separate, wavelength-optimized spectrographs. A visible camera, primarily intended for target acquisition and secondary guiding, will also provide a scientific "light" imaging mode. In this paper we present the current status of the design of the SOXS instrument control software, which is in charge of controlling all instrument functions and detectors, coordinating the execution of exposures, and implementing all observation, calibration and maintenance procedures. Given the extensive experience of the SOXS consortium in the development of instruments for the VLT, we decided to base the design of the Control System on the same standards, both for hardware and software control. We illustrate the control network, the instrument functions and detectors to be controlled, the overall design of SOXS Instrument Software (INS) and its main components. Then, we provide details about the control software for the most SOXS-specific features: Control of the COTS-based imaging camera, the flexures compensation system and secondary guiding. © 2018 SPIE.
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    Development status of the UV-VIS detector system of SOXS for the ESO-NTT telescope
    (SPIE, 2020) Cosentino, Rosario; Hernandez, Marcos; Ventura, Hector; Campana, Sergio; Claudi, Riccardo; Schipani, Pietro; Aliverti, Matteo; Baruffolo, Andrea; Ben-Ami, Sagi; Biondi, Federico; Capasso, Giulio; D'Alessio, Francescoi; D'Avanzo, Paolo; Hershko, Ofir; Kuncarayakti, Hanindyoj; Landoni, Marco; Munari, Matteo; Pignata, Giuliano; Rubin, Adam; Scuderi, Salvatore; Vitali, Fabrizio; Young, David; Achrén, Jani; Araiza-Duran, José Antonio; Arcavi, Iair; Brucalassi, Anna; Bruch, Rachel; Cappellaro, Enrico; Colapietro, Mirko; della Valle, Massimo; de Pascale, Marco; Di Benedetto, Rosario; D'Orsi, Sergio; Gal-Yam, Avishay; Genoni, Matteo; Kotilainen, Jari; Li Causi, Gianluca; Mattila, Seppo; Rappaport, Michael; Radhakrishnan, Kalyan; Ricci, Davide; Riva, Marco; Salasnich, Bernardo; Smartt, Stephen; Sanchez, Ricardo Zanmar; Stritzinger, Maximilian; Accardo, Matteo; Mehrgan, Leander H.; Hopgood, Joshn
    SOXS will be the new spectroscopic facility for the ESO NTT telescope able to cover the optical and NIR bands by using two different arms: the UV-VIS (350-850 nm), and the NIR (800-2000 nm). In this article, we describe the development status of the visible camera cryostat, the architecture of the acquisition system and the progress in the electronic design. The UV-VIS detector system is based on a CCD detector 44-82 from e2v, a custom detector head, coupled with the ESO continuous flow cryostats (CFC), a custom cooling system, based on a Programmable Logic Controller (PLC), and the New General Controller (NGC) developed by ESO. This paper outlines the development status of the system, describes the design of the different parts that make up the UV-VIS arm and is accompanied by a series of information describing the SOXS design solutions in the mechanics and in the electronics parts. The first tests of the detector system with the UV-VIS camera will be shown. © 2020 SPIE
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    MITS: The multi-imaging transient spectrograph for SOXS
    (SPIE, 2018-06) Rubin, Adam; Ben-Ami, Sagi; Hershko, Ofir; Rappaport, Michael; Diner, Oz; Gal-Yam, Avishay; Campana, Sergio; Claudi, Riccardo; Schipani, Pietro; Aliverti, Matteo; Baruffolo, Andread; Biondi, Federico; Brucalassi, Anna; Capasso, Giulio; Cosentino, Rosario; D'Alessio, Francesco; D'Avanzo, Paolo; Kuncarayakti, Hanindyo; Munari, Matteo; Scuderi, Salvatore; Vitali, Fabrizio; Achrén, Jani; Araiza-Duran, José Antonio; Arcavi, Iair; Bianco, Andrea; Cappellaro, Enrico; Colapietro, Mirko; Della Valle, Massimo; D'Orsi, Sergio; Fantinel, Daniela; Fynbo, Johan; Genoni, Matteo; Hirvonen, Mika; Kotilainen, Jari; Kumar, Tarun; Landoni, Marco; Lehti, Jussi; Li Causi, Gianluca; Marafatto, Luca; Mattila, Seppo; Pariani, Giorgio; Pignata, Giuliano; Ricci, Davide; Riva, Marco; Salasnich, Bernardo; Zanmar Sanchez, Ricardo; Smartt, Stephen; Turatto, Massimo
    The Son Of X-Shooter (SOXS)1 is a medium resolution spectrograph (R ∼ 4500) proposed for the ESO 3.6m NTT. We present the optical design of the UV-VIS arm of SOXS which employs high efficiency ion-etched gratings used in first order (m = 1) as the main dispersers. The spectral band is split into four channels which are directed to individual gratings, and imaged simultaneously by a single three-element catadioptric camera. The expected throughput of our design is > 60% including contingency. The SOXS collaboration expects first light in early 2021. This paper is one of several papers presented in these proceedings2-10 describing the full SOXS instrument. © 2018 SPIE.
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    Optical design of the SOXS spectrograph for ESO NTT
    (SPIE, 2018-06) Zanmar Sanchez, Ricardo; Munari, Matteoa; Rubin, Adam; Ben Ami, Sagi; Brucalassi, Anna; Kuncarayakti, Hanindyo; Achrén, Jani; Campana, Sergio; Claudi, Riccardo; Schipani, Pietro; Aliverti, Matteo; Baruffolo, Andrea; Biondi, Federico; Capasso, Giulio; Cosentino, Rosario; D'Alessio, Francesco; D'Avanzo, Paolo; Scuderi, Salvatore; Vitali, Fabrizio; Araiza-Durán, José Antonio; Arcavi, Iair; Bianco, Andrea; Cappellaro, Enrico; Colapietro, Mirko; Della Valle, Massimo; Diner, Oz; D'Orsi, Sergio; Fantinel, Daniela; Fynbo, Johano; Gal-Yam, Avishay; Genoni, Matteo; Hershko, Ofir; Hirvonen, Mika; Kotilainen, Jari; Kumar, Tarunk; Landoni, Marco; Lehti, Jussi; Li Causi, Gianluca; Marafatto, Luca; Mattila, Seppo; Pariani, Giorgio; Pignata, Giuliano; Rappaport, Michael; Ricci, Davide; Riva, Marco; Smartt, Stephen; Turatto, Massimo; Salasnich, Bernardo
    An overview of the optical design for the SOXS spectrograph is presented. SOXS (Son Of X-Shooter) is the new wideband, medium resolution (R>4500) spectrograph for the ESO 3.58m NTT telescope expected to start observations in 2021 at La Silla. The spectroscopic capabilities of SOXS are assured by two different arms. The UV-VIS (350-850 nm) arm is based on a novel concept that adopts the use of 4 ion-etched high efficiency transmission gratings. The NIR (800- 2000 nm) arm adopts the 4C' design (Collimator Correction of Camera Chromatism) successfully applied in X-Shooter. Other optical sub-systems are the imaging Acquisition Camera, the Calibration Unit and a pre-slit Common Path. We describe the optical design of the five sub-systems and report their performance in terms of spectral format, throughput and optical quality. This work is part of a series of contributions1-9 describing the SOXS design and properties as it is about to face the Final Design Review. © 2018 SPIE.
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    The Type IIn Supernova SN 2010bt: The Explosion of a Star in Outburst
    (Institute of Physics Publishing, 2018-06) Elias-Rosa, Nancy; Van Dyk, Schuyler D.; Benetti, Stefano; Cappellaro, Enrico; Smith, Nathan; Kotak, Rubina; Turatto, Massimo; Filippenko, Alexei V.; Pignata, Giuliano; Fox, Ori D.; Galbany, Lluis; González-Gaitán, Santiago; Miluzio, Matteo; Monard L.A.G.; Ergon, Mattias
    It is well known that massive stars (M > 8 M ) evolve up to the collapse of the stellar core, resulting in most cases in a supernova (SN) explosion. Their heterogeneity is related mainly to different configurations of the progenitor star at the moment of the explosion and to their immediate environments. We present photometry and spectroscopy of SN 2010bt, which was classified as a Type IIn SN from a spectrum obtained soon after discovery and was observed extensively for about 2 months. After the seasonal interruption owing to its proximity to the Sun, the SN was below the detection threshold, indicative of a rapid luminosity decline. We can identify the likely progenitor with a very luminous star (log L/L ≈ 7) through comparison of Hubble Space Telescope images of the host galaxy prior to explosion with those of the SN obtained after maximum light. Such a luminosity is not expected for a quiescent star, but rather for a massive star in an active phase. This progenitor candidate was later confirmed via images taken in 2015 (∼5 yr post-discovery), in which no bright point source was detected at the SN position. Given these results and the SN behavior, we conclude that SN 2010bt was likely a Type IIn SN and that its progenitor was a massive star that experienced an outburst shortly before the final explosion, leading to a dense H-rich circumstellar environment around the SN progenitor. © 2018. The American Astronomical Society. All rights reserved.