eROSITA science book: mapping the structure of the energetic universe

By A. Merloni, P. Predehl, W. Becker, H. Böhringer, T. Boller, H. Brunner, M. Brusa, K. Dennerl, M. Freyberg, P. Friedrich and 15 more. 2012

416 citations recorded by the source corpus.

eROSITA is the primary instrument on the Russian SRG mission. In the first four years of scientific operation after its launch, foreseen for 2014, it will perform a deep survey of the entire X-ray sky. In the soft X-ray band (0.5-2 keV), this will be about 20 times more sensitive than the ROSAT all sky survey, while in the hard band (2-10 keV) it will provide the first ever true imaging survey of the sky at those energies. Such a sensitive all-sky survey will revolutionize our view of the high-energy sky, and calls for major efforts in synergic, multi-wavelength wide area surveys in order to fully exploit the scientific potential of the X-ray data. The design-driving science of eROSITA is the detection of very large samples (~10^5 objects) of galaxy clusters out to redshifts z>1, in order to study the large scale structure in the Universe, test and characterize cosmological models including Dark Energy. eROSITA is also expected to yield a sample of around 3 millions Active Galactic Nuclei, including both obscured and un-obscured objects, providing a unique view of the evolution of supermassive black holes within the emerging cosmic structure. The survey will also provide new insights into a wide range of astrophysical phenomena, including accreting binaries, active stars and diffuse emission within the Galaxy, as well as solar system bodies that emit X-rays via the charge exchange process. Finally, such a deep imaging survey at high spectral resolution, with its scanning strategy sensitive to a range of variability timescales from tens of seconds to years, will undoubtedly open up a vast discovery space for the study of rare, unpredicted, or unpredictable high-energy astrophysical phenomena. In this living document we present a comprehensive description of the main scientific goals of the mission, with strong emphasis on the early survey phases.

Subfields: Artificial Intelligence, Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7bf22641ddad3d5ba61f5c8b887fe17fe1334718

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Citations in the corpus

The many flavours of photometric redshifts (2018, background): “This is particular relevant considering that wide or all-sky surveys such as eROSITA [108] in X-ray and EMU [109] in the Radio are expected to detect million of AGN that will be used as cosmological probes and for evolutionary studies.”
Observational probes of cosmic acceleration (2012, background): “…to produce an all-sky catalog of ∼ 105 X-ray selected clusters, with X-ray temperature measurements and resolved profiles for the brighter clusters (Merloni et al., 2012).9 The completion of the Astro2010 Decadal Survey and the Euclid selection by ESA make this an opportune time to review the…”
SDSS-V: Pioneering Panoptic Spectroscopy (2017, background): “…optical spectroscopic measurements (to about iAB < 21.5), including identifications and redshifts, of∼400,000 eROSITA X-ray sources detected in the first 1.5 years of the all sky survey (i.e., those to a 0.5–2 keV flux limit of ∼2.5× 10−14 erg s−1 cm−2; see Figure 8 and Merloni et al. 2012).”
Dynamical vacuum energy in the expanding Universe confronted with observations: a dedicated study (2014, background): “servables can help to break degeneracies between the { 3 { vacuum models and can be especially useful in the context of realistic and future X-ray and Sunyaev-Zeldovich cluster surveys such as eROSITA[40] and SPT[41, 42], as shown in previous work[19, 20]. For other implications of dynamical models ”
Towards a realistic population of simulated galaxy groups and clusters (2013, background): “In the future, large samples of homogeneously analysed and selected X-ray groups will be available through the XXL (Pierre et al. 2011) and eRosita (Merloni et al. 2012) surveys.”
Active galactic nuclei: what’s in a name? (2017, background): “…the order of a milliparsec, as inferred from their rapid variability (e.g. Ulrich et al. 1997), implying high energy densities; (3) strong evolution of their luminosity functions (LFs; e.g. Merloni and Heinz 2013); (4) detectable emission covering the whole electromagnetic spectrum (this review).”
x-cigale: fitting AGN/galaxy SEDs from X-ray to infrared (2020, methodology): “In the future, X-CIGALE can be used to explore deep/wide surveys of, e.g. eROSITA (e.g. Merloni et al. 2012) and Athena (e.g. Nandra et al. 2013).”
The Fermi blazar sequence (2017, background): “On the other hand, with the advent of eROSITA (Merloni et al. 2012), these objects would be detected in X–rays, helping to probe their BL Lac nature.”
The Sloan Digital Sky Survey Quasar Catalog: Fourteenth data release (2017, methodology): “In late 2018, SPIDERS plans to begin targeting sources from the eROSITA instrument on board the Spectrum Roentgen Gamma satellite (Predehl et al. 2010; Merloni et al. 2012).”
The VLT Survey Telescope ATLAS (2015, background): “Such quasar surveys will also complement future programmes such as the X-ray AGN surveys of e-ROSITA (Merloni et al. 2012).”
Obscured Active Galactic Nuclei (2018, background): “The eROSITA mission16 will identify millions of AGN over the whole sky (Merloni et al. 2012), including a significant number of obscured sources (with follow-up spectroscopy from 4MOST), although its ability to probe the complete obscured AGN population will be limited by 2http://desi.lbl.gov/…”
THE COYOTE UNIVERSE EXTENDED: PRECISION EMULATION OF THE MATTER POWER SPECTRUM (2013, background): “In the X-ray the next planned mission is eROSITA (Merloni et al. 2012), which will provide a significant update to results from prior surveys, such as the 400d cluster survey (Vikhlinin et al. 2009).”
Cosmic X-ray surveys of distant active galaxies (2015, background): “In the near term, both eROSITA and ASTRO-H are expected to become operational, with launch dates of 2015–2016. eROSITA (Merloni et al 2012) is a joint Russian–German mission and will provide imaging and spectroscopy over ≈ 0.5–10 keV.”