Space-Based
Gravitational Wave Interferometers| Space-Based
Gravitational Wave Interferometers |
In General > s.a. gravitational
wave interferometers.
* Advantages: Can detect
low frequencies, f 
10–4–1
Hz.
@ In general: Caldwell et al PRD(99)ap/98 [cmb
polarization missions as gravitational wave detectors]; Larson et al PRD(00)gq/99 [sensitivity];
Moore & Hellings PRD(02)gq/99 [angular
resolution]; Larson et al PRD(02)gq [unequal
arm length]; Rubbo et al PRD(04)gq/03 [modeling].
@ Theory: Poisson PRD(96)
[black hole parameters].
@ And gravitational wave background:
Cornish & Larson CQG(01)gq;
Smith et al PRD(06)ap/05
[from inflation].
@ Time-delay interferometry:
Tinto et al PRD(03)gq [LISA],
PRD(04)gq/03;
Tinto & Dhurandhar LRR(05)gq/04.
LISA (Laser Interferometer Space Antenna) > s.a. background;
graviton; scalar-tensor
theories.
* Idea: Proposed in 1995;
To be deployed on a heliocentric orbit with arm length L 5
Mkm, trailing the Earth by 20º; Most sensitive in the frequency range 10–4–10–2 Hz;
Will look at known ns binaries (16 as of 2004) for calibration, wd binaries,
compact objects spiraling into galactic black holes, background (bubbles from
phase transitions, cosmic strings, ...).
* Pathfinder: An ESA
precursor mission with one satellite only, to test system to keep test mass
in place
for a long time.
* Status: 2004, Pathfinder
launch possibly by 2008, LISA in 2013? 2006, LISA launch by 2016? 2007, ESA
and NASA sign formal agreement for Pathfinder mission, due for launch
to the L1 Lagrange point between Earth and the Sun in early 2010 [@ news sr(07)jun].
@ In general: Schutz gq/97, gq/97 [intro];
issue CQG(97)#6;
Vecchio gq/99-in
[impact]; issue CQG(01)#19;
Ungarelli & Vecchio
PRD(01)ap [anisotropy
of background]; issue CQG(03)#10;
Danzmann & Rüdiger CQG(03);
Centrella ap/03-in
[rev]; Cornish gq/03 [demodulation];
Lobo gq/04-in
[rev]; issue CQG(05)#10;
Hughes gq/06-in,
a0711-CQG [rev]; Benacquista et al gq/06 [analysis];
Araujo et al gq/06-in.
@ Performance: Cornish & Rubbo PRD(03)gq/02 [response
function]; Sylvestre & Tinto PRD(03) [noise]; Prince et al PRD(02)gq,
Nayak et al CQG(03)
[sensitivity].
@ Binary detection: Hellings CQG(03)gq/02;
Cornish & Larson PRD(03)ap;
Krolak & Tinto gq/03/PRD;
Rogan & Bose CQG(04)gq.
@ Supermassive black holes: Haehnelt ap/98-in;
Berti et al PRD(06)gq/05 [ringdown];
Harry et al a0804 [hierarchical search].
@ Supermassive binaries: Rhook & Wyithe MNRAS(05)ap;
Glampedakis & Babak CQG(06)gq/05 [quasi-Kerr
field]; Arun PRD(06)gq;
Brown et al a0705-in;
Cutler & Vallisneri a0707.
@ Other sources: Benacquista
et al CQG(01)gq/00 [globular
clusters]; Vinet CQG(06) [asteroids].
Other Missions
* Projects: After
LISA, there are proposals for NASA's Big Bang Observatory (BBO around 2020?),
smaller detectors with more powerful lasers for gravitational wave background
with f around 1 Hz (to fill the gap between LIGO and LISA), for example
from slow roll inflation and Advanced Laser Interferometer Antenna (ALIA),
whose main scientific goal is to study intermediate mass black holes; Japan
is studying the Deci-Hertz Interferometer Gravitational-wave Observer (DECIGO)
mission.
@ Various missions: Hellings CP(96)
[OMEGA mission]; Cornish et al ap/02-rp
[GREAT mission];
Crowder & Cornish PRD(05)gq [beyond
LISA]; Corbin & Cornish CQG(06)gq/05 [BBO
and gravitational wave background]; Pulido & Ni a0704-GRG
[ASTROD].
Online Resources > see The LISA Calculator.
Main page – Abbreviations – Journals – Comments – Other
sites – Acknowledgements
Send feedback and suggestions to bombelli at olemiss.edu – Modified
20 jun 2008