Cyclotron-line feature from GRO J1008-57 with MAXI-Suzaku ToO observation

January 24th, 2013 by Tatehiro Mihara

According to the large flux increase observed with MAXI/GSC during the giant outburst in 2012 November,  the MAXI team requested Suzaku ToO observation. It was performed at the outburst peak from 2012-11-20 (MJD 56251) 14:44 to 2012-11-22 5:21 with an exposure of 50 ks. The MAXI/GSC flux was 400 +- 11 mCrab in 4-10 keV. The flux with Suzaku was 6.8 x 10-9 erg cm-2 s-1 in 2-10 keV, and 2.65 x 10-8 erg cm-2 s-1 in 1-100 keV. The luminosity was 8.0 x 1037 erg s-1 in 1-100 keV at the 5 kpc distance (Coe et al. 1994).

Our preliminary analysis of the Suzaku HXD/PIN and GSO data revealed that the spectrum can be reproduced by an NPEX with a cyclabs model with a reduced chi squared (dof) = 0.94 (127). The derived parameters of the cyclotron-line feature are E_cyc = 75.5 (+2.5, -1.5) keV, W = 4.0 (+5.4, -4.0) keV, and D = 1.6 (+9.4, -0.6) with errors of 90% confidence limits. The feature existed throughout the entire phase of the apparent 93.6257 s spin period. The E_cyc were 77.7, 74.7, 75.5, and 76.2 keV for the devided spin phases of rise, peak, fall, and valley of the pulse shape, respectively.

Suzaku spectrum does not show any signature of cyclotron-line feature in 20-50 keV range. Thus, the feature at 76 keV is considered as the fundamental cyclotron line. It corresponds to a magnetic field strength of 6.6 x 1012 G, which is the highest among binary X-ray pulsars ever observed.

GROJ1008_spec
The spectra with Suzaku PIN and GSO fitted with a NPEX and cyclabs model. The residuals in the bottom panel are without cyclabs model.

gso_pulse1
The pulse profile of GRO J1008-57. The pulse phases are divided into four phases : rise, peak, fall, and valley.

MAXI/GSC detection of an unexpected brightening from Be/X-ray binary pulsar GRO J1008-57

November 9th, 2012 by Motoki Nakajima

MAXI/GSC is monitoring a peculiar X-ray activity of GRO J1008-57. The current long outburst started from August 2012. After the decay of the long outburst lasting for about 2 month, the flux turned into an increase again from MJD 56236 (2012-11-05). The flux reached 62 +- 7 mCrab (4-10 keV) on 2012-11-08 (MJD 56239) in 1-day bin. The latest 4-10 keV flux at 2012-11-09 03:00 UT reached 120 +- 9 mCrab in 4-hour bin. It is already as bright as the peak of the regular normal outburst at periastron. The Swift/BAT also detected the increase in 15-50 keV. According to the binary orbital parameters (Coe et al. 2007; Sootome et al. 2012), the present flare corresponds to ~0.3 orbital phase. Such a bright flare has not been recorded at this orbital phase.

Folded light curve of GRO J1008-57 bu its binary orbital period of  249.49 day.

Folded light curve of GRO J1008-57 by its binary orbital period of 249.49 day.

Does a double-peaked outburst lead to a giant outburst in GX 304-1 as A 0535+26 ?

September 25th, 2012 by Tatehiro Mihara

The Be/X-ray binary pulsar, GX 304-1, started brightening on September 17, suggesting that the source now entered a new outburst. The X-ray flux reached 40 +- 5 mCrab (4-10 keV) on September 23. It was 15 days earlier than that expected from the orbital period of 132.5 days and the phase of the outburst onset of the previous 11 outbursts.
The figure shows folded MAXI/GSC X-ray light curves by the orbital period for GX 304-1 (in red) and A 0535+25 in 2009 (in gray). The Swift/BAT curves are also overlaid. The shapes of double peaks and a precursor agree very well between the two pulsars. Then, a giant outburst may follow in GX 304-1 in mid-October.
(by Nakajima and Mihara)

Folded light curves of GX 304-1 and A 0535+26 by their orbital periods. Double-peaked outbursts of the two are similar, and now GX 304-1 is tracing the precursor in prior to the giant outburst.

Folded light curves of GX 304-1 (red) and A 0535+26 (gray) by their orbital periods. Double-peaked outbursts of the two are similar, and now GX 304-1 is tracing the precursor in prior to the giant outburst.

On-demand data archive is now open to public

November 8th, 2011 by Tatehiro Mihara

On-demand data of MAXI/GSC is available. You can get spectrum of any sky position of any time. Please visit

http://maxi.riken.jp/mxondem

There is also  a short-cut “on-demand data” on the maxi-riken top page (http://maxi.riken.jp/top), or you can select “Data Products” tab and click “go to on-demand page”.

The data are limited to those taken with 1650-V counters since 2009 October 31 to  2 days ago excepting for the GSC_3.  Please read the notes in “About this page” before you start the analysis.

MAXI detection of a super-burst from EXO 1745-248 in Terzan 5

November 1st, 2011 by Tatehiro Mihara

We analyzed the MAXI/GSC light curve of an X-ray burst from EXO
1745-248 in Terzan 5 reported in Atel #3714, #3718, #3720 and found
that the initial peak at MJD 55858.53 decayed exponential with an
e-folding time of 10 hour.
exp If the emission is a blackbody radiation, the temperature can be estimated from the hardness of two energy bands.

MJD      4-10/2-4 keV   kT [keV]      10-20/4-10 keV   kT [keV]
55858.53      2.9         2.9  +- 0.8       0.32    2.4  +- 0.6
55858.59      1.5         1.7  +- 0.4       0.19    2.0  +- 0.8
55858.78      1.05        1.4  +- 0.4       0.50    2.8  +- 1.0
55858.84      1.24        1.58 +- 0.5       0.37    1.85 +- 0.8
55858.91      1.06        1.43 +- 0.5       0.19    1.83 +- 1.5
55858.97      1.03       1.40 +- 0.5        0.06    1.80 +- 3.9
(Errors are 1-sigma.)

The values derived from 4-10/2-4 keV and 10-20/4-10 keV
are consistent with each other. It showed a softening from 2.9 keV in the beginning to 1.5 keV in the end.

tempe

The fluence is 2.4 x 1042 erg in 2-10 keV assuming 8.7 kpc distance (Cohn et al. ApJ 571 818 (2002)). Using H burning energy of 6 x 1018 erg/g, the mass of H is 4.0 x 1023 g. Using the average flux of 10 mCrab (1.7 x 1036 erg/s, 9.0 x 1015 g/s), the reputation time is calculated to be 510 yr. (<- It was a mistale. Correctly 510 days. If we use C-burning energy it becomes 5100 days = 14 yrs.  by TM 2011.11.16)

The sphere radius of the blackbody is 6.3 km with using 2 keV and 6.8 x 1037 erg/s at the peak.

These results (e-folding time, temperature, softening, fluence, and radius) are typical as a super-burst from low-mass X-ray binaries.

Atel #3729

Archived light-curve data is available at

http://maxi.riken.jp/top/index.php?cid=1&jname=J1748-248

MAXI/GSC detection of an X-ray burst from the posion consistent with the globular cluster M15

June 7th, 2011 by Mikio Morii

MAXI/GSC detected an X-ray burst at the scan transit centered at UT 2011-06-05T00:10:03.
The burst was detected at least for 30 seconds within the 62 seconds triangular transit response of MAXI/GSC.
The nominal location of the source, assuming that the source flux was constant over the transit
(which probably was not), is determined as

(R.A., Dec) = (+322.76 deg, +12.03 deg)

= (21 31 3, +12 01 44)(J2000)

with a rectangular 90% statistical error box with the following corners:

(R.A., Dec) = (+322.65 deg, +12.24 deg)

= (21 30 35, +12 14 7)(J2000)
(R.A., Dec) = (+322.93 deg, +12.19 deg)

= (21 31 42, +12 11 14)(J2000)
(R.A., Dec) = (+322.87 deg, +11.82 deg)

= (21 31 28, +11 49 28)(J2000)
(R.A., Dec) = (+322.59 deg, +11.87 deg)

= (21 30 21, +11 52 20)(J2000)

There is additional systematic uncertainty of 0.2 degree (90% containment radius).
This position is consistent with that of the globular cluster M15,
whose position is (R.A, Dec) = (322.49 deg, 12.17 deg).
The burst flux was 220 +-20 mCrab in the 4 – 10 keV band.
This burst is though to be the type I X-ray burst, because the softening of the spectrum was observed.
As reported in ATEL #3363, #3378, #3393, this source has been active recently.

MAXI data process has recovered.

March 30th, 2011 by Tatehiro Mihara

We have returned to the regular data process since March 25. The data between March 11-24 are to be filled succeedingly. In addition, we started a frequent update service in every 4 hours, first for 4U 1608-52 (ATel #3237) and Swift J164449.3+573451 (ATel #3244).

MAXI data stopped by the earthquake.

March 14th, 2011 by Tatehiro Mihara

The ISS-opration building in JAXA Tsukuba space center was damaged by the earthquake on March 11, 2011. The building contains the computers which receive MAXI telemetry data from NASA and store them. The computers have stopped since then. MAXI data also stopped and we can not issue alerts. We think it will take more than a week for the recovery. The MAXI itself in orbit has no problem and continues the observation. The data will be sent to Tsukuba space center afterwards.

Be X-ray binary pulsar A0535+262 started a new giant outburst.

February 23rd, 2011 by Tatehiro Mihara

MAXI/GSC has detected a new outburst from Be transient X-ray binary pulsar A0535+262 (Atel #3166). The figure shows the lightcurve folded with 110.2-day orbital period (Moritani 2010) in the 1.5 yr MAXI observations. Orbital phase zero corresponds to the periastron. The current light curve (orange) traces the previous giant outburst (blue) in December 2009 very well. (It may be a little smaller this time). The He I double line indicates a new gas-disk ejection from the Be star (Atel #3176). No strong precursor before MJD55601 (= Feb 9) may indicate that the gas was ejected very recently just before the “He I double line” observation (Feb 5). The short (1.2 yr) recurrent time shows that the Be star has become active.

a0535_1102day_2

MAXI/GSC detects a new activity from binary X-ray pulsar GX 304-1

December 10th, 2010 by Motoki Nakajima

MAXI/GSC detected a new activity from transient pulsar GX 304-1. The figure shows the lightcurve folded with 132.5-day orbital period. As shown in below figure, the current flux increase is about 1-week earlier than that of the previous outburst within the orbital cycle of 132.5-day period. Thus, the current activity may be a precursor, or an onset of an anomalous giant outburst that occurs out of regular recurrent phase. We have reported this news to Astronomer’s Telegram #3075.

lc_folding_crabunit