Coupling of relative intensity noise and pathlength noise to the length measurement in the optical metrology system of LISA Pathfinder

被引：4

作者：

Wittchen, Andreas ^{[1
]}

Armano, M. ^{[2
]}

Audley, H. ^{[3
,4
]}

Auger, G. ^{[5
]}

Baird, J. ^{[6
]}

Bassan, M. ^{[7
,8
]}

Binetruy, P. ^{[5
]}

Born, M. ^{[3
,4
]}

Bortoluzzi, D. ^{[9
,10
]}

Brandt, N. ^{[11
]}

Caleno, M. ^{[12
]}

Cavalleri, A. ^{[13
,14
]}

Cesarini, A. ^{[13
,14
]}

Cruise, M. ^{[15
]}

Danzmann, K. ^{[3
,4
]}

de Deus Silva, M. ^{[2
]}

De Rosa, R. ^{[16
,17
]}

Di Fiore, L. ^{[17
]}

Diepholz, I. ^{[3
,4
]}

Dolesi, R. ^{[13
,14
]}

Dunbar, N. ^{[18
]}

Ferraioli, L. ^{[19
]}

Ferroni, V. ^{[13
,14
]}

Fitzsimons, E. ^{[20
]}

Flatscher, R. ^{[11
]}

Freschi, M. ^{[2
]}

Marrirodriga, C. Garcia ^{[12
]}

Gerndt, R. ^{[11
]}

Gesa, L. ^{[21
]}

Gibert, F. ^{[13
,14
]}

Giardini, D. ^{[19
]}

Giusteri, R. ^{[13
,14
]}

Grado, A. ^{[16
,17
]}

Grimani, C. ^{[22
]}

Grzymisch, J. ^{[12
]}

Harrison, I. ^{[23
]}

Heinzel, G. ^{[3
,4
]}

Hewitson, M. ^{[3
,4
]}

Hollington, D. ^{[6
]}

Hoyland, D. ^{[15
]}

Hueller, M. ^{[13
,14
]}

Inchauspe, H. ^{[5
]}

Jennrich, O. ^{[12
]}

Jetzer, P. ^{[24
]}

Johlander, B. ^{[12
]}

Karnesis, N. ^{[3
,4
]}

Kaune, B. ^{[3
,4
]}

Korsakova, N. ^{[3
,4
]}

Killow, C. ^{[25
]}

Lobo, A. ^{[21
]}

机构：

[1] Albert Einstein Inst, Max Planck Inst Gravitat Phys, Potsdam, Germany

[2] Leibniz Univ Hannover, Hannover, Germany

[3] European Space Agcy, European Space Astron Ctr, Madrid 28692, Spain

[4] Max Planck Inst Gravitat Phys, Albert Einstein Inst, Callinstr 38, D-30167 Hannover, Germany

[5] Leibniz Univ Hannover, Callinstr 38, D-30167 Hannover, Germany

[6] Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Obs Paris,Sorbonne Paris Cite, Paris, France

[7] Imperial Coll London, High Energy Phys Grp, Blackett Lab, Phys Dept, Prince Consort Rd, London SW7 2BW, England

[8] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

[9] INFN, Sez Roma Tor Vergata, I-00133 Rome, Italy

[10] Univ Trento, Dept Ind Engn, Via Sommar 9, I-38123 Trento, Italy

[11] INFN, Trento Inst Fundamental Phys & Applicat, Rome, Italy

[12] Airbus Def & Space, Claude Dornier Str, D-88090 Immenstaad, Germany

[13] European Space Agcy, European Space Technol Ctr, Keplerlaan 1, NL-2200 AG Noordwijk, Netherlands

[14] Univ Trento, Dipartimento Fis, I-38123 Povo, Trento, Italy

[15] INFN, Trento Inst Fundamental Phys & Applicat, I-38123 Povo, Trento, Italy

[16] Univ Birmingham, Dept Phys & Astron, Birmingham, W Midlands, England

[17] INAF, Osservatorio Astron Capodimonte, I-80131 Naples, Italy

[18] INFN, Sez Napoli, I-80126 Naples, Italy

[19] Airbus Def & Space, Gunnels Wood Rd, Stevenage SG1 2AS, Herts, England

[20] Swiss Fed Inst Technol, Inst Geophys, Sonneggstr 5, CH-8092 Zurich, Switzerland

[21] Royal Observ, UK Astron Technol Ctr, Blackford Hill, Edinburgh EH9 3HJ, Midlothian, Scotland

[22] Inst Ciencies Espai CSIC IEEC, Campus UAB,Carrer Can Magrans S-N, Cerdanyola Del Valles 08193, Spain

[23] Univ Urbino Carlo Bo, DISPEA, INFN, Via S Chiara 27, I-61029 Urbino, Italy

[24] European Space Agcy, European Space Operat Ctr, D-64293 Darmstadt, Germany

[25] Univ Zurich, Phys Inst, Winterthurerstr 190, CH-8057 Zurich, Switzerland

[26] Univ Glasgow, Sch Phys & Astron, SUPA, Inst Gravitat Res, Glasgow G12 8QQ, Lanark, Scotland

[27] Univ Politecn Cataluna, Dept Engn Elect, ES-08034 Barcelona, Spain

[28] Co Gen Spazio, CGS SpA, Via Gallarate 150, I-20151 Milan, Italy

[29] NASA, Goddard Space Flight Ctr, Gravitat Astrophys Lab, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[30] Univ Firenze, Dipartimento Fis & Astron, I-50019 Florence, Italy

来源：

11TH INTERNATIONAL LISA SYMPOSIUM | 2017年 / 840卷

关键词：

D O I：

10.1088/1742-6596/840/1/012003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

LISA Pathfinder is a technology demonstration mission for the space-based gravitational wave observatory, LISA. It demonstrated that the performance requirements for the interferometric measurement of two test masses in free fall can be met. An important part of the data analysis is to identify the limiting noise sources.[1] This measurement is performed with heterodyne interferometry. The performance of this optical metrology system (OMS) at high frequencies is limited by sensing noise. One such noise source is Relative Intensity Noise (RIN). RIN is a property of the laser, and the photodiode current generated by the interferometer signal contains frequency dependant RIN. From this electric signal the phasemeter calculates the phase change and laser power, and the coupling of RIN into the measurement signal depends on the noise frequency. RIN at DC, at the heterodyne frequency and at two times the heterodyne frequency couples into the phase. Another important noise at high frequencies is path length noise. To reduce the impact this noise is suppressed with a control loop. Path length noise not suppressed will couple directly into the length measurement. The subtraction techniques of both noise sources depend on the phase difference between the reference signal and the measurement signal, and thus on the test mass position. During normal operations we position the test mass at the interferometric zero, which is optimal for noise subtraction purposes. This paper will show results from an in-flight experiment where the test mass position was changed to make the position dependant noise visible.

引用

页数：4

共 50 条

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