A. M. Sintes
Max Planck Society
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Featured researches published by A. M. Sintes.
Classical and Quantum Gravity | 2002
B. Willke; P. Aufmuth; Carsten Aulbert; S. Babak; R. Balasubramanian; B. Barr; Steven J. Berukoff; S. Bose; G. Cagnoli; M. M. Casey; D. Churches; D. Clubley; Carlo Nicola Colacino; D. R. M. Crooks; Curt Cutler; Karsten Danzmann; R. Davis; E. J. Elliffe; Carsten Fallnich; Andreas Freise; S. Gossler; A. Grant; H. Grote; Gerhard Heinzel; A. Heptonstall; M. Heurs; J. Hough; Keita Kawabe; Karsten Kötter; V. Leonhardt
The GEO 600 laser interferometer with 600 m armlength is part of a worldwide network of gravitational wave detectors. Due to the use of advanced technologies like multiple pendulum suspensions with a monolithic last stage and signal recycling, the anticipated sensitivity of GEO 600 is close to the initial sensitivity of detectors with several kilometres armlength. This paper describes the subsystems of GEO 600, the status of the detector by September 2001 and the plans towards the first science run.
Classical and Quantum Gravity | 2009
K. G. Arun; S. Babak; Emanuele Berti; Neil J. Cornish; Curt Cutler; Jonathan R. Gair; Scott A. Hughes; Bala R. Iyer; Ryan N. Lang; Ilya Mandel; Edward K. Porter; B. S. Sathyaprakash; Siddhartha Sinha; A. M. Sintes; M. Trias; Chris Van Den Broeck; Marta Volonteri
The LISA Parameter Estimation Taskforce was formed in September 2007 to provide the LISA Project with vetted codes, source distribution models and results related to parameter estimation. The Taskforces goal is to be able to quickly calculate the impact of any mission design changes on LISAs science capabilities, based on reasonable estimates of the distribution of astrophysical sources in the universe. This paper describes our Taskforces work on massive black-hole binaries (MBHBs). Given present uncertainties in the formation history of MBHBs, we adopt four different population models, based on (i) whether the initial black-hole seeds are small or large and (ii) whether accretion is efficient or inefficient at spinning up the holes. We compare four largely independent codes for calculating LISAs parameter-estimation capabilities. All codes are based on the Fisher-matrix approximation, but in the past they used somewhat different signal models, source parametrizations and noise curves. We show that once these differences are removed, the four codes give results in extremely close agreement with each other. Using a code that includes both spin precession and higher harmonics in the gravitational-wave signal, we carry out Monte Carlo simulations and determine the number of events that can be detected and accurately localized in our four population models.
Classical and Quantum Gravity | 2007
P. Ajith; S. Babak; Y. Chen; M. Hewitson; Badri Krishnan; James Whelan; Bernd Brügmann; Peter Diener; José A. González; Mark Hannam; S. Husa; Michael Koppitz; Denis Pollney; Luciano Rezzolla; L. Santamaría; A. M. Sintes; Ulrich Sperhake; Jonathan Thornburg
Recent progress in numerical relativity has enabled us to model the non-perturbative merger phase of the binary black-hole coalescence problem. Based on these results, we propose a phenomenological family of waveforms which can model the inspiral, merger and ring-down stages of black-hole coalescence. We also construct a template bank using this family of waveforms and discuss its implementation in the search for signatures of gravitational waves produced by black-hole coalescences in the data of ground-based interferometers. This template bank might enable us to extend the present inspiral searches to higher-mass binary black-hole systems, i.e., systems with total mass greater than about 80 solar masses, thereby increasing the reach of the current generation of ground-based detectors.
Proceedings of SPIE | 2004
K. A. Strain; B. Allen; P. Aufmuth; Carsten Aulbert; S. Babak; R. Balasubramanian; B. Barr; Steven J. Berukoff; Alexander Bunkowski; G. Cagnoli; C. A. Cantley; M. M. Casey; S. Chelkowski; D. Churches; T. Cokelaer; Carlo Nicola Colacino; D. R. M. Crooks; Curt Cutler; Karsten Danzmann; R. Davies; R. J. Dupuis; E. J. Elliffe; Carsten Fallnich; A. Franzen; Andreas Freise; S. Goßler; A. Grant; H. Grote; S. Grunewald; J. Harms
The GEO 600 laser interferometer with 600m armlength is part of a worldwide network of gravitational wave detectors. GEO 600 is unique in having advanced multiple pendulum suspensions with a monolithic last stage and in employing a signal recycled optical design. This paper describes the recent commissioning of the interferometer and its operation in signal recycled mode.
Physical Review D | 2004
Badri Krishnan; A. M. Sintes; M. A. Papa; Bernard F. Schutz; S. Frasca; C. Palomba
This paper describes an incoherent method to search for continuous gravitational waves based on the Hough transform, a well-known technique used for detecting patterns in digital images. We apply the Hough transform to detect patterns in the time-frequency plane of the data produced by an earth-based gravitational wave detector. Two different flavors of searches will be considered, depending on the type of input to the Hough transform: either Fourier transforms of the detector data or the output of a coherent matched-filtering type search. We present the technical details for implementing the Hough transform algorithm for both kinds of searches, their statistical properties, and their sensitivities.
Classical and Quantum Gravity | 2008
K. Wette; B. J. Owen; B. Allen; M. Ashley; J. Betzwieser; N. Christensen; T. D. Creighton; V. Dergachev; I. Gholami; E. Goetz; R. Gustafson; D. Hammer; D. I. Jones; Badri Krishnan; M. Landry; B. Machenschalk; D. E. McClelland; G. Mendell; C. Messenger; M. A. Papa; P. Patel; M. Pitkin; H. J. Pletsch; R. Prix; K. Riles; L. Sancho De La Jordana; S. M. Scott; A. M. Sintes; M. Trias; James Whelan
We describe a search underway for periodic gravitational waves from the central compact object in the supernova remnant Cassiopeia A. The object is the youngest likely neutron star in the Galaxy. Its position is well known, but the object does not pulse in any electromagnetic radiation band and thus presents a challenge in searching the parameter space of frequency and frequency derivatives. We estimate that a fully coherent search can, with a reasonable amount of time on a computing cluster, achieve a sensitivity at which it is theoretically possible (though not likely) to observe a signal even with the initial LIGO noise spectrum. Cassiopeia A is only the second object after the Crab pulsar for which this is true. The search method described here can also obtain interesting results for similar objects with current LIGO sensitivity.
Physical Review D | 2008
M. Trias; A. M. Sintes
We study parameter estimation of supermassive black hole binary systems in the final stage of inspiral using the full post-Newtonian gravitational waveforms. We restrict our analysis to systems in circular orbit with negligible spins, in the mass range
Physical Review D | 2016
Juan Calderón Bustillo; S. Husa; A. M. Sintes; M. Pürrer
{10}^{8}{M}_{\ensuremath{\bigodot}}\ensuremath{-}{10}^{5}{M}_{\ensuremath{\bigodot}}
General Relativity and Gravitation | 1996
J. Carot; A. A. Coley; A. M. Sintes
, and compare the results with those arising from the commonly used restricted post-Newtonian approximation. The conclusions of this work are particularly important with regard to the astrophysical reach of future Laser Interferometer Space Antenna measurements. Our analysis clearly shows that modeling the inspiral with the full post-Newtonian waveform, not only extends the reach to higher mass systems, but also improves in general the parameter estimation. In particular, there are remarkable improvements in angular resolution and distance measurement for systems with a total mass higher than
Physical Review D | 1998
A. M. Sintes; Bernard F. Schutz
5\ifmmode\times\else\texttimes\fi{}{10}^{6}{M}_{\ensuremath{\bigodot}}