The Wide Field Xray Telescope Andrew Ptak NASAGSFC
- Slides: 38
The Wide Field X-ray Telescope Andrew Ptak (NASA/GSFC) for the WFXT team http: //wfxt. pha. jhu. edu
Why WFXT? The only soft X-ray all-sky survey has been the ROSAT All-Sky Survey (RASS) Chandra and XMM-Newton are not survey instruments e. Rosita is slated to launch in 2017 but has ~ 30” avg. PSF Athena WFI will have 1. 4 -2 m 2 eff. area but will have a 40’ FOV and may only spend ~ 1 year on surveys Brandt & Alexander (2015) We need a dedicated survey mission to cover large areas (> 100 sq. deg. ) with flux depths matched to LSST and WFIRST: WFXT would be the X-ray SDSS
XB oo t es WFXT: The SDSS for X-rays na Athe AGN
Typical X-ray Survey Exposure Maps XMMCOSMOS AEGIS-X XMM-XXL Survey (PI: Pierre) Full XXL area = ~ 50 deg 2 WFXT
e. Rosita Will be launched as part of Russian Spektrum Roentgen Gamma (SRG) satellite to L 2, planned for Feb 2017 Will detect ~ 105 clusters, 106 AGN 27” HEW FOV-averaged spatial resolution 0. 75 deg. FOV effective area ~ 2 X XMM-Newton WFXT
WFXT Key Features Constant PSF (<= 5” HPD) across 1 degree FOV 2 Effective area ~ 15 X Chandra at 1 ke. V (goal 10000 cm ) Bandpass: ~ 0. 4 -7 ke. V Dedicated survey mission, calibrated data products released with no proprietary period Science goals: discovery and characterization of groups and clusters up z~1 -2, evolution of AGN and growth of earliest AGN, star forming galaxies traced up to z>1, halo stars, SNR and compact Galactic objects Will serve as a target finder for future X-ray missions
Grasp = Aeff x FOV measured at 1. 5 ke. V in cm 2 deg 2 Grasp measures survey speed Better angular resolution results in better efficiency and source identification. WFXT Athena e. ROSITA ROSAT XMM Chandra Grasp 5000 -9000 1150 630 900 50 HPD (“) 3 -5 5 27 25 -60 15 -25 1 -5
WFXT Surveys = 3000 X C-COSMOS = 1000 X CDFS
XMM COSMOS survey (2 deg 2) (Cappelluti et al. 2009) XMM - 1. 5 Msec 1 deg
Chandra COSMOS survey (1 deg 2) (Elvis et al. 2009) Chandra - 1. 8 Msec Bands (ke. V) [0. 5 -2] [2 -4. 5] [4. 5 -7]
WFXT simulation (one tile from the medium survey) WFXT - 13 Ksec Bands (ke. V) [0. 5 -1] [1. 0 -2] [2. 0 -7]
The Bullet cluster (z=0. 3, T=14 ke. V) observed with WFXT Deep survey: 400 ksec z=0. 5 z=1. 0 z=1. 5 10’ Joana Santos (INAF, Osservatorio Astrofisico di Arcetri) and the WFXT Team
Survey Spatial Resolution • • • Improve sensitivity for point and extended sources, AGN/cluster/group discernment at any redshift Minimize source confusion, especially in Deep survey Efficient identification of optical counterparts, Chandra-like id accuracy (<1” radius error circle, >90% correct IDs), essential for 5 x 106 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) WFXT
Telescope Design See Pareschi et al. Poster discussing technique to reach WFXT area and Fo. V requirements with a FOVaveraged HPD < 5” The Wolter New Process design with short segments will enable < few arcsec on-axis performance with < 5” over much of the Fo. V WFXT
Segmented Optics Courtesy of W. Zhang (GSFC) Tuesday Jan 20, 2009 WFXT
WFXT Performance Requirements Parameter Requirement Goal Area (1 ke. V) 7, 000 cm 2 10, 000 cm 2 Area (4 ke. V) 2, 000 cm 2 4, 000 cm 2 Field of View 1 deg 2 PSF HPD 5” 3” Pixel Size ~ 1” (24 μm) ~ 1” Energy Band 0. 2 -4 ke. V 0. 1 -6 ke. V Energy Resolution E/ΔE > 10 E/ΔE > 20 Time Resolution <3 s <1 s WFXT
log. N-log. S AGN dominate source counts down to ~ 10 -17 ergs s-1 cm-2 , ~ 10000 sources deg-2 AGN can be selected by finding an Xray counterpart but must be careful at Chandra Deep Field depths -> Total Galaxies Lehmer et al. (2012) WFXT
Quasar Surveys Courtesy of G. Richards
AGN Z>6 Evolution Very wide range of predictions for z>6 AGN: Observations of significant samples at z>6 would constrain the physics of early BH formation disentangling between several scenarios e. g. providing info on mass of BH seeds, accretion mechanisms
AGN and Galaxies WFXT surveys will detect ~ 107 AGN, 105 galaxies Athena would detect ~ 600, 000 AGN in its 1 -year notional survey (Aird et al. 2013)
High-Z AGN • • Simulated 400 ksec spectrum of highly obscured, high redshift AGN NH =1024, Γ=1. 82, EWline =1 ke. V. 530 counts total Strong iron line and allows an accurate redshift determination from the X-ray data alone. • • WFXT Pessimistic case assumes an exponential decline towards high -z in the space density of AGN at all luminosities. Synergistic: Euclid, LSST and WFIRST identify the WFXT sources, WFXT picks out the AGN (especially high-z, obscured)
Synergy with Wide-Area Surveys WFXT is the only X-ray mission that will match, in area and sensitivity, the next generation of wide-area O/IR and radio surveys z=6 Medium Survey QSO z=6 Deep Survey QSO WFXT
Source Identification (Optical) LSST 10 yr (ugrizy) LSST ~1 wk Pan STARRS (gvrizy) WFXT 20, 000 Wide 3000 Medium 100 Deep SDSS (gvriz) CDFS 2 Msec IDs (Luo et al.
Source Identification (NIR) WFIRST HLS 2400 deg 2 Euclid DS 40 deg 2 Euclid, 15000 deg 2 VISTA/Viking, 20000 deg 2 20, 000 Wide 3000 Medium 100 Deep VISTA/VHS, 20000 deg 2 WFXT
The potential of a WFXT survey With 13 ks: ~L* clusters at 13 ksec exposure z=1. 6 detected with ~ 500 counts. With 400 ks: the simulated Spiderweb cluster detected 4 with > 10 counts. Redshifts measured with ~600 counts for the 17 Proto-cluster at z=2. 1 (400 ksec) brightest z=1. 6 clusters in this field Completely X-ray based cluster redshift survey!
The potential of a WFXT survey With 13 ks: ~L* clusters at 13 ksec exposure z=1. 6 detected with ~ 500 counts. With 400 ks: the simulated Spiderweb cluster detected 4 with > 10 counts. Redshifts measured with ~600 counts for the 17 Proto-cluster at z=2. 1 (400 ksec) brightest z=1. 6 clusters in this field Completely X-ray based cluster redshift survey!
Science with WFXT: Clusters of galaxies Not just a cluster counting machine: • • Characterize ICM properties and measure mass proxies for thousands of clusters at z>1. • • Trace the epoch of entropy injection and metal enrichment of the ICM. • • Study the intense dynamics of proto-cluster assembly at z~2. • • Multi-λ synergies: a vast scientific legacy for decades to come • • Path finder follow-up studies with ELTs, Athena X-IFU, ALMA, . . .
Science with WFXT: Clusters of galaxies Not just a cluster counting machine: • • Characterize ICM properties and measure mass proxies for thousands of clusters at z>1. • • Trace the epoch of entropy injection and metal enrichment of the ICM. • • Study the intense dynamics of proto-cluster assembly at z~2. • • Multi-λ synergies: a vast scientific legacy for decades to come • • Path finder follow-up studies with ELTs, Athena X-IFU, ALMA, . . . ROSAT WFXT z>1 XMM, Chandra z>1
WFXT Cluster sample Cluster counts (Medium + Deep Surveys) Detection: 50 -100 counts T measurements: 1500 counts T profiles: 15, 000 counts Temperatures critical to cluster cosmology Profiles, cluster physics, exclude central region Large samples allow study of systematics >3, 000 clusters at z>0. 5, from which z can be measured from Fe line WFXT can reach into early groups
AGN X-ray variability with WFXT The 4 Ms CDFS dataset (courtesy of M. Paolilo) WFXT Deep survey: 400 ks per field, 100 sq. deg - will allow to sample homogeneously broad range of masses and timescales. 30% fluctuations typical in CDFS.
Wide range of science X-ray counterparts to a. LIGO detections GRB afterglows (including orphan / off-axis) Halo stars LMXB and HMXB populations SNR remnants Obscured accretion at high-z Cluster physics: Fe abundance in the ICM, evolution of cool cores in clusters and feedback, low SB regions in the outskirts of clusters Solar System Science Dark Matter search (e. g. , Zandanel et al. 2015) …
WFXT Telescope Layout 3 Telescope Design WFXT was studied by the MSFC Advanced Concepts Office (ACO) in 2012 Optics design optimized for wide-field (e. g. , Burrows, Burg & Giacconi 1992 polynomial perturbation optics design) Mirror: current state-of-the-art technologies are full-shell optics from MSFC and/or Brera (see Pareschi et al. poster) or segmented optics from GSFC Detectors: CCDs baselined in ACO study but more likely would use APS
WFXT Mission Requirements WFXT
Mass and Power WFXT
Mission Parameters o Chandra-like orbit: 16, 000 x 130, 000 km o LEO also would be a consideration for lower background, faster To. O response, impact of LEO orbit assessed in ACO study o Total mass 2200 kg (including propellant and launch vehicle adapter) o Structures sized based on FEM analysis o Reaction wheels sized for 12 deg. / min slew rate o Star trackers + ultra-fine sun sensor give 1” pointing knowledge WFXT
ACO Cost Estimate Component Cost ($M) Spacecraft 163 Instruments 181 Reserves (35%) 120 Operations 77 Total 541 Not including launch vehicle, optics assumed to be at TRL 3 -4 WFXT
Design Trades • Including a retractable grating • Cost ~ $100 -200 M • Would recover highly-rated Astro 2010 highresolution spectroscopy science below 2 ke. V not feasible with Athena • Discussed in NASA PCOS 2011 X-ray Mission Concept Study report • Orbit: LEO vs Chandra-like • Optics Technology: segmented vs full-shell optics WFXT
Conclusions • Current soft X-ray surveys consist of the RASS, shallow serendipitous source / slew surveys (~ hundreds of sq. deg. ), medium-deep surveys (several sq. deg. ), Chandra deep fields (< 1 sq. deg) that probe cluster, AGN and galaxy evolution, AGN absorption, black hole growth, etc. • Current X-ray satellites limited by FOV and/or background, primary pointed missions • e. Rosita will survey soft X-ray sky at ~ 10 X RASS sensitivity, will detect ~ 10 5 clusters, ~ 106 AGN, 103 -4 galaxies • Athena WFI baseline is to spend ~ 1 year surveying <~ 100 deg 2 • WFXT will survey soft X-ray size at ~ 10 -100 X e. Rosita sensitivity (due to higher grasp, sharper and constant PSF, longer exposures) truly matching deep survey sensitivities for LSST, Euclid and WFIRST • will detect ~ 106 clusters, ~ 107 AGN, 104 -5 galaxies • WFXT
- Xray telescope
- Extreme wide shot also known as
- Brązowy ptak wielkości kosa
- Narwiański park narodowy prezentacja
- Zoogeograficzny region australii
- Ptak z ó niewymiennym
- Kachna lyska
- Ptak z rodziny kaczek
- Kuwik ptak
- Indyjski kuglarz
- Pták moa
- Czy dzięcioł zapada w sen zimowy
- Barwny ptak o dłutowatym dziobie
- Wide field infrared survey explorer
- Wide field and planetary camera 2
- Q factor of capacitor
- Magnetic field
- 21lwuy8i6hw -site:youtube.com
- E field h field
- Field dependent vs field independent
- Data types and field properties
- Field dependent vs field independent
- Field dependent definition
- Supine chest xray
- Kub xray
- Xray laser
- Pterigoid plate
- Xray searches
- Xray gladstone
- Aryepiglotic
- Double bond extending conjugation
- Atom xray
- Mary beth sanders
- Rhese view xray
- Omegascans
- Xray laser
- Unilaterallt
- Darkroom tiles
- Talipes calcaneovarus