SIMON ZEIDLER - Academia.edu (original) (raw)

Papers by SIMON ZEIDLER

HAL (Le Centre pour la Communication Scientifique Directe), Nov 5, 2021

Physical Review D, 2022

We present a search for dark photon dark matter that could couple to gravitational-wave interfero... more We present a search for dark photon dark matter that could couple to gravitational-wave interferometers using data from Advanced LIGO and Virgo's third observing run. To perform this analysis, we use two methods, one based on cross-correlation of the strain channels in the two nearly aligned LIGO detectors, and one that looks for excess power in the strain channels of the LIGO and Virgo detectors. The excess power method optimizes the Fourier Transform coherence time as a function of frequency, to account for the expected signal width due to Doppler modulations. We do not find any evidence of dark photon dark matter with a mass between mA ∼ 10 −14 − 10 −11 eV/c 2 , which corresponds to frequencies between 10-2000 Hz, and therefore provide upper limits on the square of the minimum coupling of dark photons to baryons, i.e. U (1)B dark matter. For the cross-correlation method, the best median constraint on the squared coupling is ∼ 1.31 × 10 −47 at mA ∼ 4.2 × 10 −13 eV/c 2 ; for the other analysis, the best constraint is ∼ 1.2 × 10 −47 at mA ∼ 5.7 × 10 −13 eV/c 2. These limits improve upon those obtained in direct dark matter detection experiments by a factor of ∼ 100 for mA ∼ [2 − 4] × 10 −13 eV/c 2 .

The Astrophysical Journal, 2021

We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J... more We present a search for continuous gravitational-wave emission due to r-modes in the pulsar PSR J0537–6910 using data from the LIGO–Virgo Collaboration observing run O3. PSR J0537–6910 is a young energetic X-ray pulsar and is the most frequent glitcher known. The inter-glitch braking index of the pulsar suggests that gravitational-wave emission due to r-mode oscillations may play an important role in the spin evolution of this pulsar. Theoretical models confirm this possibility and predict emission at a level that can be probed by ground-based detectors. In order to explore this scenario, we search for r-mode emission in the epochs between glitches by using a contemporaneous timing ephemeris obtained from NICER data. We do not detect any signals in the theoretically expected band of 86–97 Hz, and report upper limits on the amplitude of the gravitational waves. Our results improve on previous amplitude upper limits from r-modes in J0537-6910 by a factor of up to 3 and place stringent...

Nature Astronomy, 2019

The recent detections of gravitational waves[1, 2, 3, 4, 5, 6] (GWs) reported by LIGO[7]/Virgo[8]... more The recent detections of gravitational waves[1, 2, 3, 4, 5, 6] (GWs) reported by LIGO[7]/Virgo[8] collaborations have made significant impact on physics and astronomy. A global network of GW detectors will play a key role to solve the unknown nature of the sources in coordinated observations with astronomical telescopes and detectors. Here we introduce KAGRA (former name LCGT; Large-scale Cryogenic Gravitational wave Telescope), a new GW detector with two 3-km baseline arms arranged in the shape of an L, located inside the Mt. Ikenoyama, Kamioka, Gifu, Japan. KAGRA's design is similar to those of the second generations such as Advanced LIGO/Virgo, but it will be operating at the cryogenic temperature with sapphire mirrors. This low temperature feature is advantageous for improving the sensitivity around 100 Hz and is considered as an important feature for the third generation GW detector concept (e.g. Einstein Telescope[9] of Europe or Cosmic Explorer[10] of USA). Hence, KA-GRA is often called as a 2.5 generation GW detector based on laser interferometry. The installation and commissioning of KAGRA is underway and its cryogenic systems have been successfully tested in May, 2018. KAGRA's first observation run is scheduled in late 2019, aiming to join the third observation run (O3) of the advanced LIGO/Virgo network. In this work, we describe a brief history of KAGRA and highlights of main feature. We also discuss the prospects of GW observation with KAGRA in the era of O3. When operating along with the existing GW detectors, KAGRA will be helpful to locate a GW source more accurately and to determine the source parameters with higher precision, providing information for follow-up observations of a GW trigger candidate.

Frontiers in Astronomy and Space Sciences

The influence of birefringence on rays entering and exiting a non-isotropic medium is a complex p... more The influence of birefringence on rays entering and exiting a non-isotropic medium is a complex process that depends on its dielectric tensor, the orientation and geometry of the medium, the surrounding material, and the inclination of the incident ray. Thus, when aiming for a calculation of the effects, many parameters need to be taken into account while simplifications are generally not applicable. Moreover, the complexity of the general issue makes it almost impossible to find an analytical solution for backward calculations of stress-birefringence from polarization measurements. In this paper, a report is given on the formulation of a birefringence ray-tracing program in Python for the convenient evaluation of optical effects inside uniaxial crystals under stress. The aim thereby is to have an easily applicable tool that can be used in interferometer commissioning for current and future gravitational-wave detectors. Results from test simulations using realistic parameters for a ...

The Astrophysical Journal Letters, 2021

We present a search for quasi-monochromatic gravitational-wave signals from the young, energetic ... more We present a search for quasi-monochromatic gravitational-wave signals from the young, energetic X-ray pulsar PSR J0537−6910 using data from the second and third observing runs of LIGO and Virgo. The search is enabled by a contemporaneous timing ephemeris obtained using Neutron star Interior Composition Explorer (NICER) data. The NICER ephemeris has also been extended through 2020 October and includes three new glitches. PSR J0537−6910 has the largest spin-down luminosity of any pulsar and exhibits fRequent and strong glitches. Analyses of its long-term and interglitch braking indices provide intriguing evidence that its spin-down energy budget may include gravitational-wave emission from a time-varying mass quadrupole moment. Its 62 Hz rotation frequency also puts its possible gravitational-wave emission in the most sensitive band of the LIGO/Virgo detectors. Motivated by these considerations, we search for gravitational-wave emission at both once and twice the rotation frequency f...

Progress of Theoretical and Experimental Physics, 2020

KAGRA is a newly built gravitational-wave telescope, a laser interferometer comprising arms with ... more KAGRA is a newly built gravitational-wave telescope, a laser interferometer comprising arms with a length of 3 km, located in Kamioka, Gifu, Japan. KAGRA was constructed under the ground and it is operated using cryogenic mirrors that help in reducing the seismic and thermal noise. Both technologies are expected to provide directions for the future of gravitational-wave telescopes. In 2019, KAGRA finished all installations with the designed configuration, which we call the baseline KAGRA. For this occasion, we present an overview of the baseline KAGRA from various viewpoints in a series of articles. In this article, we introduce the design configurations of KAGRA with its historical background.

Physical Review D, 2021

We report results from searches for anisotropic stochastic gravitational-wave backgrounds using d... more We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called PyStoch on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from Fα,Θ < (0.013 − 7.6) × 10 −8 erg cm −2 s −1 Hz −1 , and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from Ωα,Θ < (0.57 − 9.3) × 10 −9 sr −1 , depending on direction (Θ) and spectral index (α). These limits improve upon previous limits by factors of 2.9−3.5. We also set 95% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from h0 < (1.7 − 2.1) × 10 −25 , a factor of ≥ 2.0 improvement compared to previous stochastic radiometer searches.

Progress of Theoretical and Experimental Physics, 2021

KAGRA is a newly built gravitational wave observatory, a laser interferometer with a 3 km arm len... more KAGRA is a newly built gravitational wave observatory, a laser interferometer with a 3 km arm length, located at Kamioka, Gifu, Japan. In this series of articles we present an overview of the baseline KAGRA, for which we finished installing the designed configuration in 2019. This article describes the method of calibration (CAL) used for reconstructing gravitational wave signals from the detector outputs, as well as the characterization of the detector (DET). We also review the physical environmental monitoring (PEM) system and the geophysics interferometer (GIF). Both are used for characterizing and evaluating the data quality of the gravitational wave channel. They play important roles in utilizing the detector output for gravitational wave searches. These characterization investigations will be even more important in the near future, once gravitational wave detection has been achieved, and in using KAGRA in the gravitational wave astronomy era.

Astronomy & Astrophysics, 2008

Context. Hydrous silicates occur in various cosmic environments, and are among the minerals with ... more Context. Hydrous silicates occur in various cosmic environments, and are among the minerals with the most pronounced bands in the far infrared (FIR) spectral region. Given that Herschel and ALMA will open up new possibilities for astronomical FIR and sub-mm spectroscopy, data characterizing the dielectric properties of these materials at long wavelengths are desirable. Aims. We aimed at examining the FIR spectra of talc, picrolite, montmorillonite, and chamosite, which belong to four different groups of phyllosilicates. We tabulated positions and band widths of the FIR bands of these minerals depending on the dust temperature. Methods. By means of powder transmission spectroscopy, spectra of the examined materials were measured in the wavelength range 25−500 μm at temperatures of 300, 200, 100, and 10 K. Results. Room-temperature measurements yield the following results. For talc, a previously unknown band, centered at 98.5 μm, was found, in addition to bands at 56.5 and 59.5 μm. For montmorillonite, several bands at wavelengths <110 μm were detected, including a band at 105 μm with an FWHM of about 10 μm. Picrolite shows a sharp 77 μm FIR band. Chamosite is characterized by bands in the 72−92 μm range, and a prominent band at 277 μm. At decreasing temperature, most of the bands shift to shorter wavelengths. Conclusions. Examining a potential counterpart of the 105 μm band in the spectra of HD 142527 and HD 100546, we find that the broad band in the spectra of these young stars-extending from 85 to 125 μm-cannot be due to montmorillonite or any of the hydrous silicates we studied, since these materials have sharper bands in the FIR wavelength range than previously assumed, especially at low temperatures.

Optical constants are obtained by reflectance measurement with polarized light at elevated temper... more Optical constants are obtained by reflectance measurement with polarized light at elevated temperature

Optical constants are obtained by reflectance measurement with polarized light in a temperature r... more Optical constants are obtained by reflectance measurement with polarized light in a temperature range of 10 K to 928 K