New results with Swift on Supergiant Fast X-ray Transients 0 1 0 2 n L. Sidoli∗,a P. Romano,b L.Ducci,ac A.Paizis,a S.Vercellone,b G.Cusumano,b V.La a J Parola,b V.Mangano,b J.A.Kennea,d D.N. Burrows,d H.A.Krimm,efg N.Gehrels,g 4 V. Sguera,hi A.Bazzanoi 1 aINAF,IstitutodiAstrofisicaSpazialeeFisicaCosmica, ] ViaE.Bassini15,I-20133Milano,Italy E bINAF,IstitutodiAstrofisicaSpazialeeFisicaCosmica, H ViaU.LaMalfa153,I-90146Palermo,Italy . h cDipartimentodiFisicaeMatematica,UniversitàdegliStudidell’Insubria, p ViaValleggio11,I-22100Como,Italy - o dDepartmentofAstronomyandAstrophysics,PennsylvaniaStateUniversity, r t UniversityPark,PA16802,USA s a eCRESST/GoddardSpaceFlightCenter,Greenbelt,MD,USA [ fUniversitiesSpaceResearchAssociation,Columbia,MD,USA 1 gNASA/GoddardSpaceFlightCenter,Greenbelt,MD20771,USA v hINAF,IstitutodiAstrofisicaSpazialeeFisicaCosmica, 7 ViaGobetti101,I-40129Bologna,Italy 0 4 iINAF,IstitutodiAstrofisicaSpazialeeFisicaCosmica, 2 ViaFossodelCavaliere100,I-00133,Roma,Italy . 1 E-mail: [email protected] 0 0 WereporthereonthemostrecentresultsobtainedonanewclassofHighMassX–rayBinaries, 1 : theSupergiantFastX–rayTransients.SinceOctober2007,wehavebeenperformingamonitoring v i campaign with Swift of four SFXTs (IGR J17544–2916, XTE J1739–302, IGR J16479–4514 X and the X–ray pulsar AX J1841.0-0536)for about 1-2 ks, 2–3 times per week, allowing us to r a derivethepreviouslyunknownlongtermpropertiesofthisnewclassofsources(theirdutycycles, spectralpropertiesinoutburstsandout-of-outbursts,temporalbehaviour).Wealsoreporthereon additionalSwift observationsoftwoSFXTswhicharenotpartofthemonitoring:IGRJ18483– 0311(observedwithSwift/XRTduringawholeorbitalcycle)andSAXJ1818.6–1703(observed forthefirsttimesimultaneouslyintheenergyrange0.3–100keVduringabrightflare). TheExtremesky: SamplingtheUniverseabove10keV October13-172009 Otranto(Lecce)Italy ∗ Speaker. (cid:13)c Copyrightownedbytheauthor(s)underthetermsoftheCreativeCommonsAttribution-NonCommercial-ShareAlikeLicence. http://pos.sissa.it/ NewresultswithSwiftonSupergiantFastX-rayTransients L.Sidoli 1. Supergiant FastX–rayTransients SupergiantFastX-rayTransients(SFXTs)aretransientX–raysourcesinbinarysystemscom- posedofacompactobjectandabluesupergiant companion. Althoughsomeofthemwerediscov- ered before the INTEGRAL satellite launch in 2002, this new class of High Mass X–ray Binaries (HMXBs)wasrecognizedonlyafterseveralnewpeculiarX–raytransientshadbeenfoundbecause oftheGalacticplanesurveyperformedbyINTEGRAL ([18],[10]). Themembersofthisnewclass of sources display apparently short outbursts (as observed with INTEGRAL), characterized by a few hour duration flares and by a high dynamic range (1,000–100,000) between the quiescence (1032 ergs−1)andtheflarepeak(1036–1037 ergs−1). Thespectraareverysimilartothoseofaccretingpulsars,displayingaflatpowerlawspectrum below 10 keV, and a high energy cutoff in the range 10–30 keV (e.g. [26, 20]). This spectral similarity suggests that all SFXTs host a neutron star as compact object, although only in four sources pulsations have been discovered: AX J1841.0−0536 (P ∼ 4.7s, [1]), IGR J11215– spin 5952 (P ∼187s, [27]), IGR J16465–4507 (P ∼228s, [9]) and IGR J18483–0311 (P ∼ spin spin spin 21s, [19]). The distribution of their orbital periods (measured in 5 SFXTs) ranges from 3.3 days (IGRJ16479–4514,[7])to165days(inIGRJ11215–5952,[20,21,13,15]). Periodicallyrecurrent outbursts have been observed in two sources, IGR J11215–5952 [20] and IGR J18483–0311 ([8, 19]),indicative ofoutbursts triggered neartheperiastron passageinahighlyeccentric orbit. The physical mechanism responsible for their peculiar transient X–ray emission is still an open issue (see [23] for a review of the different possibilities). The main proposed mechanisms are related to the structure of the supergiant wind, accreting onto the compact object ([32, 31, 21, 11,4])and/ortotheneutron starmagneticfield(suggested tobemagnetar-like) andits(long)spin period ([6,2]). Thesedifferent scenarii needacomparison withtheSFXTsobservative properties, whichwere,ontheotherhand, largely unknown beforeourmonitoring campaign withSwift/XRT, which started in October 2007. The goal of this campaign was to address several crucial issues, in particular the source status outside the bright flaring activity: are SFXTs in quiescence (no accretion) when they are not in bright flaring activity? or are they still in accretion, but at amuch lowerlevel,toolowtobedetectedbyINTEGRAL?whichisthedutycycleoftheirtransientX-ray emission? The rapid flaring variability together with the association with a massive companion is in- dicative ofthe fact thatSFXTsarewindaccretors, similar tothe classical persistent HMXBswith supergiant companions (like Vela X–1) of the same spectral type. One of the main open issues is the linkbetween these twosubclasses ofmassive binaries. Bothkindofbinaries arecomposed by a compact object (likely aneutron star) and by an OBsupergiant companion withsimilar spectral type. Forthisreason, itwasproposed thatdifferent orbital parameters ([11])couldprobably sepa- ratethetwosubclasses: circular andnarroworbitsinpersistent HMXBs,whilewideandeccentric orbits in SFXTs. On the other hand, the recent discovery of the orbital period of 3.3 days in the SFXT IGRJ16479–4514 [7], is puzzling, because it implies a narrower orbit than that shown by several persistent HMXBs. This seems to suggest that at least in a few members of the class, the orbitisnotthemainparameterwhichseparates thetransient fromthepersistent behaviour. Before our monitoring, the broad band spectra (0.3–100 keV) were obtained only from not simultaneous observations along the whole energy range, thus the suggested spectral similarity 2 NewresultswithSwiftonSupergiantFastX-rayTransients L.Sidoli betweenSFXTsandpersistentlyaccretingX–raypulsarsneededtobetestedbysimultaneouswide band observations. The duration of the outburst phase was unknown, except in the case of the periodic SFXT IGR J11215–5952 [13], where our monitoring with Swift demonstrated that the outburstlastsafewdays,insteadofonlyafewhours(aspreviouslyobservedbyINTEGRAL during the brightest flares). Other crucial properties, like the distribution of the neutron star magnetic fields,thespinandtheorbitalperiods, werecompletely unknow,aswell. 2. Swift contribution Weperformed along-term monitoring campaign with Swift/XRTof asample of four SFXTs, XTE J1739–302, IGR J17544–2619 (the two prototypes of the class), IGR J16479–4514 and the X–ray pulsar AX J1841.0−0536, in order to try to address all these important and open issues. The campaign strategy consists of 2 or 3 XRT pointings per source per week (about ∼1 ks each) to frequently monitor the source status. Given thestructure ofthe observing plan, this monitoring canbeconsideredasacasualsamplingofthesourcelightcurvesataresolution ofabout∼4days. Weweremainly interested inthe monitoring ofthelong-term properties, togetacensus ofallthe outbursts (even the fainter ones, not triggering the Swift/BAT), to monitor the onset of each new outburst andtofollowthewholeoutburst durationwithmorefrequentsubsequent observations (in thisrespecttheSwiftflexibilityisacrucialproperty),andtogettrulysimultaneouswidebandspec- traduringbrightflaringactivity. Ourmonitoringcampaign(whichisstillon-going)hascompletely changed thepreviousviewofthistransient sources([22,14,24,25,16]). Swift observations have demonstrated that SFXTsspend mostof their life still accreting mat- ter even outside bright flaring activity, with an intermediate level of X–ray emission at 1033– 1034 erg s−1, large flux variability (at least one order of magnitude) and an absorbed power law spectrum below 10 keV (photon index of 1–2, or hot black body temperatures of 1–2 keV). Be- sides the bright outbursts (detected also with BAT)and the intermediate level of X–ray emission, several 3s upper limits were also measured, either because the source was faint or due to a very shortexposuretimebecauseoftheinterruptionbyagamma-rayburst. Inordertogetanasuniform as possible subsample for the “non-detections” state, we excluded all observations with a net ex- posurebelow900s. Anexposureof900scorresponds to2–10keVfluxlimitsof∼1–3×10−12 erg cm−2 s−1 (3s ), depending on the source (assuming the best fitabsorbed power law model for the intermediate state of each source). Then, a duty cycle of inactivity (IDC) was defined as the time fraction each source spends undetected down to a flux limit of 1–3×10−12 erg cm−2 s−1 (which means an upper limit to the time spent in quiescence). The IDCs we obtained during the cam- paign with Swift/XRT are the following: 17 % (IGR J16479–4514), 28 % (AX J1841.0–0536), 39%(XTEJ1739–302) and55%(IGRJ17544–2619). Intheeclipsing SFXTIGRJ16479−4514 a main contribution to the IDC comes from the X–ray eclipses, hence the above 17% is in fact an upper limit to the true quiescent time. To summarize, the quiescence in these transients is a rarer state [16]than what previously thought based only on INTEGRAL observations. Thelowest luminosity level we could observe with Swift/XRT, obtained accumulating all data for which no detections wereobtained assingle exposures [16],isreached inXTEJ1739–302 (6×1032 ergs−1, 2–10keV)andinIGRJ17544−2619 (3×1032 ergs−1). 3 NewresultswithSwiftonSupergiantFastX-rayTransients L.Sidoli We observed the broad band simultaneous spectra (XRT together with BAT) during 8 bright flares observed from 3 of the 4 monitored sources. The best fits could be obtained with Comp- tonized models (COMPTT or BMC in XSPEC) orwith anabsorbed flatpower lawmodel with high energy cutoffaround 10–30keV(see[14,24,25]). Thisspectral shape, andinparticular thespec- tral cutoff, iscompatible withaneutron starmagnetic fieldof∼1012 G[3], although nocyclotron lines have been detected yet in these four sources. We found evidence for variable absorbing columndensities, bothinthesamesource(XTEJ1739–302) anddifferentoutbursts andwithinthe sameoutburst,indicativeofdensecloudsofmattercomposingthesupergiantwindpassingtowards thelineofsight. Another crucial finding of our monitoring campaign is that the SFXTsbright and short flares (a few hour long) are part of a longer outburst phase lasting days [24], as already found in the periodic SFXTIGRJ11215–5952 [13]. The first optical/UV observations performed with UVOT simultaneously to our Swift/XRT monitoring of the SFXTsrevealed a possible hint of an UV flaring activity simultaneously to the X–ray bright flares in XTEJ1739−302. However this findings needs confirmation because it is a lessthan3s result[16]. 3. SAX J1818.6–1703 SAXJ1818.6–1703 isaSupergiant FastX-rayTransientassociated withaB0.5Iabtypecom- panion located at 2.1 kpc ([30]). It triggered the Swift/BAT on 2009 May 5 at 14:03:27 UT, and after theBATtrigger, thewhole outburst evolution andthedecline phase could bemonitored with XRT.Thetimeresolvedspectroscopy withXRTdidnotresultinvariabilityofthespectralparame- tersinthe1–10keVrange,withintheuncertainties. Novariabilityintheabsorbingcolumndensity couldbedetectedalongtheoutburst, aswell. SimultaneousBATandXRTspectra,between138and937ssincetheBATtrigger,allowedus to obtain the first broad band X–ray spectrum of this source during an outburst, with a joint fit in the1–10keVand14–150keVenergybandsforXRTandBAT,respectively. ThiswidebandX–ray spectrum, highly absorbed (N ∼5–7×1022 cm−2), is well deconvolved with models like power H lawswithhighenergycutoffs(CUTOFFPL inXSPEC),orComptonizationmodels[COMPTT [29]or the BMCmodel[28]inXSPEC]. AdoptingtheCOMPTT model,thepropertiesoftheComptonizing corona could beconstrained wellwithanelectron temperature kT ∼5–7keV and anoptical depth e t ∼10 (in a spherical geometry). These properties are reminiscent of the X–ray spectral shape of theprototype oftheSFXTclass,XTEJ1739–302. 4. IGRJ18483–0311 The SFXT IGR J18483−0311 is an X–ray pulsar (∼21 s, [19]) and is the second member of the class where periodically recurring outbursts have been discovered with aperiod of 18.55± 0.03days([8,19]),whichisverylikelytheorbitalperiodofthesystem. Itisassociatedwithablue supergiant (B0.5Ia)atadistance of3–4kpc[12]. We monitored with Swift an entire orbital phase (28 days for a total on-source exposure of ∼44ks),starting on2009June11with2ksperday([17]). TheXRTobservations showsahighly 4 NewresultswithSwiftonSupergiantFastX-rayTransients L.Sidoli modulated light curve with two maxima, separated by a time interval consistent with the orbital period of ∼18.5 days. A lower limit of 1200 to the dynamical range can be obtained from the observed light curve. The different duration of the two outburst peaks monitored with Swift is likely resulting from both a different sampling and a high intrinsic X–ray variability. The second peakhasaduration ofseveraldays,aspreviously observed byINTEGRAL[19]. We interpret the modulation of the light curve with the orbital phase as wind accretion along ahighly eccentric orbit. Theseobservations allowtoconstrain thedifferent mechanisms proposed to explain the nature of the new class of SFXTs. Applying the new clumpy wind model for blue supergiants developed by [4] to the evolution of the observed X–ray light curve, we found that, assuminganeccentricityofe=0.4,theX–rayemissionfromthissourcecanbeexplainedinterms of the accretion from a spherically simmetric clumpy wind, composed by clumps with masses ranging from1018 gto5×1021 g(seeDuccietal.,theseproceedings fordetailsofthemodel). 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