First radial velocity results from the MINiature Exoplanet Radial Velocity Array (MINERVA)
The MINiature Exoplanet Radial Velocity Array (MINERVA) is a dedicated observatory of four 0.7m robotic telescopes fiber-fed to a KiwiSpec spectrograph. The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combina...
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| creator | Wilson, Maurice L Eastman, Jason D Cornachione, Matthew A Wang, Sharon X Johnson, Samson A Sliski, David H Schap, William J Morton, Timothy D John Asher Johnson McCrady, Nate Wright, Jason T Wittenmyer, Robert A Plavchan, Peter Blake, Cullen H Swift, Jonathan J Bottom, Michael Baker, Ashley D Barnes, Stuart I Berlind, Perry Blackhurst, Eric Beatty, Thomas G Bolton, Adam S Bryson Cale Calkins, Michael L Colón, Ana de Vera, Jon Gilbert Esquerdo Falco, Emilio E tin, Pascal Garcia-Mejia, Juliana Geneser, Claire Gibson, Steven R Grell, Gabriel Groner, Ted Halverson, Samuel Hamlin, John Henderson, M Horner, J Houghton, Audrey Janssens, Stefaan Jonas, Graeme Jones, Damien Kirby, Annie Lawrence, George Luebbers, Julien Andrew Muirhead, Philip S Myles, Justin Nava, Chantanelle Rivera-García, Kevin O Reed, Tony Relles, Howard M Riddle, Reed Robinson, Connor est Chaput de Saintonge Sergi, Anthony |
| description | The MINiature Exoplanet Radial Velocity Array (MINERVA) is a dedicated observatory of four 0.7m robotic telescopes fiber-fed to a KiwiSpec spectrograph. The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combination of high precision and high cadence over long time periods. In this work, we detail changes to the MINERVA facility that have occurred since our previous paper. We then describe MINERVA's robotic control software, the process by which we perform 1D spectral extraction, and our forward modeling Doppler pipeline. In the process of improving our forward modeling procedure, we found that our spectrograph's intrinsic instrumental profile is stable for at least nine months. Because of that, we characterized our instrumental profile with a time-independent, cubic spline function based on the profile in the cross dispersion direction, with which we achieved a radial velocity precision similar to using a conventional "sum-of-Gaussians" instrumental profile: 1.8 m s\(^{-1}\) over 1.5 months on the RV standard star HD 122064. Therefore, we conclude that the instrumental profile need not be perfectly accurate as long as it is stable. In addition, we observed 51 Peg and our results are consistent with the literature, confirming our spectrograph and Doppler pipeline are producing accurate and precise radial velocities. |
| doi_str_mv | 10.48550/arxiv.1904.09991 |
| format | Article |
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The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combination of high precision and high cadence over long time periods. In this work, we detail changes to the MINERVA facility that have occurred since our previous paper. We then describe MINERVA's robotic control software, the process by which we perform 1D spectral extraction, and our forward modeling Doppler pipeline. In the process of improving our forward modeling procedure, we found that our spectrograph's intrinsic instrumental profile is stable for at least nine months. Because of that, we characterized our instrumental profile with a time-independent, cubic spline function based on the profile in the cross dispersion direction, with which we achieved a radial velocity precision similar to using a conventional "sum-of-Gaussians" instrumental profile: 1.8 m s\(^{-1}\) over 1.5 months on the RV standard star HD 122064. Therefore, we conclude that the instrumental profile need not be perfectly accurate as long as it is stable. In addition, we observed 51 Peg and our results are consistent with the literature, confirming our spectrograph and Doppler pipeline are producing accurate and precise radial velocities.</description><identifier>EISSN: 2331-8422</identifier><identifier>DOI: 10.48550/arxiv.1904.09991</identifier><language>eng</language><publisher>Ithaca: Cornell University Library, arXiv.org</publisher><subject>Circumstellar habitable zone ; Doppler effect ; Extrasolar planets ; Modelling ; Physics - Earth and Planetary Astrophysics ; Physics - Instrumentation and Methods for Astrophysics ; Radial velocity ; Robot control ; Spline functions ; Telescopes ; Velocity</subject><ispartof>arXiv.org, 2019-09</ispartof><rights>2019. This work is published under http://arxiv.org/licenses/nonexclusive-distrib/1.0/ (the “License”). 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Therefore, we conclude that the instrumental profile need not be perfectly accurate as long as it is stable. In addition, we observed 51 Peg and our results are consistent with the literature, confirming our spectrograph and Doppler pipeline are producing accurate and precise radial velocities.</description><subject>Circumstellar habitable zone</subject><subject>Doppler effect</subject><subject>Extrasolar planets</subject><subject>Modelling</subject><subject>Physics - Earth and Planetary Astrophysics</subject><subject>Physics - Instrumentation and Methods for Astrophysics</subject><subject>Radial velocity</subject><subject>Robot control</subject><subject>Spline 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The MINERVA mission is to discover super-Earths in the habitable zones of nearby stars. This can be accomplished with MINERVA's unique combination of high precision and high cadence over long time periods. In this work, we detail changes to the MINERVA facility that have occurred since our previous paper. We then describe MINERVA's robotic control software, the process by which we perform 1D spectral extraction, and our forward modeling Doppler pipeline. In the process of improving our forward modeling procedure, we found that our spectrograph's intrinsic instrumental profile is stable for at least nine months. Because of that, we characterized our instrumental profile with a time-independent, cubic spline function based on the profile in the cross dispersion direction, with which we achieved a radial velocity precision similar to using a conventional "sum-of-Gaussians" instrumental profile: 1.8 m s\(^{-1}\) over 1.5 months on the RV standard star HD 122064. 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| fulltext | fulltext |
| identifier | EISSN: 2331-8422 |
| ispartof | arXiv.org, 2019-09 |
| issn | 2331-8422 |
| language | eng |
| recordid | cdi_arxiv_primary_1904_09991 |
| source | arXiv.org; Free E- Journals |
| subjects | Circumstellar habitable zone Doppler effect Extrasolar planets Modelling Physics - Earth and Planetary Astrophysics Physics - Instrumentation and Methods for Astrophysics Radial velocity Robot control Spline functions Telescopes Velocity |
| title | First radial velocity results from the MINiature Exoplanet Radial Velocity Array (MINERVA) |
| url | https://sfx.bib-bvb.de/sfx_tum?ctx_ver=Z39.88-2004&ctx_enc=info:ofi/enc:UTF-8&ctx_tim=2025-01-19T05%3A15%3A50IST&url_ver=Z39.88-2004&url_ctx_fmt=infofi/fmt:kev:mtx:ctx&rfr_id=info:sid/primo.exlibrisgroup.com:primo3-Article-proquest_arxiv&rft_val_fmt=info:ofi/fmt:kev:mtx:journal&rft.genre=article&rft.atitle=First%20radial%20velocity%20results%20from%20the%20MINiature%20Exoplanet%20Radial%20Velocity%20Array%20(MINERVA)&rft.jtitle=arXiv.org&rft.au=Wilson,%20Maurice%20L&rft.date=2019-09-11&rft.eissn=2331-8422&rft_id=info:doi/10.48550/arxiv.1904.09991&rft_dat=%3Cproquest_arxiv%3E2213627751%3C/proquest_arxiv%3E%3Curl%3E%3C/url%3E&disable_directlink=true&sfx.directlink=off&sfx.report_link=0&rft_id=info:oai/&rft_pqid=2213627751&rft_id=info:pmid/&rfr_iscdi=true |