Precise radial velocities of giant stars VIII. Testing for the presence of planets with CRIRES Infrared Radial Velocities

We have been monitoring 373 very bright (V < 6 mag) G and K giants with high precision optical Doppler spectroscopy for more than a decade at Lick Observatory. Our goal was to discover planetary companions around those stars and to better understand planet formation and evolution around intermediate-mass stars. However, in principle, long-term, g-mode nonradial stellar pulsations or rotating stellar features, such as spots, could effectively mimic a planetary signal in the radial velocity data. Our goal is to compare optical and infrared radial velocities for those stars with periodic radial velocity patterns and to test for consistency of their fitted radial velocity semiamplitudes. Thereby, we distinguish processes intrinsic to the star from orbiting companions as reason for the radial velocity periodicity observed in the optical. Stellar spectra with high spectral resolution have been taken in the H-band with the CRIRES near-infrared spectrograph at ESO's VLT for 20 stars of our Lick survey. Radial velocities are derived using many deep and stable telluric CO2 lines for precise wavelength calibration. We find that the optical and near-infrared radial velocities of the giant stars in our sample are consistent. We present detailed results for eight stars in our sample previously reported to have planets or brown dwarf companions. All eight stars passed the infrared test. We conclude that the planet hypothesis provides the best explanation for the periodic radial velocity patterns observed for these giant stars.Comment: 14 pages, 6 figures, 3 tables, accepted by Astronomy & Astrophysic

Precision Radial Velocity Surveys for Exoplanets

Seit den 90-ziger Jahren haben Astronomen etwa 500 extrasolare Planeten entdeckt. Die meisten von Ihnen wurden mit der Radialgeschwindigkeits-Methode gefunden. In dieser Arbeit präsentieren wir unsere präzisen Radialgeschwindigkeitsmessungen für ein Sample von 40 M-Sternen und 30 sonnenähnlichen Sternen. Die Datensätze stammen von vier verschieden Instrumenten (UVES, CES+LC, CES+VLC, und HARPS) und werden auf Hinweise von Planeten untersucht. Dazu führen wir statistische Tests zu Exzessvariabilitäten, Langzeittrends und Periodizitäten durch. Für letzteren Zweck, haben wir ein häufig genutztes Werkzeug für die Periodenanalyse, das sogenannte Lomb-Scargle Periodogramm, weiterentwickelt. Unsere Radialgeschwindigkeitsgenaukeit von wenigen m/s ist annähernd ausreichend für die angestrebten Ziele, nämlich die Suche nach terrestrischen Planeten in der habitablen Zone von M-Sternen und die Suche nach Jupiter-artigen Planeten um sonnenähnliche Sterne. Wir demonstrieren dies mit oberen Massengrenzen. Aus unserer Datenanalyse geht kein neuer Planet hervor, während wir die bereits bekannten Planeten für die sonnenähnlichen Sterne Iota Hor und HR 506 sowie den Langzeittrend für Eps Ind A bestätigen können. Darüber hinaus konnten wir einige Doppelsterne und einen Braunen Zwerg identfizieren. Unsere Ergebnisse stimmen mit den Erwartungen für die Häufigkeit von Jupiter-artigen Planeten überein, welche etwa 1% für M-Sterne und 10% für sonnenähnliche Sterne ist

The Discovery of Stellar Oscillations in the Planet Hosting Giant Star Beta Geminorum

We present the results of a long time series of precise stellar radial velocity measurements of the planet hosting K giant star Beta Geminorum. A total of 20 hours of observations spanning three nights were obtained and the radial velocity variations show the presence of solar-like stellar oscillations. Our period analysis yields six significant pulsation modes that have frequencies in the range of 30 - 150 microHz. The dominant mode is at a frequency of 86.9 microHz and has an amplitude of 5.3 m/s. These values are consistent with stellar oscillations for a giant star with a stellar mass of approximately 2 solar masses. This stellar mass implies a companion minimum mass of 2.6 Jupiter masses. Beta Gem is the first planet hosting giant star in which multi-periodic stellar oscillations have been detected. The study of stellar oscillations in planet hosting giant stars may provide an independent, and more accurate determination of the stellar mass.Comment: 12 pages preprint, 2 figures, accepted by ApJ Letter

New HARPS and FEROS observations of GJ1046

In this paper we present new precise Doppler data of GJ1046 taken between November 2005 and July 2018 with the HARPS and the FEROS high-resolution spectographs. In addition, we provide a new stellar mass estimate of GJ1046 and we update the orbital parameters of the GJ1046 system. These new data and analysis could be used together with the GAIA epoch astrometry, when available, for braking the $\sin i$ degeneracy and revealing the true mass of the GJ1046 system.Comment: 2 pages, 1 figure, 1 table with RV data (available only in the Astro-PH version of the paper), Accepted by RNAA

Ground-based detection of an extended helium atmosphere in the Saturn-mass exoplanet WASP-69b

Hot gas giant exoplanets can lose part of their atmosphere due to strong stellar irradiation, affecting their physical and chemical evolution. Studies of atmospheric escape from exoplanets have mostly relied on space-based observations of the hydrogen Lyman-{\alpha} line in the far ultraviolet which is strongly affected by interstellar absorption. Using ground-based high-resolution spectroscopy we detect excess absorption in the helium triplet at 1083 nm during the transit of the Saturn-mass exoplanet WASP-69b, at a signal-to-noise ratio of 18. We measure line blue shifts of several km/s and post transit absorption, which we interpret as the escape of part of the atmosphere trailing behind the planet in comet-like form. [Additional notes by authors: Furthermore, we provide upper limits for helium signals in the atmospheres of the exoplanets HD 209458b, KELT-9b, and GJ 436b. We investigate the host stars of all planets with detected helium signals and those of the three planets we derive upper limits for. In each case we calculate the X-ray and extreme ultraviolet flux received by these planets. We find that helium is detected in the atmospheres of planets (orbiting the more active stars and) receiving the larger amount of irradiation from their host stars.]Comment: Submitted to Science on 14 March 2018; Accepted by Science on 16 November 2018; Published by Science on 6 December 2018. This is the author's version of the work. It is posted here by permission of the AAAS for personal use. The definitive version was published in Science, on 6 December 2018 - Report: pages 21 (preprint), 4 figures - Supplementary materials: 22 pages, 10 figures, 3 table

Practices to support co-design processes: A case-study of co-designing a program for children with parents with a mental health problem in the Austrian region of Tyrol

Forms of collaborative knowledge production, such as community-academic partnerships (CAP), have been increasingly used in health care. However, instructions on how to deliver such processes are lacking. We aim to identify practice ingredients for one element within a CAP, a 6-month co-design process, during which 26 community- and 13 research-partners collaboratively designed an intervention programme for children whose parent have a mental illness. Using 22 published facilitating and hindering factors for CAP as the analytical framework, eight community-partners reflected on the activities which took place during the co-design process. From a qualitative content analysis of the data, we distilled essential practices for each CAP factor. Ten community- and eight research-partners revised the results and co-authored this article. We identified 36 practices across the 22 CAP facilitating or hindering factors. Most practices address more than one factor. Many practices relate to workshop design, facilitation methods, and relationship building. Most practices were identified for facilitating ‘trust among partners’, ‘shared visions, goals and/or missions’, ‘effective/frequent communication’, and ‘well-structured meetings’. Fewer practices were observed for ‘effective conflict resolution’, ‘positive community impact’ and for avoiding ‘excessive funding pressure/control struggles’ and ‘high burden of activities’. Co-designing a programme for mental healthcare is a challenging process that requires skills in process management and communication. We provide practice steps for delivering co-design activities. However, practitioners may have to adapt them to different cultural contexts. Further research is needed to analyse whether co-writing with community-partners results in a better research output and benefits for participants