Spektr-RG / SRG
Spektr-RG / SRG (Spectrum Roentgen Gamma) astrophysical observatory
Spektr-RG/SRG is an international cooperative space research and technology demonstration mission of Roskosmos (Russia), ESA (Europen Space Agency), IKI (Space Research Institute), Moscow; MPE (Max-Planck-Institute for extraterrestrial Physics), Garching, Germany, and NASA/MSFC, Huntsville, AL, USA. A MOU (Memorandum of Understanding) was signed in March 2007 between DLR and Roskosmos. On Aug. 18, 2009, DLR and Roskosmos signed a detailed agreement during the MAKS International Aviation and Space Salon in Moscow, specifying all the organizational and technical boundary conditions for the eROSITA project. 1) 2)
The overall objective of the mission is to conduct the first all-sky survey with an imaging telescope in the 0.5-11 keV band to discover the hidden population of several hundred thousand obscured supermassive black holes and the first all-sky imaging X-ray time variability survey. In addition to the all-sky surveys it is foreseen to observe dedicated sky regions with high sensitivity to detect ten thousands of clusters of galaxies and thereafter to do follow-up pointed observations of selected sources, in order to investigate the nature of Dark Matter and Dark Energy. The proposed orbit provides an order of magnitude lower particle background than those of Chandra and XMM-Newton, which will allow the detailed study of low-surface-brightness diffuse objects.
The newly defined SRG mission represents a highly significant scientific and technological step beyond Chandra/XMM-Newton and is expected to provide important and timely inputs for the next generation of giant X-ray observatories like IXO (International X-ray Observatory) collaborative mission of ESA along with NASA and JAXA for the timeframe 2021.
• Roskosmos is the provider of the spacecraft bus and the launch of the satellite
• The ART-XC instrument and gamma-ray burst detector are being provided by RosKosmos (an IKI-led consortium)
• ESA will provide the communication subsystem and ground station support.
Initially (early 1990s), the high-energy international mission was called SXG (Spectrum-X Gamma), planned to be developed under the auspices of the Russian Space Agency, with instruments contributed by research groups in a number of European countries and the US. The payload consisted of a number of imaging instruments for cosmic photon observations in the energy range of 0.03 - 100 keV. A launch was planned for 1999. - However, due to repeated delays of the SXG project, caused by the economic situation in post-Soviet Russia, a new approach was taken in the timeframe 2004.
In the early SRG definition phase of the mission (2005-2007), there was a third payload in planning for SRG, namely the LWFT (Lobster-Eye Wide Field Telescope), a new technology introduction designed and developed by the Space Research Center of the University of Leicester, UK. However, the LWFT payload was removed from the SRG mission in 2008 due to budgetary problems in the UK.
The LWFT instrument is an all-sky X-ray monitor comprised of 5 telescope modules, each consisting of approximately 60 MCP (Microchannel Plate) optics, tiled to produce the required field of view and geometrical area. Each telescope module has a so-called "microwell array proportional counter" detector in the focal plane. 8) 9) 10) 11)
The ‘lobster-eye' geometry which permits this huge sky coverage as well as high sensitivity, is achieved with square-pore MCPs based on the eyes of the crustaceans themselves (Figure 1) with Micromegas detectors. This configuration rotates to cover the whole sky in ~90 minutes in continuous slew mode with a given source transiting the FOV in 300-1800 s.
Figure 1: Focal plane diagram showing the lobster-eye geometry (image credit: University of Leicester)
Spektr-RG (SRG) is an astrophysical space observatory, aimed at studying our Universe in the X-ray band of the electromagnetic spectrum once it is in position at the Lagrange point L2 of the Sun-Earth system, 1.5 million kilometers away from Earth.
The Spektr-RG astrophysical space observatory is developed by the Russian side under the Federal Space Program of Russia, section on Fundamental Space Research, by order of the Russian Academy of Sciences with the participation of Germany.
The SGR spacecraft is based on the 'Navigator' multi-use bus of the NPO Lavochkin Scientific Production Association, Khimki, Russia. The spacecraft is 3-axis stabilized and has an estimated launch mass of ~ 2650 kg (total payload mass of 1160 kg). 12) 13) 14) 15)
Figure 2: Artist's view of the deployed SRG spacecraft (image credit: IKI)
Figure 3: Illustration of the Navigator bus architecture (image credit: Lavochkin Association)
Table 1: Basic parameters of the Navigator bus
RF communications: Data transmission rate of 2 Mbit/s.
Figure 4: Illustration of the SRG spacecraft (image credit: NPO Lavochkin)
• June 22, 2019: eROSITA marks the beginning of a new era in X-ray astronomy. Because no telescope before has ever focused on the entire sky in as much detail as eROSITA will. "We built eROSITA to transform the way we see the X-ray sky, and to unravel the mysteries of cosmology and black holes", says Peter Predehl from the Max Planck Institute for Extraterrestrial Physics, the scientific Director of the mission. "The unprecedented spectral and spatial resolution will allow us to study the distribution of huge galaxy clusters and find out more about the mysterious dark energy". 16)
- The question of the nature of the mysterious dark energy, which is tearing the universe apart at an accelerated rate, has occupied astronomers for many years. Dark energy accounts for almost 70% of the total mass of the universe. It eludes direct observation. But together with dark matter, which accounts for about 30% of space, it influences the formation and evolution of galaxy clusters; these are the largest gravitationally bound objects in the universe.
- The question of the nature of the mysterious dark energy, which is tearing the universe apart at an accelerated rate, has occupied astronomers for many years. Dark energy accounts for almost 70% of the total mass of the universe. It eludes direct observation. But together with dark matter, which accounts for about 30% of space, it influences the formation and evolution of galaxy clusters; these are the largest gravitationally bound objects in the universe.
- In a detailed sky survey, eROSITA will map the large-scale structure of the universe and observe around 100,000 galaxy clusters. The researchers are not only focussing their attention on the hot intergalactic medium in these clusters but also on gas and dust in between. On a large scale, these threads of matter give the cosmos the structure of a network; the galaxy clusters arrange themselves at the nodes of this network.
- The scientists also expect the X-ray telescope to detect millions of active galactic nuclei containing massive black holes. "Earlier this year, we saw the first image of a supermassive black hole sitting in the center of a galaxy. eROSITA will now tell us when and where this monster and a million others like it grew over cosmic time," states Kirpal Nandra, Director of the High-Energy Astrophysics group at MPE. "It's staggering to think how much our understanding of the Universe has advanced."
- Within our Milky Way, eROSITA will also discover many X-ray sources, including double stars and the remains of stellar explosions (supernovae). Rare objects such as isolated neutron stars (i.e. the burnt out and super dense relics of dead, massive suns) are also on the observation plan.
• On 25 April 2019, the Spektr-RG Space Observatory was transported to the Baikonur Cosmodrome - the final stage in preparation for its launch on 21 June. Spektr-RG carries the X-ray telescope eROSITA, which was developed and built at MPE. Its aim is to perform a highly sensitive survey of the entire sky in X-ray light, once it arrives at its observation point L2. 17)
Figure 5: Spektr-RG with eROSITA is transported to the Baikonur Cosmodrome (image credit: Roskosmos)
- In Baikonur, the Spektr-RG space observatory will be subject to final ground tests and will be integrated into the launch vehicle. The launch is planned for 21 June 2019 with a Proton M launcher and a DM-03 upper stage. Members of the eROSITA team will carry out final tests and preparations for launch at the beginning of May.
- The eROSITA X-ray space telescope consists of seven identical mirror modules with 54 nested gold-coated mirrors each, manufactured very precisely to collect the high-energy photons and guide them to the X-ray sensitive cameras placed at their focus. These cameras have also been developed and custom-built at MPE, containing special X-ray CCDs manufactured from high-purity silicon. For maximum performance, these cameras have to be cooled to -90°C using a complex heat pipe system.
- In addition to eROSITA, Spektr-RG also carries the Russian telescope "ART-XC". Both instruments will fly from the Russian launch site Baikonur in Kazakhstan with a rocket to the second Lagrange point (L2) of the Sun-Earth system.
Figure 6: Spektr-RG carries the eROSITA X-ray telescope developed and built at MPE as well as the Russian telescope ART-XC (image credit: Roscosmos)
- Leaving Earth behind, eROSITA will then travel to the second Lagrange point (L2) of the Sun-Earth system, at a distance of about 1.5 million kilometers. Over a period of four years, eROSITA will carry out a total of eight scans of the entire sky to measure about 100,000 galaxy clusters, find about three million supermassive black holes and make many other interesting discoveries. This new sky survey, with much improved energy resolution and 20 times higher sensitivity than the previous one performed by ROSAT, will give scientists a closer insight into the origin and evolution of the universe.
• September 18, 2018: During 2018, Russian specialists conducted assembly and testing of the Spektr-RG X-ray observatory in preparation for launch in the following year. 18)
- On 19 April 2018, the press-service of the RKS Corporation said that it had delivered the Spektr-RG's radio system, BRK, and that the launch of the space observatory would occur in March 2019.
- By the end of May, both operational instruments of the observatory — the Russian ART-XC and the German eRosita — had been integrated with the flight version of the Navigator service module and tested. At the time, engineers were still working on a software update in the flight control system, BKU, of the spacecraft for handling the interface with the ART-XC instrument, industry sources said.
- On May 29, NPO Lavochkin announced that from May 3 to May 21, a joint team of its engineers and specialists from the Space Research Institute, IKI, in Moscow and Max Planck Institute in Germany had conducted electric tests of the flight-worthy onboard radio complex, BRK, integrated with eRosita and ART-XC telescopes. According to NPO Lavochkin, the electric tests were necessary to check interaction between the service systems of the spacecraft and scientific instruments. The company also said that the spacecraft had been transferred to the assembly room and was a process of preparation for thermal and vacuum tests which had been scheduled to begin in July.
- In the meantime, on May 22, Roskosmos abruptly cancelled a routine status meeting of participants in the Spektr-RG project scheduled in Moscow just two days later on May 24. According to the official explanation sent to the German side, a letter from the German space agency, DLR, requesting the review had come too late for the Russian side to process for the given date. However, the Russian leadership of the Spektr-RG project unofficially informed their German colleagues that the cancellation might be related to another management shakeup at the top of Roskosmos.
- The sources familiar with the situation expressed optimism that the Spektr-RG had remained on track for its latest launch window at the end of March — beginning of April 2019. At the time, the launch window for Spektr-RG was reported to be extending from February 27 to April 11, 2019.
• On January 20, 2017, the completed eROSITA X-ray telescope boarded a cargo plane and was transported from Munich, where it had been built at the MPE (Max Planck Institute for Extraterrestrial Physics), to Moscow. At NPO Lavochkin Scientific Production Association, Khimki near Moscow, eROSITA will be further tested and integrated with the SRG (Spectrum Roentgen Gamma) spacecraft in preparation for launch in spring 2018. 19)
- "With its much higher sensitivity than previous survey missions, eROSITA will discover a multitude of new X-ray sources," expects Dr. Andrea Merloni, eROSITA project scientist. "We will be able to study not only the distribution of clusters of galaxies – eROSITA will detect more than 100,000 of these most massive bound objects in the Universe – but also millions of active black holes at the centers of galaxies, as well as rare objects in the Milky Way, such as isolated neutron stars. The survey will thus provide new insights into a wide range of high-energy astrophysical phenomena – maybe even reveal some completely new phenomena – and give us new clues about the mysterious "Dark Energy", the force behind the accelerated expansion of the Universe."
- SRG also carries the Russian telescope "ART-XC". Both instruments will be launched with a Proton rocket from the Russian launch site Baikonur in Kazakhstan after another 2600 km transport.
Figure 7: After about ten years of development and integration the eROSITA X-ray telescope is complete: with 7 mirror modules and 54 mirror shells each combined with 7 specially built X-ray cameras. You see the telescope here after final integration at MPE, shortly before transport to further testing (image credit: MPE)
• December 2016: The Russian-built ART-XC telescope and the Navigator platform (which would carry both instruments into space), were reported to be in a high degree of readiness for flight. The ART-AC instrument was finally delivered from RKTs Progress in Samara to NPO Lavochkin by Dec. 27, 2016, according to Anatoly Zak.
- The final assembly and the integrated testing of the Spektr-RG / SRG spacecraft is expected to take around nine months, making the spacecraft available for the delivery to Baikonur around October 2017.
• December 2016: The final test campaign on the full telescope (vibration, mass properties and EMC) took place at IAGB (Ottobrunn), prior to the Moscow flight of eROSITA.
• November 2016: The eROSITA FM (Flight Model) telescope has been fully integrated in the MPE integration Lab. After completion of the work in September 2016, the telescope left MPE to be transported to the PANTER test facility, where it underwent an extensive test campaign. 20)
• April 2016: The final calibration of eROSITA's 8 MAs (Mirror Assemblies) is still ongoing in the PANTER facility of MPE, while the calibration of all CAs (Camera Assemblies) is underway in the smaller PUMA facility at MPE. 21)
- In parallel, the project started the preparation for the complete telescope integration (Figure 8), each of the 7 MA-CA pairs will be mounted first, thereby precisely adjusting the distance between mirror and camera to the individual focal lengths which has been measured during the mirror calibration.
- The SRG spacecraft is assembled in proto-flight configuration, waiting for the integration of the radio complex FM, expected for May 2016. The development for the GCS (Ground Control Segment) is ongoing, with no delays. The SRG GCC (Ground Control Center) will be operative in Q2 of 2017. A compatibility test with the MPE GCS is scheduled for early 2017. The launch vehicle are available and the SRG launch is confirmed for September 2017.
Figure 8: The integration of the MAs and MCs (shown here) requires an extreme accuracy: the individual focal length (1600 mm) of each pair has to be within 50 µm. The metrology system has been developed at MPE (image credit: MPE)
Launch: The Spektr-RG/SRG spacecraft (liftoff mass of 2,704 kg) was launched on 13 July 2019 (12:30:57 UTC) on a Proton/Block-DM-03 upper stage from the Baikonur Cosmodrome, Kazakhstan. 22) 23) 24) 25)
Figure 9: The launch sequence and ground track during the booster phase of the Spektr-RG launch (image credit: Anatoly Zak, Russian SpaceWeb.com)
Orbit: The orbit of SRG has been selected to be at L2 (Lagrangian Point 2). The spacecraft will be in a Lissajous (or halo) orbit about the Lagrangian point L2. In the Sun‐Earth system the L2 point is on the rotating Sun-Earth axis about the same distance away as L1 (1.5 million km, representing 1/100 the distance from Earth to the Sun) but at the opposite side of the Earth. The L1 location is inside the Earth orbit while the L2 location is outside the Earth orbit. 26)
Note: The initial LEO circular orbit of the mission of 580 km altitude was revised in 2008 to a Lagrangian orbit at L2.
Figure 10: Illustration of the Lagrangian points in the Sun-Earth system (image credit: IKI)
• The 3 months flight to L2 will be used in the verification and calibration of the payload.
• 4 years - duration of an all sky survey; 8 all sky surveys (scanning mode: 6 rotations/day, 1 degree advance per day)
• 3 years - follow-up period (goal) used for pointed observations of a selection of the most interesting galaxy clusters and AGNs (Active Galactic Nuclei).
Figure 11: The eROSITA X-ray telescope - On the hunt for Dark Energy (video credit: DLR)
• On 22 October 2019, the beautiful first X-ray images of the eROSITA telescope were presented to the public at the Max Planck Institute for Extraterrestrial Physics (MPE) in Garching. After an extended commissioning phase, since October 13 all seven X-ray telescope modules with their custom-designed CCD cameras have been observing the sky simultaneously. The first combined X-ray images of our neighboring galaxy, the Large Magellanic Cloud, and a pair of interacting clusters of galaxies at a distance of about 800 million lightyears, show remarkable details and demonstrate the promise of the ambitious science program planned with the spaceborne telescope. 27)
- "These first images from our telescope show the true beauty of the hidden Universe," enthuses Peter Predehl, Principal Investigator of eROSITA. "To meet our science goals we needed enough sensitivity to detect the most distant clusters of galaxies in the Universe over the whole sky, and resolve them spatially. These First Light images show that we can do exactly that, but we can go a lot further." In addition to the sharp X-ray vision provided by each of eROSITA's seven mirrors, each telescope is equipped with state-of-the-art CCD cameras with superb spectral and timing resolution. "The potential for new discoveries is immense. Now we can start reaping the fruits of more than ten years of work," adds Predehl.
- The eROSITA ‘First Light' images were obtained in a series of exposures of all seven telescope modules with a combined integration time of about one day for both the Large Magellanic Cloud (LMC), our neighboring galaxy, and the A3391/3395 system of interacting clusters of galaxies at a distance of about 800 million lightyears.
- In our neighboring galaxy, the LMC, eROSITA not only shows the distribution of the diffuse hot gas, but also some remarkable details, such as supernova remnants like SN1987A. The eROSITA image now confirms that this source is becoming fainter, as the shock wave produced by the stellar explosion in 1987 propagates through the interstellar medium. In addition to a host of other hot objects in the LMC itself, eROSITA also reveals a number of foreground stars from our own Milky Way galaxy as well as distant Active Galactic Nuclei, whose radiation pierces the diffuse emission of the hot gas in the LMC.
- "X-rays give us a unique view of the Universe, hidden in visible light", explains Kirpal Nandra, director of High Energy astrophysics at MPE. "Looking at an apparently normal star, in X-rays we might see an orbiting white dwarf or neutron star in the process of devouring its companion. Visible light shows the structure of a galaxy traced by its stars, but the X-rays are dominated by supermassive black holes growing at their centers. And where we see clusters of galaxies with optical telescopes, X-rays reveal the huge reservoirs of gas filling the space between them and tracing out the dark matter structure of the Universe. With its performance demonstrated, we now know that eROSITA will lead to a breakthrough in our understanding of the evolution of the energetic Universe."
Figure 12: This image shows our neighboring galaxy, the LMC (Large Magellanic Cloud), observed in series of exposures with all seven eROSITA telescope modules taken from 18 to 19 October 2019. The diffuse emission originates from the hot gas between the stars with temperatures typically a few million degrees. The more compact nebulous structures in the image are mainly supernova remnants, i.e. stellar atmospheres expelled in huge explosions at the end of a massive star's lifetime. The most prominent one, SN1987A, is seen as the bright source close to the center. A host of other sources in the LMC itself include accreting binary stars or stellar clusters with very massive young stars (up to 100 solar masses and more). There are also a number of point sources, either foreground stars from our home Galaxy or distant Active Galactic Nuclei (image credit: MPE/IKI, F. Haberl, M. Freyberg and C. Maitra)
- Reaching further out into the Universe, the eROSITA image of the A3391/3395 system of interacting clusters of galaxies highlights the dynamical processes which lead to the formation of gigantic structures in the Universe. The clusters, appearing as large, elliptical nebulae in the eROSITA images, span tens of millions of lightyears across, and contain thousands of galaxies each. Clusters are one of the main science targets for eROSITA; astronomers expect to find some 100,000 X-ray emitting galaxy clusters as well as several million active black holes in the centers of galaxies during its 4-year all-sky survey in the soft and hard X-ray bands. "By measuring the evolution of these clusters over cosmic time, we can make precision measurements of the cosmological parameters to better understand the dark matter and dark energy that dominate the Universe" says astrophysicist Esra Bulbul, who leads the work on clusters and cosmology at MPE.
Figure 13: These two eROSITA images show the two interacting galaxy clusters A3391, to the top of the image, and the double-peaked cluster A3395, to the bottom, highlighting eROSITA's superb view of the distant Universe. They were observed in a series of exposures with all seven eROSITA telescope modules taken from 17 to 18 October 2019. The individual images were subjected to different analysis techniques, and then colored in different schemes to highlight the different structures. In the left-hand image, the red, green and blue colors refer to the three different energy bands of eROSITA. One clearly sees the two clusters as nebulous structures, which shine brightly in X-rays due to the presence of extremely hot gas (tens of millions of degrees) in the space between galaxies. The image on the right highlights the "bridge" or "filament" between the two clusters, confirming the suspicion that these two huge structures do interact dynamically. The eROSITA observations also show hundreds of point-like sources, signposting either distant supermassive black holes or hot stars in the Milky Way [image credit: T. Reiprich (Univ. Bonn), M. Ramos-Ceja (MPE), F. Pacaud (Univ. Bonn), D. Eckert (Univ. Geneva), J. Sanders (MPE), N. Ota (Univ. Bonn), E. Bulbul (MPE), V. Ghirardini (MPE), MPE/IKI]
- "This is a dream come true. We now know that eROSITA can deliver on its promise and create a map of the whole X-ray sky with unprecedented depth and detail," confirms Andrea Merloni, eROSITA Project Scientist. "The legacy value will be enormous. Beside the beautiful images like the ones we're showing today, catalogues of millions of exotic celestial objects such as black holes, galaxy clusters, neutron stars, supernovae and active stars will be used by astronomers for years to come."
- Launched on 13 July 2019 as part of the Russian-German Spektrum-Roentgen-Gamma (SRG) space mission, which also includes the Russian ART-XC telescope, eROSITA completed its 1.5 million kilometer journey to the second Lagrange point (L2) of the Earth-Sun-system on October 21, and has now – 100 days after launch – entered its target orbit around L2. The commissioning phase of the telescope was officially completed on October 13. While the scientific performance of the system is outstanding, this first phase was not problem-free.
- "The commissioning phase lasted longer than expected, after we found some anomalies in the electronic controls of the cameras," explains Peter Predehl. "But teasing out these problems is exactly why we have such a phase. After a careful analysis we determined that the issues are not critical. We're still working on them, but in the meantime the program can go forward normally." The telescope has now entered the so-called calibration and performance verification (CalPV) phase, during which astronomical observations are carried out to better understand the instrument and verify its full potential to meet the scientific requirements. At the end of the CalPV phase, after a final review by the operations team, SRG and eROSITA will enter into its prime phase, the four year all-sky X-ray survey.
- The development and construction of the eROSITA X-ray telescope was led by the Max Planck Institute for Extraterrestrial Physics with contributions from the Institute for Astronomy and Astrophysics of the University Tübingen, the Leibniz Institute for Astrophysics Potsdam (AIP), University Observatory Hamburg, and Dr. Karl Remeis Observatory Bamberg, with the support of the German space agency DLR. The Ludwig-Maximilians-Universität Munich and the Argelander Institute for Astronomy of the University Bonn also participated in the science preparation for eROSITA. The Russian partner Institute is the Space Research Institute IKI in Moscow; NPOL, Lavochkin Association, in Khimky, near Moscow, is responsible for the technical implementation of the whole SRG mission, which is a joint project of the Russian and German space agencies, Roscosmos and DLR.
• The Spektr-RG observatory successfully separated from the upper stage! Next stage: 3 months after launch — cruise to L2, positioning, performance verification (PV) and calibration phase (Ref. 25).
- 4 years — all-sky survey in 0.3–11 keV energy band (Ref. 11);
- 2.5 years — observations of selected objects and regions in the harder X-ray range up to30 keV in a 3-axis stabilization mode.
Sensor complement: (eROSITA, ART-XC)
The scientific payload consists of two independent telescopes — a soft-X-ray survey instrument, eROSITA, being provided by Germany, and a medium-X-ray-energy survey instrument, ART-XC (Astronomical Roentgen Telescope- X-ray Concentrator), being developed by Russia.
eROSITA (extended ROentgen Survey with an Imaging Telescope Array):
eROSITA is an instrument designed and developed at the MPE (Max-Planck-Institut für Extraterrestrik), Garching, Germany (lead institute and project management) with DLR funding. Further cooperating institutions and companies in the eROSITA project are: Institut für Astronomie und Astrophysik der Universität Tübingen (IAAT); Astrophysikalisches Institut Potsdam (AIP); Dr.-Remeis-Sternwarte, Bamberg; Hamburger Sternwarte; Space Research Institute (IKI), Moscow; Roskosmos, Moscow; Kayser-Threde GmbH, Munich; Carl Zeiss AG, Oberkochen; MLT (Media Lario Technologies), Italy.
The general design of the eROSITA X-ray telescope is derived from that of ABRIXAS (A Broadband Imaging X-ray All-Sky Survey). A bundle of 7 mirror modules with short focal lengths make up a compact telescope which is ideal for survey observations. Similar designs had been proposed for the missions DUO (Dark Universe Observatory) and ROSITA but were not realized due to programmatic shortfall. Compared to those, however, the effective area in the soft X-ray band has now much increased by adding 27 additional outer mirror shells to the original 27 ones of each mirror module. The requirement on the on-axis resolution has also been confined, namely to 15 arc seconds HEW (Half Energy Width). For these reasons the prefix "extended" was added to the original name "ROSITA". The scientific motivation for this extension is founded in the ambitious goal to detect about 100,000 clusters of galaxies which trace the large scale structure of the Universe in space and time. 28) 29)
- An extension of the ROSAT imaging all-sky survey to higher X-ray energies up to 10 keV with unprecedented spectral and angular resolution. Thereby, eROSITA will act as a pathfinder for the next X-ray observatories, particularly the SIMBOL-X and the IXO (International X-ray Observatory) missions.
- With the detection of a sufficiently large number of clusters of galaxies, precise measurements will be feasible of the equation of state of Dark Energy and of "baryonic acoustic oscillations" in the power density spectrum of galaxy clusters.
• To detect systematically all obscured accreting Black Holes in nearby galaxies, as well as many (> 170000) new, distant active galactic nuclei
• To detect the hot intergalactic medium of 50-100 thousand galaxy clusters and groups and hot gas in filaments between clusters, so as to map out the large-scale structure in the Universe for the study of cosmic structure evolution
• To study in detail the physics of galactic X-ray source populations, like pre-main sequence stars, supernova remnants and X-ray binaries.
eROSITA will perform a deep survey of the entire X-ray sky. In the soft band (0.5-2 keV), it will be about 30 times more sensitive than ROSAT, while in the hard band (2-8 keV) it will provide the first ever true imaging survey of the sky. The design driving science is the detection of large samples of galaxy clusters to redshifts z > 1 in order to study the large scale structure in the Universe and test cosmological models including Dark Energy. In addition, eROSITA is expected to yield a sample of around 3 million AGN (Active Galactic Nuclei), including obscured objects, revolutionizing our view of the evolution of supermassive black holes and of their role in the structure formation process. The survey will also provide new insights into a wide range of astrophysical phenomena, including X-ray binaries, active stars and diffuse emission within the Galaxy.
The X-ray telescope of eROSITA consists of 7 identical and co-aligned mirror modules, each with 54 nested Wolter-1 type mirror shells. The mirror shells are glued onto a spider wheel which is screwed to the mirror interface structure making a rigid mechanical unit. The assembly of 7 modules forms a compact hexagonal configuration with 1300 mm diameter (Figure 15) and will be attached to the telescope structure which connects to the 7 separate CCD cameras in the focal planes. The co-alignment of the mirror module enables eROSITA to perform also pointed observations.
Figure 14: Schematic view of the eROSITA instrument (image credit: MPE, Ref. 15)
Figure 15: Configuration of the eROSITA mirror modules (image credit: MLT, MPE)
The mirrors manufacturing is based on a replication process from the ultra-smooth polished master. The mirror manufacturing process is divided into the following main steps (Figure 16):
1) The master is created in order to have a shape that is the negative of the final reflective surface of the mirror to be produced.
2) The master is then super-polished to have appropriate roughness and shape accuracy.
3) A layer of gold is deposited onto the master.
4) The master is then mounted on a support frame that holds it during electroforming, allowing also a proper rotation inside the galvanic bath. The master is then placed in the electroforming bath containing a proprietary chemistry, where the metal layer is deposited up to the desired thickness forming directly the mirror.
5) After the electroforming process is completed the mirror and the master are separated by thermal separation. The particular properties of the separation layer ensure a clean interface separation at the original master's outer surface, thus reproducing the master's optical surface quality onto the mirror.
6) Integration in VOB (Vertical Optical Bench).
7) X-ray test.
Figure 16: Overview of the mirror manufacturing process (image credit: MLT, MPE)
In the frame of the eROSITA mission Media Lario Technologies is in charge of the production of the new mandrels from n. 27 to n. 1, which are the bigger ones. The remaining mandrels from n. 54 to n. 28 are provided by the Max Planck Institute and are the ones used for the ABRIXAS mission (Ref. 28).
Table 2: Basic data of the eROSITA telescope 42)
Figure 17: Illustration of the eROSITA instrument (image credit: MPE)
Each telescope consists of a highly nested mirror system with 54 paraboloid-hyperboloid mirror shells and a frame store pnCCD (pn-junction CCD detectors) camera with a 3 cm x 3 cm large image area (corresponding to a field of view of 1º in diameter on the satellite) with a pixel size of 75 µm by 75 µm. The imaging area consists of 384 x 384 pixels.
The camera is equipped with seven dedicated focal plane pnCCD detectors which are located at the focal point of each of the mirror modules. The pnCCD detector concept permits accurate spectroscopy of X-rays as well as imaging with high time resolution. The pnCCD detector is based on the successful XMM-Newton pnCCD detector concept but was further improved in terms of design and technology. 43)
In particular, a frame store section is added to the image area for the purpose of simultaneous imaging and a readout capability in separate CCD areas. The thickness of the whole pnCCD chip of 450 µm is uniformly sensitive to X-rays from very low up to very high energies. The X-ray photon detection efficiency is at least 90% in the energy band from 0.3 keV to 10 keV. Frame store operation allows very high frame rates of up to 200 X-ray images per second without smearing of the image (Figure 18).
Operating the CCD in frame store (i.e. frame transfer) mode is accomplished by transferring rapidly the image into the frame store area within 200 µs after the 50 ms exposure time. Since the frame store area is shielded against X-rays, the stored image can be read out without interference row by row, while the photons of the next image accumulate in the image area. The readout time is less than 10 ms for the complete image, in the remaining time the CAMEX (CMOS Amplifier and MultiplEXer) readout chip is switched into standby mode to minimize the average heat dissipation to the focal plane CCD.
Figure 18: Prototype of the eROSITA pnCCD detector module with 2 cm x 2 cm large pnCCD (image credit: MPI-HLL)
The pnCCD shows best energy resolution at temperatures below -60º C. For the satellite mission a lower temperature is required due to the proton environment which causes radiation damage by creating defects in the silicon lattice. The eROSITA pnCCD detector offers in addition the possibility to select the optimum gain out of a choice of 16 discrete levels. This option allows spectroscopy and imaging of higher energetic particles, e.g. electrons or protons, on ground as well as in space.
Detector module: The pnCCD is a column-parallel device. Each of the 384 CCD channels is equipped for this purpose with an anode, which is connected to the gate of the on-chip JFET (Junction Field-Effect Transistor). The CCD on-chip transistors are operated in source follower mode and are read out in parallel by the CAMEX chip. This mixed signal ASIC comprises 128 parallel readout channels; each of them includes an eightfold correlated double sampling filter. The specific settings, which determine one of the various possible operating modes, are stored in digital registers of the CAMEX. Programming is done via a serial interface. The ASIC features the following functional blocks:
- Current source to bias the pnCCD JFET
- JFET preamplifier for pnCCD signal amplification
- Programmable RC low pass for bandwidth limitation
- Eight-fold correlated double sampling filter
- Sample and hold stage
- 128 to 1 multiplexer
- Output buffer
- On-chip digital sequencer (16 x 64 bit)
- Serial programming interface with LVDS
- Option of integrated bias current DACs (digital analog converters).
Figure 19: Schematic drawing and geometry of the eROSITA flight detector (image credit: MPI-HLL)
eROSITA camera: The entire eROSITA camera including control and readout electronics is developed in a close cooperation by MPE Garching and MPI-HLL (Max-Planck-Institut Halbleiterlabor), Munich.
The electronics of each eROSITA camera can be subdivided into frontend electronics nearby the detector and the other electronics, which is located in a particular box per camera system. That way the seven eROSITA cameras are independent of each other. Their arrangement is shown in Figure 20.
The camera housing provides also a thermal interface and protects the detector against light, dust and radiation (Figure 21). A cylindrical titanium block, which is glued on top of the Al2O3 detector PCB (Printed Circuit Board), is fitted into the CCD-module casing and fixed with a single screw (Figure 22). The aluminum CCD module casing is cooled to -80ºC using heat pipes; it is thermally insulated with MLI (Multilayer Insulation). The module is mounted with thin glass fiber brackets to the surrounding proton shield providing a temperature of approximately +20ºC.
Figure 20: Arrangement of the seven eROSITA camera modules (without electronics boxes), image credit: MPE
Figure 21: Cross section of the eROSITA camera module (image credit: MPE)
Legend to Figure 21: X-rays enter the pnCCD image area top left through the cut-out in the proton shield. While the copper proton shield is not cooled, the camera casing, which surrounds the CCD detector, is connected with a heat pipe to the central cooling system for all seven cameras. The electronics box with the DAQ (Data Acquisition) system belonging to the camera is not shown.
Figure 22: Illustration of the eROSITA detector module (image credit: MPE)
Figure 23: Photo of the eROSITA QM (Qualification Model) camera (image credit: MPE) 44)
Data acquisition system electronics: Apart from the detector electronics, each camera comprises a DAQ system and electrical interfaces (Figure 24). The main interfaces are a synchronous bidirectional bus for telecommands and telemetry and a power line (+27 V nominal and redundant from power distribution unit).
The DAQ electronics provides the following subsystems:
- Power converters and control units. Some voltages are switchable and/or commandable by telecommands
- Sequencer with reprogrammable FPGA, which generates all necessary timing signals for the detector and the ADCs (Analog Digital Converters)
- ADCs, which digitize the differential analog CAMEX signals into 14 bit data for each CCD pixel per frame. The digital data are delivered to a DSP via a FIFO implemented in the FPGA using DMA transfers.
- DSP event processor: A digital signal processor (DSP) calculates offset as well as noise tables and is able to transmit unprocessed raw data for testing purposes. The DSP applies offset and common mode corrections, event thresholds (low and high), and optionally performs split event recognition. The processed data (with energy, position and time information) are transmitted to the interface controller. The event processor executes and distributes telecommands, collects housekeeping and science data and is able to upload new software to itself and the FPGA. Memory uploads can be stored temporarily in volatile memory or permanently in reprogrammable FLASH memory. The initial program will be stored in higher qualified boot-PROMs. The DSP uses its fast internal memory for calculations. An external memory is available for additional data tables and testing.
- Onboard calibration wheel control: Movement and position readout of the calibration mechanism with its selectable positions: open (nominal), closed (testing) and X-ray source (calibration).
The event processor must complete the digital signal processing of a frame, i.e. of 147,456 pixels, during the cycle time of 50 ms. This includes in particular for each pixel offset subtraction as well as common mode determination and subtraction per row. Finally, events are discriminated from noise by comparison with a low threshold and they are rejected, if a high threshold is exceeded, i.e. they are recognized as particles.
Figure 24: Block diagram of the eROSITA camera electronics (image credit: MPI)
Figure 25: eROSITA performance (image credit: MPE)
The point source sensitivity of eROSITA: ~30 times better than ROSAT (soft band 0.5-2 keV) and ~100 times better than HEAO/RXTE (hard band 2-10 keV).
Figure 26: Photo of the eROSITA telescope structure during the integration phase at MPE, in spring 2012 (image credit: MPE) 45)
Data share policy of the SRG project:
Data Rights and Policies (MPE):
• German eROSITA data are made public after a 2 year proprietary period.
• Periodic data releases envisaged (e.g. 6, 24, 48 months)
• Proprietary data via eROSITA_DE collaboration (consortium)
• Projects/Papers regulated by Working Groups
• Individual External Collaborations
• Group External Collaborations.
Figure 27: The data of the SRG project are evenly shared between IKI and MPE (image credit: MPE)
ART-XC (Astronomical Roentgen Telescope - X-ray Concentrator)
ART-XC is a Russian-led complementary instrument to eROSITA. It is also a 7-module X-ray telescope system that provides higher energy coverage, up to 30 keV (with limited sensitivity above 12 keV).
Table 3: ART-XC collaboration (Ref. 15)
• All-sky X-ray survey in the 6-11 keV energy region with a sensitivity of 3 x 10-13 erg s-1 cm-2 keV-1; discovery in the course of survey at local Universe several thousand new AGNs (Active Galactic Nuclei)
• Study of intrinsically heavily absorbed/Compton thick AGNs (NH ≥ 3 x 1023 cm-2)
• Study of massive nearby galaxie clusters with T ≥ 4 keV in pointing observation mode
• Study heavily obscured galactic X-ray binary systems
• Study broadband spectra of Galactic objects (including binary systems, anomalous pulsars, supernova remnants) up to30 keV, spectroscopy and timing of point sources
• Study non-thermal component in the Galaxy diffuse emission
• Search for cyclotron line features X-ray pulsar spectra.
Instrument: ART-XC will consist of seven independent, but co-aligned, telescope modules with seven corresponding cadmium telluride (CdTe) focal plane detectors. Each will operate over the approximate energy range of 6-30 keV, with an angular resolution of 1 arcmin, a field of view of ~30 arcmin and an energy resolution about 10% at 14 keV. NASA/MSFC (Marshall Space Flight Center) fabricated 4 of the 7 mirror modules, to complement those fabricated by VNIIEF (All-Russian Federal Nuclear Center) in Russia. 48) 49) 50) 51)
Table 4: Performance characteristics of the ART-XC and eROSITA instruments aboard the SRG mission
ART-XC is the smaller one of the two telescopes and has a worse resolution compared to eROSITA. But it works in the range of 5-30 keV and therefore is used for the higher-energetic X-rays. The combination of both telescopes will result in an extremely detailed broadband all sky survey.
Figure 28: The ART-XC Instrument with seven mirror modules and seven focal-plane detectors (image credit: ART-XC collaboration)
Telescope consist of 7 identical co-aligned mirror modules, each nesting 28 mirror shells. Shells were fabricated at the Marshall Space Flight Center and made from nickel-cobalt alloy with iridium coating. The telescope modules have a large field of view (0.3º x 0.3º, 36' diameter), good angular resolution (HPD~ 30" on-axis at 8 keV) and wide energy range from 5 to 30 keV.
Figure 29: A cross section of an ART X-ray mirror module. The inner baffle and the heaters are not shown (image credit: ART-XC collaboration)
Table 5: Overview of ART-XC instrument design parameters
• The X-ray modules are fabricated by the VNIIEF (Russia) and MSFC (USA)
• The NASA-IKI reimbursable agreement has been signed on February 7, 2011 to build 4 flight units
• NASA is to deliver 4 flight modules for the ART-XC instruments by the summer of 2014
• The work at the MSFC has been started on March 24, 2011.
X-ray optics designs:
• Both the VNIIEF and the MSFC designs are based on the single spider scheme
• The shell diameters vary from 50 to 150 mm
• The VNIIEF X-ray module design calls for the mirror shell thickness of 250 µm. The vibration tests for the qualification unit are in progress
• MSFC is exploring the variable thickness option. The design of the ART spider and housing is in progress.
Finding the traces of black holes requires X-ray vision. But unlike visible light, X-rays only reflect off surfaces at glancing angles - as a rock might skip off the surface of a lake. X-ray mirrors must therefore be designed with the reflecting surfaces almost parallel to the incoming X-rays. Just one mirror isn't enough, however, to collect very much X-ray light. To intercept as much light as possible, X-ray telescopes require a series of nearly parallel mirror surfaces. This is accomplished with the use of thin shells of mirrors, nested together like Russian dolls. 52)
- The challenge for ART-XC's mirrors is that high-energy X-ray light reflects at angles that are even more glancing, or close to parallel. As a result, more shells are needed. To collect enough X-ray light, ART-XC has seven sets of 28 nested shells, with special reflective coatings. Each mirror is most efficient at reflecting a particular range of X-ray wavelengths.
- ART-XC's mirrors are electroformed from a nickel-cobalt alloy and coated with ultra-thin layers of reflective iridium coating which are smooth to 0.5 nanometers - about 1/1000 the wavelength of visible light. Researchers at Marshall have been developing and refining this mirror-making technology since the 1990s. SRG provides the first opportunity to use it on an orbiting X-ray observatory.
Figure 30: One of seven mirror modules designed and built by the optics team at NASA's Marshall Space Flight Center in Huntsville, Alabama, for Russia's recently-launched Spectrum X-Gamma mission (image credit: NASA, Emmett Given)
Figure 31: The detectors were designed and manufactured at IKI RAS. They are a semiconductor CdTe double-sided strip detectors which provide both good energy resolution (about 10% above 10 keV) and timing capabilities (image credit: IKI)
Figure 32: Two views of an ART-XC teleccope (image credit: ART-XC consortium)
Figure 33: Illustration of the ART-XC instrument (image credit: ART-XC consortium)
Figure 34: Optical performance requirements of ART-XC and eROSITA (image credit: ART-XC consortium)
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The information compiled and edited in this article was provided by Herbert J. Kramer from his documentation of: "Observation of the Earth and Its Environment: Survey of Missions and Sensors" (Springer Verlag) as well as many other sources after the publication of the 4th edition in 2002. - Comments and corrections to this article are always welcome for further updates (email@example.com).