![]() ![]() Deep digital sky surveys, future UVOIR space observatoryĬoncepts, automated classification and cluster finding algorithms, astronomical data simulation,Ģ017 - present: Distinguished Astronomer, STScIġ996 - 2001 Associate Astronomer with tenure, STScIġ994 - 2002: Adjunct Associate Professor, JHUġ993 - 1994: Adjunct Assistant Professor, JHUġ986 - 1989: Postdoctoral Fellowship, Princeton Universityġ981 - 1986: Research Associate, Harvard UniversityĢ022 - present: Interim Deputy Director of STScIĢ005 - 2019: Head, Community Missions OfficeĢ010 - 2017: Principle Investigator, CLASHĢ008 - 2009: Principle Investigator, NASA Astrophysics Strategic Mission Concept Study:ġ997 - 2003: Head of the Multi-mission Archiive at STScIĢ002 - 2006: HST Advanced Camera for Surveys teamĢ019: NASA Silver Achievement Medal: TESS TeamĢ018: NASA Group Achievement Award: WFIRST Design Reference TeamĢ015: NASA Group Achievement Award: Advanced Mirror Technology Development TeamĢ013: AURA Outstanding Scientific Achievement AwardĢ010: P.I., HST Multi-Cycle Treasury Program: 524 OrbitsĢ008: P.I., NASA Astrophysics Strategic Mission Concept StudyĢ003: GSFC Group Achievement Award: ACS Flight Teamġ998: STScI Group Achievement Award: MASTġ995: STScI Group Achievement Award: Digitized Sky Survey CD-ROMsġ993: AURA Outstanding Scientific Achievement AwardĢ020 - present: Co-chair, Keck Obs. Physical properties of superclusters, gravitational lensing of distant galaxies, observationalĬonstraints on cosmological parameters. Galaxy distance indicators, morphology and dynamics of groups and clusters of galaxies, ![]() Margaret Geller)įormation and evolution of large-scale structure in the universe, large-scale velocity fields, ![]() About Research (back to top) My CV Publications Contact.The full cluster database, including dark matter maps and ancillary data, will be the largest uniform resource for the study of nearby galaxy clusters available before the release of the LSST Year 2 data (depending on the chosen cadence for LSST). Our data will reveal the full range of cluster galaxy populations, map the dark matter distribution on sub-cluster scales, test cluster scaling relations, reveal lensed sources and serve as the first epoch for the study of supernovae and other transients in and behind clusters with LSST. We obtain u,g,r,i,z images reaching at least to LSST Year-1 depth for the entire virial region of these clusters, which are close enough for detailed spectroscopic, X-ray, and radio analysis. Local Volume Complete Cluster Survey (LoVoCCS): We are conducting a complete survey of all massive galaxy clusters in the local (z < 0.12) Universe accessible to the Dark Energy Camera, DECam, in the southern hemisphere (104 clusters) and the Hyper Suprime-Cam, HSC, in the northern hemisphere (41 clusters). See the LUVOIR final report to NASA and the Astro2020 Decadal Review committee for a thorough description of LUVOIR's capabilities. I serve on the LUVOIR Science and Technology Definition Team and was the lead scientist on the design of LUVOIR's VIS-NIR imager instrument, HDI. LUVOIR will be the first telescope capable of performing a census of the exoplanets in the Habitable Zones of hundreds of stars like the Sun. LUVOIR's broad wavelength coverage, large aperture, and powerful instruments will revolutionize much of astronomy. LUVOIR: Space Telescope Concept for the 2030s. Explaining it with undetected galaxies requires the galaxy-count faint-end slope to steepen markedly at V>24 or that existing surveys are missing half the galaxies with V 7 (when the Universe was younger than 800 million years old - or less than 6% of its current age) and (4) Study the internal structure and evolution of the galaxies in and behind these clusters. Subtraction of the integrated light of galaxies (IGL) fainter than the photometric detection-limit from the total COB level leaves a diffuse flux component of unknown origin. ![]() Doing these subtractions yields a highly significant detection of the COB. Isolating the COB contribution to the raw total requires subtracting scattered light from bright stars and galaxies, faint stars below the photometric detection-limit within the fields, and diffuse Milky Way light scattered by infrared cirrus. This is about 10 times darker than the darkest sky accessible to the Hubble Space Telescope, highlighting the utility of New Horizons for detecting the cosmic optical background (COB). The average raw level measured while New Horizons was 42 to 45 AU from the Sun is 33.2 (+/-0.5) nW/m^2/sr. Highlights of my recent and current research collaborations:Ĭosmic Optical Background: using data from the LORRI camera onboard the New Horizons probe, we measured the optical-band sky brightness within seven high galactic latitude fields. ![]()
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