PoS(MULTIF2017)083 https://pos.sissa.it/ ∗ 2 , 1 Speaker. The recent progress in picosatellitesbased on technology, miniaturized scientific allows payload. to We suggest consider possiblewith astrophysical their emphasis payloads on for use high–energy cubesats for and UV astrophysics, astrophysics. ∗ Copyright owned by the author(s) under the terms of the Creative Commons Czech Technical University in Prague, Faculty of Electrical Engineering, Engelhardt Astronomical observatory, Kazan Federal University, Kremlyovskaya street 18, c Attribution-NonCommercial-NoDerivatives 4.0 International License (CC BY-NC-ND 4.0). XII Multifrequency Behaviour of High Energy12-17 Cosmic June, Sources 2017 Workshop Palermo, Italy 1 Technická 2, 16000 Prague, Czech2 Republic 420008 Kazan, Russia [email protected] René Hudec Multifrequency astrophysics with very small satellites PoS(MULTIF2017)083 2 , × 1 10 × René Hudec 1 10 cm or less (3U, i.e. 3 cubesat modules), they must be of low weight, typically × 10 30 cm, typically up to 12U. × × BRITE X 8U CubeSat (left) and Small scientific 16U satellite BRITE CZ with combined payload 10 × The Lobster Eye (LE) X-ray optics was originally proposed by Schmidt (1975) and Angel The recent situation in experimental satellite astronomy and astrophysics is affected by funding On the other hand, in the recent years, there was essential improvement in cubesats technology, The pico and nanosatellites are recently in development at many universities, mostly with In this paper, we briefly discuss few ideas for application of pico and cubesatellites in high- (1979). Since then, numerous test(e.g. specimens Inneman of et Lobster al. Eye 1999; telescopesEye Hudec were (LE) et designed X-ray al. and telescope tested 2000,scopes can 2003, are 2004; be novel Tichý miniaturized wide et field for al. X-ray an telescopes 2009, with application 2011). the in The field picosatellites. of Lobster- view (FOV) The of 100 LE sq. tele- deg. They are 3. Payload example 1: Miniature X-ray monitor Figure 1: UV-BRITE and X-BRITE (right) problems. For example, there isseveral very dozens large proposals competition for for one ESA call M delivered. and L missions, with typically allowing scientific payloads forin cubesats development to at be many considered. institutesfast and The development universities, miniature of mostly satellites the with are relatedpayloads a for recently techniques these participation and satellites. of technologies students. enables to The consider smallinvolvement scientific of students and education. The CubeSat standard size is 1 Liter Volume, i.e. 10 energy and space astronomy and astrophysics. Westrict note that requirements these for payloads the must meet scientific thetypically payload following 30 for picosatellites. They must fit into a small volume, Picosats 1. Introduction 10 cm, and a typical weighti.e. is 1.3 10 kg, but multiple modules are possible, i.e. 3U = 3 modules/units, 2. Scientific payload for pico and nanosatellite less than 1 kg, with low power consumption of about 10 Watts or less. PoS(MULTIF2017)083 2 , 1 René Hudec 10 cm), a special coating × 2 The VZLUSAT1 2U cubesatellite (left) and the 1D LE optics module onboard (right), Urban et The 1st LE X–ray monitor was launched into Earth orbit in June 23, 2017, onboard small The LE payload for picosatellites also requires miniaturized focal detectors. The best available However, the following items are important: 1. The detector is not yet space qualified; 2.However, a Its more suitable spacecraft is a 6U CubeSat as it allows to accommodate several LE Czech 2U cubesatellite VZLUSAT1 (Figs. 1small and X–ray 2, experiment Urban is et based al. onrecord 2017a, 1D the 2017b, LE focal Daniel X–ray images. 2016). optics The module The future main and larger goal on experiments is based Timepix the on detector technology analogous usedintensities demonstration hardware. to and in The also orbit, 1D harder LE X-rays with (5 is potential – more of slit), 20 suitable keV). so for Optics low that above 35 X-ray the keV behaves gain asTimepix is a can collimator only (Soller be 1. used Maximum also energy for is measurement limited of by the spectrum Timepix of detector astrophysical (3-50 objects. keV). The designed Figure 2: al. 2017a, 2017b, Daniel et al., 2016. to increase the reflectivity atkept higher at energies, 250 a mm. better manufacturing technology, the focal length option for the author team ofphoton counting this pixel paper detectors is developed the by detector anCTU international in Medipix Prague collaboration, (Timepix). is hosted a Medipix by member is CERN. of The adetector this cooperation. family for The of a Medipix use detector in represents space a suitable LE imaging telescopes. spectral coverage starts only in energiesin above the 3 Schmidt keV, arrangement while is the typically spectral from coverage the of visible the light LE up optics tomodules the to energies of increase 8 the orprototype final 10 as keV. FOV follows. (Tichý More et mirrors: al. 333 per set, 2013a). a larger We input elaborated area (10 a design of a new SLE Picosats more easily possible (a classical X-raya optics real analogy has with the the FOV lobster of eyes. only 1 deg or less) and are based on PoS(MULTIF2017)083 2 , 1 René Hudec 3 m in size. The objective prism and/or grating should be µ m x 11.53 µ Wide field X–ray monitors of Lobster Eye type were demonstrated to play an important role The LE telescopes can typically serve in two basic operation modes as follows. (i) Starrying Also UV telescopes can be miniaturized for cubesat applications. For example, for the pro- For Gemini UV experiments, the used UV lens had aperture 22 mm, f =73 mm, f/3.3, and FOV The Skylab UV experiment was larger, based f/3 Ritchey-Chretien telescope with aperture 15 The scientific objective of the proposed cubesat UV experiment is analogous to he historical The possible platform for the UV experiment is 3U to 8U cubesat with deploy-able mecha- included for spectroscopy. in modern astrophysics (e.g. Hudeccases et are al. briefly 2007; summarized Švéda below. etbright (i) al. persistent A 2004). long-term X-ray (months) The binaries measurement most inband. of important the (ii) scientific the direction Detection light and toward curves measurement the of of center thein light the of curves direction the of toward bright Galaxy the transient in events center of the of X-ray the soft binaries Galaxy X-ray in3.2 the soft Modes X-ray of band. Operation (pointed) mode – onlyand/or for stabilization satellite required). with We pointing, notefor and pointed that observations. (ii) many cubesats Scanning do mode not (no have satellite any pointing stabilization suitable 4. Example 2: Miniature UV experiment posed BRITE UV cubesat, thenificantly payload upgraded is camera based system on which the wasSkylab miniature used UV UV by experiments spectrographic led NASA in by camera, Prof. Gemini sig- (Henize Karl et G. al., Henize 1968) (Figs. and 330 and degrees, 4). with working range 2300lines/mm – as 5000 well as A. prism Grating 1400 wasGemini A/mm used X, at with XI 2500 184 and A. XII A/mm Gemini experiments at XI, used(outside 2000 XII a spacecraft). A, experiments grating, used 600 all a these prism, experiments were while operated during EVA cm and FOV of 4x5 deg, equippedand with 2800 prism with A, dispersion and of spectral 64, resolution 365 of and 2, 1281 A 12, at and 1400, 41 2000, UV A. experiments on Gemini (Morganobtain et line al., spectra 1975) in and the Skylab wavelengthUV (Ocalaghan 2200 camera et to with 4000 al. a A UV 1978), lens of with namely stars.diameter a (preliminary to The 30 values). system mm CMOS aperture, will or 100 be cooled mm representedthe CCD focal by focal length detector a and will plane. a be As field used of an as 30Angstroms alternative, an degrees per an image in mm objective detector grating at in will 2000 A. beof In used 1400 addition, to Angstroms the produce per quartz a mm objective dispersion at prism of 2500 which 180 A produces is a considered dispersion tonisms be to used. extend length and UVeg lens e2V1 or CIS101–00–M05 folded reflector chip, with can1430 aperture serve (V) 3 as to pixels possible 10 each focal cm. 14.81 detector. sCMOS detector, This device has 1415 (H) x Picosats FOV is 3 x 3 deg. 3.1 Science objectives PoS(MULTIF2017)083 2 , 1 René Hudec 4 This work was supported by the grant GA CR 13-33324S. New scans performed in 2016 from original Skylab UV expriment films. Figure 3: The proposed mission (miniature LE X-ray telescope/monitor in a picosatellite) can acquire We also note additional, more advanced science potential of using network of identical Cube- Acknowledgments If compared with the Skylab UV experiment, the main difference is that the recording medium scientifically important data for ascientific low justification price. is The strong, optics including several forprototype perspective the areas of presented of the mission modern optics astrophysics. is (based A feasible.and new on tested. The the Also for optimized UV design astrophysics, forcould miniature be UV a telescope/spectrograph considered picosatellite) for as was cubesat well. application already developed Sats for particular scientific tasks.missions. This is potential area where CubeSats can compete with larger will be CMOS insteadmagnitude of limit film, was 9 hence mag with lim essential mag, compared increase to in BRITE UV sensitivity estimated (e.g. limit of5. for 12 mag). Skylab, Conclusions the Picosats PoS(MULTIF2017)083 2 , 1 René Hudec 5 Prof. K. Henize Gemini UV experiment (left) and the photographic plate archive with these data S019, Applied Optics, Volume 16, id.973 (1977) 11 of stars in Orion, The Astrophysical Journal, Volume 197, id.371 (1975) with miniature lobster eye X-ray telescopespace and application, qualification Acta of Astronautica, the Volume 140, radiation id.96 shielding (2017) composite for in Exploring the Cosmic Frontier, ESOpp.73-74, Astrophysics 2007 Symposia European Southern Observatory 2007, 2004); doi: 10.1117/12.551915, 2004 and XII manned space flights., Bulletinid.279 of (1968) the Astronomical Institutes of Czechoslovakia, Volume 19, [4] Angel, J. R. P., 1979, Astroph.[5] J., 364,Inneman, 233 A., et al., 2000, Proc.[6] SPIE, 4138,Hudec, 94 R., et al., 2000, SPIE[7] Proc. 4012,Hudec, 432 R., et al., 2003, SPIE[8] Proc. 4851,Hudec, 578 R., et al., 2004a, SPIE[9] Proc. 5488,Hudec, 449 R., et al., 2004b, Nucl. Phys. B Proc. Suppl. 132, 320 [3] Hudec, R., Pína, L., Inneman, A., Švéda, L., LOBSTER - Astrophysics with Lobster Eye Telescopes, [2] Hudec, R., et al., Proc. SPIE 5488, UV and Gamma-Ray Space Telescope Systems, (11 October [1] Henize, K. G., J. D. Wray, and L. R. Wackerling: Ultraviolet objective-prism spectra from Gemini XI [10] Ocalaghan, F. G., K. G. Henize, and J. D. Wray: SKYLAB[11] ultraviolet stellarMorgan, astronomy T. experiment H., G. G. Spear, Y. Kondo, and K. G. Henize:[12] Ultraviolet spectrophotometryUrban, from M., Gemini O. Nentvich, V. Stehlikova, T. Baca, V. Daniel, and R. Hudec: VZLUSAT-1: Nanosatellite References Figure 4: (right). Picosats PoS(MULTIF2017)083 2 , 1 René Hudec 6 processing from two 1D modules, ContributionsVolume 47, of id.178 the (2017) Astronomical Observatory Skalnate Pleso, Timepix, Contributions of the Astronomical Observatory Skalnate Pleso, Volume 47, id.151 (2017) type optics, Society of Photo-Optical Instrumentation10235, Engineers id.102350N (SPIE) (2017) Conference Series, Volume CubeSat, CubeSats and NanoSats for Remote Sensing, Volume 9978, id.99780D (2016) and Electronic Systems Magazine 21 (2006), S. 9-14, 2006 Pico-Satellite UWE-2. In: Space Technology 28. 2009, pp.67-74, 2009 Picosats [13] Nentvich, O., M. Urban, V. Stehlikova, L. Sieger, and R. Hudec: Lobster eye X-ray optics: Data [14] Urban, M., O. Nentvich, V. Stehlikova, and L. Sieger: Detection of X-ray[15] spectra andNentvich, images O., by V. Stehlikova, M. Urban, R. Hudec, and L. Sieger: Data processing from lobster eye [16] Daniel, V., L. Pina, A. 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