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A proposal for additional L ow F requency G ravitational W ave I nterferometric D etectors at LIGO

A proposal for additional L ow F requency G ravitational W ave I nterferometric D etectors at LIGO. Riccardo DeSalvo California Institute of Technology Globular Cluster 17 th October 2003 LIGO- xxx. Status of observations now and here!!. TAMA has been running for >3 years

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A proposal for additional L ow F requency G ravitational W ave I nterferometric D etectors at LIGO

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  1. A proposal for additional Low FrequencyGravitational WaveInterferometric Detectorsat LIGO Riccardo DeSalvo California Institute of Technology Globular Cluster 17th October 2003 LIGO-xxx

  2. Status of observationsnow and here!! • TAMA has been running for >3 years • Steadily improving sensitivity >100 Hz • < factor of 10 from nominal sensitivity • LIGO has been acquiring data for > 1 year (with GEO) • Steadily improving sensitivity ~100 Hz • < factor of 10 from nominal sensitivity • Virgo commissioning • Taking data in ~< 1 year • > 20 Hz • AdLIGO starting up • Foreseen for > 2007 • > 40 Hz Low Frequency Threshold defined as mirror thermal noise corner! LIGO-xxx-00-R

  3. Why LF-GWIDs? • Adv-LIGO will cover the detection of pulsars, NS-NS and low-mass BH inspirals, the coalescence phase, and other GW physicswith its best sensitivity around100 Hz • Can ground based GWIDs monitor even lower frequencies • Is this useful to study globular clusters? LIGO-xxx-00-R

  4. What is necessary fora LF-GWID? • GW Interferometers can be optimized for LF with the following changes • Reduce beam power and different finesse (rad. Pressure) • Use longer suspensions (susp. TN) • Use Supersized, double weight, mirrors (coating TN, rad. Pr) • Use Fused Silica (instead of Sapphire) mirrors (bulk TN) • LF-tuning would divert AdLIGO from its original mission! • Need operation of separate Low and High Frequency complementary interferometers LIGO-xxx-00-R

  5. AdLLF-GWIDcomplementarity Newtonian Noise limit LIGO-xxx-00-R

  6. AdLLF-GWIDcomplementarity Triggered searches LF trigger HF strongly relativistic signal study Template Signal integration BH ring down in the frequency mass area above the purple line Merger phase follow-up in the frequency mass area above the yellow line End inspiral frequency First BH Kerr resonance LIGO-xxx-00-R

  7. AdL andLF-GWID 3.6 Gpc @37+37sm Blue: Low seismic Day Purple: High seismic Day Green: Ad-LIGO Seismic variability 1.15 Gpc @16+16 sm LIGO-xxx-00-R

  8. Can we accommodate a LF interferometer next to Adv-LIGO? • There seems to be space in the LIGO beam pipe just above and forwards of the Adv-LIGO mirrors • Advanced LIGO nominal beam positions LIGO-xxx-00-R

  9. And there appears to be space in the halls Virgo-like towers TAMA-like towers LIGO-xxx-00-R

  10. Conclusions • IMBH are important and compelling potential GW sources for a LF interferometer • Optimized LF sensitivity would allow: • Increase quite significantly theexplored volume in the Universe for heavier mass objects (3.6 Gpc, real cosmology reach). • Study of the genesis of the large galactic BH(believed to be central to the dynamics of galaxies) • Mapping the globular clusters in our neighborhood • Enhancement of the performance of both Virgo and LIGO • They would be “triggered” by the LF detection and follow up studying final inspiral and merge signals • Advanced LIGOs are freer to be narrow banded • Splitting up the frequency range between two different interferometers eases lots of design constraints and allows better performance from both LIGO-xxx-00-R

  11. LF-GWID proposal pointers Should all be in LIGO DCC, if not available LF-GWID Amaldi proceedings (LIGO- P030047-00-D): www.ligo.caltech.edu/~desalvo/manuscript-Amaldi2003.doc LF-GWID Elba proceedings (LIGO-P030040-00-D): www.ligo.caltech.edu/~desalvo/DESALVO_ELBA_manuscript.doc LF-GWID Amaldi power point presentation (LIGO-G030332-00-R ): www.ligo.caltech.edu/~desalvo/desalvo_amaldi.ppt LF-GWID Elba power point presentation (LIGO-G030292-00-R): www.ligo.caltech.edu/~desalvo/desalvo-elba.ppt LIGO-xxx-00-R

  12. Aspen GWDAW workshop winter 2004 • The LIGO S. C. equivalent of this informal meeting is the Aspen meeting. • February 15 to 21st 2004 • Please consider participating. • Input on what is relevant and important to make good astronomy is very important. • You can help !! LIGO-xxx-00-R

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