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.
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.
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.
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 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.
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 ART-XC instrument is an X-ray grazing-incidence telescope system in an ABRIXAS-type optical configuration
optimized for the survey observational mode of the Spectrum-RG astrophysical mission which is scheduled to be
launched in 2011. ART-XC has two units, each equipped with four identical X-ray multi-shell mirror modules. The
optical axes of the individual mirror modules are not parallel but are separated by several degrees to permit the four
modules to share a single CCD focal plane detector, 1/4 of the area each. The 450-micron-thick pnCCD (similar to the
adjacent eROSITA telescope detector) will allow the detection of
X-ray photons up to 15 keV. The field of view of the
individual mirror module is about 18×18 arcminutes2 and the sensitivity of the ART-XC system for 4 years of survey
will be better than 10-12 erg s-1 cm-2 over the 4-12 keV energy band. This will allow the ART-XC instrument to discover
several thousands new AGNs.
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.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.