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1. Premerger observation and characterization of massive black hole binaries

Author

Davies, Gareth Cabourn, Harry, Ian, Williams, Michael J., Bandopadhyay, Diganta, Barack, Leor, Bayle, Jean-Baptiste, Hoy, Charlie, Klein, Antoine, Middleton, Hannah, Moore, Christopher J., Nuttall, Laura, Pratten, Geraint, Vecchio, Alberto, and Woan, Graham

Subjects
High Energy Physics - Experiment, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract

We demonstrate an end-to-end technique for observing and characterizing massive black hole binary signals before they merge with the LISA space-based gravitational-wave observatory. Our method uses a zero-latency whitening filter, originally designed for rapidly observing compact binary mergers in ground-based observatories, to be able to observe signals with no additional latency due to filter length. We show that with minimal computational cost, we are able to reliably observe signals as early as 14 days premerger as long as the signal has accrued a signal-to-noise ratio of at least 8 in the LISA data. We also demonstrate that this method can be used to characterize the source properties, providing early estimates of the source's merger time, chirp mass, and sky localization. Early observation and characterization of massive black holes is crucial to enable the possibility of rapid multimessenger observations, and to ensure that LISA can enter a protected operating period when the merger signal arrives., Comment: 16 pages, 11 figures

Published
2024

2. Communicating the gravitational-wave discoveries of the LIGO-Virgo-KAGRA Collaboration

Author

Middleton, Hannah, Berry, Christopher P L, Arnaud, Nicolas, Blair, David, Bondell, Jacqueline, Bonino, Alice, Bonne, Nicolas, Chatterjee, Debarati, Chaty, Sylvain, Colloms, Storm, Cominsky, Lynn, Conti, Livia, Cordero-Carrión, Isabel, Coyne, Robert, Doctor, Zoheyr, Freise, Andreas, Geller, Aaron, Green, Anna C, Gupta, Jen, Holz, Daniel, Katzman, William, Kaur, Jyoti, Keitel, David, Key, Joey Shapiro, Kijbunchoo, Nutsinee, Knox, Carl, Krawczyk, Coleman, Lang, Ryan N, Larson, Shane L, Milde, Susanne, Napolano, Vincenzo, North, Chris, Rieger, Sascha, Rossi, Giada, Shinkai, Hisaaki, Simonnet, Aurore, and Spencer, Andrew

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology, Physics - Physics Education, Physics - Popular Physics
Abstract

The LIGO-Virgo-KAGRA (LVK) Collaboration has made breakthrough discoveries in gravitational-wave astronomy, a new field that provides a different means of observing our Universe. Gravitational-wave discoveries are possible thanks to the work of thousands of people from across the globe working together. In this article, we discuss the range of engagement activities used to communicate LVK gravitational-wave discoveries and the stories of the people behind the science, using the activities surrounding the release of the third Gravitational-Wave Transient Catalog as a case study., Comment: 15 pages, 7 figures, published in JCOM: https://doi.org/10.22323/2.23070803

Published
2024
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3. Search for continuous gravitational waves directed at sub-threshold radiometer candidates in O3 LIGO data

Author

Knee, Alan M., Du, Helen, Goetz, Evan, McIver, Jess, Carlin, Julian B., Sun, Ling, Dunn, Liam, Strang, Lucy, Middleton, Hannah, and Melatos, Andrew

Subjects
General Relativity and Quantum Cosmology
Abstract

We present results of a follow-up search for continuous gravitational waves (CWs) associated with sub-threshold candidates from the LIGO-Virgo-KAGRA (LVK) All-Sky All-Frequency (ASAF) directed radiometer analysis, using Advanced LIGO data from the third observing run (O3). Each ASAF candidate corresponds to a $1/32\,\,\mathrm{Hz}$ frequency band and ${\sim}13\,\,\mathrm{deg}^2$ sky pixel. Assuming they represent possible CW sources, we analyze all $515$ ASAF candidates using a semi-coherent, $\mathcal{F}$-statistic-based matched filter search. The search algorithm incorporates a hidden Markov model (HMM), expanding the signal model to allow frequency spin-wandering, as well as unmodeled frequency evolution of less than $10^{-5}$ Hz per day that is not captured by the searched range of $\pm10^{-9}\,\,\mathrm{Hz/s}$ in frequency derivative. Significance thresholds with a $5\%$ probability of false alarm per ASAF candidate are determined empirically by searching detector noise at various off-target sky positions. We obtain $14$ outliers surviving a set of vetoes designed to eliminate instrumental artifacts. Upon further investigation, these outliers are deemed unlikely to represent astrophysical signals. We estimate the sensitivity of our search to both isolated and binary sources with orbital period greater than one year by recovering simulated signals added to detector data. The minimum detectable strain amplitude at $95\%$ confidence for isolated (long-period binary) sources is $h_0^{95\%} = 8.8\times 10^{-26}$ ($9.4\times 10^{-26}$) at a frequency of $222.6\,\,\mathrm{Hz}$. While this study focuses on ASAF sub-threshold candidates, the method presented could be applied to follow up candidates from future all-sky CW searches, complementing currently existing methods., Comment: 20 pages, 12 figures. Published in PRD

Published
2023
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4. Precision tracking of massive black hole spin evolution with LISA

Author

Pratten, Geraint, Schmidt, Patricia, Middleton, Hannah, and Vecchio, Alberto

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The Laser Interferometer Space Antenna (LISA) will play a vital role in constraining the origin and evolution of massive black holes throughout the Universe. In this study we use a waveform model (IMRPhenomXPHM) that includes both precession and higher multipoles, and full Bayesian inference to explore the accuracy to which LISA can constrain the binary parameters. We demonstrate that LISA will be able to track the evolution of the spins -- magnitude and orientation -- to percent accuracy, providing crucial information on the dynamics and evolution of massive black hole binaries and the galactic environment in which the merger takes place. Such accurate spin-tracking further allows LISA to measure the recoil velocity of the remnant black hole to better than $100\,\mathrm{km}\,\mathrm{s}^{-1}$ (90\% credibility) and its direction to a few degrees, which provides additional important astrophysical information on the post-merger association. Using a systematic suite of binaries, we showcase that the component masses will be measurable at the sub-percent level, the sky area can be constrained to within $\Delta \Omega_{90} \approx 0.01 \, \rm{deg}^2$, and the binary redshift to less than $0.01$., Comment: 14+6 pages, 8 figures, fixed typo

Published
2023

5. The gravitational-wave background null hypothesis: Characterizing noise in millisecond pulsar arrival times with the Parkes Pulsar Timing Array

Author

Reardon, Daniel J., Zic, Andrew, Shannon, Ryan M., Di Marco, Valentina, Hobbs, George B., Kapur, Agastya, Lower, Marcus E., Mandow, Rami, Middleton, Hannah, Miles, Matthew T., Rogers, Axl F., Askew, Jacob, Bailes, Matthew, Bhat, N. D. Ramesh, Cameron, Andrew, Kerr, Matthew, Kulkarni, Atharva, Manchester, Richard N., Nathan, Rowina S., Russell, Christopher J., Osłowski, Stefan, and Zhu, Xing-Jiang

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics, General Relativity and Quantum Cosmology
Abstract

The noise in millisecond pulsar (MSP) timing data can include contributions from observing instruments, the interstellar medium, the solar wind, solar system ephemeris errors, and the pulsars themselves. The noise environment must be accurately characterized in order to form the null hypothesis from which signal models can be compared, including the signature induced by nanohertz-frequency gravitational waves (GWs). Here we describe the noise models developed for each of the MSPs in the Parkes Pulsar Timing Array (PPTA) third data release, which have been used as the basis of a search for the isotropic stochastic GW background. We model pulsar spin noise, dispersion measure variations, scattering variations, events in the pulsar magnetospheres, solar wind variability, and instrumental effects. We also search for new timing model parameters and detected Shapiro delays in PSR~J0614$-$3329 and PSR~J1902$-$5105. The noise and timing models are validated by testing the normalized and whitened timing residuals for Gaussianity and residual correlations with time. We demonstrate that the choice of noise models significantly affects the inferred properties of a common-spectrum process. Using our detailed models, the recovered common-spectrum noise in the PPTA is consistent with a power law with a spectral index of $\gamma=13/3$, the value predicted for a stochastic GW background from a population of supermassive black hole binaries driven solely by GW emission., Comment: 18 pages, 10 figures. Accepted for publication in ApJL

Published
2023
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6. Implications of pulsar timing array observations for LISA detections of massive black hole binaries

Author

Steinle, Nathan, Middleton, Hannah, Moore, Christopher J., Chen, Siyuan, Klein, Antoine, Pratten, Geraint, Buscicchio, Riccardo, Finch, Eliot, and Vecchio, Alberto

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Pulsar timing arrays (PTAs) and the Laser Interferometer Space Antenna (LISA) will open complementary observational windows on massive black-hole binaries (MBHBs), i.e., with masses in the range $\sim 10^6 - 10^{10}\,$ M$_{\odot}$. While PTAs may detect a stochastic gravitational-wave background from a population of MBHBs, during operation LISA will detect individual merging MBHBs. To demonstrate the profound interplay between LISA and PTAs, we estimate the number of MBHB mergers that one can expect to observe with LISA by extrapolating direct observational constraints on the MBHB merger rate inferred from PTA data. For this, we postulate that the common signal observed by PTAs (and consistent with the increased evidence recently reported) is an astrophysical background sourced by a single MBHB population. We then constrain the LISA detection rate, $\mathcal{R}$, in the mass-redshift space by combining our Bayesian-inferred merger rate with LISA's sensitivity to spin-aligned, inspiral-merger-ringdown waveforms. Using an astrophysically-informed formation model, we predict a 95$\%$ upper limit on the detection rate of $\mathcal{R} < 134\,{\rm yr}^{-1}$ for binaries with total masses in the range $10^7 - 10^8\,$ M$_{\odot}$. For higher masses, i.e., $>10^8\,$ M$_{\odot}$, we find $\mathcal{R} < 2\,(1)\,\mathrm{yr}^{-1}$ using an astrophysically-informed (agnostic) formation model, rising to $11\,(6)\,\mathrm{yr}^{-1}$ if the LISA sensitivity bandwidth extends down to $10^{-5}$ Hz. Forecasts of LISA science potential with PTA background measurements should improve as PTAs continue their search.

Published
2023

7. On the LISA science performance in observations of short-lived signals from massive black hole binary coalescences

Author

Pratten, Geraint, Klein, Antoine, Moore, Christopher J., Middleton, Hannah, Steinle, Nathan, Schmidt, Patricia, and Vecchio, Alberto

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The observation of massive black hole binary systems is one of the main science objectives of the Laser Interferometer Space Antenna (LISA). The instrument's design requirements have recently been revised: they set a requirement at $0.1\,\mathrm{mHz}$, with no additional explicit requirements at lower frequencies. This has implications for observations of the short-lived signals produced by the coalescence of massive and high-redshift binaries. Here we consider the most pessimistic scenario: the (unlikely) case in which LISA has no sensitivity below $0.1\,\mathrm{mHz}$. We show that the presence of higher multipoles (beyond the dominant $\ell = |m| = 2$ mode) in the gravitational radiation from these systems, which will be detectable with a total signal-to-noise ratio $\sim 10^3$, allows LISA to retain the capability to accurately measure the physical parameters, the redshift, and to constrain the sky location. To illustrate this point, we consider a few select binaries in a total (redshifted) mass range of $4 \times10^6 - 4 \times 10^7\,M_\odot$ whose ($\ell = |m| = 2$) gravitational-wave signals last between $\approx 12$ hours and $\approx 20$ days in band. We model the emitted gravitational radiation using the highly accurate (spin-aligned) waveform approximant IMRPhenomXHM and carry out a fully coherent Bayesian analysis on the LISA noise-orthogonal time-delay-interferometry channels., Comment: 13 pages, 6 figures, comments welcome!

Published
2022
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8. Identifying LISA verification binaries among the Galactic population of double white dwarfs

Author

Finch, Eliot, Bartolucci, Giorgia, Chucherko, Daniel, Patterson, Ben G., Korol, Valeriya, Klein, Antoine, Bandopadhyay, Diganta, Middleton, Hannah, Moore, Christopher J., and Vecchio, Alberto

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Double white dwarfs (DWDs) will be the most numerous gravitational-wave (GW) sources for the Laser Interferometer Space Antenna (LISA). Most of the Galactic DWDs will be unresolved and will superpose to form a confusion noise foreground, the dominant LISA noise source around $\sim 0.5\mathrm{-}3\,\mathrm{mHz}$. A small fraction of these sources will stand out from the background and be individually detectable. Uniquely among GW sources, a handful of these binaries will be known in advance from electromagnetic (EM) observations and will be guaranteed sources of detectable GWs in the LISA band; these are known as verification binaries (VBs). High-cadence photometric surveys are continuously discovering new VB systems, and their number will continue to grow ahead of the launch of LISA. We analyse, in a fully Bayesian framework, all the currently known VB candidates with the latest design requirements for the LISA mission and find that 25 of the considered sources can be detected within a $4\,\mathrm{yr}$ observation time. We explore what can be expected from GW observations, both alone and in combination with EM observations, and estimate the VB's time to detection in the early months of LISA operations. We also show how VBs can be analysed in the case where their GW signals compete with many other unknown binary signals (both resolved and unresolved) from a realistic Galactic population of DWDs., Comment: 13 pages, 8 figures, plus appendices (accepted in Monthly Notices of the Royal Astronomical Society on 26 April 2023)

Published
2022
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9. Bayesian analysis of systematic errors in the determination of the constant of gravitation

Author

Rinaldi, Stefano, Middleton, Hannah, Del Pozzo, Walter, and Gair, Jonathan

Subjects
General Relativity and Quantum Cosmology
Abstract

Measurements of the gravitational constant $G$ are notoriously difficult. Individual state-of-the-art experiments have managed to determine the value of $G$ with high precision: although, when considered collectively, the range in the measured values of $G$ far exceeds individual uncertainties, suggesting the presence of unaccounted for systematic effects. Here, we propose a Bayesian framework to account for the presence of systematic errors in the various measurement of $G$ while proposing a consensus value, following two paths: a parametric approach, based on the Maximum Entropy Principle, and a non-parametric one, the latter being a very flexible approach not committed to any specific functional form. With both our methods, we find that the uncertainty on this fundamental constant, once systematics are included, is significantly larger than what quoted in CODATA 2018. Moreover, the morphology of the non-parametric distribution hints towards the presence of several sources of unaccounted for systematics. In light of this, we recommend a consensus value for the gravitational constant $G = 6.6740^{+0.0015}_{-0.0015} \times 10^{-11}\ \mathrm{m}^3\ \mathrm{kg}^{-1}\ \mathrm{s}^{-2}$., Comment: 11 pages, 2 figures. Accepted for publication in EPJ C

Published
2022

10. Validating continuous gravitational-wave candidates from a semicoherent search using Doppler modulation and an effective point spread function

Author

Jones, Dana, Sun, Ling, Carlin, Julian, Dunn, Liam, Millhouse, Meg, Middleton, Hannah, Meyers, Patrick, Clearwater, Patrick, Beniwal, Deeksha, Strang, Lucy, Vargas, Andrés, and Melatos, Andrew

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Following up large numbers of candidates in continuous gravitational wave searches presents a challenge, particularly in regard to computational power and the time required to manually scrutinize each of the candidates. It is important to design and test good follow-up procedures that are safe (i.e., minimize false dismissals) and computationally efficient across many search configurations. We investigate two follow-up procedures, or "vetoes," both of which exploit the Doppler modulation predicted in astrophysical signals. In particular, we introduce the concept of using an effective point spread function as part of our veto criteria. We take advantage of a well-established semicoherent search algorithm based on a hidden Markov model to study various search configurations and to generalize the veto criteria by considering the overall veto performance in terms of efficiency and safety. The results can serve as a guideline for follow-up studies in future continuous gravitational wave searches using a hidden Markov model algorithm. The results also apply qualitatively to other semicoherent search algorithms., Comment: 24 pages, 15 figures

Published
2022
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11. An estimate of the stochastic gravitational wave background from the MassiveBlackII simulation

Author

Sykes, Bailey, Middleton, Hannah, Melatos, Andrew, Di Matteo, Tiziana, DeGraf, Colin, and Bhowmick, Aklant

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

A population of super-massive black hole binaries is expected to generate a stochastic gravitational wave background (SGWB) in the pulsar timing array (PTA) frequency range of $10^{-9}$--$10^{-7}$ Hz. Detection of this signal is a current observational goal and so predictions of its characteristics are of significant interest. In this work we use super-massive black hole binary mergers from the MassiveBlackII simulation to estimate the characteristic strain of the stochastic background. We examine both a gravitational wave driven model of binary evolution and a model which also includes the effects of stellar scattering and a circumbinary gas disk. Results are consistent with PTA upper limits and similar to estimates in the literature. The characteristic strain at a reference frequency of $1 yr^{-1}$ is found to be $A_{yr^{-1}} = 6.9 \times 10^{-16}$ and $A_{yr^{-1}} = 6.4 \times 10^{-16}$ in the gravitational-wave driven and stellar scattering/gas disk cases, respectively. Using the latter approach, our models show that the SGWB is mildly suppressed compared to the purely gravitational wave driven model as frequency decreases inside the PTA frequency band., Comment: 10 pages, 3 figures, 1 table, accepted for publication in MNRAS

Published
2022
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12. Continuous gravitational waves in the lab: recovering audio signals with a table-top optical microphone

Author

Gardner, James W., Middleton, Hannah, Liu, Changrong, Melatos, Andrew, Evans, Robin, Moran, William, Beniwal, Deeksha, Cao, Huy Tuong, Ingram, Craig, Brown, Daniel, and Ng, Sebastian

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Instrumentation and Methods for Astrophysics, Physics - Physics Education
Abstract

Gravitational-wave observatories around the world are searching for continuous waves: persistent signals from sources such as spinning neutron stars. These searches use sophisticated statistical techniques to look for weak signals in noisy data. In this paper, we demonstrate these techniques using a table-top model gravitational-wave detector: a Michelson interferometer where sound is used as an analog for gravitational waves. Using signal processing techniques from continuous-wave searches, we demonstrate the recovery of tones with constant and wandering frequencies. We also explore the use of the interferometer as a teaching tool for educators in physics and electrical engineering by using it as an "optical microphone" to capture music and speech. A range of filtering techniques used to recover signals from noisy data are detailed in the Supplementary Material. Here, we present highlights of our results using a combined notch plus Wiener filter and the statistical log minimum mean-square error (logMMSE) estimator. Using these techniques, we easily recover recordings of simple chords and drums, but complex music and speech are more challenging. This demonstration can be used by educators in undergraduate laboratories and can be adapted for communicating gravitational-wave and signal-processing topics to non-specialist audiences., Comment: 13 pages, 8 figures. Supplementary Material: 15 pages, 6 figures. To be published in the American Journal of Physics (accepted December 2021)

Published
2022
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13. Mode changing in J1909$-$3744: the most precisely timed pulsar

Author

Miles, Matthew T., Shannon, Ryan M., Bailes, Matthew, Reardon, Daniel J., Buchner, Sarah, Middleton, Hannah, and Spiewak, Renee

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present baseband radio observations of the millisecond pulsar J1909$-$3744, the most precisely timed pulsar, using the MeerKAT telescope as part of the MeerTime pulsar timing array campaign. During a particularly bright scintillation event the pulsar showed strong evidence of pulse mode changing, among the first millisecond pulsars and the shortest duty cycle millisecond pulsar to do so. Two modes appear to be present, with the weak (lower signal-to-noise ratio) mode arriving $9.26$ $\pm 3.94$ $\mu$s earlier than the strong counterpart. Further, we present a new value of the jitter noise for this pulsar of $8.20 \pm 0.14$ ns in one hour, finding it to be consistent with previous measurements taken with the MeerKAT ($9 \pm 3$ ns) and Parkes ($8.6 \pm 0.8$ ns) telescopes, but inconsistent with the previously most precise measurement taken with the Green Bank telescope ($14 \pm 0.5$ ns). Timing analysis on the individual modes is carried out for this pulsar, and we find an approximate $10\%$ improvement in the timing precision is achievable through timing the strong mode only as opposed to the full sample of pulses. By forming a model of the average pulse from templates of the two modes, we time them simultaneously and demonstrate that this timing improvement can also be achieved in regular timing observations. We discuss the impact an improvement of this degree on this pulsar would have on searches for the stochastic gravitational wave background, as well as the impact of a similar improvement on all MeerTime PTA pulsars.

Published
2021
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14. Evidence for hierarchical black hole mergers in the second LIGO--Virgo gravitational-wave catalog

Author

Kimball, Chase, Talbot, Colm, Berry, Christopher P. L., Zevin, Michael, Thrane, Eric, Kalogera, Vicky, Buscicchio, Riccardo, Carney, Matthew, Dent, Thomas, Middleton, Hannah, Payne, Ethan, Veitch, John, and Williams, Daniel

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

We study the population properties of merging binary black holes in the second LIGO--Virgo Gravitational-Wave Transient Catalog assuming they were all formed dynamically in gravitationally bound clusters. Using a phenomenological population model, we infer the mass and spin distribution of first-generation black holes, while self-consistently accounting for hierarchical mergers. Considering a range of cluster masses, we see compelling evidence for hierarchical mergers in clusters with escape velocities $\gtrsim 100~\mathrm{km\,s^{-1}}$. For our most probable cluster mass, we find that the catalog contains at least one second-generation merger with $99\%$ credibility. We find that the hierarchical model is preferred over an alternative model with no hierarchical mergers (Bayes factor $\mathcal{B} > 1400$) and that GW190521 is favored to contain two second-generation black holes with odds $\mathcal{O}>700$, and GW190519, GW190602, GW190620, and GW190706 are mixed-generation binaries with $\mathcal{O} > 10$. However, our results depend strongly on the cluster escape velocity, with more modest evidence for hierarchical mergers when the escape velocity is $\lesssim 100~\mathrm{km\,s^{-1}}$. Assuming that all binary black holes are formed dynamically in globular clusters with escape velocities on the order of tens of $\mathrm{km\,s^{-1}}$, GW190519 and GW190521 are favored to include a second-generation black hole with odds $\mathcal{O}>1$. In this case, we find that $99\%$ of black holes from the inferred total population have masses that are less than $49\,M_{\odot}$, and that this constraint is robust to our choice of prior on the maximum black hole mass., Comment: 15 pages, 11 figures, 1 appendix

Published
2020
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15. Massive black hole binary systems and the NANOGrav 12.5 year results

Author

Middleton, Hannah, Sesana, Alberto, Chen, Siyuan, Vecchio, Alberto, Del Pozzo, Walter, and Rosado, Pablo A.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, General Relativity and Quantum Cosmology
Abstract

The North American Nanohertz Observatory for Gravitational Waves (NANOGrav) has recently reported evidence for the presence of a common stochastic signal across their array of pulsars. The origin of this signal is still unclear. One of the possibilities is that it is due to a stochastic gravitational wave background (SGWB) in the $\sim 1-10\,{\rm nHz}$ frequency region. Taking the NANOGrav observational result at face value, we show that this signal would be fully consistent with a SGWB produced by an unresolved population of in-spiralling massive black hole binaries (MBHBs) predicted by current theoretical models. Considering an astrophysically agnostic model we find that the MBHB merger rate is loosely constrained to the range $10^{-11} - 2$ $\mathrm{Mpc}^{-3}\,\mathrm{Gyr}^{-1}$. Including additional constraints from galaxy pairing fractions and MBH-bulge scaling relations, we find that the MBHB merger rate is $10^{-5} - 5\times10^{-4}$ $\mathrm{Mpc}^{-3}\,\mathrm{Gyr}^{-1}$, the MBHB merger time-scale is $\le 3\,\mathrm{Gyr}$ and the norm of the $M_\mathrm{BH}-M_\mathrm{bulge}$ relation $\ge 1.2\times 10^{8}\,M_\odot$ (all intervals quoted at 90\% confidence). Regardless of the astrophysical details of MBHB assembly, this result would imply that a sufficiently large population of massive black holes pair up, form binaries and merge within a Hubble time., Comment: 6 pages, 4 figures, to be submitted

Published
2020
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16. Search for gravitational waves from five low mass X-ray binaries in the second Advanced LIGO observing run with an improved hidden Markov model

Author

Middleton, Hannah, Clearwater, Patrick, Melatos, Andrew, and Dunn, Liam

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, General Relativity and Quantum Cosmology
Abstract

Low mass X-ray binaries are prime targets for continuous gravitational wave searches by ground-based interferometers. Results are presented from a search for five low-mass X-ray binaries whose spin frequencies and orbital elements are measured accurately from X-ray pulsations: HETE J1900.1-2455, IGR J00291+5934, SAX J1808.4-3658, XTE J0929-314, and XTE J1814-338. Data are analysed from Observing Run 2 of the Advanced Laser Interferometer Gravitational-wave Observatory (LIGO). The search algorithm uses a hidden Markov model to track spin wandering, the $\mathcal{J}$-statistic maximum likelihood matched filter to track orbital phase, and a suite of five vetoes to reject artefacts from non-Gaussian noise. The search yields a number of low-significance, above threshold candidates consistent with the selected false-alarm probability. The candidates will be followed up in subsequent observing runs., Comment: 24 pages, 11 figures; accepted for publication in Physical Review D

Published
2020
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18. *ABA syncretism patterns in pronominal morphology

Author

Middleton, Hannah Jane

Subjects
415
Abstract

Syncretism patterns in strong free-standing pronominal forms (specifically anaphors, diaphors, and pronouns) show that they share an underlying functional structure. Based on a new typology of 80 languages, I argue for a hierarchical structure such that diaphors contain pronouns, and anaphors contain diaphors. Each layer of the structure introduces a functional head which places an additional restriction on the antecedent of the pronominal form. The proposed structure derives the fact that of five logically possible patterns of syncretism, only four are attested. I argue further that morphological variation in the realisation of Strict and Sloppy interpretations of anaphors and diaphors can be captured if the features A and D are optionally allowed to drop in the interpretation of alternatives (Sauerland 2013), and that morphological variation in the exponence of anaphors, diaphors and pronouns in languages such as Peranakan Javanese of Semarang can be captured if the notion of Optional Impoverishment is adopted from Nevins & Parrott 2010. Finally, I consider two analyses of pseudo-ABA patterns of syncretism, and argue that only the simple analysis is compatible with the broader analysis of the morphology and morphological behaviour of pronominal forms that I propose in this thesis. In the simple analysis, A and D are not cyclic nodes, and the pronominal tree spells out when it merges with K(ase) (or some higher node). Pseudo-ABA patterns arise when a spanned exponent for [A [D]] and an exponent for P together spell out more of the pronominal structure than any other combination of exponents. The alternative analysis, in which A and D are cyclic nodes, is incompatible with the analysis of variable exponence found in pronominal forms.

Published
2020

19. Characterization of low-significance gravitational-wave compact binary sources

Author

Huang, Yiwen, Middleton, Hannah, Ng, Ken K. -Y., Vitale, Salvatore, and Veitch, John

Subjects
General Relativity and Quantum Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are roughly distributed uniformly in comoving volume. In this paper we simulate weak signals from compact binary coalescences of various morphologies and optimal network signal-to-noise ratios (henceforth SNRs), and analyze if and to which extent their parameters can be measured by advanced LIGO and Virgo in their third observing run. We show that subthreshold binary neutron stars, with SNRs below 12 (10) yield uncertainties in their sky position larger than 400 (700) $\mathrm{deg}^2$ (90% credible interval). The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for BNSs and neutron star black hole mergers. For sources with SNRs below 8, it is not uncommon that the extrinsic parameters, sky position and distance, cannot be measured. Next, we look at the intrinsic parameters, masses and spins. We show that the detector-frame chirp mass can sometimes be measured with uncertainties below 1% even for sources at SNRs of 6, although multimodality is not uncommon and can significantly broaden the posteriors. The effective inspiral spin is best measured for neutron star black hole mergers, for which the uncertainties can be as low as $\sim0.08$ ($\sim 0.2$) at SNR 12 (8). The uncertainty is higher for systems with comparable component masses or lack of spin precession., Comment: 15 pages, 12 figures, 6 tables; Results unchanged from previous versions, provided additional details; public data release for posterior samples: https://git.ligo.org/yiwen.huang/public-lowsnr-data-release/

Published
2018
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20. Astrophysical inference from pulsar timing array searches for gravitational waves

Author

Middleton, Hannah Rose

Subjects
500, QB Astronomy, QC Physics
Abstract

Gravitational waves (GWs) have been detected for the first time in 2015 by the LIGO-Virgo Scientific Collaboration. The source of the GWs was a binary black hole (BBH). The observation caught the final fraction of a second as the two black holes spiralled together and merged. This observation (and the others to follow) marked the beginnings of GW astronomy, ‘a new window on the dark universe’, providing a means to observe astronomical phenomena which may be completely inaccessible via other avenues as well as a new testing ground for Einstein’s theory of general relativity (GR). However, this is just the beginning – like electromagnetic astrophysics, there is a full spectrum of GW frequencies to explore. At very low frequencies, pulsar timing arrays (PTAs) are being used to search for the GW background from the merging population of massive black hole binaries (MBHBs). No detection has yet been made, but upper limits have been placed. Here we present results on what inference on the MBHB population can be learnt from present and possible future PTA results, and also compare current upper limits with astrophysical predictions, finding them to be fully consistent so far. We also present a generic method for testing the consistency of a theory against experimental evidence in the situation where there is no strong viable alternative (for example GR). We apply this to BBH observations, finding them to be fully consistent with GR and also to Newton’s constant of gravitation, where there is considerable inconsistency between measurements.

Published
2018

21. No tension between assembly models of supermassive black hole binaries and pulsar observations

Author

Middleton, Hannah, Chen, Siyuan, Del Pozzo, Walter, Sesana, Alberto, and Vecchio, Alberto

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Pulsar timing arrays (PTAs) are presently the only means to search for the gravitational wave stochastic background from supermassive black hole binary populations, considered to be within the grasp of current or near future observations. However, the stringent upperlimit set by the Parkes PTA (Shannon et al. 2013, 2015) has been interpreted as excluding at $> 90\%$ confidence the current paradigm of binary assembly through galaxy mergers and hardening via stellar interactions, suggesting evolution is accelerated (by stars and/or gas) or stalled. Using Bayesian hierarchical modelling, we consider implications of this upperlimit for a comprehensive range of astrophysical scenarios, without invoking stalling nor more exotic physical processes. We find they are fully consistent with the upperlimit, but (weak) bounds on population parameters can be inferred. Bayes factors between models vary between $\approx 1.03$ -- $5.81$ and Kullback-Leibler divergences between characteristic amplitude prior and posterior lie between $0.37$ -- $0.85$. Considering prior astrophysical information on galaxy merger rates, recent upwards revisions of the black hole-galaxy bulge mass relation (Kormendy & Ho 2013) are disfavoured at $1.6\sigma$ against lighter models (e.g. Shankar et al. 2016). We also show, if no detection is achieved once sensitivity improves by an order of magnitude, the most optimistic scenario is disfavoured at $3.9\sigma$., Comment: 20 pages, 7 figures

Published
2017
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22. Probing the assembly history and dynamical evolution of massive black hole binaries with pulsar timing arrays

Author

Chen, Siyuan, Middleton, Hannah, Sesana, Alberto, Del Pozzo, Walter, and Vecchio, Alberto

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We consider the inverse problem in pulsar timing array (PTA) analysis, investigating what astrophysical information about the underlying massive black hole binary (MBHB) population can be recovered from the detection of a stochastic gravitational wave background (GWB). We employ a physically motivated model that connects the GWB spectrum to a series of parameters describing the underlying redshift evolution of the MBHB mass function and to the typical eccentricity they acquire while interacting with the dense environment of post merger galactic nuclei. This allows the folding in of information about the spectral shape of the GWB into the analysis. The priors on the model parameters are assumed to be uninformative and consistent with the current lack of secure observations of sub-parsec MBHBs. We explore the implications of current upper limits as well as of future detections with a variety of PTA configurations. We confirm our previous finding that current upper limits can only place an upper bound on the overall MBHB merger rate. Depending on the properties of the array, future detections can also constrain several MBHB population models at different degrees of fidelity. In particular, a simultaneous detection of a steepening of the spectrum at high frequency and a bending at low frequency will place strong constraints on both the MBHB mass function and on the typical eccentricity of inspiralling MBHBs, providing insights on MBHB astrophysics unlikely to be achievable by any other means., Comment: 14 pages, 6 figures, 1 table, published in MNRAS

Published
2016
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25. Parameter estimation on gravitational waves from neutron-star binaries with spinning components

Author

Farr, Ben, Berry, Christopher P. L., Farr, Will M., Haster, Carl-Johan, Middleton, Hannah, Cannon, Kipp, Graff, Philip B., Hanna, Chad, Mandel, Ilya, Pankow, Chris, Price, Larry R., Sidery, Trevor, Singer, Leo P., Urban, Alex L., Vecchio, Alberto, Veitch, John, and Vitale, Salvatore

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Inspiraling binary neutron stars are expected to be one of the most significant sources of gravitational-wave signals for the new generation of advanced ground-based detectors. We investigate how well we could hope to measure properties of these binaries using the Advanced LIGO detectors, which began operation in September 2015. We study an astrophysically motivated population of sources (binary components with masses $1.2~\mathrm{M}_\odot$--$1.6~\mathrm{M}_\odot$ and spins of less than $0.05$) using the full LIGO analysis pipeline. While this simulated population covers the observed range of potential binary neutron-star sources, we do not exclude the possibility of sources with parameters outside these ranges; given the existing uncertainty in distributions of mass and spin, it is critical that analyses account for the full range of possible mass and spin configurations. We find that conservative prior assumptions on neutron-star mass and spin lead to average fractional uncertainties in component masses of $\sim 16\%$, with little constraint on spins (the median $90\%$ upper limit on the spin of the more massive component is $\sim 0.7$). Stronger prior constraints on neutron-star spins can further constrain mass estimates, but only marginally. However, we find that the sky position and luminosity distance for these sources are not influenced by the inclusion of spin; therefore, if LIGO detects a low-spin population of BNS sources, less computationally expensive results calculated neglecting spin will be sufficient for guiding electromagnetic follow-up., Comment: 10 pages, 9 figures

Published
2015
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26. Astrophysical constraints on massive black hole binary evolution from Pulsar Timing Arrays

Author

Middleton, Hannah, Del Pozzo, Walter, Farr, Will M., Sesana, Alberto, and Vecchio, Alberto

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We consider the information that can be derived about massive black-hole binary populations and their formation history solely from current and possible future pulsar timing array (PTA) results. We use models of the stochastic gravitational-wave background from circular massive black hole binaries with chirp mass in the range $10^6 - 10^{11} M_\odot$ evolving solely due to radiation reaction. Our parameterised models for the black hole merger history make only weak assumptions about the properties of the black holes merging over cosmic time. We show that current PTA results place an upper limit on the black hole merger density which does not depend on the choice of a particular merger history model, however they provide no information about the redshift or mass distribution. We show that even in the case of a detection resulting from a factor of 10 increase in amplitude sensitivity, PTAs will only put weak constraints on the source merger density as a function of mass, and will not provide any additional information on the redshift distribution. Without additional assumptions or information from other observations, a detection cannot meaningfully bound the massive black hole merger rate above zero or any particular mass., Comment: Accepted by MNRAS Letters, 6 pages, 3 figures

Published
2015
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27. Parameter estimation for binary neutron-star coalescences with realistic noise during the Advanced LIGO era

Author

Berry, Christopher P. L., Mandel, Ilya, Middleton, Hannah, Singer, Leo P., Urban, Alex L., Vecchio, Alberto, Vitale, Salvatore, Cannon, Kipp, Farr, Ben, Farr, Will M., Graff, Philip B., Hanna, Chad, Haster, Carl-Johan, Mohapatra, Satya, Pankow, Chris, Price, Larry R., Sidery, Trevor, and Veitch, John

Subjects
Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Advanced ground-based gravitational-wave (GW) detectors begin operation imminently. Their intended goal is not only to make the first direct detection of GWs, but also to make inferences about the source systems. Binary neutron-star mergers are among the most promising sources. We investigate the performance of the parameter-estimation \edit{(PE)} pipeline that will be used during the first observing run of the Advanced Laser Interferometer Gravitational-wave Observatory (aLIGO) in 2015: we concentrate on the ability to reconstruct the source location on the sky, but also consider the ability to measure masses and the distance. Accurate, rapid sky-localization is necessary to alert electromagnetic (EM) observatories so that they can perform follow-up searches for counterpart transient events. We consider PE accuracy in the presence of \edit{non-stationary}, non-Gaussian noise. We find that the character of the noise makes negligible difference to the PE performance \edit{at a given signal-to-noise ratio}. The source luminosity distance can only be poorly constrained, the median $90\%$ ($50\%$) credible interval scaled with respect to the true distance is $0.85$ ($0.38$). However, the chirp mass is well measured. Our chirp-mass estimates are subject to systematic error because we used gravitational-waveform templates without component spin to carry out inference on signals with moderate spins, but the total error is typically less than $10^{-3} M_\odot$. The median $90\%$ ($50\%$) credible region for sky localization is $\sim600~\mathrm{deg^{2}}$ ($\sim150~\mathrm{deg^{2}}$), with $3\%$ ($30\%$) of detected events localized within $100~\mathrm{deg^{2}}$. Early aLIGO, with only two detectors, will have a sky-localization accuracy for binary neutron stars of hundreds of square degrees; this makes EM follow-up challenging, but not impossible., Comment: 21 pages, 24 figures. Matches published version. Data release at http://www.ligo.org/scientists/first2years/

Published
2014
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29. The Gravitational-wave Background Null Hypothesis: Characterizing Noise in Millisecond Pulsar Arrival Times with the Parkes Pulsar Timing Array

Author

Reardon, Daniel J., primary, Zic, Andrew, additional, Shannon, Ryan M., additional, Di Marco, Valentina, additional, Hobbs, George B., additional, Kapur, Agastya, additional, Lower, Marcus E., additional, Mandow, Rami, additional, Middleton, Hannah, additional, Miles, Matthew T., additional, Rogers, Axl F., additional, Askew, Jacob, additional, Bailes, Matthew, additional, Bhat, N. D. Ramesh, additional, Cameron, Andrew, additional, Kerr, Matthew, additional, Kulkarni, Atharva, additional, Manchester, Richard N., additional, Nathan, Rowina S., additional, Russell, Christopher J., additional, Osłowski, Stefan, additional, and Zhu, Xing-Jiang, additional

Published
2023
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32. Validating continuous gravitational-wave candidates from a semicoherent search using Doppler modulation and an effective point spread function

Author

Jones, Dana, primary, Sun, Ling, additional, Carlin, Julian, additional, Dunn, Liam, additional, Millhouse, Meg, additional, Middleton, Hannah, additional, Meyers, Patrick, additional, Clearwater, Patrick, additional, Beniwal, Deeksha, additional, Strang, Lucy, additional, Vargas, Andrés, additional, and Melatos, Andrew, additional

Published
2022
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33. On the determination of the constant of gravitation

Author

Rinaldi, Stefano, Middleton, Hannah, Del Pozzo, Walter, and Gair, Jonathan

Subjects
FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology
Abstract

Measurements of the gravitational constant G are notoriously difficult. Individual state-of-the-art experiments have managed to determine the value of G with high precision: although, when considered collectively, the range in the measured values of G far exceeds individual uncertainties, suggesting the presence of unaccounted for systematic effects. Here, we look at models for systematic errors on G and find that its uncertainty is significantly larger than quoted in CODATA 2018., 8 pages, 3 figures

Published
2022

34. Validating continuous gravitational-wave candidates based on Doppler modulation

Author

Jones, Dana, Sun, Ling, Carlin, Julian, Dunn, Liam, Millhouse, Meg, Middleton, Hannah, Meyers, Patrick, Clearwater, Patrick, Beniwal, Deeksha, Strang, Lucy, Vargas, Andrés, Melatos, Andrew, Jones, Dana, Sun, Ling, Carlin, Julian, Dunn, Liam, Millhouse, Meg, Middleton, Hannah, Meyers, Patrick, Clearwater, Patrick, Beniwal, Deeksha, Strang, Lucy, Vargas, Andrés, and Melatos, Andrew

Abstract

Following up large numbers of candidates in continuous gravitational wave searches presents a challenge, particularly in regard to computational power and the time required to manually scrutinize each of the candidates. It is important to design and test good follow-up procedures that are safe (i.e., minimize false dismissals) and computationally efficient across many search configurations. We investigate two existing follow-up procedures, or "vetoes," both of which exploit the Doppler modulation predicted in astrophysical signals. We take advantage of a well-established semicoherent search algorithm based on a hidden Markov model to study a wide variety of search configurations and to generalize the veto criteria by considering the overall veto performance in terms of efficiency and safety. The results can serve as a guideline for follow-up studies in future continuous gravitational wave searches using a hidden Markov model algorithm. The results also apply qualitatively to other semicoherent search algorithms., Comment: 20 pages, 11 figures

Published
2022

37. Evidence for Hierarchical Black Hole Mergers in the Second LIGO–Virgo Gravitational Wave Catalog

Author

Kimball, Chase, primary, Talbot, Colm, additional, Berry, Christopher P L, additional, Zevin, Michael, additional, Thrane, Eric, additional, Kalogera, Vicky, additional, Buscicchio, Riccardo, additional, Carney, Matthew, additional, Dent, Thomas, additional, Middleton, Hannah, additional, Payne, Ethan, additional, Veitch, John, additional, and Williams, Daniel, additional

Published
2021
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39. estimate of the stochastic gravitational wave background from the MassiveBlackII simulation.

Author

Sykes, Bailey, Middleton, Hannah, Melatos, Andrew, Di Matteo, Tiziana, DeGraf, Colin, and Bhowmick, Aklant

Subjects
*SUPERMASSIVE black holes, *SIGNAL detection, *GRAVITATIONAL waves, *BLACK people
Abstract

A population of supermassive black hole (SMBH) binaries is expected to generate a stochastic gravitational wave background (SGWB) in the pulsar timing array (PTA) frequency range of 10−9 to |$10^{-7}\, {\rm Hz}$|⁠. Detection of this signal is a current observational goal and so predictions of its characteristics are of significant interest. In this work, we use SMBH binary mergers from the MassiveBlackII simulation to estimate the characteristic strain of the stochastic background. We examine both a gravitational wave (GW) driven model of binary evolution and a model which also includes the effects of stellar scattering and a circumbinary gas disc. Results are consistent with PTA upper limits and similar to estimates in the literature. The characteristic strain at a reference frequency of |$1\, {\rm yr}^{-1}$| is found to be |$A_{\rm {yr}^{-1}}= 6.9 \times 10^{-16}$| and |$A_{\rm {yr}^{-1}}= 6.4 \times 10^{-16}$| in the GW-driven and stellar scattering/gas disc cases, respectively. Using the latter approach, our models show that the SGWB is mildly suppressed compared to the purely GW-driven model as frequency decreases inside the PTA frequency band. [ABSTRACT FROM AUTHOR]

Published
2022
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42. First-Year Students, Pen Pals, and Educational Transitions: A Service-Learning Project

Author

Middleton, Hannah, NC DOCKS at The University of North Carolina at Pembroke, Middleton, Hannah, and NC DOCKS at The University of North Carolina at Pembroke

Abstract

Throughout the academic career of a student, many important transitions occur. One of the most important transitions is that from high school to college made by first-year university students. This project takes a close look at this transition through the researcher’s experience coordinating a service-learning project that engages first-year students. Since fall 2016, UNCP students enrolled in Honors UNV 1000: First-year Seminar have participated in a service-learning project in which they write letters to middle school students enrolled at CIS Academy in Pembroke. Their letters relate their experiences as a new student at the university, what they are experiencing as they transition from high school to university, and advice about how their pen pals can also successfully make this transition. The CIS students in turn advise their first-year pen pals about success in school, describe their hopes and goals for the future, and ask questions about the experiences of university students.

Published
2019

43. Characterization of low-significance gravitational-wave compact binary sources

Author

Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Huang, Yiwen, Ng, Ken K. Y., Vitale, Salvatore, Middleton, Hannah, Veitch, John, Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Huang, Yiwen, Ng, Ken K. Y., Vitale, Salvatore, Middleton, Hannah, and Veitch, John

Abstract

Advanced LIGO and Virgo have so far detected gravitational waves from 10 binary black hole mergers (BBH) and 1 binary neutron star merger (BNS). In the future, we expect the detection of many more marginal sources, since compact binary coalescences detectable by advanced ground-based instruments are roughly distributed uniformly in comoving volume. In this paper we simulate weak signals from compact binary coalescences of various morphologies and optimal network signal-to-noise ratios (henceforth SNRs), and analyze if and to which extent their parameters can be measured by advanced LIGO and Virgo in their third observing run. We show that subthreshold binary neutron stars, with SNRs below 12 (10) yield uncertainties in their sky position larger than 400 (700) deg^{2} (90% credible interval). The luminosity distance, which could be used to measure the Hubble constant with standard sirens, has relative uncertainties larger than 40% for BNSs and neutron star black hole mergers. For sources with SNRs below 8, it is not uncommon that the extrinsic parameters, sky position and distance, cannot be measured. Next, we look at the intrinsic parameters, masses and spins. We show that the detector-frame chirp mass can sometimes be measured with uncertainties below 1% even for sources at SNRs of 6, although multimodality is not uncommon and can significantly broaden the posteriors. The effective inspiral spin is best measured for neutron star black hole mergers, for which the uncertainties can be as low as ∼0.08 (∼0.2) at SNR 12 (8). The uncertainty is higher for systems with comparable component masses or lack of spin precession., Solomon Buchsbaum AT&T Research Fund, National Science Foundation (U.S.), Laser Interferometer Gravitational Wave Observatory

Published
2019

45. Full band all-sky search for periodic gravitational waves in the O1 LIGO data

Author

Abbott, Benjamin P., Abbott, Rich, Abbott, Thomas D., Acernese, Fausto, Ackley, Kendall, Adams, Carl, Adams, Thomas, Addesso, Paolo, Adhikari, Rana X., Adya, Vaishali B., Affeldt, Christoph, Afrough, Mohammad, Agarwal, Bhanu, Agathos, Michalis, Agatsuma, Kazuhiro, Aggarwal, Nancy, Aguiar, Odylio D., Aiello, Lorenzo, Ain, Anirban, Allen, Bruce, Allen, Gabrielle, Allocca, Annalisa, Altin, Paul A., Amato, Alex, Ananyeva, Alena, Anderson, Stuart B., Anderson, Warren G., Angelova, Svetoslava V., Antier, Sarah, Appert, Stephen, Arai, Koji, Araya, Melody C., Areeda, Joseph S., Arnaud, Nicolas, Ascenzi, Stefano, Ashton, Gregory, Ast, M., Aston, Stuart M., Astone, Pia, Atallah, Dany V., Aufmuth, Peter, Aulbert, Carsten, AultONeal, K., Austin, Corey, Avila-Alvarez, A., Babak, Stanislav, Bacon, Philippe, Bader, Maria K.M., Bae, Sangwook, Baker, Paul T., Baldaccini, Francesca, Ballardin, Giulio, Ballmer, Stefan W., Banagiri, Sharan, Barayoga, Juan C., Barclay, Sheena E., Barish, Barry C., Barker, David, Barkett, Kevin, Barone, Fabrizio, Barr, Bryan, Barsotti, Lisa, Barsuglia, Matteo, Barta, Daniel, Bartlett, Jeffrey, Bartos, Imre, Bassiri, Riccardo, Basti, Andrea, Batch, James C., Bawaj, Mateusz, Bayley, Joseph C., Bazzan, Marco, Bécsy, Bence, Beer, Christian, Bejger, Michal, Belahcene, Imene, Bell, Angus S., Berger, Beverly K., Bergmann, Gerald, Bero, John J., Berry, Christopher P.L., Bersanetti, Diego, Bertolini, Alessandro, Betzwieser, Joseph, Bhagwat, Swetha, Bhandare, Rohan, Bilenko, Igor A., Billingsley, Garilynn, Billman, Chris R., Birch, Jeremy, Birney, Ross, Birnholtz, Ofek, Biscans, Sebastien, Biscoveanu, Sylvia, Bisht, Aparna, Bitossi, Massimiliano, Biwer, Christopher, Bizouard, Marieanne A., Blackburn, J.K., Blackman, Jonathan, Blair, Carl D., Blair, David G., Blair, Ryan M., Bloemen, Steven, Bock, Oliver, Bode, Nina, Boer, Michel, Bogaert, Gilles, Bohe, Alejandro, Bondu, Francois, Bonilla, Edgard, Bonnand, Romain, Boom, Boris A., Bork, Rolf, Boschi, Valerio, Bose, Sukanta, Bossie, Ken, Bouffanais, Yann, Bozzi, Antonella, Bradaschia, Carlo, Brady, Patrick R., Branchesi, Marica, Brau, Jim E., Briant, Tristan, Brillet, Alain, Brinkmann, Marc, Brisson, Violette, Brockill, Patrick, Broida, Jacob E., Brooks, Aidan F., Brown, Duncan A., Brown, Daniel D., Brunett, Sharon, Buchanan, Christopher C., Buikema, Aaron, Bulik, Tomasz, Bulten, Henk J., Buonanno, Alessandra, Buskulic, Damir, Buy, Christelle, Byer, Robert L., Cabero, Miriam, Cadonati, Laura, Cagnoli, Giampietro, Cahillane, Craig, Calderón Bustillo, J., Callister, Thomas A., Calloni, Enrico, Camp, Jordan B., Canepa, Maurizio, Canizares, Priscilla, Cannon, Kipp C., Cao, H., Cao, Junwei, Capano, Collin D., Capocasa, Eleonora, Carbognani, Franco, Caride, Santiago, Carney, Matthew F., Casanueva Diaz, J., Casentini, Claudio, Caudill, Sarah, Cavaglià, Marco, Cavalier, Fabien, Cavalieri, Roberto, Cella, Giancarlo, Cepeda, Christian B., Cerdá-Durán, P., Cerretani, Giovanni, Cesarini, Elisabetta, Chamberlin, Sydney J., Chan, Manleong, Chao, Shiuh, Charlton, Philip, Chase, Eve, Chassande-Mottin, E., Chatterjee, Deep, Cheeseboro, Belinda D., Chen, H.Y., Chen, Xu, Chen, Yanbei, Cheng, H.-P., Chia, Hanyu Y., Chincarini, Andrea, Chiummo, Antonino, Chmiel, Theresa, Cho, Heesuk S., Cho, M., Chow, Jong H., Christensen, Nelson, Chu, Qi, Chua, Alvin J.K., Chua, Sheon, Chung, A.K.W., Chung, Shinkee, Ciani, Giacomo, Ciecielag, P., Ciolfi, Riccardo, Cirelli, Carissa E., Cirone, Alessio, Clara, Filiberto, Clark, James A., Clearwater, Patrick, Cleva, Frederic, Cocchieri, Camillo, Coccia, Eugenio, Cohadon, P.-F., Cohen, David, Colla, Alberto, Collette, Christophe G., Cominsky, Lynn R., Constancio, M., Conti, Livia, Cooper, Sam J., Corban, Paul, Corbitt, Thomas R., Cordero-Carrión, I., Corley, Kenneth R., Cornish, Neil, Corsi, Alessandra, Cortese, Stefano, Costa, Cesar A., Coughlin, Eric T., Coughlin, Michael W., Coughlin, Scott B., Coulon, J.-P., Countryman, Stefan T., Couvares, Peter, Covas, Pep B., Cowan, Erika E., Coward, David M., Cowart, Matthew J., Coyne, Dennis C., Coyne, Robert, Creighton, Jolien D.E., Creighton, Teviet D., Cripe, Jonathan, Crowder, Sgwynne G., Cullen, Torrey J., Cumming, Alan, Cunningham, Liam, Cuoco, Elena, Dal Canton, Tito, Dálya, Gergely, Danilishin, Stefan L., D'Antonio, S., Danzmann, Karsten, Dasgupta, Arnab, Da Silva Costa, C.F., Dattilo, Vincenzo, Dave, Ishant, Davier, Michel, Davis, Derek, Daw, Edward J., Day, Brian, De, Soumi, Debra, D., Degallaix, Jerome, De Laurentis, M., Deléglise, Samuel, Del Pozzo, W., Demos, Nicholas, Denker, Timo, Dent, Thomas, De Pietri, R., Dergachev, Vladimir, De Rosa, R., DeRosa, R.T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, Jan, Dhurandhar, Sanjeev, Díaz, Mario C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Zoheyr, Dolique, Vincent, Donovan, Fred, Dooley, Katherine L., Doravari, Suresh, Dorosh, O., Dorrington, Iain, Douglas, Rebecca, Dovale Álvarez, M., Downes, Thomas P., Drago, Marco, Dreissigacker, Christoph, Driggers, Jenne C., Du, Zhihui, Ducrot, Marine, Dupej, Peter, Dwyer, Sheila E., Edo, Tega B., Edwards, Matthew C., Effler, Anamaria, Eggenstein, H.-B., Ehrens, Phil, Eichholz, Johannes, Eikenberry, Stephen S., Eisenstein, Robert A., Essick, Reed C., Estevez, Dimitri, Etienne, Zachariah B., Etzel, Todd, Evans, Matthew, Evans, Tom M., Factourovich, Maxim, Fafone, Viviana, Fair, Hannah, Fairhurst, Stephen, Fan, Xilong, Farinon, Stefania, Farr, Benjamin, Farr, Will M., Fauchon-Jones, E.J., Favata, Marc, Fays, Maxime, Fee, Campbell, Fehrmann, Henning, Feicht, Jon, Fejer, Martin M., Fernandez-Galiana, A., Ferrante, Isidoro, Ferreira, Elvis C., Ferrini, Federico, Fidecaro, Francesco, Finstad, Daniel, Fiori, Irene, Fiorucci, Donatella, Fishbach, Maya, Fisher, Ryan P., Fitz-Axen, M., Flaminio, Raffaele, Fletcher, Mark, Fong, Heather, Font, J.A., Forsyth, Perry W.F., Forsyth, Steven S., Fournier, J.-D., Frasca, Sergio, Frasconi, Franco, Frei, Zsolt, Freise, Andreas, Frey, Raymond, Frey, Valentin, Fries, Eric M., Fritschel, Peter, Frolov, Valery V., Fulda, Paul, Fyffe, Michael, Gabbard, Hunter, Gadre, Bhooshan U., Gaebel, Sebastian M., Gair, Jonathan R., Gammaitoni, Luca, Ganija, Miftar R., Gaonkar, Sharad G., Garcia-Quiros, C., Garufi, Fabio, Gateley, B., Gaudio, Sergio, Gaur, Gurudatt, Gayathri, V., Gehrels, Neil, Gemme, Gianluca, Genin, Eric, Gennai, Alberto, George, Daniel, George, Jogy, Gergely, Laszlo, Germain, Vincent, Ghonge, Sudarshan, Ghosh, Abhirup, Ghosh, Archisman, Ghosh, Shaon, Giaime, Joe A., Giardina, K.D., Giazotto, Adalberto, Gill, Kiranjyot, Glover, Lamar, Goetz, Evan, Goetz, Ryan, Gomes, Sandra, Goncharov, Boris, González, Gabriela, Gonzalez Castro, J.M., Gopakumar, A., Gorodetsky, Michael L., Gossan, Sarah E., GOSSELIN, Matthieu, Gouaty, Romain, Grado, Aniello, Graef, Christian, Granata, Massimo, Grant, Alastair, Gras, Slawomir, Gray, Corey, Greco, Giuseppe, Green, Anna C., Gretarsson, Elizabeth M., Groot, Paul, Grote, Hartmut, Grunewald, Steffen, Gruning, Pierre, Guidi, Gianluca M., Guo, Xiangyu, Gupta, Anuradha, Gupta, Manojipr K., Gushwa, Kaitlin E., Gustafson, Eric K., Gustafson, R., Halim, O., Hall, Bernard R., Hall, Evan D., Hamilton, Eleanor Z., Hammond, Giles, Haney, Maria, Hanke, Manuela M., Hanks, Jonathan, Hanna, Chad, Hannam, Mark D., Hannuksela, Otto A., Hanson, Joe, Hardwick, Terra, Harms, Jan, Harry, Gregg M., Harry, Ian W., Hart, Martin J., Haster, C.-J., Haughian, Karen, Healy, James, Heidmann, Antoine, Heintze, Matthew C., Heitmann, Henrich, Hello, Patrice, Hemming, Gary, Hendry, Martin, Heng, I.S., Hennig, J., Heptonstall, Alastair W., Heurs, Michele, Hild, Stefan, Hinderer, Tanja, Hoak, Daniel, Hofman, David, Holt, Kathy, Holz, Daniel E., Hopkins, Paul, Horst, Christian, Hough, James, Houston, Ewan A., Howell, Eric J., Hreibi, A., Hu, Yiming M., Huerta, Eliu A., Huet, Dominique, Hughey, Brennan, Husa, Sascha, Huttner, Sabina 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Abstract

We report on a new all-sky search for periodic gravitational waves in the frequency band 475-2000 Hz and with a frequency time derivative in the range of [-1.0,+0.1]×10-8 Hz/s. Potential signals could be produced by a nearby spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the data from Advanced LIGO's first observational run O1. No gravitational-wave signals were observed, and upper limits were placed on their strengths. For completeness, results from the separately published low-frequency search 20-475 Hz are included as well. Our lowest upper limit on worst-case (linearly polarized) strain amplitude h0 is ∼4×10-25 near 170 Hz, while at the high end of our frequency range, we achieve a worst-case upper limit of 1.3×10-24. For a circularly polarized source (most favorable orientation), the smallest upper limit obtained is ∼1.5×10-25. © 2018 American Physical Society.

Published
2018

50. Parameter Estimation on Gravitational Waves from Neutron-Star Binaries With Spinning Components

Author

MIT Kavli Institute for Astrophysics and Space Research, Vitale, Salvatore, Farr, Ben, Berry, Christopher P. L., Farr, Will M., Haster, Carl-Johan, Middleton, Hannah, Cannon, Kipp, Graff, Philip B., Hanna, Chad, Mandel, Ilya, Pankow, Chris, Price, Larry R., Sidery, Trevor, Singer, Leo P., Urban, Alex L., Vecchio, Alberto, Veitch, John, MIT Kavli Institute for Astrophysics and Space Research, Vitale, Salvatore, Farr, Ben, Berry, Christopher P. L., Farr, Will M., Haster, Carl-Johan, Middleton, Hannah, Cannon, Kipp, Graff, Philip B., Hanna, Chad, Mandel, Ilya, Pankow, Chris, Price, Larry R., Sidery, Trevor, Singer, Leo P., Urban, Alex L., Vecchio, Alberto, and Veitch, John

Abstract

Inspiraling binary neutron stars (BNSs) are expected to be one of the most significant sources of gravitational-wave signals for the new generation of advanced ground-based detectors. We investigate how well we could hope to measure properties of these binaries using the Advanced LIGO detectors, which began operation in September 2015. We study an astrophysically motivated population of sources (binary components with masses $1.2 M☉-1.6 M☉ and spins of less than 0.05) using the full LIGO analysis pipeline. While this simulated population covers the observed range of potential BNS sources, we do not exclude the possibility of sources with parameters outside these ranges; given the existing uncertainty in distributions of mass and spin, it is critical that analyses account for the full range of possible mass and spin configurations. We find that conservative prior assumptions on neutron-star mass and spin lead to average fractional uncertainties in component masses of ~16%, with little constraint on spins (the median 90% upper limit on the spin of the more massive component is ~0.7). Stronger prior constraints on neutron-star spins can further constrain mass estimates but only marginally. However, we find that the sky position and luminosity distance for these sources are not influenced by the inclusion of spin; therefore, if LIGO detects a low-spin population of BNS sources, less computationally expensive results calculated neglecting spin will be sufficient for guiding electromagnetic follow-up., Science and Technology Facilities Council (Great Britain), National Science Foundation (U.S.), Laser Interferometer Gravitational Wave Observatory

Published
2016

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