MAXI detected a flare from HR 1099 in Taurus at 2022 September 26, 21:22:49 UT. It is the 23rd flare detected with MAXI since 2009. The distance to HR 1099 is 97 lt-yr. HR 1099 is so-called "RS CVn type variable", which is a close binary of G(or F)-type main-sequence star and K-type subgiant star. Somehow, this combination of the close binary is active. According to Perdelwitz et al. (2018) , HR 1099 has a "star cycle", similar to the sun's 11-year cycle. The period is 14 - 20 years. The optical (6 magnitude in visual) light curve showed brightness hollows around 1980, 1995, and 2007. It is due to star spots. When dim with many star spots, the star is active. Next active phase may come around 2021 - 2027. Since we do not have enough data to predict it. Continuous observation is needed. Keep watch.
OHMAN caught X-ray burst from M 15news-1340 September 15, 2022 by Mihara
OHMAN triggered an X-ray burst from the globular cluster M 15 on 2022 September 13 12:27:20 UT (=T0). NICER acted automatically, slewed from T0+45s to T0+330s and started the observation of M 15 at 12:32:50 UT. It was 5 min 30 s after the MAXI trigger. Unfortunately it was not a long burst and the burst itself had ended by that time.
Luminous transient NS-LMXB XTE J1701-462 shines againnews-1339 September 8, 2022 by Mihara
MAXI detected a new outburst from XTE J1701-462 on 2022 September 6, since 2006
( ATel #15592 ).
Swift confirmed it
( ATel #15594 ).
It is a luminous transient neutron-star low-mass X-ray binary (NS-LMXB). It showed both behaviors in the color-color diagram as the luminosity decreased. That is Z-source type in bright phase, and Atoll-source type in dim phase. It is almost the first one that showed both types from one source. In that sense, it is the Rosetta stone in NS-LMXB.
Outburst from the globular cluster M 15news-1338 September 8, 2022 by Mihara
MAXI detected a new outburst from the globular cluster M15 on 2022 August 26, since 2013
( ATel #15586 ).
There are millions of stars in a globular cluster.
But in M 15 only two X-ray sources, AC 211 and X-2, are bright, almost equally.
Swift confirmed the outburst
( ATel #15589 )
but cannot tell which source is in the outburst.
NICER detected an X-ray burst, indicating the neutron star binary X-2
is in the outburst
( ATel #15593 ).
M 15 is the most dense, the oldest (12 billions years old), the most metal-poor (1/100 of the solar abundance) globular cluster. It is 6th magnitude, and locates in the constellation Pegasus. The distance from the Earth is 33600 lt-year.
Complex dim transient 4U 0923-31news-1337 September 5, 2022 by Mihara
MAXI detected an X-ray increase from 4U 0923-31
on 2022 August 31
( ATel #15583 ).
There was no followup due to the sun angle.
This is a complex region. Probably some transients exist in this field. The non-imaging X-ray detector such as UHURU, Ariel, HEAO, EXOSAT, Tenma, Ginga, RXTE detected one of the sources, but could not distiguish them. Now it remains in mystery which source they observed.
Blackhole GX 339-4 comesnews-1336 September 1, 2022 by Mihara
MAXI detected a new outburst from the balackhole binary GX 339-4 on 2022 August 29, since 2021 ( ATel #15577 ). It was confirmed by Swift ( ATel #15578 ) and radio ( ATel #15580 ) and NICER and NuSTAR ( ATel #15585 )
ms Accreting X-ray Pulsar SAX J1808.4-3658news-1335 August 25, 2022 by Mihara
MAXI detected a new outburst from SAX J1808.4-3658 on 2022 August 19 ( ATel #15563 ). It is the first ms accreting X-ray pulsar discovered in 1996. Since then, it repeats outbursts in every 3-4 years. NICER confirmed the outburst ( ATel #15559 ) and detected 2.5 ms pulsation and 2.0 h orbital motion. The orbital ascending node came 15 s later than the prediction of the previous outburst in 2019. It tells the 2.0 h orbital period has got longer by 1 ms since 2019.
MAXI 13 yearsnews-1334 August 18, 2022 by Mihara
After the second sudden shutdown in June, MAXI has been operated with the low-load mode (only GSC mode). Since June 23 it has been functioning normally for about 2 months.
Meanwhile, MAXI detected a peculiar GRB 220706A and the summer-of-even-year outburst from XTE J1829-098, this summer again, on 2022 August 1.
Start of possible Mega outburst of 4U 1630-472news-1333 August 4, 2022 by Mihara
MAXI found a start of an outburst from the blackhole binary 4U 1630-472 on 2022 July 28. It repeats outburst in 400-600 days. The first detection was in 1969 by Vela 5B satellite. 4U 1630-472 is known for such a long time, has the shortest recurrent time as a blackhole binary, and therefore it is one of the best studied backhole binary. The blackhole mass is about 10 solar mass, the distance is about 33000 lt-yr. The 10000 days (27 years) of RXTE/ASM - MAXI light curve shows us a habit. There are two kinds of outbursts; normal lasting for 100 days and mega for 2 years. After 4-5 normal, a mega comes. Especially, the last normal outburst just before the mega is split into two close outbursts. The one just before today's outburst was also split. Today's outburst may be the start of the next mega outburst.
Electrons hit solar paddle behindnews-1332 July 28, 2022 by Mihara
At around 2022/07/21 19:13 UT MAXI detected many electrons from the forward right direction. MAXI X-ray detector can sense low-energy electrons, too. In the sky plot it appears in white, which means the electron energy is widely spread from the low (2 keV, red) to the high (20 keV, blue) energies. But, the color in the lower part was green (4 - 10 keV). This part was shadowed by the solar paddle. The spectrum consisted of copper fluorescent line (8 keV). The electron from the right was stopped by the paddle (Si, Cu, O, Ti? ,,,). Then the fluorescent X-ray was emitted from the paddle. The copper K X-ray penetrated the thin solar cell and reached MAXI.
Outburst of 4U 1608-52news-1331 July 21, 2022 by Mihara
MAXI detected an X-ray outburst from 4U 1608-52 on 2022 July 11 in the southern constellation Norma. It is a contact binary of a neutron star and a low-mass star. The gas from the low-mass star accretes towards the neutron star and forms a accretion disk around it. Since the disk is bi-stable, the gas falls intermittently onto the neutron star. It causes outbursts in about every year. MAXI light curves shows a large outburst every about three years, and two-or-three smaller ones in between.
Pecurier GRB 220706Anews-1330 July 14, 2022 by Mihara
MAXI detected a bright X-ray
source at 17:33:25 UT on 2022 July 6 in the constellation Cetus
(blue in figure).
The position was consistent with the GRB 220706A, which was detected by Swift/BAT,
but at 5051 s before
It was also detected in the next MAXI scan at 10 minutes later.
The spectrum taken with NICER was unusual for a GRB
( ATel #15507 ).
The light curve (black in figure) is very similar to the LMXB Swift J0840.7-3516 (red) in the point of a bright peak at about an hour later and sharp drop after it.
MAXI J0655-013 was an X-ray pulsarnews-1329 July 4, 2022 by Mihara
MAXI data processor hang-up on 2022 June 21 again.
MAXI recovered on 2022 June 23. But this time
SSC is power-off for the light loads to the power module and CPU.
The MAXI nova which was discovered on June 18 was successfully observed with NuSTAR. The 1130 s pulsation was found ( ATel #15495 ). The 1 day variation was a fake. It was produced by the beat of the 1130 s pulsation and the MAXI scan period (5577 s).
MAXI J0655-013 was discoverednews-1328 June 25, 2022 by Mihara
MAXI discovered a new X-ray source MAXI J0655-013 at 10:23 UT on 2022 June 18 in the constellation Monoceros ( ATel #15442 ). The intensity was 61 mCrab. Swift/BAT also triggered it at 20:26 on June 18 ( ATel #15443 ). Monoceros is in winter milky way. MAXI J0655-013 locates on the Galactic plane, but towards the outer direction of the Galaxy. The X-ray spectrum is a power-law with the index of 0.89, which is shaped like the X-ray binary pulsars. The X-ray intensity in June 17-21 looked like changing periodically with 0.98 days ( ATel #15453 ). Then, unfortunately, MAXI stopped because of the data processor hang up at June 21. Swift/XRT and NICER cannot observe it due to the sun constraint. Instead, Nu-STAR observed it on June 22.
XTE J1709-267 outburstnews-1327 June 16, 2022 by Mihara
MAXI detected an outburst from XTE J1709-267 (RX J170930.2-263927) on 2022 June 8. It is a neutron star - Low mass X-ray binary in the globular cluster NGC 6293 in the constellation Ophiuchus. The distance from the Earth is about 30000 lt-yr. The discovery of the outburst was in 1997. The outburst lasts for about 100 days. The peak flux is about 100-200 mCrab. Since then XTE J1709-267 made outbursts in 2002, 2004, 2007, 2010, 2012, 2013, 2016, 2017, 2020, and 2022 (this time). (MAXI detection is the last 7 times). So it repeats an outburst in every 2-3 years. The repetition is caused by the instability of the accretion disk.
MAXI J1816-195 discoverednews-1326 June 9, 2022 by Mihara, Orbital added June 14
MAXI data processor hang-up on 2022 June 3 for the first time in the 13 years.
We made a recovery operation on June 7.
Just after the restart,
MAXI team discovered an X-ray nova MAXI J1816-195 in the constellation Sagittarius
( ATel #15418 ).
The intensity was 100 mCrab.
Upon this, NICER made a raster scan from 14:32, and
Swift made a follow-up from 15:56.
Swift confirmed it a new source with the 3 arcsecond accuracy
( ATel #15421 ).
NICER discovered a 1.9 ms pulsation and detected an X-ray burst
( ATel #15425 ).
Thus, MAXI J1816-195 turned out to be a neutron star binary (accreting ms pulsar).
The orbit was determined by NICER's monotoring of the pulse period. The orbital period is 4.8h. ( ATel #15431 ).
OHMAN startednews-1325 June 2, 2022 by Mihara, ID corrected June 14
On 2022 May 26 OHMAN (On-orbit Hook-up of MAXI and NICER, also known as Orbiting High-energy Monitor Alert Network)
passed the initial test and started the operation.
The OHMAN laptop PC on Express Rack in JEM receives the MAXI ethernet data and analyses it to find a nova by comparing the current X-ray intensity with those in the previous scans which is typically 90 minutes ago and before. When a nova is found, a program checks the visibility of the nova for NICER. If the nova is observable from NICER, OHMAN-PC sends out information to NICER. If the OHMAN action in NICER is set active, NICER moves the telescope to the nova. If it is a new source, NICER makes multi-pointings around the MAXI position to find a more accurate position.
OHMAN action has been set active since May 26. On May 28 there was an alert of a new source from OHMAN-PC. NICER started scan about 3 minutes later. However, no source was found. It was a tail of Sco X-1. Sco X-1 is so strong that the image is spread out, and so variable. OHMAN thought that there was a new star in the outer part of Sco X-1 image. Of course, there was no new star.
OHMAN is running and waiting for an appearance of a real X-ray nova.
Short Gamma-ray burst from SGR 1935+2154 and X-ray burst from GS1826-238news-1324 May 26, 2022 by Mihara
MAXI detected a short gamma-ray burst from SGR 1935+2154
at 2022 May 23 18:36:29 UT.
The burst lasted only for less than 1 s.
The intensity was more than 30 Crab.
MAXI Flash Report Click "Link to LC" in scan No.2.
MAXI detected an X-ray burst from GS 1826-238 at 2022 May 19 04:43:34 UT. The burst lated more than 50 s, and the intensity was 0.5 Crab.
MAXI Flash Report See the thumbnail image of scan No.16.
GRB 220514Bnews-1323 May 19, 2022 by Mihara
MAXI detected a gamma-ray burst GRB 220514B with 140 mCrab at 23:24:21 UT (=T0) on 2022 May 14 in the constellation Draco (GCN #32046). Konus/wind also detected it from T0-26 s to T0+74 s (GCN #32056). Swift observed it in 15 hour later and did detect any source. The upper limit was 0.05 mCrab (GCN #32053). It was so late that non-detection is reasonable according to the regular GRB decaying light curve. Draco is an unfamiliar constellation in the MAXI news. It is 41 degree above the galactic plane. A galactic transient would not appear in such a high latitude. On the other hand, GRB appears uniformly in the sky.
GRB 220506A / MAXI J1558-266news-1322 May 17, 2022 by Mihara
MAXI detected a new X-ray source at 06:28:15 UT on 2022 May 6 in the constellation Scorpius. We reported it as GRB 220506A / MAXI J1558-266 (GCN #32001, ATel #15365 ). The intensity was 100 mCrab (4.0-10.0 keV). There was no flux (less than 20 mCrab) in the previous and the next MAXI scan. Swift's follow-up observation of 11 h later found a faint X-ray source (GCN #32006). There is no optical counterpart at the position (GCN #32008, #32012, #32014). A look-back analysis of Konus-Wind revealed a gamma-ray burst, which occurred 100 s before the MAXI detection (GCN #32057). Therefore the MAXI's source was a tail of the GRB emission or the afterglow, and Swift's source would be the afterglow.
Transient near Galactic center : SAX J1747.0-2853news-1321 April 27, 2022 by Mihara
MAXI team noticed that the X-ray flux from the galactic center region had been increasing since 2022 April 19 ( ATel #15346 ). The flux had reached 150 mCrab. The MAXI error region contains two known sources, SAX J1747.0-2853 and 1E1743.1-2843. Moreover there was a possibility that the MAXI source might be a new source. Swift made a follow-up observation and clarified that SAX J1747.0-2853 had become brighter ( ATel #15347 ). An outburst from SAX J1747 was once detected with MAXI in 2011 ( ATel #3123 , #3163 ).
X-class flare and Space-Xnews-1320 April 21, 2022 by Mihara
The count rate of MAXI/GSC camera 4 increased by 4 times aroud 2022 April 17 3:35 UT. It was from the ISS solar paddle which came into the field of view. An X-class solar flare occurred and the X-ray is reflected by the solar paddle. The red color means reflected solar X-ray and Si K line (1.7 keV). Meanwhile, GSC camera 5 have an X-ray reflection near the right end. This appeared in green. It seems to be a reflection at the solar panel on the space-X dragon. The X-ray spectrum contains Si K (1.7 keV), Sn L (3.5 keV), Cr K (5.4 keV) and Cu K (8.0 keV). Si is solar cell itself and Sn and Cu would be solder and circuit. Peak at 5.4 keV might be a mixture of Cr and Fe from stainless steel.
OHMAN is startingnews-1319 April 14, 2022 by Mihara
OHMAN (On-orbit Hookup of MAXI and NICER) is starting. On April 8, OHMAN-PC was activated and it began reading MAXI data. The novasearch program receives MAXI data and seeks for an X-ray nova. The results are stored in a log file. We downloaded it and checked the output. The function of novasearch is normal.
Be X-ray binary IGR J06074+2205 after 19 yearsnews-1318 March 24, 2022 by Mihara
MAXI found an X-ray source of 20 mCrab in the constellation Gemini at 2022 March 23 07:16 UT ( ATel #15294 ). The location is consistent with IGR J06074+2205, a Be X-ray binary ( ATel #682 ). It was discovered in 2003 and dimmed out ( ATel #223 ). MAXI's outburst detection is the first time since then.
GRB 220310A in Leonews-1317 March 17, 2022 by Mihara
MAXI detected a sudden X-ray increase in the constellation Leo at 2022-03-10 00:27:57 UT (GCN #31725). It was GRB 220310A. "On-going alert" is sent out to the GCN and the registered astronomers in 15 s later automatically. The CALET light curve showed MAXI triggered the very beginning of GRB 220310A (GCN #31730). MASTER Robotic telescope on ground found an optical transient (OT) of 15 magnitude in 30 minutes later (GCN #31732). The time-difference analysis between Konus-Wind in sun-earth L1 point and Mars Odyssey in Mars orbit indicated the position of the OT (GCN #31756). Swift made a follow-up observation in the MAXI central region at 10 h later and there was no X-ray counterpart (GCN #31731). But it was because the OT position is near the edge of the MAXI error region and out of Swift fields of view.
Dust echo of MAXI J1421-613news-1316 March 3, 2022 by Mihara
An X-ray ring around MAXI J1421-613 was reported in Astronomical society meeting of Japan on March 2. MAXI J1421-613 appeared on 2014 Jan 9 ( ATel #5750 ). Suzaku made a follow-up observation on 2014 Jan 31 - Feb 3. It was so late that MAXI J1421 had dimmed out and was not detected. But instead, an X-ray ring appeared around it with a radius of about 0.1 degrees. Nobukawa et al. (2020) reported that it is a dust echo of the X-ray from MAXI J1421. The dust plane (CO cloud) was in between MAXI J1421 and the earth. The scattered X-ray traced a little longer path and reached the earth 3 weeks later. This geometry gives the distance to MAXI J1421 to be 9000 lt-yr.
AMON 220220A non-detectionnews-1315 Febuary 24, 2022 by Mihara
MAXI reported non-detection of X-ray from AMON 220220A on 2022 Feb 20. AMON stands for Astrophysical Multimessenger Observatory Network. This event was a coincidence of HAWC (High Altitude Water Cherenkov gamma-ray observatory) in Mexico and IceCube neutrino detector in antarctica (GCN #31615). The event was toward the constellation Bootes with an accuracy of about 0.5 deg. There was no X-ray from this direction during this event (Feb 20 08:08 - 14:19 UT).
EXO 2030+375 got bright againnews-1314 Febuary 18, 2022 by Mihara
The Be X-ray binary EXO 2030+375 is brightening up at 100 mCrab ( ATel #15228 ).
MAXI J1910-057 rebrightenednews-1313 Febuary 10, 2022 by Mihara
MAXI detected a reappearance of the black hole candidate MAXI J1910-057 in the constellation Aquila on 2022 February 4 ( ATel #15214 ). The X-ray flux reached 17 mCrab on February 5. The source was discovered by MAXI and Swift on 2012 May 31 ( ATel #4139 , #4140 ). The X-ray outburst continued until 2013 January 26 (Nakahira et al. 2014). The outburst of this time is 9 years since the disappearance.
MAXI J0709-159 was identified to Be star LY CManews-1312 Febuary 3, 2022 by Mihara
Quest for MAXI J0709-159 continued.
NuSTAR's X-ray telescope identified MAXI J0709-159 as a 9-magnitude Be star
( ATel #15193 ).
The name means the 196th
variable star in the constellation Canis Major.
The distance is 21000 lt-yr with GAIA.
It's on the outer arm of our galaxy.
Contrary to everyone's thoughts, MAXI J0709-159 had flared up again in the third MAXI scan. The behavior and the flux are typical for a Supergiant Fast X-ray Transient (SFXT). LY CMa is surely a supergiant. Sudden X-ray brightening after tens of years is commonly seen in the Be X-ray binary (BeXRB). LY CMa is also a B1e star. An optical follow-up detected a much stronger H alpha emission line than before ( ATel #15194 ). It means the Be star is active (has a bigger steller disk). Since LY CMa is a supergiant Be star, MAXI J0709 is considered to have both attributes of SFXT and BeXRB.
New MAXI nova, MAXI J0709-159news-1311 January 27, 2022 by Mihara
MAXI discovered an X-ray nova MAXI J0709-159
at 10:42 UT on 2022 January 25 in the constellation Canis Major
( ATel #15178 ).
The intensity was 270 mCrab. It was far above the upper limit 20 mCrab in the previous scan.
MAXI did not detect it in the next scan at 12:15.
But detected it again in the 3rd scan at 13:48 at 100 mCrab.
There was no detection after it.
NICER made multi-poinitings in 3 hours later and confirmed the new source
at 10 mCrab at 13:54
( ATel #15181 ).
It was only 6 minutes after the MAXI 3rd scan by chance.
MAXI J0709 had dimmed from 100 mCrab to 10 mCrab in 6 minutes.
Intermediate Polar EX Hya flares upnews-1310 January 20, 2022 by Mihara
MAXI detected an flux increase at 30 mCrab from EX Hya
at January 15 06:18 UT.
It is the brightest white dwarf (WD) binary.
It usually shines at 10 mCrab and sometimes flares up.
The surface magnetic fields is strong, more than 1000 Tesla (10^7 Gauss).
The spin period of the WD is 1.1 hour.
The orbital period of the binary is 1.6 hour.
Since they are not synchronized, EX Hya is categorized as the Intermediate Polar.
The distance from the Earth is 210 light-year.
Blazer Mrk 501 is outburtingnews-1309 January 6, 2022 by Mihara
MAXI detected a gradual flux increase from Mrk 501.
It is an elliptical galaxy in Hercules located at 456 million lt-yr away.
The central core is very bright and variable, and is categorized as BL Lac object, or more widely, Blazer.
Swift/XRT is monitoring Mrk 501 and reported the increase ( ATel #15059 ). Optical flux increased as well by 40 % ( ATel #15134 ). MAXI light curve shows two outbursts in 2012 and 2014, and the flux rise since 2019.
Soft Gamma-ray burst GRB 211225Anews-1308 December 28, 2021 by Mihara
MAXI detected a gamma-ray burst GRB 211225A in the constellation Hydra at 03:22 UT on 2021 December 25 (GCN #31303). The intensity was 200 mCrab. There was no flux in the previous nor the next MAXI scan. The spectrum was soft, and probably therefore, Swift/BAT did not detect it. Such a soft X-ray transient is a suitable target for OHMAN.
X-ray flare from the flare star AU Micnews-1307 December 23, 2021 by Mihara
MAXI detected a flare from AU Mic at 2021/12/15 22:48 UT with an intensity of
( ATel #15139 ).
AU Mic is a "hot topic" flare star of 8th magnitude. It is very close (32 lt-yr), very young (24 million years old), still wears a dust disk (discovered in 2003) where planets were born, and has two planets (a Neptune size and an Earth size, just discovered in 2020 with TESS). The planets orbit around AU Mic in 8 and 18 days, respectively. AU Mic itself is a small star (80% of the sun size, M-type pre-main sequence) rotating fast in only 4.8 day. It would have two large sun spots on the surface. The star is vary active and causes flares frequently. The MAXI's X-ray flare was very large, 10^25 W, which is 1/10 of the whole emitting energy of the sun. The flare typically lasts for some thousands of seconds.
Two X-ray pulsars outbursting around Aquilanews-1306 December 16, 2021 by Mihara
MAXI detected a new outburst from 4U 1907+09 in Aquila on 2021 Nov 27 at 150 mCrab.
It is an X-ray binary pulsar with the spin period of 438 s.
Also MAXI detected a new outburst from XTE J1829-098 in Scutum (south neighbor of Aquila) on 2021 Dec 13 at 50 mCrab.
It is also an X-ray binary pulsar of 7.8 s.
Both pulsars locate on the Galactic plane (galactic latitude is 0.5 deg and 0.3 deg, respectively) and both pulsars have a high-mass companion star (O-type supergiant, and B-type star, respectively). The companion star of XTE J1829-098 has not yet identified, but would be a Be star as MAXI has reported periodical activities probably due to the orbital motion. The activity of XTE J1829-098 were also reported on MAXI news #1261 2020 Aug 13 and MAXI news #1284 2021 Apr 16.
Stars are born on the Galactic plane. High-mass stars are young and have not traveled so much. They are on the plane. The pulsar in 4U 1907+09 would still maintain a strong magnetic fields, and the spin would have slowed down to 438 s.
Both 4U 1907+09 and XTE J1829-098 pulsars are on the Galactic plane. Both have a high-mass companion, and "just born". Other X-ray binaries in the figure (Ser X-1, H 1822-000, 4U 1957+115, Aql X-1) have a low-mass companion and not on the Galactic plane.
Long X-ray burst again from 4U 1820-30news-1305 December 2, 2021 by Mihara
MAXI detected a long X-Ray Burst at 2021 November 25 23:24 UT from 4U 1820-30
( ATel #15071 ).
The intensity was 1.1 Crab.
In the next scan, the intensity was 0.4 Crab and the burst was still lasting.
The e-folding decay time is 1.1 hour, indicating a long burst.
MAXI had just reported a long burst from this source in August, 2021
( ATel #14871 ).
It is in the globular cluster
in the constellation Sagittarius.
The globular cluster is an old system born in the early age of the universe. Heavier stars than the sun have already burnt out and have become a neutron star (NS) or a white dwarf (WD). Many WD are seen in the globular cluster with the Hubble telescope. Also, there are 6 radio pulsars (NS) and one X-ray binary 4U 1820-30 (NS-WD binary) in NGC 6624 ( Revnivtsev et al. 2002 ).
GRB 211115A and OHMAN test-runningnews-1304 November 25, 2021 by Mihara
MAXI detected a Gamma-Ray Burst at 2021 November 15 16:31:19 UT in the constellation Puppis
The GRB 211115A lasted only 12 s (figure).
The intensity was 330 mCrab.
CALET/GBM and Fermi/GBM also detected it.
OHMAN (MAXI-NICER) is in the running-test on ground for two months. It also detected the GRB and issued an on-going alert.
GRB 211115A detected by MAXI. S and E note the start and end time when the source is in the MAXI field of view. Taken from MAXI Flash Report of GRB 211115A. Click 16: link to LC.
Outburst from NGC 6440news-1303 November 18, 2021 by Mihara
MAXI detected X-ray
in the constellation Sagittarius on 2021 November 13 13:31 UT
( ATel #15033 ).
There lies a globular cluster NGC 6440. The distance form the earth is 28,000 lt-yr,
which is almost as far as the galactic center.
MAXI has detected outbursts from NGC 6440
twice, in December 2009 and February 2015.
There are two bright X-ray binaries in this globular cluster,
SAX J1748.9-2021 and NGC 6440 X-2.
Pooley et al. (2002) shows Chandra image taken in 2000 (figure).
Both are milli-second pulsars.
The spin periods are
2.2 ms (Altamirano et al. 2008)
4.9 ms (Altamirano et al. 2010),
The MAXI's twice outbursts were from SAX J1748,
The star this time may be SAX J1748 again, NGC 6440 X-2 in stead, or another new star.
Since the sun is close to NGC 6440 now, Swift and NICER cannot observe it until 2022 Feb. NuSTAR is the only X-ray telescope that can observe it. Although the image resolution of NuSTAR is not enough to separate the stars in the globular cluster, it can tell which star is the MAXI's outburst by detecting the pulsation. We asked for NuSTAR observation and it was approved.
NuSTAR detected 2.2 ms pulsation and confirmed it SAX J1748 ( ATel #15048 , ATel #15095 ).
Chandra image of NGC 6440. (Pooley et al. 2002, Fig.1). 24 sources are detected. They are concentlated within 30 arcsec (4 lt-yr) in diameter. 1 is SAX J1748.9-2021 and 2 is NGC 6440 X-2. Which star is the MAXI's outburst ?
MAXI J1735-272 quickly fadednews-1302 October 21, 2021 by Mihara
MAXI found a faint X-ray transient source at 06:22 UT on 2021 October 17 in the constellation Ophiuchus ( ATel #14979 ). The intensity was 30 mCrab. As it was apart from any known sources, we named it MAXI J1735-272. The source was not detected in the next MAXI scan. Follow-up searches were made by NICER, Swift (10 h later, ATel #14983 ) and INTEGRAL (5-17h later, ATel #14985 ), but any source was detected. The source may have disappeared quickly. Such an event is a target of OHMAN.
Short burst from SGR 1935+2154news-1301 October 7, 2021 by Mihara
MAXI detected a short burst from SGR 1935+2154 on 2021 October 7 11:57UT. The intensity was 60 Crab (200 Crab was a miscalculation), but lasted only for 0.2 s. It is in the constellation Vulpecula again ( after previous MAXI news #1300). It is considered to be a neutron star with a very strong magnetic field (some 10^14 Gauss at surface). The burst is caused by an abrupt energy release of the magnetic fields. SGR 1935 is famous for the first identified galactic Fast Radio Burst, FRB 200428 in 2020 ( Bochenek et al. 2020). Also MAXI news #1251. The distance to SGR 1935 is about 30,000 lt-yr.
XTE J1946+274 makes Cygnus more livelynews-1300 September 30, 2021 by Mihara
MAXI found an appearance of XTE J1946+274 in the constellation Vulpecula on 2021-09-23 ( ATel #14936 ). The flux was 66 mCrab and is increasing. It is a binary of a Be star and a 15 second pulsar. The orbit is eccentric and the period is 172.7 day. The pulsar will pass the periastron on September 29. However, the pulsar does not always emits X-ray at periastron. This is the fourth detection of an outburst since its discovery in 1998. Cygnus has got more lively.
Cygnus has changed to livelynews-1299 September 16, 2021 by Mihara
There are three bright persistent sources in Cygnus. Cyg X-1 (BH), Cyg X-2 (LMXB) and Cyg X-3 (BH). But now, Be X-ray binary pulsar EXO 2030+375 which appeared in July is at the peak of the giant outburst. It is shining as the forth bright star in Cygnus. Additionally the white dwarf SS Cyg is staying in its maximum brightness. Two more pulsars Be pulsar GRO 2058+42 and long-period pulsar 4U 1954+319 appeared.
GRB 140814A was the first merger-triggered core-collapse supernovanews-1298 September 9, 2021 by Mihara
MAXI detected a 15s-lasting bright soft burst in 2014,
and named it GRB 140814A
Swift follow-up was undetection, and the nature was left unknown.
We include the source in MAXI Unidentified Short Soft Transient (MUSST).
In the Science issue on 2021 Sep.3, Dong et al. reported that GRB 140814A was the first merger triggered super nova (and GRB). They found a very luminous source VLASS J121001+495647 in the VLA sky survey made in 2017. It lies in a small galaxy at 480 million lt-yr in Ursa Major. The location coincides with GRB 140814A. They understand it as a blackhole or a neutron star went into the companion star, spiraled-in for 300 years, finally merged with the stellar core and ended up as a super nova and GRB.
We have noticed MUSST a possible new kind of object, and GRB 140814A was it in fact.
The object that a neutron star goes into the companion star is called Thorne-Zytkow ojbject. GRB 140814A was such a object.
Long X-ray burst of 4U 1820-30, every 10 years ?news-1297 August 26, 2021 by Mihara
MAXI detected a bright X-ray burst from 4U 1820-30 at 11:27 UT on 2021 August 23
( ATel #14871 ).
It is a low-mass X-ray binary in the globular cluster
The burst flux was 1.8 Crab, and it decayed to 0.49 Crab in the next MAXI scan at 13:01.
In the third scan at 14:34 it had gone back to the usual level of 0.2 Crab (figure).
The burst spectrum was shaped as a blackbody with a temperature of 24 million degree K.
Considering the distance of 25000 lt-yr, the X-ray luminosity was 2.8 x 10^31 W,
which is 74 % of the Eddington luminosity of the He accretion.
Such a long X-ray burst from 4U 1820-30 was first observed in 1999 ( Strohmayer & Brown 2002 ), and the second one was in 2010 ( ATel #3625 ). It is a rare phenomenon. MAXI detection suggests that it might occur in every 10 years.
4U 1820-30 has a short orbital period (11 minutes). The binary separation is only 120,000 km (1/3 of earth-moon distance). The companion star is considered to be a white dwarf. The rapid binary rotation emits gravitational wave radiation. A calculation tells that the two stars are getting closer by 0.4 m/day. That is, the two stars will collide after 1 million years.
RS Ophiuchus eruption after 15 yearsnews-1296 August 12, 2021 by Mihara
MAXI detected an X-ray emergence from the recurrent nova RS Oph
at 2021 Aug. 10 18:28 UT
( ATel #14846 ).
The intensity was 36 mCrab.
By looking back the data, the brightening had started around Aug. 9 12h UT.
Even half a day before it, an optical amateur astronomer had reported the optical brightening
of Aug. 8 22h UT
vsnet-alert 26131 )
at 5 magnitude with 10cm binoculars and digital camera.
(It is usually 10 mag.)
Surprisingly, almost at the same time, Fermi/LAT had detected GeV gamma-ray at Aug. 8 18-24 UT
( ATel #14834 ).
Optical spectroscopy by Seimei telescope in Okayama Observatory shows the ejecta is expanding at the high speed of 2600 km/s at Aug. 9 10 UT ( ATel #14838 ). So it is a nova explosion. Swift and NICER and radio observatory followed ( ATel #14848 , #14849 , #14850 ).
The last nova from RS Oph was in 2006 ( O'Brien et al. 2006 ). Current one is several times bigger than that. Recurrent nova is a white dwarf binary and repeats nova in some tens of years. RS Oph is a bright and famous one.
EXO 2030+375 giant outburst after 15 yearsnews-1295 July 29, 2021 by Mihara
MAXI detected the onset of a possible giant outburst from Be/X-ray binary pulsar
EXO 2030+375 in Cygnus on 2021 July 20
( ATel #14809 ).
The last giant outburst was in 2006.
EXO 2030+375 made the orbital phase shift of the normal outburst in 2016
( Laplace et al. 2017 ).
Since then it has been showing the normal outburst at every periastron passage of 46 days orbit. However, after the last periastron passage, the flux stayed high at 20 mCrab. And then, the flux started to increase with the rate of 10 mCrab/day on July 20. The light curve traces remarkably well the previous giant outburst in 2006 (figure). If it grows up to a giant outburst, it will be the first one for MAXI. The peak will be about 800 mCrab around September 17.
GRS 1915+105 and absorption lines with NICERnews-1294 July 21, 2021 by Mihara
MAXI detected a flux increase from the black hole GRS 1915+105 on July 9, 2021. It dimmed in 2018 after 26 years of activity ( ATel #11828 ). Upon the MAXI GCN alert, NICER pointed GRS 1915+105 ( ATel #14792 ). GRS 1915 showed a transition from ~25 cts/s to 250 cts/s. The spectra, linked from the ATel, are remarkable to have over a dozen strong absorption lines from Si, S, Ar, Ca, Fe, and Ni, as well as an Fe emission line.
GRB 210709B / MAXI J1849-237 or Ross 154news-1293 July 15, 2021 by Mihara
MAXI detected an X-ray of 110 mCrab in the constellation Sagittarius at 22:12 UT on 2021 July 9 ( ATel #14772 ). There was no flux in the scans 1.5h before and 3h after. We reported the source as either a gamma-ray burst or a new star, GRB 210709B / MAXI J1849-237. Actually there are many stars in the error box. Ross 154 is a famous one of them. It is the 7th closest star system at only 10 light-year away. It is a single small red star with 10th visual magnitude. But, it is known as a flare star. If the MAXI event (0.1 counts/s/cm2) came from Ross 154, the X-ray luminosity would be 3 x 10^23 W, which is 100 times stronger than the usual X-ray intensity. However, it is possible, as such a strong X-ray flare was once observed with Chandra in 2002 ( Wargelin et al. 2008 ). It lasted for about 1000s. It is consistent with the MAXI detection of only one scan.
MAXI J0903-531 redetection suggesting orbital period 57 daynews-1292 July 1, 2021 by Mihara
On 2021 June 22, MAXI detected X-ray (10 mCrab) again from MAXI J0903-531.
It is a Be X-ray binary pulsar which was discovered with MAXI on
2021 April 14
( ATel #14555 ).
It had been shining at 10 mCrab for about 10 days in April and then went
out below the MAXI detection.
The reappearance in June was also reported from
Fermi/GBM and Swift/BAT
( ATel #14730 ).
Look-back analysis of Fermi/GBM detected positive fluxes
around 2020 Dec 22 and 2021 Feb 12.
Then MAXI J0903-531 repeats an outburst every about 57 days.
It is a typical value for an orbital period of a Be binary.
Monitoring is important to understand the new system.
A 0535+262 started an outburst while sun protectionnews-1291 June 24, 2021 by Mihara
Since the sun is a very bright X-ray emitter (~1000 Crab in quiescence),
we shutdown MAXI detectors for protection in closer than 5 degrees from it.
The sun is in the Taurus in June, and
the Be/X-ray binary pulsar A 0535+262, located just next to the Crab nebula
in the Taurus, was not observable from June 10 to 19, 2021.
There was no emission (<20 mCrab) on June 9. In fact it had been off
for 200 days.
However, when the pulsar came out from the protection region on June 20,
it had brightened up to 380 mCrab
( ATel #14173 ).
The Be/X-ray binary pulsar occurs an outburst at the periastron passage of the binary orbit, but not always. It does only when the activity of the Be star is high and much gas is expelled. The orbital period of A 0535+262 binary is 111.07 days.
4U1543-47, brightest 10 Crab X-ray novanews-1290 June 17, 2021 by Mihara
MAXI found a bright star in the constellation Lupus (wolf) at 12:00 on June 11, 2021
( ATel #14701 ).
The position was consistent with the black hole binary 4U 1543-47.
The X-ray flux rapidly rose up and reached about 10 Crab on June 14.
It has become the brightest X-ray nova that MAXI ever detected in 11 years.
X-ray luminosity reached in fact the maximum one that an X-ray source can emit,
so-called the Eddington luminosity
( ATel #14708 ).
Previous outbursts were in 1971, 1983, 1992, and 2002.
Thus 4U 1743 usually makes an outburst in every 10 years, but the one in 2012 was absent.
The flux was usually 3 - 5 Crab at peak, but this time it is doubled to 10 Crab.
The X-ray spectrum is that from an accretion disk around the black hole.
The temperature of the innermost part is 1 keV, = 10 million K.
The inner radius of the accretion disk is 75 km, suggesting a cavity around the
4U1730-22 came again after 49 yearsnews-1289 June 10, 2021 by Mihara
MAXI detected a new X-ray star with 59 mCrab in constellation Ophiuchus
at 19:43 UT on 2021 June 7 (figure)
( ATel #14683 ).
the previous nor in the next MAXI scan it was not detected (<20 mCrab).
Swift made follow-up observations at 8:53 UT and 23:16 UT on June 8 and identified the source as 4U 1730-22 and CXOU J173357.5-220156
( ATel #14688 ).
4U 1730-22 was discovered in 1972. The outburst lasted for 200 days and the peak flux was 120 mCrab. CXOU J1733 was a faint (0.3 mCrab) star in the error box of 4U 1730 detected with Chandra in 2004. The nature is a neutron star ( Tomsick et al. 2007 ). MAXI detected an outburst from 4U 1730-22 after 49 years, for the first time since 1972.
4U 1705-32 first time with MAXInews-1288 June 3, 2021 by Mihara
MAXI detected a new X-ray source in the constellation Scorpius on May 25, 2021,
with 25 mCrab intensity
( ATel #14663 ).
NICER confirmed the source was 4U 1705-32 with 4 mCrab
( ATel #14669 ).
It was the first detection with MAXI in the 11 years. The upper
limit of the period was < 1 mCrab.
Looking back MAXI data in the long term, 4U 1705-32 had brightened to 2 mCrab
in December 2020.
On May 24, 2021, the X-ray flux suddenly increased to 20 mCrab.
However, the flux dropped on May 25, and even below the MAXI detection limit
(5 mCrab) on May 28
( ATel #14670 ).
The intensity of 25 mCrab was the brightest since the discovery with UHURU in 1971.
An X-ray burst was detected by Beppo-SAX in 2000 implying the nature is
a neutron star (1RXS J170854.4-321857,
in't Zand et al. 2005 ).
NS-LMXB SAX J1810.8-2609 in Outburstnews-1287 May 27, 2021 by Mihara
MAXI detected a new X-ray outburst from the neutron-star low-mass X-ray binary
SAX J1810.8-2609 in the constellation Sagittarius on 2021 May 13
( ATel #14649 ).
The X-ray flux was about 40 mCrab and increasing slowly.
This is the fourth outburst from SAX J1810.8-2609 detected by MAXI.
The first one was 2012 May 12, the second one on 2015 Jan 20, and the third
one on 2018 Apr 27
( ATel #11593 ).
However, the current outburst looks quite different with previous ones.
The outburst is lasting long, emitting hard X-ray (Swift/BAT),
( ATel #14659 ).
Discovery of MAXI J1803-298, a black hole binarynews-1286 May 6, 2021 by Mihara
MAXI discovered an X-ray nova (about 50 mCrab) on 2021 May 1 19:50 UT
at the "bow and arrow" of the constellation Sagittarius
( ATel #14587 ).
NICER performed multi-pointing observations at May 2 03:36 after seeing off
Crew-1 departure from ISS,
and identified a new source within the MAXI error circle
( ATel #14588 ).
The source kept brightening, and
the BAT, XRT and UVOT onboard Swift automatically detected the source on May 2 17:39
( ATel #14591 ).
Almost at the same time 17:56, the followup optical observation with MITSuME
at Okayama observatory detected a
15 magnitude star in R (red) and I (infrared) bands
( ATel #14594 ).
Southern African Large Telescope obtained the optical spectrum from May 2 22:56
( ATel #14597 )
Bowen fluorescence emission lines,
Hα P Cyg-like emission line and
Hβ double-peaked emission line.
Those suggest a central UV light source ionizing the surrounding gas,
outflow of the surrounding gas, and a rapidly (800 km/s) rotating accretion disk,
It is the spectrum of the low-mass X-ray binaries (LMXB).
INTEGRAL showed the spectrum extending to a hard X-ray (100-200 keV)
( ATel #14598 ).
NICER's detailed observation showed a spectrum of a 0.3 keV disk blackbody
and 0.2Hz QPO, suggesting a black hole binary
( ATel #14602 ).
It is the 31st nova that MAXI discovered and probably the 14th black hole.
Discovery of MAXI J0903-531, a Be binary pulsarnews-1285 April 20, 2021 by Mihara
MAXI found a new X-ray source at 04:33 UT on 2021 April 14
in the constellation Vela
( ATel #14555 ).
We named it MAXI J0903-531.
The intensity was of 16 mCrab.
Swift/XRT (X-ray telescope) and UVOT (UV telescope) identified it.
There is a star of 13 magnitude at 10 kpc
( ATel #14557 ).
There is the Perseus arm. (figure)
Considering the distance, the optical luminosity of the star is 2000 times of the sun, suggesting a high mass star (8 solar mass). NICER detected 14 s pulsation ( ATel #14559 ). Southern African Large Telescope detected a strong H alpha emission line ( ATel #14564 ).
It is the 30th nova that MAXI discovered. Thanks to the quick followups over the world, the nature of the nova turned out to be a Be X-ray binary pulsar.
Orbital period updated for the Be X-ray pulsar XTE J1829-098news-1284 April 16, 2021 by Mihara
MAXI detected an X-ray star (70 mCrab) in the constellation Scutum
on 2021 April 12
( ATel #14554 ).
The source position is consistent with the Be X-ray pulsar XTE J1829-098.
After the MAXI's report in the last summer
( ATel #11927 ),
SRG reported a
beginning of a new outburst on 2021 April 5
( ATel #14521 ).
The MAXI detection shows the pulsar is brightening to an outburst.
Although two outburst periods (orbital period of the Be binary) were proposed,
480 days by
Halpern et al. (2007)
and 246 day by
Markwardt et al. ( ATel #2007 ),
the 246 day is turned out to be correct
by the date separations of the April outburst.
X-ray burst from NS-LMXB 4U 1323-619news-1283 March 25, 2021 by Mihara
MAXI detected an X-ray burst (90 mCrab) from 4U 1323-619 in the constellation
Centaurus on 2021 March 23 04:11 UT.
It is a binary of a neutron star (NS, 1.4 solar mass) and
a low-mass star (0.3 solar mass)
(Gambino et al. 2016).
The binary period is 2.94 hour.
The binary separation is 860 thousand km, which is only 2.3 times of the earth-moon
It is so close that the gas on the stellar surface flows onto the NS.
When it accumulates to a certain amount,
a sudden nuclear fusion (an X-ray burst) occurs on the surface of the NS.
Such a system is called NS low-mass X-ray binary (NS-LMXB).
The distance from the earth is 14 thousand light-year.
It locates 1 degree east of the coal sack, but
is much further than the coal sack (600 lt-yr).
Reappearance of Be X-ray binary Swift J1626.6-5156news-1282 March 18, 2021 by Mihara
MAXI detected an appearance of X-ray star of about 40 mCrab on 2021 March 11
in the constellation Norma
( ATel #14454 ).
The position was consistent with the Be X-ray binary Swift J1626.6-5156.
Follow up observation with NICER on March 11
( ATel #14457 )
found a pulsation of
15.34 s, which is the pulse period of Swift J1626.
NICER detected a 9.1 keV dip in the spectrum. It is the cyclotron resonance
of an electron in the magnetic field, whose strength is 8e11 Gauss.
Since the source located on the course of SRG scan, SRG/ART-XC also detected it.
Follow up observation with NuSTAR confirmed the cyclotron resonance and
also found the
second harmonic at 17 keV
( ATel #14462 ).
Swift J1626 was discovered in 2005 with Swift.
MAXI detected a small outburst in 2014 September
( ATel #14498 ),
and this is the third detection in history.
GRB 210222A wih MAXI, CALET, and Konus-windnews-1281 March 11, 2021 by Mihara
MAXI detected a bright (390 mCrab in 4-10 keV) transient in the constellation Sculptor
at 2021/02/22 15:59:29 UT (
GRB 210222A) (figure).
At 116 seconds before, CALET Gamma-ray Burst Monitor (CGBM) triggered it
and Konus-wind also did
The peak flux was about 40 Crab (100 - 1000 keV) and
the burst duration was 87 second.
When MAXI detected it, the GRB had already darkened under CGBM sensitivity.
MAXI detected the tail of the long GRB.
In 5 years, simultanious detection with MAXI and CALET is 18 out of total 55 MAXI detections. Those with MAXI, CALET and Konus-wind is 13.
Chandra confirmed MAXI J1848-015 is a new starnews-1280 March 4, 2021 by Mihara
Swift localized MAXI J1848-015 to a star cluster GLIMPSE-C01 with an accuracy of 2.3 arcsec
( ATel #14420 ).
To find out which star in the cluster made the outburst,
Chandra observed MAXI J1848 on Feb. 21 with an accuracy of 0.8 arcsec
( ATel #14424 ).
They found a bright star (1 mCrab) around the boundary of Swift's error circle.
In the previous observations in 2006 and 2019 with sensitivity down to 0.1 micro Crab, this star did not exist (figure).
Although 17 stars had been detected, the brightest star was only 2 micro Crab.
So, MAXI J1848-015 was really a new star.
NICER observed MAXI J1848 on Feb. 23 and found many iron lines ( ATel #14429 ).
Swift confirmed MAXI J1848-015news-1279 February 25, 2021 by Mihara
MAXI nova MAXI J1848-015 which was discovered on Dec. 20 last year was observed with Swift satellite at last on Feb. 21 ( ATel #14420 ). Swift had to wait until the sun moved far from the source. It was lucky that the star was still bright and Swift found it within the NuSTAR error box. The position became 40 times more accurate, and there sits a hidden globular cluster GLIMPSE C01. It is on the Galactic plane and the optical lights are absorbed by the interstellar gas. This hidden cluster was discovered recently in 2005 with Spitzer infrared satellite. X-ray luminosity was calculated using the cluster distance (5 kpc). The low luminosity suggests the source to be a neutron star binary rather than a blackhole binary. The position was also consistent with ASCA source AX J184848-0129. The spectral changes with MAXI NuSTAR Swift and ASCA also indicate a NS binary. The nova ended in the common view as a NS binary in globular cluster.
Blackhole GX 339-4 brighteningnews-1278 February 18, 2021 by Mihara
After reported on Jan. 28, X-ray flux from the blackhle binary GX 339-4
Today's flux is 0.07 photon/cm2/s in 10-20 keV.
From the three-times experience of MAXI, GX 339-4 made a spectral state
transition at 0.12 - 0.18 ph/cm2/s from the hard spectrum to the soft one.
This indicates that the accretion disk emitting the soft X-ray
comes closer to the blackhole and it finally reaches the 3 times of the
There is a variance on the threshold level.
So the state change may be tomorrow or 3 weeks later,
Many astronomers is keeping their eyes on the behavior of this famous blackhole.
Blackhole GX 339-4 started an outburstnews-1277 January 28, 2021 by Mihara
The recurrent black-hole transient GX 339-4 started an outburst.
It was first noticed by the weekly monitoring with the MeerKAT
radio telescope on 2021 Jan. 4
( ATel #14336 ).
NuSTAR and Swift/XRT made TOO observations and detected
a weak X-ray on Jan. 23
( ATel #14352 ).
Swift/BAT detected a positive hard X-ray on Jan 25, and also,
MAXI detected a soft X-ray on Jan. 26
( ATel #14351 ).
Looking back the data, INTEGRAL had detected X-ray on Jan. 17 and 21
( ATel #14354 ).
Now the flux is 40 mCrab and is rising.
It is still in the hard spectral state (beginning of an outburst).
The last outburst had ended in 2020 April.
Now, a new outburst has begun.
NuSTAR confirmed MAXI J1848-015news-1276 January 21, 2021 by Mihara
After the MAXI's discovery on 2020 Dec. 20, NuSTAR
detected MAXI J1848-015 successfully on Dec. 23
( ATel #14290 ).
The location of MAXI J1848 looks slightly offset
(about 71 arcsec) from the known source AX J1848.8-0129.
But, it is within the error of Nu-STAR and they could not confirm it a new star.
Just after it on Dec. 23 the X-ray flux dropped quickly below the MAXI detection limit
( ATel #14292 ).
One explanation was that the source might have made a soft-to-hard state
transition and soft X-ray decreased.
To confirm it we made a NuSTAR TOO observation on Dec.31 - Jan.1
( ATel #14327 ).
The spectrum had changed to that of the hard state and our idea was confirmed.
The image looks similar and identification is not certain yet.
Very soft Gamma-ray burst GRB 210102Bnews-1275 January 7, 2021 by Mihara, Negoro, Serino
MAXI detected a bright uncatalogued X-ray source at 2021 January 2 09:03:48 UT in the constellation Aquarius with the 240 mCrab intensity. We reported as GRB 210102B (GCN #29223). Swift made a follow-up observation in 6 hour later with 7 pointings and found a source with 0.1 mCrab (GCN #29230). At the refined position, an optical transient was found with 22 magnitude in 28 hour later (GCN #29240). However, the second Swift follow-up in 58 h later did not detect the source ( weaker than 0.01mCrab, GCN #29271). Nor, the second optical follow-up in 76 hour later (weaker than 23 magnitude, GCN #29270). GRB 210102B was a very soft Gamma-ray burst, showed a quick decay in X-ray and optical, and there was no star or galaxy at that position.
New star MAXI J1848-015 or a cataloged star ?news-1274 December 24, 2020 by Mihara, Negoro
MAXI found an X-ray transient source in the constellation Aquila
at 05:04 UT on 2020 December 20
( ATel #14282 ).
The X-ray flux was 63 +- 10 mCrab (4.0-10.0keV).
The source locates just on the galactic plane (figure).
The source may be a new source as MAXI J1848-015, or may be
rebrightening of a cataloged
weak X-ray source AX J1848.8-0129, whose nature is unknown yet.
Swift and NICER cannot observe it because of sun angle constraints.
We asked the Nu-STAR team for a follow-up,
and they observed it from 02:50 UT on Dec. 23.
They detected the source at 71 arcsec away from AX J1848.8-0129 ( ATel #14290 ). But it is marginally within the positional error, and they could not reach a conclusion.
Active binary star AT Microscopiumnews-1273 December 17, 2020 by Mihara
MAXI detected a flare from AT Mic at 19:11 UT on 2020 December 12, with the intensity of 300 mCrab. Considering that the distance to AT Mic is 35 light-years from the earth, the X-ray power was as huge as 10^25 W, which is 1/10 of the optical solar luminosity. AT Mic consists of two dwarf M-type stars with emission lines (dMe stars). Size of each star is about 40 % of the sun.
Solar flare and Si from Crew Dragonnews-1272 December 3, 2020 by Mihara
A large solar flare occurred around 2020 November 29 13:00 UT. Reflected X-ray on the Crew Dragon around the nose cap was seen with MAXI. The spectrum showed a strong Si line. It would be the fluorescent X-ray from the Crew Dragon material.
A0535+26 in its highest fluxnews-1271 November 26, 2020 by Mihara, Nakajima
The Be X-ray binary pulsar A 0535+26 has brightened since the report of two weeks ago. MAXI team reported the giant outburst ( ATel #14173 ). After the periastron passage the pulsar remains in the high level against expectation. It is twice higher than the 2009's outburst (figure). In fact, in the 10-20 keV range it is about 10 Crab. It is much brighter than the Crab nebula in the daily image on 2020.11.24 (figure).
A0535+26 in the giant outburstnews-1270 November 14, 2020 by Mihara, Nakajima
MAXI detected a slight X-ray from the Be X-ray binary pulsar
A 0535+26 at 2020/11/3 20:46.
It locates next to the Crab nebula (Figure), both in the constellation Taurus.
The orbital phase was 0.90, whereas the orbital period of the system is 111 day.
The system makes, but not always, an outburst near periastron (phase=0).
Sometimes it is a normal outburst of about 200 mCrab, and rarely it is
a giant outburst reaching 1 Crab.
We were watching the growth of the X-ray light curve, meanwhile a group
reported the outburst on Nov. 6
( ATel #14157 ).
On Nov. 12 it reached almost 1 Crab and it clearly means a giant outburst.
The light curve and hardness curve are shown in the figure ( ATel #14173 ).
Latest light curve and hardness curve .
GRB 201021Bnews-1269 October 22, 2020 by Mihara
MAXI nova alert system triggered an uncatalogued bright X-ray source (210 mCrab) at 2020-10-21 16:18:55UT in the constellation Tucana. We reported it as a gamma-ray burst GRB 201021B (GCN #28726). The star was not detected in the previous (14:46 UT) nor the next (17:51 UT) MAXI scans.
Superburst from Aquila X-1 and NICER follow-upnews-1268 October 15, 2020 by Mihara
MAXI detected a superburst from the neutron-star low-mass X-ray binary
Aquila X-1 on 2020 October 8, 16:59 UT
( ATel #14079 ).
The luminosity was about a half of the Eddington luminosity
( = 40000 times of the sun)
and the temperature was 2.0 keV ( = twenty million K).
We waited for the next scan at 18:32 when the burst was still going on,
and confirmed it the superburst lasting for hours, not an X-ray burst lasting
for 100 s.
We issued an alert mail and also informed the NICER team at 19:55. Since Aql X-1 had been in an outburst for a month ( MAXI Light curve ) and NICER had been observing it every day, NICER could quickly turn the telescope and started the observation at 20:05, that is 10 minutes after the mail. It was the quickest record.
Short X-ray burst from the UCXB 4U 1820-303news-1267 October 8, 2020 by Mihara
MAXI detected an X-ray burst from the neutron-star low-mass X-ray binary
4U 1820-303 in the globular cluster
in the constellation
at 2020/10/6 01:32.
It lasted for 10s (figure), which is categorized in the
short (~15 s) X-ray burst. (see
MAXI news #1256 figure 2)
The shortness comes from the He burning.
The system is an ultra compact X-ray binary with a neutron star and a low-mass star. The orbital period is only 11 minutes. The separation of the two stars is only 120,000 km, which is 1/3 of earth-moon distance. The low-mass star is probably a white dwarf. The surface would consist of Helium. Then the short burst and the ultra compact orbit is related.
Flare from the active binary UX Arinews-1266 September 17, 2020 by Mihara
MAXI detected a flare from UX Arietis at 7:59 UT on 2020 September 13.
The flare lasted for 12 hours and the peak intensity was 100 mCrab (figure).
The luminosity was one million times of the largest solar flare.
UX Ari is a 6 magnitude star located at 6 degrees north-west of the Pleiades
star cluster. The distance from the earth is 165 lt-yr by GAIA.
It is a RS CVn type variable, that is, a close binary system with a K-type subgiant star and a small G-type main-sequence star. They rotate around each other by 6.4 days orbital period. The system with this combination is very active.
Record high X-ray from dwarf nova SS Cygnews-1265 September 11, 2020 by Mihara, Negoro
MAXI recorded the highest X-ray flux 40 mCrab from the dwarf nova SS Cyg. Increase of flux stared around 2018 October ( ATel #13744 ) and were succeedingly reported by MAXI news #1237 in 2019 July and MAXI news #1253 in 2020 May. The average X-ray flux is about 10 times higher then before. It is the highest in the 25 years since 1995 when RXTE/ASM started monitoring. The optical flux in the quiescence is also 2.5 times higher than before and may be the highest in the 110 years since 1909.
Aql X-1's 13th outburst triggered by Swift/BAT, radio, and opticalnews-1264 September 3, 2020 by Mihara
Aquila X-1 is a neutron-star low-mass X-ray binary known since 1973.
It repeats bright outbursts lasting for a month in roughly once in a year.
According to the MAXI light curve (figure), the current outburst is the 13th one.
This outburst was first suggested with the Swift/BAT on 2020 August 9
and the brightest radio from this source on August 12
( ATel #13016 ).
Optical monitoring had detected a brightening from 18.1 mag. to 16.7 mag.,
at least by one magnitude (= 2.5 times) (ATel #13020, 13953, 13981).
( ATel #13029 ,
( ATel #13953 ,
( ATel #13981 ).
They expected emergence of MAXI's X-ray around 20 August.
MAXI did detect X-ray on August 31 after the source came out of the un-scanned region.
Extrapolating the light curve, the rise might be about August 27.
MAXI J1216-655 : Very Fast X-ray Transientnews-1263 August 27, 2020 by Mihara, Negoro
MAXI found a faint transient MAXI J1216-655 in the
constellation musca on 2020 August 9 in one-day bin light curve
( ATel #13946 ).
Peak flux was 30 mCrab in 4-10 keV in 00h-04h UT on Aug. 9.
It went down < 10 mCrab on Aug. 10.
On Aug. 15, Swift performed a 7-point tiling observations covering the whole MAXI's error region ( ATel #13951 ) (figure). But, there was no new source. There was one supernova remnant, G299.2-02.9. MAXI J1216-655 would have faded out below < 0.1mCrab in the 5 days. It might be a very fast X-ray transient (VFXT) like MAXI J1957+032 ( ATel #7504 ).
The nature of the source is unknown.
AT2019wey : Mysterious slow transientnews-1262 August 20, 2020 by Mihara, Negoro
The optical transient AT 2019wey was discovered by ATLAS telescope on 2019
Dec. 7 in the constellation Camelopardalis.
Spectrum Roentgen Gamma satellite discovered the X-ray source
on 2020 Mar. 18
( ATel #13571 ).
X-ray brightening has been monitored by Swift and NICER since Apr. 12.
The type of this source remains uncertain.
We made a long-term MAXI light curve of the source
( ATel #13948 ).
There was no X-ray before the optical discovery. At the discovery there was a possible X-ray flare at 00:13 on 2019 Dec. 6, in only one scan. In the next observation period from Dec. 30 to 2020 Jan. 18, MAXI detected a significant X-ray (~3.4 sigma level). So, AT 2019wey had already started the X-ray emission before the SRG detection. The X-ray intensity has kept increasing exponentially since then to date. Thus, MAXI can trace back the past activities even after a later notice.
XTE J1829-098 : hot summer outbursternews-1261 August 13, 2020 by Mihara
MAXI detected a slight enhancement (~ 20 mCrab) of X-ray
in the constellation Scutum
on 2020 July 31, August 6, and August 10.
The source positions are consistent with the Be X-ray pulsar XTE J1829-098.
Since the discovery on 2004 July 31
( ATel #317 ),
XTE J1829-098 made outbursts on 2008 August 4 with RXTE
( ATel #2007 ),
2018 August 6 with MAXI
( ATel #11927 )
and this time.
All of the four were around the beginning of August of the even-number year,
suggesting 2 years is a multiple of the orbital period of the binary.
X-ray flares from the second youngest pulsar (and also a magnetar) AX J1846.4-0258news-1260 August 7, 2020 by Mihara, Negoro
The MAXI/GSC nova alert system triggered a weak X-ray transient source
at 07:49 UT on 2020-07-30 (59060 MJD) in the one-day accumulation
( ATel #13922 ).
The source position was (R.A., Dec) = (281.47 deg, -2.63 deg)
= (18 45 53, -02 37 33) (J2000) with a statistical error of 0.26 deg
and a systematic error of 0.1 deg.
There were three scans (2020-07-30 01:38, 03:11, and 04:44 UT) with a significant X-ray flux (see MAXI nova page 2 : Possibly AX J1846.4-0258 , scan No. 13, 14, and 16, respectively). The averaged flux over the three scans was 50 +- 15 mCrab in 4.0-10.0keV. There was no significant excess flux in the previous transit at 00:01 UT (scan No. 12) and in the next transit at 06:17 UT (scan No. 17) with an upper limit of 20 mCrab for each.
However, there were several scans with less significant (~2 sigma) fluxes (~30 mCrab). They are previous scans at 07-28 00:03 (page 1 : No. 22) and 01:36 (page 1 : No. 23), 07-29 11:41 (No. 4) and 14:47 (No. 6), and a next scan at 07-30 21:46 (No. 28). Here the page 1 refers to here, AX J1846.4-0258
There were three known sources in the error region. On 2020-08-01 20:11 UT Swift/BAT detected a flare from AX J1846.4-0258, which is one of the three sources (GCN #28187 and ATel #13913 ).
AX J1846.4-0258 is the second youngest (700 yerars old) pulsar in our galaxy (and also a magnetar) and shows a magnetar-like activity (Gotthelf et al. 2000).
Intermittent detections with MAXI from 2020-07-28 to 07-30 are consistent with the flaring behavior of the source. Therefore, the X-ray fluxes which MAXI detected would also come from AX J1846.4-0258.
Spectrum tells the bright flare was from SFXT XTE J1739-302news-1259 July 17, 2020 by Negoro, Mihara
MAXI detected a bright X-ray (~300 mCrab) from ~2 degrees west of the
Galactic center (GC) at 9:34 UT on 2020 July 9
( ATel #13871 ).
There were no detections in the previous and the next MAXI scans.
The short flare reminds us an X-ray burst, but there is no X-ray burster
in the region. The spectrum can be fit by a 2 keV blackbody,
typical for an X-ray burst, but an interstellar gas absorption is not needed.
It is unusual for an X-ray source near the GC.
Another kind of X-ray sources with short (~1000s) flares is supergiant fast X-ray transient (SFXT). There is one SFXT in the region in fact, XTE J1739-302. MAXI detected a short flare in 2015 ( ATel #6900 ), too. The spectrum can also be fit with a power-law with the photon index of 1.5 and the galactic absorption of 5 x 10^22 cm^-2. Those are reasonable values for a SFXT and we conclude the flare was from XTE J1739-302.
Intermediate duration X-ray burst from IGR J17062-6143news-1258 June 25, 2020 by Mihara, Iwakiri
MAXI detected a bright (~ 2 Crab) X-ray burst from IGR J17062-6143
at 2020 June 22 8:15 UT
in Ara constellation (
ATel #13827 )
It was a rare "intermediate duration X-ray burst" lasting a few hours
(see figure 2 of
MAXI news #1256 ),
and was shining when
NICER turned the telescope at 3.0 hours after the MAXI detection.
Such a long X-ray burst were reported in 2012
( ATel #8241 )
from this source.
Since the discovery in 2008
( ATel #1840 ),
observations have revealed that
the spin period of the neutron star (NS) is 6.1 ms,
the orbital period of the binary is 38 minutes and
the distance from the Earth is about 30,000 lt-years
(Strohmayer et al. 2017).
It is the NS low-mass X-ray binary.
The separation of the two stars is only 0.5 of the solar radius.
Such a small system is called "ultra compact X-ray binary (UCXB)".
Somehow, the long burst tends to occur in UCXB.
(see also MAXI news #1254 )
SpaceX crew-Dragon shadows (DEMO-2)news-1257 June 18, 2020 by Mihara
SpaceX crew-Dragon space ship (DEMO-2) docked the ISS on May 31, 2020. Since then, right ends of 25 degrees in the MAXI horizontal camera and 10 degrees in the zenithal camera are shadowed (figure). Because the X-ray in the MAXI's energy band cannot penetrate the star ship, Dragon hides X-ray stars behind it, including the now-outbursting GRO J1008-57 ( MAXI news #1252 ). The shadow moves on the sky with 70-day precession period as arrows in the figure. The shadowed part is a little bluer (harder X-ray) in the figure, since the Dragon stops the cosmic X-ray background (CXB), while the particle background is still there which is harder than the CXB.
Short X-ray burst from GRS 1747-312news-1256 June 11, 2020 by Mihara, Negoro, Serino
MAXI detected a short spike at 5:50:13 UT on June 5, 2020 from the constellation Scorpius. The X-ray emission lasted only for 4 s (figure 1). There locates the low-mass X-ray binary GRS 1747-312, which is known to emit short X-ray bursts. An X-ray burst is a sudden thermo-nuclear burning on the surface of a neutron star. The duration distribution is spread in 10-100 s with two peaks at about 15 s and 80 s (figure 2). Those are interpreted as He fuel (15 s), and mixed (H and He) fuel (80 s), respectively. The reason that GRS 1747-312 always emits short X-ray bursts is considered as that H is slowly burning into He on the surface, and since the accumulation time in GRS 1747-312 is relatively long, all of H has turned to He when a burst ignites.
Short X-ray burst from GRS 1747-312. S and E are when the source is in the MAXI field of view. The burst occurred in the middle.
Taken from "Understanding superbursts" MAXI 7year conference proc. p121 In't Zand (2017)
Flares ! from sleeping GRS 1915+105news-1255 June 4, 2020 by Mihara, Iwakiri
At 15:20 UT on 2020 May 26, MAXI detected a strong (~1 Crab) X-ray from GRS 1915+105 in Aquila. It is known as a violently variable blackhole binary since 1992, but recently has darkened and kept undetected with MAXI ( MAXI news #1232 , ATel #13652 ). Responding to the alert mail from MAXI, through OHMAN ground route, NICER quickly observed the source at 16:31. GRS 1915+105 was still in the bright flare and NICER recorded excellent data of rapid variations shorter than 0.1 s, "strange cycles of X-ray emission", and blowing-out iron lines. 1 hour 11 minutes has become the shortest record of OHMAN. The conditions were lucky, as MAXI's detection with zenithal cameras and NICER's observation at the next rise from the horizon.
Long X-ray burst from MAXI J0911-655news-1254 May 28, 2020 by Mihara, Iwakiri
MAXI detected a bright (~ 1 Crab) X-ray burst from the globular cluster
NGC 2808 in the constellation Carina at 17:04 on May 22, 2020 (
ATel #13754 ).
It contains the low-mass X-ray binary MAXI J0911-655 discovered in 2016 (
ATel #8872 ).
Since the discovery, it kept shining at about 10 mCrab in X-ray (
MAXI news #1242 ).
The distance from the earth is 31000 light-year.
The neutron star is an accreting ms pulsar
(Pspin=2.9 ms, Porbit = 44.3 minutes, Sanna et al. 2017).
This X-ray burst was long-lasting (~100 minutes), and
this kind of the X-ray burst is known to occur in the ultra-compact binary
like MAXI J0911-655.
NICER quickly turned the telescope by the command from the ground, and observed the source at 18:57 successfully ( ATel #13760 ). It was 1 hour 53 minutes after the MAXI detection and became the quickest record of the MAXI-NICER connection.
MAXI X-ray image at burst detection at 17:04 on May 22, 2020. The intensity was about 1 Crab. In the next MAXI scan at 18:37, it had faded to about 100 mCrab.
Dwarf nova SS Cyg getting brighternews-1253 May 21, 2020 by Mihara, Negoro
MAXI found X-ray flux from SS Cygni has been continuously increasing since around 2018 October ( ATel #13744 ). The activity was reported in MAXI news #1237 in 2019 July. Since then the X-ray flux has kept increasing, and reached about 30 mCrab in 2020 May. It is the highest flux that MAXI has ever observed from SS Cyg since 2009 August. Comparing the MAXI data with the optical data by AAVSO, both fluxes are increasing (figure). Usually X-ray is emitted only at the beginning and the end of an optical outburst (Wheatley et al. 2003), and optical flux is low between the outbursts. So, it is very strange that X-ray and optical flux remains high even between the outbursts.
GRO J1008-57 starting a giant outburstnews-1252 May 14, 2020 by Mihara, Nakajima
MAXI is monitoring the activity of the Be X-ray binary pulsars.
A normal outburst was reported in
MAXI news #1206 .
The data in the recent several days shows that GRO J1008-57
seems to start a giant outburst.
Figure is the X-ray flux in log scale
vs. orbital phase. The orbital period is 250 days
and phase zero is set at the periastron passage.
The light curve (pink) is tracing that of the giant outburst in 2012
(green) very well.
After a normal outburst at phase -0.05 the flux has kept in a constant level, and at phase 0.24 it dropped once and started to rise immediately after it.
The BeXRB monitor by ESAC/ESA summarizes the data from MAXI, Swift/BAT and Fermi/GBM.
Now the activity of GRO J1008-57 is ranked at the top.
( A snap shot was taken on May 28 2020 ).
Recent light curve of GRO J1008-57 in pink (updated on May 22 at the time of ATel #13750 ). It traces the light curcve of the giant outburst in the 2012 in green. Two kinds of outbursts, normal and giant ones, are shown in black and others.
SGR 1935+2154 became activenews-1251 April 30, 2020 by Mihara, Sugita
MAXI detected two bright short bursts from the Soft Gamma-ray Repeater
SGR 1935+2154 on 2020-04-27
The first one was at 20:01:45.99 UT
and had a double-peaked light curve with a total duration of only ~100 ms
The peak width was 5ms and the peak flux was about 75 Crab in the 2-20 keV band,
for each pulse.
The second burst started at 21:56:02.63 UT and had a single-peaked structure
with a width of 50 ms. This peak flux was about 40 Crab in 5 ms.
The activity was first reported from Swift/BAT at 2020-04-27 18:26:20 UT (GCN #27657, ATel #13675 ). and Fermi/GBM at 2020-04-27 18:26:20.16 UT (GCN #27659). NICER, INTEGRAL, AGILE, Konus-Wind, and HXMT also detected the SGR activities.
This was the second detection of the short burst from SGR with MAXI. The first one was also from SGR 1935+2154. It was 2016 Jun 20 (GCN #19545).
Light curve of the first short burst from SGR 1935+2154 with MAXI. The X axis is the time in sec. The red line indicates the burst duration, which was only 0.1 s. There were two spikes in the burst. The Y axis is the count rates. The bin size is 5 ms. Each step corresponds to one photon. For example, the highest peak had 9 photons in 5 ms. The detector area was about 9 cm2. Those yields about 200 c/s/cm2.
GRB 200205A -> Swift J0840.7-3516news-1250 February 13, 2020 by Mihara
MAXI detected a bright (72 mCrab) uncatalogued X-ray source at 2020 February 5 06:54 UT in the southern constellation Pyxis
The position was consistent with the gamma-ray burst GRB 200205A triggered
at 06:35. But it was 19 minutes ago.
In the next MAXI scan at 07:16 the intensity increased to
262 mCrab in 4.0-10.0 keV. This is unusual. There is no GRB whose afterglow is
brighter than the prompt emission.
In the third scan at 8:27 it started to decrease down to 66 mCrab.
The X-rays in the MAXI prior transit at 05:43
and in the next transit at 08:49 were not detected, < 20 mCrab for each.
The light curve is very peculiar (Figure).
Swift reported a detection of 9 s pulsation and renamed it Swift J0840.7-3516 ( ATel #13452 ). However, the pulsation was not confirmed with NICER and the star faded out ( ATel #13456 ). The spectrum and the rapid time variations are similar to those of a black hole. 9 s pulsation might be a quasi periodic oscillation (QPO) seen from a BH. So, the nature of the star remains unknown.
Light curve of GRB 200205A, later renamed as Swift J0840.7-3516. Light curve is very peculiar as a GRB. It is also peculiar as a galactic transient.
Violent flares from XTE J1901+014news-1249 December 5, 2019 by Mihara
On December 3 2019 MAXI detected a flare (80 mCrab) from XTE J1901+014 in the constellation Aquila ( ATel #13328 ). The flare lasted only for two scans separated by 90 minutes. Looking back the MAXI alerts, it was the third detection with MAXI after 2012 and 2015. The source was discovered with the former all-sky monitor RXTE/ASM in 2002 ( ATel #88 ). But in reality the first detection was in 1997. Swift/BAT detected flares in 2006 and 2010, which lasted for only from tens of seconds to hundreds of seconds ( ATel #2375 ). XMM and Chandra localized the position, but there is no optical or infrared star ( ATel #1268 ). The spectrum with ROSAT, RXTE and Integral is a simple power-law in a wide range of 0.6 - 100 keV ( Karasev et al. 2007 ). These properties are similar to the violent-type of the black hole binary such as V4641 Sgr and V404 Cyg. However, the nature of this source remains unknown.
Be X-ray binary RX J0209.6-7427 in Magellanic bridgenews-1248 November 28, 2019 by Mihara
MAXI discovered a faint (23 mCrab) source near Small Magellanic Cloud (SMC) on 2019 November 20, and named it MAXI J0206-74 ( ATel #13300 ). By the follow-up observation with Swift/XRT it was identified as RX J0209.6-7427 ( ATel #13303 ). The source was discovered in 1993 with ROSAT and was identified to a Be star ( Kahabka and Hilker 2005 ). This time , too, a strong and broad H alpha emission line was detected with SALT telescope in South Africa, which indicates an active phase of the Be star ( ATel #13307 ). IRSF telescope also detected a little brightening in infrared ( ATel #13315 ). By the following NICER observation the 9.29 s pulsation was discovered ( ATel #13309 ). The system was turned out to be a Be X-ray binary pulsar located in the Magellanic bridge, which is a gas stream connecting SMC and LMC (figure). The distance is 200,000 lt-yr from Earth. Although it looks dim apparently, it is very luminous in fact, three times as bright as the Eddington luminosity.
Location of MAXI detection. The Be X-ray binary RX J0209.6-7427 lies on the Magellanic bridge. It was born in SMC and travelling in the vast space for 200 million years.
Massive star binary Eta Carinae is activenews-1247 November 14, 2019 by Mihara
MAXI detected an X-ray increase from Eta Carinae on 2019 November 5 and 6. Usually it is 5 mCrab, while it is 10 mCrab now. It is a very massive star binary (~90 and ~30 solar masses). The X-ray outburst occurs in every 5.54 year, which is considered to be the binary period. After the peak the flux drops sharply probably due to the eclipse of the X-ray emitting shock region in the stellar wind by the primary star. The previous drop was around 2014 August 2 and the next one is expected on 2020 February 16. The flux has already started to increase towards that day.
MAXI 10 years light curve of Eta Carinae. X-ray has started to increase towards the periastron in 2020 February.
MAXI J0637-430 : New black hole was foundnews-1246 November 5, 2019 by Mihara
MAXI discovered a new source MAXI J0637-430 on 2019 November 2 in constellation Columba ( ATel #13256 ). The spectrum was soft and the 2-4 keV flux was 60 mCrab. Swift performed a follow-up observation on November 3 and confirmed an uncatalogued new X-ray source ( ATel #13257 ). The spectrum was disk-blackbody of 0.9 keV temperature with a hard power-law tail, which is typical for a black hole transient. It is the 13th black hole binary that MAXI discovered. The UV telescope (UVOT) on Swift also detected a new bright star (15th magnitude). A follow-up spectroscopy of the star was carried out by a ground telescope in Chile on November 3 and they found a double-peaked strong H alpha emission line, which would come from an accretion disk ( ATel #13260 ). The dim and soft X-ray state indicates a far distance of about 10 kpc. The star would be a black hole low-mass X-ray binary wandering far in the galactic halo.
New black hole binary MAXI J0637-430 was discovered on 2019 November 2. The red color of the source indicates that it emits soft X-ray.
A Be X-ray binary pulsar became activenews-1245 October 24, 2019 by Mihara
When MAXI recovered from the power-saving operation (2019.10.18-20),
the Be X-ray binary pulsar (BeXBP) XTE J1858+034 had
already started an outburst
( ATel #13217 )
following the previous one in 2011
( ATel #3766 ).
The intensity was about 20 mCrab. Swift/BAT also confirmed the outburst.
The BeXBP generally has an outburst at the periastron passage
of the elongated orbit, but not always.
This is the fifth outburst of XTE J1858+034 in history.
The discovery was in 1998
( Paul and Rao 1998 ).
The pulse period of XTE J1858+034 is 221 s, while
the orbital period is not known.
Nova ? No, again. Transient Swift J1845.7-0037 = XMMSL1 J194555.4-003941news-1244 October 17, 2019 by Mihara
MAXI detected an outburst in the constellation Aquila on 2019 October 11
( ATel #13189 ).
The X-ray intensity changed violently between 20 mCrab and 190 mCrab in Oct. 12-13.
The followup observation of Swift on Oct. 14 identified the source to the known Swift J1845.7-0037
( ATel #13191 ).
It had been detected by Swift/BAT with 15-30 mCrab on 2012 May 16, and followed by Swift/XRT with 4 mCrab on 2012 http://maxi.riken.jp/star_data/J1911+005/J1911+005.html May 24 ( ATel #4130 ).
Far before that, XMM-Newton observatory had discovered the source, XMMSL1 J184555.4-003941, on 2005 September 20 during the slew at 0.1 mCrab. The quiescence at 0.1 mCrab was also observed serendipitously by Swift/XRT on 2011 June 27. There is an infrared star of 15th magnitude.
However, the nature of this source still remains unknown.
Nova ? No. Neutron star transient GRS 1747-312news-1243 October 3, 2019 by Mihara
MAXI detected an outburst from the region
near (2 degrees south of) the galactic center
on 2019 September 29
( ATel #13154 ).
Followup observations of Integral and Swift identified the source to
( ATel #13155,
It is a binary of a neutron-star (NS) and a low-mass star in the globular cluster Terzan 6.
The distance is 24000 lt-years.
The peak flux is 50 mCrab, corresponding to
an X-ray power of 6 x 10^29 W, which is 1500 times larger than the emission of the sun.
It repeats an outburst every about half a year
( in't Zand et al. 2003 ).
The X-ray binary with this luminosity range repeats outbursts in every ~100 days
due to the instability of the accretion disk.
It is similar to Aql X-1 in the MAXI News on 2019 August 8.
Long-lasting MAXI nova MAXI J0911-655news-1242 September 26, 2019 by Mihara
MAXI detected an X-ray increase from MAXI J0911-655 on 2019 September 24.
It is a MAXI nova discovered on 2016 February 19
and also detected independently by Swift BAT (Swift J0911.9-6452).
Observations with X-ray telescoples of Swift/XRT
identified MAXI J0911 as a star in the globular cluster NGC 2808,
which is source 15 in
Servillat et al. (2008).
NGC 2808 is a large globular cluster at the distance of 31000 lt-years.
MAXI J0911 is the longest-lasting MAXI source. The X-ray flux is about 10 mCrab for the three years.
It brightened up by 10000 times since the first Chandra observation.
XMM-Newton and NuSTAR observations found a pulsation of 2.9 ms ( Sanna et al. 2017).
It once faded out in 2019 June (ATel #12831), and this time MAXI detected a reflaring.
(left) The globular cluster NGC 2808 taken by Hubble Space Telescope. (c) NASA, ESA, A. Sarajedini (University of Florida) and G. Piotto (University of Padua)
(right) MAXI J0911-655 was the source 15 in the Chandra image. The two circles are core radius and half-mass radius of the globular cluster. Taken from figure 1 in Servillat et al. (2008).
MAXI J1820+070 rebrightened again. It also did 100 years agonews-1241 September 5, 2019 by Mihara
When the ISS changed the attitude back for 60S docking in late August,
the black hole binary MAXI J1820+070 moved into the scan area of MAXI's good cameras.
Then by chance, MAXI detected a rebrightening of MAXI J1820+070 on 2019 August 24.
It was discovered with MAXI on 2018 March 11, faded out,
and rebrightened to make a small outburst on 2019 March 21.
This time (~30 mCrab) is the second rebrightening.
Recently optical astronomers found in the digital archive that MAXI J1820+070 had made outbursts in 1898 and 1934 (ATel #13066), suggesting that the outbursts repeat with a recurrence period of about 40 years. The astronomers who took photographs 100 years ago would never have thought that they had taken photographs of a blackhole binary.
An outburst of MAXI J1820+070 taken in photographs in 1898. The star had become as bright as this time in 2018.
"Missing-link" object, accreting ms pulsar SAX J1808.4-3658 starts an outburstnews-1240 August 15, 2019 by Mihara
MAXI detected an X-ray from the accreting ms pulsar SAX J1808.4-3658 on 2019 August 9,
following the optical on July 25
on August 6.
X-ray flux with MAXI was about 40 mCrab, which is consistent with the latest Nu-star observation on August 11
SAX J1808.4-3658 is the first ms pulsar in a binary system
( Wijnands & van der Klis 1998).
The pulsation is 2.5 ms, which is considered to result from
the acceleration by the mass accretion from the companion star.
It makes an outburst in about every 3 years, and this is the eighth outburst.
Recurrent transient Aql X-1 starts an outburstnews-1239 August 8, 2019 by Mihara
MAXI detected a start of an outburst from Aql X-1 on August 5, 2019.
It is a neutron star binary with a low-mass star.
Due to the instability of the accretion disk around the neutron star,
Aql X-1 makes a bright outburst in every about 300 days
(Asai et al. 2012).
The previous outburst was detected by MAXI on November 18, 2018.
Aql X-1 in MAXI HP.
Blackhole binary EXO 1846-031 woke up after 34 years of quiescencenews-1238 August 2, 2019 by Mihara
MAXI detected a X-ray transient in the constellation Aquila
on 2019 July 23
There are two known X-ray sources in the MAXI error circle.
The transient has increased to about 100 mCrab on July 28,
and Swift/BAT identified it as EXO 1846-031.
EXO 1846-031 was a black hole binary discovered in 1985 (Parmar et al. 1993). The outburst lasted for half a year, and then went into a quiescence. This outburst is since then after 34 years.
The follow-up observation with Swift/XRT was performed only 1 hour and 10 minutes after the MAXI alert, and obtained the source position as accurately as 2 arcsec (ATel #12969), which is 10 times better than before. There are still two infrared-cataloged stars within the error circle. The next day the VLA detected radio emission from the source and the position was determined with the accuracy of 0.03 arcsec (even 100 times better) (ATel #12977). Neither of the two infrared stars is EXO 1846-031.
MAXI detected X-ray outburst from SS Cygnews-1237 July 25, 2019 by Mihara
MAXI detected an X-ray increase from SS Cyg on 2019 July 22
following the detection on 2019 February 3.
The flux was about 15 mCrab for both.
SS Cyg has become active in 2019.
SS Cyg is a dwarf nova at 374 light-years away. It is a non-magnetic cataclysmic variable (CV = a white dwarf binary). SS Cyg makes an optical outburst in every about 50 days. Compared to the optical light curve, the X-ray detections with MAXI were not at the peak, but almost at the end of the outbursts. It is consistent with the light curve taken with RXTE (figure, Wheatley et al. 2003). When the accreting matter becomes less, the plasma turns to optically thin and the temperature rises. Then it starts to emit X-ray.
Optical, UV, and X-ray light curves of the dwarf nova SS Cyg with RXTE taken from Wheatley et al. (2003).
Soft MAXI gamma-ray burst GRB120714A was in fact an X-ray flare of a M-type starnews-1236 July 17, 2019 by Mihara
MAXI detected a bright (230 mCrab) X-ray transient in
the constellation Hercules at 13:20 UT on 2019 July 14
MAXI team reported it as GRB 190714A.
Swift promptly performed followup observations in about 3 hours later,
and found an X-ray star with 2 mCrab
The location was consistent with an M-type star named UCAC4 525-061488 in 113
light-years away. It was also a cataloged X-ray source, 2E 1624.6+1504.
The prompt followup revealed that the MAXI detection was not a gamma-ray burst, but a flare from the nearby M-type star.
MAXI's soft gamma-ray burst GRB190708B was in fact a soft tail of the GRBnews-1235 July 15, 2019 by Mihara
MAXI triggered a bright uncatalogued soft X-ray transient at 19:49:58 UT on 2019 July 8
in the constellation Pegasus
The X-ray flux was 394 +- 60 mCrab (4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 19:29
and in the next transit at 21:02 UT with an upper limit of 20 mCrab for each.
KONUS/WIND detected a gamma-ray burst at ~240 s before the MAXI trigger
So the MAXI source was the tail, or early afterglow of the GRB.
There was a faint source in the Swift/XRT follow-up observations
in 16 hours later
and it faded in the following observation
after 6 days. The swift source was the afterglow of the GRB
X-ray flare from sigma Gem, a RS CVn type variablenews-1234 June 20, 2019 by Mihara
MAXI detected a flare from sigma Gemini at 01:03 UT on 2019 June 19.
The flare was about 80 mCrab and lasted for about ten hours.
Sigma Gem is at 125 light-years and a 4-magnitude star locating just next to Pollux.
It is a binary star which consists of a K-type giant star
and a smaller main-sequence star.
This type of binary is called as the RS CVn variable.
This combination is active due to the large sun spot on the K giant star.
The previous flares from sigma Gem with MAXI occurred on February 4 and January 24, 2019.
MAXI J1348-630 rebrightenednews-1233 June 6, 2019 by Mihara
MAXI detected X-ray rebrightening of the black hole candidate MAXI J1348-630
It was discovered with MAXI on 2019 January 26 (58509 MJD)
and had a peak in intensity on February 11.
The outburst declined and once disappeared on May 11.
Then usually the X-ray nova goes to a quiescent state. But MAXI J1348
reappeared on May 31 and is still getting brighter and brighter.
X-ray light curves of MAXI J1348-630 with MAXI (top) and Swift/BAT (middle). A distance 3 kpc is assumed. The bottom curve is the hardness ratio between BAT and MAXI. After once it fainted out on 2019 May 11 (58614 MJD), it started shining again on May 31 (58634 MJD). We can tell the spectral states by the hardness ratio (HR). That with HR ~ 1 is the hard state, and that with HR ~ 0.1 is the soft state.
GRS 1915+105 woke up ?news-1232 May 16, 2019 by Mihara
Flares from the micro-quasar GRS 1915+105 were detected by MAXI/GSC
on 2019 May 14 (ATel #12761).
One of the peak flux reached 316 +/- 30 mCrab (1 sigma error) in 2 - 20 keV.
The 15 - 50 keV flux by Swift/BAT exceeded 1000 mCrab.
The source was in an unusual low-flux state (90 mCrab with MAXI)
for the last one year (ATel #11828, #12742, #12743, #12755).
We are watching whether GRS 1915+105 is going to the quiescence (ATel #12755),
or becoming active again.
Recent X-ray light curves of GRS 1915+105. The flux went down to zero level, and suddenly some flares occurred.
Cyg X-3 in the quench statenews-1231 April 25, 2019 by Mihara
Cyg X-3 is a mysterious star. We do not know exactly what kind of a star it is.
A blackhole binary has been suggested.
The X-ray flux and spectrum changes violently (figure).
Since February 2019, Cyg X-3 entered a quenched state
It is a rare state when the radio emission drops down and
X-ray spectrum changes to a pure blackboby (ultra soft state).
It was the 4th during MAXI 10 years of observations.
The quench state ended on April and a strong radio was emitted
At the same time, a hard X-ray emerged in the MAXI spectrum
as the hardness ratio went up in the figure.
Recent Cyg X-3 went into the fourth radio quench state, or X-ray ultra soft state.
LIGO/Virgo O3 startednews-1230 April 11, 2019 by Mihara
The operation 3 (O3) of LIGO/Virgo gravitational wave detectors has
started. The first event S190408an
occurred at 18:18:02.29 UT on 2019 April 8,
which is likely a BH-BH merger
MAXI/GSC was operating at the instant and scanning a small part of the GW
error region. However, there was no flaring event.
Within one orbital period of ISS, MAXI covered about 82% of the 90%
There was no event again, whose 1-sigma upper limit was 28 mCrab in 2-20 keV
(The O3 was terminated on March 27, 2020 due to COVID-19.)
Short GRB, GRB 190503A detectednews-1229 March 6, 2019 by Mihara
MAXI detected an X-ray increase of 100 mCrab at 2019 March 5 13:07:43 UT
in the constellation Phoenix (GCN #23933).
Swift/XRT follow-up found 6 X-ray sources (#1-6) within MAXI error circle
At about 13:05:18, which was
2 minutes before the MAXI detection, gamma-ray satellites :
AGILE, CALET, Konus-Wind, INTEGRAL, Swift, and Insight-HXMT had detected a
very-strong short (1.8 s) Gamma-ray burst
(GCN #23930, GRB 190305A).
IPN localization by Konus, INTEGRAL and BAT is consistent with the #1 source
MAXI's detection would be an "extended X-ray emission" of a short GRB.
If this is the case, it is the first one for MAXI.
We note that a short GRB is the most promising candidate of a NS (neutron star) - NS merger.
Gamma-ray light curves are available from Konus-wind page.
MAXI's error circle and localization with IPN, and Swift/XRT. Taken from GCN #23936 and the link in it http://www.ioffe.ru/LEA/GRBs/GRB190305_T47118/IPN/
4U 1901+03 revealednews-1228 February 20, 2019 by Mihara
On 2019 February 8, MAXI detected X-ray brightening
from the binary X-ray pulsar 4U 1901+03
This is the fourth X-ray outburst in 40 years of X-ray astronomy history,
after the ones in 1970, 2003 and in 2011
(Sootome+ ATel #3829).
The flux was 120 mCrab on Feb. 9 and will reach the maximum
of 300 mCrab around Feb. 24 (figure is on Feb. 20).
Because 4U 1901+03 locates on the milky way in the constellation Aquila,
the optical star was not identified due to crowdedness and absorption.
But this time, precise follow-up observations have changed the situation.
The location was obtained precisely by Swift/XRT and
there was an infrared star
NICER observations were performed
(ATel #12515) suggesting a Be star.
The Chandra archive had detected 3 X-ray photons from this star
The GAIA has shown the distance to this star, 2.9 kpc.
X-ray all-sky map on 2019 February 20. The marked bright source is 4U 1901+03. The color blue means a hard spectrum. X-ray binary pulsars appear in blue.
Swift J1728.9-3613 appearednews-1227 February 6, 2019 by Mihara
On 2019 January 26, MAXI detected an X-ray increase from the constellation Scorpius.
We first misidentified this source as EXO 1722-363 (ATel #12437).
On Jan. 28 Swift/BAT detected it independently, and reported it as a new source
Swift J1728.9-3613 (ATel #12436).
It was followed up by Swift/XRT (ATel #12445) on Jan. 28 and NICER (ATel #12455) on Jan. 29.
The spectrum and the quasi periodic oscillation indicate that it is a black hole binary.
It reached a peak of 0.5 Crab on Feb. 2.
X-ray all-sky map on 2019 February 1. Three novae are shining brightly in the southern sky. All of them have turned out to be blackhole binaries.
MAXI J1348-630 was discoverednews-1226 January 30, 2019 by Mihara
MAXI discovered an X-ray nova MAXI J1348-630 in the constellation Centaurus
at 03:16 UT on 2019 January 26 (ATel #12425).
Swift/XRT obtained the precise location (ATel #12434).
There is a 16 magnitude star
(ATel #12430) getting brighter (
NICER observation suggests that it is a black hole binary
MAXI J1348-630 has reached 1.5 Crab on January 30 (figure).
Now it is the second brightest star in the X-ray sky.
Discovery of MAXI J1631-479news-1225 January 13, 2019 by Mihara
MAXI discovered a bright hard X-ray transient source at 04:33 UT on December 21, 2018 in the constellation Norma ( ATel #12320).
The intensity was 209 +- 27 mCrab (4-10 keV).
The Swift/BAT also detected it with flare-like behavior.
There exists the 1309 second X-ray pulsar AX J1631.9-4752/IGR J16320-4751.
But the MAXI intensity was about 10 times higher than the previous observations.
The Nu-STAR X-ray telescope made a follow-up observation on Dec.28 ( ATel #12340). The MAXI star was 0.21 degrees away from AX J1631.9-4752 (figure), and was found to be a new star. The name is MAXI J1631-479. The X-ray spectrum taken with the Nu-STAR indicates that MAXI J1631-479 would be a black hole binary. Then it is the fifth new black hole found with MAXI in 2018.
MAXI light curve of MAXI J1631-479. Taken from MAXI HP.
It became very bright, more than 1 Crab.
X-ray image taken with Nu-STAR X-ray telescope. White circle is the error circle which MAXI reported. AX J1631.9-4752 is in the error circle, but the new star is not AX J1631. MAXI J1631-479 is a new star.
The magnetar XTE J1810-197 woke upnews-1224 December 20, 2018 by Mihara
MAXI has detected another new faint source at (272.6, -19.6) since the end of November (see the figure in the previous news).
Radio telescopes reported intense flares from the magnetar XTE J1810-197 on Dec 9 and 11 after 10 years of quiescence
( ATel #12284,
Since the locations coincide, MAXI's source seems to be XTE J1810-197
( ATel #12291).
(MAXI light curve : XTE J1810-197).
Nu-STAR TOO observations confirmed that this X-ray source is XTE J1810-197 indeed ( ATel #12297). It is a magnetar, which was discovered at the outburst in 2003. Magnetars are faint. XTE J1810-197 is the only magnetar whose emission is detected with MAXI.
Discovery of MAXI J1810-222news-1223 December 12, 2018 by Mihara
MAXI discovered a new source, MAXI J1810-222, on December 1, 2018 in constellation Sagittarius
( ATel #12254).
This is a peculiar source which emits only soft X-ray below 4 keV.
The 2-4 keV intensity was 20-40 mCrab (Figure).
Looking back the MAXI data, the source appeared in the beginning of November.
Such long-lasting soft X-ray source is unusual.
It can be a neutron star binary in a low state, a bright blackhole binary at a far distance, or a new kind of X-ray source.
Since the source locates close to the Sun with the separation of about 25 deg, X-ray followup observation is impossible with Swift and NICER. It is only possible with Nu-STAR, the hard X-ray telescope.
Nu-STAR carried out 25 tiling observations on Dec. 9 and confirmed the existence of MAXI J1810-222 ( ATel #12283). The position is better determined with an accuracy of 2 arcminutes (=0.03 deg.) The spectrum is similar to that of the soft state of a black hole.
MAXI 2-4 keV X-ray image of MAXI J1810-222 and aother new source. They appeared among 5 bright X-ray stars. The new source (indicated "unknown" in the figure) was found to be a magnetar XTE J1810-197 (see the next news).
Rapid variability from Swift J1858.6-0814news-1222 November 7, 2018 by Mihara
MAXI confirmed an X-ray emission (4 mCrab) from Swift J1858.6-0814
( ATel #12163),
which was discovered with Swift/BAT on 2018 October 25
( ATel #12151).
The source showed flaring variabilities as
NICER detected an X-ray increase by a factor of a few hundred in 15 s
( ATel #12158).
Such fast variability is very rare among X-ray binaries.
Magnetic white dwarf AM Herculesnews-1221 October 17, 2018 by Mihara
On October 10, 2018, MAXI detected an X-ray increase from the white dwarf (WD) binary, AM
It is a persistent source of a few mCrab, but has brightened to 10mCrab,
the bightest in the 2 years.
This star is categorized as "Polar", which shows a strong optical polarization, resulted
from the strong magnetic field (100 M Gauss = 10^4 T) of the WD.
The binary period is 3.1 hour. The star locates 286 light-years away.
Two Be X-ray binary pulsars made outburstsnews-1220 October 10, 2018 by Mihara
MAXI detected outbursts from the two Be X-ray binaries,
A 0535+26 and GRO J1008-57
( ATel #12092).
They are binaries of a pulsar (neutron star) and a B-emission type star.
Brightening of A 0535+26 was found on 2018 September 22,
and that of GRO J1008-57 was on 2018 September 30.
(MAXI homepage : A 0535+26, GRO J1008-57)
Their binary orbits are eccentric. The binary stars become the closest in every 111 days and 250 days (orbital period). Sometimes around the periastron, but not always, the stellar gas falls onto the pulsar and an X-ray outburst starts. The Be X-ray binary pulsar is one of the major categories in X-ray binaries.
MAXI J1820+070 goes back to the hard statenews-1219 September 26, 2018 by Mihara
The black hole candidate MAXI J1820+070 showed a soft-to-hard spectral transition on September 22 ( ATel #12057).
The soft state, whose emission is from the standard accretion disk, lasted from 2018 July 1 (58300 MJD) to September 22 (58383 MJD).
(MAXI homepage : MAXI J1820+070. MAXI-BAT light curve).
Light curves of MAXI J1820+070 with MAXI and Swift/BAT, and their intensity ratio.
Outburst from H 1743-322 again and againnews-1218 September 18, 2018 by Mihara
The blackhole binary, H 1743-322, in Scorpio is brightening. It reached 100 mCrab on September 18 with MAXI. This outburst was found by the INTEGRAL observatory (ESA) on September 3, 2018 at 40 mCrab ( ATel #12007). It was a 408 day after the previous outburst, and actually the 12th outburst detected by MAXI in 9 years (Figure). H 1743-322 repeats outbursts in 200 - 400 days due to the accretion-disk instability. MAXI (X-ray) and Swift/BAT (gamma-ray) have been watching the activity.
Repeated outbursts from H 1743-322 in 9 years with MAXI and Swift/BAT. The bottom is the BAT/MAXI intensity ratio. A distance of 34,000 light-year is assumed.
Stellar flares FT Psc and CF Tucnews-1217 September 6, 2018 by Mihara
MAXI detected two stellar flares this week. One is from FT Psc at 14:31 UT on September 1, 2018 ( ATel #12016). The instensity was 160 mCrab. This detection was the second one following that on May 1, 2017. FT Psc is a 10-magnitude small star of spectral type dMe at 38 light-year, but is very active in X-ray. Another flare was from CF Tuc at 07:24 UT on September 3 2018 ( ATel #12009). The intensity was 150 mCrab. This is the second detection with MAXI following that on January 30, 2012 ( ATel #3897). It is a RS CVn type binary at 290 light-year, which is a star-pair with a very high X-ray activity.
GRB180809A with MAXI, Calet/GBM, Fermi/GBM and Swift/XRTnews-1216 August 23, 2018 by Mihara
MAXI detected a Gamma-ray burst GRB180809A on 2018 August 9 11:38:25 in the constellation Sagittarius ( GCN #23103 ). The intensity was 2 Crab. Calet/GBM, which is mounted on ISS, also detected it (GCN#23117) as well as Fermi/GBM (GCN#23118). Since both are non-imaging detector, MAXI was the only one that could localize the position. Being informed by MAXI, after 4-6 hours, the X-ray telescope Swift/XRT searched the MAXI error circle by 7 tiling and found an X-ray afterglow of 1.5 mCrab (GCN#23106). It had decayed out below 0.01 mCrab on 5 days later (GCN#23141). An optical telescope searched the region after 73 minutes from the MAXI detection, but there was no new star brighter than 20 magnitude (GCN#23107). There is no known galaxy at the position. The GRB180809A must have exploded in a very distant galaxy.
MAXI image of GRB180809A at detection.
Mysterious star Cir X-1 flared upnews-1215 July 18, 2018 by Mihara
MAXI detected Cir X-1, which flared up suddenly from under detection level (<30mCrab) to 250 mCrab on 2018 July 12 16:53 UT.
In the next two scans (90 and 180 minutes later) it stayed at 50 mCrab,
and then it flared up again to 150 and 300 mCrab in the following two scans.
( MAXI alert page of Cir X-1 ).
The spectrum was shaped as a blackbody of 1.2 keV ( = 10 million degree K).
Cir X-1 is a peculiar binary consisting of a neutron star with weak magnetic
fields and a Be star.
In 2013 a supernova remnant was found around it and the age is estimated to be younger than 4600 years (Heinz et.al (2013) ApJ 779 171).
The flares occur near periastron of the 16.6 day orbit, but not always. The last flare was 130 days ago.
The flare lasts only for some hours to a few days. Violent behavior of the
X-ray emission still remains ununderstandable.
Latest MAXI light curve of Cir X-1
MAXI X-ray light curve of Cir X-1, which started to flare up on July 12.
The Demon Star fired up in X-raysnews-1214 July 11, 2018 by Mihara
MAXI detected a large X-ray flare from Algol at 2018-07-04 05:52 (UT) ( ATel #11812).
The flux was 300 mCrab. It was the largest among 14 flares which MAXI observed from Algol
in 8 years.
Distance to Algol is 90 light-years. Then the X-ray luminosity was 7 x 10^25 W,
which is 1/6 of the optical energy of the sun !
Algol is an eclipsing variable star.
The orbiting period is 2.86 day. MAXI team predicted an eclipse (in X-ray ! ) of this flare.
MAXI's alert was followed by NICER, and NICER successfully detected the flare and the eclipse (Figure).
From these observations, location and evolution of the huge X-ray flare will be analyzed.
The overall view of the "Demon" star will be revealed.
Latest MAXI light curve of Algol
X-ray light curve of Algol which flared up on July 4, 2018.
MAXI detection was followed by NICER observations.
Gamma-ray burst GRB 180701A was detectednews-1213 July 4, 2018 by Mihara
At 06:47 UT on July 1, 2018, MAXI detected a gamma-ray burst GRB180701A ( GCN #22880) in constellation Aquarius. The intensity was 74 +- 19 mCrab, and it shone only for 10 s. It was so weak that the nova search program did not find it. Instead, a graduate student found it. Although GRB occurs one in every day, it is rather rare that it occurs in the MAXI field of view (2% of all-sky). This event was the second GRB for MAXI in 2018.
List of MAXI GRBs
X-ray image of GRB 170701A at detection.
Taken from MAXI alert page of GRB 180701A.
NS-LMXB 4U 1608-52 started an outburstnews-1212 June 27, 2018 by Mihara
On June 19 2018 MAXI detected a sudden X-ray increase from the neutron-star
low-mass X-ray binary 4U 1608-52 in constellation Norma.
The star is usually under MAXI detection (quiescence) and occurs an outburst intermittently about every year.
It is because the accretion disk around the neutron star is unstable for this mass accretion rate.
Spectral ratio (HR = Swift/BAT counts / MAXI/GSC counts) is an indicator of a spectral state (Figure).
On June 20, 4U 1608-52 made a spectral state transition from hard to soft state as HR went down below 0.2.
On June 22, it reached 700 mCrab and is staying in an almost flat level since then.
Latest MAXI light curve of 4U 1608-52
Rise of an outburst of NS-LMXB 4U 1608-52.
Taken from Spectral hardness monitor with MAXI and BAT.
4U 1608-52 is listed by the name of H 1608-522.
Blackhole binary MAXI J1727-203 was discoverednews-1211 June 6, 2018 by Mihara
MAXI J1727-203 was discovered by MAXI in constellation Ophiuchus at 9:41 UT
on June 5, 2018 ( ATel #11683).
In response to the MAXI's ATel, NICER on ISS tuened the X-ray telescope
and confirmed the new source at 15:40 UT ( ATel #11689).
The intensity is 150 mCrab now (June 6, 3h UT) and increasing.
The spectral transition which was observed by MAXI, and the spectrum taken
with NICER both indicate the source is likely a blackhole binary ( ATel #11696).
Latest MAXI light curve of MAXI J1727-203
MAXI J1727-203 at discovery.
MAXI J1727-203 appeared at a blank position (red cross). No.3 source is a bright LMXB GX 9+9. No.7 is a weak X-ray source Ophiuchus cluster of galaxies. No.1 is Kepler's SNR which is too soft to be deteced by MAXI/GSC.
Superburst from the neutron star binary SAX J1712.6-3739news-1210 May 16, 2018 by Mihara
MAXI detected an X-ray brightening from SAX J1712.6-3739 on May 8, 2018 ( ATel #11636). The source is in the constellation Scorpio, and was discovered in 1999 by the Italian X-ray satellite BeppoSAX. The distance is 23,000 lt-years and almost as far as the Galactic center. The source is known to be a close binary of a neutron star and a low-mass star because it sometimes exhibits an X-ray burst. It is a thermo-nuclear-fusion runaway on the surface of a neutron star. The burst lasts for 10-100 seconds. Meantime, about 10^19 kg of H and He burns, and emits X-ray with 100,000 times more energy per second than the light from the Sun per second. Surprising on May-8 burst was that it had already started 8 minutes ago, as detected by Swift/BAT ( ATel #11623). It turns out a "super burst", which is a rare phenomenon known to us only recently since around 2000. It lasts for some hours, and emits 100 times more energy than a regular X-ray burst. Only about 16 superburst-sources are known.
Blackhole binary MAXI J1535-571 dimmed outnews-1209 April 24, 2018 by Mihara
The X-ray nova with a blackhole,
MAXI J1535-571, decayed under MAXI detection last week (2018 April 16, MJD 58224).
( ATel #11568).
It appeared on September 2, 2017
It reached 5 Crab on September 19 and shone as the brightest X-ray nova
in the 21st century.
MAXI had monitored the X-ray flux for 7 months after the discovery
( MAXI light curve of MAXI J1535-571).
It started to decay more rapidly around March 26, 2018
when the flux went down to 1 % of the peak.
Then the peak in late September is supposed to be the Eddington luminosity.
The distance can be calculated about 30000 light years.
MAXI operation has been extended for another 3 years (2018.4 - 2021.3.) by JAXA. MAXI will find more and more X-ray novas.
MAXI-BAT light curves of MAXI J1535-571Taken from http://maxi.riken.jp/home/asai/maxibatHR/
A distance of 11 kpc was assumed for flux-luminosity conversion.
IGR J17379-3747 was a ms pulsarnews-1208 April 11, 2018 by Mihara
MAXI detected a postive flux (37 mCrab) from the gamma-ray source
IGR J17379-3747 on March 19 2018 ( ATel #11447).
This source was discovered at the outburst in 2004 by the INTEGRAL satellite. The system was turned out to be a binary of a neutron star and a low-mass star. It had an outburst again in 2008, when Swift/XRT determined the accurate position ( ATel #1714). At the MAXI detection of the 3rd outburst this time, VLA radio observatory poionted the position and detected a radio flux on March 22 ( ATel #11487). It means that a compact jet was emitted just like a ms pulsar.
Follow-up observation by NICER on ISS which has a good timing capability in fact detected an X-ray pulsation of 2.1 ms (468 rotations per second !) on March 29 ( ATel #11507). NICER also measured the orbital period, which is only 1.88 hours, and then the companion star weighs only 0.06 solar mass (or somewhat heavier).
Thus MAXI's detection triggers many observations, which in cooperation reveal a secret of the nature.
ATel : Astronomer's Telegram http://www.astronomerstelegram.org
X-ray nova MAXI J1820+070news-1207 March 27, 2018 by Mihara
The X-ray nova MAXI J1820+070 is now the second brightest star in the X-ray sky.
MAXI J1820+070 was discovered by the Japanese payload MAXI on ISS on March 11 2018
( ATel #11399).
J1820+070 means the location (alpha, delta) = (18h 20m, +7.0deg) in J2000 coordinate. It is in Ophiuchus.
MAXI is monitoring the flux in every ISS orbit (~90minutes).
At first it was only 30 mCrab. It gradually brightened up and reached 2 Crab on March 21.
Since then in this week, it has stayed in almost the same brightness till today (March 27).
Many follow up observations are carried out by Swift, NICER on ISS (USA), XMM-Newton, Integral (ESA), HXMT (China), as well as many optical and radio observatories.
It is revealed to be a binary of a blackhole and a normal star.
Crab is the unit of X-ray flux. 1 Crab is the flux from the Crab nebula.
MAXI J1820+070 on 2018 3 23.
Shift of onset orbital-phase of the normal outburst in GRO J1008-57news-1206 January 30th, 2018 by Nakajima and Mihara
MAXI/GSC detected X-ray
birghtening from the Be/X-ray binary pulsar GRO J1008-57 from 2018
January 23 (MJD 58141) ( ATel #11244 ).
The onset of this outburst occurred at the orbital phase of 0.90,
using the the orbital parameters, T0=54416.65 (MJD)
and Porb=249.48 d (Kühnel et al. 2013).
In 2009-2015 season, MAXI/GSC observations showed that the onset phase of the normal outbursts was in a narrow range (0.92-0.93) in orbital phase. However, the last 4 normal outbursts started from the orbital phase of 0.91. The shift of the outburst onset might imply that the geometrical parameters of the circumstellar disc around the Be star have changed.
Folded light curves of outbursts in GRO J1008-57.Latest MAXI light curve of GRO J1008-57
Brightest blackhole nova ever in MAXI historynews-1205 September 29th, 2017 by Tatehiro Mihara
MAXI discovered the X-ray nova MAXI J1535-571 in constellation Norma at 2017 September 2nd 23:55 UT (57998 MJD)
( ATel #10699 ).
In 4 hour prior to it (20:00 UT) Swift/BAT discovered it independently ( GCN #21788 ).
More 5 hours prior to it (14:41 UT) MAXI nova-search program had detected it automatically.
Further observation with MAXI revealed that it is a black hole binary ( ATel #10708 ). The brightness of MAXI J1535-571 kept rising and finally reached 5 Crab on September 19th (58015 MJD). It has become the brightest X-ray nova ever in MAXI history. Appearance of an X-ray nova brighter than 3 Crab was for the first time in 18 years since 1999. In other words, MAXI J1535-571 is the brightest X-ray nova in this century. In fact, it is the seventh brightest blackhole X-ray nova in history [ Top list of Blackhole nova]．
MAXI all-sky map on 2017 September 19th
MAXI light curve of MAXI J1535-571Latest MAXI light curve of MAXI J1535-571
We will hold an international conference,
7 years of MAXI : Monitoring X-ray Transients
on 5-7 December, 2016
at Suzuki Umetaro Hall, RIKEN
2-1 Hirosawa, Wako, Saitama, 351-0198, Japan
It is just three months ahead !
Program is available and Registration page is open at
We call for contributed talks/posters.
The deadline of registration is 30 September 2016.
Please join us.
On July14, 2016, MAXI instrument was awarded for b01Innovation in Earth and Space Scienceb01 in the b012016 ISS Research and Development conferenceb01 held in San Diego, USA. Organizers of the conference, which are American Astronautical Society (AAS), NASA and CASIS, select a top research in each of seven categories in the ISS R&D every year.
MAXI has been observing the X-ray sky for seven years since August,
2009. MAXI team issued 350 Astronomerb01s telegrams noticing variability
in the X-ray celestial bodies to the world-wide astronomers. MAXI data
is open from MAXI homepage in Riken, which contains light curves and
spectra of blackhole binaries and X-ray binary pulsars, etc. They are
used in more than 150 refereed papers in the high energy astronomy.
In February, 2016, the first detection of gravitational wave (GW) was reported by LIGO team. MAXI scanned the GW source region in 4 b01 30 minutes after the event and obtained an upper limits for an X-ray emission. Next GW event may occur in the field of view of MAXI. Combination of MAXI with new instruments will make MAXI more valuable. They are CALET (high energy electron and gamma-ray detector) on JEM and NICER (X-ray telescope on ISS coming up in early 2017).
JAXA ISS news (2016.7.15) (in Japanese)
RIKEN topics (2016.7.22) (in Japanese)
MAXI presentation on ISS R&D conference (pdf 18MB) (2016.7.13)
Suzaku & MAXI special issue of PASJ (2016.6.1)
In the last four years, the Be/X-ray binary EXO 2030+375 has displayed an unusual behaviour: its X-ray activity decreased and type I outbursts were not detected at several periastron passages. At the same time, its pulse-period derivative changed from a constant spin up to almost zero (ATEL #8835). Optical observations revealed a large equivalent width of the H alpha line (ATEL #8927).
We report a shift of the outburst peak phase in the most recent (MJD 57589) type I X-ray outburst of EXO 2030+375. The peak flux of the latest outburst was ~30 mCrab on 2016 July 20 (MJD 57589) for both MAXI/GSC and Swift/BAT. This corresponds to an orbital phase of 0.015 (orbital ephemeris of Wilson et al. 2008) and represents a significant change from the almost constant value of ~0.13 for all the detected type I outbursts since 2007. The peak time changed from ~5 days after the periastron to ~0.7 days after the periastron.
In addition, the latest Fermi/GBM spin frequency measurement (2016 April 25) suggests that the source is now starting to spin down.
All these observations are strikingly similar to the events which occurred from January 1994 to October 1995. The X-ray flux decreased, leading to several undetected outbursts, followed by a slow transition to spin down. In October 1995, a sudden shift of the outburst peak time from ~5 days after the periastron to ~5 days before the periastron was observed (Wilson et al. 2002).
The first giant outburst was detected on MJD 46204 (1985 May). The peak could be 0-30 days earlier than this date. The orbital phase shift occurred at MJD 50040 (1995 October). The time between these events is of 3836 ~ 3866 days. The peak of the second giant outburst was around MJD 53960 (2006 May), which is 3920 days after the phase shift. The time between the second giant outburst and the current phase shift is of 3629 days. All these time spans are similar.
We strongly encourage optical and infra-red observations to better understand the origin of this apparently recurrent events.
The recent outburst compared to the last two brightest outbursts is shown below.
The latest evolution of the outburst can be followed at the BeXRB monitor page: http://integral.esac.esa.int/bexrbmonitor/ which combines data from MAXI/GSC, Swift/BAT and Fermi/GBM. This news has been posted to ATEL #9263.
On 2016 January 24 (MJD 57411), the MAXI/GSC nova-search system
detected an X-ray emission from the recurrent Be/X-ray transient pulsar,
GX 304-1 (ATel #8592).
The Swift/BAT also observed the brightening from January 23. The MAXI
trigger time corresponds to the orbital phase of 0.019 (adopting
Porb=132.189 d and To=55425.6 (MJD) ; Sugizaki et al. 2015). Thus the
present event is a normal outburst.
Comparing it with the recent four normal outbursts, we found that their onsets steadily shifted later and later (from ~0.90 orbital phase on 2014 December to 0.02 on 2016 January). Such a shift has been observed from three other Be X-ray binaries (GS 0834-430 ; Wilson et al. 1997, EXO 2030+375 ; Wilson et al. 2002, A0535+26 ; Nakajima et al. 2014). Although not all of the Be X-ray binaries show the shift, the shift of the outburst phase might be a common phenomenon in the Be X-ray binaries and it might be based on some physical mechanism.
The MAXI 2-20keV light curves of the recent 6 orbits of GX 304-1 from the top to the bottom. The horizontal axis is the orbital phase. A steady shift of the onset phase is seen in the succeeding 4 outbursts.
The neutron-star low-mass X-ray binary GS 1826-238 turned into a
soft state on June 8, 2014. This source remained in the hard state
since the discovery in 1988 (Cocchi et al, 2010, Ubertini et al. 1999, Barret et al. 1996, Tanaka 1989) including the recent five years of MAXI observation.
However, on 8 June 2014, the MAXI/GSC hardness ratio (7-20keV / 2-7 keV) showed a rapid drop from ~ 0.4 (previous level) into 0.1, which meant a softening. The 2-10 keV X-ray flux accordingly increased from 50 mCrab (before May 2014) to 140 mCrab (15 June 2014) (Fig.1). On the other hand, Swift/BAT light curve shows a decline in the hard X-ray band (15-50 keV) after 2014 June 8. The GSC spectra of the hard state and the soft state are shown in Fig.2. These results indicate that the source entered into a soft state for the first time.
Fig.1. Light curves with MAXI/GSC and Swift/BAT. The MAXI flux started to increase and the BAT flux started to decrease from MJD 56816 (2014/06/08). The two jumping points in MAXI at 56793 and 56815 MJD are X-ray bursts. The BAT light curve is taken from http://swift.gsfc.nasa.gov/results/transients/Ginga1826-238/ .
Fig.2. Spectra of the hard state (black, 56770- 56800 MJD) and the soft state (red, 56820 b01 56827 MJD) of GS 1826-238 with MAXI/GSC. The fit model is wabs*(diskbb+compbb). Now the disk-blackbody is dominabt in the soft energy band.
The GSC spectrum can be obtained through MAXI On-demand page http://maxi.riken.jp/mxondem/ .
The extremely bright GRB 140219A has been detected by MAXI/GSC. The position of the source was not in the field of view of any of GSC cameras. The photons came through counter walls, shields, or collimator sheets. Part of the signals might be produced by the Compton-scattered electrons induced by the gamma-rays.
The pulse period (about 7.6 s) and change rate of the pulse period (about -2.6 x 10-11 s/s) of the X-ray Binary Pulsar 4U1626-67 are obtained with MAXI/GSC data.
The pulse period (red points in the figure, plotted in frequency) was obtained in each 60-day MAXI/GSC data from MJD 55110 up to 56249. The results were superposed with those with Fermi/GBM (black points). MAXI data are consistent with the Fermi/GBM data. Each red bar with the red point represents an average change-rate of the pulse period with MAXI in the 60 days. The pulse period is getting shorter and shorter (= spinning up) with alomost a constant change rate.
The next figure shows residuals from a linear fit to the Fermi/GBM data. Red points and black points represent MAXI and Fermi/GBM data, respectively. The vertical axis is in frequency. MAXI data points have an error bar, but it is small enough as is sometimes included in the size of the red points. The data is V-shaped, and there is a break in the middle. We found that the flux after this point was brighter than that before. We interprete that amount of gas accreting to the neutron star increased at this point to cause an increase in the spin-up rate.