Sign on

SAO/NASA ADS Astronomy Abstract Service


· Find Similar Abstracts (with default settings below)
· Electronic Refereed Journal Article (HTML)
· arXiv e-print (arXiv:0811.1011)
· References in the article
· Citations to the Article (17) (Citation History)
· Refereed Citations to the Article
· Also-Read Articles (Reads History)
·
· Translate This Page
Title:
Massive black-hole binary inspirals: results from the LISA parameter estimation taskforce
Authors:
Arun, K. G.; Babak, Stas; Berti, Emanuele; Cornish, Neil; Cutler, Curt; Gair, Jonathan; Hughes, Scott A.; Iyer, Bala R.; Lang, Ryan N.; Mandel, Ilya; Porter, Edward K.; Sathyaprakash, Bangalore S.; Sinha, Siddhartha; Sintes, Alicia M.; Trias, Miquel; Van Den Broeck, Chris; Volonteri, Marta
Affiliation:
AA(LAL, Univ. Paris-Sud, IN2P3/CNRS, Orsay, France ; Institut d'Astrophysique de Paris, UMR 7095-CNRS, Université Pierre et Marie Curie, 98bis boulevard Arago, 75014 Paris, France ), AB(Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Am Mühlenberg 1, D-14476 Golm bei Potsdam, Germany ), AC(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA ; Department of Physics and Astronomy, The University of Mississippi, University, MS 38677-1848, USA ), AD(Department of Physics, Montana State University, Bozeman, MT 59717, USA ), AE(Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109, USA ; Theoretical Astrophysics, California Institute of Technology, Pasadena, CA 91125, USA ), AF(Institute of Astronomy, University of Cambridge, Cambridge, CB30HA, UK ), AG(Department of Physics and Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA ), AH(Raman Research Institute, Bangalore, 560 080, India ), AI(Department of Physics and Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA ), AJ(Department of Physics and Astronomy, Northwestern Univ., Evanston, IL, USA ), AK(Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Am Mühlenberg 1, D-14476 Golm bei Potsdam, Germany ; APC (AstroParticules et Cosmologie), 10, rue Alice Domon et Léonie Duquet, 75205 Paris Cedex 13, France ), AL(School of Physics and Astronomy, Cardiff University, 5, The Parade, Cardiff, CF24 3YB, UK ), AM(Raman Research Institute, Bangalore, 560 080, India ; Department of Physics, Indian Institute of Science, Bangalore, 560 012, India ), AN(Max-Planck-Institut für Gravitationsphysik (Albert-Einstein-Institut), Am Mühlenberg 1, D-14476 Golm bei Potsdam, Germany ; Departament de Física, Universitat de les Illes Balears, Cra. Valldemossa Km. 7.5, E-07122 Palma de Mallorca, Spain ), AO(Departament de Física, Universitat de les Illes Balears, Cra. Valldemossa Km. 7.5, E-07122 Palma de Mallorca, Spain ), AP(School of Physics and Astronomy, Cardiff University, 5, The Parade, Cardiff, CF24 3YB, UK ), AQ(Department of Astronomy, University of Michigan, Ann Arbor, MI 48109, USA)
Publication:
Classical and Quantum Gravity, Volume 26, Issue 9, pp. 094027 (2009).
Publication Date:
05/2009
Origin:
IOP
DOI:
10.1088/0264-9381/26/9/094027
Bibliographic Code:
2009CQGra..26i4027A

Abstract

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 Taskforce's goal is to be able to quickly calculate the impact of any mission design changes on LISA's science capabilities, based on reasonable estimates of the distribution of astrophysical sources in the universe. This paper describes our Taskforce's 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 LISA's 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.
Bibtex entry for this abstract   Preferred format for this abstract (see Preferences)

   

Find Similar Abstracts:

Use: Authors
Title
Abstract Text
Return: Query Results Return    items starting with number
Query Form
Database: Astronomy
Physics
arXiv e-prints