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Full list of authors: Taverna, Roberto; Turolla, Roberto; Muleri, Fabio; Heyl, Jeremy; Zane, Silvia; Baldini, Luca; Gonzalez-Caniulef, Denis; Bachetti, Matteo; Rankin, John; Caiazzo, Ilaria; Di Lalla, Niccolo; Doroshenko, Victor; Errando, Manel; Gau, Ephraim; Kirmizibayrak, Demet; Krawczynski, Henric; Negro, Michela; Ng, Mason; Omodei, Nicola; Possenti, Andrea; Tamagawa, Toru; Uchiyama, Keisuke; Weisskopf, Martin C.; Agudo, Ivan; Antonelli, Lucio A.; Baumgartner, Wayne H.; Bellazzini, Ronaldo; Bianchi, Stefano; Bongiorno, Stephen D.; Bonino, Raffaella; Brez, Alessandro; Bucciantini, Niccolo; Capitanio, Fiamma; Castellano, Simone; Cavazzuti, Elisabetta; Ciprini, Stefano; Costa, Enrico; De Rosa, Alessandra; Del Monte, Ettore; Di Gesu, Laura; Di Marco, Alessandro; Donnarumma, Immacolata; Doviak, Michal; Ehlert, Steven R.; Enoto, Teruaki; Evangelista, Yuri; Fabiani, Sergio; Ferrazzoli, Riccardo; Garcia, Javier A.; Gunji, Shuichi; Hayashida, Kiyoshi; Iwakiri, Wataru; Jorstad, Svetlana G.; Karas, Vladimir; Kitaguchi, Takao; Kolodziejczak, Jeffery J.; La Monaca, Fabio; Latronico, Luca; Liodakis, Ioannis; Maldera, Simone; Manfreda, Alberto; Marin, Frederic; Marinucci, Andrea; Marscher, Alan P.; Marshall, Herman L.; Matt, Giorgio; Mitsuishi, Ikuyuki; Mizuno, Tsunefumi; Ng, Stephen C-Y; O'Dell, Stephen L.; Oppedisano, Chiara; Papitto, Alessandro; Pavlov, George G.; Peirson, Abel L.; Perri, Matteo; Pesce-Rollins, Melissa; Pilia, Maura; Poutanen, Juri; Puccetti, Simonetta; Ramsey, Brian D.; Ratheesh, Ajay; Romani, Roger W.; Sgro, Carmelo; Slane, Patrick; Soffitta, Paolo; Spandre, Gloria; Tavecchio, Fabrizio; Tawara, Yuzuru; Tennant, Allyn F.; Thomas, Nicolas E.; Tombesi, Francesco; Trois, Alessio; Tsygankov, Sergey; Vink, Jacco; Wu, Kinwah; Xie, Fei., Magnetars are neutron stars with ultrastrong magnetic fields, which can be observed in x-rays. Polarization measurements could provide information on their magnetic fields and surface properties. We observed polarized x-rays from the magnetar 4U 0142+61 using the Imaging X-ray Polarimetry Explorer and found a linear polarization degree of 13.5 ± 0.8% averaged over the 2– to 8–kilo–electron volt band. The polarization changes with energy: The degree is 15.0 ± 1.0% at 2 to 4 kilo–electron volts, drops below the instrumental sensitivity ~4 to 5 kilo–electron volts, and rises to 35.2 ± 7.1% at 5.5 to 8 kilo–electron volts. The polarization angle also changes by 90° at ~4 to 5 kilo–electron volts. These results are consistent with a model in which thermal radiation from the magnetar surface is reprocessed by scattering off charged particles in the magnetosphere. © 2022 The Authors., R.Ta. and R.Tu. acknowledge financial support from the Italian MUR through grant PRIN 2017LJ39LM. J.H., D.G.-C., I.C., and D.K. acknowledge the support of the Natural Sciences and Engineering Research Council of Canada (NSERC), funding reference number 5007110, and the Canadian Space Agency. D.G.-C. is a Canadian Institute for Theoretical Astrophysical (CITA) National Fellow (grant no. CITA 490888-16). E.G. and H.K. acknowledge NASA support under grants 80NSSC18K0264, 80NSSC22K1291, 80NSSC21K1817, and NNX16AC24G. M.Ne. acknowledges support from NASA under award 80GSFC21M0002. T.T. was supported by grant JSPS KAKENHI JP19H05609. F.Mu., J.R., S.B., E.Co., E.D.M., A.D.M., Y.E., S.F., R.F., F.L.M., G.M., M.Pe., A.R., P.So., and A.T. were supported by ASI and INAF under grants ASI-INAF-2017-12-H0 and ASI-INAF-2022-14-HH.0. L.B., L.L., R.Be., R.Bo., A.B., S.Ca., S.M., A.Mar., C.O., M.P.-R., C.S., and G.S. were supported by ASI and INFN under grants ASI-INFN-2017.13-H0 and ASI-INFN-2021-43-HH.0., With funding from the Spanish government through the Severo Ochoa Centre of Excellence accreditation SEV-2017-0709.

We have demonstrated high-precision cutting and drilling of CFRP using a 3-kW CW single-mode fiber laser and a galvanometer scanner. A 3-mm-thick thermoset CFRP was successfully cut with 100 scans at the scanning speed of 13 m/s, which corresponds to effective cutting speed of 7.8 m/min. We employed the multi-pass method, in which a laser is scanned on the same position at high speed, and the optimized scanning position shift to realize short-time cutting. The time interval between scans was less than 20 ms, which was much shorter than general time interval in multi-pass method. Even with such short interval, the width of heat-affected zone (HAZ) was controlled to 97 μm on average. Drilling demonstration was carried out by using the same setup as the cutting experiment. Holes with a diameter of 6.4 mm have been successfully drilled on a 2-mm-thick thermoset CFRP. The processing time was 2.7 seconds, which was equivalent to that in mechanical processing. Since a HAZ tends to expand in the direction of the carbon fibers due to their high heat conductivity, it is difficult to reduce the width of HAZ in all directions around the processed area. To overcome this challenge, we optimized the gas injection condition as well as the scanning condition. As a result, the widths of HAZs were successfully controlled to about 100 μm in all directions.

This paper introduces a second-generation balloon-borne hard X-ray polarimetry mission, XL-Calibur. X-ray polarimetry promises to give qualitatively new information about high-energy astrophysical sources, such as pulsars and binary black hole systems. The XL-Calibur contains a grazing incidence X-ray telescope with a focal plane detector unit that is sensitive to linear polarization. The telescope is very similar in design to the ASTRO-H HXT telescopes that has the world’s largest effective area above ~10 keV. The detector unit combines a low atomic number Compton scatterer with a CdZnTe detector assembly to measure the polarization making use of the fact that polarized photons Compton scatter preferentially perpendicular to the electric field orientation. It also contains a CdZnTe imager at the bottom. The detector assembly is surrounded by the improved anti-coincidence shielding, giving a better sensitivity. The pointing system with arcsecond accuracy will be achieved.

All-sky surveys are crucial to discover transient objects. In reality, however, it is impossible to achieve high sensitivity, high cadence, wide sky coverage, and broad wavelength range at the same time. This is where observations with small telescopes can come in significant, as small telescopes often can make high cadence monitoring and flexible operations, playing a complementary role to large observatories. We plan to launch a new 6U-size CubeSat X-ray observatory, NinjaSat, in 2022 to conduct a flexible X-ray observation program. The satellite is equipped with two identical non-imaging Gas Multiplier Counters (GMCs) sensitive to X-rays in the 2–50 keV band with a total effective area of 36 cm2 at 6 keV. Coupled with X-ray collimators of a 2.1° field-of-view, NinjaSat is suitable for flexible multi-wavelength coordinated observations of bright (g10 mCrab) X-ray sources with particular emphasis on their time variability. An example of our targets is one of the brightest celestial X-ray objects, Scorpius X-1, which hosts a fast-spinning neutron star and is a candidate source for coherent gravitational waves. The quasi-periodic oscillation (QPO) of neutron-star systems is considered to carry important information on the neutron star’s rotational frequency, which is useful for sensitive gravitational-wave searches. Scorpius X-1, being one of the brightest, provides the best opportunity to study the QPO. Combining with coordinated simultaneous monitoring observations with recently-developed fast optical photometry, the mechanism of the mass accretion of the disk can also be studied. We plan to use NinjaSat also for space science education, particularly X-ray astronomy, for students and the general public.

The source position determination method of the multiplexing lobster-eye optics (MuLE), which is a newly proposed configuration of the Lobster-Eye (LE) optics to reduce the number of focal plane detectors significantly, was developed. In the MuLE configuration, X-rays came from different field-of-views (FoVs) were focused on a single imager. To separate the multiplexed FoVs, the optics was designed so that cross-like responses of LE mirror in different FoVs had different azimuthal rotation angles. In this paper, we show the method to determine the rotation angles and verify the FoV discrimination power by using a ray tracing simulation. The configuration we assumed in the simulation was nine multiplexed FoVs projecting onto a single imager (nine-segment MuLE optics) with a 30 cm focal length and a 9×9 cm2 effective area of each LE segment. One LE segment covers 9.6°× 9.6° FoV and the total FoV of the nine-segment MuLE configuration was 9 times of that. Our method provided 100% correct FoV discrimination at the 5σ detection limit flux (35–70 mCrab) for a transient source with a duration of 100 s except for the edge of the FoV.

A high power single-mode fiber laser has received a lot of attention in various materials processing fields. In order to carry out processing under proper conditions with single-mode fiber laser, the dynamic flows of fluids inside the materials should be precisely understood. We carried out the numerical analysis of materials processing using a 5-kW single-mode fiber laser. The dynamic flows of the copper fluid during the bead-on-plate tests are calculated and the results agree well with the experimental results. The processing with the different scan speed and spot size, and at the output power of 10 kW are numerically calculated as well. The proper processing conditions with less spatters and dross for each materials can be determined by the dynamic analysis.

We propose a concept of multiplexing lobster-eye (MuLE) optics to achieve significant reductions in the number of focal plane imagers in lobster-eye (LE) wide-field X-ray monitors. In the MuLE configuration, an LE mirror is divided into several segments and the X-rays reflected on each of these segments are focused on a single image sensor in a multiplexed configuration. If each LE segment assumes a different rotation angle, the azimuthal rotation angle of a cross-like image reconstructed from a point source by the LE optics identifies the specific segment that focuses the X-rays on the imager. With a focal length of 30 cm and LE segments with areas of 10 x 10 cm^2, ~1 sr of the sky can be covered with 36 LE segments and only four imagers (with total areas of 10 x 10 cm^2). A ray tracing simulation was performed to evaluate the nine-segment MuLE configuration. The simulation showed that the flux (0.5 to 2 keV) associated with the 5-sigma detection limit was ~2 x 10^-10 erg cm^-2 s^-1 (10 mCrab) for a transient with a duration of 100 s. The simulation also showed that the direction of the transient for flux in the range of 14 to 17 mCrab at 0.6 keV was determined correctly with 99.7% confidence limit. We conclude that the MuLE configuration can become an effective on-board device for small satellites for future X-ray wide-field transient monitoring., 20 pages, 14 figures

Stimulated Raman scattering gives back reflection sensitivity to a high power fiber laser. Therefor SRS suppression is necessary in order to realize stable laser processing by a high power fiber laser. A 5-kW single-mode ytterbium doped fiber laser with a 20-m long delivery fiber has been realized. The fiber laser is an all-fiber single-stage Fabry-Perot system in a co-pumping configuration. The optical to optical efficiency was 80% at the output power of 5.0 kW. And the M-squared figure of 1.3 was obtained. The Stokes light by SRS is suppressed to 45 dB below the laser output by using fibers with the effective mode area of 600 μm2 . While SRS was well suppressed, four wave mixing was observed with the frequency shift of ~6 THz. Four wave mixing between the fundamental mode and the secondary modes is believed to take place. Four wave mixing is believed not to give back reflection sensitivity to the fiber laser. The 5-kW single-mode fiber laser was applied to laser processing. Bead-on-plate tests were carried out with a galvanometer scanner. The laser ran without stopping nor damaging the laser system even during processing highly reflective material. This implies that our SRS suppressed single-mode fiber laser can be used practically in most of processing systems.

A 3 kW single stage all-fiber Yb-doped single-mode fiber laser with bi-directional pumping configuration has been demonstrated. Our newly developed high-power LD modules are employed for a high available pump power of 4.9 kW. The length of the delivery fiber is 20 m which is long enough to be used in most of laser processing machines. An output power of 3 kW was achieved at a pump power of 4.23 kW. The slope efficiency was 70%. SRS was able to be suppressed at the same output power by increasing ratio of backward pump power. The SRS level was improved by 5dB when 57% backward pump ratio was adopted compared with the case of 50%. SRS was 35dB below the laser power at the output power of 3 kW even with a 20-m delivery fiber. The M-squared factor was 1.3. Single-mode beam quality was obtained. To evaluate practical utility of the 3 kW single-mode fiber laser, a Bead-on-Plate (BoP) test onto a pure copper plate was executed. The BoP test onto a copper plate was made without stopping or damaging the laser system. That indicates our high power single-mode fiber lasers can be used practically in processing of materials with high reflectivity and high thermal conductivity.

Microfluidic systems will be widely used in the future μ-TAS and DNA analyses. Due to the small Reynolds number in a microchannel, mixing is performed by increasing the contact area between two liquid. Here, we propose an active method to stir a liquid using an optically-driven micro-rotator. In this report, we have analyzed the micro-liquid velocity vectors around the rotators at different depths for both horizontal and vertical rotations.