研究者業績
基本情報
- 所属
- 国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 宇宙物理学研究系 助教
- 学位
- 博士 (理学)(2020年3月 東京大学)修士 (理学)(2017年3月 東京大学)
- 研究者番号
- 30881213
- ORCID ID
https://orcid.org/0000-0001-6426-7079- J-GLOBAL ID
- 202001006174951270
- researchmap会員ID
- R000002942
経歴
3-
2025年7月 - 現在
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2023年1月 - 2025年6月
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2020年4月 - 2022年12月
主要な受賞
6-
2020年11月
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2019年3月
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2017年3月
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2015年3月
論文
40-
Classical and Quantum Gravity 41(21) 215013-215013 2024年10月10日 査読有りAbstract A series of quantum locking theories have been proposed to enhance the quantum-noise-limited target sensitivity of the DECi-hertz Interferometer Gravitational wave Observatory. The quantum locking that uses a square completion optimizes the sensitivity across all frequencies. However, a substantial amount of data-series must be post-processed since the square completion is a form of signal processing technique. This paper approaches the optimal sensitivity across all frequencies from an alternative perspective: by optimizing the frequency dependence of a servo gain in a feedback loop. The optimal servo gain is formulated by comparing the alternative method with the square completion method for the same optical setup. This will be shown in general noise issues extending the framework of the quantum locking. We find that the optimal servo gain forms a non-feasible filter but has certain characteristics. We also find that the noise of the measurement signal deteriorates proportionally to the noise measured in the feedback loop when the servo gain is slightly imperfect.
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Physical Review A 110(2) 2024年8月1日 査読有り
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Physical Review Research 5(4) 2023年10月
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Physical Review D 107(2) 022007 2023年1月19日Decihertz Interferometer Gravitational Wave Observatory (DECIGO) is a future mission for a space-borne laser interferometer. DECIGO has 1000-km-long arm cavities mainly to detect the primordial gravitational waves (PGWs) at lower frequencies around 0.1 Hz. Observations in the electromagnetic spectrum have lowered the bounds on the upper limit of PGWs energy density (Ω_(gw) ∼ 10⁻¹⁵ → 10⁻¹⁶). As a result, DECIGO’s target sensitivity, which is mainly limited by quantum noise, needs further improvement. To maximize the feasibility of detection while constrained by DECIGO’s large diffraction loss, a quantum locking technique with an optical spring was theoretically proposed to improve the signal-to-noise ratio of the PGWs. In this paper, we experimentally verify one key element used in the theory: sensitivity optimization by completing the square of multiple detector outputs. This experiment is operated on a simplified tabletop optical setup with classical noise simulating quantum noise. We succeed in getting the best of the sensitivities with two different laser powers by the square completion method.
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The Fifteenth Marcel Grossmann Meeting 1599-1605 2022年6月22日
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Applied Optics 61(13) 3901-3901 2022年5月1日
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2022年1月1日DECi-hertz Interferometer Gravitational Wave Observatory (DECIGO) is a future mission for a space-borne laser interferometer. DECIGO has 1,000-km-long arm cavities mainly to detect the primordial gravitational waves (PGW) at lower frequencies around 0.1 Hz. Observations in the electromagnetic spectrum have lowered the bounds on the upper limit of PGW energy density ($Ω_{\rm gw} \sim 10^{-15} \to 10^{-16}$). As a result, DECIGO's target sensitivity, which is mainly limited by quantum noise, needs further improvement. To maximize the feasibility of detection while constrained by DECIGO's large diffraction loss, a quantum locking technique with an optical spring was theoretically proposed to improve the signal-to-noise ratio of the PGW. In this paper, we experimentally verify one key element of the optical-spring quantum locking: sensitivity optimization by completing the square of multiple detector outputs. This experiment is operated on a simplified tabletop optical setup with classical noise simulating quantum noise. We succeed in getting the best of the sensitivities with two different laser powers by the square completion method. 10 pages, 14 figures
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Quantum Approximate Optimization for Continuous Problems on a Programmable Photonic Quantum ComputerOptics InfoBase Conference Papers 2022年
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Science Advances 7 eabj6624 2021年11月12日 査読有り筆頭著者
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Physical Review A 104(3) 2021年9月2日
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The Astrophysical Journal Letters 915(1) L5-L5 2021年7月1日Abstract We report the observation of gravitational waves from two compact binary coalescences in LIGO’s and Virgo’s third observing run with properties consistent with neutron star–black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo and the second by all three LIGO–Virgo detectors. The source of GW200105 has component masses $8.{9}_{-1.5}^{+1.2}$ and $1.{9}_{-0.2}^{+0.3}\,{M}_{\odot }$, whereas the source of GW200115 has component masses $5.{7}_{-2.1}^{+1.8}$ and $1.{5}_{-0.3}^{+0.7}\,{M}_{\odot }$ (all measurements quoted at the 90% credible level). The probability that the secondary’s mass is below the maximal mass of a neutron star is 89%–96% and 87%–98%, respectively, for GW200105 and GW200115, with the ranges arising from different astrophysical assumptions. The source luminosity distances are ${280}_{-110}^{+110}$ and ${300}_{-100}^{+150}\,\mathrm{Mpc}$, respectively. The magnitude of the primary spin of GW200105 is less than 0.23 at the 90% credible level, and its orientation is unconstrained. For GW200115, the primary spin has a negative spin projection onto the orbital angular momentum at 88% probability. We are unable to constrain the spin or tidal deformation of the secondary component for either event. We infer an NSBH merger rate density of ${45}_{-33}^{+75}\,{\mathrm{Gpc } }^{-3}\,{\mathrm{yr } }^{-1}$ when assuming that GW200105 and GW200115 are representative of the NSBH population or ${130}_{-69}^{+112}\,{\mathrm{Gpc } }^{-3}\,{\mathrm{yr } }^{-1}$ under the assumption of a broader distribution of component masses.
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Physical Review Letters 126(24) 2021年6月16日
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The Astrophysical Journal Letters 913(2) L27-L27 2021年6月1日
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Physics Letters A 402 127365-127365 2021年6月
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Progress of Theoretical and Experimental Physics 2021(5) 2021年5月18日
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Progress of Theoretical and Experimental Physics 2021(5) 2021年5月18日<jats:title>Abstract</jats:title> <jats:p>KAGRA is a newly build gravitational wave observatory, a laser interferometer with 3 km arm length, located in Kamioka, Gifu, Japan. In this paper, one of a series of articles featuring KAGRA, we discuss the science targets of KAGRA projects, considering not only the baseline KAGRA (current design) but also its future upgrade candidates (KAGRA+) for the near to middle term ($\sim$5 years).</jats:p>
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Progress of Theoretical and Experimental Physics 2021(5) 2021年5月18日
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Classical and Quantum Gravity 38(8) 085013-085013 2021年4月22日Abstract We report the mirror suspension design for large-scale cryogenic gravitational wave telescope, KAGRA, during bKAGRA phase 1. Mirror thermal noise is one of the fundamental noises for room-temperature gravitational-wave detectors such as Advanced LIGO and Advanced Virgo. Thus, reduction of thermal noise is required for further improvement of their sensitivity. One effective approach for reducing thermal noise is to cool the mirrors. There are many technical challenges that must be overcome to cool the mirrors, such as cryocooler induced vibrations, thermal drift in suspensions, and reduction in duty cycling due to the increased number of potential failure mechanisms. Our mirror suspension has a black coating that makes radiative cooling more efficient. For conduction cooling, we developed ultra high purity aluminum heat links, which yield high thermal conductivity while keeping the spring constant sufficiently small. A unique inclination adjustment system, called moving mass, is used for aligning the mirror orientation in pitch. Photo-reflective displacement sensors, which have a large range, are installed for damping control on marionette recoil mass and intermediate recoil mass. Samarium cobalt magnets are used for coil-magnet actuators to prevent significant change of magnetism between room temperature and cryogenic temperature. In this paper, the design of our first cryogenic payload and its performance during bKAGRA phase 1 are discussed.
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Journal of Physics: Conference Series 1857(1) 012002-012002 2021年4月1日
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Living Reviews in Relativity 23(1) 3-3 2020年12月<title>Abstract</title>We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star–black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of <inline-formula><alternatives><tex-math>$$10^{5}, 10^{6}, 10^{7}\mathrm {\ Mpc}^3$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:mrow> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>5</mml:mn> </mml:msup> <mml:mo>,</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>6</mml:mn> </mml:msup> <mml:mo>,</mml:mo> <mml:msup> <mml:mn>10</mml:mn> <mml:mn>7</mml:mn> </mml:msup> <mml:msup> <mml:mrow> <mml:mspace /> <mml:mi>Mpc</mml:mi> </mml:mrow> <mml:mn>3</mml:mn> </mml:msup> </mml:mrow> </mml:math></alternatives></inline-formula> for binary neutron star, neutron star–black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of <inline-formula><alternatives><tex-math>$$1^{+12}_{-1}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>1</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>12</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>(<inline-formula><alternatives><tex-math>$$10^{+52}_{-10}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>10</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>52</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>) for binary neutron star mergers, of <inline-formula><alternatives><tex-math>$$0^{+19}_{-0}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>0</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>19</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>(<inline-formula><alternatives><tex-math>$$1^{+91}_{-1}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>1</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>91</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>) for neutron star–black hole mergers, and <inline-formula><alternatives><tex-math>$$17^{+22}_{-11}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>17</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>11</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>22</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>(<inline-formula><alternatives><tex-math>$$79^{+89}_{-44}$$</tex-math><mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML"> <mml:msubsup> <mml:mn>79</mml:mn> <mml:mrow> <mml:mo>-</mml:mo> <mml:mn>44</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>89</mml:mn> </mml:mrow> </mml:msubsup> </mml:math></alternatives></inline-formula>) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.
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Physics Letters, Section A: General, Atomic and Solid State Physics 384(26) 2020年9月18日 査読有り
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Physical Review D 102(2) 2020年7月24日 査読有り
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Progress of Theoretical and Experimental Physics 2020(5) 2020年5月1日
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CLASSICAL AND QUANTUM GRAVITY 37(3) 035004-035004 2020年2月 査読有り責任著者
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Journal of Physics: Conference Series 1342 012014-012014 2020年1月
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PHYSICAL REVIEW A 101(1) 2020年1月 査読有り
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CLASSICAL AND QUANTUM GRAVITY 36(20) 2019年10月 査読有り
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Classical and Quantum Gravity 36(16) 165008-165008 2019年8月22日 査読有り
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Classical and Quantum Gravity 36(9) 095015-095015 2019年5月9日 査読有り
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Nature Astronomy 3(1) 35-40 2019年1月 査読有り
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PHYSICAL REVIEW D 97(12) 2018年6月 査読有り
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Direct approach for the fluctuation-dissipation theorem under nonequilibrium steady-state conditionsPHYSICAL REVIEW D 97(10) 2018年5月 査読有り
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15th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics, and Relativistic Field Theories, MG 2018 2018年
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PROGRESS OF THEORETICAL AND EXPERIMENTAL PHYSICS 2018(1) 2018年1月 査読有り
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CLASSICAL AND QUANTUM GRAVITY 34(22) 2017年11月 査読有り
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PHYSICS LETTERS A 380(46) 3871-3875 2016年12月 査読有り
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CLASSICAL AND QUANTUM GRAVITY 33(14) 2016年7月 査読有り筆頭著者
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PHYSICAL REVIEW A 94(1) 2016年7月 査読有り筆頭著者
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PHYSICS LETTERS A 380(9-10) 983-988 2016年3月 査読有り
共同研究・競争的資金等の研究課題
2-
日本学術振興会 科学研究費助成事業 若手研究 2021年4月 - 2023年3月
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日本学術振興会 科学研究費助成事業 特別研究員奨励費 2017年4月 - 2020年3月
