X-ray Astronomy X-ray Astronomy in the Near in the Near

FutureFutureSome ThoughtsSome Thoughts

Victoria Kaspi(McGill University)

Weizmann Institute, June 7, 2010

X-ray TargetsX-ray Targets accreting neutron stars, white dwarfsaccreting neutron stars, white dwarfs microquasars & accreting black holesmicroquasars & accreting black holes Rotation-powered pulsars, cooling NSsRotation-powered pulsars, cooling NSs MagnetarsMagnetars AGNAGN Galaxy clustersGalaxy clusters supernova remnantssupernova remnants SupernovaeSupernovae Gamma-ray burstsGamma-ray bursts

X-ray ObservablesX-ray Observables ImagesImages SpectraSpectra TimingTiming MonitoringMonitoring

XTE J1810-197

Current X-ray MissionsCurrent X-ray Missions

NASA ChandraNASA Chandra ESA XMM-NewtonESA XMM-Newton NASA RXTENASA RXTE ESA INTEGRALESA INTEGRAL JAXA/NASA SuzakuJAXA/NASA Suzaku NASA SwiftNASA Swift JAXA/MAXIJAXA/MAXI

Upcoming MissionsUpcoming Missions ASTROSAT (>2011)ASTROSAT (>2011) NuSTAR 2012NuSTAR 2012 eROSITA 2012eROSITA 2012 Astro-H 2014Astro-H 2014 GEMS 2014GEMS 2014 HMXT 20?? (China)HMXT 20?? (China) IXO 2021??IXO 2021?? EXIST, WFXT, AXTAR: proposed...EXIST, WFXT, AXTAR: proposed...

MAXI on ISSMAXI on ISS JAXA/ISS JAXA/ISS 3 0.5-30 keV X-ray slit cameras scan 3 0.5-30 keV X-ray slit cameras scan

entire sky every 96 mins though only entire sky every 96 mins though only 1-2% of sky visible at any time1-2% of sky visible at any time

PSF 1.5 deg, posn det ~6aminPSF 1.5 deg, posn det ~6amin 5sigma 10 mCrab (1 orbit), 5sigma 10 mCrab (1 orbit),

1 mCrab (1 week)1 mCrab (1 week) Not better than ASM...Not better than ASM...

ASTROSATASTROSAT Launch >2011, ISRO w/CSALaunch >2011, ISRO w/CSA 5 instruments: UVIT, LAXPC, SXT, SSM, CzTl5 instruments: UVIT, LAXPC, SXT, SSM, CzTl UVIT:UVIT: 130-180nm, 180-300nm, 320-530nm, twin FOV 28’ diameter 130-180nm, 180-300nm, 320-530nm, twin FOV 28’ diameter

circle, ang res 1.8” UV, 2.5” visible channel, 50cm2 eff area, 10 ms circle, ang res 1.8” UV, 2.5” visible channel, 50cm2 eff area, 10 ms time res, 21time res, 21stst mag (5sigma) in 1800s mag (5sigma) in 1800s For UV channels, grating can be used, sliltless spectroscopy w/res ~100For UV channels, grating can be used, sliltless spectroscopy w/res ~100

SXTSXT: 0.3-8keV, like Swift XRT, CCD focusing 3-4’ HPD, : 0.3-8keV, like Swift XRT, CCD focusing 3-4’ HPD, 0.35 deg FOV, 200 cm2 @ 1 keV 10 uCrab (5sig) in 10ks0.35 deg FOV, 200 cm2 @ 1 keV 10 uCrab (5sig) in 10ks

LAXPC:LAXPC: PCA clone 3-80 keV, 3 PCs, 1degx1deg, 6000 PCA clone 3-80 keV, 3 PCs, 1degx1deg, 6000 cm2 @ 10 keV, 10 us timing, 0.1 mCrab (3sig) in 1kscm2 @ 10 keV, 10 us timing, 0.1 mCrab (3sig) in 1ks

CZTl:CZTl: CDZnTl ~1000cm2 geom area, 10-150 keV, 10 deg CDZnTl ~1000cm2 geom area, 10-150 keV, 10 deg FOV up to 100 keV, 2% res @ 60 keV, 2D coded maskFOV up to 100 keV, 2% res @ 60 keV, 2D coded mask

SSM:SSM: 3 PCs w/1-d coded mask, like ASM 3 PCs w/1-d coded mask, like ASM

NuSTARNuSTAR

SMEX; First focusing of hard X-rays; 10m SMEX; First focusing of hard X-rays; 10m deployabledeployable

CdZnTe pixel detectors; multi-layer coated CdZnTe pixel detectors; multi-layer coated segmented mirros in Wolter I like configsegmented mirros in Wolter I like config

5-80 keV, ang res 43” HPC, 7.5” FWHM5-80 keV, ang res 43” HPC, 7.5” FWHM 13’x13’ FOV but e-dependent; 3’x3’ @ 60 13’x13’ FOV but e-dependent; 3’x3’ @ 60

keVkeV Eres 1.2 keV @ 68 keV; tres 0.1 msEres 1.2 keV @ 68 keV; tres 0.1 ms ~100x pt src sensitivity of INTEGRAL~100x pt src sensitivity of INTEGRAL

eRositaeRosita Extended Roentgen Survey with an Imaging Extended Roentgen Survey with an Imaging

Telescope ArrayTelescope Array Primary instrument on Spectrum-Roentgen-Gamma Primary instrument on Spectrum-Roentgen-Gamma

(SRG)(SRG) Launch 2012 from Baikonur/Soyuz 2 into L2 orbitLaunch 2012 from Baikonur/Soyuz 2 into L2 orbit Imaging all-sky survey 6-30 keV, will last ~4 yrImaging all-sky survey 6-30 keV, will last ~4 yr 7 Wolter I modules, CdTe7 Wolter I modules, CdTe Effective area 1500 cm2 @ 1.5 keVEffective area 1500 cm2 @ 1.5 keV On-axis PSF HEW 15”, FOV ~0.8 deg2On-axis PSF HEW 15”, FOV ~0.8 deg2 See Predehl et al. arXiv:1001.2502See Predehl et al. arXiv:1001.2502 Science: detect 50k-100k galaxy clusters to Science: detect 50k-100k galaxy clusters to

z~1.3 for LSS; complements SPTz~1.3 for LSS; complements SPT

Astro-H (Astro-H (ISAS/ISAS/JAXA/NASAJAXA/NASA))arXiv:0.807.2007v1; PI TakahashiarXiv:0.807.2007v1; PI Takahashi

Launch planned 2014, 550 km 96 minLaunch planned 2014, 550 km 96 min 4 instruments: HXI, SXS, SXI, SGD4 instruments: HXI, SXS, SXI, SGD HXIHXI: 2 HXTs 5-80keV, 12m focal length; 300cm2@30keV; : 2 HXTs 5-80keV, 12m focal length; 300cm2@30keV;

1.9’ (HPD); 9’x9’ FOV1.9’ (HPD); 9’x9’ FOV SXSSXS: 210cm2@6keV, 6m focal, 0.3-10 keV w/7eV energy : 210cm2@6keV, 6m focal, 0.3-10 keV w/7eV energy

resolution, 2.85’ FOV on side, 1.7’ (HPD)resolution, 2.85’ FOV on side, 1.7’ (HPD)at 6keV 60% higher eff area than Suzaku, about same at 1keVat 6keV 60% higher eff area than Suzaku, about same at 1keV

SXI:SXI: 35’x35’, CCDs, 6-m focal length, 1.7’ (HPD), eres 150 35’x35’, CCDs, 6-m focal length, 1.7’ (HPD), eres 150 eV@6keV; 360 cm2 @ 6keVeV@6keV; 360 cm2 @ 6keV

SGDSGD: non-focussing, 10-600 keV, 10x more eff area than : non-focussing, 10-600 keV, 10x more eff area than Suzaku HXD at 300 keV; 2 keV @ 40 keV; 0.55x0.55 deg2 Suzaku HXD at 300 keV; 2 keV @ 40 keV; 0.55x0.55 deg2 FOVFOV

Possible Canadian Space Agency involvement: metrology Possible Canadian Space Agency involvement: metrology systemsystem

GEMS (SMEX, PI Swank)GEMS (SMEX, PI Swank) Gravity and Extreme Magnetism SMEXGravity and Extreme Magnetism SMEX Launch 2014; 2 yrs; Core: 35 srcs in 9 mosLaunch 2014; 2 yrs; Core: 35 srcs in 9 mos 2-10 keV; 3 foil mirrors (4.5m focal length) w/e- 2-10 keV; 3 foil mirrors (4.5m focal length) w/e-

scattering detectors; eff area 510cm2@6keV; scattering detectors; eff area 510cm2@6keV; 12’ FOV; PSF 1.5’12’ FOV; PSF 1.5’

Spacecraft rotates 0.1 rpm to mitigate systematicsSpacecraft rotates 0.1 rpm to mitigate systematics MDP 1% for 20 mCrab in 100 ks; MDP 1% for 20 mCrab in 100 ks; Detector: small gas chamber; X-ray absorbed, e- Detector: small gas chamber; X-ray absorbed, e-

emitted starting in dir related to polarization. emitted starting in dir related to polarization. Measure dir of ionization track as e- movesMeasure dir of ionization track as e- moves

Contrasts w/scattering polarimeter which doesn’t Contrasts w/scattering polarimeter which doesn’t focusfocus

XPOL: Scientific XPOL: Scientific MotivationMotivation

For compact objects imaging generally For compact objects imaging generally useless as source too smalluseless as source too small Exceptions pulsar wind nebulae, Exceptions pulsar wind nebulae,

microquasars, AGNmicroquasars, AGN Compact objects generally studied via:Compact objects generally studied via:

SpectroscopySpectroscopy TimingTiming

X-ray polarimetry adds:X-ray polarimetry adds: Polarization fractionPolarization fraction Polarization position angle Polarization position angle

Energy Dependent

IXO IXO (ESA, NASA, JAXA)(ESA, NASA, JAXA)

3m2@1.25keVkeV, , 0.65m2@6keV; ; 0.015m2@30keV

20 m focal length, 800,000 km around 20 m focal length, 800,000 km around L2L2

Atlas V or Ariane 5 launch, 2021??Atlas V or Ariane 5 launch, 2021?? 6 instruments under study:6 instruments under study:

XMS, XGS, WFI, HXI, HRTS, XPOLXMS, XGS, WFI, HXI, HRTS, XPOL

How Phase Space Being How Phase Space Being Covered?Covered?

Improved imaging, ang res < 1” Improved imaging, ang res < 1” <10 keV: CXO; >10 keV ???<10 keV: CXO; >10 keV ???

High throughput below 10 keVHigh throughput below 10 keV Focusing: IXO; Not focusing: AXTARFocusing: IXO; Not focusing: AXTAR

Wide Field Surveys: Wide Field Surveys: Soft: eROSITA; Hard: WFXT, EXIST; Harder: ACTSoft: eROSITA; Hard: WFXT, EXIST; Harder: ACT

High-res spectrscopy: Astro-H, IXOHigh-res spectrscopy: Astro-H, IXO Hard X-ray imaging: NuSTAR, Astro-HHard X-ray imaging: NuSTAR, Astro-H Multiwavelength: AstrosatMultiwavelength: Astrosat Monitor: ASM, MAXI, SSMMonitor: ASM, MAXI, SSM

What Can be Done?What Can be Done?

Wide-field hard X-ray imaging Wide-field hard X-ray imaging X-ray PolarimetryX-ray Polarimetry Sensitive all-sky monitoringSensitive all-sky monitoring

Argos-X Argos-X (2008 SMEX unfunded proposal; PI Remillard (2008 SMEX unfunded proposal; PI Remillard

MIT)MIT)

3pi sr instantaneous sky coverage by 25 3pi sr instantaneous sky coverage by 25 2D coded-mask cameras w/pixelated Si 2D coded-mask cameras w/pixelated Si detectors (NRL)detectors (NRL)

50% avg live-time of any point in sky50% avg live-time of any point in sky 1.5-28 keV, 600 eV resolution; 122 us 1.5-28 keV, 600 eV resolution; 122 us

time restime res 1-2 amin positions1-2 amin positions 1 mCrab (4sig) for known sources in 1 1 mCrab (4sig) for known sources in 1

day (10x better than ASM/SSM/MAXI)day (10x better than ASM/SSM/MAXI)

X-ACTX-ACTX-ray Astronomy Canadian X-ray Astronomy Canadian

TelescopeTelescopeTHE MISSIONTHE MISSION: X-ray polarimeter (XPOL), all-sky monitor : X-ray polarimeter (XPOL), all-sky monitor

(ASM)(ASM)THE TARGETSTHE TARGETS: black holes, AGN, neutron stars, magnetars, : black holes, AGN, neutron stars, magnetars,

supernova remnants, plerions, blazars, gamma ray bursts, …supernova remnants, plerions, blazars, gamma ray bursts, …THE REASONTHE REASON: promise of major breakthroughs in compact : promise of major breakthroughs in compact

object physics from XPOL; ASM, crucial for monitoring the object physics from XPOL; ASM, crucial for monitoring the volatile high-energy sky, included for small extra costvolatile high-energy sky, included for small extra cost

THE OPPORTUNITYTHE OPPORTUNITY: XPOL neglected over past 30 yr; virgin: XPOL neglected over past 30 yr; virginterritory of which Canada could become leader. Good ASMterritory of which Canada could become leader. Good ASMcrucial to success of GLAST, VERITAS, HESS,… crucial to success of GLAST, VERITAS, HESS,…

WHY CANADA: WHY CANADA: World-class, young, active compact object, SNR, World-class, young, active compact object, SNR, TeV, GR research community in Canada. Small satellite nicheTeV, GR research community in Canada. Small satellite nichepossible; good match for Canadian industry.possible; good match for Canadian industry.

V. Kaspi, D. Hanna; McGill U.

Disk with 75.5° inclination (Conners, Piran and Stark,1980)

Predicted polarization fractions and position angles as a function of energy for disk models near a spinning black hole.

Meszaros et al. 1988

AmplitudeAmplitude

Polarization Fraction

PolarizationAngle

Model predictions of accreting neutron starpolarization propertiesfor different viewinggeometries at differentenergies.

Addressing ConcernsAddressing Concerns Maybe nothing will be polarized.Maybe nothing will be polarized.

If If nothingnothing polarized at few % level, would be polarized at few % level, would be revolutionary…revolutionary…

If we don’t look, we’ll never know.If we don’t look, we’ll never know. A non-detection will teach us nothing.A non-detection will teach us nothing.

Non-detections at few % level for many sources Non-detections at few % level for many sources will be shocking…back to model drawing boardwill be shocking…back to model drawing board

All future models will have to satisfy constraintsAll future models will have to satisfy constraints Physics of polarimetry complicated.Physics of polarimetry complicated.

If we build it, theorists will come.If we build it, theorists will come. Spectroscopy is easy? Yet we want Con-X, Spectroscopy is easy? Yet we want Con-X,

XEUS…XEUS…New observational phase space carrying unique information with potential for high impact!