Protostars and Planets VI, Heidelberg, July 15-20, 2013
Poster 2K024
Correcting Astrophysical Noise in HARPS-N RV Measurements
Gettel, Sara (Harvard-Smithsonian Center for Astrophysics)
Pepe, Francesco (Observatoire de l\'Universite de Geneve)
Collier Cameron, Andrew (SUPA - University of St. Andrews)
Latham, David (Harvard-Smithsonian Center for Astrophysics)
Molinari, Emilio (INAF - TNG)
Udry, Stephane (Observatoire de l\'Universite de Geneve)
Charbonneau, David (Harvard-Smithsonian Center for Astrophysics)
Lopez-Morales, Mercedes (Harvard-Smithsonian Center for Astrophysics)
Lovis, Christophe (Observatoire de l\'Universite de Geneve)
Micela, G. (INAF - Observatorio Astronomico de Palermo)
Philips, David (Harvard-Smithsonian Center for Astrophysics)
Piotto, G. (University of Padua)
Pollacco, D. (Queens University Belfast)
Queloz, Didier (Observatoire de l\'Universite de Geneve)
Rice, K. (SUPA - University of Edinburgh)
Sasselov, Dimitar (Harvard-Smithsonian Center for Astrophysics)
Segrasan, D. (Observatoire de l\'Universite de Geneve)
Sozzetti, Alessandro (INAF - TNG)
Szentgyorgyi, A. (Harvard-Smithsonian Center for Astrophysics)
Mayor, Michel (Observatoire de l\'Universite de Geneve)
HARPS-N Collaborators, ()
Abstract:
Radial velocity instrumental precision has improved to the degree that measurements are now limited in part by the noise intrinsic to the host
star, or stellar ‘jitter’. Several different phenomena contribute to the observed jitter, including pressure waves, granulation, magnetic features caused
by stellar activity, and solar-like magnetic cycles. The amplitude of these effects ranges from 10 to 400 cm/s, depending on stellar type, and pose a
significant limitation to detecting Earth analogues. We carry out a survey of bright, quiet stars with the new HARPS-N instrument, an ultra-stabilized
R=115,000 cross-dispersed spectrograph located on the 3.6m Telescopio Nazionale Galileo on the island of La Palma. We look for correlations
between these radial velocity measurements and known activity indicators, including line bisector measurements and the CaII index. We will correct
for the presence of starspots by locating and removing quasi-periodic signals consistent with stellar rotation rate. We also investigate new
correlations between radial velocity measurements and other observables, including variations in line depth ratios. By correcting for these combined
effects, we can improve the radial velocity precision, enabling the detection of low-mass planets.
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