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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

A proposal for additional Low FrequencyGravitational WaveInterferometric Detectorsat LIGO

Riccardo DeSalvo

California Institute of Technology

Globular Cluster 17th October 2003

LIGO-xxx

status of observations now and here
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

why lf gwids
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

what is necessary for a lf gwid
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

adl lf gwid complementarity
AdLLF-GWIDcomplementarity

Newtonian

Noise

limit

LIGO-xxx-00-R

adl lf gwid complementarity1
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

adl and lf gwid
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

can we accommodate a lf interferometer next to adv ligo
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

slide9

And there appears to be

space in the halls

Virgo-like towers

TAMA-like towers

LIGO-xxx-00-R

conclusions
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

lf gwid proposal pointers
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

aspen gwdaw workshop winter 2004
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