SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

P. Lognonné; W. B. Banerdt; D. Giardini; W. T. Pike; U. Christensen; P. Laudet; S. de Raucourt; P. Zweifel; S. Calcutt; M. Bierwirth; K. J. Hurst; F. Ijpelaan; J. W. Umland; R. Llorca-Cejudo; S. A. Larson; R. F. Garcia; S. Kedar; B. Knapmeyer-Endrun; D. Mimoun; A. Mocquet; M. P. Panning; R. C. Weber; A. Sylvestre-Baron; G. Pont; N. Verdier; L. Kerjean; L. J. Facto; V. Gharakanian; J. E. Feldman; T. L. Hoffman; D. B. Klein; K. Klein; N. P. Onufer; J. Paredes-Garcia; M. P. Petkov; J. R. Willis; S. E. Smrekar; M. Drilleau; T. Gabsi; T. Nebut; O. Robert; S. Tillier; C. Moreau; M. Parise; G. Aveni; S. Ben Charef; Y. Bennour; T. Camus; P. A. Dandonneau; C. Desfoux; B. Lecomte; O. Pot; P. Revuz; D. Mance; J. tenPierick; N. E. Bowles; C. Charalambous; A. K. Delahunty; J. Hurley; R. Irshad; Huafeng Liu; A. G. Mukherjee; I. M. Standley; A. E. Stott; J. Temple; T. Warren; M. Eberhardt; A. Kramer; W. Kühne; E. P. Miettinen; M. Monecke; C. Aicardi; M. André; J. Baroukh; A. Borrien; A. Bouisset; P. Boutte; K. Brethomé; C. Brysbaert; T. Carlier; M. Deleuze; J. M. Desmarres; D. Dilhan; C. Doucet; D. Faye; N. Faye-Refalo; R. Gonzalez; C. Imbert; C. Larigauderie; E. Locatelli; L. Luno; J. R. Meyer; F. Mialhe; J. M. Mouret; M. Nonon; Y. Pahn; A. Paillet; P. Pasquier; G. Perez; R. Perez; L. Perrin; B. Pouilloux; A. Rosak; I. Savin de Larclause; J. Sicre; M. Sodki; N. Toulemont; B. Vella; C. Yana; F. Alibay; O. M. Avalos; M. A. Balzer; P. Bhandari; E. Blanco; B. D. Bone; J. C. Bousman; P. Bruneau; F. J. Calef; R. J. Calvet; S. A. D’Agostino; G. de los Santos; R. G. Deen; R. W. Denise; J. Ervin; N. W. Ferraro; H. E. Gengl; F. Grinblat; D. Hernandez; M. Hetzel; M. E. Johnson; L. Khachikyan; J. Y. Lin; S. M. Madzunkov; S. L. Marshall; I. G. Mikellides; E. A. Miller; W. Raff; J. E. Singer; C. M. Sunday; J. F. Villalvazo; M. C. Wallace; D. Banfield; J. A. Rodriguez-Manfredi; C. T. Russell; A. Trebi-Ollennu; J. N. Maki; E. Beucler; M. Böse; C. Bonjour; J. L. Berenguer; S. Ceylan; J. Clinton; V. Conejero; I. Daubar; V. Dehant; P. Delage; F. Euchner; I. Estève; L. Fayon; L. Ferraioli; C. L. Johnson; J. Gagnepain-Beyneix; M. Golombek; A. Khan; T. Kawamura; B. Kenda; P. Labrot; N. Murdoch; C. Pardo; C. Perrin; L. Pou; A. Sauron; D. Savoie; S. Stähler; E. Stutzmann; N. A. Teanby; Jeroen Tromp; M. van Driel; M. Wieczorek; R. Widmer-Schnidrig; J. Wookey

doi:10.1007/s11214-018-0574-6

SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

P. Lognonné, W. B. Banerdt, D. Giardini, W. T. Pike, U. Christensen, P. Laudet, S. de Raucourt, P. Zweifel, S. Calcutt, M. Bierwirth, K. J. Hurst, F. Ijpelaan, J. W. Umland, R. Llorca-Cejudo, S. A. Larson, R. F. Garcia, S. Kedar, B. Knapmeyer-Endrun, D. Mimoun, A. MocquetM. P. Panning, R. C. Weber, A. Sylvestre-Baron, G. Pont, N. Verdier, L. Kerjean, L. J. Facto, V. Gharakanian, J. E. Feldman, T. L. Hoffman, D. B. Klein, K. Klein, N. P. Onufer, J. Paredes-Garcia, M. P. Petkov, J. R. Willis, S. E. Smrekar, M. Drilleau, T. Gabsi, T. Nebut, O. Robert, S. Tillier, C. Moreau, M. Parise, G. Aveni, S. Ben Charef, Y. Bennour, T. Camus, P. A. Dandonneau, C. Desfoux, B. Lecomte, O. Pot, P. Revuz, D. Mance, J. tenPierick, N. E. Bowles, C. Charalambous, A. K. Delahunty, J. Hurley, R. Irshad, Huafeng Liu, A. G. Mukherjee, I. M. Standley, A. E. Stott, J. Temple, T. Warren, M. Eberhardt, A. Kramer, W. Kühne, E. P. Miettinen, M. Monecke, C. Aicardi, M. André, J. Baroukh, A. Borrien, A. Bouisset, P. Boutte, K. Brethomé, C. Brysbaert, T. Carlier, M. Deleuze, J. M. Desmarres, D. Dilhan, C. Doucet, D. Faye, N. Faye-Refalo, R. Gonzalez, C. Imbert, C. Larigauderie, E. Locatelli, L. Luno, J. R. Meyer, F. Mialhe, J. M. Mouret, M. Nonon, Y. Pahn, A. Paillet, P. Pasquier, G. Perez, R. Perez, L. Perrin, B. Pouilloux, A. Rosak, I. Savin de Larclause, J. Sicre, M. Sodki, N. Toulemont, B. Vella, C. Yana, F. Alibay, O. M. Avalos, M. A. Balzer, P. Bhandari, E. Blanco, B. D. Bone, J. C. Bousman, P. Bruneau, F. J. Calef, R. J. Calvet, S. A. D’Agostino, G. de los Santos, R. G. Deen, R. W. Denise, J. Ervin, N. W. Ferraro, H. E. Gengl, F. Grinblat, D. Hernandez, M. Hetzel, M. E. Johnson, L. Khachikyan, J. Y. Lin, S. M. Madzunkov, S. L. Marshall, I. G. Mikellides, E. A. Miller, W. Raff, J. E. Singer, C. M. Sunday, J. F. Villalvazo, M. C. Wallace, D. Banfield, J. A. Rodriguez-Manfredi, C. T. Russell, A. Trebi-Ollennu, J. N. Maki, E. Beucler, M. Böse, C. Bonjour, J. L. Berenguer, S. Ceylan, J. Clinton, V. Conejero, I. Daubar, V. Dehant, P. Delage, F. Euchner, I. Estève, L. Fayon, L. Ferraioli, C. L. Johnson, J. Gagnepain-Beyneix, M. Golombek, A. Khan, T. Kawamura, B. Kenda, P. Labrot, N. Murdoch, C. Pardo, C. Perrin, L. Pou, A. Sauron, D. Savoie, S. Stähler, E. Stutzmann, N. A. Teanby, Jeroen Tromp, M. van Driel, M. Wieczorek, R. Widmer-Schnidrig, J. Wookey

Research output: Contribution to journal › Review article › peer-review

202 Scopus citations

Abstract

By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of M _w ∼ 3 at 40 ^∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.

Original language	English (US)
Article number	12
Journal	Space Science Reviews
Volume	215
Issue number	1
DOIs	https://doi.org/10.1007/s11214-018-0574-6
State	Published - Jan 1 2019

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

InSight
Mars seismology

Access to Document

10.1007/s11214-018-0574-6

Cite this

Lognonné, P., Banerdt, W. B., Giardini, D., Pike, W. T., Christensen, U., Laudet, P., de Raucourt, S., Zweifel, P., Calcutt, S., Bierwirth, M., Hurst, K. J., Ijpelaan, F., Umland, J. W., Llorca-Cejudo, R., Larson, S. A., Garcia, R. F., Kedar, S., Knapmeyer-Endrun, B., Mimoun, D., ... Wookey, J. (2019). SEIS: Insight’s Seismic Experiment for Internal Structure of Mars. Space Science Reviews, 215(1), [12]. https://doi.org/10.1007/s11214-018-0574-6

@article{88fce7083d314670b72db953d11bef46,

title = "SEIS: Insight{\textquoteright}s Seismic Experiment for Internal Structure of Mars",

abstract = " By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars{\textquoteright} surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking{\textquoteright}s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars{\textquoteright} surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of M w ∼ 3 at 40 ∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.",

keywords = "InSight, Mars seismology",

author = "P. Lognonn{\'e} and Banerdt, {W. B.} and D. Giardini and Pike, {W. T.} and U. Christensen and P. Laudet and {de Raucourt}, S. and P. Zweifel and S. Calcutt and M. Bierwirth and Hurst, {K. J.} and F. Ijpelaan and Umland, {J. W.} and R. Llorca-Cejudo and Larson, {S. A.} and Garcia, {R. F.} and S. Kedar and B. Knapmeyer-Endrun and D. Mimoun and A. Mocquet and Panning, {M. P.} and Weber, {R. C.} and A. Sylvestre-Baron and G. Pont and N. Verdier and L. Kerjean and Facto, {L. J.} and V. Gharakanian and Feldman, {J. E.} and Hoffman, {T. L.} and Klein, {D. B.} and K. Klein and Onufer, {N. P.} and J. Paredes-Garcia and Petkov, {M. P.} and Willis, {J. R.} and Smrekar, {S. E.} and M. Drilleau and T. Gabsi and T. Nebut and O. Robert and S. Tillier and C. Moreau and M. Parise and G. Aveni and {Ben Charef}, S. and Y. Bennour and T. Camus and Dandonneau, {P. A.} and C. Desfoux and B. Lecomte and O. Pot and P. Revuz and D. Mance and J. tenPierick and Bowles, {N. E.} and C. Charalambous and Delahunty, {A. K.} and J. Hurley and R. Irshad and Huafeng Liu and Mukherjee, {A. G.} and Standley, {I. M.} and Stott, {A. E.} and J. Temple and T. Warren and M. Eberhardt and A. Kramer and W. K{\"u}hne and Miettinen, {E. P.} and M. Monecke and C. Aicardi and M. Andr{\'e} and J. Baroukh and A. Borrien and A. Bouisset and P. Boutte and K. Brethom{\'e} and C. Brysbaert and T. Carlier and M. Deleuze and Desmarres, {J. M.} and D. Dilhan and C. Doucet and D. Faye and N. Faye-Refalo and R. Gonzalez and C. Imbert and C. Larigauderie and E. Locatelli and L. Luno and Meyer, {J. R.} and F. Mialhe and Mouret, {J. M.} and M. Nonon and Y. Pahn and A. Paillet and P. Pasquier and G. Perez and R. Perez and L. Perrin and B. Pouilloux and A. Rosak and {Savin de Larclause}, I. and J. Sicre and M. Sodki and N. Toulemont and B. Vella and C. Yana and F. Alibay and Avalos, {O. M.} and Balzer, {M. A.} and P. Bhandari and E. Blanco and Bone, {B. D.} and Bousman, {J. C.} and P. Bruneau and Calef, {F. J.} and Calvet, {R. J.} and D{\textquoteright}Agostino, {S. A.} and {de los Santos}, G. and Deen, {R. G.} and Denise, {R. W.} and J. Ervin and Ferraro, {N. W.} and Gengl, {H. E.} and F. Grinblat and D. Hernandez and M. Hetzel and Johnson, {M. E.} and L. Khachikyan and Lin, {J. Y.} and Madzunkov, {S. M.} and Marshall, {S. L.} and Mikellides, {I. G.} and Miller, {E. A.} and W. Raff and Singer, {J. E.} and Sunday, {C. M.} and Villalvazo, {J. F.} and Wallace, {M. C.} and D. Banfield and Rodriguez-Manfredi, {J. A.} and Russell, {C. T.} and A. Trebi-Ollennu and Maki, {J. N.} and E. Beucler and M. B{\"o}se and C. Bonjour and Berenguer, {J. L.} and S. Ceylan and J. Clinton and V. Conejero and I. Daubar and V. Dehant and P. Delage and F. Euchner and I. Est{\`e}ve and L. Fayon and L. Ferraioli and Johnson, {C. L.} and J. Gagnepain-Beyneix and M. Golombek and A. Khan and T. Kawamura and B. Kenda and P. Labrot and N. Murdoch and C. Pardo and C. Perrin and L. Pou and A. Sauron and D. Savoie and S. St{\"a}hler and E. Stutzmann and Teanby, {N. A.} and Jeroen Tromp and {van Driel}, M. and M. Wieczorek and R. Widmer-Schnidrig and J. Wookey",

note = "Funding Information: The French team acknowledges and thanks all contractors and industrial partners who have contributed to the EC/VBB/VBB Electronics/cradle subsystems and associated tests through industrial contracts (SODERN, EREMS. DELTAPRESI, MICROCERTEC, AIRBUS DS, SMAC, MECANO ID). IMAGO and VR2PLANET contributed also to the SEIS portal and outreach VR tools. CNES Toulouse team acknowledges and thanks the contractors having supported integration and environment tests (ALTEN SUD OUEST, LOGI-QUAL ET ALTRAN, XLM, EPSILON, THALES SERVICE, LANAGRAM), performance tests (ATELIER IMAGES, R-TECH, ASSYSTEM, AKKA, VERITAS) and SISMOC (CS, CAPGEMINI). IPGP technical team acknowledges and thanks collaborators who provided support at IPGP{\textquoteright}s Observatoire de Saint Maur (D. Baillivet, C. Choque Cortez, F. Rolfo, A. Simonin from ALTRAN, R. Crane from ASSYSTEM and M.A. Desnos, O. Mbeumou from NEXEYA). Additional support to IPGP was provided by IRAP for VBB proximity electronics packaging and from ENPC/Navier for SEIS feet design. IPGP VBB team acknowledges also those who contributed to the early design of the VBBs prior InSight, especially J.F. Karczewski, S. Cacho, C. Cavoit and P. Schibler and E. Wielandt for fruitful advice. Funding Information: The Swiss contribution in implementation of the SEIS electronics was made possible through funding from the federal Swiss Space Office (SSO), the contractual and technical support of the ESA-PRODEX office and the industrial contractor SYDERAL SA. We thank in particular A. Werthm{\"u}ller (SSO), C. Bramanti (ESA) and C/Barraud (SYDERAL) for their strong contribution to the successful completion of the SEIS EBox. The Marsquake service was partly supported by funding from the (1) Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 “Seismology on Mars”) and the (2) Swiss State Secretariat for Education, Research and Innovation (SEFRI project “MarsQuake Service— Preparatory Phase”). Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s682. Funding Information: Funding of all subsystems has been made without fund transfer and has been therefore supported by the French (CNES), US (NASA within JPL Discovery contract), German (DLR), Swiss (SSO) and UK (UKSA) space agencies. Additional human resources support has been made by the national academic and research organizations. See details in the Acknowledgement section. CNES has in addition done the overall project management and ESA has managed the Swiss ETHZ contribution through PRODEX. Funding Information: The French Team acknowledge the French Space Agency CNES which as supported and funded all SEIS related contracts and CNES employees. Very large human resource support has been also provided by the Centre National de la Recherche Scientifique (CNRS), by Institut National des Sciences de l{\textquoteright}Univers (INSU) for contract administrative management and by several French Universities or Engineer Schools, including Universit{\'e} Paris Diderot, Institut de Physique du Globe de Paris, Institut National de l{\textquoteright}A{\'e}onautique et de l{\textquoteright}Espace/Supaero. The cleaning of all VBBs have been performed by IPGP with support of IMPMC in the clean rooms of the Paris Diderot Space Campus funded by the Ile de France under the SESAME project “Pole Terre-Plan{\`e}tes”, while the cold test have been performed in facilities funded by CNES and Ile de France under SESAME project “Centre de Simulation Martien”. Extra scientific support of the French SEIS team has been provided by ANR under the ANR SEISMARS project, by UnivEarthS Labex program (ANR-10-LABX-0023), IDEX Sorbonne Paris Cit{\'e} (ANR-11-IDEX-0005-0) and by GENCI (A0030407341) for supercomputing resource. P. Lognonn{\'e} acknowledges the long support of CNES and of R. Bonneville, F. Rocard and especially F. Casolli, as well as CNRS and the Institut Universitaire de France for extra support enabling full dedication to the SEIS project during the critical implementation time. Funding Information: The MPS SEIS team acknowledges the funding for the SEIS Leveling system development by the DLR German Space Agency. SEIS-SP development and delivery were funded by the UK Space Agency. Publisher Copyright: {\textcopyright} 2019, The Author(s).",

year = "2019",

month = jan,

day = "1",

doi = "10.1007/s11214-018-0574-6",

language = "English (US)",

volume = "215",

journal = "Space Science Reviews",

issn = "0038-6308",

publisher = "Springer Netherlands",

number = "1",

}

Lognonné, P, Banerdt, WB, Giardini, D, Pike, WT, Christensen, U, Laudet, P, de Raucourt, S, Zweifel, P, Calcutt, S, Bierwirth, M, Hurst, KJ, Ijpelaan, F, Umland, JW, Llorca-Cejudo, R, Larson, SA, Garcia, RF, Kedar, S, Knapmeyer-Endrun, B, Mimoun, D, Mocquet, A, Panning, MP, Weber, RC, Sylvestre-Baron, A, Pont, G, Verdier, N, Kerjean, L, Facto, LJ, Gharakanian, V, Feldman, JE, Hoffman, TL, Klein, DB, Klein, K, Onufer, NP, Paredes-Garcia, J, Petkov, MP, Willis, JR, Smrekar, SE, Drilleau, M, Gabsi, T, Nebut, T, Robert, O, Tillier, S, Moreau, C, Parise, M, Aveni, G, Ben Charef, S, Bennour, Y, Camus, T, Dandonneau, PA, Desfoux, C, Lecomte, B, Pot, O, Revuz, P, Mance, D, tenPierick, J, Bowles, NE, Charalambous, C, Delahunty, AK, Hurley, J, Irshad, R, Liu, H, Mukherjee, AG, Standley, IM, Stott, AE, Temple, J, Warren, T, Eberhardt, M, Kramer, A, Kühne, W, Miettinen, EP, Monecke, M, Aicardi, C, André, M, Baroukh, J, Borrien, A, Bouisset, A, Boutte, P, Brethomé, K, Brysbaert, C, Carlier, T, Deleuze, M, Desmarres, JM, Dilhan, D, Doucet, C, Faye, D, Faye-Refalo, N, Gonzalez, R, Imbert, C, Larigauderie, C, Locatelli, E, Luno, L, Meyer, JR, Mialhe, F, Mouret, JM, Nonon, M, Pahn, Y, Paillet, A, Pasquier, P, Perez, G, Perez, R, Perrin, L, Pouilloux, B, Rosak, A, Savin de Larclause, I, Sicre, J, Sodki, M, Toulemont, N, Vella, B, Yana, C, Alibay, F, Avalos, OM, Balzer, MA, Bhandari, P, Blanco, E, Bone, BD, Bousman, JC, Bruneau, P, Calef, FJ, Calvet, RJ, D’Agostino, SA, de los Santos, G, Deen, RG, Denise, RW, Ervin, J, Ferraro, NW, Gengl, HE, Grinblat, F, Hernandez, D, Hetzel, M, Johnson, ME, Khachikyan, L, Lin, JY, Madzunkov, SM, Marshall, SL, Mikellides, IG, Miller, EA, Raff, W, Singer, JE, Sunday, CM, Villalvazo, JF, Wallace, MC, Banfield, D, Rodriguez-Manfredi, JA, Russell, CT, Trebi-Ollennu, A, Maki, JN, Beucler, E, Böse, M, Bonjour, C, Berenguer, JL, Ceylan, S, Clinton, J, Conejero, V, Daubar, I, Dehant, V, Delage, P, Euchner, F, Estève, I, Fayon, L, Ferraioli, L, Johnson, CL, Gagnepain-Beyneix, J, Golombek, M, Khan, A, Kawamura, T, Kenda, B, Labrot, P, Murdoch, N, Pardo, C, Perrin, C, Pou, L, Sauron, A, Savoie, D, Stähler, S, Stutzmann, E, Teanby, NA, Tromp, J, van Driel, M, Wieczorek, M, Widmer-Schnidrig, R & Wookey, J 2019, 'SEIS: Insight’s Seismic Experiment for Internal Structure of Mars', Space Science Reviews, vol. 215, no. 1, 12. https://doi.org/10.1007/s11214-018-0574-6

TY - JOUR

T1 - SEIS

T2 - Insight’s Seismic Experiment for Internal Structure of Mars

AU - Lognonné, P.

AU - Banerdt, W. B.

AU - Giardini, D.

AU - Pike, W. T.

AU - Christensen, U.

AU - Laudet, P.

AU - de Raucourt, S.

AU - Zweifel, P.

AU - Calcutt, S.

AU - Bierwirth, M.

AU - Hurst, K. J.

AU - Ijpelaan, F.

AU - Umland, J. W.

AU - Llorca-Cejudo, R.

AU - Larson, S. A.

AU - Garcia, R. F.

AU - Kedar, S.

AU - Knapmeyer-Endrun, B.

AU - Mimoun, D.

AU - Mocquet, A.

AU - Panning, M. P.

AU - Weber, R. C.

AU - Sylvestre-Baron, A.

AU - Pont, G.

AU - Verdier, N.

AU - Kerjean, L.

AU - Facto, L. J.

AU - Gharakanian, V.

AU - Feldman, J. E.

AU - Hoffman, T. L.

AU - Klein, D. B.

AU - Klein, K.

AU - Onufer, N. P.

AU - Paredes-Garcia, J.

AU - Petkov, M. P.

AU - Willis, J. R.

AU - Smrekar, S. E.

AU - Drilleau, M.

AU - Gabsi, T.

AU - Nebut, T.

AU - Robert, O.

AU - Tillier, S.

AU - Moreau, C.

AU - Parise, M.

AU - Aveni, G.

AU - Ben Charef, S.

AU - Bennour, Y.

AU - Camus, T.

AU - Dandonneau, P. A.

AU - Desfoux, C.

AU - Lecomte, B.

AU - Pot, O.

AU - Revuz, P.

AU - Mance, D.

AU - tenPierick, J.

AU - Bowles, N. E.

AU - Charalambous, C.

AU - Delahunty, A. K.

AU - Hurley, J.

AU - Irshad, R.

AU - Liu, Huafeng

AU - Mukherjee, A. G.

AU - Standley, I. M.

AU - Stott, A. E.

AU - Temple, J.

AU - Warren, T.

AU - Eberhardt, M.

AU - Kramer, A.

AU - Kühne, W.

AU - Miettinen, E. P.

AU - Monecke, M.

AU - Aicardi, C.

AU - André, M.

AU - Baroukh, J.

AU - Borrien, A.

AU - Bouisset, A.

AU - Boutte, P.

AU - Brethomé, K.

AU - Brysbaert, C.

AU - Carlier, T.

AU - Deleuze, M.

AU - Desmarres, J. M.

AU - Dilhan, D.

AU - Doucet, C.

AU - Faye, D.

AU - Faye-Refalo, N.

AU - Gonzalez, R.

AU - Imbert, C.

AU - Larigauderie, C.

AU - Locatelli, E.

AU - Luno, L.

AU - Meyer, J. R.

AU - Mialhe, F.

AU - Mouret, J. M.

AU - Nonon, M.

AU - Pahn, Y.

AU - Paillet, A.

AU - Pasquier, P.

AU - Perez, G.

AU - Perez, R.

AU - Perrin, L.

AU - Pouilloux, B.

AU - Rosak, A.

AU - Savin de Larclause, I.

AU - Sicre, J.

AU - Sodki, M.

AU - Toulemont, N.

AU - Vella, B.

AU - Yana, C.

AU - Alibay, F.

AU - Avalos, O. M.

AU - Balzer, M. A.

AU - Bhandari, P.

AU - Blanco, E.

AU - Bone, B. D.

AU - Bousman, J. C.

AU - Bruneau, P.

AU - Calef, F. J.

AU - Calvet, R. J.

AU - D’Agostino, S. A.

AU - de los Santos, G.

AU - Deen, R. G.

AU - Denise, R. W.

AU - Ervin, J.

AU - Ferraro, N. W.

AU - Gengl, H. E.

AU - Grinblat, F.

AU - Hernandez, D.

AU - Hetzel, M.

AU - Johnson, M. E.

AU - Khachikyan, L.

AU - Lin, J. Y.

AU - Madzunkov, S. M.

AU - Marshall, S. L.

AU - Mikellides, I. G.

AU - Miller, E. A.

AU - Raff, W.

AU - Singer, J. E.

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N1 - Funding Information: The French team acknowledges and thanks all contractors and industrial partners who have contributed to the EC/VBB/VBB Electronics/cradle subsystems and associated tests through industrial contracts (SODERN, EREMS. DELTAPRESI, MICROCERTEC, AIRBUS DS, SMAC, MECANO ID). IMAGO and VR2PLANET contributed also to the SEIS portal and outreach VR tools. CNES Toulouse team acknowledges and thanks the contractors having supported integration and environment tests (ALTEN SUD OUEST, LOGI-QUAL ET ALTRAN, XLM, EPSILON, THALES SERVICE, LANAGRAM), performance tests (ATELIER IMAGES, R-TECH, ASSYSTEM, AKKA, VERITAS) and SISMOC (CS, CAPGEMINI). IPGP technical team acknowledges and thanks collaborators who provided support at IPGP’s Observatoire de Saint Maur (D. Baillivet, C. Choque Cortez, F. Rolfo, A. Simonin from ALTRAN, R. Crane from ASSYSTEM and M.A. Desnos, O. Mbeumou from NEXEYA). Additional support to IPGP was provided by IRAP for VBB proximity electronics packaging and from ENPC/Navier for SEIS feet design. IPGP VBB team acknowledges also those who contributed to the early design of the VBBs prior InSight, especially J.F. Karczewski, S. Cacho, C. Cavoit and P. Schibler and E. Wielandt for fruitful advice. Funding Information: The Swiss contribution in implementation of the SEIS electronics was made possible through funding from the federal Swiss Space Office (SSO), the contractual and technical support of the ESA-PRODEX office and the industrial contractor SYDERAL SA. We thank in particular A. Werthmüller (SSO), C. Bramanti (ESA) and C/Barraud (SYDERAL) for their strong contribution to the successful completion of the SEIS EBox. The Marsquake service was partly supported by funding from the (1) Swiss National Science Foundation and French Agence Nationale de la Recherche (SNF-ANR project 157133 “Seismology on Mars”) and the (2) Swiss State Secretariat for Education, Research and Innovation (SEFRI project “MarsQuake Service— Preparatory Phase”). Additional support came from the Swiss National Supercomputing Centre (CSCS) under project ID s682. Funding Information: Funding of all subsystems has been made without fund transfer and has been therefore supported by the French (CNES), US (NASA within JPL Discovery contract), German (DLR), Swiss (SSO) and UK (UKSA) space agencies. Additional human resources support has been made by the national academic and research organizations. See details in the Acknowledgement section. CNES has in addition done the overall project management and ESA has managed the Swiss ETHZ contribution through PRODEX. Funding Information: The French Team acknowledge the French Space Agency CNES which as supported and funded all SEIS related contracts and CNES employees. Very large human resource support has been also provided by the Centre National de la Recherche Scientifique (CNRS), by Institut National des Sciences de l’Univers (INSU) for contract administrative management and by several French Universities or Engineer Schools, including Université Paris Diderot, Institut de Physique du Globe de Paris, Institut National de l’Aéonautique et de l’Espace/Supaero. The cleaning of all VBBs have been performed by IPGP with support of IMPMC in the clean rooms of the Paris Diderot Space Campus funded by the Ile de France under the SESAME project “Pole Terre-Planètes”, while the cold test have been performed in facilities funded by CNES and Ile de France under SESAME project “Centre de Simulation Martien”. Extra scientific support of the French SEIS team has been provided by ANR under the ANR SEISMARS project, by UnivEarthS Labex program (ANR-10-LABX-0023), IDEX Sorbonne Paris Cité (ANR-11-IDEX-0005-0) and by GENCI (A0030407341) for supercomputing resource. P. Lognonné acknowledges the long support of CNES and of R. Bonneville, F. Rocard and especially F. Casolli, as well as CNRS and the Institut Universitaire de France for extra support enabling full dedication to the SEIS project during the critical implementation time. Funding Information: The MPS SEIS team acknowledges the funding for the SEIS Leveling system development by the DLR German Space Agency. SEIS-SP development and delivery were funded by the UK Space Agency. Publisher Copyright: © 2019, The Author(s).

PY - 2019/1/1

Y1 - 2019/1/1

N2 - By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of M w ∼ 3 at 40 ∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.

AB - By the end of 2018, 42 years after the landing of the two Viking seismometers on Mars, InSight will deploy onto Mars’ surface the SEIS (Seismic Experiment for Internal Structure) instrument; a six-axes seismometer equipped with both a long-period three-axes Very Broad Band (VBB) instrument and a three-axes short-period (SP) instrument. These six sensors will cover a broad range of the seismic bandwidth, from 0.01 Hz to 50 Hz, with possible extension to longer periods. Data will be transmitted in the form of three continuous VBB components at 2 sample per second (sps), an estimation of the short period energy content from the SP at 1 sps and a continuous compound VBB/SP vertical axis at 10 sps. The continuous streams will be augmented by requested event data with sample rates from 20 to 100 sps. SEIS will improve upon the existing resolution of Viking’s Mars seismic monitoring by a factor of ∼ 2500 at 1 Hz and ∼200000 at 0.1 Hz. An additional major improvement is that, contrary to Viking, the seismometers will be deployed via a robotic arm directly onto Mars’ surface and will be protected against temperature and wind by highly efficient thermal and wind shielding. Based on existing knowledge of Mars, it is reasonable to infer a moment magnitude detection threshold of M w ∼ 3 at 40 ∘ epicentral distance and a potential to detect several tens of quakes and about five impacts per year. In this paper, we first describe the science goals of the experiment and the rationale used to define its requirements. We then provide a detailed description of the hardware, from the sensors to the deployment system and associated performance, including transfer functions of the seismic sensors and temperature sensors. We conclude by describing the experiment ground segment, including data processing services, outreach and education networks and provide a description of the format to be used for future data distribution.

KW - InSight

KW - Mars seismology

UR - http://www.scopus.com/inward/record.url?scp=85060754712&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=85060754712&partnerID=8YFLogxK

U2 - 10.1007/s11214-018-0574-6

DO - 10.1007/s11214-018-0574-6

M3 - Review article

C2 - 30880848

AN - SCOPUS:85060754712

SN - 0038-6308

VL - 215

JO - Space Science Reviews

JF - Space Science Reviews

IS - 1

M1 - 12

ER -

SEIS: Insight’s Seismic Experiment for Internal Structure of Mars

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