First Radial Velocity Results From the MINiature Exoplanet Radial Velocity Array (MINERVA)

Wilson, Maurice L. and Eastman, Jason D. and Cornachione, Matthew A. and Wang, Sharon X. and Johnson, Samson A. and Sliski, David H. and Schap, William J., III and Morton, Timothy D. and Johnson, John Asher and McCrady, Nate and Wright, Jason T. and Wittenmyer, Robert A. and Plavchan, Peter and Blake, Cullen H. and Swift, Jonathan J. and Bottom, Michael and Baker, Ashley D. and Barnes, Stuart I. and Berlind, Perry and Blackhurst, Eric and Beatty, Thomas G. and Bolton, Adam S. and Cale, Bryson and Calkins, Michael L. and Colon, Ana and de Vera, Jon and Esquerdo, Gilbert and Falco, Emilio E. and Fortin, Pascal and Garcia-Mejia, Juliana and Geneser, Claire and Gibson, Steven R. and Grell, Gabriel and Groner, Ted and Halverson, Samuel and Hamlin, John and Henderson, M. and Horner, J. and Houghton, Audrey and Janssens, Stefaan and Jonas, Graeme and Jones, Damien and Kirby, Annie and Lawrence, George and Luebbers, Julien Andrew and Muirhead, Philip S. and Myles, Justin and Nava, Chantanelle and Rivera-García, Kevin O. and Reed, Tony and Relles, Howard M. and Riddle, Reed and Robinson, Connor and Chaput de Saintonge, Forest and Sergi, Anthony (2019) First Radial Velocity Results From the MINiature Exoplanet Radial Velocity Array (MINERVA). Publications of the Astronomical Society of the Pacific, 131 (1005). pp. 1-19. ISSN 0004-6280

Abstract

The MINiature Exoplanet Radial Velocity Array (MINERVA) is a dedicated observatory of four 0.7 m 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<SUP>-1</SUP> 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.


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Item Type: Article (Commonwealth Reporting Category C)
Refereed: Yes
Item Status: Live Archive
Additional Information: Files associated with this item cannot be displayed due to copyright restrictions.
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Faculty/School / Institute/Centre: Current - Institute for Advanced Engineering and Space Sciences - Centre for Astrophysics (1 Aug 2018 -)
Date Deposited: 24 Jan 2020 06:55
Last Modified: 07 Feb 2020 01:32
Uncontrolled Keywords: Astrophysics - Instrumentation and Methods for Astrophysics; Astrophysics - Earth and Planetary Astrophysics
Fields of Research : 02 Physical Sciences > 0201 Astronomical and Space Sciences > 020110 Stellar Astronomy and Planetary Systems
Socio-Economic Objective: E Expanding Knowledge > 97 Expanding Knowledge > 970102 Expanding Knowledge in the Physical Sciences
Identification Number or DOI: 10.1088/1538-3873/ab33c5
URI: http://eprints.usq.edu.au/id/eprint/37413

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