Journal Article•
Progress in particle and nuclear physics
TL;DR: In particular, the role of mesons, isobars and quarks in nuclear structure and the use of complex nuclei for probing fundamental symmetries is discussed in this paper.
About: This article is published in Progress in Particle and Nuclear Physics.The article was published on 2000-01-01 and is currently open access. It has received 665 citations till now. The article focuses on the topics: Form factor (quantum field theory).
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TL;DR: In this article, the authors describe the detailed design of the KAGRA interferometer as well as the reasoning behind the design choices, including the length and alignment sensing schemes for the robust control of the inter-ferometer.
Abstract: KAGRA is a cryogenic interferometric gravitational-wave detector being constructed at the underground
site of Kamioka mine in Gifu prefecture, Japan. We performed an optimization of the interferomter
design, to achieve the best sensitivity and a stable operation, with boundary conditions of classical
noises and under various practical constraints, such as the size of the tunnel or the mirror cooling capacity.
Length and alignment sensing schemes for the robust control of the interferometer are developed. In this
paper, we describe the detailed design of the KAGRA interferometer as well as the reasoning behind
design choices.
846 citations
Cites background from "Progress in particle and nuclear ph..."
...There are several next generation interferometric gravitational wave detectors being built around the world[2]....
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...Several large-scale interferometric gravitational wave detectors were built and successfully operated to prove the feasibility of such detectors [2]....
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Posted Content•
TL;DR: The white paper summarizes the workshop "U.S. Cosmic Visions: New Ideas in Dark Matter" held at University of Maryland on March 23-25, 2017.
Abstract: This white paper summarizes the workshop "U.S. Cosmic Visions: New Ideas in Dark Matter" held at University of Maryland on March 23-25, 2017.
464 citations
Cites background from "Progress in particle and nuclear ph..."
...beryllium-polypropylene test bodies (4 times increase in sensitivity to B-L coupled DM) [149]...
[...]
TL;DR: The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016 as discussed by the authors, which achieved a strain sensitivity of better than 10^(−23)/√Hz around 100 Hz.
Abstract: The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10^(−23)/√Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M⊙ could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.
404 citations
Cites background from "Progress in particle and nuclear ph..."
...These instruments target gravitational waves produced by compact binary coalescences, supernovae, non-axisymmetric pulsars, cosmological background as well as any unknown astrophysical sources in the audio frequency band, from 10 Hz to 10 kHz [7]....
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TL;DR: In this paper, a new experiment using matter-wave interferometry confirms that different atoms free fall in gravity at the same rate in the same way as other atoms in the universe.
Abstract: A new experiment using matter-wave interferometry confirms that different atoms free fall in gravity at the same rate.
298 citations
TL;DR: In this article, the authors present lower bounds on the mass of DM particles, coming from various dSphs, using both information about the current phase space distribution and both the initial and final distributions.
Abstract: We discuss the bounds on the mass of Dark Matter (DM) particles, coming from the analysis of DM phase-space distribution in dwarf spheroidal galaxies (dSphs). After reviewing the existing approaches, we choose two methods to derive such a bound. The first one depends on the information about the current phase space distribution of DM particles only, while the second one uses both the initial and final distributions. We discuss the recent data on dSphs as well as astronomical uncertainties in relevant parameters. As an application, we present lower bounds on the mass of DM particles, coming from various dSphs, using both methods. The model-independent bound holds for any type of fermionic DM. Stronger, model-dependent bounds are quoted for several DM models (thermal relics, non-resonantly and resonantly produced sterile neutrinos, etc.). The latter bounds rely on the assumption that baryonic feedback cannot significantly increase the maximum of a distribution function of DM particles. For the scenario in which all the DM is made of sterile neutrinos produced via non-resonant mixing with the active neutrinos (NRP) this gives mNRP > 1.7 keV. Combining these results in their most conservative form with the X-ray bounds of DM decay lines, we conclude that the NRP scenario remains allowed in a very narrow parameter window only. This conclusion is independent of the results of the Lyman-α analysis. The DM model in which sterile neutrinos are resonantly produced in the presence of lepton asymmetry remains viable. Within the minimal neutrino extension of the Standard Model (the νMSM), both mass and the mixing angle of the DM sterile neutrino are bounded from above and below, which suggests the possibility for its experimental search.
294 citations
Cites background from "Progress in particle and nuclear ph..."
...The existence of such objects may also have insteresting astrophysical applications [82]....
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References
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TL;DR: This analysis expands upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars.
Abstract: On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parametrization of the defining function pðρÞ of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as R1 ¼ 10.8 þ2.0 −1.7 km for the heavier star and R2 ¼ 10.7 þ2.1 −1.5 km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than 1.97 M⊙ as required from electromagnetic observations and employ the equation-of-state parametrization, we further constrain R1 ¼ 11.9 þ1.4 −1.4 km and R2 ¼ 11.9 þ1.4 −1.4 km at the 90% credible level. Finally, we obtain constraints on pðρÞ at supranuclear densities, with pressure at twice nuclear saturation density measured at 3.5 þ2.7 −1.7 × 1034 dyn cm−2 at the 90% level.
1,595 citations
TL;DR: In this article, the authors describe the detailed design of the KAGRA interferometer as well as the reasoning behind the design choices, including the length and alignment sensing schemes for the robust control of the inter-ferometer.
Abstract: KAGRA is a cryogenic interferometric gravitational-wave detector being constructed at the underground
site of Kamioka mine in Gifu prefecture, Japan. We performed an optimization of the interferomter
design, to achieve the best sensitivity and a stable operation, with boundary conditions of classical
noises and under various practical constraints, such as the size of the tunnel or the mirror cooling capacity.
Length and alignment sensing schemes for the robust control of the interferometer are developed. In this
paper, we describe the detailed design of the KAGRA interferometer as well as the reasoning behind
design choices.
846 citations
Posted Content•
TL;DR: The white paper summarizes the workshop "U.S. Cosmic Visions: New Ideas in Dark Matter" held at University of Maryland on March 23-25, 2017.
Abstract: This white paper summarizes the workshop "U.S. Cosmic Visions: New Ideas in Dark Matter" held at University of Maryland on March 23-25, 2017.
464 citations
TL;DR: The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016 as discussed by the authors, which achieved a strain sensitivity of better than 10^(−23)/√Hz around 100 Hz.
Abstract: The Laser Interferometer Gravitational Wave Observatory (LIGO) consists of two widely separated 4 km laser interferometers designed to detect gravitational waves from distant astrophysical sources in the frequency range from 10 Hz to 10 kHz. The first observation run of the Advanced LIGO detectors started in September 2015 and ended in January 2016. A strain sensitivity of better than 10^(−23)/√Hz was achieved around 100 Hz. Understanding both the fundamental and the technical noise sources was critical for increasing the astrophysical strain sensitivity. The average distance at which coalescing binary black hole systems with individual masses of 30 M⊙ could be detected above a signal-to-noise ratio (SNR) of 8 was 1.3 Gpc, and the range for binary neutron star inspirals was about 75 Mpc. With respect to the initial detectors, the observable volume of the Universe increased by a factor 69 and 43, respectively. These improvements helped Advanced LIGO to detect the gravitational wave signal from the binary black hole coalescence, known as GW150914.
404 citations
TL;DR: In this article, the authors present lower bounds on the mass of DM particles, coming from various dSphs, using both information about the current phase space distribution and both the initial and final distributions.
Abstract: We discuss the bounds on the mass of Dark Matter (DM) particles, coming from the analysis of DM phase-space distribution in dwarf spheroidal galaxies (dSphs). After reviewing the existing approaches, we choose two methods to derive such a bound. The first one depends on the information about the current phase space distribution of DM particles only, while the second one uses both the initial and final distributions. We discuss the recent data on dSphs as well as astronomical uncertainties in relevant parameters. As an application, we present lower bounds on the mass of DM particles, coming from various dSphs, using both methods. The model-independent bound holds for any type of fermionic DM. Stronger, model-dependent bounds are quoted for several DM models (thermal relics, non-resonantly and resonantly produced sterile neutrinos, etc.). The latter bounds rely on the assumption that baryonic feedback cannot significantly increase the maximum of a distribution function of DM particles. For the scenario in which all the DM is made of sterile neutrinos produced via non-resonant mixing with the active neutrinos (NRP) this gives mNRP > 1.7 keV. Combining these results in their most conservative form with the X-ray bounds of DM decay lines, we conclude that the NRP scenario remains allowed in a very narrow parameter window only. This conclusion is independent of the results of the Lyman-α analysis. The DM model in which sterile neutrinos are resonantly produced in the presence of lepton asymmetry remains viable. Within the minimal neutrino extension of the Standard Model (the νMSM), both mass and the mixing angle of the DM sterile neutrino are bounded from above and below, which suggests the possibility for its experimental search.
294 citations