eROSITA on SRG

By P. Predehl, R. Andritschke, H. Böhringer, W. Bornemann, H. Bräuninger, H. Brunner, M. Brusa, W. Burkert, V. Burwitz, N. Cappelluti and 46 more. Astronomical Telescopes + Instrumentation, 2010

165 citations recorded by the source corpus.

eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission which is scheduled for launch in late 2012. eROSITA is fully approved and funded by the German Space Agency DLR and the Max-Planck-Society. The instrument development is in phase C/D since fall 2009. The design driving science is the detection 100.000 Clusters of Galaxies up to redshift z ~1.3 in order to study the large scale structure in the Universe and test cosmological models, especially Dark Energy. This will be accomplished by an all-sky survey lasting for four years plus a phase of pointed observations. eROSITA consists of seven Wolter-I telescope modules, each equipped with 54 Wolter-I shells having an outer diameter of 360 mm. This would provide an effective area of ~1500 cm2 at 1.5 keV and an on axis PSF HEW of 15 arcsec resulting in an effective angular resolution of 28 - 30 arcsec, averaged over the field of view. In the focus of each mirror module, a fast frame-store pn-CCD provides a field of view of 1° in diameter.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

THE MULTI-OBJECT, FIBER-FED SPECTROGRAPHS FOR THE SLOAN DIGITAL SKY SURVEY AND THE BARYON OSCILLATION SPECTROSCOPIC SURVEY (2012, methodology): “In a program to follow up x-ray sources in new 0.28 keV data obtained from the extended ROentgen Survey with an Imaging Telescope Array (eROSITA: Predehl et al. 2010), the SPectroscopic IDentification of eROSITA Sources (SPIDERS) survey will follow up 50,000 – 100,000 objects.”
Scaling Properties of a Complete X-ray Selected Galaxy Group Sample (2014, background): “In the near future, eROSITA (e.g., Predehl et al. 2010; Merloni et al. 2012) is expected to detect ∼105 clusters, most of them in the low-mass regime (Pillepich et al. 2012).”
Towards a new generation axion helioscope (2011, methodology): “0−225 0.14−0.54 203 [103, 122] BeppoSAX cone replication 1.85 33−81 0.26−0.62 30 [115] Chandra Wolter I monolithic 10.0 320−600 0.45−0.85 4 [123] eRosita Wolter I replication 1.60 38−180 0.33−1.60 54 [116, 118] HEFT cone seg. glass 6.00 40−120 0.09−0.29 72 [106] NuSTAR cone seg. glass 10.2 54−191 0.”
THE TENTH DATA RELEASE OF THE SLOAN DIGITAL SKY SURVEY: FIRST SPECTROSCOPIC DATA FROM THE SDSS-III APACHE POINT OBSERVATORY GALACTIC EVOLUTION EXPERIMENT (2013, background): “…and constrain cosmological parameters in the critical and largely unexplored redshift range 0.6 < z < 2.1. eBOSS will also obtain spectra of X-ray sources detected by the eROSITA satellite (Predehl et al. 2010), as well as of variable stars and quasars to understand their physical nature.”
Weighing the Giants - I. Weak-lensing masses for 51 massive galaxy clusters: project overview, data analysis methods and cluster images (2012, background): “…the Atacama Cosmology Telescope (ACT, Sehgal et al. 2011), Planck (Planck Collaboration et al. 2011), the Dark Energy Survey (The Dark Energy Survey Collaboration 2005, DES), and eROSITA (Predehl et al. 2010) will find hundreds to many thousands of massive clusters in the redshift range 0.5 . z .”
The SPTpol Extended Cluster Survey (2019, background): “This work will complement the wide-area cluster surveys to be conducted at X-ray (eROSITA; Predehl et al. 2010; Merloni et al. 2012) and optical/IR wavelengths (e.g., LSST, LSST Science Collaboration et al. 2009; Euclid, Euclid Collaboration et al. 2019; WFIRST, Spergel et al. 2015), as well as SZ…”
Multi-messenger astrophysics (2019, background): “2 MeV to > ∼10 GeV and the German eROSITA [91] 0.”