The Astronomical Roentgen Telescope X-ray Concentrator (ART-XC) is a medium X-ray instrument with operating energy range 4-30 keV which will be launched onboard the Spectrum Roentgen Gamma (SRG) mission. ART-XC consists of seven co-aligned mirror modules coupled with seven focal plane CdTe double-sided strip detectors. The mirror modules were fabricated and calibrated at the NASA Marshall Space Flight Center (MSFC). The Russian Space Research Institute (IKI) developed and tested the X-ray detectors. Flight mirror modules and detector units were integrated into the ART-XC instrument in 2016. For more detailed studies we have used the spare mirror module and spare detector unit. We present some results of the on-ground calibration of the ART-XC spare detector unit without a mirror system and estimation of the detector efficiency.
M. Pavlinsky, V. Levin, V. Akimov, A. Krivchenko, A. Rotin, M. Kuznetsova, I. Lapshov, A. Tkachenko, R. Krivonos, N. Semena, M. Buntov, A. Glushenko, V. Arefiev, A. Yaskovich, S. Grebenev, S. Sazonov, A. Lutovinov, S. Molkov, D. Serbinov, M. Kudelin, T. Drozdova, S. Voronkov, R. Sunyaev, E. Churazov, M. Gilfanov, B. Ramsey, S. O'Dell, J. Kolodziejczak, V. Zavlin, D. Swartz
ART-XC is an X-ray grazing incidence mirror telescopes array onboard the Spectrum-Roentgen-Gamma (SRG) mission, that is currently scheduled for launch in March 2019. This instrument was developed by the Space Research Institute (IKI) and the All-Russian Scientific Research Institute for Experimental Physics (VNIIEF). The NASA Marshall Space Flight Center (MSFC) has developed and fabricated flight X-ray mirror modules. Each mirror module is aligned with a focal plane CdTe double-sided strip detector which will operate over the energy range of 4−30 keV, with an angular resolution of <1′, a field of view of ~0.3 deg2 in double reflection and an expected energy resolution of about 9% at 14 keV. The ART-XC instrument will be used to perform an all-sky survey simultaneously with the other instrument of the SRG mission, eROSITA, operational in a softer energy range 0.3-10 keV. We present an overview of the ARTXC/SRG instrument and an update on the current status of the project.
The Astronomical Roentgen Telescope – X-ray Concentrator (ART-XC) is a hard x-ray instrument with energy response 6–30 keV that will to be launched on board of the Spectrum Roentgen Gamma (SRG) Mission. ART-XC consists of seven co-aligned mirror modules coupled with seven focal plane CdTe double-sided strip detectors. The mirror modules had been fabricated and calibrated at the NASA Marshall Space Flight Center (MSFC). The Russian Space Research Institute (IKI) has developed and tested the X-ray detectors. The joint x-ray calibration of the mirror modules and focal plane detectors was carried out at the IKI test facility. Details of the calibration procedure and an overview of the results are presented here.
The Russian Space Research Institute (IKI) has developed seven flight models and three spare models of the X-ray detectors for the ART-XC/SRG telescope. Each detector situated in the focal plane of ART-XC X-ray optics and includes CdTe die, front-end electronics, data processing, storage and telemetry units. In the Space Research Institute performed a vibration, thermal cycling and thermal vacuum tests of X-ray detectors. During this tests have been studied the leakage current stability, polarization rate, spectroscopic and imaging performance in the working temperature range. The current status of the X-ray detectors development and testing presented.
Spectrum Roentgen Gamma (SRG) is an X-ray astrophysical observatory, developed by Russia in collaboration with Germany. The mission will be launched in 2017 from Baikonur and placed in a 6-month-period halo orbit around L2. The scientific payload consists of two independent telescope arrays – a soft-x-ray survey instrument, eROSITA, being provided by Germany and a medium-x-ray-energy survey instrument ART-XC being developed by Russia. ART-XC will consist of seven independent, but co-aligned, telescope modules. The ART-XC flight mirror modules have been developed and fabricated at the NASA Marshall Space Flight Center (MSFC). Each mirror module will be aligned with a focal plane CdTe double-sided strip detector which will operate over the energy range of 6−30 keV, with an angular resolution of <1′, a field of view of ~34′ and an expected energy resolution of about 12% at 14 keV. The current status of the ART-XC/SRG instrument is presented here.
ART-XC – a medium-x-ray-energy survey instrument of “Spectrum-Roentgen-Gamma” (SRG) project is being developed in Russia under the leadership of the Space Research Institute (IKI). Main requirements to the telescope temperature control system are provided by two key elements – module of seven semiconductor DSSD CdTe detectors which have to operate at the temperature −22.5±2.5 °C to prevent CdTe crystals fast polarization (large polarization time allows to keep detector energy spectral characteristics during continuous 2 – 3 days expositions) and the module of seven mirror systems which have to operate at a temperature 20±2 °C (which is the temperature used in the on Earth mirror systems calibration tests).Thermal control system ART-XC consists of 36 tunable film heaters placed in different places on the telescope structure and controlled according to indications of thermal sensors. The maximum power of each heater is 10 W. There are 21 heaters located on seven mirror systems. Each mirror system case is equipped with two heaters, additional one is located on the mirror system baffle. Seven heaters are placed on detectors. Remaining eight heaters are placed in different telescope parts – one on the protective cover, one on the explosive pin, one under the star tracker, three on the mirror system and star tracker mount plate, one on the detector block mount plate and one on the calibration sources control system block. Thermal control system constantly checks temperature from 36 thermal sensors and regulate the heater’s power supply. There is one passive thermal control element in the telescope – radiator, which is connected to detectors via three heat pipes and cools them down. The QM (qualification model) of ART-XC was manufacture and tested. QM completely corresponds to flight model. Conditions of thermo-vacuum tests were corresponded to real external thermal conditions in flight. The vacuum, cold of space, temperature of mounting planes and shielding by eRosita telescope were reproduced at this test. During the test operating and calibration thermal telescope modes were simulated. Results of the QM thermo-vacuum test are presented in this paper.
Spectrum Roentgen Gamma (SRG) is an X-ray astrophysical observatory, developed by Russia in collaboration with Germany. The mission will be launched in beginning 2017 from Baikonur and placed in a 6-month-period halo orbit around L2. 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 being developed by Russia. ART-XC will consist of seven independent, but co-aligned, telescope modules. The ART-XC flight mirror modules has been developed and fabricated at the NASA Marshall Space Flight Center (MSFC). Each mirror module will be aligned with a focal plane CdTe double-sided strip detector which will operate over the energy range of 6−30 keV, with an angular resolution of <1′, a field of view of ~34′ and an expected energy resolution of about 12% at 14 keV. The current status of the ART-XC/SRG instrument will be present.
The Russian Space Research Institute (IKI) has developed CdTe detectors for the focal plane of the ART-XC/SRG instrument. The CdTe crystal has dimensions about 30 × 30 × 1 mm. Top and bottom sides of the detector each contain 48 strips and a guard ring. The ASIC VA64TA1 is connected to the CdTe crystal by AC-coupling for both DSSD sides. This approach allows one to have the same ground level for both electronic parts and to operate detectors with different leakage currents without reconfiguration of the VA64TA1 chips. One CdTe crystal and two ASICs are integrated with thermal sensors and Peltier cooler in a big hybrid integrated circuit. This detector is hermetically sealed by a cover with beryllium window. For ground testing the detector volume is filled with dry nitrogen. Peltier cooler is used during ground tests only. Together with the hermetic case package it allows us to operate the detector at low temperature during all ART-XC telescope development tests. When in space, the detector cooling will be provided by a radiator and heat pipes. Polarization rate temperature and voltage dependences as well as splitting charges between electrodes are being studied. IKI manufactured dozen X-ray cameras with detectors and supporting electronics for EM, QM and flight model of the ART-XC telescope. Spectroscopic and imaging performances of the detectors were tested on the IKI’s X-Ray Calibration Facility. Current status of the focal plane detector development and testing will be presented.
Spectrum Roentgen Gamma (SRG) is an X-ray astrophysical observatory, developed by Russia in collaboration with Germany. The mission will be launched in March 2016 from Baikonur, by a Zenit rocket with a Fregat booster and placed in a 6-month-period halo orbit around L2. The scientific payload consists of two independent telescopes – a softx- ray survey instrument, eROSITA, being provided by Germany and a medium-x-ray-energy survey instrument ART-XC being developed by Russia. ART-XC will consist of seven independent, but co-aligned, telescope modules. The NASA Marshall Space Flight Center (MSFC) is fabricating the flight mirror modules for the ART-XC/SRG. Each mirror module will be aligned with a focal plane CdTe double-sided strip detector which will operate over the energy range of 6−30 keV, with an angular resolution of <1′, a field of view of ~34′ and an expected energy resolution of about 10% at 14 keV.
Spectrum Roentgen Gamma (SRG) is an X-ray astrophysical observatory, developed by Russia in collaboration with Germany. The mission will be launched in 2014 from Baikonur, by a Zenit rocket with a Fregat booster and placed in a 6-month-period halo orbit around L2. 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 being developed by Russia. ART-XC will consist of seven independent, but co-aligned, telescope modules with seven corresponding cadmium-telluride focal plane detectors. Each will operate over the approximate energy range of 6−30 keV, with an angular resolution of <1′, a field of view of ~30' and an energy resolution about 10% at 14 keV. The NASA Marshall Space Flight Center (MSFC) will fabricate some of the mirror modules, to complement others fabricated by VNIIEF in Russia.
M. Revnivtsev, N. Semena, V. Akimov, V. Levin, D. Serbinov, A. Rotin, M. Kuznetsova, S. Molkov, M. Buntov, V. Tambov, I. Lapshov, E. Gurova, D. Simonenkov, A. Tkachenko, M. Pavlinsky, A. Markov, V. Konoshenko, D. Sibirtsev
MVN (Monitor Vsego Neba) - new small X-ray astronomical experiment, which will be mounted on Russian segment of International Space Station. The main scientific goal for the instrument is the precise measurement of cosmic X-ray background in energy range 6-70 keV, which is important for theories of black hole evolution in the Universe. The ultimate aim of the experiment is to reach the accuracy of the CXB measurements, which will allow us to measure the large scale anisotropy of the Cosmic X-ray Background caused by inhomogeneities of the matter distribution in the local Universe. The MVN instrument is a simple collimated spectrometer, equipped with 4 CdTe pixellated detectors. The field of view of the instrument will be scanning the zenith of the ISS. The accuracy of the instrumental background subtraction, which is the main obstacle for the proposed task, will be provided by a cover, which will periodically block the aperture of detectors. According to our estimates, with not unfavourable radiation environment on orbit of ISS during period of operation of MVN we will be able to measure the CXB surface brightness at different sky directions with accuracy better than 1% after 2 years of the experiment. The planned dates of the experiment is 2013-2016.
Spectrum Roentgen Gamma (SRG) is an X-ray astrophysical observatory, developed by Russia in collaboration with
Germany. The mission will be launched in 2013 from Baikonur, by a Zenit rocket with a Fregat booster and placed in a
6-month-period halo orbit around L2. 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 being
developed by Russia.
ART-XC will consist of seven independent, but co-aligned, telescope modules with seven corresponding cadmiumtelluride
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. The NASA
Marshall Space Flight Center (MSFC) will fabricate some of the mirror modules, to complement others fabricated by
VNIIEF in Russia.
The Spectrum-Roentgen-Gamma mission will be launched in the 2012 year into a L2 orbit with Soyuz launcher and
Fregat buster from Baikonur. The mission will conduct all-sky survey with X-ray mirror telescopes eROSITA and
ART-XC up to 11 keV. It will allow detection of about 100 thousand clusters of galaxies and discovery large scale
Universe structure. It will also discover all obscured accreting Black Holes in nearby galaxies and many (about
3 millions) new distant AGN. Then it is planned to observe dedicated sky regions with high sensitivity and thereafter to
perform follow-up pointed observations of selected sources.
The hard X-ray telescope-concentrator ART-XC on board the Spectrum-X-Gamma X-ray astrophysical observatory
(launching in 2011) is one of the main instruments of the mission. The instrument will be used for an all-sky survey and
then for pointed observations which are planned for the first four and the next three years of the Mission, respectively.
ART-XC will be sensitive in the 4-30 keV energy range and will have an effective area of several hundred square
centimeters at 10 keV. It will have a field of view of about ~28 arcmin, angular resolution better than 1 arcmin and will
be an order of magnitude more sensitive than the current generation of collimated instruments and coded mask telescopes
in the survey mode and a two or three orders of magnitude more sensitive in the pointing mode. With its high sensitivity
in the hard X-ray band and good imaging capabilities, ART-XC will extend the operating energy range of the
observatory (complementing the capabilities of the primary science instrument eROSITA), thus significantly enhancing
the mission both in the all-sky survey over the energy band 4-10 keV and, especially, in pointed observations over the
energy band 4-30 keV. During the 4-year survey, this ART-XC would detect more than ~104 sources over 4-10 keV. For
a 105 second pointed observation, the telescope will provide better than 10 microCrab sensitivity in the 4-20 keV energy
range.
Hard X-ray concentrators based on glass poly-capillary lenses (Kumakhov optics) can bring new flavor for the next generation of astrophysical instruments. We discuss the advantage of such a concentrator for missions such as new Spectrum-X-Gamma, for both scanning and pointing observational modes. Even though an X-ray concentrator has no true imaging capabilities and therefore can not compete with grazing incident mirror instruments, it could be quite useful. For pointing observations the instrument with large area poly-capillary glass concentrator combined with small CZT detector sensitive in the 5-80 keV energy range would significantly improve the faint point sources spectroscopy in hard X-rays. This is of particular interest due to recent INTEGRAL and Swift discovery of the large number of obscured AGNs and comparison of their spectra with the spectrum of the cosmic hard X-ray background. The other important areas to be explored are detection of the Ti-44 line in the supernova remnants and detailed study of high-energy hyrolines in the spectra of X-ray pulsars. The expected parameters of the instrument show that it could be an order of magnitude more sensitive compared to standard coded aperture telescopes. We also explore the potentials of the X-ray concentrator in the scanning mode during the survey phase of the mission.
The methane absorption spectra were obtained behind a shock wave (temperature 1370 K), at 293 K by devised nonlinear IR spectrograph. The spectra calculated on the basis of HITRAN92 data accord with experimental ones. The possibility of temperature determination of methane containing mixture on absorption spectra shape is discussed.
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