A5033191564- Astro and Planetary Science
- Planetary Science and Exploration
- Space Exploration and Technology
- Isotope Analysis in Ecology
- Geology and Paleoclimatology Research
- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Ionosphere and magnetosphere dynamics
- Astronomy and Astrophysical Research
- Astronomical Observations and Instrumentation
- Atmospheric Ozone and Climate
- Molecular Spectroscopy and Structure
- Space Science and Extraterrestrial Life
- Laser-induced spectroscopy and plasma
- Space Satellite Systems and Control
- Galaxies: Formation, Evolution, Phenomena
- Solar and Space Plasma Dynamics
- Photocathodes and Microchannel Plates
- Advanced Chemical Physics Studies
- Optical Coatings and Gratings
- Geomagnetism and Paleomagnetism Studies
- Adaptive optics and wavefront sensing
- Mass Spectrometry Techniques and Applications
- Advanced optical system design
- Gas Dynamics and Kinetic Theory
University of Central Florida
2010-2023
University of Arizona
2008
Laboratory for Atmospheric and Space Physics
2007-2008
University of Colorado Boulder
2004-2008
Johns Hopkins University Applied Physics Laboratory
2008
University of Maryland, College Park
2008
University of Colorado System
2007
University of Rochester
1982
We present the Bolocam Galactic Plane Survey (BGPS), a 1.1 mm continuum survey at 33 effective resolution of 170 square degrees visible from northern hemisphere.The BGPS is one first large area, systematic surveys in millimeter without
We present a catalog of 8358 sources extracted from images produced by the Bolocam Galactic Plane Survey (BGPS). The BGPS is survey millimeter dust continuum emission northern plane. are using custom algorithm, Bolocat, which was designed specifically to identify and characterize objects in large-area maps generated instrument. products facilitate follow-up observations these relatively unstudied objects. 98% complete 0.4 Jy 60 over all object sizes for sensitive (<35). find that can best be...
MESSENGER from Mercury The spacecraft passed by in October 2008, what was the second of three fly-bys before it settles into planet's orbit 2011. Another visited mid-1970s, which mapped 45% surface. Now, after MESSENGER, only 10% Mercury's surface remains to be imaged up close. Denevi et al. (p. 613 ) use this near-global data look at mechanisms that shaped crust, likely formed eruption magmas different compositions over a long period time. Like Moon, is dotted with impact craters. Watters...
The Bolocam Galactic Plane Survey (BGPS) data for a six square degree region of the plane containing center is analyzed and compared to infrared radio continuum data. BGPS 1.1 mm emission consists clumps interconnected by network fainter filaments surrounding cavities, few which are filled with diffuse near-IR indicating presence warm dust or characteristic HII regions supernova remnants. New 350 {\mu}m images environments two brightest regions, Sgr A B, presented. B2 mm-emitting clump in...
During MESSENGER's first Mercury flyby, the Atmospheric and Surface Composition Spectrometer measured Mercury's exospheric emissions, including those from antisunward sodium tail, calcium close to planet, hydrogen at high altitudes on dayside. Spatial variations indicate that multiple source loss processes generate maintain exosphere. Energetic connected solar wind magnetospheric interaction with planet likely played an important role in determining distributions of species during flyby.
During MESSENGER's third flyby of Mercury, the Mercury Atmospheric and Surface Composition Spectrometer detected emission from ionized calcium concentrated 1 to 2 radii tailward planet. This measurement provides evidence for magnetospheric convection photoions produced inside magnetosphere. Observations neutral sodium, calcium, magnesium above planet's north south poles reveal altitude distributions that are distinct each species. A two-component sodium distribution markedly different two...
[1] The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed Titan's dayside limb in the extreme ultraviolet (EUV) and far (FUV) on 22 June 2009 from a mean distance of 23 Titan radii. These high-quality observations reveal same EUV FUV emissions arising photoelectron excitation photofragmentation molecular nitrogen (N2) as found Earth. We investigate both these solar driven processes with terrestrial airglow model adapted to find that total predicted radiances for two brightest N2 band...
The Cassini spacecraft's Ultraviolet Imaging Spectrograph (UVIS) includes a high-speed photometer (HSP) that has observed more than 100 stellar occultations by Saturn's rings. Here, we document standardized technique applied to the UVIS-HSP ring occultation datasets delivered Planetary Data System as higher level data products. These observations provide measurements of structure approaches scale largest common particles (∼5 m). combination multiple at different viewing geometries enables...
We present the 1.1 mm Bolocam Galactic Plane Survey (BGPS) observations of Gemini OB1 molecular cloud complex, and targeted NH3 BGPS sources. When paired with spectroscopy a dense gas tracer, millimeter yield physical properties such as masses, radii, mean densities, kinetic temperatures, line widths. detect 34 distinct sources above 5σ = 0.37 Jy beam−1 corresponding detections in NH3(1,1) transition. Eight objects show water maser emission (20%). find source FWHM 1.12 pc temperature 20 K...
In this paper we present the first nightside EUV and FUV airglow limb spectra of Titan showing molecular emissions. The Cassini Ultraviolet Imaging Spectrograph (UVIS) observed photon emissions Titan's day night limb‐airglow disk‐airglow on multiple occasions, including during an eclipse observation. 71 observations analyzed in show (600–1150 Å) (1150–1900 atomic multiplet lines band arising from either photoelectron induced fluorescence solar photo‐fragmentation nitrogen (N 2 ) or...
Abstract The Cassini Ultraviolet Imaging Spectrometer (UVIS) observed the airglow (dayglow and nightglow) of Titan over a range solar zenith angles (SZA) from 14 to 150° on five separate observations obtained between 2008 2012. modeling cycle normalized UVIS indicates that Chapman layer function provides satisfactory fit intensity EUV FUV molecular emissions N 2 Lyman‐Birge‐Hopfield band system (LBH ), Carroll‐Yoshino ( several atomic multiplets nitrogen (NI, II) as SZA. This result shows...
Solar XUV photons can provide enough energy to account for the observed nitrogen UV dayglow emissions above 800 km, but a small or sporadic contribution from energetic particles cannot be ruled out. Furthermore, ion production at altitudes deeper than km as inferred radio occultation produced by solar stimulation and implies deposition protons oxygen ions. Here we examine spectra visible‐wavelength images of Titan in Saturn's shadow, when is absent. are one three sets spectra, intensity...
Abstract A planet’s Ly α emission is sensitive to its thermospheric structure. Here we report joint Hubble Space Telescope and Cassini cross-calibration observations of the Saturn made 2 weeks before grand finale. To investigate long-term airglow observed by different ultraviolet instruments, cross-correlate their calibration, finding that while official Cassini/UVIS sensitivity should be lowered ∼75%, Voyager 1/UVS sensitivities enhanced ∼20% at channels. This comparison also allowed us...
The angular distribution of the radiation emitted into far field by TE0 and TM0 optical guided waves was measured compared with a theory assuming surface roughness to be source scattering. comparison made in such way that detailed knowledge under investigation not required.
A broad range of mathematical techniques, ranging from statistics to fuzzy logic, have been used great advantage in intelligent data analysis. Topology – the fundamental mathematics shape has date conspicuously absent this repert