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7. METIS: final design of the Imager sub-system

Author

Bizenberger, P., Baumeister, H., Barriere, J.-C., Bertram, T., Böhm, A., Brandl, B., Cárdenas Vázquez, M.C., Chamorro, E., Feldt, M., Glauser, A.M., Henning, T., Laun, W., Lesman, D., Mohr, L., Raskin, G., Rohloff, R.-R., Scheithauer, S., Serra, B., Stepien, P., Stuik, R., Todd, S., Boekel, R. van, Evans, C.J., Bryant, J.J., Motohara, K., Evans, C.J., Bryant, J.J., and Motohara, K.

Published
2022
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9. MedRes

Author

Gratton, R., Keller, C.U., Diolaiti, E., Baruffolo, A., Bonnefoy, M., D'Orazi, V., Langlois, M., Loupias, M., N'Diaye, M., Pantin, E., Stadler, E., Wildi, F., Beuzit, J.-L., Boccaletti, A., Chauvin, G., Desidera, S., Mouillet, D., Bianco, A., Cascone, E., Cortecchia, F., De Caprio, V., De Rosa, A., Desgrange, C., Frangiamore, M., Landman, R., Lombini, M., Malaguti, G., Mesa, D., Milli, J., Morgante, G., Pichon, T., Schiavone, F., Schreiber, L., Terenzi, L., Zanutta, A., Evans, C.J., Bryant, J.J., Mohohara, K., Evans, C.J., Bryant, J.J., and Mohohara, K.

Published
2022

10. Upgrading the high contrast imaging facility SPHERE: science drivers and instrument choices

Author

Boccaletti, A., Chauvin, G., Wildi, F., Milli, J., Stadler, E., Diolaiti, E., Gratton, R., Vidal, F., Loupias, M., Langlois, M., Cantalloube, F., N'Diaye, M., Gratadour, D., Ferreira, F., Tallon, M., Mazoyer, J., Segransan, D., Mouillet, D., Beuzit, J.-L., Bonnefoy, M., Galicher, R., Vigan, A., Snellen, I.A.G., Feldt, M., Desidera, S., Rousseau, S., Baruffolo, A., Goulas, C., Baudoz, P., Bechet, C., Benisty, M., Bianco, A., Carry, B., Cascone, E., Charnay, B., Choquet, E., Christiaens, V., Cortecchia, F., Di Capprio, V., De Rosa, A., Desgrange, C., D'Orazi, V., Douté, S., Frangiamore, M., Gendron, E., Ginski, C., Huby, E., Keller, C.U., Kulcsár, C., Landman, R., Lagarde, S., Lagadec, E., Lagrange, A.-M., Lombini, M., Kasper, M., Ménard, F., Magnard, Y., Malaguti, G., Maurel, D., Mesa, D., Morgante, G., Pantin, E., Pichon, T., Potier, A., Rabou, P., Rochat, S., Terenzi, . l ., Thiébaut, E., Tallon-Bosc, I., Raynaud, H.-F., Rouan, D., Sevin, A., Schiavone, F., Schrieber, L., Zanutta, A., Evans, C.J., Bryant, J.J., Motohara, K., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Pôle Planétologie du LESIA, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Universidad de Chile = University of Chile [Santiago] (UCHILE), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève = University of Geneva (UNIGE), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Météo-France, INAF - Osservatorio Astronomico di Bologna (OABO), Istituto Nazionale di Astrofisica (INAF), INAF - Osservatorio Astronomico di Padova (OAPD), Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL), Laboratoire d'Astrophysique de Marseille (LAM), and Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), High Contrast Imaging, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Exoplanets, FOS: Physical sciences, Adaptive Optics, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Earth and Planetary Astrophysics, Coronagraphy
Abstract

SPHERE+ is a proposed upgrade of the SPHERE instrument at the VLT, which is intended to boost the current performances of detection and characterization for exoplanets and disks. SPHERE+ will also serve as a demonstrator for the future planet finder (PCS) of the European ELT. The main science drivers for SPHERE+ are 1/ to access the bulk of the young giant planet population down to the snow line ($3-10$ au), to bridge the gap with complementary techniques (radial velocity, astrometry); 2/ to observe fainter and redder targets in the youngest ($1-10$\,Myr) associations compared to those observed with SPHERE to directly study the formation of giant planets in their birth environment; 3/ to improve the level of characterization of exoplanetary atmospheres by increasing the spectral resolution in order to break degeneracies in giant planet atmosphere models. Achieving these objectives requires to increase the bandwidth of the xAO system (from $\sim$1 to 3\,kHz) as well as the sensitivity in the infrared (2 to 3\,mag). These features will be brought by a second stage AO system optimized in the infrared with a pyramid wavefront sensor. As a new science instrument, a medium resolution integral field spectrograph will provide a spectral resolution from 1000 to 5000 in the J and H bands. This paper gives an overview of the science drivers, requirements and key instrumental trade-off that were done for SPHERE+ to reach the final selected baseline concept., To appear in the Proceedings of the SPIE Astronomical Telescopes + Instrumentation (2022), 13 pages, 6 figure

Published
2022
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11. Status update on the development of METIS, the mid-infrared ELT imager and spectrograph

Author

Brandl, B.R., Bettonvil, F.C.M., Van Boekel, R., Glauser, A., Quanz, S.P., Absil, O., Feldt, M., Garcia, P.J.V., Glasse, A., Guedel, M., Labadie, L., Meyer, M., Pantin, E., Wang, S.-Y., Van Winckel, H., Agócs, T., Amorim, A., Bertram, T., Burtscher, L.H., Delacroix, C., Laun, W., Lesman, D., Raskin, G., Salo, C., Scheithauer, S., Stuik, R., Todd, S., Haupt, C., Siebenmorgen, R., Evans, C.J., Bryant, J.J., and Motohara, K.

Published
2022
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12. First on-sky results of ERIS at VLT

Author

Kravchenko, K., Dallilar, Y., Absil, O., Berbel, A.A., Baruffolo, A., Bonse, M., Buron, A., Cao, Y., Cortes, A., Dannert, F., Davies, R., De Rosa, R.J., Deysenroth, M., Doelman, D.S., Eisenhauer, F., Esposito, S., Feuchtgruber, H., Förster Schreiber, N., Gao, X., Gemperlein, H., Genzel, R., Gillessen, S., Ginski, C., Glauser, A., Glindemann, A., Grani, P., Haguenauer, P., Hartwig, J., Hayoz, J., Heida, M., Kenworthy, M.A., Kolb, J., Kuntschner, H., Lutz, D., Liu, D., MacIntosh, M., Marsset, M., Orban de Xivry, G., Özdemir, H., Puglisi, A., Quanz, S., Rau, C., Riccardi, A., Schuppe, D., Snik, F., Sturm, E., Tacconi, L., Taylor, W.D., Wiezorrek, E., Evans, C.J., Bryant, J.J., and Motohara, K.

Subjects
FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

ERIS (Enhanced Resolution Imager and Spectrograph) is a new adaptive optics instrument installed at the Cassegrain focus of the VLT-UT4 telescope at the Paranal Observatory in Chile. ERIS consists of two near-infrared instruments: SPIFFIER, an integral field unit (IFU) spectrograph covering J to K bands, and NIX, an imager covering J to M bands. ERIS has an adaptive optics system able to work with both LGS and NGS. The Assembly Integration Verification (AIV) phase of ERIS at the Paranal Observatory was carried out starting in December 2021, followed by several commissioning runs in 2022. This contribution will describe the first preliminary results of the on-sky performance of ERIS during its commissioning and the future perspectives based on the preliminary scientific results., Proceeding of SPIE Astronomical Telescopes + Instrumentation 2022

Published
2022
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16. Warm calibration unit of the mid-infrared ELT instrument METIS

Author

Rutowska, M., Sharma, T.K., Wiest, M., Graf, S., Labadie, L., Straubmeier, C., Eckart, A., Todd, S., Agócs, T., Raskin, G., Goris, J., Gerbers, M., Burtscher, L.H., Boekel, R. van, Glauser, A., Lynn, J., Brandl, B.R., Bettonvil, F.C.M., Evans, C.J., Bryant, J.J., and Motohara, K.

Published
2022
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18. Using structured, person-centred measures for people with dementia unable to self-report to identify and meet palliative care needs : reflections from empowering better end of life dementia care

Author

de Wolf-Linder, Susanne, Kupeli, N., Crawley, S., Reisinger, Margarete, Kenten, C., Gohles, E., Ellis-Smith, C., Davies, N., Moore, K., Sleeman, K., Schubert, Maria, Sampson, E.L., Murtagh, F.E.M., and Evans, C.J.

Subjects
616.8: Neurologie und Krankheiten des Nervensystems, 610.73: Pflege
Published
2021

22. Warm calibration unit of the mid-infrared E-ELT instrument METIS: overview and current status of the project

Author

Rutowska, M., Sharma, T., Wiest, M., Graf, S., Straubmeier, C., Rost, S., Labadie, L., Eckart, A., Burtscher, L., Agocs, T., Lesman, D., Stuik, R., Glauser, A., Brandl, B.R., Bettonvil, F.C.M., Evans, C.J., Bryant, J.J., and Motohara, K.

Subjects
Cryostat, Computer science, Interface (computing), Optical engineering, Systems engineering, Metis, Mid infrared, Calibration, Extremely Large Telescope, Unit (housing)
Abstract

The warm calibration unit (WCU) is one subsystem of the future METIS instrument on the European Extremely Large Telescope (E-ELT). Operating at daytime temperature, the WCU is mounted above the main cryostat of METIS and will be employed as calibration reference for science observations, as well as for verification and alignment purposes during the AIT phase. The WCU is designed and constructed at the University of Cologne, partner in the METIS consortium. The WCU, together with the full METIS instrument, went recently through a successful preliminary design review (PDR) phase at ESO and is entering now the Phase C of the project. In this paper, we present the current status of the WCU and summarize the mostly mechanical and optical engineering work. We adopted a hexapod unit to interface with the METIS cryostat and a CFRP-based optical bench to optimally cope with alignment flexure. We develop the case for fiber-fed laser sources feeding the integrating sphere for spectral calibration of the LM-Spectrograph of METIS. We detail the activity foreseen for Phase C including the optical tolerances analysis, the eigenfrequency and earthquake analysis and a preparation of the sub-system MAIT work, finishing the paper with a short overview of the WCU future plans.

Published
2020

23. 2D kinematics of massive stars near the Galactic Center

Author

Libralato, M., Lennon, D.J., Bellini, A., van der Marel, R., Clark, S.J., Najarro, F., Patrick, L.R., Anderson, J., Bedin, L.R., Crowther, P.A., de Mink, S.E., Evans, C.J., Platais, I., Sabbi, E., and Sohn, S.T.

Subjects
Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, Computer Science::Information Theory
Abstract

The presence of massive stars (MSs) in the region close to the Galactic Centre (GC) poses several questions about their origin. The harsh environment of the GC favours specific formation scenarios, each of which should imprint characteristic kinematic features on the MSs. We present a 2D kinematic analysis of MSs in a GC region surrounding Sgr A* based on high-precision proper motions obtained with the Hubble Space Telescope. Thanks to a careful data reduction, well-measured bright stars in our proper-motion catalogues have errors better than 0.5 mas yr−1. We discuss the absolute motion of the MSs in the field and their motion relative to Sgr A*, the Arches, and the Quintuplet. For the majority of the MSs, we rule out any distance further than 3–4 kpc from Sgr A* using only kinematic arguments. If their membership to the GC is confirmed, most of the isolated MSs are likely not associated with either the Arches or Quintuplet clusters or Sgr A*. Only a few MSs have proper motions, suggesting that they are likely members of the Arches cluster, in agreement with previous spectroscopic results. Line-of-sight radial velocities and distances are required to shed further light on the origin of most of these massive objects. We also present an analysis of other fast-moving objects in the GC region, finding no clear excess of high-velocity escaping stars. We make our astro-photometric catalogues publicly available.

Published
2020

25. High Speed Grinding of Silicon Nitride With Electroplated Diamond Wheels

Author

Hwang, T.W., Evans, C.J., and Malkin, S.

Subjects
Production engineering research -- Analysis, Surface preparation -- Analysis, Silicon nitride -- Research, Diamond wheels -- Usage, Electroplating -- Analysis, Engineering and manufacturing industries, Science and technology
Abstract

This is the second in a series of two papers concerned with high speed grinding of silicon nitride with electroplated diamond wheels. In the first article (ASME J. Manuf. Sci. Eng., 122, pp. 32-41), it was shown that grinding of silicon nitride is accompanied by dulling of the abrasive grains and a significant increase in the grinding forces and power. High wheel speed caused more wheel wear, which was attributed to a longer accumulated sliding length between the abrasive grains and the workpiece. This second paper is concerned with the progressive change in wheel topography during grinding and how it affects the grinding process. A statistical model is developed to characterize the wheel topography during grinding in terms of active cutting grains and wear flat area. According to this model, continued grinding is accompanied by an increase in both the number of active grains and the wear flat area on the wheel surface as the wheel wears down. The measured increase in grinding forces and power was found to be proportional to the wear flat area, which implies a constant average contact pressure and friction coefficient between the wear flats and the workpiece. Increasing the wheel speed from 85 to 149 m/s significantly reduced the contact pressure, which may be attributed to a reduction of the interference angle, but had almost no effect on the attritious wear rate of the diamond abrasive. Therefore, more rapid wear of the diamond wheel at higher wheel speeds due to a longer sliding length may be offset by reduced contact pressures and lower grinding forces.

Published
2000

27. A five-compartment model of body composition of healthy subjects assessed using in vivo neutron activation analysis

Author

Ryde, S.J.S., Birks, J.L., Morgan, W.D., Evans, C.J., and Dutton, J.

Subjects
Body composition -- Research, Radioactivation analysis -- Usage, Water -- Analysis
Abstract

In vivo neutron activation analysis and tritiate water analysis aided the development of a five-compartment model to estimate the body composition of healthy subjects of both sexes. The results obtained compare favorably with those arrived at using conventional methodology. A prediction equation provides the estimation of total body nitrogen in healthy humans, and is advantageous over the two-compartment model.

Published
1993

28. Spectroscopic confirmation of a galaxy at redshift z = 8.6

Author

Lehnert, M.D., Nesvadba, N.P.H., Cuby, J.-G., Swinbank, A.M., Morris, S., Clement, B., Evans, C.J., Bremer, M.N., and Basa, S.

Subjects
Observations, Usage, Methods, Spectroscopy -- Usage -- Methods, Activation analysis -- Methods -- Usage, Galaxies -- Observations -- Methods -- Usage, Radioactivation analysis -- Methods -- Usage, Spectrum analysis -- Usage -- Methods
Abstract

UDFy-38135539 was selected as a candidate z [approximately equal to] 8.6 galaxy from deep Wide Field Camera 3 observations of the Hubble Ultra Deep Field (5). Its red [Y.sub.105]-[J.sub.125] colour [...], Galaxies had their most significant impact on the Universe when they assembled their first generations of stars. Energetic photons emitted by young, massive stars in primeval galaxies ionized the intergalactic medium surrounding their host galaxies, cleared sightlines along which the light of the young galaxies could escape, and fundamentally altered the physical state of the intergalactic gas in the Universe continuously until the present day (1,2). Observations of the cosmic microwave background (3), and of galaxies and quasars at the highest redshifts (4), suggest that the Universe was reionized through a complex process that was completed about a billion years after the Big Bang, by redshift z ≅ 6. Detecting ionizing Lyman-a photons from increasingly distant galaxies places important constraints on the timing, location and nature of the sources responsible for reionization. Here we report the detection of Lyα photons emitted less than 600 million years after the Big Bang. UDFy-38135539 (ref. 5) is at a redshift of z = 8.5549 ± 0.0002, which is greater than those of the previously known most distant objects, at z = 8.2 (refs 6 and 7) and z = 6.96 (ref. 8). We find that this single source is unlikely to provide enough photons to ionize the volume necessary for the emission line to escape, requiring a significant contribution from other, probably fainter galaxies nearby (9).

Published
2010
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30. MOSAIC: the ELT multi-object spectrograph

Author

Jagourel, P., Fitzsimons, E., Hammer, F., De Frondat Laadim, F., Puech, M., Evans, C.J., Sanchez, R., Guinouard, I., Chemla, F., Frotin, M., Yang, Y., Parr-Burman, P., Morris, T., Dubbeldam, M., Close, M., Middleton, K., Rousset, G., Gendron, E., Kelz, A., Janssen, A., Pragt, J., Navarro, R., Larrieu, M., El Hadi, K., Dohlen, K., Dalton, G., Lewis, I., Rodrigues, M., Morris, S., Kaper, L., Barbuy, B., Cuby, J.-G., Le Fèvre, O., Simard, L., Takami, H., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), UK Astronomy Technology Centre, Royal Observatory Edinburgh (UKATC), Duke University [Durham], STFC Rutherford Appleton Laboratory, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Haute résolution angulaire en astrophysique, Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Leibniz-Institut für Astrophysik Potsdam (IAP), TNO/TPD-Space Instrumentation, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Univ. of Oxford (United Kingdom), Amsterdam, Departamento de Astronomia, Universidade de São Paulo, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Computer science, business.industry, media_common.quotation_subject, Near-infrared spectroscopy, Phase (waves), Mosaic (geodemography), 01 natural sciences, 010309 optics, Optics, Conceptual design, Sky, 0103 physical sciences, Extremely Large Telescope, business, Adaptive optics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Spectrograph, media_common
Abstract

International audience; Following a successful Phase A study, we introduce the delivered conceptual design of the MOSAIC1 multi-object spectrograph for the ESO Extremely Large Telescope (ELT). MOSAIC will provide R 5000 spectroscopy over the full 460-1800 nm range, with three additional high-resolution bands (R 15000) targeting features of particular interest. MOSAIC will combine three operational modes, enabling integrated-light observations of up to 200 sources on the sky (high-multiplex mode) or spectroscopy of 10 spatially-extended fields via deployable integral-field units: MOAO6 assisted high-definition (HDM) and Visible IFUs (VIFU). We will summarise key features of the sub-systems of the design, e.g. the smart tiled focal-plane for target selection and the multi-object adaptive optics used to correct for atmospheric turbulence, and present the next steps toward the construction phase.

Published
2018
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34. List of Contributors

Author

Abercrombie, E.D., primary, Benveniste, H., additional, Bungay, P.M., additional, Camp, D.M., additional, Damsma, G., additional, Dedrick, R.L., additional, De Boer, J., additional, Di Chiara, G., additional, During, M.J., additional, Evans, C.J., additional, Finlay, J.M., additional, Flentge, F., additional, Hamberger, A., additional, Hansen, A.J., additional, Hsiao, J.K., additional, Hernandez, L., additional, Hillered, L., additional, Hoebel, B.G., additional, Jacobson, I., additional, Justice, J.B., additional, Kendrick, K.M., additional, Kissinger, P.T., additional, Korf, J., additional, Larsson, S., additional, Legan, S.J., additional, Levine, J.E., additional, Lönnroth, P., additional, Maidment, N.T., additional, Mark, G.P., additional, Mefford, I.N., additional, Meredith, J.M., additional, Morrison, P.F., additional, Nyström, B., additional, Persson, L., additional, Pettit, H.O., additional, Postema, F., additional, Robinson, T.E., additional, Sandberg, M., additional, Schwartz, D.H., additional, Ståhle, L., additional, Ungerstedt, U., additional, Venema, K., additional, Vogelsong, K.M., additional, West, H.L., additional, and Westerink, B.H.C., additional

Published
1991
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35. PLC-controlled cryostats for the BlackGEM and MeerLICHT detectors

Author

Raskin, G., Morren, J., Pessemier, W., Bloemen, S., Klein-Wolt, M., Roelfsema, R., Groot, P.J., Aerts, C., Evans, C.J., and Evans, C.J.

Subjects
Cryostat, 010308 nuclear & particles physics, business.industry, Computer science, Gravitational wave, Interface (computing), Astronomy, Detector, Electrical engineering, FOS: Physical sciences, Field of view, 01 natural sciences, law.invention, Telescope, Nova (rocket), Proceedings of SPIE - the International Society for Optical Engineering, law, Observatory, 0103 physical sciences, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, business, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

BlackGEM (BG) is an array of telescopes, currently under development at the Radboud University Nijmegen and at NOVA. It targets the detection of the optical counterparts of gravitational waves. The first 3 BG telescopes are planned to be installed in 2018 at the La Silla observatory. A single prototype telescope, named MeerLICHT, will already be commissioned early 2017 in Sutherland to provide an optical complement for the MeerKAT radio array. The BG array consists of, initially, a set of 3 robotic 65-cm wide-field telescopes. Each telescope is equipped with a single STA1600 CCD detector with 10.5k x 10.5k 9-mum pixels that covers a 2.7 square degrees field of view. The cryostats for housing these detectors are developed and built at the KU Leuven University. The operational model of BG requires long periods of reliable ands-off operation. Therefore, we designed the cryostats for long vacuum hold time and we make use of a closed-cycle cooling system, based on Polycold PCC Joule-Thomson coolers. A single programmable logic controller (PLC) controls the cryogenic systems of several BG telescopes simultaneously, resulting in a highly reliable, cost-efficient and maintenance-friendly system. PLC-based cryostat control offers some distinct advantages, especially for a robotic facility. Apart of temperature monitoring and control, the PLC also monitors the vacuum quality, the power supply and the status of the PCC coolers (compressor power consumption and temperature, pressure in the gas lines, etc.). Furthermore, it provides an alarming system and safe and reproducible procedures for automatic cool down and warm up. The communication between PLC and higher-level software takes place via the OPC-UA protocol, offering a simple to implement, yet very powerful interface. Finally, a touch-panel display on the PLC provides the operator with a user-friendly and robust technical interface., 11 pages, SPIE Astronomical Telescopes and Instrumentation 2016 Conference Proceedings

Published
2016

37. The ELT-MOS (MOSAIC)

Author

Morris, S., Hammer, F., Jagourel, P., Evans, C.J., Puech, M., Dalton, G.B., Rodrigues, M., Sanchez-Janssen, R., Fitzsimons, E., Barbuy, B., Cuby, J.-G., Kaper, L., Roth, M., Rousset, G., Myers, R., Le Fèvre, O., Finogenov, A., Kotilainen, J., Castilho, B., Ostlin, G., Feltzing, S., Korn, A., Gallego, J., Castillo Morales, Á., Iglesias-Páramo, J., Pentericci, L., Ziegler, B., Afonso, J., Dubbledam, M., Close, M., Parr-Burman, P., Morris, T.J., Chemla, F., De Frondat, F., Kelz, A., Guinouard, I., Lewis, I.J., Middleton, K., Navarro, R., Larrieu, M., Pragt, J., Janssen, A., Dohlen, K., El Hadi, K., Gendron, É., Yang, Y., Wells, M., Conan, J.-M., Fusco, T., Schaerer, D., Bergin, E., Taburet, S., Frotin, M., Berkourn, N., Simard, L., Takami, H., Department of Physics [Durham University], Durham University, Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), ​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​​ISIS Neutron and Muon Source (ISIS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC)-Science and Technology Facilities Council (STFC), Universidade de São Paulo (USP), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Universiteit van Amsterdam (UvA), Leibniz-Institut für Astrophysik Potsdam (AIP), University of Helsinki, Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Laboratorio Nacional de Astrofisica, Oskar Klein Centre [Stockholm], Stockholm University, Lund University [Lund], Uppsala University, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), Instituto de Astrofísica de Andalucía (IAA), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), INAF - Osservatorio Astronomico di Roma (OAR), Istituto Nazionale di Astrofisica (INAF), Universität Wien, Observatório Astronómico de Lisboa, University of Oxford [Oxford], Netherlands Research School for Astronomy, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), DOTA, ONERA, Université Paris Saclay (COmUE) [Châtillon], ONERA-Université Paris Saclay (COmUE), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), University of Michigan [Ann Arbor], University of Michigan System, High Energy Astrophys. & Astropart. Phys (API, FNWI), Universidade de São Paulo = University of São Paulo (USP), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Helsingin yliopisto = Helsingfors universitet = University of Helsinki, University of Oxford, Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), and Université de Genève = University of Geneva (UNIGE)

Subjects
Astrofísica, ASTRONOMICAL IMAGING, Age of the universe, Computer science, media_common.quotation_subject, Dark matter, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Cosmology, 010309 optics, [SPI]Engineering Sciences [physics], Optical Fibres, 0103 physical sciences, Adaptive optics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Spectrograph, Galaxy rotation curve, media_common, ADAPTIVE OPTICS, [PHYS]Physics [physics], Multi-Object, GALACTIC ASTRONOMY, Astronomy, Galaxy, NEAR INFRARED, Sky, TELESCOPES, SPECTROGRAPHS, VISIBLE RADIATION, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

When combined with the huge collecting area of the ELT, MOSAIC will be the most effective and flexible Multi-Object Spectrograph (MOS) facility in the world, having both a high multiplex and a multi-Integral Field Unit (Multi-IFU) capability. It will be the fastest way to spectroscopically follow-up the faintest sources, probing the reionisation epoch, as well as evaluating the evolution of the dwarf mass function over most of the age of the Universe. MOSAIC will be world-leading in generating an inventory of both the dark matter (from realistic rotation curves with MOAO fed NIR IFUs) and the cool to warm-hot gas phases in z=3.5 galactic haloes (with visible wavelenth IFUs). Galactic archaeology and the first massive black holes are additional targets for which MOSAIC will also be revolutionary. MOAO and accurate sky subtraction with fibres have now been demonstrated on sky, removing all low Technical Readiness Level (TRL) items from the instrument. A prompt implementation of MOSAIC is feasible, and indeed could increase the robustness and reduce risk on the ELT, since it does not require diffraction limited adaptive optics performance. Science programmes and survey strategies are currently being investigated by the Consortium, which is also hoping to welcome a few new partners in the next two years., 6 pages, 3 figures, Submitted to SPIE Proceedings, AS18

Published
2018
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38. Simulating Surveys for ELT-MOSAIC: Status of the MOSAIC Science Case after Phase A

Author

Puech, M., Evans, C.J., Disseau, K., Japelj, J., Ramírez-Agudelo, O.H., Rahmani, H., Trevisan, M., Wang, J.L., Rodrigues, M., Sánchez-Janssen, R., Yang, Y., Hammer, F., Kaper, L., Morris, S.L., Barbuy, B., Cuby, J.-G., Dalton, G., Fitzsimons, E., Jagourel, P., Simard, L., Takami, H., Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Exploit, 010308 nuclear & particles physics, Computer science, FOS: Physical sciences, Mosaic (geodemography), Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Phase (combat), Conceptual design, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Systems engineering, High definition, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the consolidated scientific case for multi-object spectroscopy with the MOSAIC concept on the European ELT. The cases span the full range of ELT science and require either 'high multiplex' or 'high definition' observations to best exploit the excellent sensitivity and wide field-of-view of the telescope. Following scientific prioritisation by the Science Team during the recent Phase A study of the MOSAIC concept, we highlight four key surveys designed for the instrument using detailed simulations of its scientific performance. We discuss future ways to optimise the conceptual design of MOSAIC in Phase B, and illustrate its competitiveness and unique capabilities by comparison with other facilities that will be available in the 2020s., Comment: Paper presented at SPIE 2018 - Ground-based and Airbone Instrumentation for Astronomy VII

Published
2018
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39. Revisiting the science case for near-UV spectroscopy with the VLT

Author

Evans, C.J., Barbuy, B., Castilho, B., Smiljanic, R., Melendez, J., Japelj, J., Cristiani, S., Snodgrass, C., Bonifacio, P., Puech, M., Quirrenbach, A., Simard, L., Takami, H., High Energy Astrophys. & Astropart. Phys (API, FNWI), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Landessternwarte Königstuhl [ZAH] (LSW), Universität Heidelberg [Heidelberg], School of Physical Sciences [Milton Keynes], Faculty of Science, Technology, Engineering and Mathematics [Milton Keynes], and The Open University [Milton Keynes] (OU)-The Open University [Milton Keynes] (OU)

Subjects
Physics, Very Large Telescope, Current generation, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy, 01 natural sciences, Wavelength, Ultraviolet visible spectroscopy, 0103 physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Visible spectrum
Abstract

In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at far-blue visible wavelengths for the foreseeable future. High-efficiency (>20%) observations of the ground UV (300-400 nm) at medium resolving power (R~20,000) are required to address a number of exciting topics in stellar astrophysics, while also providing new insights in extragalactic science. Anticipating strong demand to better exploit this diagnostic-rich wavelength region, we revisit the science case and instrument requirements previously assembled for the CUBES concept for the Very Large Telescope., 10 pages, in Ground-based & Airborne Instrumentation for Astronomy VII, Proc. SPIE 10702

Published
2018
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40. The key science drivers for MICHI: a thermal-infrared instrument for the TMT

Author

Packham, C., Honda, M., Chun, M., Sakon, I., Richter, M., Okamoto, Y., Kataza, H., Marois, C., Meyer, M., Puravankara, M., Birkby, J., Crossfield, I., Curry, T., Greathouse, T., Herczeg, G., Ichikawa, K., Inami, H., Imanishi, M., Lopez-Rodriguez, E., Evans, C.J., Simard, L., Takami, H., and Low Energy Astrophysics (API, FNWI)

Abstract

With the imminent launch of the JWST, the field of thermal-infrared (TIR) astronomy will enjoy a revolution. It is easy to imagine that all areas of infrared (IR) astronomy will be greatly advanced, but perhaps impossible to conceive of the new vistas that will be opened. To allow both follow-up JWST observations and a continuance of work started on the ground-based 8m’s, we continue to plan the science cases and instrument design for a TIR imager and spectrometer for early operation on the TMT. We present the current status of our science cases and the instrumentation plans, harnessing expertise across the TMT partnership. This instrument will be proposed by the MICHI team as a second-generation instrument in any upcoming calls for proposals.

Published
2018

41. Trade-offs in the visible spectrograph of the ELT instrument MOSAIC

Author

Janssen, A.W., Sokolova, E., Pragt, J., Kragt, J., Navarro, R., Tromp, N., Fitzsimons, E., Rodrigues, M., Larrieu, M., Kelz, A., Morris, T., Jagourel, P., Chemla, F., Kaper, L., Dalton, G., Evans, C.J., Simard, L., Takami, H., and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Diffraction, Computer science, business.industry, Bandwidth (signal processing), Trade offs, 01 natural sciences, 010309 optics, Cardinal point, Optics, 0103 physical sciences, Large core, Spectral resolution, business, 010303 astronomy & astrophysics, Spectrograph, Visible spectrum
Abstract

MOSAIC is a concept for a multi-object spectrograph for the Extremely Large Telescope (ELT). It is planned to cover the wavelength range from 460 nm to 1800 nm with two types of spectrographs, optimized for the visible and the near-infrared. There are two observing modes; multiplex mode with 200 sampling points and Integral Field Unit (IFU) mode with 10 fields. The instrument consists of 5 visible spectrographs and 5 near-infrared spectrographs. The ELT is far from diffraction limited in the visible wavelength range. Rather than developing a large and complex AO system, it was decided that the instrument will be seeing limited in the visible. Spot sizes are therefore about 2.8 mm in diameter in the ELT focal plane, and need to be sampled by multiple fibers with large core diameter. As a result, large optics is required to achieve the science requirements on spectral resolution, bandwidth and multiplex. We work in close collaboration with manufacturers to design an instrument that is feasible and meets the scientific requirements.

Published
2018

42. Abstracts from the NIHR INVOLVE Conference 2017

Author

Muir, D., Vat, L.E., Keller, M., Bell, T., Jørgensen, C.R., Eskildsen, N.B., Johnsen, A.T., Pandya-Wood, R., Blackburn, S., Day, R., Ingram, C., Hapeshi, J., Khan, S., Baird, W., Pavitt, S.H., Boards, R., Briggs, J., Loughhead, E., Patel, M., Khalil, R., Cooper, D., Day, P., Boards, J., Wu, J., Zoltie, T., Barber, S., Thompson, W., Kenny, K., Owen, J., Ramsdale, M., Grey-Borrows, K., Townsend, N., Johnston, J., Maddison, K., Duff-Walker, H., Mahon, K., Craig, L., Collins, R., O’Grady, A., Wadd, S., Kelly, A., Dutton, M., McCann, M., Jones, R., Mathie, E., Wythe, H., Munday, D., Millac, P., Rhodes, G., Roberts, N., Simpson, J., Barden, N., Vicary, P., Wellings, A., Poland, F., Jones, J., Miah, J., Bamforth, H., Charalambous, A., Dawes, P., Edwards, S., Leroi, I., Manera, V., Parsons, S., Sayers, R., Pinfold, V., Dawson, P., Gibbons, B., Gibson, J., Hobson-Merrett, C., McCabe, C., Rawcliffe, T., Frith, L., Gudgin, B., Wellings, A.., Horobin, A., Ewart, C., Higton, F., Vanhegan, S., Stewart, J., Wragg, A., Wray, P., Widdowson, K., Brighton, L.J., Pask, S., Benalia, H., Bailey, S., Sumerfield, M., Etkind, S., Murtagh, F.E.M., Koffman, J., Evans, C.J., Hrisos, S., Marshall, J., Yarde, L., Riley, B., Whitlock, P., Jobson, J., Ahmed, S., Rankin, J., Michie, L., Scott, J., Barker, C.R., Barlow-Pay, M., Kekere-Ekun, A., Mazumder, A., Nishat, A., Petley, R., Brady, L-M.., Templeton, L., Walker, E., Moore, D., Shaw, L., Nunns, M., Thompson Coon, J., Blomquist, P., Cochrane, S., Edelman, N., Calliste, J., Cassell, J., Mader, L.B., Kläger, S., Wilkinson, I.B., Hiemstra, T.F., Hughes, M., Warren, A., Atkins, P., Eaton, H., Keenan, J., Rhodes, C., Skrybrant, M., Chatwin, L., Darby, M-A., Entwistle, A., Hull, D., Quann, N., Hickey, G., Dziedzic, K., Eltringham, S.A., Gordon, J., Franklin, S., Jackson, J., Leggett, N., Davies, P., Nugawela, M., Scott, L., Leach, V., Richards, A., Blacker, A.., Abrams, P., Sharma, J., Donovan, J.., Whiting, P., Stones, S.R., Wright, C., Boddy, K., Irvine, J., Harris, J., Joseph, N., Kok, M., Gibson, A., Evans, D., Grier, S., MacGowan, A., Matthews, R., Papoulias, C., Augustine, C., Hoffman, M., Doughty, M., Surridge, H., Tembo, D., Roberts, A., Chambers, E., Beever, D., Wildman, M., Davies, R.L., Staniszewska, S., Stephens, R., Schroter, S., Price, A., Richards, T., Demaine, A., Harmston, R., Elliot, J., Flemyng, E., Sproson, L., Pryde, L., Reed, H., Squire, G, Stanton, A.., Langley, J., Briggs, M., Brindle, P., Sanders, R., McDermott, C., Coyle, D., Heron, N., Davies, S., Wilkie, M., Coldham, T., Ballinger, C., Kerridge, L., Mullee, M., Eyles, C., Johns, T., Paylor, J., Turner, K., Whiting, L., Roberts, S., Petty, J., Meager, G., Grinbergs-Saull, A., Morgan, N., Collins, F., Gibson, S., Passmore, S., Evans, L., Green, S.A., Trite, J., Thomson, R., Green, D., Atkinson, H., Mitchell, A., Corner, L., McKenzie AM, A., Nguyen, R, Frank, B., McNeil, N., and Harrison, H.

Subjects
lcsh:R5-920, lcsh:R, lcsh:Medicine, lcsh:Medicine (General), Meeting Abstracts
Published
2017

43. The VLT-FLAMES Tarantula Survey

Author

Garland, R., Dufton, P.L., Evans, C.J., Crowther, P.A., Howarth, I.D., de Koter, A., de Mink, S.E., Grin, N.J., Langer, N., Lennon, D.J., McEvoy, C.M., Sana, H., Schneider, F.R.N., Símon Díaz, S., Taylor, W.D., Thompson, A., and Vink, J.S.

Abstract

A spectroscopic analysis has been undertaken for the B-type multiple systems (excluding those with supergiant primaries) in the VLT-FLAMES Tarantula Survey (VFTS). Projected rotational velocities, vesini, for the primaries have been estimated using a Fourier Transform technique and confirmed by fitting rotationally broadened profiles. A subset of 33 systems with vesini ≤ 80 km s-1 have been analysed using a TLUSTY grid of model atmospheres to estimate stellar parameters and surface abundances for the primaries. The effects of a potential flux contribution from an unseen secondary have also been considered. For 20 targets it was possible to reliably estimate their effective temperatures (Teff) but for the other 13 objects it was only possible to provide a constraint of 20 000 ≤ Teff ≤ 26 000 K – the other parameters estimated for these targets will be consequently less reliable. The estimated stellar properties are compared with evolutionary models and are generally consistent with their membership of 30 Doradus, while the nature of the secondaries of 3 SB2 system is discussed. A comparison with a sample of single stars with vesini ≤ 80 km s-1 obtained from the VFTS and analysed with the same techniques implies that the atmospheric parameters and nitrogen abundances of the two samples are similar. However, the binary sample may have a lack of primaries with significant nitrogen enhancements, which would be consistent with them having low rotational velocities and having effectively evolved as single stars without significant rotational mixing. This result, which may be actually a consequence of the limitations of the pathfinder investigation presented in this paper, should be considered as a motivation for spectroscopic abundance analysis of large samples of binary stars, with high quality observational data.

Published
2017

46. Response to Comment on 'An excess of massive stars in the local 30 Doradus starburst'

Author

Schneider, F.R.N., Sana, H., Evans, C.J., Bestenlehner, J.M., Castro, N., Fossati, L., Grafener, G., Langer, N., Ramirez-Agudelo, O.H., Sabin-Sanjulian, C., Simon-Diaz, S., Tramper, F., Crowther, P.A., Koter, A. de, Mink, S.E. de, Dufton, P.L., Garcia, M., Gieles, M., Henault-Brunet, V., Herrero, A., Izzard, R.G., Kalari, V., Lennon, D.J., Apellaniz, J.M., Markova, N., Najarro, F., Podsiadlowski, P., Puls, J., Taylor, W.D., Loon, J.T. van, Vink, J.S., Norman, C., Schneider, F.R.N., Sana, H., Evans, C.J., Bestenlehner, J.M., Castro, N., Fossati, L., Grafener, G., Langer, N., Ramirez-Agudelo, O.H., Sabin-Sanjulian, C., Simon-Diaz, S., Tramper, F., Crowther, P.A., Koter, A. de, Mink, S.E. de, Dufton, P.L., Garcia, M., Gieles, M., Henault-Brunet, V., Herrero, A., Izzard, R.G., Kalari, V., Lennon, D.J., Apellaniz, J.M., Markova, N., Najarro, F., Podsiadlowski, P., Puls, J., Taylor, W.D., Loon, J.T. van, Vink, J.S., and Norman, C.

Abstract

Contains fulltext : 195471.pdf (publisher's version ) (Closed access)

Published
2018

47. An excess of massive stars in the local 30 Doradus starburst

Author

Schneider, F.R.N., Sana, H., Evans, C.J., Bestenlehner, J.M., Castro, N., Fossati, L., Henault-Brunet, V., Vink, J.S., Norman, C., Schneider, F.R.N., Sana, H., Evans, C.J., Bestenlehner, J.M., Castro, N., Fossati, L., Henault-Brunet, V., Vink, J.S., and Norman, C.

Abstract

Contains fulltext : 181982.pdf (preprint version ) (Closed access)

Published
2018

50. The E-ELT multi-object spectrograph: latest news from MOSAIC

Author

Hammer, F., Morris, S., Kaper, L., Barbuy, B., Cuby, J.G., Roth, M., Jagourel, P., Evans, C.J., Puech, M., Fitzsimons, E., Dalton, G., Rodrigues, M., Simard, L., Takami, H., Low Energy Astrophysics (API, FNWI), High Energy Astrophys. & Astropart. Phys (API, FNWI), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Pôle instrumental, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Duke University [Durham], Amsterdam, Departamento de Astronomia, Universidade de São Paulo, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Leibniz-Institut für Astrophysik Potsdam (IAP), UK Astronomy Technology Centre, Royal Observatory Edinburgh (UKATC), and Univ. of Oxford (United Kingdom)

Subjects
Physics, Galactic astronomy, 010308 nuclear & particles physics, Milky Way, James Webb Space Telescope, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Exoplanet, Galaxy, law.invention, Telescope, law, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Spectrograph, Reionization, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics
Abstract

There are 8000 galaxies, including 1600 at z larger than 1.6, which could be simultaneously observed in an E-ELT field of view of 40 sq. arcmin. A considerable fraction of astrophysical discoveries require large statistical samples, which can only be obtained with multi-object spectrographs (MOS). MOSAIC will provide a vast discovery space, enabled by a multiplex of 200 and spectral resolving powers of R=5000 and 20000. MOSAIC will also offer the unique capability of more than 10 "high-definition" (multi-object adaptive optics, MOAO) integral-field units, optimised to investigate the physics of the sources of reionization. The combination of these modes will make MOSAIC the world-leading MOS facility, contributing to all fields of contemporary astronomy, from extra-solar planets, to the study of the halo of the Milky Way and its satellites, and from resolved stellar populations in nearby galaxies out to observations of the earliest "first-light" structures in the Universe. It will also study the distribution of the dark and ordinary matter at all scales and epochs of the Universe. Recent studies of critical technical issues such as sky-background subtraction and MOAO have demonstrated that such a MOS is feasible with state-of-the-art technology and techniques. Current studies of the MOSAIC team include further trade-offs on the wavelength coverage, a solution for compensating for the non-telecentric new design of the telescope, and tests of the saturation of skylines especially in the near-IR bands. In the 2020s the E-ELT will become the world's largest optical/IR telescope, and we argue that it has to be equipped as soon as possible with a MOS to provide the most efficient, and likely the best way to follow-up on James Webb Space Telescope (JWST) observations., Comment: 10 pages, 3 Figures, in Ground-based and Airborne Instrumentation for Astronomy VI, 2016, Proc. SPIE

Published
2016
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