SkyHopper is a proposed CubeSat mission to simultaneously observe 4 bands in the wavelength range from 0.8 to 1.7 micron. The light is captured by a telescope with a 100 mm × 200 mm primary and a field of view of 0.6° × 2.6°. A preliminary definition (phase B) of the optical telescope assembly for the mission is now completed. It is designed to make high precision intensity measurements of every object in the field of view. This brought a series of constraints to avoid stray light. Different optical designs were studied. A Kösters prism is used to split the light into 4 bands on a 2k x 2k detector. The telescope design is based on a 3 mirror anastigmat with additional lenses to provide good image quality in the final focal plane for all bands and also in the intermediate focal plane and the pupil plane where cold stops are needed. Aberrations and vignetting of the prism had to be removed. Science applications include exoplanet transits in front of low-mass stars, rapid Infrared follow-up of Gamma Ray Bursts and exploring the Cosmic Infrared Background.
M. Feroci, E. Bozzo, S. Brandt, M. Hernanz, M. van der Klis, L.-P. Liu, P. Orleanski, M. Pohl, A. Santangelo, S. Schanne, L. Stella, T. Takahashi, H. Tamura, A. Watts, J. Wilms, S. Zane, S.-N. Zhang, S. Bhattacharyya, I. Agudo, M. Ahangarianabhari, C. Albertus, M. Alford, A. Alpar, D. Altamirano, L. Alvarez, L. Amati, C. Amoros, N. Andersson, A. Antonelli, A. Argan, R. Artigue, B. Artigues, J.-L. Atteia, P. Azzarello, P. Bakala, D. Ballantyne, G. Baldazzi, M. Baldo, S. Balman, M. Barbera, C. van Baren, D. Barret, A. Baykal, M. Begelman, E. Behar, O. Behar, T. Belloni, F. Bernardini, G. Bertuccio, S. Bianchi, A. Bianchini, P. Binko, P. Blay, F. Bocchino, M. Bode, P. Bodin, I. Bombaci, J.-M. Bonnet Bidaud, S. Boutloukos, F. Bouyjou, L. Bradley, J. Braga, M. Briggs, E. Brown, M. Buballa, N. Bucciantini, L. Burderi, M. Burgay, M. Bursa, C. Budtz-Jørgensen, E. Cackett, F. Cadoux, P. Cais, G. Caliandro, R. Campana, S. Campana, X. Cao, F. Capitanio, J. Casares, P. Casella, A. Castro-Tirado, E. Cavazzuti, Y. Cavechi, S. Celestin, P. Cerda-Duran, D. Chakrabarty, N. Chamel, F. Château, C. Chen, Y. Chen, J. Chenevez, M. Chernyakova, J. Coker, R. Cole, A. Collura, M. Coriat, R. Cornelisse, L. Costamante, A. Cros, W. Cui, A. Cumming, G. Cusumano, B. Czerny, A. D'Aì, F. D'Ammando, V. D'Elia, Z. Dai, E. Del Monte, A. De Luca, D. De Martino, J. P. C. Dercksen, M. De Pasquale, A. De Rosa, M. Del Santo, S. Di Cosimo, N. Degenaar, J. W. den Herder, S. Diebold, T. Di Salvo, Y. Dong, I. Donnarumma, V. Doroshenko, G. Doyle, S. Drake, M. Durant, D. Emmanoulopoulos, T. Enoto, M. H. Erkut, P. Esposito, Y. Evangelista, A. Fabian, M. Falanga, Y. Favre, C. Feldman, R. Fender, H. Feng, V. Ferrari, C. Ferrigno, M. Finger, G. Fraser, M. Frericks, M. Fullekrug, F. Fuschino, M. Gabler, D. K. Galloway, J. L. Gálvez Sanchez, P. Gandhi, Z. Gao, E. Garcia-Berro, B. Gendre, O. Gevin, S. Gezari, A. B. Giles, M. Gilfanov, P. Giommi, G. Giovannini, M. Giroletti, E. Gogus, A. Goldwurm, K. Goluchová, D. Götz, L. Gou, C. Gouiffes, P. Grandi, M. Grassi, J. Greiner, V. Grinberg, P. Groot, M. Gschwender, L. Gualtieri, M. Guedel, C. Guidorzi, L. Guy, D. Haas, P. Haensel, M. Hailey, K. Hamuguchi, F. Hansen, D. Hartmann, C. A. Haswell, K. Hebeler, A. Heger, M. Hempel, W. Hermsen, J. Homan, A. Hornstrup, R. Hudec, J. Huovelin, D. Huppenkothen, S. Inam, A. Ingram, J. In't Zand, G. Israel, K. Iwasawa, L. Izzo, H. Jacobs, F. Jetter, T. Johannsen, P. Jenke, P. Jonker, J. Josè, P. Kaaret, K. Kalamkar, E. Kalemci, G. Kanbach, V. Karas, D. Karelin, D. Kataria, L. Keek, T. Kennedy, D. Klochkov, W. Kluzniak, E. Koerding, K. Kokkotas, S. Komossa, S. Korpela, C. Kouveliotou, A. Kowalski, I. Kreykenbohm, L. Kuiper, D. Kunneriath, A. Kurkela, I. Kuvvetli, F. La Franca, C. Labanti, D. Lai, F. Lamb, C. Lachaud, P. Laubert, F. Lebrun, X. Li, E. Liang, O. Limousin, D. Lin, M. Linares, D. Linder, G. Lodato, F. Longo, F. Lu, N. Lund, T. Maccarone, D. Macera, S. Maestre, S. Mahmoodifar, D. Maier, P. Malcovati, J. Malzac, C. Malone, I. Mandel, V. Mangano, A. Manousakis, M. Marelli, J. Margueron, M. Marisaldi, S. Markoff, A. Markowitz, A. Marinucci, A. Martindale, G. Martínez, I. McHardy, G. Medina-Tanco, M. Mehdipour, A. Melatos, M. Mendez, S. Mereghetti, S. Migliari, R. Mignani, M. Michalska, T. Mihara, M. C. Miller, J. M. Miller, T. Mineo, G. Miniutti, S. Morsink, C. Motch, S. Motta, M. Mouchet, G. Mouret, J. Mulačová, F. Muleri, T. Muñoz-Darias, I. Negueruela, J. Neilsen, T. Neubert, A. Norton, M. Nowak, A. Nucita, P. O'Brien, M. Oertel, P. E. H. Olsen, M. Orienti, M. Orio, M. Orlandini, J. Osborne, R. Osten, F. Ozel, L. Pacciani, F. Paerels, S. Paltani, M. Paolillo, I. Papadakis, A. Papitto, Z. Paragi, J. Paredes, A. Patruno, B. Paul, F. Pederiva, E. Perinati, A. Pellizzoni, A. V. Penacchioni, U. Peretz, M. Perez, M. Perez-Torres, B. Peterson, V. Petracek, C. Pittori, J. Pons, J. Portell, A. Possenti, K. Postnov, J. Poutanen, M. Prakash, I. Prandoni, H. Le Provost, D. Psaltis, J. Pye, J. Qu, D. Rambaud, P. Ramon, G. Ramsay, M. Rapisarda, A. Rashevski, I. Rashevskaya, P. Ray, N. Rea, S. Reddy, P. Reig, M. Reina Aranda, R. Remillard, C. Reynolds, L. Rezzolla, M. Ribo, R. de la Rie, A. Riggio, A. Rios, D. Rischke, P. Rodríguez-Gil, J. Rodriguez, R. Rohlfs, P. Romano, E. M. Rossi, A. Rozanska, A. Rousseau, B. Rudak, D. Russell, F. Ryde, L. Sabau-Graziati, T. Sakamoto, G. Sala, R. Salvaterra, D. Salvetti, A. Sanna, J. Sandberg, T. Savolainen, S. Scaringi, J. Schaffner-Bielich, H. Schatz, J. Schee, C. Schmid, M. Serino, N. Shakura, S. Shore, J. Schnittman, R. Schneider, A. Schwenk, A. Schwope, A. Sedrakian, J.-Y. Seyler, A. Shearer, A. Slowikowska, M. Sims, A. Smith, D. Smith, P. Smith, M. Sobolewska, V. Sochora, P. Soffitta, P. Soleri, L. Song, A. Spencer, A. Stamerra, B. Stappers, R. Staubert, A. Steiner, N. Stergioulas, A. Stevens, G. Stratta, T. Strohmayer, Z. Stuchlik, S. Suchy, V. Suleimanov, F. Tamburini, T. Tauris, F. Tavecchio, C. Tenzer, F. Thielemann, A. Tiengo, L. Tolos, F. Tombesi, J. Tomsick, G. Torok, J. M. Torrejon, D. F. Torres, E. Torresi, A. Tramacere, I. Traulsen, A. Trois, R. Turolla, S. Turriziani, S. Typel, P. Uter, P. Uttley, A. Vacchi, P. Varniere, S. Vaughan, S. Vercellone, M. Vietri, F. Vincent, V. Vrba, D. Walton, J. Wang, Z. Wang, S. Watanabe, R. Wawrzaszek, N. Webb, N. Weinberg, H. Wende, P. Wheatley, R. Wijers, R. Wijnands, M. Wille, C. Wilson-Hodge, B. Winter, S. Walk, K. Wood, S. Woosley, X. Wu, R. Xu, W. Yu, F. Yuan, W. Yuan, Y. Yuan, G. Zampa, N. Zampa, L. Zampieri, L. Zdunik, A. Zdziarski, A. Zech, B. Zhang, C. Zhang, S. Zhang, M. Zingale, F. Zwart
The Large Observatory For x-ray Timing (LOFT) is a mission concept which was proposed to ESA as M3 and M4 candidate in the framework of the Cosmic Vision 2015-2025 program. Thanks to the unprecedented combination of effective area and spectral resolution of its main instrument and the uniquely large field of view of its wide field monitor, LOFT will be able to study the behaviour of matter in extreme conditions such as the strong gravitational field in the innermost regions close to black holes and neutron stars and the supra-nuclear densities in the interiors of neutron stars. The science payload is based on a Large Area Detector (LAD, >8m2 effective area, 2-30 keV, 240 eV spectral resolution, 1 degree collimated field of view) and a Wide Field Monitor (WFM, 2-50 keV, 4 steradian field of view, 1 arcmin source location accuracy, 300 eV spectral resolution). The WFM is equipped with an on-board system for bright events (e.g., GRB) localization. The trigger time and position of these events are broadcast to the ground within 30 s from discovery. In this paper we present the current technical and programmatic status of the mission.
Polarimeters for Energetic Transients (POET) is a mission concept designed to t within the envelope of a NASA Small Explorer (SMEX) mission. POET will use X-ray and gamma-ray polarimetry to uncover the energy release mechanism associated with the formation of stellar-mass black holes and investigate the physics of extreme magnetic ields in the vicinity of compact objects. Two wide-FoV, non-imaging polarimeters will provide polarization measurements over the broad energy range from about 2 keV up to about 500 keV. A Compton scatter polarimeter, using an array of independent scintillation detector elements, will be used to collect data from 50 keV up to 500 keV. At low energies (2{15 keV), data will be provided by a photoelectric polarimeter based on the use of a Time Projection Chamber for photoelectron tracking. During a two-year baseline mission, POET will be able to collect data that will allow us to distinguish between three basic models for the inner jet of gamma-ray bursts.
We present the Microchannel X-ray Telescope, a new light and compact focussing telescope that will be ying on the Sino-French SVOM mission dedicated to Gamma-Ray Burst science. The MXT design is based on the coupling of square pore micro-channel plates with a low noise pnCCD. MXT will provide an effective area of about 50 cm2, and its point spread function is expected to be better than 3.7 arc min (FWHM) on axis. The estimated sensitivity is adequate to detect all the afterglows of the SVOM GRBs, and to localize them to better then 60 arc sec after five minutes of observation.
Gamma-Ray Imaging, Polarimetry and Spectroscopy (GRIPS) is a proposed space mission for gamma-ray astrophysics. It will be capable of imaging gamma-rays via Compton scattering and pair production in the energy range from ~200 keV up to ~50MeV. GRIPS will address fundamental astrophysical questions through observations of energetic gamma-ray phenomena such as gamma-ray bursts, blazars and supernovae in this unique energy window. The Medium-Energy Gamma-ray Astronomy library (MEGAlib) is an open-source object-oriented software library designed to simulate and analyse data from low-to-medium-energy gamma-ray telescopes, especially Compton telescopes such as GRIPS. The library comprises all necessary data analysis steps from initial simulations through to event reconstruction and image reconstruction. Simulations are being carried out to optimize the sensitivity of GRIPS to gamma-ray sources using MEGAlib and the results are presented here. GRIPS will offer an improvement in sensitivity in its operational energy range by a factor of ~40 compared with previous missions.
The astronomical instrument GROND (Gamma-Ray Burst Optical and Near-Infrared Detector), mounted on the 2.2m
MPI/ESO telescope in La Silla (Chile) is an imaging system covering seven wavelength bands from the visual to the
NIR spectral range (380-2400 nm). The instrument consists of more than 30 optical elements allowing the simultaneous
observation of four wavelength bands in the visible spectral range (g, r, I, z) and three bands (J, K, H) in the near
infrared. The deposition of high quality optical coatings on the optical elements of the system is one of the major
challenges for the implementation of GROND. In order to tailor the instrument performance with respect to the required
sensitivity parameters, a set of broad band anti reflection coatings and dichroic filter coatings on quartz, YAG and
different fluoride compound lenses had to be optimized. The performance and deposition control of the optical coatings
on plane and curved surfaces was evaluated with the aid of witness samples, which were deposited together with the real
substrate. The global optical performance of the instrument can be determined combining the single components
properties or by an overall measurement of the finalised instrument. In this contribution, a comparison of the measured
performance and the operation characteristics predicted from the properties of the single elements is presented.
The next large NASA mission in the field of gamma-ray astronomy, GLAST, is scheduled for launch in 2007. Aside from the main instrument LAT (Large-Area Telescope), a gamma-ray telescope for the energy range between 20 MeV and > 100GeV, a secondary instrument, the GLAST burst monitor (GBM), is foreseen. With this monitor one of
the key scientific objectives of the mission, the determination of the high-energy behaviour of gamma-ray bursts and transients can be ensured. Its task is to increase the detection rate of gamma-ray bursts for the LAT and to extend the energy range to lower energies (from ~10 keV to ~30 MeV). It will provide real-time burst locations over a wide FoV with sufficient accuracy to allow repointing the GLAST spacecraft. Time-resolved spectra of many bursts recorded with LAT and the burst monitor will allow the investigation of the relation between the keV and the MeV-GeV emission from GRBs over unprecedented seven decades of energy. This will help to advance our understanding of the mechanisms by which gamma-rays are generated in gamma-ray bursts
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