NICER Mission on the ISS and Initial Results of Magnetars T

NICER Mission on the ISS and Initial Results of Magnetars T. Enoto (Kyoto University) Z. Arzoumanian, K. Gendreau, and NICER Science Team

中性子星の観測と理論: 研究活性化ワークショップ2017 2017年11月25日@国立天文台

June 3, 2017 SpaceX CRS-11 Cargo Mission Launch Photo Credit: (NASA/Bill Ingalls) advertisement Neutron star Physics “Photonuclear reactions triggered by lightning discharge” Nature Letter, 2017 Nov. 23 NICER at home on ISS

3 NICER/SEXTANT — Overview

• PI: Keith Gendreau, NASA GSFC • Science: Neutron star structure, dynamics, & energetics through soft X-ray timing spectroscopy • Launched: June 3, 2017, SpaceX-11 resupply • Platform: ISS external attached payload with active pointing • Duration: 18 months baseline science mission; likely GO extension • Instrument: 0.2–12 keV “concentrator” optics, silicon-drift detectors, GPS absolute time tagging and position • Enhancements: – Demonstration of pulsar-based navigation – PI discretionary & ToO time • Status: – Installed on ISS June 13, 2017 – Commissioning complete, Phase E underway

Courtesy: Gendreau & Arzoumanian 4 Modeling surface emission to infer M-R Gravitational light-bending saves the day!

Weak Gravity

Courtesy: Gendreau & Arzoumanian 5 Inferring neutron star radii through lightcurve modeling — geometry

Bogdanov, Rybicki, & Grindlay, ApJ, 670, 668 (2007)

α=10°, ζ=30°

α=30°, ζ=60°

α=60°, ζ=80°

α=20°, ζ=80°

9 km

12 km for M = 1.4 M! 16 km}

Courtesy: Gendreau & Arzoumanian 6 NICER X-ray Observatory

~1.1 m ~0.8 m

~0.8 m

ExPRESS Logistic Carrier X-ray Timing Instrument = X-ray Concentrator (XRC) + Silicon Drift Detector ~109 m Soft X-ray (0.2-10 keV) NICER

• Large effective area (x2 of XMM-Newton at 1.5 keV) ISS • High time resolution (<300 ns time tag) Launch in 2016 7 X-ray Concentrator optics

Single reflection, grazing-incidence nested gold-coated Al foils

Courtesy: Gendreau & Arzoumanian 8 Detector plate

Radiation shielding

Au/Ag “traffic cone”

Pb collar

Pb disk

Courtesy: Gendreau & Arzoumanian 9 X-ray Timing Instrument (XTI) capabilities

A novel combination of sensitivity, timing, and energy resolution

• Spectral band: 0.2–12 keV • Timing resolution: < 100 nsec RMS absolute • Energy resolution: 140 eV @ 6 keV • Non-imaging FOV: 6 arcmin diameter • Background: < 0.5 cps • Sensitivity, 5σ: 1 x 10–13 erg/s/cm2 – 0.5–10 keV, 10 ksec (Crab-like) – ~3x better than XMM-Newton’s timing capability (PN clocked) • Max countrate: ~38,000 cps (3.5 Crab) – Deadtime accounted for in telemetry

Gendreau et al., SPIE (2012), Arzoumanian et al., (2014) 10 Launch! 2017 June 3

Launch! 2017 June 3

SpaceX CRS-11 Cargo Mission Launch June 3, 2017 Photo Credit: (NASA/Bill Ingalls)

Transport and installation (cont.)

Dragon and NICER proceed to ISS transfer orbit

20 Transport and installation (cont.) Extraction from Dragon was delicate…

Courtesy: Gendreau & Arzoumanian 21 Installation and Deployment … but not nearly as complicated as robotic installation!

Courtesy: Gendreau & Arzoumanian 22 Range of motion test

Courtesy: Gendreau & Arzoumanian 23 Watch NICER collect your photons! Occasional / on-demand live ISS video

24 The NICER Payload

25 Live ISS telemetry ~80% of the time

Cen X-3 pulsations in real time

Courtesy: Gendreau & Arzoumanian 26 Coordination across wavelengths and facilities Two targets, two ground-based telescopes, three successive ISS orbits GRS 1915+105

Ibaraki, Japan

Crab

GTC, Canary Islands

27 Crab Pulse Profile Observed with NICER the Crab Pulsar X-ray Proﬁle (ftools “efold”, all events) Crab Pulsar (PSR B0531+21) / NICER Relative Count Rate

0.94

0.80 1 0.5 1.2 1.4 1 1.6 1.5 2 Phase Crab Pulse Profile Observed with NICER Detection Significance of the Crab Pulsar Exposure required to the Crab Pulse Exposure for Detection of the Crab Pulsar (Real Data)

Exposure (sec) 0.1 1

1 Reduced chi-square Z22 0.1 Phase bin 34

0.01 3 sigma 10−3

10−4 Probability

10−5

10−6 5 sigma

10−7 1 10 100 Number of pulses Magnetar & Magnetosphere (M&M) Group

Young High-B • Covers highly magnetized neutron stars (NSs) • Diversity: magnetars, high-B pulsars, rotation-powered pulsars, X-ray isolated neutron stars • Baseline science in the NICER proposal…

• “Characterise spin variations and outbursts during glitches” • “NICER shall spectrally distinguish between thermal and non- thermal X-ray pulse spectra and measure their absolute phases to ±100 us(1σ)”

• “Phase resolved spectroscopy with NICER will probe line origins by localising absorption sites relative to the magnetic axis and any non thermal emission” • Monitoring of timing behaviours of fainter magnetars and high-B pulsars, and their spectral comparison B P P˙ • / ˙ Phase-resolved spectroscopy of rotation-powered and ⌧c = pP/(2P ) isolated NSs: absorption feature, thermal/non-thermal Low-B Old Magnetar & Magnetosphere (M&M) Group

Young High-B magneta • Covers highly magnetized neutron stars (NSs) rs high-B • Diversity: magnetars, high-B pulsars, rotation-powered pulsar pulsars, X-ray isolated neutron stars • Baseline science in the NICER proposal… rotatio n- • “Characterise spin variations and outbursts during glitches” powere • “NICER shall spectrally distinguish between thermal and non- d thermal X-ray pulse spectra and measure their absolute low-B (low- phases to ±100 us(1σ)” Pdot) • “Phase resolved spectroscopy with NICER will probe line magnetar origins by localising absorption sites relative to the magnetic axis and any non thermal emission” • Monitoring of timing behaviours of fainter magnetars and high-B pulsars, and their spectral comparison B P P˙ • / ˙ Phase-resolved spectroscopy of rotation-powered and ⌧c = pP/(2P ) isolated NSs: absorption feature, thermal/non-thermal Low-B Old Magnetar & Magnetosphere (M&M) Group

2 Pdot) − SGR 0501+4516 SGR 0418+5729 Swift J1822.3-1606 Swift J1834.9-0846 cm 4U 0142+61 origins by localising absorption sites relative to the magnetic

1 10 magnetar 10− − axis and any non thermal emission”

11 • 10− 1E 1547.0-5408 Monitoring of timing behaviours of fainter magnetars and high-B pulsars, and their spectral comparison X-ray ﬂux (erg s 12 B P P˙ 10− • / ˙ Phase-resolved spectroscopy of rotation-powered and ⌧c = pP/(2P ) isolated NSs: absorption feature, thermal/non-thermal 13 TE+2017 Low-B 10− Old 2004 2005 2006 2007 2008Gendreau 2009 2010 et al., SPIE 2011 (2012), 2012 Arzoumanian 2013 2014 2015 Year et al., (2014) Magnetar & Magnetosphere (M&M) Group

• Total 1.5 Ms exposure

• Targets: Priority A (12 sources), B (7 sources)

• (Reserved) ToO for transient sources (>200 ks) • Magnetar

• CXOU J164710.2-455216 — low-ﬁeld-13 magnetar? Outburst in 2006, CXOU precise measurement of Pdot (<4x10 , An+2013) with NICER J1647-45 • High-B pulsars • PSR J1119-6127 — radio pulsar to exhibit a magnetar-like outburst in 2016 July. Now in declining state. • Rotation powered

• PSR B0656+14 —ﬂux and timing variability analysis; non-thermal X- ray pulse to constrain the location of the high-energy emission • Absorption feature of isolated NSs

• 1E 1207.4-5209 — absorption features at 0.7 & 1.4 keV seen by XMM and Chandra. Other lines at higher energies, 2.1 and 2.8 keV?

NICER White Paper “Magnetar & Magnetosphere” Magnetar & Magnetosphere (M&M) Group

PSR • Total 1.5 Ms exposure J1119-61 • Targets: Priority A (12 sources), B (7 sources) • (Reserved) ToO for transient sources (>200 ks) • Magnetar

• PSR B0656+14 —ﬂux and timing variability analysis; non-thermal X- ray pulse to constrain the location of the high-energy emission • Absorption feature of isolated NSs

• 1E 1207.4-5209 — absorption features at 0.7 & 1.4 keV seen by XMM and Chandra. Other lines at higher energies, 2.1 and 2.8 keV?

NICER White Paper “Magnetar & Magnetosphere” Magnetar & Magnetosphere (M&M) Group

PSR • Total 1.5 Ms exposure J1119-61 • Targets: Priority A (12 sources), B (7 sources) • (Reserved) ToO for transient sources (>200 ks) • Magnetar

• CXOU J164710.2-455216 — low-ﬁeld-13 magnetar? Outburst in 2006, PSR CXOU precise measurement of Pdot (<4x10 , An+2013) with NICER B0656+14 J1647-45 • High-B pulsars • PSR J1119-6127 — radio pulsar to exhibit a magnetar-like outburst in 2016 July. Now in declining state. • Rotation powered

• PSR B0656+14 —ﬂux and timing variability analysis; non-thermal X- ray pulse to constrain the location of the high-energy emission • Absorption feature of isolated NSs

• 1E 1207.4-5209 — absorption features at 0.7 & 1.4 keV seen by XMM and Chandra. Other lines at higher energies, 2.1 and 2.8 keV?

NICER White Paper “Magnetar & Magnetosphere” Magnetar & Magnetosphere (M&M) Group

PSR • Total 1.5 Ms exposure J1119-61 • Targets: Priority A (12 sources), B (7 sources) • (Reserved) ToO for transient sources (>200 ks) • Magnetar

• CXOU J164710.2-455216 — low-ﬁeld-13 magnetar? Outburst in 2006, PSR CXOU precise measurement of Pdot (<4x10 , An+2013) with NICER B0656+141E J1647-45 • High-B pulsars • PSR J1119-6127 — radio pulsar to exhibit a magnetar-like outburst 1207-52 in 2016 July. Now in declining state. • Rotation powered

• PSR B0656+14 —ﬂux and timing variability analysis; non-thermal X- ray pulse to constrain the location of the high-energy emission • Absorption feature of isolated NSs

• 1E 1207.4-5209 — absorption features at 0.7 & 1.4 keV seen by XMM and Chandra. Other lines at higher energies, 2.1 and 2.8 keV?

NICER White Paper “Magnetar & Magnetosphere”

NICER Example: PSR B1509-58

21 P ~150 ms pulse proﬁle PSR Count / s 20 B1509-58 NICER (13 ks) 19 June 20 - July 11

13 0 0.2 0.4 0.6 0.8 1 1.2 1.4 1.6 1.8 2 Phase

• A 150-ms young rotation-powered pulsar for calibrations. • Pulse proﬁle and pulse-on-off (background free) spectrum are consistent with previous results. NICER Example: PSR B1509-58

PSR B1509−58 sum pulsed NH=1.19e+22cm−2, G=1.13, K=3.59e−3ph/cm2/s/keV@1keV

PSR − 1 keV B1509-58 − 1 Pulse on-off spectrum phabs * pow ﬁt

0.01 0.1 1 10 -11 2

normalized counts s Γ=1.1, F=(3.6±0.2)x10 erg/s/cm

− 3 agreement with Chen et al., 2015 10 ratio 01234 2510 Energy (keV)

• A 150-ms young rotation-powered pulsar for calibrations. • Pulse proﬁle and pulse-on-off (background free) spectrum are consistent with previous results. Magnetar Outburst : 4U 0142+61

• 4U 0142+61 — 8.9 s prototypical bright magnetar previously observed with most of 4U 0142+61 past X-ray observatories • Fermi GBM detected a SGR-like short burst at 23:54 UT on 13 July during the NICER’s commissioning phase (GCN 21342). • NICER follow-up ToO observations, ~0.88, 1.0, 2.0, 3.0, 4.0 days after the burst, from July 14 to 18 (total ~75 ks) • Signature of a glitch around the outburst from Swift monitoring (Atel 10576) • NICER observation was around the glitch? • Additional coordinated observations with NuSTAR on August 11 to search for the hard X-ray enhancement (magnetosphere). Magnetar Outburst : 4U 0142+61

• 4U 0142+61 — 8.9 s prototypical bright 4U magnetar previously observed with most of 0142+61 past X-ray observatories • Fermi GBM detected a SGR-like short burst at 23:54 UT on 13 July during the NICER’s commissioning phase (GCN 21342). • NICER follow-up ToO observations, ~0.88, 1.0, 2.0, 3.0, 4.0 days after the burst, from July 14 to 18 (total ~75 ks) • Signature of a glitchNICER around band the outburst from Swift monitoring (Atel 10576) • NICER observation was around the glitch? (previous result) • Additional coordinated observations with 4U 0142+61 NuSTAR on August 11 to search for the broad-band spectrum hard X-ray enhancement (magnetosphere). TE+2011 Magnetar Outburst : 4U 0142+61

NICER launchShort burst • 4U 0142+61 — 8.9 s prototypical bright June 3 magnetar previously observed with most of past X-ray observatories 1 month • Fermi GBM detected a SGR-like short burst at 23:54 UT on 13 July during the NICER’s commissioning phase (GCN 21342). • Signature of a glitch around the outburst 5.7912×10 4 135.792×10 4 145.794×10 154 5.796 16 ×10 4 5.798×10 4 5.8×10 4 from Swift monitoring (Atel 10576) • NICER follow-up ToO observations, ~0.88, 1.0, 2.0, 3.0, 4.0 days after the burst, from July 14 to 18 (total ~75 ks)

• 4U 0142+61 Swift NICER observation was around the glitch? monitoring • Additional coordinated observations with (C) Robert Archibald / NuSTAR on August 11 to search for the McGill U. hard X-ray enhancement (magnetosphere). (Previous outburst) Archibald+2017 Magnetar Outburst : 4U 0142+61

NICER launchShort burst • 4U 0142+61 — 8.9 s prototypical bright June 3 magnetar previously observed with most of past X-ray observatories 1 month NICER observations • Fermi GBM detected a SGR-like short burst just after the short burst at 23:54 UT on 13 July during the NICER’s commissioning phase (GCN 21342). • Signature of a glitch around the outburst 5.7912×10 4 135.792×10 4 145.794×10 154 5.796 16 ×10 4 5.798×10 4 5.8×10 4 from Swift monitoring (Atel 10576) • NICER follow-up ToO observations, ~0.88, 1.0, 2.0, 3.0, 4.0 days after the burst, from July 14 to 18 (total ~75 ks)

Pulse proﬁle of 4U 0142+61

Folded period: 8.68936000000000 s Norm Intens Ser 1

Relative NICER 0.9 1 1.1 0.4-12 keV in Outburst 0 0.5 1 1.5 2 Phase 1 2 5 Start Time 17949 0:16:43:996 Stop Time 17949 22:31:05:632 Energy 3 21 • Pulse period is consistent with the Swift result. − 1 0.8-4 keV • 20 Pulse proﬁle shows four-ﬁve peaks (two peaks at quiescent state). Additional hot spots on a stellar surface. Suzaku Counts / Counts sec Counts 19 in quiescent (a)• Phase-average spectrum is approximated with 2BB model of kT ~ 0.34 and 0.75 keV.

0.9 0 1.0 • Analysis of the data is underway. (Note)− 1 Epoch is not the same Phase 0.8 Counts sec Counts 0.7 (b)

− 1 0.62

Counts sec Counts 0.58 (c)

8 − 1

7.9 Counts sec Counts (d)

00.511.5 Phase PSR J1622-4950 — Radio-loud magnetar

Radio- • Most of magnetars are radio quiet. emitting • PSR J1622-4960 is one of rare radio- magnetars loud magnetars (~5 known), PSR discovered in 2009 at the Parkes radio J1622-4950 observatory. • Previous X-ray and radio observations in 2007-2011. Radio ceased in 2014 and remained undetectable during 2015-2016. • Radio re-brightening in 2017 (Atel 10346). X-ray ﬂux at 5x10-12 erg/s/cm2 (1-10 keV) from Swift on 27 April.

Ref: Levin+2010, Anderson+2012, Scholz +2017 PSR J1622-4950 — Radio-loud magnetar

• Most of magnetars are radio quiet. • PSR J1622-4960 is one of rare radio- loud magnetars (~5 known), discovered in 2009 at the Parkes radio observatory. • Previous X-ray and radio observations in 2007-2011. Radio ceased in 2014 and remained undetectable during 2015-2016. • Radio re-brightening in 2017 (Atel -12 (Anderson 10346). X-ray ﬂux at 5x10 erg/s/cm2 +2012) (1-10 keV) from Swift on 27 April.

Ref: Levin+2010, Anderson+2012, Scholz +2017 PSR J1622-4950 — Radio-loud magnetar

• Radio observations with Deep Space Network (DSN) 70-m diameter • at 2.3 and 8.4 GHz in Australia on 23 May 2015 (Atel 10581). Period is 4.327 sec. • NICER observations from July 8 to 18 with a total 7.5 ks exposure. -12 • NICER X-ray ﬂux ~5x10 erg/s/cm2 (2-6 keV).

• Obtained spectra are consistent with Swift follow-up observations in April-June 2017. • No pulsation detected with NICER. Pulsed Preliminary fraction upper-limit at 20% (3σ, 2-6 keV).

• 70% upper-limit in the 0.3-4.0 keV (3σ) from the previous XMM EPIC-PN observations (Levin X-ray / radio coordinated +2010). observations with NICER 19

Vela Pulsar — Simultaneous with Radio 19

19 • Vela Pulsar (PSR B0833-45) γ-rays • Rotation-powered, P = 89.3 sec • Variability in radio pulse peak intensity — stronger pulses arriving earlier than that of the average proﬁle

• X-ray/radio correlation — ﬂux of the main X- ray pulse is higher during the more intense radio pulses arriving earlier (Lommen+2007) X-rays • ➡ Non-thermal X-ray and radio emission are physically linked (Harding+2008) • Simultaneous radio observations at 26-m radio at Mt. Pleasant observatory in Tasmania. • NICER observations on July 7-21, NICER covers thermal and non-thermal emission NICER White Paper (C) Harding

Figure 9. Light curves of the Vela pulsar at radio to γ-ray energies. From ().

Radio observation at Mt. Pleasant / University of Tasmania (J. Dickey, J. Palfreyman et al.) X-ray pulses detected by XMM (Marelli et al. 2014) are very unusual in being 1/4 period out of phase with the gamma-ray pulses. Modeling of the γ-ray and X-ray profiles suggest that we could be seeing non-thermal X rays from the polar cap pair cascade for the first time. If so, the X-ray spectrum should be extremely hard and extend up to around 10 MeV (Timokhin & Harding 2015). This is unique behavior and the pulse profile and the extremely hard spectrum can be confirmed and extended to higher energy with NICER. Figure 9. Light curves of the Vela pulsar at radio to γ-ray energies. From (). PSR B0540-69: This is a young ( 103 yr), Crab-like pulsar in the Large Magellanic Cloud. It is a radio, optical ∼ and γ-ray pulsar with purely non-thermal X-ray emission. The pulse peaks at all energies are aligned in phase (Fermi LAT Collaboration et al. 2015), similar to the Crab pulsar, and is only the second young pulsar showing this behavior.X-ray pulses It recently detected was by observed XMM (Marelli to undergo et al. an2014 increase) are in very spin-down unusual rate in being of 36% 1/4 (Marshall period et out al. of2015 phase), that with could the Figure 9. Light curves of the Vela pulsar at radio to γ-ray energies. From (). begamma-ray a change pulses. in the magnetosphere Modeling of the involvingγ-ray and a change X-ray profiles in current suggest flow or that conductivity. we could be After seeing the non-thermal spin-downrate X rays change, from the pulsar polar cap breaking pair cascade index also for changed the first from time. 2.2to0 If so,. the031 X-ray(Marshall spectrum et al. 2016 should). Such be extremely an extremely hard low and breaking extend upindex to couldaround indicate 10 MeV a change (Timokhin in magnetic & Harding dipole2015 moment,). This asis unique flux is re-emerging behavior and from the the pulse neutron profile star and following the extremely suppression hard ofspectrumX-ray the initialpulses can field detected be confirmed by a by fallback XMM and diskextended (Marelli (Ho 2015 to et higher al.).2014 NICER energy) are observation withvery NICER. unusual will in verify being this 1/4 low period breaking out index of phase and with possibly the detectgamma-rayPSR other B0540-69: pulses. spin-down This Modeling stateis a young changes. of the (γ-ray103 andyr), X-ray Crab-like profiles pulsar suggest in the that Large we could Magellanic be seeing Cloud. non-thermal It is a radio, X rays optical from ∼ andthePSR polarγ-ray B0943+10: cap pulsar pair with cascade This purely older for (5 the non-thermal Myr) first radio time. X-ray pulsar If so, emission. the that X-ray exhibits The spectrum regular pulse should peaks mode-switching beat extremelyall energies on several-hourhard are and aligned extend timescales in phaseup to and(aroundFermi was LAT 10 recently MeV Collaboration ( observedTimokhin to et & show al. Harding2015 changes),2015 similar in). its This to pulsed the is Crab unique X-ray pulsar, behavior emission and andcorrelated is only the the pulse with second profile the young radio and mode-switching pulsarthe extremely showing hard (thisHo 2015behavior.spectrum). The can It X-ray recently be confirmed pulsations was observed and and extended spectrum to undergo to in higherthe an two increase energy radio inBright with spin-down NICER. and Quiet rate modes of 36% is ( diMarshallfferent, showinget al. 2015 strong), that thermal could pulsationsbePSR a change B0540-69: in in the the Q Thismagnetosphere mode is a and young non-thermal involving ( 103 yr), a unpulsed change Crab-like in emission current pulsar inflow in the the or B conductivity.Large mode. Magellanic Further After analysis Cloud. the spin-down It by isMereghetti a radio, rate change, optical et al. ∼ (theand2016 pulsarγ)-ray discovered breaking pulsar that with index weak purely also thermal changed non-thermal pulsations from 2 X-ray.2to0 also emission.are.031 present (Marshall The in the et pulse B al. mode2016 peaks). and Such at that all an both energies extremely modes are hadlow aligned breakingsome unpulsed in phase index could(Fermi indicate LAT Collaboration a change in magnetic et al. 2015 dipole), similar moment, to the as Crab flux is pulsar, re-emerging and is from only the the neutron second young star following pulsar showing suppression this ofbehavior. the initial It recently field by was a fallback observed disk to ( undergoHo 2015). an NICER increase observation in spin-down will rate verify of 36% this ( lowMarshall breaking et al. index2015 and), that possibly could detectbe a change other in spin-down the magnetosphere state changes. involving a change in current flow or conductivity. After the spin-down rate change, thePSR pulsar B0943+10: breakingThis index older also changed (5 Myr) from radio 2. pulsar2to0.031 that (Marshall exhibits regular et al. 2016 mode-switching). Such an extremely on several-hour low breaking timescales index andcould was indicate recently a change observed in magnetic to show changes dipole moment, in its pulsed as flux X-ray is re-emerging emission correlated from the with neutron the radio star following mode-switching suppression (Ho 2015of the). initial The X-ray field pulsations by a fallback and disk spectrum (Ho 2015 in the). two NICER radio observation Bright and willQuiet verify modes this is dilowfferent, breaking showing index strong and possibly thermal pulsationsdetect other in spin-down the Q mode state and changes. non-thermal unpulsed emission in the B mode. Further analysis by Mereghetti et al. (2016PSR) discovered B0943+10: that This weak older thermal (5 Myr) pulsations radio pulsar also are that present exhibits in the regular B mode mode-switching and that both on modes several-hour had some timescales unpulsed and was recently observed to show changes in its pulsed X-ray emission correlated with the radio mode-switching (Ho 2015). The X-ray pulsations and spectrum in the two radio Bright and Quiet modes is different, showing strong thermal pulsations in the Q mode and non-thermal unpulsed emission in the B mode. Further analysis by Mereghetti et al. (2016) discovered that weak thermal pulsations also are present in the B mode and that both modes had some unpulsed Vela Pulsar — Simultaneous with Radio

876 A. A. Danilenko et al. • Vela Pulsar (PSR B0833-45) • Rotation-powered, P = 89.3 sec

Danilenko et al., 2011 • Variability in radio pulse peak intensity — stronger pulses arriving earlier than that of the average proﬁle

• X-ray/radio correlation — ﬂux of the main X- ray pulse is higher during the more intense radio pulses arriving earlier (Lommen+2007)

• ➡ Non-thermal X-ray and radio emission are physically linked (Harding+2008) Red box: • Simultaneous radio observations at 26-m NICER range at Mt. Pleasant observatory in Tasmania. • NICER observations on July 7-21, NICER covers thermal and non-thermal emission

Radio observation at Mt. Pleasant / University of Tasmania (J. Dickey, J. Palfreyman et al.)

Figure 7. Multiwavelength unabsorbed spectra for the Vela and Geminga pulsars from the radio to hard γ -rays compiled from the data obtained with different instruments, as indicated in the plots. Mid-IR fluxes are marked by the circles. The squares mark the radio fluxes. The down-triangles mark upper limits.The filled squares in the radio range of Geminga are its radio detections by Malofeev & Malov (1997). observed mid-IR excess is much less significant. Nevertheless, the steep IR flux increase towards low frequencies cannot be excluded 4DISCUSSION by the derived mid-IR flux upper limits. This suggests that at sev- The subarcsecond positional coincidence of the detected point-like eral tens of µm the mid-IR flux density might be comparable with object at 3.6 and 5.8 µmwiththeVelapulsarcoordinatessuggests the soft X-ray thermal BB-like emission bump from the Geminga that this object is likely to be the mid-IR counterpart of the pulsar. surface (BB) and compatible with the low-frequency extension of This is also supported by the consideration of its spectral energy the non-thermal soft-X-ray spectral tail, as in the Vela case. distribution (SED), showing that the measured mid-IR fluxes are However, from the spectral behaviour of both pulsars shown in compatible with the long-wavelength spectral excess observed early Figs 6 and 7, it is most likely that the Spitzer mid-IR observations in the near-IR. The same is likely to be true for fainter Geminga, reveal us a new spectral component in the emission of these rotation- with a caution that its mid-IR counterpart candidate is detected powered pulsars, whose origin is different from those of the rest only marginally and solely in the 3.6-µm band. Additional confir- components detected early and perhaps from that of the Crab pulsar mation can be obtained from near-IR detections of both pulsars in in the mid-IR. the K band, where they have not been observed, and by deeper

C ⃝ 2011 The Authors, MNRAS 415, 867–880 C Monthly Notices of the Royal Astronomical Society ⃝ 2011 RAS Vela Pulsar — Simultaneous with Radio

NICER pulse proﬁle of Vela pulsar • Vela Pulsar (PSR B0833-45) (Preliminary) • Rotation-powered, P = 89.3 sec 21 ks exposure 0.4-3 keV • Variability in radio pulse peak intensity — stronger pulses arriving earlier than that of the average proﬁle

• X-ray/radio correlation — ﬂux of the main X- ray pulse is higher during the more intense radio pulses arriving earlier (Lommen+2007)

• ➡ Non-thermal X-ray and radio emission are physically linked (Harding+2008) • Simultaneous radio observations at 26-m at Mt. Pleasant observatory in Tasmania. • NICER observations on July 7-21, NICER covers thermal and non-thermal emission

Radio observation at Mt. Pleasant / University of Tasmania (J. Dickey, J. Palfreyman et al.) Giant Radio Pulses of Crab Pulsar

• Giant Radio Pulses (GRPs) 3% • sporadic & bright (~MJy) radio pulse emission 2-3 • ﬂux is 10 times stronger than regular pulses • detected from ~12 pulsars • randomly occur at either the main or inter pulses • power-law energy distribution (connection to FRBs?) Optical • Multi-wavelength GRP studies • optical enhancement has been discovered at GRPs Radi • 3% brightness increase @ Crab main pulse (Strader • Upper-limits in the higher energy (X-ray, gamma-ray) 0.98 0.99 Phase Radio coherent emission is somehow linked to incoherent radiation in optical-to-Xray? ➡ search for X-ray enhancement! (a few percent level enhancement?)

Shearer+2003, Bilous+2008, Majid+2011, Strader+2013, Lewandowska+2015 Giant Radio Pulses of Crab Pulsar

14 Publications of the Astronomical Society of Japan,(2014),Vol.00,No.0 Hitomi collaboration • Giant Radio Pulses (GRPs) χ2 2017 • –10keVbandwiththereduced of 305.85 and 301.18 for 250 VERITAS sporadic & bright (~MJy) radio pulse emission 1000 CGRO 2-3 degrees of freedom, respectively, as shown in the figure 6. The Fermi • CGRO flux is 10 times stronger than regular pulses pulsed flux obtained with Hitomi accumulated within the time Hitomi/SGD • detected from ~12 pulsars interval of ∆ϕ phase was summarized in table 6. Therefore, the Hitomi/SXS gamma-ray • randomly occur at either the main or inter pulse 3 σ upper limit values of enhancement in terms of flux can be 100 obtained by multiplying the values in table 5 (section 3.1) with Hitomi/HXI • power-law energy distribution (connection to FRBs?) Hitomi those in table 6. The upper limits of enhancements of MP-GRPs Suzaku Hale Tel. • Chandra Multi-wavelength GRP studies 10 in 0.02~0.03 phase in the X-ray flux in the 2 – 300 keV band within the phases of in wide-phase bin 12 2 •

MP-GRP Enhancement (%) Enhancement MP-GRP optical enhancement has been discovered at GRPs 0.20 or 0.03 become (24 or 3.3) 10− erg cm− ,respectively, opt. × 12 2 X-ray • and the same for IP-GRPs were (93 or 9.9) 10− erg cm− , William Herschel Tel. 3% brightness increase @ Crab main pulse × respectively. 1 • Upper-limits in the higher energy (X-ray, gamma-ray) 1 103 106 109 1012 Energy (eV)

4Discussion Fig. 7. The enhancement of MP-GRPs of Crab pulsar in various energy bands obtained by theHilliamHerschelTelescope (Shearer et al. 2003), With the simultaneous observations of the Crab with Hitomi and Hale telescopeRadio (Strader coherent et al. 2013), Chandra emission (Bilous et al. 2012), Suzakuis somehow linked to incoherent radiation Kashima radio observatory, the correlation studies in the X-ray (Mikami et al. 2014), Hitomi (this work), CGRO (Lundgren et al. 1995; Ramanamurthyin optical-to-Xray? & Thompson 1998), Fermi (Bilous et al.➡ 2011), search and VERITAS for X-ray enhancement! (a few percent band with about 1,000 GRPs have been performed (Section 2). (Aliu et al. 2012) All the upper limits shown in arrows represent 3 σ values. No significant changes in the X-ray pulse profiles were detected The red and blue cases indicate the enhancement measuredlevel in a short- enhancement?) along all the phase bins at the GRP cycles (Section 3), and the 3- phase width (∆ϕ = 0.02 – 0.03 phase) and wider-phase width (∆ϕ > 0.1), σ upper-limit values for the MP-GRPs in the 2 – 300 keV band respectively.Shearer+2003, Note that the thresholds Bilous+2008, of GRP detections Majid+2011, in the radio band Strader+2013, Lewandowska+2015 were different among them. with Hitomi were ξ = 22% and 80% within the time interval of ∆ϕ =0.200 phase, as summarized in table 5. The upper limits in the 4.5 – 10 keV and the 70 – 300 keV were obtained for the emission, like X-ray pulses, because the optical emission seems first time with Hitomi, and those in other bands were consistent to have the same origin as that of the X-rays from the multi- with previous works (Mikami et al. 2014; Bilous et al. 2012) wavelength spectrum of the pulsed component of the pulsar as shown in Fig. 7. Our result constitutes the second case of (e.g. see Bühler & Blandford 2014). To increase the syn- astudyinthehardX-raybandwheretheflux(inνFν space) chrotron emission temporarily on a short time scale of µs, whilst of the pulsed component of the Crab pulsar became the high- maintaining the structure of the magnetosphere, only two can- est, following a previous report of a marginal detection at the didates can be considered; a) an increase in the number of par- 2.7σ level with Suzaku Mikami et al. (2014). Our results were ticles for radiation, or b) a change in the local magnetic field mainly limited by the photon numbers in the X-ray band, and strength. However, case b) would be considered difficult to the statistical errors dominated the results. The pulse shape in achieve normally, and the pulse phase needs not be aligned to the X-ray band was observationally confirmed to be stable with the main or inter pulses, and therefore it is straightforward to the 1 σ fluctuation of 0.7 %levelbyRXTEshowingabout- think that the case a) is the origin of the optical enhancement ∼ two-times intensive pulses (Patt et al. 1999; Vivekanand 2001), at GRPs. Such occasion might occur after a magnetic recon- which could be shallow “giant X-ray pulses” (GXPs) but the nection near the light cylinder (Istomin, Y. N. 2004) resulting timing correlations between these shallow GXPs and the GRPs ahigherdensityplasmathantheGoldreich-Juliandensityin were unknown. In our X-ray correlation study using the Hitomi the GRP region (Lyutikov, M. 2007). In the Crab pulsar, the satellite, we could not identify such GXPs due to a poor effec- emission regions for the radio, optical, and X-rays are normally tive area. considered to be close to each other because the pulses are well As described in section 3.1, no significant variabilities were aligned in these energy bands, although the pulse profile in the detected in the X-ray pulse profiles of 14 cycles before and X-ray band is wider than that in radio. If the number of particles after the GRPs. Similarly, in the optical band, the enhance- for synchrotron emission increases in a local region that emits ments related to the GRPs only happen in narrow time intervals very short GRPs, a possible X-ray enhancement should also oc- ( 100 µs) at the pulse peak, and the pulse profiles in other cur very shortly, within about 10 µsjustonthepulsepeak,like ∼ phases were stable (Shearer et al. 2003). These facts indicated the optical and radio cases. If such short enhancement will be that the magnetosphere is stable during the GRPs, which should detected in the X-ray band, we are able to reinforce the idea a), originate from a local place within the magnetosphere. but the fine pulse profiles divided by 1/128 phases with Hitomi What happens during the GRP on the pulsar, when the struc- (Fig. 3) do not show such enhancement at the peak statistically. ture of the magnetosphere does not change? Here, we assumed Finally, we discuss the energy balance between the X-ray up- the emission mechanism of the optical pulses is synchrotron per limit of the pulse-peak flux (ξ)andtheradiationenergyof Radio Campaign Simultaneous with NICER

Crab Folded period: 0.337386716000000E −01 s 4 10 • NICER observations of Crab 1.6×

1.6 NICER Crab proﬁle • Started from 2017 August 5 August 9 (7.2 ks) 4 Count/s • 4 Preliminary 1 Crab X-ray intensity ~ 10 counts/sec 4 10 1.4× • Pulse detection only with a short exposure 1.4 10 • GRP enhancement in X-rays? statistics! 4 Count/sec 10 1.2× • Simultaneous radio monitoring 1.2 • 2, 8 GHz @ 64 m Usuda / JAXA

• 4 6 GHz @ 32 m Hitachi / Ibaraki University 1.010 • 325 MHz @ 31 m Iidate / Tohoku University 0 0.5 1 1.5 2 • ~18 ks simultaneous with NICER in August 0.0 0.5 1.0Phase 1.5 2.0

Fig.7 The 0.4-10 keV pulse proﬁleStart of Time Crab 17974 pulsar 17:11:58:921obtained with NICER Stop Time(phase 17974 bin 200). 22:13:28:807 Crab observation (ObsID 1708091713) was performed with NICER on August 9, 2017 17:09—22:17 (DOYPhase 221, Exposure 7.16 ks, Total events 7.4e+7 counts including DC, and average rate of 1.0e+4 cps). Extrapolated from the Jodrell Bank Observatory (JBO) ephemeris, pulse period and derivatives are expected to be ~33.738727 ms and Pdot=4.19687e-13 s/s at DOY 221. As a quick look approach, with Pdot ﬁxed at the expected value, the best period is 33.7386716 ms with epoch of MJD=57974.7166539606 (close to the start of observation). Identifying GRPs at radio ➡ X-ray studies with NICER 8 Additional Crab campaign in September? Campaign in optical / other observatories?

Mikami+2016, (Radio contribution from T. Terasawa, H. Takeuchi, Y. Murata, Y. Yonekura, H. Misawa, F. Tsuchiya, M. Sekido, K. Takefuji, T. Aoki, et al.,) Usuda S-band (2194-2322 MHz) on 9 Aug 2017

P=33.738645568ms, Pdot=4.196980E-013 s/s (from JB 2017/7/24) Intensity Spectra of Crab Giant Radio Pulse Candidates (S/N>5.5) GRPs 7433 MP IP GRPs

MP Prelimina dN/d(S/N) (arbitrary unit)

Phase angle (deg) ry S/N (S/N=100 ~ 2.2 UTC on 10 Aug 2017 (doy 221) kJy) GRP candidates (S/N>5.5) : ~7400 pulses for the main pulse + ~470 有効データ 16:48:15-23:59:59 UTC – [Data gap合計]＝25884秒 for the Interpulse Data gap 毎時59m59s UTCから1秒間(ファイルの切れ目） 19:00:54-19:01:07 UTC (RFI) 位相で選択後のGRP数(S/N>5.5) MP=7433個、 IP=469個 (C) Terasawa, Murata, Takeuchi et al. (only data from the Usuda radio observatory) 25884秒間の全パルス767191の0.97%がMPGRP (0.06%がIPGRP) 1. NICER Magnetar & Magnetosphere (M&M) Summary working group covers highly magnetised young neutron stars. 2. Example scheduled targets are CXO J164710.2-455216 (low-B magnetar), PSR J1119-6127 (high-B pulsar), 1E 1207.4-5209 (absorption feature), PSR B0656+14 (rotation powered) 3. A prototypical magnetar 4U 0142+61 was observed with NICER during the outburst just after a SGR short burst. A pulsar glitch is suggested before or around the NICER observation. 4. We performed coordinated X-ray/radio observations for a radio-loud magnetar PSR J1622-4950 and Vela pulsar. 5. Simultaneous radio observations were performed with NICER for Crab pulsar in October to search for X-ray enhancement associated with giant radio pulses. 6. Analysis of the data is underway.