Thermal Systems Brochure
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www.arianespace.com www.starsem.com www.avio Arianespace’s eighth launch of 2021 with the fifth Soyuz of the year will place its satellite passengers into low Earth orbit. The launcher will be carrying a total payload of approximately 5 518 kg. The launch will be performed from Baikonur, in Kazakhstan. MISSION DESCRIPTION 2 ONEWEB SATELLITES 3 Liftoff is planned on at exactly: SOYUZ LAUNCHER 4 06:23 p.m. Washington, D.C. time, 10:23 p.m. Universal time (UTC), LAUNCH CAMPAIGN 4 00:23 a.m. Paris time, FLIGHT SEQUENCES 5 01:23 a.m. Moscow time, 03:23 a.m. Baikonur Cosmodrome. STAKEHOLDERS OF A LAUNCH 6 The nominal duration of the mission (from liftoff to separation of the satellites) is: 3 hours and 45 minutes. Satellites: OneWeb satellite #255 to #288 Customer: OneWeb • Altitude at separation: 450 km Cyrielle BOUJU • Inclination: 84.7degrees [email protected] +33 (0)6 32 65 97 48 RUAG Space AB (Linköping, Sweden) is the prime contractor in charge of development and production of the dispenser system used on Flight ST34. It will carry the satellites during their flight to low Earth orbit and then release them into space. The dedicated dispenser is designed to Flight ST34, the 29th commercial mission from the Baikonur Cosmodrome in Kazakhstan performed by accommodate up to 36 spacecraft per launch, allowing Arianespace and its Starsem affiliate, will put 34 of OneWeb’s satellites bringing the total fleet to 288 satellites Arianespace to timely deliver the lion’s share of the initial into a near-polar orbit at an altitude of 450 kilometers. -
GEORIX Single-Frequency Multi - Constellation GNSS Receiver
GEORIX Single-Frequency Multi - Constellation GNSS Receiver GEORIX, the RUAG Space single-frequency GNSS Receiver for GTO and GEO appli- cations provides an excellent on-board real-time navigation solution accuracy of below 20 meter (in GEO) based on an arbitrary mix of GPS and GALILEO space vehicles. Data Products Based on dedicated RF- and Mixed-Signal ASICs as well as – Navigation solution based on GPS/GALILEO constellations the AGGA-4 ASIC, GEORIX is able to use the following signals: – Generation of the PPS signal synchronized to GPS/GALILEO second – GPS C/A on L1 – Carrier phase measurements for each tracked signal – Galileo E1 B/C – code phase measurements for each tracked signal – Support data: Main Features - Tracking state – Antenna with gain pattern optimised for GEO - GDOP – Detached LNAs for improved performance figures - Carrier to noise (C/N) measurement of each tracked signal – GTO support, e.g. for electric propulsion satellites - Noise measurements of each RF down-conversion chain – Support for cross-coupling of two non-redundant antenna/LNA sets - Satellites in view status to cold-redundant electronics box - Satellite navigation message – Accurate force model-based orbit propagator – Advanced Kalman filtering allows high on-board navigation perfor- Interfaces mance – TC/TM interface: MIL-STD-1553B or UART (RS-422) or SpaceWire – Flexible acquisition and tracking concept providing: – PPS output nom/red/test (RS-422) – single frequency signal processing of up to 12 satellites – Primary power interface 100 V regulated – -
The X-Ray Imaging Polarimetry Explorer
Call for a Medium-size mission opportunity in ESA‟s Science Programme for a launch in 2025 (M4) XXIIPPEE The X-ray Imaging Polarimetry Explorer Lead Proposer: Paolo Soffitta (INAF-IAPS, Italy) Contents 1. Executive summary ................................................................................................................................................ 3 2. Science case ........................................................................................................................................................... 5 3. Scientific requirements ........................................................................................................................................ 15 4. Proposed scientific instruments............................................................................................................................ 20 5. Proposed mission configuration and profile ........................................................................................................ 35 6. Management scheme ............................................................................................................................................ 45 7. Costing ................................................................................................................................................................. 50 8. Annex ................................................................................................................................................................... 52 Page 1 XIPE is proposed -
Max-Planck-Institut Für Extraterrestrische
The X-ray Universe 2011, Berlin Max-Planck-Institut für extraterrestrische Physik Download this poster here: http://www.xray.mpe.mpg.de/~hbrunner/Berlin2011Poster.pdf eROSITA: all-sky survey data reduction, source characterization, and X-ray catalogue creation Hermann Brunner1, Thomas Boller1, Marcella Brusa1, Fabrizia Guglielmetti1, Georg Lamer2, Jan Robrade3, Christian Schmid4, Nico Cappelluti5, Francesco Pace6, Mauro Roncarelli7 1Max-Planck-Institut für extraterrestrische Physik, Garching, 2Leibniz-Institut für Astrophysik, Potsdam, 3Hamburger Sternwarte, 4Dr. Karl Remeis-Sternwarte und ECAP, 5INAF-Osservatorio Astronomico di Bologna, 6Zentrum für Astronomie der Universität Heidelberg, 7Dipartimento di Astronomico, Università di Bologna eROSITA on SRG All-sky survey sensitivity eROSITA (extended Roentgen Survey with an Imaging Telescope Array) is the primary instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission, scheduled for launch in 2013. eROSITA consists of Effective area on axis 15´Background off-axis 30´off-axis seven Wolter-I telescope modules, each of which is equipped with 54 mirror shells with an outer diameter of 36 cm and a fast frame-store pn-CCD, resulting in a field-of-view (1o diameter) averaged PSF of 25´´-30´´ 1 keV HEW (on-axis: 15´´ HEW) and an effective area of 1500 cm2 at 1.5 keV. eROSITA/SRG will perform a four year long all-sky survey, to be followed be several years of pointed observations (Predehl et al. 2010). More info on eROSITA: http://www.mpe.mpg.de/erosita/ 4 keV eROSITA orbit and scanning strategy 7 keV Orbit: eROSITA/SRG will be placed in an Averaged all-sky survey PSF (examples) L2 orbit with a semi-major axis of about 1 million km and an orbital period of about 6 months. -
Command & Data Handling
Command & Data Handling We help our customers, the satellite primes, and their customers, the fl eet operators, to manage their spacecraft. We put pride in designing Spacecraft Management Units that are capable of interfacing all the types of equipment you normally find on-board a satellite. Furthermore, we offer our customers a hardware and software environment that makes it easy for them to develop the necessary applications while we take care of system start-up and configuration, software drivers and system debug support. We do all this, and on top we see to that the latest technology available is applied to minimize requirements on mass, volume and power consumption. Ideally, you will not notice our presence! The units handle all commonly used interfaces like reaction wheels, magnetorquers and thrusters as well as standardized analogue and digital interfaces and thermistors. The same basic design is applicable to LEO and GEO satellites and also to interplanetary missions. Features • Everything you need for spacecraft control in a single box • Design scalable to platform size • Highly reliable using internal redundancy and cross-strappings • Advanced hardware support for autonomous missions • Standard interfaces: -Multiple MIL-STD-1553 -SpaceWire -RS-422 UART -Synchronous serial links Functions • On-board satellite telecommand functions as decoding, authen- tication, decryption and distribution of commands • On-board satellite telemetry functions including telemetry data acquisition or generation, formatting, encoding and transmis- -
Exploring the Sky with Erosita
Exploring the X-ray Sky with eROSITA for the eROSITA Team Observatories and mission timelines Basic Scientific Idea …. to extend the ROSAT all-sky survey up to 12 keV with an XMM type sensitivity Historical Development Spectrum-XG Jet-X, SODART, etc. ROSAT 1990-1998 First X-ray all-sky survey with an imaging telescope Negotiations between Roskosmos and ESA ABRIXAS 1999 on a "new" Spectrum-XG mission (2005) To extend the all-sky survey towards higher energies Agreement between Roskosmos and DLR (2007) ROSITA 2002 Spectrum-RG ABRIXAS science on the eROSITA International Space Station Dark Energy 105 Clusters of Galaxies extended ROentgen Survey with an Imaging Telescope Array Mission scenario & Instrument specification • 3 month calibration & science verification phase • 4 yrs all-sky survey (8 sky coverages) • 2.7 yrs pointed observations • Energy range 0.2 - 12 keV • FOV: 1 degree • All-sky survey sensitivity ~ 6 x10-14 erg cm-2 s-1 ~ (10 – 30) x ROSAT • Deep survey field(s) (~100 sqdeg) with 5×10-15 erg cm-2 s-1 • Temporal resolution ~ 50 ms • Energy resolution ~ 130 ev @ 6 keV / 80 ev @ 1.5 keV • Angular resolution ~ 15” (20” survey) eROSITA status: completely approved and funded Mr. Putin gets informed about Dark Energy... Signature of the "Detailed Agreement" (Reichle, Wörner, Perminov) 50:50 data share between Ru / Germany HERCULES BOOTES URSA MAIOR DRACO URSA MINOR LEO CEPHEUS VIRGO CASSIOPEIA CYGNUS AURIGA AQUILA GEMINI PERSEUS ANDROMEDA SCORPIUS PEGASUS SAGITTARIUS CENTAURUS TAURUS ORION VELA CRUX CANIS MAIOR AQUARIUS CARINA HEMISPHAERA ORIENTALIS HEMISPHAERA OCCIDENTALIS Actual definition depends on mission planning eROSITA: Launch date …. -
The X-Ray Background and the ROSAT Deep Surveys
THE X–RAY BACKGROUND AND THE ROSAT DEEP SURVEYS G. HASINGER Astrophysikalisches Institut Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany E-mail : [email protected] G. ZAMORANI Osservatorio Astronomico, Via Zamboni 33, Bologna, 40126, Italy E-mail: [email protected] In this article we review the measurements and understanding of the X-ray back- ground (XRB), discovered by Giacconi and collaborators 35 years ago. We start from the early history and the debate whether the XRB is due to a single, homo- geneous physical process or to the summed emission of discrete sources, which was finally settled by COBE and ROSAT. We then describe in detail the progress from ROSAT deep surveys and optical identifications of the faint X-ray source popula- tion. In particular we discuss the role of active galactic nuclei (AGNs) as dominant contributors for the XRB, and argue that so far there is no need to postulate a hypothesized new population of X-ray sources. The recent advances in the under- standing of X-ray spectra of AGN is reviewed and a population synthesis model, based on the unified AGN schemes, is presented. This model is so far the most promising to explain all observational constraints. Future sensitive X-ray surveys in the harder X-ray band will be able to unambiguously test this picture. 1 Introduction It is a heavy responsibility for us, as it would be for everybody else, to write a paper on the X–ray Deep Surveys and the X–ray background (XRB) for this book, in honour of Riccardo Giacconi. -
Towards a New Generation Axion Helioscope
Towards a new generation axion helioscope Igor G Irastorza Universidad de Zaragoza International Conference onParticle Physics IstambulIstambul,, Turkey,Turkey, June 2020--25th25th 2011 Outline TlkTalk bdbased on JCAP 06 (2011) 013 OutlineOutline:: – Axions: motivation,motivation, theorytheory,, cosmologycosmology.. – Solar axions & the axion helioscopppe concept ––PreviousPrevioushelioscopes & CAST ––TechnicalTechnicalprospects for a new helioscope – Sensitivity prospects ––ConclusionsConclusions ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 2 Zaragoza AXION motivation Strong CP problem: why strong interactions seem not to violate CP? – CP violating term in QCD is not forbidden . But neutron electric dipole moment not observed. Natural answer if Peccei-Quinn mechanism exist. – New U(1) gl lob al symmet ry spontlbktaneously broken. As a result, new pseudoscalar, neutral and very light particle is predicted, the axion. It couples to the photon in every model. PRIMAKOFF EFFECT ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 3 Zaragoza AXION motivation: Cosmology Axions are produced in the earlyyy Universe by a number of processes: – Axion realignment – Decay of axion strings NONNON--RELATIVISTICRELATIVISTIC – Decay of axion walls (COLD) AXIONS In general, Range of axion masses of 10--66 ––1010--33 eV are of interest for the axionto be the (main component of the) CDM. – Thermal production RELATIVISTIC (HOT) AXIONS In order to have substantial relativistic axiondensity, the axion mass must be close to 1 eV.eV. (ma >1.02 eV gives densities too much in excess to be compatible with latest CMB data) Hannestad et al, JCAP 0804 (2008) 019 [0803.1585 (astro-ph)] ICPP, Istambul, June 2011 Igor G. Irastorza / Universidad de 4 Zaragoza Solar Axions SlSolar axi ons prod uced db by ph otonoton--toto-- axion conversion of the solar plasma photons Solar axion flux [van Bibber PRD 39 (89)] [CAST JCAP 04(2007)010] Solar physics + Primakoff effect Only one unknown parameter ga ICPP, Istambul, June 2011 Igor G. -
Vega Lofts Two Satellites on Second Launch This Year 2 August 2017
Vega lofts two satellites on second launch this year 2 August 2017 Optsat-3000 has a design life of seven years and Ven?s four and a half years. Flight VV10 marks the debut of Vega's new lighter payload fairing that protects the satellites during the ascent to space. It was developed under ESA's Launchers Exploitation Accompaniment Programme and manufactured by RUAG Space Switzerland with ELV in Italy as prime contractor. The technology was first proved on 28 June on Ariane 5. The new Vega fairing structure features fewer On 2 August 2017, Vega flight VV10 lifted off from panels and no metallic joints. Different composite Europe’s Spaceport in French Guiana to deliver two material and improved manufacturing have lowered Earth observation satellites, Optsat-3000 and Ven?s, the production cost. into their planned Sun-synchronous orbits. Credit: ESA A launch pad modification for this flight reduced the acoustic loads – the pressure caused by sound waves on the payloads at liftoff – from the first- This morning, Arianespace launched a Vega rocket stage plume striking the structure. carrying two Earth observation satellites for Italy, France and Israel encased in Vega's lighter The changes exploited a computer model of the protective fairing. acoustic environment at liftoff developed under an ESA–NASA knowledge exchange agreement for Liftoff of Vega's 10th mission from Europe's launchers. Flight and ground measurements from Spaceport in Kourou, French Guiana came at this flight will help to gauge the improvements. 01:58 GMT on 2 August (03:58 CEST; 22:58 local time on 1 August) on a mission lasting 97 minutes The payload mass for this launch was about 982 to deliver Optsat-3000 and Ven?s into their kg. -
PLANETARIAN Journal of the International Planetarium Society Vol
PLANETARIAN Journal of the International Planetarium Society Vol. 26, No.4, December 1997 Articles 6 Planetarium Mystique-Our Secret Weapon ..... Jon A. Marshall 12 Astronomy Link Update ........................................... Jim Manning 18 Invitations to IPS 2002 ............................................................. hosts 22 Minutes of the 1972 Council Meeting ............... Lee Ann Hennig Features 27 Computer Corner: Moontool & Jupiter's Moons ...... Ken Wilson 29 Regional Roundup ..................................................... Lars Broman 32 Book Reviews ............................................................ April S. Whitt 38 Planetarium Memories ................................... Kenneth E. Perkins 40 Mobile News Network ............................................. Sue Reynolds 43 Forum: NASA & Public Education ............................ Steve Tidey 47 Gibbous Gazette .................................................. Christine Shupla 50 What's New ................................................................ Jim Manning 53 Opening the Dome: Spirit of Dome .. Jon U. Bell/Carrie Meyers 56 President's Message ............................................. Thomas Kraupe 59 Planetechnica: Computer Imaging Basics ... Richard McColman 66 Jane's Corner ............................................................. Jane Hastings Seeing Is Believing! (Ps EDi'i[ZEe,arlums For further information contact Pearl Reilly: 1-800 .. 726-8805 I NSTRLJrvl fax: 1-504-764-7665 Planetarium Division email: [email protected] -
Erosita Extended Roentgen Survey with an Imaging Telescope Array
eROSITA extended ROentgen Survey with an Imaging Telescope Array Vadim Burwitz for the eROSITA Team: PI: Peter Predehl Co-Is: Hans Böhringer, Ulrich Briel, Hermann Brunner, Evgeniy Churazov, Michael Freyberg, Peter Friedrich, Günther Hasinger, Eckhard Kendziorra, Dieter Lutz, Norbert Meidinger, Mikhail Pavlinsky, Andrea Santangelo, Jürgen Schmitt, Axel Schwope, Matthias Steinmetz, Lothar Strüder, Rashid Sunyaev, Jörn Wilms System Engineer: Josef Eder Product Assurance: H. Bräuninger, M. Hengmith Electronics Engineering: W. Bornemann, O. Hälker, S. Hermann, W. Kink, S. Müller, O. Hans Mechanical Engineering: H. Huber, Chr. Rohé, L. Tiedemann, R. Schreib, B. Mican, K. Lehmann, H. Eibl, F. Huber, R. Sandmair, P. Straube, H. Kestler, F. Soller, J. Liebhart Mirror System, PANTER: P. Friedrich, W. Burkert, M. Freyberg, B. Budau, E. Pfeffermann, V. Burwitz + students CliThlEiiCooling, Thermal Engineering: MFüM. Fürmetz + stu dents CCD-Camera: N. Meidinger, R. Hartmann, G. Schächner, J. Elbs, S. Ebermayer Attitude: A. Schwope Calibration, Analysis: G. Hartner, U. Briel, K. Dennerl, R. Andritschke, Chr. Tenzer Laboratory, PUMA, Tests: M. Vongehr, R. Gaida, K. Dittrich, F. Schrey Ground Software, Simulation: H. Brunner,,pp, N. Cappelluti, G. Lamer, M. Mühlegg gg,,yer, J. Wilms, I. Kreykenbohm , Chr. Schmid Mission Planning: J. Schmitt, J. Robrade Institutes: Industry: Max-Planck-Institut für extraterrestrische Physik, Garching/D Media Lario/I Mirrors, Mandrels Space Research Institute IKI, Moscow/Ru Kayser-Threde/D Mirror Mechanics Univ. Tübingen/D Carl Zeiss/D Mirror Mandrels Univ. Hamburg/D Invent/D Telescope Structure Univ. Erlangen-Nürnberg/D pnSensor/D CCDs Astroppyhysikalisches Institut Potsdam/D EHP/B Cooling Max-Planck-Institut für Astrophysik/D RUAG/A Mechanisms, MLI .. -
LAUNCH KIT April 2021 VV18 Pléiades Neo and Five Auxiliary Payloads
LAUNCH KIT April 2021 VV18 Pléiades Neo and five auxiliary payloads VV18 Pléiades Neo 3 Five auxiliary payloads with the Small Spacecraft Mission Service FLIGHT VV18 For its third mission of the year and the first Vega flight of 2021, Arianespace will put in orbit the Pléiades Neo 3 satellite on behalf of Airbus Defence and Space along with five auxiliary payloads through the piggyback mission, Small Spacecraft Mission Service (SSMS). Flight VV18 underscores Arianespace’s comprehensive range of innovative and very competitive services to address the nano- and micro-satellite market sub-segment, serving both institutional and commercial needs. Pléiades Neo 3 satellite The ambitious project of Airbus Defence and Space: Pléiades Neo, the first European CONTENTS satellite constellation at 30 cm resolution. Pléiades Neo 3 is the first of the Pléiades Neo constellation to be launched. Entirely funded, > THE LAUNCH manufactured, owned and operated by Airbus, Pléiades Neo is a breakthrough in Earth observation domain. VV18 mission Pages 2- 4 With 30 cm resolution, best-in-class geolocation accuracy and twice-a-day revisit, the four Pléiades Neo satellites unlock new possibilities with ultimate reactivity. Thanks to these state-of- Pléiades Neo 3 satellite the-art satellites, each step of the acquisition and delivery cycle offers top-level Earth observation Page 5 services now and going forward for the next ten years. In addition, their reactive tasking ability allows urgent acquisitions 30 to 40 minutes following request - which is five times higher than > FURTHER INFORMATION previous constellations - and respond to the most critical situations in near real-time, very useful Vega launch vehicle for natural disaster.