eROSITA on SRG

Predehl, P.; Andritschke, Robert; Babyshkin, V.; Becker, Werner; Bornemann, W.; Bräuninger, H.; Brunner, H.; Böller, Thomas; Burwitz, V.; Burkert, Wolfgang; Clerc, N.; Churazov, E.; Coutinho, Diogo; Dennerl, K.; Dwelly, T.; Eder, Josef; Emberger, Valentin; Freyberg, M. J.; Friedrich, Péter; Fürmetz, Maria; Georgakakis, A.; Gilfanov, M.; Großberger, C.; Haberl, F.; Hälker, Olaf; Hartner, Gisela; Kienlin, A. von; Kink, W.; Kreykenbohm, I.; Lamer, G.; Lomakin, I.; Lapshov, I.; Meidinger, Norbert; Merloni, A.; Mican, Benjamin; Müller, S.; Nandra, K.; Pavlinsky, M.; Pfeffermann, E.; Pietschner, Daniel; Robrade, J.; Salvato, M.; Santangelo, A.; Sasaki, M.; Scheuerle, H.; Schmitt, J. H. M. M.; Schwope, A. D.; Sunyaev, R.; Tenzer, C.; Yaroshenko, Valeri; Wilms, J.

doi:10.1117/12.2235092

Cited by 30 publications

(12 citation statements)

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“…Detailed studies of the X-ray properties of Galactic SyXBs can be used as an independent instrument to test the evolution of binary stars in the Galaxy. We expect that the forthcoming all-sky X-ray survey like the SRG-eROSITA mission (Predehl et al 2016(Predehl et al , 2018 will be able to discover a dozen of Galactic SyXBs similar to the objects described in the present paper.…”

Section: Discussionmentioning

confidence: 62%

Wind-accreting symbiotic X-ray binaries

Yungelson

Куранов

Постнов

2019

Monthly Notices of the Royal Astronomical Society

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We present a new model of the population of symbiotic X-ray binaries (SyXBs) that takes into account non-stationary character of quasi-spherical sub-sonic accretion of the red giant's stellar wind onto slowly rotating neutron stars. Updates of the earlier models are given, which include more strict criteria of slow NS rotation for plasma entry into the NS magnetosphere via Rayleigh-Taylor instability, as well as more strict conditions for settling accretion for slow stellar winds, with an account of variations in the specific angular momentum of captured stellar wind in eccentric binaries. These modifications enabled a more adequate description of the distributions of observed systems over binary orbital periods, NS spin periods and their X-ray luminosity in the ∼ 10 32 − 10 36 erg s −1 range and brought their model Galactic number into reasonable agreement with the observed one. Reconciliation of the model and observed orbital periods of SyXBs requires a low efficiency of matter expulsion from common envelopes during the evolution that results in the formation of NS-components of symbiotic X-ray systems.

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Section: Discussionmentioning

confidence: 62%

Wind-accreting symbiotic X-ray binaries

Yungelson

Куранов

Постнов

2019

Monthly Notices of the Royal Astronomical Society

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“…Within the next few years, the eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) mission will detect and measure the position and properties of about 3 million active galactic nuclei (AGN) and 100 000 clusters of galaxies over the full sky (Merloni et al 2012;Predehl et al 2016). Such large numbers of AGN will enable us to compute accurately at least their 1-and 2-point distribution functions over cosmological volumes, and thereby tightly interconnect the evolution of growing supermassive black holes in the overall galaxy population with the large scale structure of dark matter (Fanidakis et al 2011).…”

Section: Introductionmentioning

confidence: 99%

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

Comparat

Merloni

Salvato

et al. 2019

Monthly Notices of the Royal Astronomical Society

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In the context of the upcoming SRG/eROSITA survey, we present an N-body simulation-based mock catalogue for X-ray selected AGN samples. The model reproduces the observed hard X-ray AGN luminosity function (XLF) and the soft X-ray logN-logS from redshift 0 to 6. The XLF is reproduced to within ±5% and the logN-logS to within ±20%. We develop a joint X-ray -optical extinction and classification model. We adopt a set of empirical spectral energy distributions to predict observed magnitudes in the UV, optical and NIR. With the latest eROSITA all sky survey sensitivity model, we create a high-fidelity full-sky mock catalogue of X-ray AGN. It predicts their distributions in right ascension, declination, redshift and fluxes. Using empirical medium resolution optical spectral templates and an exposure time calculator, we find that 1.1×10 6 (4×10 5 ) fiber-hours are needed to follow-up spectroscopically from the ground the detected X-ray AGN with an optical magnitude 21 < r < 22.8 (22.8 < r < 25) with a 4-m (8-m) class multi-object spectroscopic facility. We find that future clustering studies will measure the AGN bias to the percent level at redshift z < 1.2 and should discriminate possible scenarios of galaxy-AGN co-evolution. We predict the accuracy to which the baryon acoustic oscillation standard ruler will be measured using X-ray AGN: better than 3% for AGN between redshift 0.5 to 3 and better than 1% using the Lyα forest of X-ray QSOs discovered between redshift 2 and 3. eROSITA will provide an outstanding set of targets for future galaxy evolution and cosmological studies.

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“…Kavanagh (2020) reviewed the future prospects of the X-ray observations of SFRs, in particular superbubbles and massive clusters, discussed above. In the nearest future two new X-ray observatories will provide new data: Spectrum Roentgen Gamma (SRG) (Pavlinsky et al 2015, Predehl et al 2016, launched in 2019 and The X-Ray Imaging Spectroscopy Mission (XRISM) (Tashiro et al 2018), which launch is planned in 2022. The X-ray telescopes eROSITA and ART-XC aboard the SRG observatory are expected to provide detailed observations of LMC and superbubbles therein and also allow thorough spectral studies of large Galactic superbubbles.…”

Section: X-ray Facilitiesmentioning

confidence: 99%

High-Energy Particles and Radiation in Star-Forming Regions

et al. 2020

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Non-thermal particles and high-energy radiation can play a role in the dynamical processes in star-forming regions and provide an important piece of the multiwavelength observational picture of their structure and components. Powerful stellar winds and supernovae in compact clusters of massive stars and OB associations are known to be favourable sites of high-energy particle acceleration and sources of non-thermal radiation and neutrinos. Namely, young massive stellar clusters are likely sources of the PeV (petaelectronvolt) regime cosmic rays (CRs). They can also be responsible for the cosmic ray composition, e.g., 22 Ne/ 20 Ne anomalous isotopic ratio in CRs. Efficient particle acceleration can be accompanied by super-adiabatic amplification of the fluctuating magnetic fields in the systems converting a part of kinetic power of the winds and supernovae into the magnetic energy through the CR-driven instabilities. The escape and CR propagation in the vicinity of the sources are affected by the non-linear CR feedback. These effects are expected to be important in starburst galaxies, which produce high-energy neutrinos and gamma-rays. We give a brief review of the theoreti-A. M. Bykov

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eROSITA on SRG

Cited by 30 publications

References 0 publications

Wind-accreting symbiotic X-ray binaries

Wind-accreting symbiotic X-ray binaries

Active galactic nuclei and their large-scale structure: an eROSITA mock catalogue

High-Energy Particles and Radiation in Star-Forming Regions

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