DOCSLIB.ORG

Physics of Gravitational Waves

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Physics of Gravitational Waves Physics of Gravitational Waves Valeria Ferrari SAPIENZA UNIVERSITÀ DI ROMA Invisibles17 Workshop Zürich 12-16 June 2017 1 September 15th, 2015: first Gravitational Waves detection first detection:GW150914 +3.7 m1 = 29.1 4.4 M − +5.2 +0.14 m2 = 36.2 3.8 M a1,a2 = 0.06 0.14 − − − +3.7 M = 62.3 3.1 M − final BH +0.05 a = J/M =0.68 0.06 − +150 +0.03 DL = 420 180Mpc z =0.09 0.04 − − 2 SNR=23.7 radiated EGW= 3M¤c week ending PRL 116, 241103 (2016) PHYSICAL REVIEW LETTERS 17 JUNE 2016 second detection:GW151226 +2.3 m1 =7.5 2.3 M − +8.3 +0.20 m2 = 14.2 3.7 M a1,a2 =0.21 0.10 − − +6.1 M = 20.8 1.7 M FIG. 1. The gravitational-wave event GW150914 observed by the LIGO Hanford (H1, left column panels) and Livingston (L1, − right column panels) detectors. Times are shown relative to September 14, 2015 at 09:50:45 UTC. For visualization, all time series +0.06 final BH are filtered with a 35–350 Hz band-pass filter to suppress large fluctuations outside the detectors’ most sensitive frequencya band,= andJ/M =0.74 0.06 band-reject filters to remove the strong instrumental spectral lines seen in the Fig. 3 spectra. Top row, left: H1 strain. Top row, right: L1 − +0.5 +180 +0.03 strain. GW150914 arrived first at L1 and 6.9 0.4 ms later at H1; for a visual comparison the H1 data are also shown, shifted in time − DL = 440 190Mpc z =0.09 0.04 by this amount and inverted (to account for the detectors’ relative orientations). Second row: Gravitational-wave strain projected onto − − each detector in the 35–350 Hz band. Solid lines show a numerical relativity waveform for a system with parameters consistent with those recovered from GW150914 [34, 35] confirmed by an independent calculation based on [11]. Shaded areas show 90% credible regions for two waveform reconstructions: one that models the signal as a set of sine-Gaussian wavelets [36, 37] and one that models 2 the signal using binary-black-hole template waveforms [38]. These reconstructions have a 95 % overlap, as shown in [38].SNR=13.0Third radiated EGW= 1M¤c row: Residuals after subtracting the filtered numerical relativity waveform from the filtered detector time series. Bottom row: A time- frequency decompositionfor both detections the significance is > 5 σ [39] of the signal power associated with GW150914. Both plots show a signal with frequency increasing over time. 2 planation for this evolution is the inspiral of two orbiting where f and f˙ are the observed frequency and its time masses, m1 and m2, due to gravitational-wave emission. derivative and G and c are the gravitational constant and At the lower frequencies, such evolution is characterized speed of light. Estimating f and f˙ from the data in Fig. 1 by the chirp mass [44] we obtain a chirp mass of 30 M , implying that the M '> total mass M = m1 + m2 is 70 M in the detector 3/5 3 3/5 frame. This bounds the sum of the⇠ Schwarzschild radii of (m1m2) c 5 8/3 11/3 FIG. 1. GW151226= observed= by the LIGO⇡− Hanfordf − (leftf˙ column), and Livingston (right column) detectors,2 > where times are relative to M (m + m )1/5 G 96 the binary components to 2GM/c 210 km. To reach December 26, 20151 at 03:38:53.6482 UTC. First row: Strain data from the two detectors, where the data⇠ are filtered with a 30–600-Hz bandpass filter to suppress large fluctuations outside this range and band-reject filters to remove strong instrumental spectral lines [46]. Also shown (black) is the best-match template from a nonprecessing7 spin waveform model reconstructed using a Bayesian analysis [21] with the same filtering applied. As a result, modulations in the waveform are present due to this conditioning and not due to precession effects. The thickness of the line indicates the 90% credible region. See Fig. 5 for a reconstruction of the best-match template with no filtering applied. Second row: The accumulated peak signal-to-noise ratio (SNRp) as a function of time when integrating from the start of the best-match template, corresponding to a gravitational-wave frequency of 30 Hz, up to its merger time. The total accumulated SNRp corresponds to the peak in the next row. Third row: Signal-to-noise ratio (SNR) time series produced by time shifting the best-match template waveform and computing the integrated SNR at each point in time. The peak of the SNR time series gives the merger time of the best-match template for which the highest overlap with the data is achieved. The single-detector SNRs in LIGO Hanford and Livingston are 10.5 and 7.9, respectively, primarily because of the detectors’ differing sensitivities. Fourth row: Time-frequency representation [47] of the strain data around the time of GW151226. In contrast to GW150914 [4], the signal is not easily visible. from 35 Hz to a peak amplitude at 450 Hz. The signal-to- Hanford and Livingston, respectively. The time-frequency noise ratio (SNR) accumulates equally in the early inspiral representation of the detector data shows that the signal is not (∼45 cycles from 35 to 100 Hz) and late inspiral to merger easily visible. The signal is more apparent in LIGO Hanford (∼10 cycles from 100 to 450 Hz). This is different from the where the SNR is larger. The SNR difference is predomi- more massive GW150914 binary for which only the last 10 nantly due to the different sensitivities of the detectors at the cycles, comprising inspiral and merger, dominated the time. Only with the accumulated SNR from matched filtering SNR. As a consequence, the parameters characterizing does the signal become apparent in both detectors. GW151226 have different precision than those of GW150914. The chirp mass [26,45], which controls the III. DETECTORS binary’s evolution during the early inspiral, is determined very precisely. The individual masses, which rely on The LIGO detectors measure gravitational-wave strain information from the late inspiral and merger, are measured using two modified Michelson interferometers located in far less precisely. Hanford, WA and Livingston, LA [2,3,46]. The two Figure 1 illustrates that the amplitude of the signal is less orthogonal arms of each interferometer are 4 km in length, than the level of the detector noise, where the maximum strain each with an optical cavity formed by two mirrors acting as 0.7 −22 0.8 −22 of the signal is 3.4−þ0.9 × 10 and 3.4−þ0.9 × 10 in LIGO test masses. A passing gravitational wave alters the 241103-2 week ending PRL 118, 221101 (2017) PHYSICAL REVIEW LETTERS 2 JUNE 2017 5 calibration uncertainties for strain data in both detectors for the times used in this analysis are better than 5% in third candidate: LVT151012 2σ 3σ 4σ 5σ > 5σ 2σ3σ 4σ 5σ > 5σ amplitude and 3° in phase over the frequency range 20– 2σ 3σ 4σ 5σ > 5σ +4 104 104 2σ 3σ 4σ 5σ > 5σ m1 = 13 5 M 1024 Hz. − 3 Search Result 3 Search Result +18 +0.3 10 At the time of GW170104, both LIGO detectors were 10 m2 = 23 6 M a1,a2 =0.0 0.2 2 Search Background Background including all search results − − 10 102 +14 operating with sensitivityBackground excluding typical of GW150914 the observing run to Background excluding only GW150914 M = 35 4 M 101 1 − date and were in an observation-ready state. Investigations 10 +0.09 0 0 a = J/M =0.66 0.10 10 10 − similar to the detection validation procedures for previous +0.5 +0.09 10 1 10 1 DL =1 0.5Gpc z =0.20 0.09 events− [2,14] found no evidence that instrumental or − − − 2 LV T 1 5 1 0 1 2 2 10− 10 environmental disturbances contributed to GW170104.GW150914 − GW150914 10 3 3 the significance is ≤ 2 σ − 10− 10 4 10 4 − III. SEARCHES − 5 5 Number of events 10 Number of events − 10− 10 6 GW170104 was first identified by inspection of low- 6 − 10− 10latency7 triggers from Livingston data [15 17]. An auto- 7 − – 10− 10mated8 notification was not generated as the Hanford 8 Third detection :GW170104 − 10− detector8 10’s calibration12 14 state16 was18 temporarily20 22 set incorrectly24 10 20 30 40 50 60 70 80 90 Detection statistic ρˆc Detection statistic ln in the low-latency system. After it was manually deter- L mined that the calibration2σ 3σ 4 ofσ both5σ detectors> was5σ in a 2σ 3σ 4σ 5σ 4 2σ 3σ 4σ 5σ > 5σ 2σ 3σ 4σ 5σ 10nominal state,+5 an.3 alert with anSNR= initial 13 source localization 104 m1 = 19.4 5.9 M 10[18,19]3 was distributed− toSearch collaborating Result astronomers [20] 103 Search Result m = 31.2+8.4 M Background excluding GW150914 Background excluding only GW150914 10for2 the2 purpose6 of.0 searching for a transient counterpart. 102 − Background excluding Background excluding 1 2 1 10About 30 groups of observersGW150914radiated covered and GW151226 E theGW parts = 2 M of☉ the c sky 10 GW150914 and GW151226 10localization0 using+5.7 ground- and space-based instruments, 100 M = 48.7 4.6 M 10spanning1 from−γ ray to radio frequencies as well as high-10 1 − a = J/M =0.64+0.09 − 2 0.20 2 10energy− neutrinos [21]−. 10 +450 +0GW151226.08 − GW151226 10 3 OfflineDL = analyses 880 390Mpc are used to z determine=0.18 0.07 the significance of 3 − − − 10− 10 4 4 candidate− events.
Load more

Recommended publications
  • Probing the Nuclear Equation of State from the Existence of a 2.6 M Neutron Star: the GW190814 Puzzle
    S S symmetry Article Probing the Nuclear Equation of State from the Existence of a ∼2.6 M Neutron Star: The GW190814 Puzzle Alkiviadis Kanakis-Pegios †,‡ , Polychronis S. Koliogiannis ∗,†,‡ and Charalampos C. Moustakidis †,‡ Department of Theoretical Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece; [email protected] (A.K.P.); [email protected] (C.C.M.) * Correspondence: [email protected] † Current address: Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece. ‡ These authors contributed equally to this work. Abstract: On 14 August 2019, the LIGO/Virgo collaboration observed a compact object with mass +0.08 2.59 0.09 M , as a component of a system where the main companion was a black hole with mass ∼ − 23 M . A scientific debate initiated concerning the identification of the low mass component, as ∼ it falls into the neutron star–black hole mass gap. The understanding of the nature of GW190814 event will offer rich information concerning open issues, the speed of sound and the possible phase transition into other degrees of freedom. In the present work, we made an effort to probe the nuclear equation of state along with the GW190814 event. Firstly, we examine possible constraints on the nuclear equation of state inferred from the consideration that the low mass companion is a slow or rapidly rotating neutron star. In this case, the role of the upper bounds on the speed of sound is revealed, in connection with the dense nuclear matter properties. Secondly, we systematically study the tidal deformability of a possible high mass candidate existing as an individual star or as a component one in a binary neutron star system.
    [Show full text]
  • Recent Observations of Gravitational Waves by LIGO and Virgo Detectors
    universe Review Recent Observations of Gravitational Waves by LIGO and Virgo Detectors Andrzej Królak 1,2,* and Paritosh Verma 2 1 Institute of Mathematics, Polish Academy of Sciences, 00-656 Warsaw, Poland 2 National Centre for Nuclear Research, 05-400 Otwock, Poland; [email protected] * Correspondence: [email protected] Abstract: In this paper we present the most recent observations of gravitational waves (GWs) by LIGO and Virgo detectors. We also discuss contributions of the recent Nobel prize winner, Sir Roger Penrose to understanding gravitational radiation and black holes (BHs). We make a short introduction to GW phenomenon in general relativity (GR) and we present main sources of detectable GW signals. We describe the laser interferometric detectors that made the first observations of GWs. We briefly discuss the first direct detection of GW signal that originated from a merger of two BHs and the first detection of GW signal form merger of two neutron stars (NSs). Finally we present in more detail the observations of GW signals made during the first half of the most recent observing run of the LIGO and Virgo projects. Finally we present prospects for future GW observations. Keywords: gravitational waves; black holes; neutron stars; laser interferometers 1. Introduction The first terrestrial direct detection of GWs on 14 September 2015, was a milestone Citation: Kro´lak, A.; Verma, P. discovery, and it opened up an entirely new window to explore the universe. The combined Recent Observations of Gravitational effort of various scientists and engineers worldwide working on the theoretical, experi- Waves by LIGO and Virgo Detectors.
    [Show full text]
  • LIGO Magazine, Issue 7, 9/2015
    LIGO Scientific Collaboration Scientific LIGO issue 7 9/2015 LIGO MAGAZINE Looking for the Afterglow The Dedication of the Advanced LIGO Detectors LIGO Hanford, May 19, 2015 p. 13 The Einstein@Home Project Searching for continuous gravitational wave signals p. 18 ... and an interview with Joseph Hooton Taylor, Jr. ! The cover image shows an artist’s illustration of Supernova 1987A (Credit: ALMA (ESO/NAOJ/NRAO)/Alexandra Angelich (NRAO/AUI/NSF)) placed above a photograph of the James Clark Maxwell Telescope (JMCT) (Credit: Matthew Smith) at night. The supernova image is based on real data and reveals the cold, inner regions of the exploded star’s remnants (in red) where tremendous amounts of dust were detected and imaged by ALMA. This inner region is contrasted with the outer shell (lacy white and blue circles), where the blast wave from the supernova is colliding with the envelope of gas ejected from the star prior to its powerful detonation. Image credits Photos and graphics appear courtesy of Caltech/MIT LIGO Laboratory and LIGO Scientific Collaboration unless otherwise noted. p. 2 Comic strip by Nutsinee Kijbunchoo p. 5 Figure by Sean Leavey pp. 8–9 Photos courtesy of Matthew Smith p. 11 Figure from L. P. Singer et al. 2014 ApJ 795 105 p. 12 Figure from B. D. Metzger and E. Berger 2012 ApJ 746 48 p. 13 Photo credit: kimfetrow Photography, Richland, WA p. 14 Authors’ image credit: Joeri Borst / Radboud University pp. 14–15 Image courtesy of Paul Groot / BlackGEM p. 16 Top: Figure by Stephan Rosswog. Bottom: Diagram by Shaon Ghosh p.
    [Show full text]
  • Gravitational Waves
    Gravitational Waves Intuition In Newtonian gravity, you can have instantaneous action at a distance. If I suddenly • replace the Sun with a 10, 000M! black hole, the Earth’s orbit should instantly repsond in accordance with Kepler’s Third Law. But special relativity forbids this! The idea that gravitational information can propagate is a consequence of special relativity: nothing• can travel faster than the ultimate speed limit, c. Imagine observing a distant binary star and trying to measure the gravitational field at your• location. It is the sum of the field from the two individual components of the binary, located at distances r1 and r2 from you. As the binary evolves in its orbit, the masses change their position withrespecttoyou, and• so the gravitational field must change. It takes time for that information to propagate from the binary to you — tpropagate = d/c,whered is the luminosity distance to the binary. The propagating effect of that information is known as gravitational radiation, which you should• think of in analogy with the perhaps more familiar electromagnetic radiation Far from a source (like the aforementioned binary) we see the gravitational radiation field oscillating• and these propagating oscillating disturbances are called gravitational waves. Like electromagnetic waves • ! Gravitational waves are characterized by a wavelength λ and a frequency f ! Gravitational waves travel at the speed of light, where c = λ f · ! Gravitational waves come in two polarization states (called + [plus]and [cross]) × The Metric and the Wave Equation There is a long chain of reasoning that leads to the notion of gravitational waves. It • begins with the linearization of the field equations, demonstration of gauge transformations in the linearized regime, and the writing of a wave equation for small deviations from the background spacetime.
    [Show full text]
  • 1 Introduction 2 Gravitational Wave Sources
    GRAVITATIONAL WAVES FROM A COSMOLOGICAL DISTRIBUTION OF SOURCES Sidharth Kumar Abstract The advent of gravitational wave detectors such as the Laser Interferometer Space Antenna and the Advanced-Laser Interferometer Gravitational wave Observatory will make it possible to observe many gravitational wave emission phenomena that may or may not have electromagnetic counterparts. In many cases, gravitational waves serve as probes of length and time scales that rangemany orders of magnitudeas compared to electromagnetic waves. Sources of gravitational waves can be classified into non-primordial and primordial. Non-primordial sources include binary compact object inspirals, core-collapse super- novae and Neutron stars. Primordial sources include cosmological defects, phase transitions in the early universe, and inflation. In this paper we briefly outline the signatures of gravitational waves from different types of sources. We also provide a simple theorem to calculate the gravitational wave background due to a cosmological distribution of these sources. We determine that the background is cosmology indepen- dent and is a function of the cosmological distribution, the total time integrated energy spectrum of an individual source and the present-day comoving number density of remnants. 1 Introduction Gravitational waves are produced wherever the quadrupolar moment of a mass distribution has a non-vanishingsecond derivative in time. Because of this simple requirement, these waves would be produced abundantly in the universe. However, being a quadrupolar field, it is extremely weak. Therefore, regular astronomical sources, such as stars or galaxies would radiate negligibly in gravitational waves. More likely sources include compact object inspirals, core-collapse supernovae, cosmological defects, non-axisymmetric Neutron stars, and inflation itself! Gravitational wave observations will give us a whole new perspective on the universe.
    [Show full text]
  • Properties of the Binary Neutron Star Merger GW170817
    PHYSICAL REVIEW X 9, 011001 (2019) Properties of the Binary Neutron Star Merger GW170817 B. P. Abbott et al.* (LIGO Scientific Collaboration and Virgo Collaboration) (Received 6 June 2018; revised manuscript received 20 September 2018; published 2 January 2019) On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary’s properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg2. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 M⊙ when allowing for large component spins, and to lie between 1.16 1 60 2 73þ0.04 and . M⊙ (with a total mass . −0.01 M⊙) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large component spins, we constrain the dimensionless spins of the components to be less than 0.50 for the primary and 0.61 for the secondary.
    [Show full text]
  • Arxiv:2010.12558V2 [Astro-Ph.HE] 3 Nov 2020
    Draft version November 4, 2020 Typeset using LATEX twocolumn style in AASTeX63 GW190521 may be an intermediate mass ratio inspiral Alexander H. Nitz1, 2 and Collin D. Capano1, 2 1Max-Planck-Institut f¨urGravitationsphysik (Albert-Einstein-Institut), D-30167 Hannover, Germany 2Leibniz Universit¨atHannover, D-30167 Hannover, Germany ABSTRACT GW190521 is the first confident observation of a binary black hole merger with total mass M > 100 M . Given the lack of observational constraints at these masses, we analyze GW190521 considering two different priors for the binary's masses: uniform in mass ratio and source-frame total mass, and uniform in source-frame component masses. For the uniform in mass-ratio prior, we find that the src +15 src +33 component masses are m1 = 168−61 M and m2 = 16−3 M . The uniform in component-mass src prior yields a bimodal posterior distribution. There is a low-mass-ratio mode (q < 4) with m1 = +17 src +17 src +16 100−18 M and m2 = 57−16 M and a high-mass-ratio mode (q ≥ 4) with m1 = 166−35 M and src +14 m2 = 16−3 M . Although the two modes have nearly equal posterior probability, the maximum- src src likelihood parameters are in the high-mass ratio mode, with m1 = 171 M and m2 = 16 M , and a signal-to-noise ratio of 16. These results are consistent with the proposed \mass gap" produced by pair-instability in supernova. Our results are inconsistent with those published in Abbott et al. (2020b). We find that a combination of the prior used and the constraints applied may have prevented that analysis from sampling the high-mass-ratio mode.
    [Show full text]
  • Gravitational Waves in the Post-Detection Era
    GRAVITATIONAL WAVES IN THE POST-DETECTION ERA: CHARACTERISING BINARY BLACK HOLE SIGNALS AND POPULATIONS by Sebastian Michael Gaebel A thesis submitted to the University of Birmingham for the degree of Doctor of Philosophy School of Physics and Astronomy and Institute for Gravitational Wave Astronomy College of Engineering and Physical Sciences University of Birmingham September 2019 University of Birmingham Research Archive e-theses repository This unpublished thesis/dissertation is copyright of the author and/or third parties. The intellectual property rights of the author or third parties in respect of this work are as defined by The Copyright Designs and Patents Act 1988 or as modified by any successor legislation. Any use made of information contained in this thesis/dissertation must be in accordance with that legislation and must be properly acknowledged. Further distribution or reproduction in any format is prohibited without the permission of the copyright holder. 2 Abstract The detection of GW150914 has marked the start of the era of gravitational wave (GW) astronomy, and the number of detections available for astro- physical interpretation has been growing ever since. Similarly, this thesis progresses from considering individual signals to analysing the population of gravitational wave sources. We explore how much we expect to be able to learn from a loud binary black hole merger like GW150914, were it to appear in the detector net- works we currently have, as well as those which are being planned or under construction. Afterwards, we develop a model which allows us to obtain un- biased estimates of the rate with which the universe produces such signals, and the distribution of intrinsic gravitational wave source parameters such as the component masses, despite the fact that the observed distribution is inherently biased by the fact that source parameters affect the loudness of the emitted signal, and contaminated by terrestrial noise artefacts inherent to the detectors.
    [Show full text]
  • GW170814: Gravitational Wave Polarization Analysis
    GW170814: Gravitational wave polarization analysis Robert C Hilborn American Association of Physics Teachers, One Physics Ellipse, College Park, MD 20740, United States of America Email: [email protected] Received Accepted for publication Published Abstract To determine the polarization character of gravitational waves, we use strain data from the GW170814 binary black hole coalescence event detected by the three LIGO-Virgo observatories, extracting the gravitational wave strain signal amplitude ratios directly from those data. Employing a geometric approach that links those ratios to the gravitational wave polarization properties, we find that there is a range of source sky locations, partially overlapping the LIGI-Virgo 90% credible range of GW170814 source locations, for which vector polarization is consistent with the observed amplitude ratios. A Bayesian inference analysis indicates that the GW170814 data cannot rule out vector polarization for gravitational waves. Confirmation of a vector polarization component of gravitational waves would be a sign of post- general relativity physics. Keywords: gravitational wave polarization, tests of general relativity 1 1. Introduction The observation of the binary black hole gravitational wave (GW) event GW170814 by the three LIGO-Virgo observatories [1] allows for a test of the polarization modes of GWs, something not possible with the previous GW observations involving just the two LIGO observatories [2]. General relativity (GR) predicts that GWs will exhibit only tensor polarization modes [1,3-6], an aspect of GR that has not been directly tested before. Any detection of non-tensorial polarization (that is, vector or scalar polarization modes) will be a signal of post-GR physics [7,8].
    [Show full text]
  • Arxiv:1805.11579V1 [Gr-Qc]
    Properties of the binary neutron star merger GW170817 The LIGO Scientific Collaboration and The Virgo Collaboration (Compiled 30 May 2018) On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved model- ing, and re-calibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as com- pared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of 16 deg2. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for non-zero component spins. The component masses are inferred to lie between 1:00 and 1:89 M when allowing for large component spins, and to lie between 1:16 +0:04 and 1:60 M (with a total mass 2:73−0:01 M ) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Using a precessing model and allowing for large com- ponent spins, we constrain the dimensionless spins of the components to be less than 0:50 for the primary and 0:61 for the secondary.
    [Show full text]
  • Arxiv:2009.07626V2 [Astro-Ph.HE] 25 Sep 2020 Kavli Institute for Astronomy and Astrophysics at Peking University, Yi He Yuan Lu 5, Beijing 100871, P
    Distortion of Gravitational-wave Signals by Astrophysical Environments Xian Chen ∗ Abstract Many objects discovered by LIGO and Virgo are peculiar because they fall in a mass range which in the past was considered unpopulated by compact objects. Given the significance of the astrophysical implications, it is important to first under- stand how their masses are measured from gravitational-wave signals. How accurate is the measurement? Are there elements missing in our current model which may result in a bias? This chapter is dedicated to these questions. In particular, we will highlight several astrophysical factors which are not included in the standard model of GW sources but could result in a significant bias in the estimation of the mass. These factors include strong gravitational lensing, a relative motion of the source, a nearby massive object, and a gaseous background. Keywords Gravitational waves, Chirp mass, Redshift, Acceleration, Hydrodynamical friction. Introduction The detection of gravitational waves (GWs) by LIGO and Virgo has reshaped our understanding of stellar-mass black holes (BHs). Before the detection, stellar-mass BHs were exclusively found in X-ray binaries. Their masses fall in a range of about Xian Chen Astronomy Department, Peking University, Yi He Yuan Lu 5, Beijing 100871, P. R. China, arXiv:2009.07626v2 [astro-ph.HE] 25 Sep 2020 Kavli Institute for Astronomy and Astrophysics at Peking University, Yi He Yuan Lu 5, Beijing 100871, P. R. China e-mail: [email protected] ∗ corresponding author 1 2 Xian Chen 5 20M . Below or above this range, no (stellar-mass) BH was detected. There were− also speculations based on theoretical grounds that stellar evolution can hardly produce a BH between 3 and 5M (known as the “lower mass gap”) or between 50 and 120M (the “upper mass∼ gap”).
    [Show full text]
  • Insights Into Binary Evolution from Gravitational Waves
    Insights into binary evolution from gravitational waves Simon Stevenson [email protected] @simon4nine For the COMPAS team Alejandro Vigna-Gomez, Jim Barrett, Coen Nijssell, Christopher Berry, Ilya Mandel and more GW150914 LVC 2016 arXiv:1602.03840 KITP, UCSB 14/3/2017 GW151226 LVC 2016 arXiv:1606.04855 KITP, UCSB 14/3/2017 Masses Stevenson+ 2015, Stevenson+ 2017 (in press), Mandel+ 2017 KITP, UCSB 14/3/2017 Measured masses ¤ Combination of component masses: ¤ Chirp mass for low mass events ¤ Total mass for high mass events LVC 2016 arXiv:1606.04856 KITP, UCSB 14/3/2017 BBH (total) mass distribution ¤ Assumes our Fiducial model values of hyperparameters, integrated across cosmic history ¤ Data from Stevenson+ 2017 in press ¤ Evolution of BBH merger rate over cosmic history studied in Neijssel+ 2017 in prep KITP, UCSB 14/3/2017 Progenitors of O1 events (maybe) Stevenson et al 2017 in press KITP, UCSB 14/3/2017 Typical evolutionary channel for GW151226 Time M1 ST1 ST2 M2 a [Myr] [M ] [M ] [R ] − − 0.0 63.6 MS MS 27.8 729.93 4.1 60.4 HG MS 27.7 757.5 4.12 24.6 HeMS MS 30.6 622.07 4.49 19.1 BH MS 30.6 692.7 7.21 19.1 BH CHeB 30.3 697.48 7.42 19.1 BH CHeB 29.7 706.33 7.42 19.1 BH HeMS 10.6 5.18 7.88 19.1 BH BH 5.7 8.82 Stevenson et al 2017 in press KITP, UCSB 14/3/2017 1 Uncertainties in binary evolution ¤ Initial conditions (Recent progress e.g.
    [Show full text]