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Wide Field X-Ray Surveys Wide Field X-ray Telescope (WFXT) Stephen Murray on behalf of The WFXT Team JHU, CfA, MSFC, GSFC, ESO, INAF-Brera, INAF- Bologna, INAF-Trieste, INAF-Capodimonte, U.Naples, U. Trieste, ASI Science Center, … S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years WFXT Collaboration JHU: Stephen S. Murray (PI), Kip Kuntz, U. Michigan: Gus Evrard Riccardo Giacconi, Timothy Heckman, STScI: Kathryn Flanagan, Carol Christian Suvi Gezari U. Chicago: Andrey Kravtsov APL: Hal Weaver, Carey Lisse, Neil Miller, U. Waterloo: Brian McNamara Cheryl Reed ESO: Piero Rosati, Paolo Padovani CfA: Alexey Vikhlinin, William Forman, MPE: Rashid Sunyaev Christine Jones, Andrew Goulding, U. Trieste: Stefano Borgani Paul Reid, Andreas Zezas, U. Naples: Maurizio Paolillo Pepi Fabbiano INAF-Brera: Giovanni Pareschi, MSFC: Martin Weiskopf, Brian Ramsey, Oberto Citterio, Ron Elsner, Steve ODell Gianpiero Tagliaferri, Sergio Campana, GSFC: Andrew Ptak Ginevra Trinchieri, Marta Civitani, MIT: Mark Bautz Alberto Moretti, Anna Wolter Dartmouth: Ryan Hickox INAF-Bologna: Roberto Gilli PSU: Niel Brandt, Eric Feigleson, INAF-Trieste: Paolo Tozzi, Joana Santos, Don Schneider Barbara Sartoris Princeton: Neta Bahcall INAF-Capodimonte: Massimo Della Valle, Stanford: Steve Allen Domitilla de Martino MSU: Megan Donahue, Mark Voit ASI Science Data Center: Paolo Giommi S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Mission Science Goals • Cosmology with Clusters of Galaxies • Dark Energy EoS and its evolution • Growth of structure, deviations from GR • Physics of Clusters of Galaxies • ICM entropy, metalicity enrichment, feedback • AGN Growth and Evolution • Accretion and feedback history of SMBHs • AGN clustering and dark matter halos • The Milky Way and Nearby Galaxies • Hot gas distribution on Milky Way • Star formation rate and X-ray properties S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Science of Future of X-ray Surveys First SMBHs, galaxy/AGN co-evolution, feedback mechanisms, cosmic cycle of baryons, structure formation, precision cosmology - all require: High sensitivity Wide Good angular survey area resolution Can be done with a specific X-ray optical design and modest technological development, ready to be done now S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Enabling Technology is (essentially) in hand • Wide field X-ray optics design is understood • Wide field performance has been demonstrated by Brera/MSFC (‘improved’ manufacturing in development) • Detectors based on MIT Lincoln Lab CCDs that have already been flown (Chandra and Suzaku) May consider newer APS (CMOS) detectors • Spacecraft requirements are far from state-of- the art (roughly 5-10 times less demanding than Chandra) • Photon counting image reconstruction standard for X-ray spatial-spectral detectors S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Beyond eROSITA: WFXT • Three co-aligned telescopes • 5” HEW • 1 degree FoV • CCD camera • ∼10x Chandra effective Chandra-like HEO or area @ 1 keV Sun-Earth L2 Low-earth orbit (550 km @ 6 deg) Robust multiple telescope/ Large field of regard minimizes particle detector system Long observations background S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years WFXT: “SDSS” for X-rays Shallow, Medium and Deep Surveys Dramatic advance over existing/planned missions in combined solid angle/ sensitivity Proven large discovery space XBootes Three (two) surveys •Shallow 15-20,000 deg2 •Medium 3000 deg2 (750 times COSMOS) •Deep 100 deg2 (800 times CDF) GO Program 40% Observing time S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years WFXT Deep Survey = 100 sq deg WFXT Surveys ~800 times solid angle equivalent of Chandra Deep Fields Description of the WFXT Surveys Survey Quantity Shallow Deep Medium Shallow Ω (deg2) 100 3,000 15,000 Exposure 400* ksec 13-20 ksec 2-3 ksec Total Time 1.5 yr 1.5 yr 2.0 yr Medium S (0.5-2 keV) point-like min 4.0x10-17 4.5x10-16 4.0x10-15 erg s-1 cm-2 at 3σ Total AGN Detected ~4.7x105 ~4.4x106 ~7x106 S (0.5-2 keV) extended Deep min 1x10-16 1x10-15 5x10-15 erg s-1 cm-2 at 5σ Total Clusters/Groups ~5x104 ~3x105 ~2x105 * Deep surveys will consist of ~10 x 40 ksec exposures over several years for time variability studies S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Angular resolution HEW= 5“ over the entire FoV • Improve sensitivity for point and extended sources, AGN/cluster/group discernment at any redshift • Minimize source confusion, especially confusion free Deep survey • Efficient identification of optical counterparts, Chandra-like id accuracy (<1” radius error circle, >90% right IDs), essential for 5x106 AGN and 2×105 clusters! • Detect sharp features of the ICM (shocks, cold fronts, cavities) • Resolve cool cores of z>1 clusters (essential for cosmological applications, reliable mass proxy) PSPC HRI ROSAT Lockman Hole survey (25” vs 5” resolution) (Lehmann et al. 2001) S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Figure of Merit: Discovery Speed 2 2 M = (FoV) x (Aeff)/(HEWavg) cm Speed in carrying out large sensitive surveys and identifying distinct sources. Insert shows the figure of merit for survey discovery speed (Grasp/HEW2). WFXT is about 100 times better than any past or planned X-ray mission. Cumulative field of view available at a given angular resolution (HEW) as a function of HEW Wide field design matters!!! for five missions. S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Simulation: one medium survey “tile” Chandra COSMOS- 1.8 Msec (1 sq deg) Elvis 2009 [0.5-2] keV [2-4.5] keV [4.5-7] keV 36 Chandra pointings @ 50 ksec each S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Simulation: one medium survey “tile” Chandra COSMOS- 1.8 Msec (1 sq deg) WFXT – 13 Ksec Elvis 2009 Rosati and Tozzi [0.5-2] keV Bands (keV) [0.5-1] [2-4.5] keV [1.0-2] [4.5-7] keV [2.0-7] 36 Chandra pointings @ 50 ksec each 1 WFXT pointing @ 13 ksec S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Simulation: one medium survey “tile” Chandra COSMOS- 1.8 Msec (1 sq deg) WFXT – 13 Ksec Elvis 2009 Rosati and Tozzi [0.5-2] keV Bands (keV) [0.5-1] [2-4.5] keV [1.0-2] [4.5-7] keV [2.0-7] 36 Chandra pointings @ 50 ksec each 1 WFXT pointing @ 13 ksec WFXT simulation: Same sources as Chandra 5 arc second HEW, not confusion limited ~100 x faster surveys than Chandra S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Simulation: one medium survey “tile” Chandra COSMOS- 1.8 Msec (1 sq deg) WFXT – 13 Ksec Elvis 2009 Rosati and Tozzi AGN counts (Medium + Deep Surveys) With > 400 counts [0.5-2] keV Bands (keV) ~500,000 AGN with >400 cts, with full [0.5-1] [2-4.5] keV [1.0-2] spectral[4.5 -characterization7] keV (obscuration, z, etc.) [2.0-7] 36 Chandra pointings @ 50 ksec each 1 WFXT pointing @ 13 ksec WFXT simulation: Same sources as Chandra 5 arc second HEW, not confusion limited ~100 x faster surveys than Chandra S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years Obscured AGN with WFXT L(2-10 keV) = 6x1044 erg/s z > N thick 1 500 2 270 3 60 4 12 • Pessimistic case assumes an exponential decline towards high-z in the space density of AGN at all luminosities. Norman 2002, Comastri 2011 •Simulated 400 ksec spectrum of CT, high redshift AGN 24 -15 -2 -1 •NH =10 , Γ=1.82, F(2-10 keV)=3x10 erg cm s •EW=1 keV, Centroid to ~2%. •530 counts total •Strong iron line and allows an accurate redshift determination from the X-ray data alone. S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years AGN at z>6 with WFXT • WFXT detects close to 1000 unobscured z>6 QSO’s with more than 400 cts, similar number obscured • Synergistic: Euclid and LSST identify the WFXT sources, WFXT picks out the AGN (especially high-z, obscured) On the right is a plot of the limiting bolometric magnitude versus sky coverage for various surveys. The shaded regions show the number of unobscured AGN at z.6 that would be detected in these surveys, under the assumption that there is a rapid exponential decline in the space density of AGN at all luminosities. WFXT will detect ~1000 high-z unobscured AGN with more than 400 counts (and in fact a similar number of obscured AGN). This complements Euclid and LSST (and WFIRST) in two ways- WFXT identifies the high-z AGN in these surveys and provides directly their redshifts from Fe the Fe line (if present) S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years AGN Clustering Correlation function <=> halo mass & interactions correlation function function correlation separationseparation → → → Radio Clustering on large scales tells us X-ray HALO MASS: clear trends, but still large How is the growth of black holes IRACuncertainties related to the growth of large- log (halomass) scale structure? redshift → S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years AGN Clustering Correlation function <=> halo mass & interactions correlation function function correlation separationseparation → → → Radio Clustering on large scales tells us clear trends, X-ray but still large HALO MASS: clearuncertainties trends, but still large How is the growth of black holes IRACuncertainties related to the growth of large- log (halomass) scale structure? redshift → S. Murray Oct 5, 2012: X-ray Astronomy, the next 50 years AGN Clustering Correlation function <=> halo mass & interactions correlation function function correlation → Radio Clustering on small scales tells us X-ray MERGERS AND INTERACTIONS IRAC Theoretical make different predictions for AGN log (halo mass) clustering but differences can be small we need much better statistics: WFXT redshift → S.
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