DOCSLIB.ORG

Erosita: the Next Generation All Sky X-Ray Survey

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Erosita: the Next Generation All Sky X-Ray Survey eROSITA: The next generation all sky X-ray survey Paul Nandra Max Planck Institute for Extraterrestrial Physics http://www.mpe.mpg.de/eROSITA On behalf of Peter Predehl (eROSITA PI), Andrea Merloni (eROSITA Project Scientist) and the eROSITA collaborationPaul Nandra: eROSITA What is eROSITA? • Next generation all sky X-ray survey • 0.5-2 keV: 30x deeper than ROSAT • 2-10 keV: 100x HEAO-1 • Science driver: 100k clusters (LSS, cosmology) • 3 million AGN including obscured objects • 500,000 coronal stars • Many more (XRB, SNRs, NS, SF gals, E gals, groups etc.) • Instrument parameters: 2 2 • 7 telescopes: 1 deg FOV, 15” PSF, Aeff=1300 cm @1 keV • 7 pnCCD cameras: 0.3-10 keV, E/ΔE=20-50 • Built by consortium led by MPE (PI institute) • Launch aboard Russian SRG mission Paul Nandra: eROSITA eROSITA aboard SRG ART-XC IKI eROSITA MPE Navigator NPO Lavochkin - Launch: Q4 2014 from Baykonour to L2 - 4 yrs: 8 all sky surveys (scanning: 6 rotations/day, 1 degree advance per day) - 3.5 years: pointed observation phase, including ~20% of GTO. 1 AO per year - Proprietary data: shared 50/50 between MPE (Germany) and IKI (Russia) - German (MPE) half: proprietary period maximum 2 yrs - Periodic release of German all-sky data Paul Nandra: eROSITA eROSITA Hardware Replicated Ni-mirror Flight model structure CCD module Paul Nandra: eROSITA Survey Exposure Merloni et al. 2012 ~ 2 ks ~ 20 ks exposure background sensitivity Paul Nandra: eROSITA Optical vs. X-ray surveys COSMOSExample field: COSMOS Optical: X-ray point sources: Extended X-ray: Galaxies AGN Groups and clusters Scoville et al. 2009 Elvis et al. 2009 Hasinger et al. 2009 Elvis et al. 2009 HST Chandra XMM Paul Nandra: eROSITA The X-ray Universe X-rays map “hot-spots” in the evolving Large Scale Structure Diffuse X-ray emi.ng gas traces the massive knots of the cosmic web (Clusters) Point sources (Quasars) signpost the Highly biased populations (e.g. AGN, growth of black holes clusters) can by surveyed over large volumes with very high completeness Paul Nandra: eROSITA Cluster Cosmology WMAP, z = 1100 Millennium Simulation Vikhlinin et al. 2009 ROSAT, z < 0.1 • Clusters of galaxies are the largest gravitational bound structures • Exponential sensitivity to cosmological parameters • Cluster potential well revealed by hot, X-ray emitting baryons • Current samples <100 (well-calibrated) objects originally from ROSAT Paul Nandra: eROSITA Cluster mass function evolution E. Churazov z = 0 z = 0.5 z = 1.4 Number density of massive clusters is very sensitive to cosmology Paul Nandra: eROSITA A complete cluster census E. Churazov 14 eROSITA will detect all the massive clusters in the Universe (M>3 ×10 Msun) Paul Nandra: eROSITA Cosmological Constraints f vs. σ σ8 vs. Ωm NL 8 - X-ray selection - Redshift determination - Mass calibration - Mass function vs. z - Power Spectrum vs. z - fgas vs z DETF FOM: w vs. w w0 vs. Ωm a 0 eROSITA: photz 57 eROSITA: specz 103 Planck+eR: photz 174 Planck+eR: specz 263 Pillepich et al. 2012 Paul Nandra: eROSITA 3 Million eROSITA AGN • AGN Science • (Obscured) accretion history • Host galaxy co-evolution L* • High z AGN (z>6) • Clustering • Accretion Physics • Population studies • X-ray advantages • Bolometric tracer • Obscured AGN • No host contamination Merloni et al. 2012 Paul Nandra: eROSITA 0.5 Million X-ray Stars • Cool Stars (late A to late M-type, magnetic activity, coronae) • Hot Stars (O to early B-type incl. WR Stars, wind shocks) • Variables court. J. Robrade, J. Schmitt Paul Nandra: eROSITA eROSITA /LSST synergy • LSST will provide to eROSITA: • Complete IDs for all eROSITA sources (c.f. SDSS, PS, DES) • Photo-z (with variability correction for type 1 AGN) • eROSITA will provide to LSST: • Locations of the viralised DM haloes (clusters/groups) • Which galaxies are growing their SMBH • Cosmology and Large Scale Structure: • Joint cosmological constraints (clusters, SNe, WL, BAO) • WL vs. X-ray mass calibration • LSS/correlation functions via photo-z • Transients and Variables • Known unknowns, unknowns Paul Nandra: eROSITA eROSITA cluster members RedshiC distribuDon of eROSITA clusters color-coded by the number of galaxies in the magnitude range 18.5<i<20.5 Paul Nandra: eROSITA eROSITA AGN identification - At these relatively bright X- ray flux levels, X-ray positional uncertainty is an issue: test with (degraded XMMCOSMOS) = ~87 (+5)% secure ID at i=24 [~60-70% in VHS] - Expected rAB magnitude distribution of 0.5-2 keV selected AGN in eROSITA surveys CALIBRATED ON XMM-COSMOS CALIBRATED Merloni et al. 2012 Paul Nandra: eROSITA AGN clustering Using photo-z to measure the clustering of AGN in the AEGIS survey Photo-z: CFHTLS Spectra: DEEP2 Mountrichas et al. 2013 Paul Nandra: eROSITA Transients and Variables Cadence map: passes per 6 month survey (8 surveys in total) 10 100 >1000 Paul Nandra: eROSITA Transients and Variables Paul Nandra: eROSITA Spectroscopic followup plan (DE) • Need for spectroscopy: • Accurate z (e.g. clustering) • Photo-z training • Astrophysics (e.g. BH masses, AGN hosts, vel dispersions) • North: AS3/SPIDERS (2014-2019) • Early follow-up ~9000 deg2; >80% completenes (eRASS:4) • >100k unique X-ray selected spectra • South: VISTA/4MOST (2019-2024) • Complete (>80%) followup of eRASS:8 in South • ESO approved phase A, phase B in 2014 Paul Nandra: eROSITA The eROSITA Sky (Skies…) IKI(R) D/R split MPE(D) Nishizawa, Merloni SPIDERS - SDSS-IV Baltimore Paul Nandra: eROSITA 06/2013 eROSITA data rights and policies • eROSITA is a PI instrument • Data split 50% MPE and 50% IKI West/East • German data public after 2 years, periodic releases • Proprietary access via eROSITA_DE consortium • Projects/papers regulated by working groups • Working Groups: • Science: Clusters/Cosmology, AGN, Normal galaxies, Compact objects, Diffuse emission/SNR, Stars, Solar System • Infrastructure: Time Domain, Data analysis and catalogues, Multi- wavelength follow-up, Calibration, Background • Collaboration policy: • Individual External Collaborations (proposal to WGs) • Group External Collaborations (team-to-team MoUs) Paul Nandra: eROSITA THE HOT AND ENERGETIC UNIVERSE: 1. How does ordinary matter assemble into the large scale structures we see today? 2. How do black holes grow and influence the Universe? Athena+ Exploring the Hot and Energetic Universe Primordial stellar populations High redshift galaxy group via GRB afterglow follow up 1 1000 z=7 -1 keV 10 500 10-2 v z=1 vF 200 10-3 Normalised Counts/s/ Normalised -4 10 100 0.5 1 2 0.2 0.5 1 Energy (keV) Energy (keV) Black hole feedback at Obscured black hole in peak of activity in Universe the early Universe 0.1 0.030 0.025 z=8 Athena+ Deep Field 0.020 keV v=0.2c keV Fe Ka 0.015 z=2 0.010 0.01 Nandra, Barret, Barcons, Fabian, den Herder, Piro, Watson et al. 0.005 2013 arXiv 1306.2307 0 Normalised Counts/s/ Normalised Normalised Counts/s/ Normalised -0.005 -0.010 1.5 2.0 2.5 3.0 0.67 0.68 0.69 0.70 Energy (keV) Energy (keV) Black hole growth in the early Universe • What was the growth history of black holes in the epoch of reionization? Aird, Comastri et al. 2013 arXiv1306.2325 The first stars and black holes • When did the first generation of stars explode to form the first seed black holes and disseminate the first metals in the Universe? Gamma Ray Burst at z=7 Jonker, O'Brien et al., 2013 arXiv1306.2336 SUMMARY • eROSITA is the next generation all-sky survey, 30x deeper than ROSAT and 100x HEAO-1 • Mission 2015-2022+, 4 yr sky survey, 3 yr pointed • 100,000 clusters for Stage IV dark energy experiment • 3 Million AGN, 0.5 million stars etc. • LSST synergy: e.g. large-scale structure, transients • New era for X-ray spectroscopy and deep wide field imaging at high z in 2028 via Athena+ http://www.mpe.mpg.de/eROSITA http://the-athena-x-ray-observatory.eu Paul Nandra: eROSITA .
Load more

Recommended publications
  • Detection of Large-Scale X-Ray Bubbles in the Milky Way Halo
    Detection of large-scale X-ray bubbles in the Milky Way halo P. Predehl1†, R. A. Sunyaev2,3†, W. Becker1,4, H. Brunner1, R. Burenin2, A. Bykov5, A. Cherepashchuk6, N. Chugai7, E. Churazov2,3†, V. Doroshenko8, N. Eismont2, M. Freyberg1, M. Gilfanov2,3†, F. Haberl1, I. Khabibullin2,3, R. Krivonos2, C. Maitra1, P. Medvedev2, A. Merloni1†, K. Nandra1†, V. Nazarov2, M. Pavlinsky2, G. Ponti1,9, J. S. Sanders1, M. Sasaki10, S. Sazonov2, A. W. Strong1 & J. Wilms10 1Max-Planck-Institut für Extraterrestrische Physik, Garching, Germany. 2Space Research Institute of the Russian Academy of Sciences, Moscow, Russia. 3Max-Planck-Institut für Astrophysik, Garching, Germany. 4Max-Planck-Institut für Radioastronomie, Bonn, Germany. 5Ioffe Institute, St Petersburg, Russia. 6M. V. Lomonosov Moscow State University, P. K. Sternberg Astronomical Institute, Moscow, Russia. 7Institute of Astronomy, Russian Academy of Sciences, Moscow, Russia. 8Institut für Astronomie und Astrophysik, Tübingen, Germany. 9INAF-Osservatorio Astronomico di Brera, Merate, Italy. 10Dr. Karl-Remeis-Sternwarte Bamberg and ECAP, Universität Erlangen-Nürnberg, Bamberg, Germany. †e-mail: [email protected]; [email protected]; [email protected]; [email protected]; [email protected]; [email protected] The halo of the Milky Way provides a laboratory to study the properties of the shocked hot gas that is predicted by models of galaxy formation. There is observational evidence of energy injection into the halo from past activity in the nucleus of the Milky Way1–4; however, the origin of this energy (star formation or supermassive-black-hole activity) is uncertain, and the causal connection between nuclear structures and large-scale features has not been established unequivocally.
    [Show full text]
  • On the Possibility of Registering X-Ray Flares Related to Fast Radio
    On the possibility of registering X-ray flares related to fast radio bursts with the SRG/eROSITA telescope A.D. Khokhryakova1, D.A. Lyapina1, S.B. Popov1;2;3 1 Department of Physics, Lomonosov Moscow State University 2 Sternberg Astronomical Institute, Lomonosov Moscow State University 3 Higher School of Economics, Moscow March 27, 2019 Abstract In this note we discuss the possibility of detecting the accompanying X-ray emission from sources of fast radio bursts with the eROSITA telescope on- board the Spektr-RG observatory. It is shown that during four years of the survey program about 300 bursts are expected to appear in the field of view of eROSITA. About 1% of them will be detected by ground-based radio tele- scopes. For a total energy release ∼ 1046 ergs depending on the spectral parameters and absorption in the interstellar and intergalactic media, an X- ray flare can be detected from distances from ∼ 1 Mpc (thermal spectrum with kT = 200 keV and strong absorption) up to ∼ 1 Gpc (power-law spec- trum with photon index Γ = 2 and realistic absorption). Thus, eROSITA observations might help to provide important constraints on parameters of arXiv:1903.10991v1 [astro-ph.HE] 26 Mar 2019 sources of fast radio bursts, or may even allow to identify the X-ray tran- sient counterparts, which will help to constrain models of fast radio bursts generation. 1 1 Introduction Fast radio bursts (FRBs) are short (∼ms) bright (peak fluxes up to ∼100 Jy) radio flashes (for a review, see [1]).1 The first event from this class of tran- sients was introduced in 2007 in [2].
    [Show full text]
  • Report of Contributions
    Mapping the X-ray Sky with SRG: First Results from eROSITA and ART-XC Report of Contributions https://events.mpe.mpg.de/e/SRG2020 Mapping the X- … / Report of Contributions eROSITA discovery of a new AGN … Contribution ID : 4 Type : Oral Presentation eROSITA discovery of a new AGN state in 1H0707-495 Tuesday, 17 March 2020 17:45 (15) One of the most prominent AGNs, the ultrasoft Narrow-Line Seyfert 1 Galaxy 1H0707-495, has been observed with eROSITA as one of the first CAL/PV observations on October 13, 2019 for about 60.000 seconds. 1H 0707-495 is a highly variable AGN, with a complex, steep X-ray spectrum, which has been the subject of intense study with XMM-Newton in the past. 1H0707-495 entered an historical low hard flux state, first detected with eROSITA, never seen before in the 20 years of XMM-Newton observations. In addition ultra-soft emission with a variability factor of about 100 has been detected for the first time in the eROSITA light curves. We discuss fast spectral transitions between the cool and a hot phase of the accretion flow in the very strong GR regime as a physical model for 1H0707-495, and provide tests on previously discussed models. Presenter status Senior eROSITA consortium member Primary author(s) : Prof. BOLLER, Thomas (MPE); Prof. NANDRA, Kirpal (MPE Garching); Dr LIU, Teng (MPE Garching); MERLONI, Andrea; Dr DAUSER, Thomas (FAU Nürnberg); Dr RAU, Arne (MPE Garching); Dr BUCHNER, Johannes (MPE); Dr FREYBERG, Michael (MPE) Presenter(s) : Prof. BOLLER, Thomas (MPE) Session Classification : AGN physics, variability, clustering October 3, 2021 Page 1 Mapping the X- … / Report of Contributions X-ray emission from warm-hot int … Contribution ID : 9 Type : Poster X-ray emission from warm-hot intergalactic medium: the role of resonantly scattered cosmic X-ray background We revisit calculations of the X-ray emission from warm-hot intergalactic medium (WHIM) with particular focus on contribution from the resonantly scattered cosmic X-ray background (CXB).
    [Show full text]
  • Erosita – Mapping the X-Ray Universe by P. Predehl
    Astron. Nachr. /AN 335, No. 5, 517 – 522 (2014) / DOI 10.1002/asna.201412059 eROSITA – Mapping the X-ray universe P. Predehl Max-Planck-Institut f¨ur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany Received 2014 Apr 7, accepted 2014 Apr 10 Published online 2014 Jun 2 Key words space vehicles – surveys – telescopes – X-rays: general eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the core instrument on the Russian/German Spektrum-Roentgen-Gamma (SRG) mission which is currently scheduled for launch late 2015/early 2016. eROSITA will perform a deep survey of the entire X-ray sky. In the soft band (0.5–2 keV), it will be about 30 times more sensitive than ROSAT, while in the hard band (2–8 keV) it will provide the first ever true imaging survey of the sky. The design driving science is the detection of large samples of galaxy clusters to redshifts z>1 in order to study the large scale structure in the universe and test cosmological models including dark energy. In addition, eROSITA is expected to yield a sample of a few million active galactic nuclei, including obscured objects, revolutionizing our view of the evolution of supermassive black holes. The survey will also provide new insights into a wide range of astrophysical phenomena, including X-ray binaries, active stars, and diffuse emission within the Galaxy. eROSITA is currently (Jan 2014) in its flight model and calibration phase. All seven flight mirror modules (plus one spare) have been delivered and measured in X-rays. The first camera including the complete electronics has been extensively tested.
    [Show full text]
  • SRGA J124404. 1-632232/SRGU J124403. 8-632231: a New X-Ray
    Astronomy & Astrophysics manuscript no. main ©ESO 2021 June 29, 2021 SRGA J124404.1−632232/SRGU J124403.8−632231: a new X-ray pulsar discovered in the all-sky survey by SRG V.Doroshenko1, R. Staubert1, C. Maitra2, A. Rau2, F. Haberl2, A. Santangelo1, A. Schwope3, J. Wilms4, D.A.H. Buckley5; 6, A. Semena7, I. Mereminskiy7, A. Lutovinov7, M. Gromadzki8, L.J. Townsend5; 9, I.M. Monageng5; 6 1 Institut für Astronomie und Astrophysik, Sand 1, 72076 Tübingen, Germany 2 Max-Planck-Institut für extraterrestrische Physik, Gießenbachstraße 1, 85748 Garching, Germany 3 Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany 4 Dr. Karl Remeis-Sternwarte and Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, Sternwartstr. 7, 96049 Bamberg, Germany 5 South African Astronomical Observatory, PO Box 9, Observatory Rd, Observatory 7935, South Africa 6 Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosch 7701, South Africa 7 Space Research Institute (IKI) of Russian Academy of Sciences, Prosoyuznaya ul 84/32, 117997 Moscow, Russian Federation 8 Astronomical Observatory, University of Warsaw, Al. Ujazdowskie 4, 00-478 Warsaw, Poland 9 Southern African Large Telescope, PO Box 9, Observatory Rd, Observatory 7935, South Africa June 29, 2021 ABSTRACT Ongoing all-sky surveys by the the eROSITA and the Mikhail Pavlinsky ART-XC telescopes on-board the Spec- trum Roentgen Gamma (SRG) mission have already revealed over a million of X-ray sources. One of them, SRGA J124404.1−632232/SRGU J124403.8−632231, was detected as a new source in the third (of the planned eight) consecu- tive X-ray surveys by ART-XC.
    [Show full text]
  • Simultaneous Erosita and TESS Observations of the Ultra-Active Star AB Doradus
    Astronomy & Astrophysics manuscript no. abdor˙eros © ESO 2021 June 29, 2021 Simultaneous eROSITA and TESS observations of the ultra-active star AB Doradus J.H.M.M. Schmitt1, P. Ioannidis1, J. Robrade1, P. Predehl2, S. Czesla1, and P.C. Schneider1 1 Hamburger Sternwarte, Gojenbergsweg 112,D-21029 Hamburg, Germany 2 Max-Planck-Institut fur¨ extraterrestrische Physik, 85748 Garching, Giessenbachstraße, Germany Received / Accepted ABSTRACT We present simultaneous multiwavelength observations of the ultra-active star AB Doradus obtained in the X-ray range with the eROSITA instrument on board the Russian–German Spectrum-Roentgen-Gamma mission (SRG), and in the optical range obtained with the Transiting Exoplanet Survey Satellite (TESS). Thanks to its fortuitous location in the vicinity of the southern ecliptic pole, AB Dor was observed by these missions simultaneously for almost 20 days. With the hitherto obtained data we study the long-term evolution of the X-ray flux from AB Dor and the relation between this observable and the photospheric activity of its spots. Over the 1.5 years of eROSITA survey observations, the “quiescent” X-ray flux of AB Dor has not changed, and furthermore it appears unrelated to the photospheric modulations observed by TESS. During the simultaneous eROSITA and TESS coverage, an extremely large flare event with a total energy release of at least 4 × 1036 erg in the optical was observed, the largest ever seen on AB Dor. We show that the total X-ray output of this flare was far smaller than this, and discuss whether this maybe a general feature of flares on late-type stars.
    [Show full text]
  • Simulating the Erosita Sky Erosita on SRG Erosita Orbit And
    First eROSITA International Conference, Garmisch-Partenkirchen 2011 Max-Planck-Institut für extraterrestrische Physik Download this poster here: http://www.xray.mpe.mpg.de/~hbrunner/Garmisch2011Poster.pdf Simulating the eROSITA sky: exposure, sensitivity, and data reduction Hermann Brunner1, Thomas Boller1, Marcella Brusa1, Fabrizia Guglielmetti1, Christoph Grossberger2, Ingo Kreykenbohm2, Georg Lamer3, Florian Pacaud4, Jan Robrade5, Christian Schmid2, Francesco Pace6, Mauro Roncarelli7 1Max-Planck-Institut für extraterrestrische Physik, Garching, 2Dr. Karl Remeis-Sternwarte und ECAP, 3Leibniz-Institut für Astrophysik, Potsdam, 4Argelander-Institut für Astronomie, 5Hamburger Sternwarte, 6Institute of Cosmology & Gravitation, University of Portsmouth, 7Dipartimento di Astronomico, Università di Bologna eROSITA on SRG All-sky survey sensitivity eROSITA (extended Roentgen Survey with an Imaging Telescope Array) is the primary instrument on the Russian Spektrum-Roentgen-Gamma (SRG) mission, scheduled for launch in 2013. eROSITA consists of Effective area on axis 15´Background off-axis 30´off-axis seven Wolter-I telescope modules, each of which is equipped with 54 mirror shells with an outer diameter o ) 2 2 of 36 cm and a fast frame-store pn-CCD, resulting in a field-of-view (1 diameter) averaged PSF of 25´´-30´´ - 1 keV (cm HEW (on-axis: 15´´ HEW) and an effective area of 1500 cm2 at 1.5 keV. eROSITA/SRG will perform a four arcmin area 1 year long all-sky survey, to be followed be several years of pointed observations (Predehl et al. 2010). - keV 1 - s effective More info on eROSITA: http://www.mpe.mpg.de/erosita/ 4 keV axis - counts n o eROSITA orbit and scanning strategy 7 keV Energy (keV) Energy (keV) Orbit: eROSITA/SRG will be placed in an Averaged all-sky survey PSF (examples) L2 orbit with a semi-major axis of about 1 million km and an orbital period of about 6 months.
    [Show full text]
  • Arxiv:2007.07969V3 [Astro-Ph.CO] 22 Mar 2021
    INR-TH-2020-032 Towards Testing Sterile Neutrino Dark Matter with Spectrum-Roentgen-Gamma Mission V. V. Barinov,1, 2, ∗ R. A. Burenin,3, 4, y D. S. Gorbunov,2, 5, z and R. A. Krivonos3, x 1Physics Department, M. V. Lomonosov Moscow State University, Leninskie Gory, Moscow 119991, Russia 2Institute for Nuclear Research of the Russian Academy of Sciences, Moscow 117312, Russia 3Space Research Institute of the Russian Academy of Sciences, Moscow 117997, Russia 4National Research University Higher School of Economics, Moscow 101000, Russia 5Moscow Institute of Physics and Technology, Dolgoprudny 141700, Russia We investigate the prospects of the SRG mission in searches for the keV-scale mass sterile neutrino dark matter radiatively decaying into active neutrino and photon. The ongoing all-sky X-ray survey of the SRG space observatory with data acquired by the ART-XC and eROSITA telescopes can provide a possibility to fully explore the resonant production mechanism of the dark matter sterile neutrino, which exploits the lepton asymmetry in the primordial plasma consistent with cosmological limits from the Big Bang Nucleosynthesis. In particular, it is shown that at the end of the four year all-sky survey, the sensitivity of the eROSITA telescope near the 3.5 keV line signal reported earlier can be comparable to that of the XMM -Newton with all collected data, which will allow one to carry out another independent study of the possible sterile neutrino decay signal in this area. In the energy range below ≈ 2:4 keV, the expected constraints on the model parameters can be significantly stronger than those obtained with XMM -Newton.
    [Show full text]
  • 4MOST — 4-Metre Multi-Object Spectroscopic Telescope
    Telescopes and Instrumentation 4MOST — 4-metre Multi-Object Spectroscopic Telescope Roelof de Jong1 enough to detect chemical and kinematic metal­poor stars to constrain early gal­ substructure in the stellar halo, bulge axy formation and the nature of the first and thin and thick discs of the Milky Way, stellar generations in the Universe. 1 Leibniz­Institut für Astrophysik Potsdam and enough wavelength coverage (> 1.5 (AIP), Germany octave) to secure velocities of extra- eROSITA (extended ROentgen Survey galactic objects over a large range in red­ with an Imaging Telescope Array, Predehl shift. Such an exceptional instrument et al., 2010) will perform all­sky X­ray sur­ Team members: enables many science goals, but our veys in the years 2013 to 2017 to a limit­ 1 2 2 Svend Bauer , Gurvan Bazin , Ralf Bender , Hans design is especially intended to comple­ ing depth that is a factor 30 deeper than Böhringer3, Corrado Boeche1, Thomas Boller3, Angela Bongiorno3, Piercarlo Bonifacio4, Marcella ment two key all­sky, space­based ob ­ the ROSAT all­sky survey, and with Brusa3, Vadim Burwitz3, Elisabetta Caffau5, Art servatories of prime European interest, broader energy coverage, better spectral Carlson2, Cristina Chiappini1, Norbert Christlieb5, Gaia and eROSITA. Such a facility has resolution and better spatial resolution 4 6 1 Mathieu Cohen , Gavin Dalton , Harry Enke , been identified as of critical importance in (see Figure 3). We will use 4MOST to Carmen Feiz5, Sofia Feltzing7, Patrick François4, Eva Grebel5, Frank Grupp2, Francois Hammer4, Roger a number of recent European strategic survey the > 50 000 southern X-ray gal­ Haynes1, Jochen Heidt5, Amina Helmi8, Achim documents (Bode et al., 2008; de Zeeuw axy clusters that will be discovered by Hess2, Ulrich Hopp3, Andreas Kelz1, Andreas Korn9, & Molster, 2007; Drew et al., 2010; Turon eROSITA, measuring 3–30 galaxies in 10 4 10 Mike Irwin , Pascal Jagourel , Dave King , Gabby et al., 2008) and forms the perfect com­ each cluster.
    [Show full text]
  • All Sky X-‐Ray Survey
    PLANCK B&E workshop, SPEKTR - RG Caltech eRosita July 22, 2016 SPEKTR-RENTGEN-GAMMA (eRosita and ART-XC) all sky X-Ray survey ART-XC Rashid Sunyaev Max-Planck Instut fuer Astrophysik Space Research Instute (IKI), Moscow SRG Spektr-Roentgen-Gamma (SRG) eROSITA ART-XC Navigator plaorm Lavochkin industry ROSKOSMOS Fregat-SB Booster Space Research InsMtute (IKI), Moscow 2 SRG September 25, 2017 (TBC) L2 Parking orbit Injection into parking orbit with Zenit LV ΔV2 ΔV1 st Fregat 2nd Fregat 1 burn burn M.N. Pavlinsky SRG Ground control stations 4 SRG Radio-visibility 64 m 70 m M.N. Pavlinsky SRG No. Description Value S/C 1 Launch date 2017 2 Launch site Baikonur “Zenit-2SB” 3 Launch vehicles - “Fregat-SB” 4 Operational orbit L2 point 5 Active lifetime 7,5 years 6 S/C dry mass 2267 kg 7 Payload 1228 kg 8 S/C wet mass 2647 kg Radio line frequency 9 X range Data Transmission 512 Кbit/ 10 Rate sec Payload power 11 680 W consumption M.N. Pavlinsky SRG -Launch: Q4 2017 from Baykonour, Kazakhstan (Zenit+Fregat) - eROSITA delivery to Russia: October 25, 2016 - ART-XC delivery to Lavochkin industry: October 5, 2016 1. Three months – flight to L2, perfomance verificaon and calibraon of payload. 2. 4 years – 8 all sky surveys, (scanning mode: 6 rotations/day). 3. 3 years – follow-up pointed observaMons of a selecMon of the most interesng galaxy clusters, AGNs and other objects discovered by SRG. 7 SRG The S/C rotaon axis is always pointed between the Sun and the Earth to ensure that the Earth is always within the beam paern of the spacecra medium gain antenna.
    [Show full text]
  • X-Raying the Sco-Cen OB Association: the Low-Mass Stellar Population Revealed by Erosita J
    Astronomy & Astrophysics manuscript no. sco_cen_erass ©ESO 2021 June 29, 2021 X-raying the Sco-Cen OB association: The low-mass stellar population revealed by eROSITA J. H. M. M. Schmitt1, S. Czesla1, S. Freund1, J. Robrade1, P.C. Schneider1 Hamburger Sternwarte, Universität Hamburg, Gojenbergsweg 112, 21029 Hamburg, Germany e-mail: [email protected] Received . ; accepted . ABSTRACT We present the results of the first X-ray all-sky survey (eRASS1) performed by the eROSITA instrument on board the Spectrum- Roentgen-Gamma (SRG) observatory of the Sco-Cen OB association. Bona fide Sco-Cen member stars are young and are therefore expected to emit X-rays at the saturation level. The sensitivity limit of eRASS1 makes these stars detectable down to about a tenth of a solar mass. By cross-correlating the eRASS1 source catalog with the Gaia EDR3 catalog, we arrive at a complete identification of the stellar (i.e., coronal) source content of eROSITA in the Sco-Cen association, and in particular obtain for the first time a 3D view of the detected stellar X-ray sources. Focusing on the low-mass population and placing the optical counterparts identified in this way in a color-magnitude diagram, we can isolate the young stars out of the detected X-ray sources and obtain age estimates of the various Sco-Cen populations. A joint analysis of the 2D and 3D space motions, the latter being available only for a smaller subset of the detected stellar X-ray sources, reveals that the space motions of the selected population show a high degree of parallelism, but there is also an additional population of young, X-ray emitting and essentially cospatial stars that appears to be more diffuse in velocity space.
    [Show full text]
  • Spektr-RG All-Sky Survey Will Be a Major Step Forward for X-Ray Astronomy, Which Celebrated Its 50Th Anniversary a Few Years Ago
    CONTEXT The Spektr-RG all-sky survey will be a major step forward for X-ray astronomy, which celebrated its 50th anniversary a few years ago. 1962. Professor Riccardo Giacconi and his team are the first to identify X-ray emission originating from outside the Solar system (a neutron star dubbed Sco X-1). In 2002, he is awarded the Nobel Prize in Physics for this feat and the following discoveries of distant X-ray sources. 1970–1973. The first X-ray all-sky survey in the 2–20 keV energy band is carried out by the Uhuru space observatory (NASA). It discovers more than 300 X-ray sources in our Milky Way and beyond. 1977–1979. An even more sensitive survey is carried out by the HEAO-1 (NASA) space observatory at energies from 0.25 to 180 keV. 1989-1998. Over the initial four years of directed observations, the Granat astrophysical observatory (USSR) observes many galactic and extra-galactic X-ray sources with emphasis on the deep imaging of the Center of our Galaxy in the hard (40-150 keV) and soft (4-20 keV) X-ray ranges. Unique maps of the Galactic Center in X- and gamma- rays are created; black holes, neutron stars and the first microquasar are discovered. Then Granat carries out a sensitive all-sky survey in the 40 to 200 keV energy band. 1990–1999. In its first six months of operation the ROSAT space observatory (DLR, NASA) performs a deep all-sky survey in the soft X-ray band (0.1–2.4 keV).
    [Show full text]