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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20180905T103000
DTEND;TZID=Atlantic/Canary:20180905T113000
UID:iactalks-1193
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /iactalks/Talks/view/1193
CREATED:2018-09-05T10:30:00+01:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:The search for habitable Earth-like planets
DESCRIPTION:The search for habitable Earth-like planets\nDr. Alejandro Suá
 rez Mascareño\n\nThe search of Earth-like extrasolar planets approaches a
  key moment in its history. With the arrival of ESPRESSO (observing alread
 y!), the possibility of detecting Earth-like planets around solar-type sta
 rs is at last a reality, and the opportunities to characterize earth-like 
 planets and super-Earths are more numerous than ever. High precision radia
 l velocity (RV) measurements (better than 1 m s−1 for instruments li
 ke HARPS and HARPS-N) have given astronomers the possibility of detecting 
 and characterizing small exoplanets for a few years, down to the mass of t
 he Earth, when orbiting M-dwarfs at short orbital periods, or a few Earth-
 masses at longer periods. The arrival of the new generation of instruments
  (ESPRESSO) brings a revolution in precision, to the level of 5-10 cm s-1,
  allowing for the detection or characterization of Earth-mass planets at l
 onger orbital periods, in the habitable zone of Sun-like stars. At these l
 evels of precision, signals induced by stellar activity in the RV curves b
 ecome the most important limiting factor, even in the case of magnetically
  quiet stars. Stellar activity can induce apparent Doppler shifts of the s
 tellar spectrum, which cause periodic signals that range from less than on
 e to dozens of meters per second. The correct detection and characterizati
 on of the different star-induced signals and their effect in the RVs is on
 e of the most important steps to detect and properly characterize low-mass
  exoplanets, and its importance will greatly increase with increased preci
 sion, as even in the case of the quietest stars, these signals will surfac
 e. Unveiling the population of small-mass planets in the range of super-Ea
 rths and smaller, especially at long orbital periods (close to the habitab
 le zone of their stars and beyond), is a key step to understand the format
 ion of planetary systems. To really paint the full picture of the systems,
  and accurately derive their parameters, we need to identify and model tog
 ether the planetary companions and activity signals present in the data. I
  will present the current state of the field, the challenges and the techn
 iques to overcome them, focusing on the efforts that I have made during th
 e last years.
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