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Dissertation submitted to the Combined Faculties of the Natural Sciences and Mathematics of the Ruperto-Carola-University of Heidelberg. Germany for the degree of Doctor of Natural Sciences Put forward by ARIANNA MUSSO BARCUCCI born in Moncalieri, Italy Oral examination: 23 July 2020 THE RELATION BETWEEN DISCS AND YOUNG COMPANIONS - OBSERVATIONAL STUDIES REFEREES: PROF. DR. THOMAS HENNING PROF. DR. KEES DULLEMOND ABSTRACT The direct imaging technique brings advantages with respect to other, indirect methods of detect- ing planets. It is sensitive to larger separations, it can detect companions on a variety of orbital configurations, and it allows to simultaneously image both a companion and the circumstellar disc it resides in, thus being the perfect tool to study companion-disc interactions. Direct observations of Hα emission from young planetary and low-mass stellar companions can also shed light on the early gas accretion phase of planet formation. In this Thesis I use the direct imaging technique to study various aspects of planet-disc interaction and planet formation and evolution. I present the detection of a previously unknown low-mass stellar companion around HD 193571, observed as part of the NaCo Imaging Survey for Planets around Young Stars (ISPY). The companion appears to reside within the gap between the host star and its surrounding disc, making this the third low-mass stellar companion discovered within a debris disc. This system is thus the perfect laboratory where to study the relative importance between self- and companion-stirring models in discs. I also present the detection of Hα emission from the known substellar companion around the young star PZ Tel. The derived Hα luminosity, combined with age and disc information, indicates that the emission is likely due to chromospheric activity of the companion. This detection further proves the capability of using high-contrast imaging instruments and techniques to detect Hα signatures from companions around young stars. On a larger scale, I present the L’ band Imaging Survey to find Exoplanets in the North (LIStEN), which targeted ∼30 nearby stars with known and well characterised circumstellar discs. LIStEN focuses on characterising the population of wide-orbit giant planets around disc-hosting stars, as well as studying the intricacies of companion-disc interactions. I present the survey’s scientific goals, data selection and observational strategy, as well as the data reduction and analysis. No new planetary companions were detected, and the mass detection limits derived from the observations are combined with information on the disc size and morphology to constrain the presence of unseen planetary and low-mass stellar companion around these disc-hosting stars. ZUSAMMENFASSUNG Die Methodik der direkten Beobachtung hat Vorteile gegenuber¨ anderen, indirekten Methoden zum Nachweis von Exoplaneten. Sie ist empfindlicher fur¨ großere¨ Separationen, kann planetare und stellare Begleitobjekte auf einer Vielzahl von Bahnkonfigurationen nachweisen, und erlaubt es, gleichzeitig sowohl ein Begleitobjekt als auch die zirkumstellaren Scheibe abzubilden, was diese Methodik zum perfekten Werkzeug zur Untersuchung von Wechselwirkungen zwischen dem Begleiter und der Scheibe macht. Die direkte Beobachtung der Hα-Emission von jungen planetaren und massearmen stellaren Begleitern kann zudem Aufschluss uber¨ die fruhe¨ Gasakkre- tionsphase der Planetenbildung geben. In dieser Dissertation verwende ich die Methodik der direkten Beobachtung, um verschiedene Aspekte der Planeten-Scheiben-Wechselwirkung und der Entstehung und Entwicklung von Planeten zu untersuchen. Ich prasentiere¨ den Nachweis eines bisher unbekannten massearmen stellaren Begleiters um HD 193571, der im Rahmen der NaCo “Imaging Survey for Planets around Young Star” (ISPY) Beobachtungskampagne entdeckt wurde. Der Begleiter befindet sich in der Lucke¨ zwischen dem Zentralstern und der ihn umgebenden Scheibe; dieses massearme stellare Begleitobjekt ist bislang erst das dritte, das in einer Trummerscheibe¨ entdeckt wurde. Dies macht dieses System daher zum idealen Kandidaten zur Untersuchung der relativen Bedeutung von Eigen- und Fremdanregung bei der Enstehung und Entwicklung von Trummerscheiben.¨ Ich prasentiere¨ des Weiteren eine Detektion von Hα Emis- sion fur¨ das bekannte substellare Begleitobjekt um den jungen Stern PZ Tel. Die hergeleitete Hα Leuchtkraft, kombiniert mit Informationen uber¨ das Alter und die Scheibe, weist darauf hin, dass die Emission wahrscheinlich auf die chromospharische¨ Aktivitat¨ des Begleiters zuruckzuf¨ uhren¨ ist. Diese Entdeckung ist ein weiterer Nachweis, dass Instrumente und Techniken zur Abbildung mit hohem Kontrast großes Potential haben, Hα-Signaturen von Begleitern um junge Sterne zu entdecken. Schließlich prasentiere¨ ich Ergebnisse der Beobachtungskampagne “L’ band Imaging Survey to find Exoplanets in the North” (LIStEN), welche ∼ 30 nahe Sterne mit bekannten und gut charakterisierten zirkumstellaren Scheiben beinhaltet. LIStEN konzentriert sich auf die Charakterisierung der Population von Riesenplaneten mit großer Umlaufbahn in zirkumstellaren Scheiben von Sternen sowie auf die Untersuchung der Wechselwirkungen zwischen Begleiter und Scheibe. Ich diskutiere die wissenschaftlichen Ziele der Studie, die Auswahl der Objekte und Beobachtungsstrategie, sowie die Analyse und Reduktion der Beobachtungsdaten. Obwohl keine neuen Planeten entdeckt wurden, kann ich die aus den Beobachtungen abgeleiteten Grenzen fur¨ die Masse von Begleitobjekten in Kombination mit Informationen uber¨ die Große¨ und Morpholo- gie der Scheiben benutzen um die Prasenz¨ von nicht detektierten planetaren oder massearmen stellaren Begleitern in den Stern-Scheiben-Systemen einzuschranken.¨ Ai miei genitori. Contents LIST OF FIGURES xiii LIST OF TABLES xv List of Abbreviations xvii 1 Introduction1 1.1 Planets and where to find them..........................2 1.1.1 Circumstellar discs............................3 1.1.2 Detection techniques...........................4 1.1.3 Current state of the field.........................6 1.2 Direct imaging..................................7 1.2.1 Advantages and drawbacks........................7 1.2.2 Direct imaging observations.......................9 1.3 What can we learn from direct imaging?.....................9 1.3.1 Companion-disc interaction.......................9 1.3.2 Hα emission from low-mass stellar companions............. 11 1.3.3 Direct imaging surveys.......................... 12 1.3.3.1 The NaCo-ISPY and the LIStEN survey........... 14 1.4 Thesis outlook and scope............................. 15 2 ISPY - NaCo Imaging Survey for Planets around Young stars Discovery of an M dwarf in the gap between HD 193571 and its debris ring 17 2.1 Introduction.................................... 17 2.2 HD 193571.................................... 18 2.3 Observations and data reduction......................... 20 2.3.1 VLT/NaCo................................ 20 2.3.2 Gemini/GPI................................ 20 2.4 Analysis and results................................ 22 2.4.1 Astrometry and photometry....................... 22 2.4.2 Physical properties............................ 25 2.4.3 Orbital motion.............................. 26 2.5 Stirring mechanisms............................... 27 ix Contents x 2.6 Conclusions.................................... 30 3 Detection of Hα emission from PZ Tel B using SPHERE/ZIMPOL 33 3.1 Introduction.................................... 33 3.2 PZ Tel B...................................... 33 3.3 Observations and data reduction......................... 35 3.4 Analysis and results................................ 36 3.4.1 Astrometry and flux contrast....................... 37 3.4.2 Photometry................................ 37 3.4.3 Orbital constraints............................ 38 3.5 Discussion and conclusions............................ 42 4 LIStEN - the L’ band Imaging Survey to find Exoplanets in the North 45 4.1 Introduction.................................... 45 4.2 Target Selection.................................. 46 4.2.1 Target master list............................. 46 4.2.2 Notes on individual targets........................ 47 4.2.2.1 HD 206860........................... 48 4.2.2.2 HD 183324, HD 191174 and HD 192425........... 48 4.2.2.3 HD 48682, HD 143894, HD 161868, HD 212695 and HD 127821 49 4.2.2.4 HD 110897........................... 49 4.2.2.5 HD 50554........................... 49 4.2.2.6 HD 8907............................ 50 4.2.2.7 HIP 83043........................... 50 4.2.2.8 HD 128311........................... 50 4.2.2.9 HD 113337........................... 51 4.3 Observations................................... 53 4.4 Data Reduction & Analysis............................ 53 4.4.1 Data processing.............................. 53 4.4.2 PynPoint analysis............................. 56 4.4.3 Contrast curves & Mass limits...................... 57 4.4.4 Infrared excess characterisation..................... 60 4.5 Planetary constraints and disc analysis...................... 61 4.5.1 Self-stirring analysis........................... 61 4.5.2 Double-belt analysis........................... 64 4.5.3 Planetary constraints from proper motion anomaly........... 66 4.6 Conclusions.................................... 72 5 Summary and future perspective 75 5.1 Summary..................................... 75 5.2 Future perspective................................. 77 5.2.1 Follow-up observations.........................
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    September 2017 Issue September 2017 Next Meeting: Monday, September 11th at 7PM at HRPO nd (2 Mondays, Highland Road Park Observatory) September Program: GAE (Great American. Eclipse) Membership Reports. Club members are invited to “approach the mike. ” and share their experiences travelling hither and thither to observe the August total eclipse. What's In This Issue? HRPO’s Great American Eclipse Event Summary (Page 2) President’s Message Secretary's Summary Outreach Report - FAE Light Pollution Committee Report Recent Forum Entries 20/20 Vision Campaign Messages from the HRPO Spooky Spectrum Observe The Moon Night Observing Notes – Draco The Dragon, & Mythology Like this newsletter? See past issues back to 2009 at http://brastro.org/newsletters.html Newsletter of the Baton Rouge Astronomical Society September 2017 The Great American Eclipse is now a fond memory for our Baton Rouge community. No ornery clouds or“washout”; virtually the entire three-hour duration had an unobstructed view of the Sun. Over an hour before the start of the event, we sold 196 solar viewers in thirty-five minutes. Several families and children used cereal box viewers; many, many people were here for the first time. We utilized the Coronado Solar Max II solar telescope and several nighttime telescopes, each outfitted with either a standard eyepiece or a “sun funnel”—a modified oil funnel that projects light sent through the scope tube to fabric stretched across the front of the funnel. We provided live feeds on the main floor from NASA and then, ABC News. The official count at 1089 patrons makes this the best- attended event in HRPO’s twenty years save for the historic Mars Opposition of 2003.
  • TRUE MASSES of RADIAL-VELOCITY EXOPLANETS Robert A

    TRUE MASSES of RADIAL-VELOCITY EXOPLANETS Robert A

    APP Template V1.01 Article id: apj513330 Typesetter: MPS Date received by MPS: 19/05/2015 PE: CE : LE: UNCORRECTED PROOF The Astrophysical Journal, 00:000000 (28pp), 2015 Month Day © 2015. The American Astronomical Society. All rights reserved. TRUE MASSES OF RADIAL-VELOCITY EXOPLANETS Robert A. Brown Space Telescope Science Institute, USA; [email protected] Received 2015 January 12; accepted 2015 April 14; published 2015 MM DD ABSTRACT We study the task of estimating the true masses of known radial-velocity (RV) exoplanets by means of direct astrometry on coronagraphic images to measure the apparent separation between exoplanet and host star. Initially, we assume perfect knowledge of the RV orbital parameters and that all errors are due to photon statistics. We construct design reference missions for four missions currently under study at NASA: EXO-S and WFIRST-S, with external star shades for starlight suppression, EXO-C and WFIRST-C, with internal coronagraphs. These DRMs reveal extreme scheduling constraints due to the combination of solar and anti-solar pointing restrictions, photometric and obscurational completeness, image blurring due to orbital motion, and the “nodal effect,” which is the independence of apparent separation and inclination when the planet crosses the plane of the sky through the host star. Next, we address the issue of nonzero uncertainties in RV orbital parameters by investigating their impact on the observations of 21 single-planet systems. Except for two—GJ 676 A b and 16 Cyg B b, which are observable only by the star-shade missions—we find that current uncertainties in orbital parameters generally prevent accurate, unbiased estimation of true planetary mass.