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Cairo March 2009
Prospects for Swift studies on NS X-ray binaries
(sorry, no magnetars)
Sergio Campana
Osservatorio astronomico di Brera
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• Burst Alert Telescope (BAT)– CdZnTe detectors (7 keV
energy resolution)– 15-150 keV – 1-4’ localization over 2 sr
field of view
• X-Ray Telescope (XRT)– CCD (140 eV @ 6 keV)– 0.3-10 keV– <5” localization over
24’x24’
• (UVOT) UV/Optical Telescope – Imaging & Grism
spectroscopy– UV to V– Sub-arc localization
• Autonomous re-pointing, 60 - 300 sec
• Onboard and ground triggers
BAT
XRT
Spacecraft
UVOT
BAT
UVOT
XRT
Spacecraft
Swift Mission (Nov. 2004 - ...)
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How does Swift work?
???
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Swift strenghts (I)
Brocksopp et al. 2006
GRO J1655-40
SWIFT J1922.7-1716
Falanga et al. 2007
Multi-wavelength coverage
UVOT
BAT
XRT
XRT INTEGRALRXTE
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Swift’s strengths (II)
BAT monitoring of the X-ray sky (about 100 sources detected daily). BAT is able to discover new X-ray transient and follow them during the brightest part of the outburst. Daily 1 ks observation of the Galactic Center.
1600 s
Krim
m e
t al.
2006
Galactic Center region
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Swift’s strengths (III)Thanks to its scheduling flexibility (one shot) ideal instrument to perform short exposures to identify and to provide an accurate localization of hard X-ray sources (e.g. INTEGRAL, RXTE, Swift-BAT) as well as past and present X-ray missions (RASS, ASCA and XMMSL).
Leyder et al. 2007
Sguera et al. 2007
IGR J18483-0311
INTEGRALROSATSwift-XRT
ISGRI, JEM-XSwift-XRT
IGR J08408-4503
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Swift’s strengths (IV)
Thanks to its scheduling flexibility (multiple shots) ideal instrument to perform (loose) monitoring campaigns.
Campana 2009
23 d
RXS J171824.2-402934
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Swift NS-binaries science
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Strange transients
Wijnands et al. 2009 Consistent with a type I burst from a LMXRB
10 d
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Accreting ms X-ray pulsars
Discovery of the seventh AMXPs SWIFT 1756.9-2508
Krimm et al. 2008
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X-ray transients (AMXP)
Campana et al. 2008
SAX J1808.4-3658
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X-ray transients (classical)
Degenaar et al. 2009
unpublished
EXO 0748-676
Aql X-1
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Monitoring of the Galactic center
Degenaar & Wijnands 2009
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Fast transientsRomano et al. 2007IGR J11215-5952
INTEGRALRomano et al. 2008
P~164.6dP~164.6d
Eccentric orbitEccentric orbit
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Fast transients (II)
Sidoli et al. 2008
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Summary
Swift thanks to:
• Wide energy range UV to hard X
• Flexibility
• Sensitivity (especially for binaries and AXP that are bright objects)
Can in the next few years provide important results in this field
• Detecting (new/rare transient sources, bursts, superbursts)
• Monitoring (evolution of outbursts, long term spectral changes, timing)
• Archiving (long term light curves)
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Swift in perspective
• Monitor X-ray binary transients’ state changes, launch of micro-jet and jets (BAT, XRT, UVOT)
• X-ray burst statistics (BAT)
• Detect in real time and follow superbursts (BAT & XRT follow-up)
•Follow fast transient outbursts (XRT)
• Follow transient outbursts down to quiescence (BAT, XRT & UVOT)
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X-ray burst studies & statistics
Burst rate as a function of flux
Cor
nelis
se e
t al.
2003
Coc
chi e
t al.
2001
Gal
low
ay e
t al.
2004
Eddington-limited burst
Periodic behaviour as a function of flux
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SuperburstsIn
’t Z
and
et a
l. 20
04
Str
ohm
ayer
&
Mar
kwar
dt 2
002
4U 1636-53
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State transitions
Belloni 2007
BH XRB
NS XRB
Homan et al. 2007
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X-ray transients
Aql X-1SAX J1808.4-3658
Campana et al. 2007a
Campana et al. 1998
20022006
mC
rab