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Extreme Precision Radial Velociites to appear in PASP Preprint typeset using LAT X style emulateapj v. 01/23/15 E 1 STATE OF THE FIELD: EXTREME PRECISION RADIAL VELOCITIES Debra A. Fischer2, Guillem Anglada-Escude3, 4, Pamela Arriagada5, Roman V. Baluev6,7, Jacob L. Bean8, Francois Bouchy9, Lars A. Buchhave10, Thorsten Carroll11, Abhijit Chakraborty12, Justin R. Crepp13, Rebekah I. Dawson14,15, Scott A. Diddams16, 17, Xavier Dumusque18, Jason D. Eastman19, Michael Endl20, Pedro Figueira21, Eric B. Ford14, 15, Daniel Foreman-Mackey22, 23, Paul Fournier24, Gabor Fur} esz´ 25, B. Scott Gaudi26, Philip C. Gregory27, Frank Grundahl28, Artie P. Hatzes29, Guillaume Hebrard´ 30, 31, Enrique Herrero32, David W. Hogg22, 33, Andrew W. Howard34, John A. Johnson19, Paul Jorden35, Colby A. Jurgenson2, David W. Latham19, Greg Laughlin36, Thomas J. Loredo37, Christophe Lovis18, Suvrath Mahadevan14, 15, 38, Tyler M. McCracken2, Francesco Pepe18, Mario Perez39, David F. Phillips19, Peter P. Plavchan40, Lisa Prato41, Andreas Quirrenbach42, Ansgar Reiners43, Paul Robertson14, 15, Nuno C. Santos21, 44, David Sawyer2, Damien Segransan18, Alessandro Sozzetti45, Tilo Steinmetz46, Andrew Szentgyorgyi19, Stephane´ Udry18, Jeff A. Valenti47, Sharon X. Wang14, 15, Robert A. Wittenmyer48, 49, Jason T. Wright14, 15, 38 (Received; Accepted) to appear in PASP ABSTRACT The Second Workshop on Extreme Precision Radial Velocities defined circa 2015 the state of the art Doppler precision and identified the critical path challenges for reaching 10 cm s−1 measurement precision. The presentations and discussion of key issues for instrumentation and data analysis and the workshop recommendations for achieving this bold precision are summarized here. Beginning with the HARPS spectrograph, technological advances for precision radial ve- locity measurements have focused on building extremely stable instruments. To reach still higher precision, future spectrometers will need to improve upon the state of the art, pro- ducing even higher fidelity spectra. This should be possible with improved environmental control, greater stability in the illumination of the spectrometer optics, better detectors, more precise wavelength calibration, and broader bandwidth spectra. Key data analysis challenges for the precision radial velocity community include distinguishing center of mass Keplerian motion from photospheric velocities (time correlated noise) and the proper treat- ment of telluric contamination. Success here is coupled to the instrument design, but also requires the implementation of robust statistical and modeling techniques. Center of mass velocities produce Doppler shifts that affect every line identically, while photospheric veloc- ities produce line profile asymmetries with wavelength and temporal dependencies that are different from Keplerian signals. Exoplanets are an important subfield of astronomy and there has been an impressive rate of discovery over the past two decades. However, higher precision radial velocity measurements are required to serve as a discovery technique for potentially habitable worlds, to confirm and characterize detections from transit missions, and to provide mass measurements for other space-based missions. The future of exoplanet science has very different trajectories depending on the precision that can ultimately be achieved with Doppler measurements. Keywords: instrumentation: spectrographs - methods: observational - methods: statistical technique : radial velocities - techniques: spectroscopic debra.fi[email protected] Petersburg 196140, Russia 1 The content of this publication emerged from pre- 7 Sobolev Astronomical Institute, St Petersburg State sentations and discussion by the 150 participants in the University, Universitetskij prospekt 28, Petrodvorets, St Second Workshop on Extreme Precision Radial Velocities, Petersburg 198504, Russia held at Yale University. The talks and posters from this 8 Department of Astronomy and Astrophysics, Univer- meeting are archived at http://eprv.astro.yale.edu sity of Chicago, 5640 S. Ellis Avenue, Chicago, IL 60637, 2 Department of Astronomy, Yale University, New USA Haven, CT 06511 USA 9 Aix Marseille Universit´e, CNRS, LAM (Laboratoire 3 Centre for Astrophysics Research, Science and Tech- d'Astrophysique de Marseille) UMR 7326, 13388 Marseille, nology Research Institute, University of Hertfordshire, France College Lane, Hatfield AL10 9AB, UK 10 Centre for Star and Planet Formation, Natural 4 School of Physics and Astronomy, Queen Mary Uni- History Museum of Denmark & Niels Bohr Institute, versity of London, 327 Mile End Road, London E1 4NS, University of Copenhagen, Øster Voldgade 5-7, DK-1350 UK Copenhagen K, Denmark 5 Department of Terrestrial Magnetism, Carnegie Insti- 11 Leibniz-Institut f¨ur Astrophysik Potsdam, An der tute of Washington, Washington, DC 20015, USA Sternwarte 16, 14482 Potsdam, Germany 6 Central Astronomical Observatory at Pulkovo of 12 Astronomy and Astrophysics Division, Physical Russian Academy of Sciences, Pulkovskoje shosse 65, St Research Laboratory (PRL), Ahmedabad 380009, India 2 Fischer et al. 1. INTRODUCTION for wavelength calibration and modeling of the in- The past two decades have been a golden era for strumental profile to achieve radial velocity (RV) the discovery of exoplanets | thousands of exo- precisions of a few meters per second using general planets have been detected using Doppler measure- purpose spectrometers (Butler et al. 1996; Marcy & ments, transit photometry, microlensing, and direct Butler 1992); the stabilized HARPS spectrometer, imaging. Pioneering technology has driven remark- which set a new standard in RV precision (Mayor able acceleration in the rate of detections | of spe- et al. 2003; Pepe et al. 2002); ground-based tran- cial note: the clever use of an iodine reference cell sit surveys that evolved rapidly from demonstrating the existence of transiting extrasolar planets (Henry et al. 2000; Charbonneau et al. 2000) to achiev- 13 Department of Physics, University of Notre Dame, ing 1-mmag photometric precision (Johnson et al. South Bend, IN, USA 14 Department of Astronomy and Astrophysics, The 2009); and the Kepler space mission with a dra- Pennsylvania State University, 525 Davey Laboratory, matic improvement over the precision of ground- University Park, PA 16802, USA based photometry. The Kepler mission confirmed 15 Center for Exoplanets and Habitable Worlds, The earlier suggestions (Mayor & Udry 2008) that most Pennsylvania State University, University Park, PA 16802, USA of the stars in our galaxy have planetary systems 16 National Institute of Standards and Technology, 325 and that small planets are ubiquitous (Howard et al. Broadway, Boulder, CO 80305, USA 2012; Fressin et al. 2013; Buchhave et al. 2014). 17 Department of Physics, University of Colorado, 2000 However, while ever smaller and lower mass planets Colorado Ave, Boulder, CO, 80309, USA 18 Observatoire Astronomique de l'Universit´e de have been detected in the past few years, all cur- Gen´eve, 51 chemin des Maillettes, CH-1290 Versoix, rent techniques fall just short of detecting so-called Switzerland exo-Earths (planets that are nearly the mass of the 19 Harvard-Smithsonian Center for Astrophysics, Cam- Earth, orbiting at habitable zone distances) around bridge, MA 02138, USA 20 The University of Texas at Austin and Department of nearby stars. Astronomy and McDonald Observatory, 2515 Speedway, A generation of students has grown up thinking C1400, Austin, TX 78712, USA of exoplanet science as a booming field where the 21 Instituto de Astrof´ısica e Ci^enciasdo Espa¸co, Uni- rate of discovery and characterization has a steep versidade do Porto, CAUP, Rua das Estrelas, 4150-762 Porto, Portugal and positive trajectory. However, the key to growth 22 Center for Cosmology and Particle Physics, Depart- in this field has been the sequential improvements ment of Physics, New York University, USA in technology and measurement precision and this 23 Astronomy Department, University of Washington, Box 951580, Seattle, WA 98195, USA is also a fundamental requirement for the future of 24 Fibertech Optica Inc., Canada the field. If we keep making the same observations 25 MIT Kavli Institute for Astrophysics and Space with the same instruments, we will improve the SNR Research 77 Mass Ave 37-515, Cambridge, MA, 02139, and population size, but we will basically have the USA 26 Department of Astronomy, Ohio State University, same results and the field will stagnate; advances in 140 W. 18th Ave., Columbus, OH 43210, USA strategy, analysis and instrumentation are required 27 Physics and Astronomy, University of British to reach higher RV precision and to push into new Columbia, 6244 Agricultural Rd, British Columbia, parameter space. Canada V6T 1Z1 28 Stellar Astrophysics Centre, Department of Physics New space missions including the Transiting Ex- and Astronomy, Aarhus University, Ny Munkegade 120, oplanet Survey Satellite (TESS; Ricker et al. 2014), DK-8000 Aarhus C, Denmark the CHaracterizing ExOPlanet Satellite (CHEOPS; 29 Th¨uringerLandessternwarte, Sternwarte 5, Tauten- Fortier et al. 2014) and PLAnetary Transits and Os- burg 5, 07778 Tautenburg, Germany 30 Institut d'Astrophysique de Paris, UMR7095 CNRS, cillation of stars (PLATO; Rauer et al. 2014) will Universit´ePierre & Marie Curie, 98bis boulevard Arago, have the precision to detect transiting planets with F-75014 Paris, France small radii and will observe bright nearby stars. 31 Observatoire de Haute-Provence, Universit´e d'Aix- Marseille & CNRS, F-04870 Saint Michel lObservatoire,
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