THE STATUS OF GEO 600

Hartmut Grote for the LSC 8. Amaldi Conference New York, 23. June 2009 LSC G0900508

Astrowatch Astrowatch by GEO      and LIGO­H2 Bridge the gap between  S5(VSR1) and S6(VSR2) Triggered searches      GRB, SGR, SN,...

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The GEO600 Interferometer

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The GEO600 Interferometer Triple suspensions  with monolithic  ultimate stage 

Approx. 140 fibre years on running IFO with ~5 partial ventings

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The GEO600 Interferometer Electro­Static Drives: • Used for fast control  of diff. arm length and  alignment

• ~3 mm gap between  reaction mass and  mirror • 630 V bias,        range  0­900V • 900 V → 350µN  →  about 3.5µm @ DC

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The GEO600 Interferometer Signal­Recycling: • Shaping detector  response • Complex detector  (resonance conditions  with detuned SR) • GW signal is spread  over both quadratures  P and Q.

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Running GEO in Astrowatch Remote weekend shifts by operators (off­site) No night shifts, ­> lost only about 1.5% of total  time by not automatically relocking  interferometer at night Allowed for daytime experiments  (goal: 80% science time)

   

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GEO ­ Astrowatch Science Time

Science time: 85.85% Locked time:  92.42%

Nov 2007 – June 2009: 496 days of science data collected 8

Histogram of Lock Lengthes (>1h)

Number of locks

72.4% of locked time in locks > 1hour Longest lock: ~102 hours

Lock length [hours]

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Strain [1 / rt(Hz)]

GEO600 / Ligo H2 in Astrowatch

Frequency [Hz]

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Strain [1 / rt(Hz)]

GEO600 / Ligo H2 in Astrowatch

Jonathan Leong: Absolute amplitude calibration of GEO600 Frequency [Hz] Frequency [Hz]

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Strain [1/sqrt(Hz)]

Noise Analysis

Frequency [Hz] 12

Strain [1 / rt(Hz)]

Recent DC­Readout vs. Heterodyne

Frequency [Hz] 13

Strain [1 / rt(Hz)]

Recent DC­Readout vs. Heterodyne

Jerome Degallaix: Commissioning of the tuned DC readout at GEO600 Frequency [Hz] Frequency [Hz] 14

Plans We will end Astrowatch on 7. July 2009 Start of GEO­HF: Sequential upgrades Squeezing (tuned SR with DC­readout) 2009

OMC Adv. Ligo CDS system for SQZ, OMC, GEOcontrols

2010

2011

Circulating light power increase ~factor 8  new IMC mirrors, new EOMs ?, shadowsensors fix, thermal  compensation for BS, 35W main laser Signal recycling bandwidth increase ~factor 4 ... 15

The GEO­Squeezer

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The GEO­Squeezer

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...and a first glance at the performance

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...and a first glance at the performance

Henning Vahlbruch (Fri, 11:20): Squeezed light for Gravitational Wave Astronomy

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GEO output beam Squeezed vacuum beam

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GEO output beam Squeezed vacuum beam

Simon Chelkowski: How to inject a squeezed vacuum field[Hz] into a gravitational wave detector Frequency 21

New Vacuum Chamber

Faraday Rotator

OMC

Vibration-Isolated platform (Minus-K) 22

GEO ­ OMC

Finesse 150 Rejection of HOM and SB power > 100 23

GEO ­ OMC

Finesse 150 Rejection of HOM and SB power > 100 24

GEO ­ OMC

Finesse 150 Rejection of HOM and SB power > 100 25

GEO ­ OMC

Jerome Degallaix: Commissioning of the tuned DC readout at GEO600

Frequency [Hz]

Mirko Prijatelj: Finesse 150

Control and Automatic Alignment of the Output Mode Cleaner of GEO

Frequency [Hz]

Rejection of HOM and SB power > 100

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GEO­HF Sensitivities Its difficult to make  predictions, in particular about the  future

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Strain [1/sqrt(Hz)]

GEO­HF Sensitivities

Frequency [Hz] 28

Strain [1/sqrt(Hz)]

GEO­HF Sensitivities

Harald Lück (Thu, 3:00): The transition to GEO HF

Frequency [Hz] 29

Queuing up !

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Summary Astrowatch since Nov 2007: > 85% science time Start of GEO­HF upgrades on 7. July 2009: Squeezing (DC readout, tuned SR) OMC Circulating light power increase Signal recycling bandwidth increase

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Strain [1/sqrt(Hz)]

GEO Sensitivities 

Frequency [Hz]

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GEO600 Detector Status

Start of GEOHF: Sequential upgrades. Squeezing (tuned SR with DCreadout). OMC. Adv. Ligo CDS system for SQZ, OMC, GEOcontrols. Circulating light power increase ~factor 8 new IMC mirrors, new EOMs ?, shadowsensors fix, thermal compensation for BS, 35W main laser. Signal recycling bandwidth increase ~factor 4.

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