0 Assigned ID: 67 ----- Attempting Submission 1 (Mon Mar 02 00:48:58 GMT 2020) ----- HST Phase I Proposal 67 successfully submitted. Receipt: # 67-1 ----- Attempting Submission 2 (Wed Mar 04 16:52:59 GMT 2020) ----- HST Phase I Proposal 67 successfully submitted. Receipt: # 67-2 ----- Attempting Submission 3 (Fri Mar 06 02:49:33 GMT 2020) ----- HST Phase I Proposal 67 successfully submitted. Receipt: # 67-3 ----- Attempting Submission 4 (Fri Mar 06 03:11:21 GMT 2020) ----- The ULLYSES DDT Survey of low-mass pre-main sequence stars, coupled with forthcoming data from ALMA and JWST, will provide the foundation to revolutionize our understanding of the relationship between young stars and their protoplanetary disks. A comprehensive evaluation of the physics of disk evolution and planet formation requires understanding the intricate relationships between the mass accretion, mass outflow, and disk structure. Our team of 55 young star experts from around the world will bring their combined knowledge to bear on the ULLYSES FUV spectral database, ensuring a uniform and systematic approach in order to (1) measure how the accretion flow depends on the accretion rate and magnetic structures, (2) determine where winds and jets are launched and how mass loss rates compare to accretion, and (3) establish the influence of FUV radiation on the chemistry of the warm inner regions of planet-forming disks. We will also work together to acquire and provide contemporaneous observations at X-ray, optical, near-IR, and mm wavelengths to enhance the impact of the ULLYSES data. By the end of our comprehensive 3-year program, we will provide the best measurements of the levels and evolution of mass accretion of protoplanetary disks, the properties and magnitudes of (inner) disk mass loss, and the UV radiation fields that determine ionization levels and drive disk chemistry. This team addresses the need for labor essential to maximize the scientific return on the ULYSSES DDT young star program, in line with funding requests allocated to Legacy GO programs or Treasury programs. The ODYSSEUS team is led by PI Gregory Herczeg (non-US) and co-PI Catherine Espaillat (US, ADMIN PI for US Funds), plus Nuria Calvet (US), Kevin France (US), and Carlo Manara (non-US) as Executive Committee members. Funding will be focused primarily on labor at Boston University (budgetary PI Espaillat), University of Michigan (budgetary PI Calvet), University of Colorado (budgetary PI France), and Rice University (budgetary PI Chris Johns-Krull). Will Fischer has been the key intermediary between our team and STScI. Our team has extensive experience in far-ultraviolet spectroscopy, including COS, to study accretion, winds/jets, and disks of T Tauri stars. We also include many experts on the physics and chemistry of T Tauri stars and their disks across all relevant wavelengths (X-rays to sub-mm), to access complementary tools (e.g., Zeeman Doppler Imaging, photospheric analyses from high-resolution spectra), exploit synergies across different types of observations, and to help obtain coordinated observations. The inclusion of experts in physics and observations at other wavelengths should also help to expand FUV expertise to a broader community. Our team has four PhD students. We will focus funding from this proposal to hire additional students and postdocs. Our membership rules are below, with apologies for ascii formatting. =========== ODYSSEUS: MEMBERSHIP RULES 2019 March 24 The ULLYSES spectroscopy of disk-hosting stars will form a lasting legacy to the community, with data made available to everyone. Our complementary Legacy archival program is designed to extract and publish the exciting science that will be produced by the survey by supporting science across the community, in keeping with the accessibility of the legacy dataset. These rules are intended to motivate active participation and contributions within the team, to provide guidelines that facilitate cooperation and dissemination of data, and to protect students and postdocs within the team who are actively working on projects. We especially encourage new students and postdoc-level researchers from within the community to get involved in and contribute to this program, including taking the lead on papers. Our team is designed to be inclusive of all those interested in participating, subject to these management rules and guidelines. Team Management Executive Committee: All major decisions will be determined by majority opinion of the executive committee, following discussions. The executive committee will consist of the following science coordinators: Nuria Calvet (University of Michigan), Kevin France (University of Colorado), and Carlo Manara (ESO), in addition to the PI, Gregory Herczeg (Peking University/KIAA) and Co-PI Catherine Espaillat (Boston University). PI Decisions: For efficiency, all minor matters should be decided upon either by the relevant Science Coordinator, by PI Gregory Herczeg or by Co-PI Catherine Espaillat. Any decisions may be appealed to the executive committee. Science Coordinators: Science coordinators will be defined as a team member responsible for leadership and coordinating science output in their respective science sub-team. When appropriate, these roles will be assigned to those who have taken on responsibility for some specific aspect of the science, including X-ray/FUV connections (Christian Schneider), FUV-ZDI connections (Jerome Bouvier and the SPIRou team), and optical spectroscopy through ESO (Carlo Manara). Team membership: Membership in this team will be offered to anyone who is interested in becoming an active participant, including by providing ancillary data, performing data analysis, or modeling. Paper and authorship guidelines Lead Author: The first author of all papers should be the person who has done the most work and development in analyzing and interpreting the data. Co-Authorship: Authorship on papers will be restricted to team members who have made a substantive contribution to the paper, including active roles in (a) analysis/interpretation of results, (b) writing sections of the paper, (c) played a critical role in obtaining the complementary observations that were used in the paper, and (d) development of new ideas not previously discussed. Final authorship decisions will be determined by the first author (or the relevant advisor, in cases of junior first authors), with consultation with the Executive Committee when necessary. We will strive for short authorship lists contained within individual sub-teams. Internal Refereeing: All papers must be submitted to an internal referee prior to submission. Authors should anticipate roughly two weeks for the internal referee report to be returned. Circulation: Papers will be uploaded to the wiki page and circulated to the entire team at least two weeks prior to submission, unless exceptional circumstances warrant immediate publication. All members may read and comment on these final drafts and submitted papers. Team members must keep these drafts confidential. Draft circulation: Team members are encouraged to upload in prep drafts to the wiki page to generate comments and keep others up-to date. Data and discussion management Project approval: Contributions in terms of labor, support and leadership of papers/projects, and development of new ideas are strongly encouraged. All projects require approval by the management team to avoid conflicts related duplication of effort on the same project. New projects from anyone within the team will be approved by the team except in cases of projects that are already under development by someone within the team. For projects with interest from more than one group, we will strive to seek solutions that allow for complementary projects. In cases of conflict that involve students and/or postdocs, priority will be given to students and then postdocs over other team members. Approved projects will be posted to the team website, with the lead and key contributors identified. Inactive projects: Active projects by members of this team will be protected from internal competition, following the goals listed above. Any project deemed inactive for 6 months will no longer be protected. Many papers take longer than 6 months for publication, so inactivity is defined as lack of progress rather than lack of a draft. Data access: Team members are strongly encouraged to obtain complementary data and disseminate this data to the team and community. Publication of this complementary data will be determined by the PI of that project, with permission granted at the outset of the project. Data restrictions: Members of the team agree to only publish ULLYSES-disk data for projects that are approved by the Executive Committee, until one year after the completion of the full program. This rule is designed to avoid needless duplication of effort and to discourage members of the team from exploiting membership in the team by using raw data for competing purposes. New projects, leadership of projects, and labor contributions are all strongly encouraged. Proposal restrictions: Members agree to not propose for HST archival funding based on the science explicitly included in this proposal. Data use in proposals: Any use of ULLYSES data in proposals does not need to be approved by the team. Any use of complementary data requires permission by the relevant PI for use in proposals. Discussions: All members will be encouraged to participate in telecons, email discussions, and group meetings about the science and data related to this proposal. Related science: Our team includes many modelers. We encourage their contributions and deeper collaborations between all members. All modeling papers are complementary to this program and are not subject to any of the rules or obligations described here, especially regarding authorship. Code of Conduct All members are expected to adhere to the code of conduct of the IAU, available here: https://www.iau.org/static/archives/announcements/pdf/ann16007a.pdf Discrimination or harassment of any kind is unacceptable. We reserve the right to remove any member following a complaint. If you are harassed or witness harassment by a team member, we encourage you to file a complaint to one of the coordinators. The executive committee will then discuss and vote upon removal. Stellar Physics and Stellar Types Exoplanets and Exoplanet Formation 0 Legacy false false true false false SUPPORTED