Details
| Original language | English |
|---|---|
| Pages (from-to) | 28-37 |
| Number of pages | 10 |
| Journal | Astroparticle physics |
| Volume | 98 |
| Early online date | 31 Jan 2018 |
| Publication status | Published - 1 Mar 2018 |
Abstract
Test mass charging caused by cosmic rays will be a significant source of acceleration noise for space-based gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor made in situ measurements of the cosmic ray flux while also providing information about its energy spectrum. We describe the monitor and present measurements which show a gradual 40% increase in count rate coinciding with the declining phase of the solar cycle. Modulations of up to 10% were also observed with periods of 13 and 26 days that are associated with co-rotating interaction regions and heliospheric current sheet crossings. These variations in the flux above the monitor detection threshold (≈ 70 MeV) are shown to be coherent with measurements made by the IREM monitor on-board the Earth orbiting INTEGRAL spacecraft. Finally we use the measured deposited energy spectra, in combination with a GEANT4 model, to estimate the galactic cosmic ray differential energy spectrum over the course of the mission.
Keywords
- Charging, GCR, GEANT4, LISA, Pathfinder, Radiation Monitor
ASJC Scopus subject areas
- Physics and Astronomy(all)
- Astronomy and Astrophysics
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In: Astroparticle physics, Vol. 98, 01.03.2018, p. 28-37.
Research output: Contribution to journal › Article › Research › peer review
}
TY - JOUR
T1 - Measuring the Galactic Cosmic Ray flux with the LISA Pathfinder radiation monitor
AU - Armano, M.
AU - Audley, H.
AU - Baird, J.
AU - Binetruy, P.
AU - Born, M.
AU - Bortoluzzi, D.
AU - Castelli, E.
AU - Cavalleri, A.
AU - Cesarini, A.
AU - Cruise, A.m.
AU - Danzmann, K.
AU - De Deus Silva, M.
AU - Diepholz, I.
AU - Dixon, G.
AU - Dolesi, R.
AU - Ferraioli, L.
AU - Ferroni, V.
AU - Finetti, N.
AU - Fitzsimons, E.d.
AU - Freschi, M.
AU - Gesa, L.
AU - Gibert, F.
AU - Giardini, D.
AU - Giusteri, R.
AU - Grimani, C.
AU - Grzymisch, J.
AU - Harrison, I.
AU - Heinzel, G.
AU - Hewitson, M.
AU - Hollington, D.
AU - Hoyland, D.
AU - Hueller, M.
AU - Inchauspé, H.
AU - Jennrich, O.
AU - Jetzer, P.
AU - Karnesis, N.
AU - Kaune, B.
AU - Korsakova, N.
AU - Killow, C.j.
AU - Lobo, J.a.
AU - Lloro, I.
AU - Liu, L.
AU - Lopez-zaragoza, J.p.
AU - Maarschalkerweerd, R.
AU - Mance, D.
AU - Meshskar, N.
AU - Martín, V.
AU - Martin-polo, L.
AU - Martino, J.
AU - Martin-porqueras, F.
AU - Mateos, I.
AU - Mcnamara, P.w.
AU - Mendes, J.
AU - Mendes, L.
AU - Nofrarias, M.
AU - Paczkowski, S.
AU - Perreur-lloyd, M.
AU - Petiteau, A.
AU - Pivato, P.
AU - Plagnol, E.
AU - Ramos-castro, J.
AU - Reiche, J.
AU - Robertson, D.i.
AU - Rivas, F.
AU - Russano, G.
AU - Slutsky, J.
AU - Sopuerta, C.f.
AU - Sumner, T.
AU - Texier, D.
AU - Thorpe, J.i.
AU - Vetrugno, D.
AU - Vitale, S.
AU - Wanner, G.
AU - Ward, H.
AU - Wass, P.
AU - Weber, W.j.
AU - Wissel, L.
AU - Wittchen, A.
AU - Zweifel, P.
N1 - Funding information: This work has been made possible by the LISA Pathfinder mission, which is part of the space-science program of the European Space Agency. The French contribution has been supported by CNES (Accord Specific de Projet No. CNES 1316634/CNRS 103747), the CNRS, the Observatoire de Paris and the University Paris-Diderot. E. Plagnol and H. Inchauspé would also like to acknowledge the financial support of the UnivEarthS Labex program at Sorbonne Paris Cit (Grants No. ANR-10-LABX-0023 and No. ANR-11-IDEX-0005-02). The Albert-Einstein-Institut acknowledges the support of the German Space Agency, DLR. The work is supported by the Federal Ministry for Economic Affairs and Energy based on a resolution of the German Bundestag (Grants No. FKZ 50OQ0501 and No. FKZ 50OQ1601). The Italian contribution has been supported by Agenzia Spaziale Italiana and Instituto Nazionale di Fisica Nucleare. The Spanish contribution has been supported by Contracts No. AYA2010-15709 (MICINN), No. ESP2013-47637-P, and No. ESP2015-67234-P (MINECO). M. Nofrarias acknowledges support from Fundacion General CSIC Programa ComFuturo). F. Rivas acknowledges support from a Formacin de Personal Investigador (MINECO) contract. The Swiss contribution acknowledges the support of the Swiss Space Office (SSO) via the PRODEX Programme of ESA. L. Ferraioli acknowledges the support of the Swiss National Science Foundation. The UK groups wish to acknowledge support from the United Kingdom Space Agency (UKSA), the University of Glasgow, the University of Birmingham, Imperial College London, and the Scottish Universities Physics Alliance (SUPA). N. Korsakova would like to acknowledge the support of the Newton International Fellowship from the Royal Society. J. I. Thorpe and J. Slutsky acknowledge the support of the U.S. National Aeronautics and Space Administration (NASA). We acknowledge the NMDB database ( www.nmdb.eu ), founded under the European Union’s FP7 programme (contract no. 213007) for providing data. In addition, the Oulu NM station is operated by the University of Oulu with data available at http://cosmicrays.oulu.fi . We thank the ACE SWEPAM instrument team and the ACE Science Centre for providing the ACE data. The GOES data mentioned in this study can be obtained from the National Geophysical Data Centre at http://satdat.ngdc.noaa.gov/sem/goes/data/new_avg/ . The full Pathfinder radiation monitor dataset can be found at http://lpf.esac.esa.int/lpfsa/ . This work has been made possible by the LISA Pathfinder mission, which is part of the space-science program of the European Space Agency. The French contribution has been supported by CNES (Accord Specific de Projet No. CNES 1316634/CNRS 103747), the CNRS , the Observatoire de Paris and the University Paris-Diderot. E. Plagnol and H. Inchauspé would also like to acknowledge the financial support of the UnivEarthS Labex program at Sorbonne Paris Cit (Grants No. ANR-10-LABX-0023 and No. ANR-11-IDEX-0005-02 ). The Albert-Einstein-Institut acknowledges the support of the German Space Agency, DLR. The work is supported by the Federal Ministry for Economic Affairs and Energy based on a resolution of the German Bundestag (Grants No. FKZ 50OQ0501 and No. FKZ 50OQ1601 ). The Italian contribution has been supported by Agenzia Spaziale Italiana and Instituto Nazionale di Fisica Nucleare . The Spanish contribution has been supported by Contracts No. AYA2010-15709 ( MICINN ), No. ESP2013-47637-P , and No. ESP2015-67234-P ( MINECO ). M. Nofrarias acknowledges support from Fundacion General CSIC Programa ComFuturo). F. Rivas acknowledges support from a Formacin de Personal Investigador (MINECO) contract. The Swiss contribution acknowledges the support of the Swiss Space Office (SSO) via the PRODEX Programme of ESA. L. Ferraioli acknowledges the support of the Swiss National Science Foundation . The UK groups wish to acknowledge support from the United Kingdom Space Agency (UKSA), the University of Glasgow , the University of Birmingham , Imperial College London , and the Scottish Universities Physics Alliance (SUPA). N. Korsakova would like to acknowledge the support of the Newton International Fellowship from the Royal Society. J. I. Thorpe and J. Slutsky acknowledge the support of the U.S. National Aeronautics and Space Administration (NASA).
PY - 2018/3/1
Y1 - 2018/3/1
N2 - Test mass charging caused by cosmic rays will be a significant source of acceleration noise for space-based gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor made in situ measurements of the cosmic ray flux while also providing information about its energy spectrum. We describe the monitor and present measurements which show a gradual 40% increase in count rate coinciding with the declining phase of the solar cycle. Modulations of up to 10% were also observed with periods of 13 and 26 days that are associated with co-rotating interaction regions and heliospheric current sheet crossings. These variations in the flux above the monitor detection threshold (≈ 70 MeV) are shown to be coherent with measurements made by the IREM monitor on-board the Earth orbiting INTEGRAL spacecraft. Finally we use the measured deposited energy spectra, in combination with a GEANT4 model, to estimate the galactic cosmic ray differential energy spectrum over the course of the mission.
AB - Test mass charging caused by cosmic rays will be a significant source of acceleration noise for space-based gravitational wave detectors like LISA. Operating between December 2015 and July 2017, the technology demonstration mission LISA Pathfinder included a bespoke monitor to help characterise the relationship between test mass charging and the local radiation environment. The radiation monitor made in situ measurements of the cosmic ray flux while also providing information about its energy spectrum. We describe the monitor and present measurements which show a gradual 40% increase in count rate coinciding with the declining phase of the solar cycle. Modulations of up to 10% were also observed with periods of 13 and 26 days that are associated with co-rotating interaction regions and heliospheric current sheet crossings. These variations in the flux above the monitor detection threshold (≈ 70 MeV) are shown to be coherent with measurements made by the IREM monitor on-board the Earth orbiting INTEGRAL spacecraft. Finally we use the measured deposited energy spectra, in combination with a GEANT4 model, to estimate the galactic cosmic ray differential energy spectrum over the course of the mission.
KW - Charging
KW - GCR
KW - GEANT4
KW - LISA
KW - Pathfinder
KW - Radiation Monitor
UR - http://www.scopus.com/inward/record.url?scp=85041384466&partnerID=8YFLogxK
U2 - 10.1016/j.astropartphys.2018.01.006
DO - 10.1016/j.astropartphys.2018.01.006
M3 - Article
VL - 98
SP - 28
EP - 37
JO - Astroparticle physics
JF - Astroparticle physics
SN - 0927-6505
ER -