The Swift Supergiant Fast X-ray Transients Project
a SFXT facebook Group
Come meet us at the:
Swift Science Planning Meeting (P. Romano, October 27-30, 2013, PSU)
The Swift SFXT Project
Supergiant Fast X-ray Transients (SFXTs) are a class of High Mass X-ray Binaries (HMXBs)
associated with OB supergiants
and characterized by show short flares (a few hours, as observed with INTEGRAL;
Negueruela et al., 2005, ESA SP-604, 165; Sguera et al, 2006, ApJ, 646, 452).
These sources display short, sporadic and bright flares reaching
a peak luminosity of a few 1036 erg s-1.
Their quiescent level
is at about 1032 erg s-1,
thus making SFXTs a class of transients with a large dynamic range (about 103--5).
Our activity has been following several lines.
We studied IGR J11215-5952 which, in 2007, was the only SFXT to show periodic outbursts
with a period of 329 days. We organized a campaign to collect data with
to follow the predicted outburst around February 9, 2007.
We have been following this source since, with Swift
GI (Cycle 4)
To characterize the properties of SFXTs on
timescales of months (e.g. outburst recurrence and the quiescent level),
we have performed a monitoring campaign (between October 2007 and November 2009)
with Swift of four SFXTs:
IGR J17544-2619, and
We have been monitoring the activity of IGR J08408-4503, IGR J18483-0311,
and the candidate SFXT IGR J16418-4532.
We obtained ToO triggers for the whole sample of SFXTs through the Swift GI
and Cycle 6)
and activated it for SAX J1818.6-1703 on
2009 May 6
and for Swift J164449.31573451 (Burrows et al 2011, Nature, 476, 421), which was initially thought to be a
new SFXT discovered by Swift, on 2011 March 28.
The periodic IGR J11215-5952 (2007-2011)
IGR J11215-5952 is one of the only two SFXT to date which displays accertained periodic flares
with a period of 329 days as determined based on INTEGRAL data.
data have demonstrated that the true outburst period is about 165 days
(Romano et al. ATel 1151
Sidoli et al 2007, A&A, 476, 1307
Romano et al., 2008, ATel, 1444
Romano et al 2009, ApJ, 696, 2068
Our data sample includes:
The Swift monitoring during the 2007 February outburst proposed,
thanks to the predictable behavior of the recurrent outbursts,
to study the 5th outburst (February 9) @ P=329d
(Romano et al., 2007, A&A, 469, L5).
This represents the most complete monitoring campaign of an outburst from a SFXT and
constitutes a unique data-set for an outburst of a SFXT, thanks to the combination
of sensitivity and time coverage.
The campaigns lasted 23 days for a total on-source exposure of ~73ks
and allowed us to study IGR J11215-5952 from outburst onset to
almost quiescence showing that it reached LX ~1036 erg s-1
displaying a typical dynamic range ~103 and a hard spectrum.
These observations demonstrated that the
accretion phase during the bright flare lasts longer than
previously thought: a few days instead of hours, with only the brightest phase
lasting less than one day, and being characterized by a large variability with several flares
lasting from a few minutes to a few hours
(Romano et al., 2007, A&A, 469, L5).
Simultaneous ToO observations with XMM (23 ks) and INTEGRAL (101 pointing of 2900s each)
were performed (Sidoli, et al., 2007, A&A, 476, 1307).
These allowed us to propose an alternative hypothesis for the outburst mechanism in SFXTs, linked
to the possible presence of a second wind component, in the form of an equatorial disc from the supergiant donor.
The Swift monitoring during 2007 July to study the
following 'apastron' @P/2, with a ToO for
1.5ks-2.5ks/day from June 5 to July 31, 17 ks on-source time.
A new, unexpected outburst was observed
(Romano et al. ATel 1151).
The spectral fits and energetics are fully consistent with the ones observed
during the periastron outburst
(Sidoli, et al., 2007, A&A, 476, 1307).
The Swift 2008 March ToO observations to study the P/4.
No emission observed down to a 3sigma upper limit of 9.1x10-13 erg cm-2 s-1
(photon index=1 and NH=1x1022 cm-2). We could exclude that the period is 165/2 days
(Romano et al., 2008, ATel, 1444).
The Swift 2008 June monitoring.
The properties of the rise to this new outburst and the comparison with the
previous outbursts allow us to suggest that the true orbital period of
IGR J11215-5952 is very likely 164.6 days, and that the orbit is eccentric, with the
different outbursts produced at the periastron passage, when the neutron star
crosses the inclined equatorial wind from the supergiant companion.
(Figure 1, Romano et al., 2009, ApJ, 696, 2068).
Figure 1. XRT light curves of the 2007 February 9 `periastron'
outburst (light gray filled circles), with superimposed the 2007 July 24 `apastron' outburst
(dark gray empty diamonds), and the 2008 June 16 `apastron' outburst (orange empty squares),
folded with a period of 164.6 days. The time is relative to the peak of the 2007 February 9 outburst.
Adapted from Romano et al., 2009, ApJ, 696, 2068.
The Swift 2009 October observations.
We observed the sources for a total of about 5 ks on 2009 October 23
(Esposito et al., 2009, ATel 2257;
Romano et al., 2011, POS, Texas 2010, 117)
and 2009 October 24.
The Swift 2011 March observations.
We observed the sources for a total of about 2.3 ks on 2011 March 1 and 2
(Romano et al., 2011, ATel 3200;
Romano et al., 2011, Procs. Fermi Symposium).
Monitoring 4 SFXTs with Swift (October 2007 - November 2009)
During the first year of monitoring we collected a total of 330 Swift
as part of our program, for a total net XRT exposure of about 363 ks accumulated
on IGR J16479-4514, XTE J1739-302, IGR J17544-2619, AX J1841.0-0536.
We detect a low level X-ray activity in all four SFXTs which demonstrates that these
transient sources accrete matter even outside their outbursts
(Sidoli et al. 2008, ApJ 687, 1230, Paper I).
This fainter X-ray activity
is composed of many flares with a large flux variability, on timescales of thousands of seconds.
The light curve variability is also evident on larger timescales of days, weeks and months,
with a dynamic range of more than one order of magnitude in all four SFXTs.
The X-ray spectra are typically hard, with an average 2-10 keV luminosity during this monitoring
of about 1033-34 erg s-1.
Our monitoring demonstrates that these transients spend
most of the time accreting matter, although at
a much lower level (about 100-1000 times lower)
than during the bright flares, and that the ``true quiescence''
is probably a very rare state.
We observed the first broad-band simultaneous spectra
(0.3-150 keV) of three SFXTs:
IGR J16479-4514 (Figure 2;
Romano et al. 2008, ApJ, 680, L137, Paper II)
the prototypes XTE J1739-302 and IGR J17544-2619
(Sidoli et al., 2009, ApJ, 690, 120, Paper III;
Sidoli et al., 2009, MNRAS, 397, 1528, Paper IV).
We have shown that they can be fit with models
traditionally adopted to fit accreting neutron stars (absorbed cutoff
power laws), even in the objects where proof of the presence of a neutron star
(from a spin period) is not available.
There are considerable differences in the
behaviour of the absorbing column among the examined cases.
Swift has allowed the possibility to give SFXTs non serendipitous attention throughout all phases of their life.
In Romano et al. (2009, MNRAS, 399, 2021, paper V)
we present our results based on the first year of intense Swift monitoring of four
SFXTs, IGR J16479-4514, XTE J1739-302, IGR J17544-2619 and AX J1841.0-0536.
We obtain the first assessment of how long each source spends in each state using a systematic monitoring with a sensitive instrument.
The duty-cycle of inactivity is 17, 28, 39, 55% (5% uncertainty), for IGR J16479-4514, AX J1841.0-0536, XTE J1739-302, and IGR J17544-2619,
respectively, so that true quiescence is a rare state. This demonstrates that these transients accrete matter throughout their
life at different rates. AX J1841.0-0536 is the only source which has not undergone a bright outburst during our campaign.
Although individual sources behave somewhat differently, common X-ray characteristics of this class are emerging such as outburst
lengths well in excess of hours, with a multiple peaked structure.
A high dynamic range (including bright outbursts) of 4 orders of magnitude has been observed.
We performed out-of-outburst intensity-based spectroscopy.
We also present the UVOT data of these sources.
Figure 3. Light curves of the outbursts of SFXTs followed by Swift/XRT
referred to their respective triggers.
We show the 2005 outburst of IGR J16479-4514
(Sidoli et al. 2008, ApJ 687, 1230),
which is more complete than the one observed in 2008
(Romano et al. 2008, ApJ, 680, L137).
The IGR J11215-5952 light curve has an arbitrary start time, since
the source did not trigger the BAT (the observations were obtained as a ToO;
et al., 2007, A&AL, 469, L5 ).
The data on XTE J1739-302 and IGR J17544-2619 are presented in
Sidoli et al., 2009, ApJ, 690, 120.
The bottom plot shows the outburst from XTE J1739-302 that occurred
on 2008 August 13.
Note that where no data are plotted, no data were collected.
For clarity, we drew dashed vertical lines to mark each day (up to one week) since the trigger.
From Sidoli et al. 2008,
PoS (Integral08) 084.
During the second year we monitored IGR J16479-4514, XTE J1739-302, IGR J17544-2619,
and collected a 228 more Swift observations for a total net XRT exposure of about 243 ks.
In Romano et al.
(2011, MNRAS, 410, 1825, paper VI)
we present our results. We confirm our findings on the inactivity duty cycle, and by considering our monitoring
as a casual sampling of the X-ray light curves, we infer that the time these sources spend in bright
outbursts is between 3 and 5% of the total. The most probable X-ray flux for these sources
is about 1-2x10-11 erg cm-2 s-1 (2-10 keV, unabsorbed), corresponding to luminosities in
the order of a few 1033 to a few 1034 erg s-1
(two orders of magnitude lower than the bright
Variability in the X-ray flux is observed at all timescales and intensity ranges we can probe.
Superimposed on the day-to-day variability is intra-day flaring which involves flux variations
up to one order of magnitude that can occur down to timescales as short as 1 ks, and which can be
naturally explained by the accretion of single clumps composing the donor wind with masses
|Figure 2. Spectroscopy of the 2008 March 19 outburst of IGR J16479-4514.
Top: data from the second BAT observation (black empty circles)
and simultaneous XRT/WT data (red filled circles) fit with an absorbed power
law with a high energy cutoff.
Bottom: the residuals of the fit in units of standard deviations.
Romano et al. 2008, ApJ, 680, L137.
Our most recent results using Swift
data on outbursting SFXTs also include:
The unique multiple flaring activity in
(Romano et al.,
2009, MNRAS, 392, 45).
The 2008 XRT light curve shows a multiple-peaked structure with an initial bright flare that
reached a flux of about 10-9 erg cm-2 s-1 (2-10 keV),
followed by two equally bright flares within 75 ks. The spectral
characteristics of the flares differ dramatically, with most of the difference, as derived via
time-resolved spectroscopy, being due to absorbing column variations. We observe a gradual
decrease in the NH, derived with a fit using absorbed power-law model, as time passes. We
interpret these NH variations as due to an ionization effect produced by the first flare, resulting
in a significant decrease in the measured column density towards the source.
Figure 4. XRT 0.3-10 keV light curve of the 2008 July 5 outburst
of IGR J08408-4503.
Adapted from Romano et al. 2009, MNRAS, 392, 45.
Coverage of the outburst of SAX J1818.6-1703, obtained as part of Swift
GI (Cycle 5) program
(Romano et al., 2009, ATel 2044 ,
Sidoli et al., 2009, MNRAS, 400, 258).
We performed the first broad-band X-ray study of SAX J1818.6-1703 in outburst (2009 May 6).
The spectrum can be deconvolved well with models usually adopted to describe the emission from
HMXB X-ray pulsars, and is characterized by a very high absorption, a flat power law (photon
index 0.1-0.5) and a cut-off at about 7-12 keV. Alternatively, the
emission can be described with a Comptonized emission from a cold and optically thick
corona, with an electron temperature kTe = 5-7 keV, a hot seed photon temperature, kT0, of
1.3-1.4 keV and an optical depth for the Comptonizing plasma, of about 10. The 1-100 keV
luminosity at the peak of the flare is 3x1036 erg s-1
(assuming the optical counterpart distance
of 2.5 kpc). These properties of SAX J1818.6-1703 resemble those of the prototype of the
SFXT class, XTE J1739-302. The monitoring with Swift/XRT reveals an outburst duration of
about 5 d, similar to other members of the class of SFXTs, confirming SAX J1818.6-1703 as
a member of this class.
Monitoring of IGR J18483-0311 for a whole orbital period
(Romano et al., 2010, MNRAS, 401, 1564).
IGR J18483-0311 is one of the few SFXTs where both the orbital
(18.52 d) and spin period (21 s) are known. Our paper reports on the first complete monitoring of
the X-ray activity along an entire orbital period of a Supergiant Fast X-ray Transient. These
Swift observations, lasting 28 days, cover more than one entire orbital phase consecutively.
They are a unique data-set, which allows us to constrain the different mechanisms proposed
to explain the nature of this new class of X-ray transients. We applied the new clumpy wind
model for blue supergiants developed by
Ducci et al. (2009, 398, 2152),
to the observed X-ray light
curve. Assuming an eccentricity of e=0.4, the X-ray emission from this source can be
explained in terms of the accretion from a spherically symmetric clumpy wind, composed of
clumps with different masses, ranging from 1018g to 5x1021g.
Figure 5. Swift/XRT 0.2-10 keV light curve of IGR J18483-0311 during our
monitoring program, background-subtracted and corrected for pile-up, PSF
losses, and vignetting. Downward-pointing arrows are 3sigma upper limits.
The upper limit with the wide symbol centered on MJD 55007.9 (about 0.004 counts/s)
is obtained accumulating the 4 observations (individual upper limits)
between MJD 55006.5 and 55010.2. Different colours mark different observations, with a colour scheme
that generally mimics the phase (top axis) with a P = 18.52 days (Sguera et al. 2007).
The inset zooms on observation 024.
From Romano et al. 2010, MNRAS, 401, 1564.
Coverage of the outburst of AX J1841.0-0536 on 2010 Jun 5
( Romano et al., 2011, MNRAS, 412, L30, Paper VII).
Swift observed an outburst on 2010 June 5, and followed it with XRT for 11 days.
The X-ray light curve shows an initial flare followed by a decay and subsequent
increase, as often seen in other SFXTs, and a dynamical range of about 1600.
Our observations allow us to analyse the simultaneous broad-band (0.3-100 keV)
spectrum of this source, for the first time down to 0.3 keV,
which can be fitted well with models usually adopted to describe the emission
from accreting neutron stars in high-mass X-ray binaries,
and is characterized by a high absorption (NH ~ 2x1022 cm-2),
a flat power law (photon index 0.2), and a high energy cutoff.
Monitoring of IGR J16418-4532 along the orbital period
(Romano et al., 2011, ATel 3174,
Romano et al., 2012, MNRAS, 419, 2695).
Our Swift observations of this candidate supergiant fast X-ray transient, with known
orbital and spin period (3.7d and 1250s), span over three orbital periods and
represent the most intense and complete sampling of the light curve of this source with a
sensitive X-ray instrument. With this unique set of observations we can address the nature
of this transient. By applying the clumpy wind model for blue supergiants
(Ducci et al. 2009, 398, 2152)
to the observed
X-ray light curve, and assuming a circular orbit, the X-ray emission from this source can be
explained in terms of the accretion from a spherically symmetric clumpy wind, composed of
clumps with different masses, ranging from 5x1016g to 21g. Our data suggest, based
on the X-ray behaviour, that this is an intermediate SFXT.
We have developed an algorithm solving the radiative transfer equation in the Fokker-Planck
approximation when both thermal and bulk Comptonization take place.
(Farinelli et al., 2012, A&A, 538, A67).
The algorithm is essentially a relaxation method, where stable solutions are obtained when the
system has reached its steady-state equilibrium.
Our XSPEC model will be publically available and distributed as a contributed model to the
official XSPEC web page. The code is written using C-language, and can be easily
installed following the standard procedure reported both in the official XSPEC manual
and in the brief cookbook which will be delivered together with the source code.
The free parameters of the model are the blackbody seed photon temperature kTbb,
the electron temperature kTe, the vertical optical depth of the accretion column
tau, the radius of the accretion column r0 (in units of the NS Schwarzschild radius),
and the albedo A of the NS surface. Additional parameters for the case of accretion
with matter velocity increasing progressively with decreasing altitude are the index
eta, which corresponds to a free-fall case when it is set equal to 0.5, and the terminal
velocity beta0 at the NS surface.
The COMPGMAG model has been applied to the most recent outbursts
(2011 February 22 and March 24, respectively) of XTE J1739-302 and IGR J17544-2619,
the prototypes of the SFXT class
(Farinelli et al., 2012, MNRAS, 424, 2854).
We discuss the possible accretion scenarios derived by the different models, and we
also emphasize the fact that the electron density derived from the Comptonization models,
in the regions where the X-ray spectrum presumably forms, is lower than that estimated
using the continuity equation at the magnetospheric radius and the source X-ray
luminosity, and we give some possible explanations.
Monitoring of IGR J17354-3255 along the orbital period
(Ducci et al., 2013, A&A, 556, A72).
We performed an 11-day Swift/XRT monitoring of the field of view around IGR J17354-3255,
which is positionally associated with the AGILE/GRID gamma-ray transient AGL J1734-3310.
These new data (~24 ks, spanning 1.2 orbital periods, Porb = 8.4474 d) allow us to exploit
the timing variability properties of the sources in the field to unambiguously identify the
soft X-ray counterpart of IGR J17354-3255.
The soft X-ray light curve shows a moderate orbital modulation and a dip.
We investigated the nature of the dip by comparing the X-ray light curve with the prediction
of the Bondi-Hoyle-Lyttleton accretion theory, assuming both spherical and nonspherical
symmetry of the outflow from the donor star.
We found that the dip cannot be explained with the X-ray orbital modulation.
We propose that an eclipse or the onset of a gated mechanism is the most likely
explanation for the observed light curve.
Contact person at IASF-Palermo:
The Astronomer's Telegram
BAT Transient Monitor: IGRJ16479-4514
BAT 58-Month Source Catalog
J. Rodriguez's page on IGR sources
INTEGRAL Galactic Bulge Monitoring
The INTEGRAL Spiral Arms (ISA) Monitoring Program
RXTE Galactic Center Observation
A Catalogue of optically identified INTEGRAL sources
We acknowledge financial contribution from
ASI-INAF I/004/11/0 (Swift),
ASI-INAF I/021/12/0 (LOFT),
ASI-INAF I/009/10/0 (Analisi Dati Alte Energie),
ASI/INAF I/088/06/0 (Studio di Astrofisica delle Alte Energie).
Complete list of our SFXT publications
(Swift followup of MAXI-discovered transients).
Last Modification: Monday, October 21 2013
Edited by P. Romano