Listing of Poster Abstracts

Detailed dark matter maps of galaxy cluster substructure and direct comparison to simulations

Dr.  Dan Coe (JPL / Caltech)

Images from the next generation of telescopes will enable strikingly detailed reconstructions of the dark matter distributions in galaxy cluster cores using strong gravitational lensing analysis. This will provide a key test of Lambda-CDM cosmology on cluster scales where tensions currently exist. Observed dark matter distributions will be compared directly to those realized in simulations, forgoing any assumptions about light tracing mass. The required observations are deep, multicolor, and high-resolution, ideally supplemented with spectra of faint objects. ACS onboard HST is capable of obtaining images of sufficient quality, but for prohibitive integration times. The next generation of telescopes promises to efficiently yield the required images. An analysis method capable of processing the expected large numbers of multiple images has been developed. The full range of constraints possible from analyzing these detailed mass maps is a matter of ongoing investigation.

Matching the Local and Cosmic Star Formation Histories with a Large-Aperture Optical/UV Space Telescope

Dr.  Igor Drozdovsky (Instituto de Astrofisica de Canarias)

Our view on the formation and evolution of nearest galaxies was majority influenced by the excellent resolving power and throughput in UV and optical wavelength of the HST. These studies were based on the ``galaxy archeology'' - the detailed study of the resolved stellar populations in the Local Group galaxies, in order to reconstruct their star formation and chemical evolution histories. The methodology is well tested and based on: the photometric analysis of resolved stellar populations down to the oldest main-sequence turn-off, short-period radially pulsating stars (such as RR Lyrae and Cepheids), and low-resolution spectroscopy of evolved stars. So far this kind of studies were limited to the nearest galaxies of the Local Group. Using the Next Large (>4 m) Aperture Optical/UV Space Telescope will allow an extension of all-ages fossil records studies beyond of the Local Group and out to the Virgo Cluster, across the entire Hubble sequence of galaxies --in all environments-- and will allow us to understand the global, cumulative evolution of the Local Universe.

The Road Map for UV Astrophysics Developed by the European Network for Ultraviolet Astronomy (NUVA)

Prof.  Ana Gómez de Castro (Universidad Complutense de Madrid)

The Network for UltraViolet Astrophysics (NUVA) was first established within the OPTical Infrared COordination Network for astronomy (OPTICON),financed by the European Union via the Framework VI program. (www.ucm.es/nfo/nuva) This network has been defined to the identificate the needs and to develop the actions to structure the European astronomical community around a single large ultraviolet project. The objectives of the NUVA are to formulate and operate a UV astronomy network and to plan and execute a road mapping exercise. The current status of the NUVA work will be reported

Science with the Swift Ultraviolet/Optical Telescope

Dr.  Caryl Gronwall (Pennsylvania State University)

Currently there are four operating near-UV imaging space telescopes, one of which is the Swift Ultra-Violet/Optical Telescope (UVOT). Although the UVOT's primary missiosn observations of gamma-ray burst afterglows, it is a powerful instrument for exploring the nature of the ultraviolet universe. The UVOT has a 30 cm aperture, an f -number of 12.7 after the secondary mirror, and is of a modified Ritchey-Chrétien design. The detector is a micro-channel-plate intensified CCD and operates in a photon counting mode. UVOT has a pixel scale of 0.5 arcsec per pixel and a field of view of 17 x 17 arcmin. The wavelength response of the UVOT is 160–800 nm with a ∼2 FWHM telescope. Here we discuss the properties of the UVOT and summarize some of the science undertaken with the UVOT. On-going science project with the UVOT include from UV observations of supernovae, nearby star-forming galaxies, active galaxies, and deep UV imaging of the high-redshift universe. We also present future goals for the UVOT and discuss some lessons learned that apply to future UV telescopes.

From Cosmic Dawn to Our Solar System: A Next-Generation UV-Optical Space Facility for the Study of Star Formation

Dr.  Rolf Jansen (Arizona State University, School of Earth & Space Exploration)

We summarize our science case for a UV--Optical Space Facility that includes a wide-field mid-UV--near-IR (190--1100nm) dichroic camera and a far-UV (100--175nm) high-resolution spectrograph. We then present two possible implementations for such a facility: a camera and spectrograph on a 4m-class planet-finding mission under study as part of NASA's present ASMCS program, and a proposed concept for a dedicated 1.65m 'Star Formation Observatory'. Our aim is to conduct a *comprehensive* and *systematic* study of the astrophysical processes and environments relevant for the births and life cycles of stars and their planetary systems, and to investigate and understand the range of environments, feedback mechanisms, and other factors that most affect the outcome of the star and planet formation process. Via a 4-Tier program, we will step out from the nearest star-forming regions within our Galaxy (Tier 1), via the Magellanic Clouds and Local Group galaxies (Tier 2), to other nearby galaxies out to the Virgo Cluster (Tier 3), and on to the early cosmic epochs of galaxy assembly (Tier 4). Interpretation of the panchromatic imaging is intimately tied to far-UV R>~30,000 spectroscopic observations. Each step will build on the detailed knowledge gained at the previous one. Such a study, which addresses the origins and evolution of stars, galaxies, and cosmic structure, also has direct relevance for the formation and survival of planetary systems such as our own Solar System and planets such as Earth. This work is supported by NASA-GSFC contract NNX08AK79G (07-ASMCS07-0022).

Understanding Physical Processes in the Diffuse Interstellar Medium Using High-resolution UV Spectroscopy

Prof.  Jeffrey Linsky (JILA)

High-resolution UV spectroscopy with the GHRS and STIS instruments on HST and FUSE has provided valuable new information on the structure and physical properties of nearby diffuse gas in the ISM. However, future high-resolution instruments with greater sensitivity are needed to answer many important questions, including (1) are all or most warm gas clouds filamentary and on what scale, (2) what physical processes occur when clouds interact, (3) why is there severe pressure disequilibrium in the ISM, and (4) what physical processes occur at the edges of warm clouds embedded in hot gas? Interstellar gas in the nearby Galactic disk should provide useful prototypes for interstellar gas in the more distant universe but is much easier to study with less confused lines of sight.

New Technologies for Probing the Diversity of Brown Dwarfs and Exoplanets

Prof.  Eduardo Martin (IAC)

We will present an international meeting that will focus on the technological developments that are needed to make significant progress on the observational front for advancing in understanding of substellar-mass objects. These advancements will lead to cutting edge discoveries of new types of exoplanets and brown dwarfs such as habitable rocky planets and Y dwarfs, respectively. It will provide a venue to encourage collaboration, interactions and synergies between specialists in different technologies. During the meeting, the participants will also have the opportunity to witness the total solar eclipse of 22nd of July 2009, which will last around 6 minutes (the longest of this century) in the Shangai region.

Neutron Star Astronomy after HST and JWST

Dr.  Roberto Mignani (UCL-MSSL)

In this poster I will shortly review the major outcomes in neutron star astronomy obtained by the HST and their scientific impacts as well as the science goals achievable with the JWST and for its successor.

ATLAST configured for an EELV

Dr.  Bill Oegerle (NASA/GSFC)

We present the results of a study of a deployable version of the Advanced Technology Large Aperture Space Telescope (ATLAST) that could be launched on an Evolved Expendable Launch Vehicle (EELV). The observatory retains significant heritage from JWST, thereby taking advantage of technologies and engineering already developed for that mission. At the same time, we have identified several design changes to the JWST architecture, some of which are required due to the demanding wavefront error requirements at visible wavelengths. The optical telescope assembly has a segmented 9.2 meter aperture and consists of 36 hexagonal glass mirrors, each of which are 1.315m in size (flat-to-flat). The folding of the telescope is similar to JWST, and will fit in the 6.5m fairing on the planned upgrade to the Delta-IV heavy launch vehicle. Wavefront sensing and control is performed on-board the telescope using stars in the field of view in near real-time. The total budget on wavefront error is 40nm RMS, in order to provide diffraction limited imaging performance at 500nm wavelength. The optical design of the telescope provides an 8x20 arcmin FOV in which 4-7 instruments can be accommodated, plus fine guidance and wavefront sensors. Unlike JWST, the OTA sits at the end of a multi-gimbaled arm, allowing pitch and roll motion, and is isolated from the sunshield and spacecraft bus by an active isolation system. The sunshield is kept at a fixed angle to the sun, and the OTA's position can be adjusted to balance torque due to solar photon pressure. The stowage and deployment of the sunshield are also presented. Our design permits servicing in order to extend the life of the observatory.

The Exoplanetary Circumstellar Environments And Disk Explorer: A Science and Techology Pathfinder for the Pupil mapping Exoplanet Coronagraphic Observer

Dr.  Glenn Schneider (Steward Observatory, University of Arizona)

The EXoplanetary Circumstellar Environments and Disk Explorer (EXCEDE) is a precursor science and technology pathfinder to the Pupil mapping Exoplanet Coronagraphic Observer, designed to fit within a SMEX mission cost cap. EXCEDE will directly image starlight-scattering circumstellar material in the planet-forming regions of stars exhibiting thermal infrared emission above their stellar photospheric levels (a signpost of planetary systems in formation). EXCEDE will provide contrast-limited scattered-light detection sensitivities 100 to 1000 times more sensitive than the HST and JWST coronagraphs at a smaller inner working angle, enabling the exploration and characterization of exoplanetary circumstellar disk systems in currently inaccessible observational domains. Utilizing a laboratory-demonstrated high-performance Phase Induced Amplitude Apodized Coronagraph (PIAA-C), integrated with a 50 cm diameter unobscured aperture visible-light telescope, EXCEDE will provide an unrivaled disk-to-star imaging contrast of < 10^-7 and a 1 lambda/d inner working angle of 0.2" with 0.2” spatial resolution at 0.4 microns. Such unprecedented spatially-resolved circumstellar disk images, polarimetrically analyzed at two wavelengths, will enable determinations of disk characteristics (mass, geometry, surface brightness, grain properties) for stars over a wide range of stellar mass and age, providing a unique and comprehensive dataset to understand the formation and evolution of extrasolar planetary systems. Concomitantly, EXCEDE will provide unparalleled imagery of those rare debris disks previously resolved with inferior capabilities. These "Rosetta stones" are the basis of our current understanding of planetary disk systems and EXCEDE observations will overcome current limitations that thus-far have resulted in significant model degeneracies. EXCEDE will also directly image and characterize extrasolar giant planets with orbital distances as small as 1.5 AU and disk sub-structures influenced by co-orbiting planets - for the first time within the terrestrial planet zone (< 5 AU) around the nearest stars - while providing future missions well-honed targets sets for follow-on and multi-wavelength investigations.

Time-Domain Solar System Science

Dr.  Michael H Wong (STScI)

Time-variable phenomena with scales ranging from minutes to decades have led to a large fraction of recent advances in many aspects of solar system science. We present the scientific motivation for the Planetary Dynamics Explorer (PDX)—a dedicated facility to conduct repeated imaging and spectroscopic observations over a period of 5 to 10 years. PDX will execute a selection of long-term projects with interleaved scheduling, resulting in the acquisition of data sets with consistent calibration, long baselines, and optimized sampling intervals. Specific investigations will include volcanism and cryovolcanism (on targets including Io, Titan, Venus, Mars, and Enceladus); zonal flow, vortices, and storm evolution on the giant planets; seasonal cycles in planetary atmospheres; mutual events and orbit determination of multiple small solar system bodies; auroral activity and solar wind interactions; and cometary evolution. The mission will produce a wealth of data products, such as multi-year time-lapse movies of planetary atmospheres, with significant E/PO potential. A distributed-aperture telescope would be an ideal configuration for the mission, trading decreased sensitivity for increased resolution as a strategy to reduce payload mass. Existing and planned ground- and space-based facilities are not suitable for these time-domain optimized planetary dynamics studies for numerous reasons, including oversubscription by astrophysical users, field-of-regard limitations, sensitive detector saturation limits that preclude bright planetary targets, and limited mission duration. PDX responds to the NRC Decal Survey "New Frontiers in the Solar System," which states, "The Survey prefers to rely on the Discovery and, where appropriate, the Explorer lines to generate appropriate candidates [for an] Earth-orbiting telescope devoted exclusively to solar system studies" (p. 166).