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HUBBLES SCIENCE LEGACY: FUTURE OPTICAL-UV ASTRONOMY FROM SPACE INVITED TALKS Speaker Anne Kinney, NASA Headquarters Title Building the vision of the Future in Space Astronomy & Physics Abstract This talk will present the NASA and OSS process and rationale for the strategic planning and road mapping. The content of the current program in the Astronomy and Physics division will be presented, and the possibilities and procedures for including new content will be discussed. Speaker Alvaro Gimenez, ESTEC, The Netherlands Title The Future of Optical Astronomy in ESA's Science Programme Abstract A summary of the present status of the Science Programme of the European Space Agency will be presented, followed by a more focused discussion on the main activities in the field of optical astronomy. The missions are defined in response to specific and relevant scientific questions rather than trying to provide general-purpose facilities. In this context, GAIA will provide the necessary tool to understanding our Galaxy and its content, by surveying around one billion stars, whilst Eddington is aimed at the study of stellar structure and the search for extra-solar earth-like planets in the habitable zone. Moreover, technology developments are being pursued to ensure the availability of focal plane arrays of detectors with the required performances as well as to test capabilities in space interferometry. Speaker Roberto Gilmozzi, ESO Munich, Germany Title Ground based astronomy in 2010-2020 Abstract The second decade of the third millennium will be characterized by the mature phase of the present generation of 8 to 10m telescopes, with a complement of instruments performing at the diffraction limit through adaptive optics. Interferometry will have entered the 'faint object' regime, with VLTI obtaining milliarcsecond(s) resolution on K~20 sources. ALMA will explore the mm and sub-mm universe both locally and at very high redshifts. And one or more of the new generation of 30 to 100m telescopes (CELT, GSMT, OWL) will be in construction or starting operations. I will review the expected performance and science cases for these projects (with a slight bias for those in which ESO is involved). I will also briefly discuss the complementarities among these facilities, and between these and space missions. Speaker Alan Dressler, Carnegie Observatory Title The Optical-IR Astronomy Landscape in 2015 Speaker Martin Harwit, Cornell University Title Thoughts on a Powerful New Ultraviolet Facility Abstract The talk will seek to examine the potential of a large ultraviolet space telescope and its prospective instrumental components in the context of our continuing search through the Universe. Speaker Michael Shull, The University of Colorado at Boulder Title Highlights of the SUVO Study Abstract I provide a summary of the scientific and technological goals of the SUVO (Space Ultraviolet- Visible Observatory) mission study, commissioned by NASA in 1998-99. The full report may be obtained as the SUVO white paper, available at astro-ph/9907101 and on the UVOWG website: http://origins.colorado.edu/uvconf/uvowg.html. The UVOWG was asked to study the scientific rationale for new missions in ultraviolet/optical space astronomy. A large-aperture telescope in space would provide a major facility for understanding the Emergence of the Modern Universe and for addressing such issues as: (1) mapping dark baryons, metals, large- scale structure, and dark-energy equation of state; (2) detecting unseen matter through weak gravitational lensing; (3) studying the feedback from star formation; and (4) measuring the evolution of stars, planets, and elements from red shifts z = 3-4 down to the current epoch. In the last several years, it appears possible that the SUVO concept might also address exciting new goals in the study of extra-solar planets and their atmospheres, through UV/O coronagraphy. The UVOWG studied both 4m and 8m telescopes, and made recommendations about the critical technology development for high-quantum-efficiency ultraviolet detectors, gratings, mirrors, spectrographs, and wide-field optical/UV imagers (at least 16K x 16K). Speaker Peter Garnavich, The University of Notre Dame Title The Future of Supernova Research Abstract Supernovae are the movers and shakers of the Universe. They provide most of the heavy elements, energize the interstellar medium and their shocks can induce stars to form. Type Ia supernovae are the brightest, most precise distance indicators around and provide estimates of key cosmological parameters. The future of supernova research is bright as new facilities can help address key problems in a variety of fields. Supernovae are UV beacons which permit us to measure properties of the interstellar medium in our own and other galaxies. The slow- motion train wreck that is SN 1987A has really just begun and over the next 20 years X-ray, UV, optical and IR observations will illuminate how shocks work and how massive stars evolve. There is some evidence today that SN and GRB are linked, but much more needs to be learned about the symmetry of SN explosions and jets. And a key cosmological question concerns the progenitors and properties of type Ia supernovae. Future facilities require a rapid response to new discoveries to fully utilize the power of supernovae. Speaker John Hutchings, Dominion Astrophysical Observatory Title Accretion binaries and other stellar problems Abstract I will discuss accretion phenomena in binaries that also have wider implications. Future progress in some of these will require new optical-UV facilities in space, which will be outlined. Some other stellar topics will be mentioned that also require a new orbiting facility. Speaker Andrea Dupree, Harvard-Smithsonian, Center for Astrophysics Title Cool Stars And The Future Abstract Recent discoveries selected from ultraviolet spectroscopy and imaging of cool stars define challenging questions for future observations ranging from planet-cool star interactions, imaging of stellar surfaces and environments, to pursuit of faint objects populating the depths of globular cluster cores. Spectroscopy of fiducial galactic stars and star clusters and study of abundances, atmospheric structures, winds and mass loss drive future opportunities involving stars and clusters associated with extragalactic objects. Speaker Guisseppe Bono, Observatory of Rome Italy Title Evolutionary and pulsational properties of intermediate-mass stars: current odds and future perspectives Abstract We briefly discuss the theoretical scenario concerning evolutionary and pulsational properties of intermediate-mass stars. In particular, we focus our attention on current discrepancies between predicted and empirical Color-Magnitude diagrams during the helium burning phases (blue loops). We also outline the impact that new Optical-UV data will have on the pulsation properties of classical Cepheids, and in turn on the Cepheid distance scale. Speaker Michael Meyer, The University of Arizona, Steward Observatory Title Beyond the Cosmic Veil: Space-based Star and Planet Formation Research after SIRTF & NGST Abstract What physical processes are responsible for determining the final masses of forming stars and ultimately the initial mass function? How do planets form from circumstellar disks of gas and dust? The Hubble Space Telescope has made major contributions in helping to address these fundamental questions. In the next decade, the Space Infrared Telescope Facility (SIRTF) and the Next Generation Space Telescope (NGST) will build on this heritage in the near- to far- infrared. However several crucial questions will remain. We will review recent progress made in star and planet formation with HST, key science objectives for SIRTF and NGST, and suggest problems that are uniquely suited to large aperture UV/optical space-based telescopes. We will focus on studies that take advantage of high spatial resolution and the unique wavelength range inaccessible from the ground such as: 1) extreme populations of young stars in the local group (UV observations of massive star-forming regions); and 2) circumstellar disk structure and composition (observed in scattered light images of dust and UV spectroscopy of gas). Speaker Lee Hartmann, Harvard-Smithsonian Center for Astrophysics Title Problems in Star and Planet formation Abstract I outline some of the major unresolved questions in the field of star formation and early evolution of proto-planetary disks, with special emphasis on those issues that might be best resolved with a large space optical/UV telescope. One possible area is to determine whether the high-mass end of the stellar IMF is or is not environment-dependent; extragalactic studies in regions with much more extreme conditions than found in the Milky Way may be essential to settling this question. Our knowledge of the rate of material accreting through proto- planetary disks is dependent on observations in the blue-ultraviolet region, and needs to be expanded dramatically if we are to understand the physics of disk accretion. The chemistry and possibly evolution of proto-stellar disks may be crucially dependent upon FUV fluxes from young stars, which are poorly known at present. UV observations may also be essential to understanding how the gas is dispersed from disks, an unknown but crucial issue in understanding planetary formation and migration. Understanding the basic properties of proto- stellar jets and winds may only be possible with UV observations. Finally, images in scattered light at short
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  • The SPLASH Survey: Internal Kinematics, Chemical Abundances

    The SPLASH Survey: Internal Kinematics, Chemical Abundances

    Draft version October 29, 2018 Preprint typeset using LATEX style emulateapj v. 2/19/04 THE SPLASH SURVEY: INTERNAL KINEMATICS, CHEMICAL ABUNDANCES, AND MASSES OF THE ANDROMEDA I, II, III, VII, X, AND XIV DSPHS1,2 Jason S. Kalirai3, Rachael L. Beaton4, Marla C. Geha5, Karoline M. Gilbert6,7, Puragra Guhathakurta7, Evan N. Kirby7,8,9, Steven R. Majewski4, James C. Ostheimer4, Richard J. Patterson4, and Joe Wolf10 Draft version October 29, 2018 ABSTRACT We present new Keck/DEIMOS spectroscopic observations of hundreds of individual stars along the sightline to Andromeda’s first three discovered dwarf spheroidal galaxies (dSphs) – And I, II, and III, and leverage recent observations by our team of three additional dSphs, And VII, X, and XIV, as a part of the SPLASH Survey (Spectroscopic and Photometric Landscape of Andromeda’s Stellar Halo). Member stars of each dSph are isolated from foreground Milky Way dwarf and M31 field contamination using a variety of photometric and spectroscopic diagnostics. Our final spectroscopic sample of member stars in each dSph, for which we measure accurate radial velocities with a median uncertainty (random plus systematic errors) of 4 – 5 km s−1, includes 80 red giants in And I, 95 in And II, 43 in And III, 18 in And VII, 22 in And X, and 38 in And XIV. The sample of confirmed members in the six dSphs are used to derive each system’s mean radial velocity, intrinsic central velocity dispersion, mean abundance, abundance spread, and dynamical mass. This combined data set presents us with a unique opportunity to perform the first systematic comparison of the global properties (e.g., metallicities, sizes, and dark matter masses) of one-third of Andromeda’s total known dSph population with Milky Way counterparts of the same luminosity.