Gravitational Wave Interferometers

In General, Ground-Based > s.a. detection of gravitational waves [including atom interferometers].
* Theory: For the separation between two free particles, L / L = h^TT_ij nⁱ n ^j + O(h²).
@ Intros: Giazotto PRP(89); Saulson 94; Finn gq/96 [LIGO as a community]; Barish gq/99-in; Hough & Rowan LRR(00); Robertson CQG(00); Sintes gq/00-in.
@ Background: Allen & Brustein PRD(97)gq/96; Maggiore PRP(00)ap/99; Babusci & Giovannini CQG(00)ap/99, gq/99 [VIRGO].
@ Matter-wave interferometers: Foffa et al PRD(06); Delva et al PLA(06)gq [vs light-wave]; Tino & Vetrano CQG(07)gq [atomic, possibility].
@ Related topics: Frasca & Papa IJMPD(95) [networks]; Sun et al PRL(96) [Sagnac interferometer]; Cohadon et al PRL(99) + pn(99)sep [mirror cooling]; Bose et al Pra(99)gq [networks]; Buonanno & Chen CQG(01)gq/00 [and standard quantum limit]; Faraoni GRG(07)gq [correcting a misconception]; Corda gq/07/IJMPD [importance of magnetic component of waves].

LIGO (Laser Interferometer Gravitational-Wave Antenna)
* Idea: A pair of 4-km interferometers (Hanford, WA, and Livingston, LA, 10 light-ms apart), by a Caltech, MIT, ..., collaboration.
* Status: 1998, Under construction; 1999, 40-m prototype operational at Caltech, h 10^–19; 2000, Engineering runs; 2002, First data taking run; 2004, Three data runs completed, h 10^–22 Hz^–1/2 at 100–300 Hz; 2006, Science runs S1–S4 completed, S5 in progress with detector at design sensitivity for f > 150 Hz.
* Frequency range: f 10–10⁴ Hz, limited below by seismic noise, above by laser shot noise.
* Detection rate: Sensitive to 1 M_Sun binary coalescence at a few Mpc, with expected rate 1/13 yr.
* Advanced LIGO: Should be able to detect inspirals out to 200 Mpc, 1–100/yr; Operation may start in 2007.
@ General references: Finn gq/96-in [research community]; Barish & Weiss PT(99)oct [preview]; González gq/03-in [status]; Abbott et al a0711.
@ Bursts: Weinstein for LIGO CQG(04)gq/03; Abbott et LSC PRD(05)gq [GRB030329], PRD(05)gq; LIGO CQG(07)-a0704 [4th science run]; Thorne a0706-in.
@ Periodic sources: Abbott et LSC PRD(05)gq [ns + ns]; Abbott et al PRD(06) [black hole + black hole]; LSC gq/06 [data from S2 run]; Abbott et LSC a0704, PRD(08)-a0708, a0712 [data from S3 and S4 runs].
@ Stochastic background: Abbott et LSC PRD(04)gq/03; LSC ap/06; Abbott et LIGO + Allegro PRD(07) [cross-correlation analysis]; Fotopoulos et LSC a0801-in.
@ Related topics: González CQG(00)gq [thermal noise in suspension].

Other Detectors > s.a. space-based gravitational wave interferometers.
* VIRGO: Italian-French collaboration, 3-km arms, near Pisa, very similar to LIGO; 2004, Being commissioned; 2006, Science run.
* GEO600: British-German, near Hanover; 2004, Operating, more advanced techniques than LIGO I but shorter; 2006, Beginning of continuous operation [@ news sr(06)jun].
* TAMA300: Japanese collaboration ("prototype for 3-km"), near Tokyo; 2004, Taking data since before LIGO.
* AIGO: 2006, Proposed but not accepted, future not certain.
@ VIRGO: Hellemans SA(03)aug; Spallicci et al CQG(05)gq/04 [advanced]; Acernese et al CQG(05)gq/04, CQG(06) [status]; Virgo a0803 [search in connection with GRB 050915a].
@ GEO600: Schutz gq/99-in; Balasubramanian et al CQG(05)gq; Hild CQG(06) [status].
@ TAMA300: Tagoshi et al PRD(01); Ando et al PRD(05)gq/04.
@ Related topics: Sato et al PRD(04)gq [LISM, underground]; Nishizawa et al PRD(08) [at 100 MHz].

Specific Sources and Data Analysis > s.a. gravitational wave background; sources of gravitational waves.
* Inspirals: The main method is matched filtering, comparison of the data with a large set of templates developed for different parameter sets (not many parameters, the physics of binaries is simple); Templates presumably need to be as accurate as O(v⁶); To detect the weaker waves, may have to extract signal from many months of data.
* Other sources: Bursts, stochastic background, continuous sources (rotating stars, etc).
@ General references: Finn gq/99 [data archive]; Krolak gq/99; Sahay gq/02-PhD.
@ Techniques: Tagliaferri et al ap/99-in [neural networks]; Pradier et al IJMPD(00)gq-in, PRD(01)gq/00 [filters, triggers]; Black & Gutenkunst AJP(03) [intro].
@ Noise: Thorne & Winstein PRD(99)gq/98; Creighton PRD(99)gq; Allen et al gq/99; González gq/03.
@ Binaries: Ryan PRD(97) [massive body multipoles]; Allen et al PRL(99) [bounds from 40-m prototype]; Martel gq/99-in, & Poisson PRD(99)gq [eccentric]; Dhurandhar & Vecchio PRD(01)gq/00; Abbott et al & Akutsu et al PRD(06) [neutron star + neutron star, LIGO+TAMA300]; Mukhopadhyay et al PRD(06)gq [coherent vs coincident strategies].
@ Related topics: Jaranowski et al PRD(98)gq, & Krolak PRD(00)gq/99 [spinning neutron stars]; Anderson & Balasubramanian PRD(99)gq [unmodeled sources].

Main page – Abbreviations – Journals – Comments – Other sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified 24 jun 2008