BEGIN:VCALENDAR VERSION:2.0 PRODID:-//CERN//INDICO//EN BEGIN:VEVENT SUMMARY:Magnetic Drag and 3-D Effects in Theoretical High-Resolution Emiss ion Spectra of Ultrahot Jupiters: the Case of WASP-76b DTSTART;VALUE=DATE-TIME:20220908T141500Z DTEND;VALUE=DATE-TIME:20220908T143000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-132@meetings.aip.de DESCRIPTION:Speakers: Hayley Beltz (University of Michigan)\nUltrahot Jupi ters are ideal candidates to explore with high-resolution emission spectra . Detailed theoretical studies are necessary to investigate the range of s pectra we can expect to see from these objects throughout their orbit\, be cause of the extreme temperature and chemical longitudinal gradients that exist across day and nightside regions. Using previously published 3D GCM models of WASP-76b with different treatments of magnetic drag\, we post-pr ocess the 3D atmospheres to generate high-resolution emission spectra for two wavelength ranges and throughout the planet's orbit. We find that the high-resolution emission spectra vary strongly as a function of phase\, at times showing emission features\, absorption features\, or both\, which a re a direct result of the 3D structure of the planet. At phases exhibiting both emission and absorption features\, the Doppler shift differs in dire ction between the two spectral features\, making them differentiable inste ad of canceling each other out. Through the use of cross-correlation\, we find different patterns in net Doppler shift for models with different tre atments of drag: the nightside spectra show opposite signs in their Dopple r shift\, while the dayside phases have a reversal in the trend of net shi ft with phase.\n\nhttps://meetings.aip.de/event/16/contributions/132/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/132/ END:VEVENT BEGIN:VEVENT SUMMARY:PETS: The PEPSI Exoplanet Transit Survey - Investigating the prese nce of a silicate atmosphere on the super-Earth 55 Cnc e DTSTART;VALUE=DATE-TIME:20220908T080000Z DTEND;VALUE=DATE-TIME:20220908T081500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-109@meetings.aip.de DESCRIPTION:Speakers: Engin Keles (AIP)\nThe PEPSI Exoplanet Transit Surve y (PETS) is a spectroscopic survey of exoplanet transits\, secondary eclip ses\, and host-star characterization. In this collaborative effort from AI P\, MPIA\, INAF\, University of Arizona\, Ohio State University and the LB T\, a large number of targets have been observed with the goal to characte rize planetary atmospheres in detail. \n\nTowards the atmospheric characte rization of smaller planets\, the super-Earth exoplanet 55 Cnc e is one of the most promising terrestrial exoplanets studied to date. Here\, we pres ent a high-resolution spectroscopic transit observation of this planet wit hin the PETS survey. Assuming the presence of Earth-like crust species on the surface of 55 Cnc e\, from which a possible silicate-vapor atmosphere could have originated\, we search in its transmission spectrum for absorpt ion of various atomic and ionized species. \n\nNot finding absorption for any of the investigated species\, we are able to set absorption limits wit h a median value of 1.9 x Rp\, ruling out the evidence of a widely extend ed silicate envelope on this super-Earth reaching several planetary radii. \n\nhttps://meetings.aip.de/event/16/contributions/109/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/109/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: The UBV-module for the ANDES spectrograph DTSTART;VALUE=DATE-TIME:20220907T133100Z DTEND;VALUE=DATE-TIME:20220907T133200Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-154@meetings.aip.de DESCRIPTION:Speakers: Silva Järvinen (AIP)\nhttps://meetings.aip.de/event /16/contributions/154/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/154/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Climate-Photochemical Modeling of Earth-like Exoplanet ary Atmospheres DTSTART;VALUE=DATE-TIME:20220908T133200Z DTEND;VALUE=DATE-TIME:20220908T133300Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-164@meetings.aip.de DESCRIPTION:Speakers: Lee Grenfell (DLR)\nhttps://meetings.aip.de/event/16 /contributions/164/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/164/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Searching for flaring star-planet interactions in all known transiting systems DTSTART;VALUE=DATE-TIME:20220908T133100Z DTEND;VALUE=DATE-TIME:20220908T133200Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-163@meetings.aip.de DESCRIPTION:Speakers: Ekaterina Ilin (AIP)\nhttps://meetings.aip.de/event/ 16/contributions/163/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/163/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Model reprocessing: a new\, mathematically proven meth odology DTSTART;VALUE=DATE-TIME:20220907T083300Z DTEND;VALUE=DATE-TIME:20220907T083400Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-162@meetings.aip.de DESCRIPTION:Speakers: Doriann Blain (MPIA)\nhttps://meetings.aip.de/event/ 16/contributions/162/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/162/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Optimising Exoplanet Transit Spectroscopy Observations DTSTART;VALUE=DATE-TIME:20220907T083100Z DTEND;VALUE=DATE-TIME:20220907T083200Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-161@meetings.aip.de DESCRIPTION:Speakers: Linn Boldt-Christmas (Uppsala University)\nhttps://m eetings.aip.de/event/16/contributions/161/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/161/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Machine learning for exoplanet transit spectroscopy DTSTART;VALUE=DATE-TIME:20220908T083300Z DTEND;VALUE=DATE-TIME:20220908T083400Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-160@meetings.aip.de DESCRIPTION:Speakers: Cole Kilby (Potsdam University)\nhttps://meetings.ai p.de/event/16/contributions/160/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/160/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Pathways for exomoon detections with high-resolution s pectra DTSTART;VALUE=DATE-TIME:20220908T083200Z DTEND;VALUE=DATE-TIME:20220908T083300Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-159@meetings.aip.de DESCRIPTION:Speakers: Florian Rünger (Potsdam University)\nhttps://meetin gs.aip.de/event/16/contributions/159/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/159/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: redcross: Open-source python package for reduction and cross-correlation of exoplanet atmospheres at high-resolution DTSTART;VALUE=DATE-TIME:20220907T083200Z DTEND;VALUE=DATE-TIME:20220907T083300Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-158@meetings.aip.de DESCRIPTION:Speakers: Darío González Picos ()\nhttps://meetings.aip.de/e vent/16/contributions/158/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/158/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Enabling high-resolution K-band spectroscopy at the EL T DTSTART;VALUE=DATE-TIME:20220907T133300Z DTEND;VALUE=DATE-TIME:20220907T133400Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-157@meetings.aip.de DESCRIPTION:Speakers: Laura Kreidberg (MPIA)\nhttps://meetings.aip.de/even t/16/contributions/157/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/157/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: The PEPSI Exoplanet Transit Survey (PETS) at LBT DTSTART;VALUE=DATE-TIME:20220908T083100Z DTEND;VALUE=DATE-TIME:20220908T083200Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-156@meetings.aip.de DESCRIPTION:Speakers: Klaus Strassmeier (Leibniz-Institut for Astrophysics Potsdam (AIP))\nhttps://meetings.aip.de/event/16/contributions/156/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/156/ END:VEVENT BEGIN:VEVENT SUMMARY:Flash talk: Exoplanet atmospheres in the U-band with ELT-ANDES DTSTART;VALUE=DATE-TIME:20220907T133200Z DTEND;VALUE=DATE-TIME:20220907T133300Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-155@meetings.aip.de DESCRIPTION:Speakers: Katja Poppenhaeger (AIP)\nhttps://meetings.aip.de/ev ent/16/contributions/155/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/155/ END:VEVENT BEGIN:VEVENT SUMMARY:High Resolution Atmospheric Retrieval on an Ultra Hot Jupiter DTSTART;VALUE=DATE-TIME:20220907T081500Z DTEND;VALUE=DATE-TIME:20220907T083000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-139@meetings.aip.de DESCRIPTION:Speakers: Jorge Sanchez (Arizona State University)\nWe present High Resolution Cross Correlation Spectroscopy (HRCCS) observations and a tmospheric retrieval results of the Ultra Hot Jupiter\, MASCARA-1b. HRCCS is a novel technique used to characterize exoplanets with ground-based ins truments by utilizing the planet's time-resolved Doppler shifted signal to separate it from the dominant stellar and telluric lines. The high spectr al resolution along with wide wavelength coverage allows for robust constr aints on molecular abundances and thermal structures using bayesian retrie val techniques. \n\n\nWe present our atmospheric retrieval results of MASC ARA-1b using data taken from the IGRINS instrument (R~45000) at Gemini Sou th. This high fidelity data provides robust constraints on molecular abund ances in order to calculate C/O ratios and probe the thermal structure of the planet.\n\nhttps://meetings.aip.de/event/16/contributions/139/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/139/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Individual challenges and synergies of high- and low -resolution data for exoplanet atmospheres DTSTART;VALUE=DATE-TIME:20220907T120000Z DTEND;VALUE=DATE-TIME:20220907T124500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-147@meetings.aip.de DESCRIPTION:Speakers: Lisa Nortmann (Georg-August-Universität Göttingen )\nWhile first detections of atmospheric species were based on medium-to l ow resolution data from space\, ground-based facilities have majorly contr ibuted to our understanding of these far-away worlds since then.\nTo a lar ge part this is owed to the use of high-resolution spectroscopy\, which al lows us to identify the resolved lines of metals and molecules in the opti cal and infrared wavelength regions using cross-correlation with synthetic models or studies of isolated lines. The success of these methods on ultr a-hot to warm exoplanets have inspired the community to design instruments for the extremely large telescope facilities with the goal to extend thes e studies to the atmospheres of rocky worlds in the future. But not all ou r dreams for the bright future of exoplanet atmospheres are based on high- resolution instrumentation.\nIn parallel\, studies at lower resolution hav e been continued both from the ground as well as from space. Especially wi th the recent launch of JWST and the planned launch of ARIEL in 2029 we ca n expect space based medium resolution studies to be a main driver of the advancement of our field in the next decades.\nWith the same planets being observed at different resolutions and thus analyzed with different method s the question emerges of how these different kinds of data relate to each other. In this talk I will focus on the individual challenges and differe nces presented by low and high-res data and the methods used to analyze th em. I will address in which capacity the information derived from them is equivalent and/or complementary and what we can hope to gain when using bo th methods in unison.\n\nhttps://meetings.aip.de/event/16/contributions/14 7/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/147/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Narrow-band transmission spectroscopy of large plane ts: results and future avenues in the optical DTSTART;VALUE=DATE-TIME:20220907T091500Z DTEND;VALUE=DATE-TIME:20220907T100000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-146@meetings.aip.de DESCRIPTION:Speakers: Julia Seidel (ESO)\nThe holistic understanding of ex oplanet atmospheres continues to elude us due to the difficulty in acquiri ng data for these far-away worlds. A wide array of techniques is necessary to probe their components\, structure\, and interactions. One of these te chniques has proven to be particularly effective for large and highly irra diated exoplanets: Ground-based\, narrow-band transmission spectroscopy in ultra high-resolution (uHRS\, R > 80'000). \n\nIn uHRS\, transmission spe ctroscopy allows us to detect the resolved lines of various atomic species \, probing various orders of magnitude in pressure. Recently\, the use of highly stabilized spectrographs has opened new avenues to extract informat ion about the three dimensional nature of atmospheres: their composition i n altitude\, their dynamics\, and\, by proxy\, even their magnetic fields. The refinement of uHRS observations and analysis techniques on large and highly irradiated planets as benchmark cases will ultimately help us push towards both smaller and cooler planets with future facilities.\n\nhttps:/ /meetings.aip.de/event/16/contributions/146/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/146/ END:VEVENT BEGIN:VEVENT SUMMARY:LBT/PEPSI Observations of the Ultra Hot Jupiter KELT-20 b DTSTART;VALUE=DATE-TIME:20220907T074500Z DTEND;VALUE=DATE-TIME:20220907T080000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-126@meetings.aip.de DESCRIPTION:Speakers: Marshall Johnson (Ohio State University)\nUltra hot Jupiters around bright stars are the most favorable targets for high-resol ution exoplanetary spectroscopy. We present our emission and transmission spectroscopy observations of the ultra hot Jupiter KELT-20 b/MASCARA-2 b f rom PEPSI on LBT\, with R=130\,000. With the LBT's large aperture we obtai n some of the highest signal-to-noise ratio exoplanetary spectra to date ( stellar spectra with total SNR~3400). We obtained a 16-sigma detection of Fe I emission from the planetary atmosphere via cross-correlation\, and we consider the line profile and time variation of this signal in order to c onstrain the planetary atmospheric structure. We fail to detect any other species in emission despite the strong Fe I emission\, including several s pecies previously reported in the literature. We will discuss the implicat ions of these non-detections\, including placing limits on atmospheric inv ersion agents such as TiO and VO. These high signal-to-noise spectra give a preview of what we will be able to achieve for many more planets in the ELT era.\n\nhttps://meetings.aip.de/event/16/contributions/126/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/126/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: The Search for Signs of Life on Exoplanets DTSTART;VALUE=DATE-TIME:20220909T120000Z DTEND;VALUE=DATE-TIME:20220909T124500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-152@meetings.aip.de DESCRIPTION:Speakers: Vikki Meadows (University of Washington)\nThe search for signs of life on other worlds is an exciting and now key component of exoplanet science. In the exoplanet context\, biosignatures are potential ly-detectable impacts of life on a global planetary environment. Biosign atures may include identified and sought after molecules in a planetary at mosphere\, reflectivity signals on its surface\, or the characteristic var iation of these or other characteristics as a function of time. Biosignat ures may also be “agnostic”\, meaning that they are not associated wit h a known or postulated metabolism\, thereby allowing us to search for unk nown forms of life. Agnostic biosignatures consist of anomalous patterns or molecules that are unlikely to be generated by abiotic planetary proces sess. All biosignatures\, and particularly agnostic biosignatures\, must be interpreted in the context of their planetary environment. This conte xt can provide additional information to help rule out biosignature “fal se positives” where instead of being generated by life\, a sought after environmental characteristic is instead generated by abiotic processes lik e volcanism and photochemistry. In the near-term\, the search for life on exoplanets will focus exclusively on M dwarf exoplanets\, which\, due to t he coevolution with their star\, may undergo a very different evolutionary path than our own Earth. These searches will be undertaken using low-medi um resolution transmission spectroscopy with JWST\, and high-resolution tr ansmission and reflected light spectroscopy with ground-based telescopes. In the longer term\, a large-aperture space-based telescope will use dir ect imaging techniques to obtain reflected light from planets orbiting a b roader swath of host stars\, including the more “Sun-like” FGK dwarfs. This will expand our search for life in the universe to planetary systems that are more analogous to our own. In this talk I will introduce the fi eld of biosignatures\, and describe the potential capabilities for biosign ature searches using high-resolution spectroscopy with ground-based telesc opes\, placing these opportunities in the context of what might be possibl e with space-based telescopes over the next two decades.\n\nhttps://meetin gs.aip.de/event/16/contributions/152/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/152/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Spectrographs for exoplanets: from radial velocities to atmospheres DTSTART;VALUE=DATE-TIME:20220909T070000Z DTEND;VALUE=DATE-TIME:20220909T074500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-151@meetings.aip.de DESCRIPTION:Speakers: Pedro Figueria (University of Geneva)\nSpectrograph s for radial velocities evolved from the specifications required for Galac tic dynamics studies to those set by exoplanet mass characterization. As t ime went by\, the search for lower-mass planets on longer periods pushed f or higher measurement precision and improved instrument stability. But the detection of a transiting planet in 2000 and an exo-atmosphere in 2010 re shuffled scientific priorities. Today\, atmosphere characterization is don e mostly on spectrographs designed for precise RVs\, and yet is having a f ield day at it.\n\nhttps://meetings.aip.de/event/16/contributions/151/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/151/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: How High-Resolution Spectroscopy Measures 3D Propert ies of Exoplanets DTSTART;VALUE=DATE-TIME:20220908T120000Z DTEND;VALUE=DATE-TIME:20220908T124500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-150@meetings.aip.de DESCRIPTION:Speakers: Emily Rauscher (University of Michigan)\nIt is only mildly controversial to insist that planets are three-dimensional. Whether or not 1D models can adequately be used to interpret exoplanet observatio ns depends on some combination of how much spatial inhomogeneity exists on a planet and how sensitive the data are to its 3D structure. For atmosphe ric characterization using high resolution spectroscopy\, our highest sign al-to-noise targets are (ultra) hot Jupiters and these planets have huge s patial inhomogeneities. We are increasingly recognizing that these planets ’ 3D properties influence\, and are constrained by\, high resolution spe ctroscopy in both transmission and emission. I will discuss hot Jupiter 3D atmospheric structure\, including the pieces of complicated physics we ar e working to unravel\, and briefly show how our expectations change as we move beyond the hot Jupiter population. I will then review the multiple wa ys in which 3D structures show up in high resolution spectroscopy\, throug h spatial variations in physical properties and atmospheric winds. I will highlight the current edge of our capabilities and speculate about how thi s field may advance in the future.\n\nhttps://meetings.aip.de/event/16/con tributions/150/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/150/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Understanding the diversity of exoplanet atmospheres DTSTART;VALUE=DATE-TIME:20220908T091500Z DTEND;VALUE=DATE-TIME:20220908T100000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-149@meetings.aip.de DESCRIPTION:Speakers: Vivien Parmentier (University of Oxford)\nJust look ing through a telescope from your backyard you can see that the planets fr om our own Solar-System have widely different atmospheres. Such a large di versity is also expected for exoplanets\, particularly since they cover a much wider parameter space. Now that we are able to measure exoplanet atmo spheric spectrum our goal is to separate the effects of intrinsic differen ces\, such as elemental chemical composition\, from differences due to the ir specific circumstances\, such as their rotation period or their equilib rium temperature.\n\nI will review how radiative transfer\, atmospheric ci rculation\, chemistry and microphysics shape giant planet atmospheres and discuss how these processes can produce very different outcomes in planets that only posses small differences. I will show the expected and observed patterns in the population both at low and high spectral resolution and d iscuss how these differ from our expectation.\n\nhttps://meetings.aip.de/e vent/16/contributions/149/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/149/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: Infrared high-resolution spectroscopy of exoplanets: state-of-the art and prospects for the 2020s DTSTART;VALUE=DATE-TIME:20220908T070000Z DTEND;VALUE=DATE-TIME:20220908T074500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-148@meetings.aip.de DESCRIPTION:Speakers: Matteo Brogi (University of Warwick)\nMeasuring the chemical and thermal properties of planetary atmospheres is the main goal of current exoplanet science. It allows us to understand their true nature \, origin\, and eventually the ability to support life. Ground-based\, hig h-resolution spectroscopy (HRS\, R>25\,000) has emerged as one of the lead ing methods to detect atomic and molecular species in the atmospheres of e xoplanets. At infrared wavelengths\, it allows us to resolve molecular ban ds into the individual spectral lines and extract their signal through cro ss correlation with model templates. As an added bonus\, HRS can measure p lanet rotation\, winds and orbital motion directly.\nHRS has produced a ra pidly growing inventory of detected species. Furthermore\, recent developm ents of the technique have unlocked the ability to measure absolute abunda nces and temperatures\, at a level comparable to expected JWST observation s but using different and complementary spectral information. This ability sets the stage for a strong synergy between space and ground observations of hot and warm gaseous planets during the current decade.\n\nhttps://mee tings.aip.de/event/16/contributions/148/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/148/ END:VEVENT BEGIN:VEVENT SUMMARY:Invited talk: High Resolution Spectroscopy for Exoplanet Atmospher es: an observer’s playground DTSTART;VALUE=DATE-TIME:20220907T070000Z DTEND;VALUE=DATE-TIME:20220907T074500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-145@meetings.aip.de DESCRIPTION:Speakers: Jayne Birkby (University of Oxford)\nHigh resolutio n spectroscopy has proven a powerful and highly versatile tool in the char acterization of exoplanet atmospheres. Over the last decade we have explor ed the rich detail that its sensitivity to the position and shape of exopl anet spectral lines provides\, and with robustness thanks to the unique pa ttern of lines that each species exhibits at such high resolution. In this talk\, I will review this playground for discovery in exoplanet atmospher es with an observer’s eye\, focusing on the observational techniques it uses and their outputs. I will briefly explore its discoveries from abunda nces to the 3D dynamical nature of exoplanet atmospheres\, from the ultra hot to the increasingly cooler and smaller planets. Despite a vast range o f new discoveries\, thanks to the deluge of new high resolution instrument s from the EPRV community\, we have barely only scratch the surface of wha t we can learn with high resolution spectroscopy. I will highlight current and future avenues for discovery\, including with the ELTs. I will finish however with a primer for discussion during this workshop\, on some of th e challenges and the consensus that the field of high resolution spectrosc opy of exoplanet atmospheres needs to face as we go towards the robust cha racterisation of potentially habitable worlds.\n\nhttps://meetings.aip.de/ event/16/contributions/145/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/145/ END:VEVENT BEGIN:VEVENT SUMMARY:ExoMol line lists for high-resolution spectroscopic studies of exo planets DTSTART;VALUE=DATE-TIME:20220908T103000Z DTEND;VALUE=DATE-TIME:20220908T104500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-144@meetings.aip.de DESCRIPTION:Speakers: Sergey Yurchenko (University College London)\nThe ne xt generation of ground-based telescopes\, which complement the space miss ions\, are aimed at HR (R ~ 100\,000) studies. Ground-based high resolutio n Doppler spectroscopy (HRS)\, pioneered by Snellen\, has been used to ch aracterise the atmospheres of a growing number of exoplanets in recent yea rs. None of this is possible without the necessary laboratory data. While spectroscopic and other data needs for studies of Earth-clone exoplanets a re well met by databases constructed for studying our own atmosphere\, suc h as HITRAN\, this is not the case for those exoplanets which will be the first exoplanets to be characterised. These planets are hot and most are s ubject to strong bombardment by starlight (and presumably stellar winds). Such studies require data on hot molecules which are not generally availa ble and which are in many cases not easily amenable to laboratory experime nts. In particular\, current developments in exoplanetary observations are fueling the requirement for HR data. This creates new challenges for labo ratory spectroscopy projects like ExoMol\, which have been mainly concerne d with completeness (important for low resolution-based retrievals) rather than HR studies. The field of the HRS of exoplanets is growing extremely fast and urgently demanding high precision molecular data. Failures to det ect molecules in atmospheres of exoplanets can often be attributed to the lack of the underlying quality of the line positions. \n\nThe [ExoMol data base][1] contains extensive line lists for approximately 80 molecules\, in most cases for several isotopically substituted variants ("isotopologues" )\, with over 700 billion molecular transitions and two formal releases. T he current ExoMol activity aims at providing high accuracy spectroscopic data for high resolution studies of exoplanetary atmospheres. Novel theore tical techniques are being used to provide similar high accuracy line list s for isotopically substituted species and to generate pressure broadening data.\n\n\n [1]: http://exomol.com\n\nhttps://meetings.aip.de/event/16/c ontributions/144/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/144/ END:VEVENT BEGIN:VEVENT SUMMARY:High-resolution spectroscopic detection of atmospheric sodium on l ong-transiting inflated exoplanet KELT-11b DTSTART;VALUE=DATE-TIME:20220907T100000Z DTEND;VALUE=DATE-TIME:20220907T101500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-140@meetings.aip.de DESCRIPTION:Speakers: Dany Mounzer (University of Geneva)\nState-of-the-ar t spectrographs on large ground-based telescopes have allowed significant discoveries in the structure\, composition and dynamic processes of exopla netary atmospheres through high-resolution transit spectroscopy. However\, observations from ground-based facilities face two major challenges : The day-night cycle limits the length of observations\, and incoming signals are distorted by Earth's atmosphere. The latter can be solved by adaptive optics and precise telluric correction\, but the former is an issue for tr ansit spectroscopy. This restricts the observable planets to ones with tra nsit duration smaller than five hours.\n\nExtremely inflated exoplanet KEL T-11b is affected by this issue\, as it transits its host star for more th an seven hours. To bypass this limitation\, we observed this system for se ries of three consecutive days: Before\, during and after the transit\, in order to collect a large number of in-transit and out-of-transit baseline spectra. This allowed the computation of a strong signal-to-noise high-re solution combined transmission spectrum. The individual spectra were corre cted for telluric absorption using ESO atmospheric transmission code Molec fit.\n\nThis resulting transmission spectrum shows conclusive evidence of excess atomic sodium absorption through the 5'900 Å doublet of 0.29±0.05 % and 0.50±0.06 % in the Na D1 and D2 lines respectively. We model for w ind patterns and find day-to-night side winds with surprisingly no vertica l winds\, considering KELT-11b's extreme scale height of 2'763 km. We also highlight the robustness of our three-day observation method which allows the study of exoplanets with long transits that haven't been studied with high-resolution ground-based spectrographs.\n\nOther recent results from TESS\, HST and CHEOPS combined with KELT-11b's hot atmosphere\, bright hos t star\, long transit\, sub-Saturn mass and great bloatedness make it a un ique and ideal candidate for atmospheric characterization with the next ge neration of telescopes\, especially from space.\n\nhttps://meetings.aip.de /event/16/contributions/140/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/140/ END:VEVENT BEGIN:VEVENT SUMMARY:Auto-differentiable high-resolution spectral model for exoplanets and its application to the Barnard's Star DTSTART;VALUE=DATE-TIME:20220908T131500Z DTEND;VALUE=DATE-TIME:20220908T133000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-137@meetings.aip.de DESCRIPTION:Speakers: Hiroyuki Tako Ishikawa (Astrobiology Center)\nWe are developing an open-source auto–differentiable spectral modeling code [" ExoJAX"](http://secondearths.sakura.ne.jp/exojax/#) to perform atmospheric retrieval for high-resolution exoplanetary spectra by ab initio spectral fitting. This enables fully Bayesian inference of atmospheric parameters w ith the Hamiltonian Monte Carlo. Meanwhile\, the parameter estimation of M dwarfs\, which are important as host stars of various exoplanets\, has mo stly depended on pre-computed radiative-chemical equilibrium models. Howev er\, it has been reported in many literatures that the incompleteness of t hose models is a fundamental problem due to the spectral complexity caused by the cool atmosphere. We have retrieved the atmospheric parameters of t he well-known M dwarf Barnard's star ($T_{\\mathrm{eff}} \\sim$ 3200 K) by applying the ExoJAX to its high-resolution near-infrared spectra ($R\\sim $ 80000\, $YJH$–band) independently of stellar models. We succeeded in r eproducing well the molecular and atomic lines simultaneously at several w avelengths\, and estimated the temperature-pressure profile and mixing rat ios of each atomic and molecular species. Nevertheless\, at other wavelen gths\, we found that the same way could not reproduce the absorption featu res at all\, so we discuss the inaccuracy and missing absorption lines of the latest line list. The inspection of atmospheric retrieval of M dwarfs\ , for which is easier to obtain high-resolution spectra with high quality than in exoplanets\, will highlight the path and caveats to accurate retri eval of exoplanets.\n\nhttps://meetings.aip.de/event/16/contributions/137/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/137/ END:VEVENT BEGIN:VEVENT SUMMARY:beta Pictoris b through the eyes of the upgraded CRIRES+ DTSTART;VALUE=DATE-TIME:20220909T091500Z DTEND;VALUE=DATE-TIME:20220909T093000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-136@meetings.aip.de DESCRIPTION:Speakers: Rico Landman (Leiden University)\nDirectly imaged pl anets orbiting at very wide separation present a challenge to current plan et formation theories. We present the analysis of new observations of beta Pictoris b with the refurbished and enhanced CRIRES+\, with new constrain ts on its spin-rotation and C/O ratio. Furthermore\, we will introduce a p ython package for the reduction of CRIRES+ data specifically aimed at dire ctly imaged planets\, and our future plans for observing directly imaged p lanets with CRIRES+.\n\nhttps://meetings.aip.de/event/16/contributions/136 / LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/136/ END:VEVENT BEGIN:VEVENT SUMMARY:Keck/KPIC Emission Spectroscopy of WASP-33b DTSTART;VALUE=DATE-TIME:20220907T131500Z DTEND;VALUE=DATE-TIME:20220907T133000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-135@meetings.aip.de DESCRIPTION:Speakers: Luke Finnerty (UCLA)\nWe present Keck/KPIC high-reso lution ($R\\sim35\,000$) $K$-band thermal emission spectroscopy of the ult ra-hot Jupiter WASP-33b. The use of KPIC's single-mode fiber greatly impro ves both blaze and line-spread stabilities relative to slit spectrographs\ , enhancing the cross-correlation detection strength. We perform separate retrievals for the dayside and nightside emission spectra with a cross-cor relation-to-logL nested sampling pipeline which fits for orbital parameter s\, the atmospheric pressure-temperature profile\, and molecular abundance s. While the dayside shows a thermal inversion which is absent on the nigh tside\, we measure consistent CO and H$_2$O abundances for both hemisphere s (nightside $\\log\\rm H_2O_{MMR} = -3.3^{+0.9}_{-0.6}$\, $\\log\\rm CO_{ MMR} = -1.5^{+0.9}_{-0.6}$ versus dayside $\\log\\rm H_2O_{MMR} = -4^{+1}_ {-1}$\, $\\log\\rm CO_{MMR} = -2^{+1}_{-1}$)\, suggesting limited dayside H$_2$O dissociation at the pressures probed. The retrieved abundances sugg est a carbon- and possibly metal-enriched atmosphere\, with a gas-phase C/ O ratio of $1.0\\pm0.1$\, consistent with the accretion of high-metallicit y gas near the CO$_2$ snow line and post-disk migration. The dayside hemis phere shows a systemic redshift compared to the nightside in excess of WAS P-33b's rotation speed\, suggesting day-to-night winds may be contributing to the offset. We also find tentative evidence for $\\rm ^{13}CO/^{12}CO \\sim 40$\, consistent with values expected in protoplanetary disks. Thes e observations demonstrate KPIC's ability to characterize close-in planets and the utility of KPIC's improved instrumental stability for cross-corre lation techniques.\n\nhttps://meetings.aip.de/event/16/contributions/135/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/135/ END:VEVENT BEGIN:VEVENT SUMMARY:There’s more to life than O2: Assessing the detectability of bio signatures and environmental context for high-resolution spectroscopy of t errestrial exoplanets DTSTART;VALUE=DATE-TIME:20220909T124500Z DTEND;VALUE=DATE-TIME:20220909T130000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-131@meetings.aip.de DESCRIPTION:Speakers: Miles Currie (University of Washington)\nThe upcomin g class of extremely large telescopes (ELTs) will provide an unprecedented opportunity to use high-resolution spectroscopy to characterize terrestri al exoplanets for habitability and life. In particular\, these telescopes are likely the best near-term tools for detecting molecular oxygen in near by exoplanet atmospheres. However\, determining whether oxygen is more lik ely to have a biological origin requires contextual information from the p lanetary environment to support the identification and rule out false posi tives. Studies which investigate the ELTs’ capacity to detect other gase s can enhance the science return from these telescopes and expand our abil ities to search for signs of life. We have developed a novel pipeline to s imulate telescope observations and estimate the detectability of a suite o f gases—CH$_4$\, CO$_2$\, CO\, O$_3$\, and H$_2$O—that can help give c ontext to ELT O$_2$ detections in terrestrial exoplanet atmospheres. As in put\, we used a suite of photochemically self-consistent simulations of M dwarf planets with modern/Archean Earth-like atmospheres\, and worlds with abiotic O$_2$ buildup due to photochemical generation and ocean loss proc esses. We find that CO$_2$ and CH$_4$ are two of the most detectable molec ules in M dwarf planetary atmospheres\, and may be detectable on TRAPPIST- 1 e in less than 35 transits. This may be the only known biosignature pair accessible with ELT high-resolution spectroscopy for this target. However \, for closer targets\, the ELTs alone may be capable of discriminating an inhabited world from one without life with tens of hours of observation t ime under ideal conditions. Additionally\, we find the detectability of al l gases is strongly dependent on host star type—planets orbiting late-ty pe M dwarfs may require less overall observation time to achieve a signifi cant detection. Finally\, we develop an observing protocol that prioritize s the most detectable gas absorption bands to maximize the science output of ELT observations\, and inform instrument development beyond the first l ight capabilities.\n\nhttps://meetings.aip.de/event/16/contributions/131/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/131/ END:VEVENT BEGIN:VEVENT SUMMARY:Initial Results from the ExoGemS Survey DTSTART;VALUE=DATE-TIME:20220909T074500Z DTEND;VALUE=DATE-TIME:20220909T080000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-130@meetings.aip.de DESCRIPTION:Speakers: Laura Flagg (Cornell University)\nWe will discuss th e results from the Exoplanets with Gemini Spectroscopy (ExoGemS) survey\, which has acquired high-resolution transit spectroscopy of over a dozen e xoplanets. Because our survey covers a large range of radii\, masses\, and Teq\, we can compare how these properties affect the resulting transmissi on spectrum. The high-resolution of GRACES allows us to analyze the line profile and study the atmosphere at higher altitudes. In particular\, we w ill highlight the detections from WASP-76 b\, HAT-P-32 b\, WASP-31 b\, and WASP-85 Ab. We will also discuss the effect of stellar activity on these results.\n\nhttps://meetings.aip.de/event/16/contributions/130/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/130/ END:VEVENT BEGIN:VEVENT SUMMARY:3-d high-resolution transmission spectra with the pRT-Orange DTSTART;VALUE=DATE-TIME:20220908T143000Z DTEND;VALUE=DATE-TIME:20220908T144500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-125@meetings.aip.de DESCRIPTION:Speakers: Paul Mollière (MPIA)\nHigh resolution spectroscopy is quickly establishing itself as one of the most exciting ground-based ob servational techniques for exoplanets. Especially the doppler shifts of at omic and molecular lines are an excellent probe of dynamics and thus offer a unique window into the atmospheres of exoplanets. This information is h ighly complementary when compared to space-based telescopes\, which observ e at lower resolution. What is more\, velocity differences observed for di fferent absorbers are thought to probe their spatial distribution in the a tmosphere\, unlocking its 3-d nature. To interpret observations that probe the multi-d structure of atmospheres we are developing an open-source ext ension to our atmospheric retrieval package petitRADTRANS\, called pRT-Ora nge. pRT-Orange divides the atmosphere of the planet into (orange) segment s that share common properties such as temperature\, abundance\, or cloud structure. The location\, extent and number of segments can be freely chos en\, allowing for simple or complex atmospheric parameterizations. Arbitra ry velocity fields can be specified for the Doppler shifts\, ranging from planetary rotation to feeding in the dynamic solutions of general circulat ion models. At the moment pRT-Orange works for transmission only. In my ta lk I will present the current state of the code development\, and grant ea rly access to pRT-Orange at the meeting\, if people are interested (with t he obvious work-in-progress disclaimer).\n\nhttps://meetings.aip.de/event/ 16/contributions/125/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/125/ END:VEVENT BEGIN:VEVENT SUMMARY:Effect of Stellar activity on the atmosphere of hot Jupiters and t heir transit signatures. DTSTART;VALUE=DATE-TIME:20220908T144500Z DTEND;VALUE=DATE-TIME:20220908T150000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-123@meetings.aip.de DESCRIPTION:Speakers: Gopal Hazra (Department of Astrophysics\, University of Vienna)\nThe evolution of planetary atmospheres is very much dependent on the environment of their host stars (e.g.\, stellar radiation\, stella r wind\, stellar flares and Coronal Mass Ejections (CMEs)). For close-in p lanets\, the stellar radiation evaporates the planetary atmosphere as a fo rm of supersonic planetary outflow due to photoionization. This planetary outflow further interacts with the stellar wind\, which shapes up the plan etary atmosphere (sometimes producing a comet-like structure) and its mass loss rate. Moreover\, flares and CMEs from the star will also have a grea t impact on planetary evaporation. In this talk\, I will discuss the effec t of stellar wind\, and the impact of flares and CMEs on the atmosphere of hot Jupiters using a self-consistent 3D radiation hydrodynamic model. Amo ng all the considered stellar environments\, we find that CMEs are very ef fective in eroding planetary atmospheres. We also calculate synthetic Lyma n-alpha transit signatures and find that the flare alone cannot explain th e observed high blue shifted velocities seen in the Lyman-alpha observatio n. The CME\, however\, leads to an increase in the velocity of the escapin g atmosphere\, enhancing the transit depth at high blue shifted velocities . Finally\, I will also discuss the effect of the different orientations o f the CME magnetic field on the atmospheric escape and corresponding trans it signatures.\n\nhttps://meetings.aip.de/event/16/contributions/123/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/123/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterizing the atmosphere of the warm Neptune HAT-P-11 b with high resolution spectroscopy DTSTART;VALUE=DATE-TIME:20220908T101500Z DTEND;VALUE=DATE-TIME:20220908T103000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-119@meetings.aip.de DESCRIPTION:Speakers: Fabio Lesjak (Institut für Astrophysik und Geophysi k Göttingen)\nHigh resolution spectra of transit events enable the search for constituents in exoplanet atmospheres with a variety of methods.\nUsi ng cross correlation\, the observations can be compared to models across a wide wavelength range\, taking advantage of the large number of absorptio n lines of some species. For other species\, the excess absorption in stro ng individual lines is measurable directly by comparing the spectra taken during the transit with those before and after the transit. We analyze tra nsmission spectra of HAT-P-11 b obtained with CARMENES using these two met hods to search for a multitude of species in the planetary atmosphere. We remove stellar and telluric lines with SYSREM and find a detection of CH$_ 4$ using cross correlation. In addition\, we confirm the previously detect ed presence of He by examining the near-infrared helium triplet. Helium is known to be a tracer for extended atmospheres and to be related to stella r activity. The large eccentricity of HAT-P-11 b's orbit helps to disentan gle the planetary from the stellar absorption lines. Furthermore\, we sear ch for other species that are expected to be present in the atmosphere of warm Neptunes.\n\nhttps://meetings.aip.de/event/16/contributions/119/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/119/ END:VEVENT BEGIN:VEVENT SUMMARY:Uncovering 3D variations in the temperature chemistry\, and winds on ultra-hot Jupiters: Targeting multiple species with high-resolution spe ctroscopy DTSTART;VALUE=DATE-TIME:20220908T124500Z DTEND;VALUE=DATE-TIME:20220908T130000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-118@meetings.aip.de DESCRIPTION:Speakers: Joost Wardenier (University of Oxford)\nUltra-hot Ju piters are tidally locked gas giants with dayside temperatures high enough to dissociate hydrogen and other molecules. Featuring sharp chemical grad ients and large temperature contrasts\, their atmospheres are vastly non-u niform. In recent years\, the wealth of data from high-resolution spectrog raphs such as HARPS-N\, CRIRES\, ESPRESSO and IGRINS has yielded spectacul ar insights into the chemical inventory\, wind profiles and temperature st ructures of ultra-hot Jupiters. In particular\, high-precision observation s with ESPRESSO were able to sample the varying Doppler shift of the absor ption lines in the spectrum of a transiting exoplanet.\n\nIn this talk\, I will present a new framework for computing time-dependent\, 3D transit sp ectra of exoplanets at high spectral resolution. We post-process the outpu t of a state-of-the-art global circulation model (the SPART/MITgcm) throug h a GPU-optimised Monte-Carlo radiative transfer code\, called gCMCRT. Thi s allows us to correctly model the millions of spectral lines that can be observed with ground-based instruments\, while accounting for the complex effects of thermal and chemical inhomogeneities\, wind gradients and plane t rotation in a unified framework.\n\nI will demonstrate that different ch emical species\, such as water\, CO\, and iron\, are distributed different ly throughout the atmosphere of an ultra-hot Jupiter\, resulting in unique transit signals for certain atoms and molecules. This is because thermal dissociation and condensation impact the chemical composition of the daysi de and the nightside of the planet. I will show that our framework can qua litatively reproduce the time-dependent iron signal observed by Ehrenreich + (2020) for WASP-76b. To this end\, we either assume that iron condenses into clouds on the nightside\, or that the morning limb is substantially c ooler than expected. \n\nIn addition\, I will illustrate how signals from other species\, such as water (which is dissociated on the dayside) and CO (which is unaffected by temperature) can be used to bypass the inherent d egeneracies associated with the observation of a single species. Finally\, I will cover the results of our recent transit observations of WASP-121b with Gemini-S/IGRINS. These observations targeted water and CO absorption in the infrared\, with the objective to obtain a similar signal-to-noise r atio as the WASP-76b iron signal observed with ESPRESSO. I will discuss ho w interpreting the absorption signals of these three chemical species (wat er\, CO\, iron) within the same framework allows us to place important con straints on the 3D structure of the limb of an ultra-hot Jupiter.\n\nhttps ://meetings.aip.de/event/16/contributions/118/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/118/ END:VEVENT BEGIN:VEVENT SUMMARY:Spatially-resolving the terminator: Variation of Fe\, temperature and winds in WASP-76~b across planetary limbs and orbital phase DTSTART;VALUE=DATE-TIME:20220908T130000Z DTEND;VALUE=DATE-TIME:20220908T131500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-116@meetings.aip.de DESCRIPTION:Speakers: Siddharth Gandhi ()\nExoplanet atmospheres are inher ently three-dimensional systems in which thermal/chemical variation and wi nds can strongly influence spectra. Recently\, the ultra-hot Jupiter WASP- 76~b has shown evidence for condensation and asymmetric Fe absorption with time. However\, it is unclear whether these asymmetries are driven by che mical or thermal differences between the two limbs\, as precise constraint s on variation in these have remained elusive due to the challenges of mod elling these dynamics in a Bayesian framework as well as the procurement o f such high quality observations. To address this we develop a new model\, HyDRA-2D\, capable of simultaneously retrieving morning and evening termi nators with day-night winds\, and use this on recent high-precision termin ator observations of WASP-76~b with ESPRESSO/VLT. We explore variations in Fe\, temperature profile\, winds and opacity deck with limb and orbital p hase. In this talk I will show that with HyDRA-2D we find Fe is more promi nent on the evening for the last quarter of the transit. On the other hand the morning shows a lower abundance with a wider uncertainty\, driven by degeneracy with the opacity deck and because the stronger evening signal d ominates the overall spectrum. We also constrain a trend of higher tempera tures for the more irradiated atmospheric regions\, and a higher wind spee d for the last quarter of the transit than the first. This new spatially- and phase-resolved treatment is statistically favoured by 4.9$\\sigma$ ove r traditional 1D-retrievals\, and thus demonstrates the power of such mode lling for robust constraints with current and future facilities.\n\nhttps: //meetings.aip.de/event/16/contributions/116/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/116/ END:VEVENT BEGIN:VEVENT SUMMARY:Tantalising signs of H$_2$O in the cloudy atmosphere of a warm Nep tune from High-Resolution Spectroscopy DTSTART;VALUE=DATE-TIME:20220909T081500Z DTEND;VALUE=DATE-TIME:20220909T083000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-115@meetings.aip.de DESCRIPTION:Speakers: Spandan Dash (Department of Physics\, University of Warwick)\nCharacterization of cooler atmospheres of super-Earths and Neptu ne sized objects at low-resolution is often thwarted by the presence of cl ouds\, hazes and aerosols which effectively flatten the transmission spect ra. High-Resolution Spectroscopy (HRS) presents an opportunity to overcome this limitation by having the ability to detect molecular species whose s pectral line cores extend above the level of clouds in these atmospheres. We analyse High-Resolution observations of the warm Neptune GJ 3470b taken over one transit using CARMENES (R ~ 80400) and two transits using GIANO (R ~ 50000) and look at the possibility of signatures for first H$_2$O in isolation and then H$_2$O and CH$_4$ together. We find a tentative detecti on of H$_2$O using either the peak of the cross correlation signal or a cr oss-correlation-to-likelihood metric while comparing it to just the best f it model\, when all three nights are combined. The detection becomes even weaker when both H$_2$O and CH$_4$ are used for abundance and cloud deck l ayer values close to the best fit model. This decrease is in line with res ults from the Hubble Space Telescope\, at much lower resolution. However\, accounting for the effects of data analysis on the compared model produce s a strong detection close to the expected exoplanet position using just o ne night of CARMENES. Following this\, we are planning to use a Bayesian r etrieval tool to put simultaneous constraints on the abundance of molecula r species and the pressure of the cloud top-deck. Such a tool will also al low us to directly compare/combine our results with published HST observat ions.\n\nhttps://meetings.aip.de/event/16/contributions/115/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/115/ END:VEVENT BEGIN:VEVENT SUMMARY:Hydrocarbon-rich Mantles in Super-Earths and Mini-Neptunes: Natura l Ingredients for Haze Production DTSTART;VALUE=DATE-TIME:20220909T131500Z DTEND;VALUE=DATE-TIME:20220909T133000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-114@meetings.aip.de DESCRIPTION:Speakers: Edwin Bergin (University of Michigan)\nThe most comm on type of exoplanet discovered to date has a size that falls between Eart h-sized and Neptune-sized\, and orbits its star with a period less than 10 0 days. Atmospheric characterization of these planets often finds featurel ess transmission spectra\, which is taken as evidence for the presence in the of clouds or hazes in the upper atmosphere that obscure the presence o f deeper lying atmospheric constituents. We will present the results of a new model that suggests hazy atmospheres are innate byproducts of planet f ormation\, where volatile ingredients are outgassed from the mantle and tr ansformed in the upper atmosphere after exposure to stellar photons. Our model relates the initial mantle composition of the planet to its formatio n zone around its star\, factoring in the relative contributions of refrac tories (metals and silicates) and volatile components (solid state organic s\, water vapor/ice\, and hydrogen-dominated nebular gas). We predict that a population of super-Earths will form in particular locations in their p rotoplanetary disks such that they receive significant inventories of orga nics\, but very low amounts of water. These hydrocarbon-rich planets are n ot carbon worlds\, but rather carbon-rich planets whose subsequent evoluti on would differ from typically assumed for terrestrial planets. We will sh ow models that encompass the geochemical equilibrium of the mantle and atm osphere\, compute the resulting atmospheric chemical equilibrium\, haze pr oduction\, and predicted spectra.\n\nhttps://meetings.aip.de/event/16/cont ributions/114/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/114/ END:VEVENT BEGIN:VEVENT SUMMARY:Unveiling Oxygen on Earth-like planets with a Fabry Perot based In strument DTSTART;VALUE=DATE-TIME:20220909T143000Z DTEND;VALUE=DATE-TIME:20220909T144500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-111@meetings.aip.de DESCRIPTION:Speakers: Surangkhana Rukdee (MPE)\nThe upcoming Extremely Lar ge Telescopes (ELTs) will have the collecting area required to detect pote ntial biosignature gases such as molecular oxygen\, O2\, in the atmosphere of terrestrial planets around nearby stars. To maximize our capability to detect O2 using this method\, extreme high spectral resolution R=300\,000 -500\,000 is required to fully resolve the absorption lines in an exoplane t atmosphere and disentangle telluric lines from our own atmosphere. Curre nt high-resolution spectrographs typically achieve spectral resolution of R=100\,000. We demonstrate a new approach with an ultra-high spectral reso lution booster to be coupled in front of a high-resolution spectrograph. T he booster is a chained Fabry Perot array which imposes a hyperfine chaine d spectral profile. With a prototype we developed\, our on-sky observation s of the solar spectrum around the O2 A-band demonstrate a resolving power of R=450\,000. The capabilities of this instrument for exoplanet characte rization are substantiated by detection of multiple atomic species\, Ni I\ , Fe I\, Mg I\, K\, and Si\, hidden among the molecular oxygen feature.\n\ nhttps://meetings.aip.de/event/16/contributions/111/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/111/ END:VEVENT BEGIN:VEVENT SUMMARY:Carbon monoxide emission in the ultra-hot Jupiter WASP-33 b indica tes an eastward hot spot DTSTART;VALUE=DATE-TIME:20220907T141500Z DTEND;VALUE=DATE-TIME:20220907T143000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-143@meetings.aip.de DESCRIPTION:Speakers: Lennart van Sluijs ()\nCharacterisation of exoplanet atmospheres using high-resolution spectra provides a unique window into t heir composition\, dynamics as well as their formation and evolution pathw ays. Our MEASURE data set contains a diverse set of 11 targets with a wide range of periods\, equilibrium temperatures and masses. For one of the ta rgets\, the Ultra Hot Jupiter WASP-33 b\, we report the first detection of CO emission lines at high spectral resolution from its thermal spectrum. These emission lines provide unambiguous evidence of a thermal inversion l ayer in its atmosphere. Moreover\, by incorporating a Bayesian framework w ith 1D PHOENIX and 3D GCM atmospheric models\, we show via Cross-Correlati on-to-log-Likelihood mapping that the spectra indicate an eastward hotspot . Our resolution of R=15\,000 pushes the High-Resolution Cross-Correlation Spectroscopy method to its lowest resolution limits. This bodes well for systems that may require the use of lower resolution spectra to improve ph oton collection\, such as small planets orbiting in the close in habitable zones of small\, faint M-dwarfs. Finally\, we will show some preliminary results from the other targets in the MEASURE survey.\n\nhttps://meetings. aip.de/event/16/contributions/143/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/143/ END:VEVENT BEGIN:VEVENT SUMMARY:Constraining Volcanism on 55 Cnc e with MAROON-X DTSTART;VALUE=DATE-TIME:20220908T081500Z DTEND;VALUE=DATE-TIME:20220908T083000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-142@meetings.aip.de DESCRIPTION:Speakers: Kaitlin Rasmussen (University of Washington)\nThe cl ass of hot terrestrial worlds known as lava planets has come under signifi cant investigation in the last decade. The brightest and most well-studied of these objects is 55 Cancri e\, a nearby super-Earth with a remarkable 17-hour orbit. However\, despite numerous studies\, debate remains about t he existence and composition of its atmosphere. We present upper limits on the iron content of 55 Cnc e derived from high-resolution time-series spe ctra taken with Gemini-N/MAROON-X and discuss implications for volcanic ou tgassing models for this planet.\n\nhttps://meetings.aip.de/event/16/contr ibutions/142/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/142/ END:VEVENT BEGIN:VEVENT SUMMARY:Consistent relative abundance constraints from multiple high-resol ution transmission spectroscopy observations of WASP-121b DTSTART;VALUE=DATE-TIME:20220907T101500Z DTEND;VALUE=DATE-TIME:20220907T103000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-141@meetings.aip.de DESCRIPTION:Speakers: Cathal Maguire (Trinity College Dublin)\nHigh-resolu tion transmission spectroscopy has opened new avenues in which to characte rise the atmospheres of exoplanets. This technique has been used to unambi guously identify chemical species\, map longitudinal variations in their a bundance across the morning and evening limbs\, as well as to infer atmosp heric dynamics. We present multiple high-resolution transmission spectrosc opy observations of the ultra-hot Jupiter WASP-121b\, using the ESPRESSO s pectrograph at the VLT\, across which we consistently constrain the relati ve abundances of various neutral metals in its atmosphere. This is done vi a the cross-correlation technique\, in which our observations are cross-co rrelated with Doppler shifted model transmission spectra. This cross-corre lation value is then “mapped” to a likelihood value\, which can then b e folded into a Bayesian retrieval framework. From these retrievals\, we c an constrain atmospheric properties such as a species volume mixing ratio\ , the vertical T-P profile of the atmosphere\, and atmospheric dynamic par ameters which are then used to infer the planet’s orbital velocity\, as well as offsets caused by winds and rotation. By constraining the relative abundance of species in a planet’s atmosphere\, we can determine the pl anet’s bulk composition\, and ultimately infer the planet’s formation and evolution mechanisms.\n\nhttps://meetings.aip.de/event/16/contribution s/141/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/141/ END:VEVENT BEGIN:VEVENT SUMMARY:Searching for Day-Night variations in the Fe I emission from WASP- 33b DTSTART;VALUE=DATE-TIME:20220907T130000Z DTEND;VALUE=DATE-TIME:20220907T131500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-138@meetings.aip.de DESCRIPTION:Speakers: Ernst de Mooij (Queen's University Belfast)\nThe ult ra-hot Jupiter WASP-33b shows evidence for a thermal inversion in the form of emission lines of atoms and molecules\, including OH and Fe. Phase-cur ve measurements at optical wavelengths with TESS show a westward phase-off set while observations in the infrared with the Spitzer Space Telescope sh ow an Eastward offset. We obtained phase-curve observations at high-spectr al resolution at optical wavelengths with Subaru/HDS as well as CFHT/ESPa DOnS.\n\nUsing log-likelihood mapping and integrating a simple phase-curve model we demonstrate that it is possible to measure phase-curve variation s\, although unequal pre/post eclipse sampling can result in biases. For t he Fe I emission\, we show evidence that the peak is after eclipse at +22 +/- 12 degrees\, consistent with the optical phase-curve. We also constrai n the day-night contrast to be >0.9\, indicating that\, in the case of Fe I\, the nightside contributes less than 10% of the day-side flux in our si mple model.\n\nhttps://meetings.aip.de/event/16/contributions/138/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/138/ END:VEVENT BEGIN:VEVENT SUMMARY:The rich chemistry of exoplanetary atmospheres at high-resolution spectroscopy DTSTART;VALUE=DATE-TIME:20220907T080000Z DTEND;VALUE=DATE-TIME:20220907T081500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-134@meetings.aip.de DESCRIPTION:Speakers: Gloria Guilluy (Osservatorio Astrofisico di Torino-I NAF)\nHigh-resolution (HR) ground-based spectrographs have drastically imp roved the investigation of exoplanet atmospheres. \nWe will present result s obtained within the GAPS 2.0 long-term program for atmospheric character ization of hot giant planets using the near-infrared 0.95-2.45 \\mu m) arm of GIARPS: the high-resolution (R /sim 50 000) spectrograph GIANO-B of th e Telescopio Nazionale Galileo (TNG).\nWe will particularly focus on our o ngoing efforts to probe exoplanetary atmospheres with the transmission spe ctroscopy technique. With the detection of six molecules in the atmosphere of the hot-Jupiter HD 209458b (Giacobbe+2021)\, we have demonstrated that exoplanetary atmospheres can show a chemical richness previously unknown. Here\, we will present the atmospheric characterization of three warm pla nets\, namely the super-Neptune WASP-107b (Giacobbe+ in prep.)\, the sub-S aturn WASP-69b (Guilluy+2022\, accepted)\, and the sub-Jovian WASP-80b (Ca rleo+2022\, accepted). The simultaneous detection of multiple molecules in their atmospheres reinforces our previous finding revealing a rich atmo spheric composition also for warm giant planets. We will give an interpret ation of our results in terms of the planet’s C/O ratio and metallicity\ , which allow us to derive important clues on the formation and migration histories. These analyses represent a new frontier in the characterization of exoplanetary atmospheres\, and additional surprising discoveries are e xpected in the next future with both ground-based HR spectrographs\, such as CRIRES+\, SPIRou\, and NIRPS\, and the low-resolution (LR) spectrograph s on board the JWST telescope.\n\nhttps://meetings.aip.de/event/16/contrib utions/134/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/134/ END:VEVENT BEGIN:VEVENT SUMMARY:A Combined High- and Low-Resolution Retrieval of a Hot Jupiter usi ng IGRINS/Gemini South and WFC3/HST DTSTART;VALUE=DATE-TIME:20220907T124500Z DTEND;VALUE=DATE-TIME:20220907T130000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-133@meetings.aip.de DESCRIPTION:Speakers: Peter Smith (Arizona State University)\nRetrievals o n high spectral resolution exoplanet observations have been recently made possible\, allowing us now to place robust\, quantitative constraints on t heir atmospheres in unprecedented detail. High resolution data can also be combined with low resolution\, space-based data in retrievals\, probing a wider range of altitudes and incorporating continuum information otherwis e lost through detrending methods common in high resolution spectroscopy. We present retrieval results of combined observations of a benchmark hot J upiter WASP-77A b\, combining multiple nights taken with the IGRINS instru ment on Gemini South (R~45\,000)\, data from WFC3 on the Hubble Space Tele scope (R~100)\, and IRAC/Spitzer photometry. We report a slightly superste llar C/O ratio and a substellar metallicity\, indicative of diverse format ion pathways for hot Jupiters.\n\nhttps://meetings.aip.de/event/16/contrib utions/133/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/133/ END:VEVENT BEGIN:VEVENT SUMMARY:Atomic and molecular species in the near-infrared emission spectru m of WASP-33b DTSTART;VALUE=DATE-TIME:20220907T143000Z DTEND;VALUE=DATE-TIME:20220907T144500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-129@meetings.aip.de DESCRIPTION:Speakers: Stevanus Kristianto Nugroho (ABC\; NAOJ)\nWASP-33b i s an ultra hot Jupiter with a day-side temperature of 3100 K. In this talk \, I will present our latest results in characterising its day-side atmosp here using the InfraRed Doppler instrument on the Subaru telescope. Using high-resolution cross-correlation spectroscopy\, we confirmed our previous detection of OH emission but only after the secondary eclipse. Through an injection test\, we show that the data quality before the eclipse is enou gh to detect the same signal if exists. More importantly\, we were able to detect the emission of Fe and Si both before and after the secondary ecli pse and Ti only after the secondary eclipse. This indicates that the spati al distribution of each chemical species is different and that we are prob ing the different parts of this 3D atmosphere. We also found evidence of t he emission of Mg and Mn after combining all data sets\, which\, if confir med\, along with Ti add more chemical species that are detected on the day -side of an exoplanet.\n\nhttps://meetings.aip.de/event/16/contributions/1 29/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/129/ END:VEVENT BEGIN:VEVENT SUMMARY:Lessons learned: What We Need to explain to the Community at Large DTSTART;VALUE=DATE-TIME:20220909T093000Z DTEND;VALUE=DATE-TIME:20220909T094500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-128@meetings.aip.de DESCRIPTION:Speakers: Scott Wolk (SAO)\nI will discuss the smallsat SEEJ ( Structure & Evolution of ExoJupiter Atmospheres). It will measure both the fluxes of high-energy photons emanating from a flux limited sample of pla net-hosting stars and the absorption depth of X-rays in the atmospheres of hot Jupiter\, Saturn\, and Neptune analogs. SEEJ will measure how often h igh energy flares of a given size occur\, and establish\, for the first ti me\, the statistics of these crucial events on exoplanet hosts. Specifical ly\, the SEEJ investigation will determine the degree to which stellar hig h-energy photons inflate nearby exoplanet atmospheres and the physical cha racteristics of driven planetary winds. The investigation will determine t he bulk composition of the inflated atmosphere and will assess the presenc e of dense evaporation tails resulting from this interaction. The experime ntal objective is to measure the high energy fluence through stellar monit oring and understand the impact of the high energy fluence by measuring th e atmospheres using the X-ray transit technique.\n\nTo accomplish this goa l\, we need to be able to demonstrate to the astrophysical community at-la rge a clear connection from the observations to reality. We need to expla in what the transit results from a limited set of planets imply for the at mospheric evolution of planets more broadly. This path starts with the de tection of a transit followed by a fitted light curve and then inferences about the obstructing material. Finally\, we need to demonstrate the impl ications that the obscuring material has for the underlying atmosphere. I n this discussion\, I highlight some of our communal shortcomings. For ex ample\, while we have recently improved our simulations and the inference they provide\, the single existing positive detection of an X-ray transit (HD 189733b) makes it difficult to evaluate or quantify astrophysical and instrumental systematic issues that are associated with general transit s imulations. The utility of solar templates for the diverse and different s pot coverage of young stars and M dwarfs is undemonstrated.\n\nhttps://mee tings.aip.de/event/16/contributions/128/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/128/ END:VEVENT BEGIN:VEVENT SUMMARY:A Brief Introduction to the SOlar Terrestrial Habitability Explore r (SOTHE) DTSTART;VALUE=DATE-TIME:20220909T130000Z DTEND;VALUE=DATE-TIME:20220909T131500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-127@meetings.aip.de DESCRIPTION:Speakers: Jiajia Liu (University of Science and Technology of China)\nAmong more than 5000 exoplanets discovered up to now\, around 60 a re believed to be potentially habitable. The Sun-Earth system provides a u nique example based on which detailed insights into the properties\, forma tion\, evolution\, and thus habitability of exoplanets could be gained. Ho wever\, observing the Sun as a star and the Earth as an exoplanet has been rare. In this talk\, I will briefly introduce the SOlar Terrestrial Habit ability Explorer (SOTHE) to be deployed to the Sun-Earth L1 point around 2 025. SOTHE will carry 5 payloads to obtain the spectra of the Sun and the Earth at the same time\, together with images of the Earth at 7 unique pas sbands and the local plasma and magnetic field parameters at the L1 point. The core scientific goal of SOTHE is to conduct the first-ever simultaneo us spectral observations of the Sun and Earth to explore key characteristi cs related to the habitability of the Sun-Earth system and provide a uniqu e baseline for habitable exoplanets exploration.\n\nhttps://meetings.aip.d e/event/16/contributions/127/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/127/ END:VEVENT BEGIN:VEVENT SUMMARY:Variable atmospheric dynamics of planets experiencing gravity-dark ened seasons DTSTART;VALUE=DATE-TIME:20220907T103000Z DTEND;VALUE=DATE-TIME:20220907T104500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-124@meetings.aip.de DESCRIPTION:Speakers: Anusha Pai Asnodkar (The Ohio State University)\nPla nets on misaligned orbits around rapid rotators can experience “gravity- darkened seasons” as their orbits cross over the hot poles and cooler eq uators of rotationally-flattened stars. The periodically variable heating from these seasons presents a unique case for exploring how changes in ste llar irradiation influence planetary atmospheric dynamics. We perform a ho mogeneous analysis of day-to-nightside winds on the ultra-hot Jupiters KEL T-9 b and KELT-20 b\, enabling the comparison of a planet experiencing gra vity-darkened seasons (KELT-9 b) with a similar planet that does not (KELT -20 b). We conduct high-resolution transmission spectroscopy using two tra nsits observed by the PEPSI spectrograph on the Large Binocular Telescope to empirically constrain supersonic ~10 km/s day-to-nightside winds traced by Fe II features in the atmosphere of KELT-9 b. Reconciling our findings with two archival HARPS-N datasets suggests multi-epoch variability ~5-8 km/s over timescales between weeks to years. In contrast\, KELT-20 b’s d ay-to-nightside winds are less rapid (~2 km/s) and stable across four tran sits collectively observed by PEPSI and HARPS-N. The observed contrast of KELT-9 b’s wind variability and KELT-20 b’s stability is in accordance with our intuition on the effect of gravity-darkened seasons. A qualitati ve evaluation of our measured wind velocities and variability against curr ent ultra-hot Jupiter GCMs reveals that KELT-9 b poses unique challenges f or validating giant planet atmospheric models.\n\nhttps://meetings.aip.de/ event/16/contributions/124/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/124/ END:VEVENT BEGIN:VEVENT SUMMARY:From cross-correlations to likelihoods: What can we do with high-r esolution transmission spectroscopy? DTSTART;VALUE=DATE-TIME:20220908T074500Z DTEND;VALUE=DATE-TIME:20220908T080000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-122@meetings.aip.de DESCRIPTION:Speakers: Neale Gibson (Trinity College Dublin)\nHigh-resoluti on Doppler-resolved spectroscopy has opened up a new window into the atmos pheres of both transiting and non-transiting exoplanets. While the 'classi cal' cross-correlation approach is efficient for finding atomic and molecu lar species\, it is quite limited with its inability to recover quantitati ve information on the atmosphere such as abundances and temperature profil es - the very information we need to understand planetary atmospheres! Her e\, I will outline a new retrieval framework based on a simple Gaussian li kelihood coupled to a fast model-filtering technique that is critical to a ccount for the common pre-processing steps performed on time-series spectr a. I will demonstrate its use including the first retrievals of high-resol ution transmission spectra\, showcasing multiple detections of neutral and ionised metals (Fe\, V\, Mg\, Cr\, FeII\, etc) in ultra-hot Jupiters\, wh ich in turn place robust and precise constraints on abundance ratios and t emperature-pressure profiles\, as well as directly constrain the mean line -profile. However\, to fully realise the power of high-resolution spectros copy - which is sensitive to winds and atmospheric escape - it is clear th at we need to treat highly irradiated planets as 3D objects. This is incom patible with the requirement for ultra-fast forward model atmospheres whic h make high-resolution retrievals viable in the first place. I will finish by discussing some open questions and current limitations of high-resolut ion atmospheric retrievals\, with the goal of encouraging discussion of th e best routes forward.\n\nhttps://meetings.aip.de/event/16/contributions/1 22/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/122/ END:VEVENT BEGIN:VEVENT SUMMARY:Sodium in the atmosphere of WASP-7 b observed with UVES DTSTART;VALUE=DATE-TIME:20220907T144500Z DTEND;VALUE=DATE-TIME:20220907T150000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-121@meetings.aip.de DESCRIPTION:Speakers: Hossein Rahmati (Bu-Ali Sina University)\nContext. T ransmission spectroscopy is a prime technique to study the chemical compos ition and structure of exoplanetary atmospheres. Strong excess absorption signals have been detected in the optical Na I D1\, 2 Fraunhofer lines dur ing transits of hot Jupiters\, which are attributed to the planetary atmos pheres and allow us to constrain its structure.\nAims. We study the atmosp here of WASP-7 b by means of high-resolution transit spectroscopy in the s odium lines.\nMethods. We analyze a spectral transit time-series of 89 hig h-resolution spectra of the hot Jupiter WASP-7 b that was observed using t he Ultraviolet and Visual Echelle Spectrograph (UVES). We use the telluric lines for an accurate alignment of the spectra and carry out a telluric c orrection with molecfit. Stellar magnetic activity is monitored by investi gating chromospheric lines such as the Ca ii\nH and K and hydrogen Hα lin es. Finally\, we obtain transmission spectra and light curves in the sodiu m lines region.\nResults. The star shows no identifiable flares and\, if a ny\, marginal changes in activity during our observing run. The sodium tra nsmission spectra and corresponding light curves clearly show signs of the Rossiter-McLaughlin effect (RM) and the stellar center-to-limb variation (CLV) that we model using synthetic spectra. A statistically significant\, narrow absorption feature with a line contrast of 0.47 ± 0.06 % and a FW HM of 0.13 ± 0.03 Å is detected at the location of the Na I D2 line. For the Na I D1 line signal\, we derive an upper limit of 0.12 %.\n\nhttps:// meetings.aip.de/event/16/contributions/121/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/121/ END:VEVENT BEGIN:VEVENT SUMMARY:Characterization of exoplanetary atmospheres with SLOPpy DTSTART;VALUE=DATE-TIME:20220908T100000Z DTEND;VALUE=DATE-TIME:20220908T101500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-120@meetings.aip.de DESCRIPTION:Speakers: Luca Malavolta (Dipartimento di Fisica e Astronomia - Università degli Studi di Padova)\nHigh-resolution transmission spectro scopy is one of the most fruitful techniques to infer the main opacity sou rces\, thermospheric temperature and evaporation processes in the atmosphe re of transiting exoplanets. Before retrieving the planetary features\, ho wever\, observed spectra must be corrected for sky emission\, residual atm ospheric dispersion\, presence of telluric features and interstellar lines \, center to limb variation\, and Rossiter-McLaughlin effect\, with each o f these steps possibly introducing systematic errors and altering the fina l transmission spectrum. The current lack of a public tool able to automat ically extract a high-resolution transmission spectrum creates a problem o f reproducibility of scientific results. As a consequence\, it is very dif ficult to compare the results obtained by different research groups and to do a homogeneous characterization of the properties of exoplanetary atmos pheres. In this talk I will present a standard\, publicly available\, user -friendly tool\, named SLOPpy (Spectral Lines Of Planets with python\, Sic ilia et al. submitted)\, that automatically extracts the optical transmiss ion spectrum of exoplanets and allows the perfect reproducibility of resul ts. To validate the code and assess its performance\, we performed a compa rison with literature results of ideal targets for atmospheric characteriz ation observed with HARPS and HARPS-N\, finding a good agreement with publ ished results. I will conclude the talk by highlighting a series of best p ractices that can greatly improve the reproducibility of results even when the analysis tools are not publicly released.\n\nhttps://meetings.aip.de/ event/16/contributions/120/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/120/ END:VEVENT BEGIN:VEVENT SUMMARY:Towards Characterizing Atmospheres of Terrestrial Planets DTSTART;VALUE=DATE-TIME:20220909T080000Z DTEND;VALUE=DATE-TIME:20220909T081500Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-117@meetings.aip.de DESCRIPTION:Speakers: Ray Jayawardhana (Cornell University)\nWe aim to cha racterize transiting exoplanets spanning a wide range of sizes\, masses an d effective temperatures using a variety of high-resolution spectrographs\ , including through our on-going Gemini Large Program “Exploring the Div ersity of Exoplanet Atmospheres at High Spectral Resolution” (ExoGemS\, for short) with Gemini-N/GRACES. Here I will share a few early results fro m ExoGems\, and present our new\, complementary study of GJ 486b\, a 1.3-E arth-radius planet around a nearby M dwarf. Given its high transmission sp ectroscopy metrics\, GJ 486b is a compelling target for constraining an at mosphere in the terrestrial size regime. We observed three planetary tran sits with Subaru/IRD\, Gemini-S/IGRINS and CFHT/SPIRou\, and searched for absorption by a multitude potential atmospheric species. We are able to ru le out a H/He-dominated atmosphere with solar abundances to a confidence o f >5σ and a 100% water atmosphere to a confidence of 3σ. We also investi gate the implications of our results for the upcoming JWST transit observa tions of GJ 486b. Our findings suggest that terrestrial planets orbiting M -dwarf stars may experience significant atmospheric loss.\n\nhttps://meeti ngs.aip.de/event/16/contributions/117/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/117/ END:VEVENT BEGIN:VEVENT SUMMARY:Dynamic duos\, the interaction between exoplanet atmospheres and t heir host stars DTSTART;VALUE=DATE-TIME:20220909T141500Z DTEND;VALUE=DATE-TIME:20220909T143000Z DTSTAMP;VALUE=DATE-TIME:20240704T115815Z UID:indico-contribution-16-112@meetings.aip.de DESCRIPTION:Speakers: Gwenael Van Looveren (University of Vienna)\nWith ad vances in exoplanet detection\, thousands exoplanets have been discovered including almost 200 confirmed rocky exoplanets. This leaves us with a lar ge number of possible targets in the search for biomarkers. A quick look a t our own solar system shows that not every planet can hold on to a signif icant or habitable atmosphere for an extended amount of time. Whether a pl anet can hold on to its atmosphere depends strongly on the XUV radiation o f the star and the chemical composition of the atmosphere. To this end we use the Kompot code\, an upper atmosphere thermo-chemical code\, developed at the University of Vienna. By modelling the interaction between these t wo factors we can exclude scenarios where the atmosphere would not survive long enough for possible life to form. This work will also present how gr ids of such model atmospheres can be used to constrain the chemical compos ition and identify which biomarkers remain abundant under the stellar radi ation.\n\nhttps://meetings.aip.de/event/16/contributions/112/ LOCATION:Leibniz Institute for Astrophysics Potsdam (AIP) Lecture Hall URL:https://meetings.aip.de/event/16/contributions/112/ END:VEVENT END:VCALENDAR