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LOS Absorption Presentation for TCS Group Rupal S. Amin Tuesday, August 26, 2008 LIGO-G080428-00-L.

Published byAgnes Rhoda Anthony Modified over 9 years ago

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Presentation on theme: "LOS Absorption Presentation for TCS Group Rupal S. Amin Tuesday, August 26, 2008 LIGO-G080428-00-L."— Presentation transcript:

1 LOS Absorption Presentation for TCS Group Rupal S. Amin Tuesday, August 26, 2008 LIGO-G080428-00-L

2 Outline Motivation Theory Procedure Data Result LIGO-G080428-00-L

3 Motivation Question: 1) What do we care about the absorption of the large optics? 2) What is the absorption value? Answer: Silica mirrors inside IFO unfortunately absorb resonant laser power. LIGO-G080428-00-L

4 Motivation Ans (con’t): Mirrors expand due to temperature changes. Depending on absorption coefficient, mirrors may distort beyond or below design optimum. Cold  Hot  LIGO-G080428-00-L

5 Motivation Measuring absorption (especially the ITMS) allows TCS team to build effective absorption models (Mathematica, Matlab, Finesse, SIS) Correct setup scheme for Enhanced TCS. So…We need the absorption values of the large Fabry-Perot optics. LIGO-G080428-00-L

6 Theory Crude theory – Mirrors have body modes Finite temperature Brownian motion – Frequencies are thermally dependent Due to Young’s modulus having a Y(T). – Track body mode frequency evolutions due to  T –  f yields power absorption LIGO-G080428-00-L

7 Theory Crude theory Better theory We need f and ∆f to determine α * LIGO-G080428-00-L

8 Procedure Power Cycle IFO during fully locked state. – Do this over several hours Save data from fast ASQ sample channels and temperature sensors. Download GBs of data from LDAS and analyze. LIGO-G080428-00-L

9 Procedure Pwr t df/f 4 W 1 W LIGO-G080428-00-L

10 Data Lock data from 899867714 s Thermal data: Mirror modes are history dependent LIGO-G080428-00-L

11 Thermal Resistances and Sources BSC and contents slow LVEA to ITM interaction time. Beam tubes: heat source but negligible LIGO-G080428-00-L

12 Thermal Resistance Simulation of TM interaction with BSC. Small perturbations lead to simulation problems. LIGO-G080428-00-L

13 Analysis using raw data LIGO-G080428-00-L

14 Raw Data (noisy) LIGO-G080428-00-L

15 Fitting Data  Peak = (x0, Amplitude) DC based on noise average LIGO-G080428-00-L

16 Analysis using fitted data LIGO-G080428-00-L

17 Analysis ∆f/f for ITMy LIGO-G080428-00-L

18 Results Total uncorrected slope = 1.3(3)e-6+/- 1.3e-6 Hz/s Uncorrected for high power = 4.(43)e-7+/- 3. e-7 Hz/s Crudely Corrected slope = ? Refined df/f = Need to do LIGO-G080428-00-L

19 Ambient temperature f-drift Crude shift due to temperature fluctuations LIGO-G080428-00-L

20 Questions? 1) What is your purpose? 2) What is your favourite color? LIGO-G080428-00-L

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