Publications (660)1074.98 Total impact
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ABSTRACT: We describe directed searches for continuous gravitational waves in data from the sixth LIGO science data run. The targets were nine young supernova remnants not associated with pulsars; eight of the remnants are associated with nonpulsing suspected neutron stars. One target's parameters are uncertain enough to warrant two searches, for a total of ten. Each search covered a broad band of frequencies and first and second frequency derivatives for a fixed sky direction. The searches coherently integrated data from the two LIGO interferometers over time spans from 5.325.3 days using the matchedfiltering Fstatistic. We found no credible gravitationalwave signals. We set 95% confidence upper limits as strong (low) as $4\times10^{25}$ on intrinsic strain, $2\times10^{7}$ on fiducial ellipticity, and $4\times10^{5}$ on rmode amplitude. These beat the indirect limits from energy conservation and are within the range of theoretical predictions for neutronstar ellipticities and rmode amplitudes.12/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We present results of a search for continuouslyemitted gravitational radiation, directed at the brightest lowmass Xray binary, Scorpius X1. Our semicoherent analysis covers 10 days of LIGO S5 data ranging from 50550 Hz, and performs an incoherent sum of coherent $\mathcal{F}$statistic power distributed amongst frequencymodulated orbital sidebands. All candidates not removed at the veto stage were found to be consistent with noise at a 1% false alarm rate. We present Bayesian 95% confidence upper limits on gravitationalwave strain amplitude using two different prior distributions: a standard one, with no a priori assumptions about the orientation of Scorpius X1; and an anglerestricted one, using a prior derived from electromagnetic observations. Median strain upper limits of 1.3e24 and 8e25 are reported at 150 Hz for the standard and anglerestricted searches respectively. This proof of principle analysis was limited to a short observation time by unknown effects of accretion on the intrinsic spin frequency of the neutron star, but improves upon previous upper limits by factors of ~1.4 for the standard, and 2.3 for the anglerestricted search at the sensitive region of the detector.12/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We report the results of a multimessenger search for coincident signals from the LIGO and Virgo gravitationalwave observatories and the partially completed IceCube highenergy neutrino detector, including periods of joint operation between 20072010. These include parts of the 20052007 run and the 20092010 run for LIGOVirgo, and IceCube's observation periods with 22, 59 and 79 strings. We find no significant coincident events, and use the search results to derive upper limits on the rate of joint sources for a range of source emission parameters. For the optimistic assumption of gravitationalwave emission energy of $10^{2}$ M$_\odot$c$^2$ at $\sim 150$ Hz with $\sim 60$ ms duration, and highenergy neutrino emission of $10^{51}$ erg comparable to the isotropic gammaray energy of gammaray bursts, we limit the source rate below $1.6 \times 10^{2}$ Mpc$^{3}$yr$^{1}$. We also examine how combining information from gravitational waves and neutrinos will aid discovery in the advanced gravitationalwave detector era.Physical Review D 11/2014; 90:102002. · 4.86 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: In this paper we present the results of a coherent narrowband search for continuous gravitationalwave signals from the Crab and Vela pulsars conducted on Virgo VSR4 data. In order to take into account a possible small mismatch between the gravitational wave frequency and two times the star rotation frequency, inferred from measurement of the electromagnetic pulse rate, a range of 0.02 Hz around two times the star rotational frequency has been searched for both the pulsars. No evidence for a signal has been found and 95$\%$ confidence level upper limits have been computed both assuming polarization parameters are completely unknown and that they are known with some uncertainty, as derived from Xray observations of the pulsar wind torii. For Vela the upper limits are comparable to the spindown limit, computed assuming that all the observed spindown is due to the emission of gravitational waves. For Crab the upper limits are about a factor of two below the spindown limit, and represent a significant improvement with respect to past analysis. This is the first time the spindown limit is significantly overcome in a narrowband search.10/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We present the results of a search for gravitational waves associated with 223 gammaray bursts (GRBs) detected by the InterPlanetary Network (IPN) in 20052010 during LIGO's fifth and sixth science runs and Virgo's first, second and third science runs. The IPN satellites provide accurate times of the bursts and sky localizations that vary significantly from degree scale to hundreds of square degrees. We search for both a wellmodeled binary coalescence signal, the favored progenitor model for short GRBs, and for generic, unmodeled gravitational wave bursts. Both searches use the event time and sky localization to improve the gravitationalwave search sensitivity as compared to corresponding alltime, allsky searches. We find no evidence of a gravitationalwave signal associated with any of the IPN GRBs in the sample, nor do we find evidence for a population of weak gravitationalwave signals associated with the GRBs. For all IPNdetected GRBs, for which a sufficient duration of quality gravitationalwave data is available, we place lower bounds on the distance to the source in accordance with an optimistic assumption of gravitationalwave emission energy of $10^{2}M_{\odot}c^2$ at 150 Hz, and find a median of 13 Mpc. For the 27 shorthard GRBs we place 90% confidence exclusion distances to two source models: a binary neutron star coalescence, with a median distance of 12Mpc, or the coalescence of a neutron star and black hole, with a median distance of 22 Mpc. Finally, we combine this search with previously published results to provide a population statement for GRB searches in firstgeneration LIGO and Virgo gravitationalwave detectors, and a resulting examination of prospects for the advanced gravitationalwave detectors.Physical Review Letters 06/2014; 113(1):011102. · 7.73 Impact Factor  [Show abstract] [Hide abstract]
ABSTRACT: Gravitational waves from a variety of sources are predicted to superpose to create a stochastic background. This background is expected to contain unique information from throughout the history of the universe that is unavailable through standard electromagnetic observations, making its study of fundamental importance to understanding the evolution of the universe. We carry out a search for the stochastic background with the latest data from LIGO and Virgo. Consistent with predictions from most stochastic gravitationalwave background models, the data display no evidence of a stochastic gravitationalwave signal. Assuming a gravitationalwave spectrum of Omega_GW(f)=Omega_alpha*(f/f_ref)^alpha, we place 95% confidence level upper limits on the energy density of the background in each of four frequency bands spanning 41.51726 Hz. In the frequency band of 41.5169.25 Hz for a spectral index of alpha=0, we constrain the energy density of the stochastic background to be Omega_GW(f)<5.6x10^6. For the 6001000 Hz band, Omega_GW(f)<0.14*(f/900 Hz)^3, a factor of 2.5 lower than the best previously reported upper limits. We find Omega_GW(f)<1.8x10^4 using a spectral index of zero for 170600 Hz and Omega_GW(f)<1.0*(f/1300 Hz)^3 for 10001726 Hz, bands in which no previous direct limits have been placed. The limits in these four bands are the lowest direct measurements to date on the stochastic background. We discuss the implications of these results in light of the recent claim by the BICEP2 experiment of the detection of inflationary gravitational waves.06/2014; 

Article: First allsky search for continuous gravitational waves from unknown sources in binary systems
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ABSTRACT: We present the first results of an allsky search for continuous gravitational waves from unknown spinning neutron stars in binary systems using LIGO and Virgo data. Using a specially developed analysis program, the TwoSpect algorithm, the search was carried out on data from the sixth LIGO Science Run and the second and third Virgo Science Runs. The search covers a range of frequencies from 20 Hz to 520 Hz, a range of orbital periods from 2 to ~2,254 h and a frequency and perioddependent range of frequency modulation depths from 0.277 to 100 mHz. This corresponds to a range of projected semimajor axes of the orbit from ~0.6e3 ls to ~6,500 ls assuming the orbit of the binary is circular. While no plausible candidate gravitational wave events survive the pipeline, upper limits are set on the analyzed data. The most sensitive 95% confidence upper limit obtained on gravitational wave strain is 2.3e24 at 217 Hz, assuming the source waves are circularly polarized. Although this search has been optimized for circular binary orbits, the upper limits obtained remain valid for orbital eccentricities as large as 0.9. In addition, upper limits are placed on continuous gravitational wave emission from the lowmass xray binary Scorpius X1 between 20 Hz and 57.25 Hz.05/2014;  [Show abstract] [Hide abstract]
ABSTRACT: In this paper we report on a search for shortduration gravitational wave bursts in the frequency range 64 Hz1792 Hz associated with gammaray bursts (GRBs), using data from GEO600 and one of the LIGO or Virgo detectors. We introduce the method of a linear search grid to analyse GRB events with large sky localisation uncertainties such as the localisations provided by the Fermi Gammaray Burst Monitor (GBM). Coherent searches for gravitational waves (GWs) can be computationally intensive when the GRB sky position is not welllocalised, due to the corrections required for the difference in arrival time between detectors. Using a linear search grid we are able to reduce the computational cost of the analysis by a factor of O(10) for GBM events. Furthermore, we demonstrate that our analysis pipeline can improve upon the sky localisation of GRBs detected by the GBM, if a highfrequency GW signal is observed in coincidence. We use the linear search grid method in a search for GWs associated with 129 GRBs observed satellitebased gammaray experiments between 2006 and 2011. The GRBs in our sample had not been previously analysed for GW counterparts. A fraction of our GRB events are analysed using data from GEO600 while the detector was using squeezedlight states to improve its sensitivity; this is the first search for GWs using data from a squeezedlight interferometric observatory. We find no evidence for GW signals, either with any individual GRB in this sample or with the population as a whole. For each GRB we place lower bounds on the distance to the progenitor, assuming a fixed GW emission energy of $10^{2} M_{\odot}c^{2}$, with a median exclusion distance of 0.8 Mpc for emission at 500 Hz and 0.3 Mpc at 1 kHz. The reduced computational cost associated with a linear search grid will enable rapid searches for GWs associated with Fermi GBM events in the Advanced detector era.05/2014;  [Show abstract] [Hide abstract]
ABSTRACT: Chirped quasiphasematching (QPM) gratings offer efficient, ultrabroadband optical parametric chirped pulse amplification (OPCPA) in the midinfrared as well as other spectral regions. Only recently, however, has this potential begun to be realized [1]. In this paper, we study the design of chirped QPMbased OPCPA in detail, revealing several important constraints which must be accounted for in order to obtain broadband, highquality amplification. We determine these constraints in terms of the underlying saturated nonlinear processes, and explain how they were met when designing our midIR OPCPA system. The issues considered include gain and saturation based on the basic threewave mixing equations; suppression of unwanted noncollinear gainguided modes; minimizing and characterizing nonlinear losses associated with random duty cycle errors in the QPM grating; avoiding coincidentallyphasematched nonlinear processes; and controlling the temporal/spectral characteristics of the saturated nonlinear interaction in order to maintain the chirpedpulse structure required for OPCPA. The issues considered place constraints both on the QPM devices as well as the OPCPA system. The resulting experimental guidelines are detailed. Our results represent the first comprehensive discussion of chirped QPM devices operated in strongly nonlinear regimes, and provide a roadmap for advancing and experimentally implementing OPCPA systems based on these devices.Optics Express 04/2014; 22(8):96279658. · 3.53 Impact Factor 
Conference Paper: Concepts and research for future detectors
10th Edoardo Amaldi Conference on Gravitational Waves, Warsaw, Poland; 04/2014 

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ABSTRACT: This paper reports on an unmodeled, allsky search for gravitational waves from merging intermediate mass black hole binaries (IMBHB). The search was performed on data from the second joint science run of the LIGO and Virgo detectors (July 2009  October 2010) and was sensitive to IMBHBs with a range up to $\sim 200$ Mpc, averaged over the possible sky positions and inclinations of the binaries with respect to the line of sight. No significant candidate was found. Upper limits on the coalescencerate density of nonspinning IMBHBs with total masses between 100 and $450 \ \mbox{M}_{\odot}$ and mass ratios between $0.25$ and $1\,$ were placed by combining this analysis with an analogous search performed on data from the first LIGOVirgo joint science run (November 2005  October 2007). The most stringent limit was set for systems consisting of two $88 \ \mbox{M}_{\odot}$ black holes and is equal to $0.12 \ \mbox{Mpc}^{3} \ \mbox{Myr}^{1}$ at the $90\%$ confidence level. This paper also presents the first estimate, for the case of an unmodeled analysis, of the impact on the search range of IMBHB spin configurations: the visible volume for IMBHBs with nonspinning components is roughly doubled for a population of IMBHBs with spins aligned with the binary's orbital angular momentum and uniformly distributed in the dimensionless spin parameter up to 0.8, whereas an analogous population with antialigned spins decreases the visible volume by $\sim 20\%\,$.04/2014;  [Show abstract] [Hide abstract]
ABSTRACT: We report results from a search for gravitational waves produced by perturbed intermediate mass black holes (IMBH) in data collected by LIGO and Virgo between 2005 and 2010. The search was sensitive to astrophysical sources that produced damped sinusoid gravitational wave signals, also known as ringdowns, with frequency $50\le f_{0}/\mathrm{Hz} \le 2000$ and decay timescale $0.0001\lesssim \tau/\mathrm{s} \lesssim 0.1$ characteristic of those produced in mergers of IMBH pairs. No significant gravitational wave candidate was detected. We report upper limits on the astrophysical coalescence rates of IMBHs with total binary mass $50 \le M/\mathrm{M}_\odot \le 450$ and component mass ratios of either 1:1 or 4:1. For systems with total mass $100 \le M/\mathrm{M}_\odot \le 150$, we report a 90%confidence upper limit on the rate of binary IMBH mergers with nonspinning and equal mass components of $6.9\times10^{8}\,$Mpc$^{3}$yr$^{1}$. We also report a rate upper limit for ringdown waveforms from perturbed IMBHs, radiating 1% of their mass as gravitational waves in the fundamental, $\ell=m=2$, oscillation mode, that is nearly three orders of magnitude more stringent than previous results.03/2014; 
Article: A Scanning, AllFiber Sagnac Interferometer for High Resolution MagnetoOptic Measurements at 820 nm
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ABSTRACT: The Sagnac Interferometer has historically been used for detecting nonreciprocal phenomena, such as rotation. We demonstrate an apparatus in which this technique is employed for high resolution measurements of the MagnetoOptical Polar Kerr effecta direct indicator of magnetism. Previous designs have incorporated freespace components which are bulky and difficult to align. We improve upon this technique by using all fiberoptic coupled components and demonstrate operation at a new wavelength, 820 nm, with which we can achieve better than 1 $\mu$rad resolution. Mounting the system on a piezoelectric scanner allows us to acquire diffraction limited images with 1.5 $\mu$m spatial resolution. We also provide extensive discussion on the details and of the Sagnac Interferometer's construction.Review of Scientific Instruments 03/2014; 85(10). · 1.58 Impact Factor 
Conference Paper: Experimental Demonstration of Optical Nyquist Generation of 32Gbaud QPSK using a Combbased Tunable Optical TappedDelayLine FIR Filter
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ABSTRACT: We experimentally demonstrate tunable optical Nyquist generation of 32Gbaud QPSK signals using optical tappeddelay line. Optical Nyquist spectra for different number of taps are shown, and 20% EVM and 2.8 dB OSNR penalty at BER of 1e3 are measured.Optical Fiber Communication Conference; 03/2014  [Show abstract] [Hide abstract]
ABSTRACT: Harnessing nonlinearities strong enough to allow two single photons to interact with one another is not only a fascinating challenge but is central to numerous advanced applications in quantum information science. Currently, all known approaches are extremely challenging although a few have led to experimental realisations with attenuated classical laser light. This has included crossphase modulation with weak classical light in atomic ensembles and optical fibres, converting incident laser light into a nonclassical stream of photon or Rydberg blockades as well as alloptical switches with attenuated classical light in various atomic systems. Here we report the observation of a nonlinear parametric interaction between two true single photons. Single photons are initially generated by heralding one photon from each of two independent spontaneous parametric downconversion sources. The two heralded single photons are subsequently combined in a nonlinear waveguide where they are converted into a single photon with a higher energy. Our approach highlights the potential for quantum nonlinear optics with integrated devices, and as the photons are at telecom wavelengths, it is well adapted to applications in quantum communication.Physical Review Letters 03/2014; 113(17):173601. · 7.73 Impact Factor 
Conference Paper: Experimental Demonstration of All Optical Phase Noise Mitigation of 40Gbits/s QPSK Signals by Mixing Differentially Delayed Nonlinear Products
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ABSTRACT: We propose and demonstrate an all optical phase noise mitigation scheme by mixing differentially delayed nonlinear products. For 40Gbits/s signals, phase squeezing results in phase noise range reduction of around 50% and 1.5 dB OSNR gain at BER 1e5.Optical Fiber Communication Conference; 03/2014  [Show abstract] [Hide abstract]
ABSTRACT: We present an implementation of the $\mathcal{F}$statistic to carry out the first search in data from the Virgo laser interferometric gravitational wave detector for periodic gravitational waves from a priori unknown, isolated rotating neutron stars. We searched a frequency $f_0$ range from 100 Hz to 1 kHz and the frequency dependent spindown $f_1$ range from $1.6\,(f_0/100\,{\rm Hz}) \times 10^{9}\,$ Hz/s to zero. A large part of this frequency  spindown space was unexplored by any of the allsky searches published so far. Our method consisted of a coherent search over twoday periods using the $\mathcal{F}$statistic, followed by a search for coincidences among the candidates from the twoday segments. We have introduced a number of novel techniques and algorithms that allow the use of the Fast Fourier Transform (FFT) algorithm in the coherent part of the search resulting in a fiftyfold speedup in computation of the $\mathcal{F}$statistic with respect to the algorithm used in the other pipelines. No significant gravitational wave signal was found. The sensitivity of the search was estimated by injecting signals into the data. In the most sensitive parts of the detector band more than 90% of signals would have been detected with dimensionless gravitationalwave amplitude greater than $5 \times 10^{24}$.Classical and Quantum Gravity 02/2014; 31(16). · 3.10 Impact Factor
Publication Stats
13k  Citations  
1,074.98  Total Impact Points  
Top Journals
 Optics Letters (67)
 Physical Review D (27)
 Applied Physics Letters (26)
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Institutions

190–2014

Stanford University
 • E. L. Ginzton Laboratory
 • Solid State and Photonics Laboratory
 • Department of Applied Physics
 • Department of Materials Science and Engineering
Palo Alto, California, United States


2013

University of Wuerzburg
 Division of Technical Physics
Würzburg, Bavaria, Germany 
University of Science and Technology of China
 Department of Modern Physics
Luchow, Anhui Sheng, China


2010

Universitätsklinikum Jena
Jena, Thuringia, Germany 
National Tsing Hua University
 Institute of Photonics Technologies
Hsinchu, Taiwan, Taiwan 
ETH Zurich
 Institute of Quantum Electronics
Zürich, ZH, Switzerland


2006–2009

University of Pavia
Ticinum, Lombardy, Italy 
National Institute of Standards and Technology
 Time and Frequency Division
Gaithersburg, MD, United States


2005–2009

California Institute of Technology
Pasadena, California, United States


2004–2009

Huazhong University of Science and Technology
 Wuhan National Laboratory for Optoelectronics
Wuhan, Hubei, China


2001–2008

University of Southern California
 • Department of Electrical Engineering
 • Spatial Sciences Institute
Los Angeles, CA, United States 
Politecnico di Milano
Milano, Lombardy, Italy


2007

Oregon State University
 Department of Physics
Corvallis, OR, United States


1998–2006

IMRA America, Inc.
Fremont, California, United States


2000–2005

Purdue University
 School of Electrical and Computer Engineering
West Lafayette, IN, United States


2001–2004

Nippon Telegraph and Telephone
Edo, Tōkyō, Japan


2003

United States Navy
Monterey, California, United States


1999

Technische Universität Kaiserslautern
 Fachbereich für Physik
Kaiserslautern, RhinelandPalatinate, Germany 
University of Central Florida
 Center for Research and Education in Optics and Lasers
Orlando, FL, United States 
AT&T Labs
Austin, Texas, United States


1997

Rice University
 Rice Quantum Institute
Houston, Texas, United States 
Tel Aviv University
 Department of Electrical Engineering  Physical Electronics
Tell Afif, Tel Aviv, Israel
