Examinando por Autor "Stritzinger, Maximilian"

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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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    Monthly Notices of the Royal Astronomical Society
    (Oxford University Press, 2020-02) Clark, Peter; Maguire, Kate; Inserra, Cosimo; Prentice, Simon; Stephen, J. Smartt; Contreras, Carlos; Hossenizadeh, Griffin; Hsiao, Eric Y.; Kankare, Erkki; Kasliwal, Mansi; Nugent, Peter; Shahbandeh, Melissa; Baltay, Charles; Rabinowitz, David; Arcavi, Iair; Ashall, Chris; Burns, Christopher R.; Callis, Emma; Chen, Ting-Wan; Diamond, Tiara; Fraser, Morgan; Howell, D. Andrew; Karamehmetoglu, Emir; Kotak, Rubina; Lyman, Joseph; Morrell, Nidia; Phillips, Mark; Pignata, Giuliano; Pursiainen, Miika; Sollerman, Jesper; Stritzinger, Maximilian; Sullivan, Mark; Young, David
    This paper describes the rapidly evolving and unusual supernova LSQ13ddu, discovered by the La Silla-QUEST survey. LSQ13ddu displayed a rapid rise of just 4.8 ± 0.9 d to reach a peak brightness of −19.70 ± 0.02 mag in the LSQgr band. Early spectra of LSQ13ddu showed the presence of weak and narrow He I features arising from interaction with circumstellar material (CSM). These interaction signatures weakened quickly, with broad features consistent with those seen in stripped-envelope SNe becoming dominant around two weeks after maximum. The narrow He I velocities are consistent with the wind velocities of luminous blue variables but its spectra lack the typically seen hydrogen features. The fast and bright early light curve is inconsistent with radioactive 56Ni powering but can be explained through a combination of CSM interaction and an underlying 56Ni decay component that dominates the later time behaviour of LSQ13ddu. Based on the strength of the underlying broad features, LSQ13ddu appears deficient in He compared to standard SNe Ib. © 2019 The Author(s)
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    On the progenitor and supernova of the sn 2002cx-like supernova 2008ge
    (2010) Foley, Ryan J.; Rest, Armin; Stritzinger, Maximilian; Pignata, Giuliano; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia I.; Phillips, Mark M.; Salgado, Francisco
    We present observations of supernova (SN) 2008ge, which is spectroscopically similar to the peculiar SN 2002cx, and its pre-explosion site that indicate that its progenitor was probably a white dwarf. NGC 1527, the host galaxy of SN 2008ge, is an S0 galaxy with no evidence of star formation or massive stars. Astrometrically matching late-time imaging of SN 2008ge to pre-explosion HST imaging, we constrain the luminosity of the progenitor star. Since SN 2008ge has no indication of hydrogen or helium in its spectrum, its progenitor must have lost its outer layers before exploding, requiring that it be a white dwarf, a Wolf-Rayet star, or a lower-mass star in a binary system. Observations of the host galaxy show no signs of individual massive stars, star clusters, or H II regions at the SN position or anywhere else, making a Wolf-Rayet progenitor unlikely. Late-time spectroscopy of SN 2008ge show strong [Fe II] lines with large velocity widths compared to other members of this class at similar epochs. These previously unseen features indicate that a significant amount of the SN ejecta is Fe (presumably the result of radioactive decay of 56Ni generated in the SN), further supporting a thermonuclear explosion. Placing the observations of SN 2008ge in the context of observations of other objects in the class of SN, we suggest that the progenitor was most likely a white dwarf.
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    Supernova 2010ev: a reddened high velocity gradient type Ia supernova
    (EDP Sciences, 2016-04) Gutiérrez, Claudia P.; González-Gaitán, Santiago; Folatelli, Gastón; Pignata, Giuliano; Anderson, Joseph P.; Hamuy, Mario; Morrell, Nidia; Stritzinger, Maximilian; Taubenberger, Stefan; Bufano, Filomena; Olivares E., Felipe; Haislip, Joshua B.; Reichart, Daniel E.
    Ams. We present and study the spectroscopic and photometric evolution of the type Ia supernova (SN Ia) 2010ev. Methods. We obtain and analyze multiband optical light curves and optical/near-infrared spectroscopy at low and medium resolution spanning −7 days to +300 days from the B-band maximum. Results. A photometric analysis shows that SN 2010ev is a SN Ia of normal brightness with a light-curve shape of ∆m15(B) = 1.12 ± 0.02 and a stretch s = 0.94 ± 0.01 suffering significant reddening. From photometric and spectroscopic analysis, we deduce a color excess of E(B − V) = 0.25 ± 0.05 and a reddening law of Rv = 1.54 ± 0.65. Spectroscopically, SN 2010ev belongs to the broad-line SN Ia group, showing stronger than average Si ii λ6355 absorption features. We also find that SN 2010ev is a high velocity gradient SN with ˙vSi = 164 ± 7 km s−1 d −1 . The photometric and spectral comparison with other supernovae shows that SN 2010ev has similar colors and velocities to SN 2002bo and SN 2002dj. The analysis of the nebular spectra indicates that the [Fe ii] λ7155 and [Ni ii] λ7378 lines are redshifted, as expected for a high velocity gradient supernova. All these common intrinsic and extrinsic properties of the high velocity gradient (HVG) group are different from the low velocity gradient (LVG) normal SN Ia population and suggest significant variety in SN Ia explosions.