Glenn Schneider - Resume / Curriculum Vita - University of Arizona

Glenn Schneider – Curriculum Vita/Resume Page: 1/21 11/29/04Glenn Schneider - Resume / Curriculum VitaContact:Steward ObservatoryHome: 7742 East Oakwood Circle933 N. Cherry Avenue Tucson, Arizona 85750 USAUniversity of Arizona Phone : 1-520-296-5296Tucson, Arizona 85721 USAe-mail: gschneider@mac.comPhone: 1-520-621-5865Fax: 1-520-621-1891e-mail: gschneider@as.arizona.eduURL: http://nicmosis.as.arizona.edu:8000/Education:Ph.D. in astronomy, August 1985, University of Florida.B.S. in physics (cum laude), June 1976, New York Institute of Technology.Employment History (Chronology):1994-Present: Steward Observatory, University of ArizonaAssociate Astronomer (2003-present)NICMOS Project Instrument Scientist (1994-2004)1985-1994: Computer Sciences Corporation at Space Telescope Science InstituteOperations AstronomerStaff Scientist (1992-1994)Senior Member of the Technical Staff (1988-1992)Member Technical Staff-A (1985-1988)1987-1989: Catonsville Community College - Adjunct Faculty1984-1985: Department of Astronomy, University of Florida - Research Assistant1982-1984: Space Astronomy Laboratory , University of Florida Research Assistant1978-1982: Department of Astronomy, University of Florida - Teaching/Research Assistant1977-1980: Warner Computer Systems, Inc. - APL Technical Consultant1976-1977: Warner Computer Systems, Inc. - APL technical Analyst

Glenn Schneider – Curriculum Vita/Resume Page: 2/21 11/29/04Present Position: Steward Observatory, University of ArizonaAssociate Astronomer & Instrument Scientist for the Near Infrared Camera and Multi-Object Spectrometer (NICMOS) Project at UofA. Current Annual Salary: $--,---Synopsis. Dr. Schneider holds an appointment at the University of Arizona’s Steward Observatoryas an Associate Astronomer. For the past ten years he has served as the Project Instrument Scientistfor the Hubble Space Telescope’s (HST) Near Infra-red Camera and Multi-Object Spectrometer(NICMOS). His research and instrumental interests are centered on the formation, evolution, andcharacterization of extrasolar planetary systems, and high contrast space-based (coronagraphic)imaging systems. His studies have focused on the direct detection of sub-stellar and planetary masscompanions to young and near-by stars and the circumstellar environments from which suchsystems may arise and interact. In concert with his scientific investigations of circumstellar dust anddebris disks and co-orbital bodies they may harbor, he has played a leading role in the developmentof very high contrast space-based coronagraphic and near-infrared imaging systems and techniqueswith HST, leading to spatially resolved scattered light images of nascent exoplanetary disks. As akey member of the NICMOS Instrument Definition (IDT) and Guaranteed Time Observing (GTO)teams, and lead for the Environments of Nearby Stars (EONS) programs, these and follow-upGeneral Observer (GO) investigations under his direction have borne substantial fruit (seePublication List).Environments of Nearby Stars (EONS) Programs. A significant portion of the NICMOSGTO time under Dr. Schneider's stewardship was dedicated to obtaining observations leading to abetter understanding of the physical processes inherent in the formation of extrasolarprotoplanetary systems (i.e., post-natal circumstellar disks) and stellar systems harboring substellarcomponents. Dating from 1995, the initial foundation of the programs under the EONS umbrellawas embodied in a set of (now partially answered) questions: Is there a continuity of companionobjects across the sub-stellar mass-spectrum bridging the stellar main sequence into the planetarydomain? How do the formative processes of protoplanetary disks and the physical properties oftheir constituent grains influence the evolutionary pathways that give rise to planetary systems? Inwhat sort of local environments will such objects form, and at what distances will they be foundfrom their host stars? How are these systemic parameters biased by the characteristics of theprimary and companion objects and those of the circumstellar regions? What implications will thediscovery and characterization of such objects have for our understanding of formationmechanisms? These fundamental questions defined the goals of the EONS investigations. Inseeking to shed light on these, and related questions, Dr. Schneider assumed a leading role inoverseeing and organizing the implementation of these highly successful programs.In concert with the conduction of these investigations, Dr. Schneider played a pivotal part indevelopment the HST/NICMOS coronagraphic capability, which was essential to the their success.Through his efforts, the NICMOS coronagraph has been proven as a unique instrumental andscientific resource by enabling very high contrast detection of very faint companion objects, anddiffuse circumstellar extended features in scattered light imaging, in the close proximity to verybright sources. Post-calibration image processing and reconstruction methodologies, which hedeveloped, uniquely tuned to NICMOS coronagraphic data, but generically applicable to highcontrast imaging on other instrumental platforms, continue to be used by the EONS team andfollow-on investigators in the analysis and interpretation of technically challenging observations andare yielding exceptional scientific results. Recent EONS discoveries of sculpted debris disksaround young stars seen in scattered light may be explained by the dynamical influences exerted byunseen planetary-mass companions, and modeling of multi-wavelength SEDs (thermal IR, sub-mm,and mm) in concert with high contrast imaging elucidates the physical properties of the disk grains.Such imagery, indeed, provides a stepping-stone to answer the fundamental questions alreadyposited.

Glenn Schneider – Curriculum Vita/Resume Page: 3/21 11/29/04With the successful completion of the GTO observations, Dr. Schneider has continued incollaboration with many other NICMOS science team members in the reduction, calibration,analysis, and interpretation of data amassed during the accelerated observing program. He hasactively lead, participated in, and contributed to a significant number of scientific investigations incollaboration with other team members and "outside" investigators, including follow-up programsto the NICMOS projects utilizing resources and facilities at Steward Observatory, Keck, Palomar,IRTF, Lick, and with other HST instruments. He has secured additional multi-wavelength follow-upobservations to the NICMOS EONS programs as approved HST/GO programs. Additionalobserving time has most recently been granted for both follow-up studies and new comprehensivecircumstellar disk and giant-planet companion surveys under the HST Cycle 13 call for proposals.Dr. Schneider, as a practitioner and advocate for space-based high-contrast imaging, has served thebroader community interest through solicited investigatory studies such as his recent, widelydistributed, report (issued by the the Space Telescope Science Institute, STScI) on the domains ofobservability in the near-IR with HST and ground-based AO systems, and with his service to theCongressionally requested Black committee report (and a source of input to the recent Bachallpanel) on considerations of the scientific merit of an extended (then post-SM4) HST mission.Functional Responsibilities and Experience as NICMOS Project Instrument Scientist. Formore than nine years, as the NICMOS Project Instrument Scientist, Dr. Schneider saw theinstrument through its final pre-launch design, implementation, integration and test, on-orbitcalibration, science/operational, and post-mission recomissioning phases while taking on a numberof pivotal leading and supervisory hardware, software, and programmatic responsibilities. Thecompression of the observational phase of the GTO program into a single HST observing cycleposed many unanticipated challenges in maintaining coherence in data calibration and analysis, aswell as in reformulating many aspects of those investigations. In accomplishing the completion ofthose programs he worked with and for the NICMOS science team in many diverse aspects ofplanning (and replanning) GTO observations while continuing to serve as the Project's primarytechnical interface to the STScI, and Goddard Space Flight Center's (GSFC) codes 440, 441 and512. During the pre-launch and commissioning phases of the NICMOS mission he worked closelywith Ball Aerospace & Technology Corporation's (BATC) integrated product teams leading to thesuccessful emergence of NICMOS as a facilities class instrument in the Hubble Space Telescope.His responsibilities have included frequent interaction with the aforementioned agencies in thedevelopment and implementation of ground and flight systems, procedures, software, interfaces,supporting on-orbit and ground calibration methodologies and data, on-orbit test procedures anddetailed observing proposals to assure that the primary goals of NICMOS science programs werecarried to successful conclusion. Concomitant with these activities were his daily interactions withsoftware and technical support staff lending guidance and supervision on a diverse variety of teamsupporttasks. With the advent and rapid acquisition of NICMOS data, particularly in thecoronagraphic programs that were enabled in the later phases of HST Cycle 7, his labors weresuccessfully divided between science and functional support.With the instruments' solid cryogen depletion, a significant portion of his efforts were devoted notonly to post-mission calibration, characterization, and performance evaluation but in support of alarge integrated systems engineering effort readying NICMOS for "resurrection" with theinstallation of an active cooling system (successfully installed on HST servicing mission 3B). Inthat regard, Dr. Schneider lead test teams both at the NICMOS Detector Laboratory at StewardObservatory and at the EMI/EMC facility at GSFC in conducting comprehensive experiments witha flight spare array replicating the on-orbit performance of the NICMOS detectors under on-orbitthermal conditions and integrated with the to-be-flown NICMOS cooling system. During that erahis responsibilities extended to detailed end-to-end instrumental systems evaluations, incollaboration with GSFC and STScI personnel, in preparation for both serving mission (SM)3Band the Cycle 11 Observatory Verification (SMOV) program to follow, including leading theplanning and analyses of key elements of the NICMOS recomissioning activities (e.g., detector

Glenn Schneider – Curriculum Vita/Resume Page: 4/21 11/29/04performance, optical alignment and focus, target acquisition reactivation, etc.), which werecompleted successfully as a precursor to re-enabling post-SM3B near-IR science on HST.- Science Team Support. The complex process of developing viable observational strategies forcarrying out near-IR astronomical investigations with HST did not relax as the mission evolved.Indeed, the rapid acceleration of the program demanded a closer and more detailed level ofinvolvement in the monitoring, execution, and evaluation of observations than if the observingprograms were played out over three cycles as originally envisioned. This was exacerbated with anew instrument whose characteristics were changing on short time scales. Dealing with thisrequired vigilance in shepherding many of our needs through the "system", which Dr. Schneiderattacked with success. He attributes this to the fact that he has worked closely in numerous aspectsof HST operations and planning for nineteen years and, through trial-by-fire, has gained first-handintimate knowledge of both the HST and NICMOS systems. Together these have afforded him theability to assist team members, and the larger community of HST/NICMOS users, in dealing withunrelenting minutiae associated with the implementation of their scientific programs. He has seenthis as a pivotal aspect of this position, and accordingly such activities have occupied much of hisattention. Thus, he has directed his efforts toward making NICMOS as scientifically a productiveinstrument as possible (often, in the face of seemingly adversarial external forces to be overcome).The emergence of the continuing stream of NICMOS GTO and follow-on science, is demonstrativeof his success in working toward that goal.- Instrument Operations, Data Reduction, Processing and Analysis. Dr. Schneider continuesto work on a daily basis as the UofA/IDT technical interface with STScI's PRESTO, CMD/ESB,Systems Engineering and NICMOS Instrument support groups. In addition to identifying andresolving proposal planning, execution, and instrument operations problems, he has recommendedspecific strategies to improve on-orbit efficiency, instrument stability and calibratability to expandthe scope of NICMOS capabilities both in solid cryogen (Cycle 7) and NCC (Cycle 11 andbeyond) eras. Such recommendations resulted from an expenditure of a considerable effort tounderstanding the on-orbit characteristics of NICMOS (as interfaced with HST) enabling theextraction of photometric and astrometric data from NICMOS images unbiased of systematiceffects to the greatest extent possible. In doing so he has iterated many times with both STScI'sNICMOS support group, and NICMOS Project software and database personnel, in improvingcalibration reference files as well as reduction and analysis software. He had also worked withSTScI in planning for, and analyzing the results of the NICMOS warm-up in light of the concernsof an independent science review committee established by NASA (the Harwitt committee), and forpost SM-3B science operations. He assumed an active role in coordinating the "warm up anomaly"testing in the NICMOS detector lab based upon test goals discussed with the HST Project at GSFCand STScI as well as the responsibility for supervising the integrated test team and laboratorypersonnel.- Pre-launch Instrument Calibration (SLTV, RAS/HOMS, EMI/EMC testing). To exploreand evaluate the operating characteristics of NICMOS, Dr. Schneider took a leading role in thedefinition, execution and analysis of the pre-launch calibration programs at BATC. Workingclosely during round-the-clock shifts with BATC project management, hardware, S/W, and testteam personnel he investigated anomalous behaviors, which led to both a better understanding of theinstrument, and changes in the methods and philosophy of instrument operation.- HST Systems Level Integration, Test, and Verification (VEST, STOCC), SOGS/SPSS.The exercise of pre-deployment validation of a new HST science instrument required extensive subsystemand integrated tests to be run with both ground and flight hardware and software. Dr.Schneider supported these efforts by defining, contributing to, and participating in numerousground system and functional tests (unit and end-to-end) and simulations. To validate the commandgeneration capability of the HST ground system for NICMOS, and the response to those commandrequests by the instrument, he worked with STScI ESB/Commanding personnel in creating testproposals, calendars, and Science Mission Specifications used in these series of tests and

Glenn Schneider – Curriculum Vita/Resume Page: 5/21 11/29/04subsequently analyzed resulting image data and engineering telemetry. He worked with BATC I&Tand MOSES SI/SE personnel in reviewing Real-Time command and operations proceduresrequired for these tests and in preparation for flight. In addition, he monitored and evaluated theground system and instrument behavior during test execution, and participated in real-time hardwareand software anomaly analysis and resolution.- SM-2 and SM-3B On-Orbit Instrument Checkout (AT/FT Planning and Execution). Dr.Schneider was an active member of the SM-2 and 3B flight preparation and operations teamsdefining and improving procedures for the NICMOS on-orbit installation and checkout. Heparticipated in defining the NICMOS requirements and implementation details of the ServicingMissions Integrated Timeline, Command Plan, on-orbit Aliveness and Functional tests, developedevaluation/acceptance criteria and real-time analysis S/W for the latter. This included on-console atthe STOCC for all SMGTs, JISs, and during the mission as the IDT science support representative.- SM OV 2 and 3B Program Planning, Implementation, and Analysis. Dr. Schneider served(and continues to serve) as the UofA/IDT representative and technical lead for the NICMOSServicing Mission Observatory Verification programs. This engendered defining the NICMOSSMOV plans and requirements in concert with HST and STScI project management. As PrincipleInvestigator for many of the SMOV programs (and co-I on most others), he developed andimplemented on-orbit check-out, engineering, and calibration proposals, operations procedures andanalysis plans in consultation and association with STScI and the BATC I&T teams. Post-launchhe worked extensively at STScI to support near-RT analysis and a dynamically evolving andchanging SMOV program in light of unexpected instrumental performance anomalies.Hubble Space Telescope Research and Calibration ProgramsCurrent/Recently Funded Hubble Space Telescope Science ProgramsNEWLY APPROVED (CYCLE 13) HST OBSERVING PROGRAMSProgram HSTID Orbits AwardSolar Systems In Formation: A NICMOS Coronagraphic Survey 10177 56 $---,---of Protoplanetary and Debris DisksCoronagraphic Survey for Giant Planets Around Nearby Young 10176 116 $---,---Imaging Polarimetry of Young Stellar Objects with ACS and 10178 19 $---,---NICMOS: A Study in Dust Grain EvolutionImaging of Ices in Circumstellar Disks 10167 15 $---,---Spatially Relsoved Spectroscopy of HR 4796A's Dust Ring 10168 3 $---,---RECENT HST PROGRAM AWARDS AS P.I. AT STEWARD OBSERVATORYProgram HSTID Orbits AwardA Search for Stellar Duplicity and Variability from FGS Guide 5811 N/A $---,---Star Acquisitions and Guiding DataConfirmation and Characterization of Brown Dwarfs and Giant 8176 20 $---,---Planets from NICMOS 7226/7667Duplicity and Variability in HST Guide Stars – An FGS 8371 N/A $---,---Serendipitous SurveyEnabling Coronagraphic Polarimetry with NICMOS 9768 6 $---,---Near-IR Photometry of a Candidate companion to Proxima 7847 4 $---,---CentauriDirect Imaging of a Circumstellar Disk: β Pictoris, a Case Study 6058 8 $---,---Imaging and Spectroscopy of Dusty Circumstellar Disks 8624 17 $---,---

Glenn Schneider – Curriculum Vita/Resume Page: 6/21 11/29/04HST GO, GTO, AR Program Summaries as Principal or Co- Investigator 1Solar Systems In Formation: A NICMOS Coronagraphic Survey of Protoplanetary andDebris Disks, PI/GO (10177): Until recently, despite decades of concerted effort applied tounderstanding the formation processes that gave birth to our solar system, the detailed morphologyof circumstellar material that must eventually form planets has been virtually impossible to discern.The advent of high contrast, coronagraphic imaging as implemented with the instruments aboardHST has dramatically enhanced our understanding of natal planetary system formation. Even so,only a handful of evolved disks (~ 1 Myr and older) have been imaged and spatially resolved inlight scattered from their constituent grains. To elucidate the physical processes and properties inpotentially planet-forming circumstellar disks, and to understand the nature and evolution of theirgrains, a larger spatially resolved and photometrically reliable sample of such systems must beobserved. Thus, we are conducting a highly sensitive circumstellar disk imaging survey of a welldefinedand carefully selected sample of YSOs (1-10 Myr T Tau and HAeBe stars) and (> app 10Myr) main sequence stars, to probe the posited epoch of planetary system formation, and to providethis critically needed imagery. Our resolved images will shed light on the spatial distributions of thedust in these thermally emissive disks. In combination with their long wavelength SEDs thephysical properties of the grains will be discerned, or constrained by our photometrically accuratesurface brightness sensitivity limits for faint disks which elude detection. Our sample builds on thesuccess of the exploratory GTO 7233 program, using two-roll per orbit PSF-subtracted NICMOScoronagraphy to provide the highest detection sensitivity to the smallest disks around bright starswhich can be imaged with HST. Our sample will discriminate between proposed evolutionaryscenarios while providing a legacy of cataloged morphologies for interpreting mid- and far-IRSEDs that the recently launched Spitzer Space Telescope will deliver. This project cannot be donefrom the ground, and becomes untenable for HST after Cycle 13 under the anticipated use of twogyropointing control mode.Coronagraphic Survey for Giant Planets Around Nearby Young, co-I/GO (10176): Asystematic imaging search for extra-solar Jovian planets is now possible thanks to recent progressin identifying "young stars near Earth". For most of the proposed young (

Glenn Schneider – Curriculum Vita/Resume Page: 7/21 11/29/04images in the optical and infrared, we can sensitively constrain not only the geometry and opticaldepth of the scattering medium, but also the grain size distribution. By observing objectsrepresentative of the earliest evolutionary sequence of YSOs, we will be able to investigate how thedust population evolves in size and distribution during the crucial transition from a disk-plusenvelopesystem to a disk-plus-starstar system. This study will help to establish the fundamentaltime scales for the initial depletion of ISM-like grains: the first step in understanding thetransformation from small submicron sized dust grains, to large millimeter sized grains, anduntimely to planetary bodies.Imaging of Ices in Circumstellar Disks, co-I/GO (10167): The link between the material of theinterstellar medium and the ultimate composition of planets lies in the way gas and dust areprocessed in circumstellar disks. Planet formation models rely upon a knowledge of the diskconstituents and temperature profiles to simulate how small grains eventually combine intoterrestrial planets and gas giant cores. Disks around other stars may be analogs for our own earlySolar System and thus allow the direct measurement of such phenomena. Only recently, however,have well-resolved images of dust disks around several late T Tauri or main sequence stars beensecured. HST provides a uniquely stable platform for making such sensitive high dynamic rangeimages. Now, for those handful of disks already resolved, we are able to go beyond the discoveryphase and begin making astrophysical measurements to deepen our understanding of the course ofdisk evolution. We therefore are conducting a multi-wavelength study with NICMOS designed todiscover the spatial distribution of two common Solar System materials -- methane and water ices --in other systems.Spatially Relsoved Spectroscopy of HR 4796A's Dust Ring, co-I/GO (10168): HST's highcontrastcapabilities provide exciting imaging of circumstellar debris disks with complex structures.In particular, broad-band imaging using the coronagraphs in NICMOS and STIS has elucidated thedisk morphology of HR 4796A exquisitely, but can only provide colors, not detailed compositionalinformation on its dust. With spectra, we will measure the detailed albedo of the disk dust over alarge wavelength range and search for interstellar medium-like molecules and water ice. We willalso use our spatially resolved spectra for very high angular resolution profiles of the disk width toconstrain models for planets circling inside the dust. We have demonstrated in a previous programhow to use STIS for spatially resolved disk spectroscopy. We now will apply our technique tostudy HR 4796A.Imaging and Spectroscopy of Dusty Circumstellar Disks, co-I/GO (8624): Understandingthe properties and evolution of dusty disks in the circumstellar environments of young stars is a keyelement in furthering our concepts of the formation mechanisms of extra-solar planetary systems.The advent of NICMOS and STIS coronagraphy has given rise to the first scattered light imaging,other than for β Pictoris, of dusty circumstellar disks with spatially resolved morphologicalstructures. NICMOS has taken a first step in imaging these new disks, elucidating their geometries,morphologies, and bulk photometric properties, while increasing the number of such knownsystems from one to half a dozen. These dusty disks vary in physical size by over two orders ofmagnitude and exhibit radial anisotropies in their brightness distributions that may be indicative ofdynamical confinement or sculpting of the disk particles by unseen planetary bodies. STIS followonimaging and spectroscopy are needed to provide further insight into the nature of the diskparticles. With spectra, the albedo of the disk dust is measured and signatures of complexmolecules and water ice are sought. With coronagraphic images, the scattering phase function andhence the composition of the disk dust is investigated in concert with direct determination of thedisk sizes and shapes with high precision. Such observations are of fundamental importance inestablishing the physical basis for emergent theories of disk evolution and planet-building.Imaging the Dust Disk around Epsilon Eridani, co-I/GO (9037): Epsilon Eridani is theclosest star to the Sun around which a planet has been discovered. An asymmetric dust disk aroundthe star has been detected in sub-millimeter observations. Clumps in the disk have been interpretedas resulting from resonant interaction, and the pattern has been predicted to revolve around star at a

Glenn Schneider – Curriculum Vita/Resume Page: 8/21 11/29/04rate of ~ 0.7° per year. Multi-epoch observations of the dust disk with STIS will obtained. Theseobservations will not only reveal what may be the first extra-solar Kuiper belt, but will also providea crucial step in the development of observational techniques that can determine the presence andproperties of planets, from the visible morphology of the disks around the parent stars.Confirmation and Characterization of Brown Dwarfs and Giant Planets from NICMOS7226/7227, P.I./GO (8176): A selected candidate list of 74 stars was observed using the NICMOScoronagraph at 1.6 µm. Eight companion candidate objects as faint as H = 20, up to 13 magnitudesfainter than their primaries with separations less than 5" were found (and a majority subsequentlyconfirmed as low mass companions by common proper motions). For the stars in this sample thiscovers minimum physical separations of 1.2-50 AU at the inner spatial detection limit. The lowermass limit depends on age, distance, and spectral type, but is as low as 3-5 M Jupiter for many of theprogram targets. Spectrographic observations are essential to characterize the physical nature of theputative companions we have discovered. These observations address fundamental questions suchas: Is there a continuity of objects across the substellar mass spectrum bridging the main sequenceto planetary objects? What is their frequency of occurrence? At what distances are they found fromtheir primaries? And, what implications will these discoveries have for our understanding ofstellar/planetary formation mechanisms?A Search for Low Mass/Sub-Luminous Companions to M-Stars, P.I./GTO (7227):Knowledge of stellar and sub-stellar masses and luminosities at and below the ~ 0.08 M sunHydrogen burning limit is of fundamental importance in many inter-related areas such as probingthe end of the stellar mass function, the theory of stellar evolution, the end of the main sequence, thegalactic missing mass, age and evolution. Yet, this transition region in the mass spectrum of objectsbetween low-mass stars and giant planets is poorly understood and ill-observed. Until very recently,with the discovery of the Brown Dwarf companion to GL 229, the very existence of such objectsremained in the conjectural realm. To make further progress in low end of the mass distributionfunction, additional objects first must be found. Potentially fruitful hunting-grounds to search forsuch transitional objects using NICMOS, in parameter spaces which do not overlap with groundbasedcapabilities, are as companions to M-dwarfs which are: Nearby (d < 6 pc) and spectral typeslater than ~ M3.5; Young (≤ 10 8 years) and at d ≤ 25 pc.; and Spectrally the latest known(> ~ M8.5). This investigation carried out a coronagraphic imaging program aimed at discoveringsuch objects.A Search for Massive Jupiters. Co-I/GTO (7226): NICMOS was used to search for massiveplanets around nearby, young main sequence stars. Camera 2 was employed to search from 0.3" to3" around coronagraphically occulted targets at the wavelength band of 1.4 – 1.8 µm (F160W)which corresponds to strong emission in the brown dwarf candidates GL 229B and GD 165B aswell as to strong reflections in Jupiter and Titan. Because of the extreme youth of these objects, anylow-mass brown dwarf and planetary companions will still be in a higher luminosity phase and thuseasily detectable. The lower mass limit depends on age, distance, and spectral type, but can be aslow as 3 – 5 M jupiter for targets in our sample. Follow-up observations of candidate companions willprovide proof of true physical association with the primary. The typical separations observable withNICMOS are near the empirical maximum in the binary distribution of stars (~ 20 – 40 AU), whichalso corresponds to the mean distance of the giant planets in our own solar system.Dust Disks Around Main Sequence Stars. Co-I/GTO (7233): A selection of mostly mainsequence stars which have (a) τ dust > 10 -3 or (b) other characteristics that suggest the presence ofcircumstellar dust disks were observed. The observations were made with the NICMOScoronagraph to minimize the effects of glare from the bright central star. We rotationally ditheredthe pointing by means of a spacecraft roll for best background subtraction. As a primary objective,all images were examined for the presence of dust disks. An important secondary objective was tosearch of all images for possible brown dwarfs or high-mass planets. Following detections,

Glenn Schneider – Curriculum Vita/Resume Page: 9/21 11/29/04additional observations were conducted to characterize the physical properties of those objectsfound.(Spectroscopy and) Polarimetry of the β Pictoris Disk, Co-I/GTO (7248): Little is knownabout the β Pictoris disk within 50 AU of the central star. No near-infrared spectrophotometry orpolarimetry exists within this dynamically interesting region, which is about the same size as ourown solar system and which appears to be relatively depleted of disk material. Grism spectroscopy(R ~ 75) and polarimetry of the disk from within 5 AU of the star to the outer limits of the disk asdetermined by the total integration time. Such observations will help to characterize the chemicaland physical properties of the disk particles as a function of their distance from the star. By movingthe star close to the edge of the coronagraphic hole, the disk was be probed as close as 2 AU fromthe star.Near-IR Photometry of Candidate Companion to Proxima Centauri, Co-Investigator/GO(7847): A putative low luminosity companion to the closest star to the Sun, Proxima Centauri (dist.~ 1.3 pc) has been identified. The candidate companion was discovered during Cycle 6 using theFOS as a coronagraphic camera (Program ID: 6059). The candidate companion is within ~ 0.4" ofProximal Cen, too close to be detected with WFPC2. It's apparent motion on the sky is similar tothe parallactic motion of Proxima Cen, which makes its effect upon Proxima Cen difficult to detectwith FGS astrometry. If the candidate companion is in orbit about Proxima Cen, modeling indicatesthe orbital period would be ~1 year. The ideal time to image the companion is when it is farthestfrom Proxima Cen. HST NICMOS camera 1 observations are obtained to confirm/rejectcompanionship, determine IR magnitudes, and to constrain orbital elements. Due to the small spatialseparation and large magnitude differences, direct image detection of the companion cannot be donefrom the ground.(Spectrophotometer and) High Resolution Imaging of HD 98800, Co-I/GTO (7232):HD98800, located nearby at a probable distance of 20 pc, is a unique stellar system consisting oftwo K7-V stars separated by 0.8 arcsec. Composite optical spectra show Lithium absorption,indicating pre-main sequence age, and IRAS found extraordinarily large amounts 165 K dustemission, suggesting the presence of a possible “zodiacal dust cloud in the making”. NICMOSCamera 1 was be used in five bands from 0.9 to 2.0 µm to make fully saturated MULTIACCUMimages that can be deconvolved to separate the two well resolved bright stars from light scattered bythe dust. If the dust cloud is sustained by a recently “failed planet” it should also be resolved atabout 0.2" diameter. Comparisons of dust properties such as (a) scattered to emitted light, (b) colorof scattered light and (c) size of the dust cloud can then be made with corresponding data for thesolar system. Repeated observations enabled the dynamics of the systems to be established.Spectrophotometry and Imaging of Pluto and Charon, Co-Investigator/GTO (7223):Detailed spectra of the individual members of the Pluto-Charon system were obtained. Theconjecture of differing surface compositions, suggested by evidence obtained when the two wereundergoing mutual eclipses were explored via grism spectrophotometry. These observationsprovided a direct comparison of the surface materials of each member of the double planet at theirleading and trailing edges. Dispersed spectra were obtained at four separate orbital positions to todifferentiate surface variations on the two objects. Charon's leading (in Charon's orbital direction)trailing, Pluto-facing and non-Pluto-facing hemispheres were observed.A Search for Stellar Duplicity and Variability form FGS Guide Star Acquisition andGuiding Data, P.I./AR (5811): The HST Fine Guidance Sensors (FGS) have the uniqueastrometric capabilities of revealing faint companions in close binary systems. They can measuretheir position angles and component separations, with a precision which exceeds that which ispossible using any ground based techniques for primary components in the magnitude range V = 9to 14. In addition, the intensity data, which are produced by the FGS PMTs, provide high precisionrelative photometry on rapid time scales. In mid Cycle 4 a new telemetry format was adopted for allnormal operations which serendipitously provide these astrometric and photometric data at 40 Hz

Glenn Schneider – Curriculum Vita/Resume Page: 10/21 11/29/04for all guide star acquisitions and periods of active guiding. This program conducted a systematicexamination of these data, obtained from the HST engineering telemetry, to search for stellarduplicity and determine the incidence of doubles in the Guide Star Catalog as well as theseparations, position angles, and relative brightnesses of the individual stellar components in suchbinaries. The light curves and power spectra of the photometric data were also reduced and analyzedin an effort to perform an astroseismological survey of these stars, as well as look for andcharacterize variations due to other intrinsic mechanisms.Duplicity and Variability in HST Guide Stars - An FGS Serendipitous Survey, P.I./AR(8370) - A continuation of 5811. N.B.: Data resulting from all 40, 258 observations analyzed in thisprogram have been ingested into the SIMBAD database.High Spatial Resolution Imaging of Comet Hale-Bopp (C/1995 O1), Co-Investigator/GTO(7240): Comet Hale-Bopp provided an excellent opportunity for high-resolution imaging of thenuclear and inner coma regions of a bright comet. Observations in the near-infrared offered highcontrast between the coma and nucleus since reflected sunlight/fluorescence are at a minimum andthermal emission from coma dust is important only at longer wavelengths. The production of gasand dust in the inner coma very near the nucleus and to monitor the emergence and activity of jetstructures were probed. Images were obtained in/out of known spectral features due to water ice(2.04 µm), gaseous water (1.9 µm), and C2 (1.9 – 2.0 µm). With a nuclear rotation perioddetermined prior to the time of the observations, this will be used to devise an optimal strategy formeasuring the nuclear brightness as a function of rotational phase. There also existed the possibilityof nuclear fragmentation or flaring and indeed spiral jetting was seen. Observations were obtainedas soon as possible after the comet emerged from solar avoidance and coordinated withcontemporaneous imaging in the UV with the Space Telescope Imaging Spectrograph.Pyramid Imaging of Circumstellar Material About Nearby Stars, Co-I/GO (6469):Observations obtained with the Infrared Astronomical Satellite (IRAS) have indicated that many ofthe nearby, bright stars have an infrared excess from a comparable sample of stars of similarspectral types. This IR excess has been attributed to emission from heated dust. Despite the definitepresence of circumstellar dust for approximately one third of the nearby A-F stars, attempts atimaging candidates (other than β Pictoris) have yielded null results. Failure to detect these diskslikely stemmed from the extreme differences in surface brightness between the central star and anysurrounding disk material, as well as the evolution of such disks over time. The WFPC-2 pyramidedge will be used in a psuedo-coronagraphic manner in an attempt to detect and characterizecircumstellar material about seven nearby stars which may have β Pic like disks as inferred fromtheir IR excesses. Theories of planet formation based on nebular cosmogonies postulate thatplanets form during the contraction of a rotating gas cloud. Accretion of dust particles and volatileices form planetesimals, the larger of which sweep up material from the nebula and grow into protoplanets.If disks are normal by-products during contraction of a nebular cloud and are commonplace, then what are their compositions, grain size, and how do they evolve with time? If disks existabout other stars, where are they? One would expect the inner regions of a disk close to the centralstar to experience rapid evolution through sublimation of ices and clearing of the disk throughcollisions with bigger bodies or particles falling into the central star, while the evolution of the outerdisk regions will proceed at a much slower rate. The scenario involving infall and evaporation ofcomet-like bodies has been used to explain the presence of circumstellar dust about β Pic. If thismodel for processing of the disk material is valid, this process could be expected to occur aboutother stars, and in turn could explain the reported large IR excesses for many of the nearby stars.Direct Imaging of the Circumstellar Disk of β Pictoris, Co-Investigator/GO (6058): Theimaging capabilities of HST/WFPC2 were used to obtain high contrast, high resolution images ofthe dust disk (V = 16 mag/arcsec 2 ) about β Pictoris (V = 3.9). With these, more accuratephotometry of the disk was obtained, the reported morphology (gaps) and variable disk thicknesswere investigated along with the optical properties and size distribution of the circumstellar dust. At

Glenn Schneider – Curriculum Vita/Resume Page: 11/21 11/29/04the time of observation, β Pictoris represented the best candidate for an extrasolar proto-planetarysystem or possibly a massive Kuiper belt (then, the only circumstellar disk that had been detectedwith ground-based coronagraphy). Accurate photometry is essential to determine the properties ofthe disk. Smith and Terrile reported an r -4.3 power law for the light distribution within the disk, whileArtymowicz, Burrows, and Paresce reported a slightly less steep distribution of r -3.6 . Their diskmodel suggested an upper limit for the tilt between the plane of the disk and the line of sight of 14°,with a mixture of grain sizes (radii between 1 and 20 µm) to explain the light scattering in thevisible and IR images. Telesco et al. suggest an inner disk to 50 AU (3") from β Pictoris based on10 and 20 µm observations, while Backman, Gillett, and Witteborn suggest the disk reaches inwardto between 1 and 30 AU from IRTF observations. R-band images obtained with the Johns HopkinsUniversity AO Coronagraph indicate an inverted asymmetry in the light distribution within 100 AUimplicating a change in the scattering properties of the grains or a lower grain density in this regionof the disk. There are possibly three processes involved in moving grains about in the disk:radiation pressure blowing small grains away from the vicinity of β Pictoris, Poynting-Roberstondrag causing small grains to spiral into β Pictoris, and hidden planetary bodies perturbing the dustdisk. Backman and Paresce suggest that planetary-like bodies orbiting at the inner boundaries ofinfrared-emitting regions could explain the central voids in circumstellar disks, while the outer diskmay represent a Kuiper belt. This program investigated whether this model is correct andresponding to the question "Do disks represent success or failure modes in planet building?''HST/NICMOS Early Release Observation ProgramsSee Publication List for: NGC 2264 IRS [ref 10R], Orion 114-426 Silhouette Disk, [ref 11R],Nuclei of ARP 220, [ref 12R] Nucleus of IC 5063, [ref 13R], OMC-1, [ref 14R], and CRL 2688,[ref 15R].HST/NICMOS Instrument Calibration and Engineering Programs 2GO/CAL (CYCLE 12):Enabling Coronagraphic Polarimetry with NICMOS, co-Investigator, 9768NICMOS Coronagraphic Performance Assessment 2, Principal Investigator, 9693SMOV3B (CYCLE 11):NICMOS Filter Wheel/Mechanisms Functional Test, Principal Investigator, 8944NICMOS SMOV3B Transfer Function Verification Test, Principal Investigator, 8976NICMOS Optimum Coronagraphic Focus Determination, Principal Investigator, 8979NICMOS Mode-2 Target Acquisition Test, Principal Investigator, 8983NICMOS Coronagraphic Performance Assessment, Principal Investigator, 8984NICMOS Coronagraphic Performance Assessment Part 1, Principal Investigator, 8984NICMOS Filter Wheel/Mechanisms Functional Test, Principal Investigator, 8944SMOV2 (CYCLE 7):NICMOS Internal Parallel (Electrical Cross Talk) Test, Principal Investigator, 7032 & 7136NICMOS Field Offset Mirror Operations Test, co-Investigator, 8973NICMOS Pupil Alignment ("Tilt") Test, co-Investigator, 9645NICMOS Transfer Function Verification Test, Principal Investigator, 70372 See Publication List for results from the above Science and Instrument Calibration Programs

Glenn Schneider – Curriculum Vita/Resume Page: 12/21 11/29/04NICMOS Target Acquisition Test Principal Investigator, 7038NICMOS Coarse Optical Alignment, Principal Investigator, 7041 & 7150NICMOS Fine Optical Alignment, Principal Investigator, 7042NICMOS Focus Monitor, Principal Investigator, 7043NICMOS Coronagraphic Performance Verification, Principal Investigator, 7052NICMOS Pre-Alignment Check-out, Principal Investigator, 7134NICMOS Intermediate Focus/Alignment, Principal Investigator, 7135NICMOS Coronagraphic Hole Monitor, Principal Investigator, 7154NICMOS Revised Field Offset Mechanism Test, Principal Investigator, 7156NICMOS Optimum Coronagraphic Focus Determination, Principal Investigator, 7157NICMOS Coronagraphic Hole Location Test, Principal Investigator, 7808 & 7924Other Research Activities - CurrentInner Planetary Transits:(I) Liason to the Past. Historically, the visual manifestation of the “Black Drop effect,” theappearance of a band linking the solar limb to the disk of a transiting planet near the point ofinternal tangency, had limited the accuracy of the determination of the Astronomical Unit and thescale of the solar system in the 18th and 19th centuries. This problem was misunderstood in thecase of Venus during its rare transits due the presence of its atmosphere. In preparation for the rareopportunity later presented by the 08 June 2004 transit of Venus, observations of the 15 November1999 transit of Mercury were obtained, without the degrading effects of the Earth’s atmosphere,with the Transition Region and Coronal Explorer (TRACE) spacecraft. In spite of the telescope'slocation beyond the Earth's atmosphere and the absence of a significant Mercurian atmosphere, afaint Black Drop effect was detected. The observed black drop was fully attributable solarphotospheric limb-darkening back-lighting the Mercurian disk, and blurred by the instrumentalpoint-spread function. These effects (and those of atmospheric turbidity) were elaborated upon inlight of earlier ground-based observations of inner planet transits to explain the historical basis forthe Black Drop effect. The methodologies developed for improving upon space-based transitimagery are applicable to ground-based (adaptive optics augmented) and space-based observationsof the 8 June 2004 and 5-6 June 2012 transits of Venus, providing a path to achieving highprecisionmeasurements of transit phenomenon. (see DPS [56M] 3 , Icarus [40R], IAU Proc [33P]).(II) Contemporary Extra-Solar Planet Studies & Liaison to the Future. Coordinated spaceand ground-based observations of the 08 June 2004 transit of Venus were obtained to: (a) testobserving methods, strategies and techniques which are being contemplated for future spacemissions to detect and characterize extrasolar terrestrial planets as they transit their host stars; (b)investigate, in detail, the properties of the circum-Cytherian "aureola" (sunlight scattered by aerosolsand refracted in the back-lit planetary atmosphere); (c) study the (detectability of) optical absorptionby sulfur allotropes and other species by the upper atmosphere of Venus. Combining high spatialand temporal resolution broadband imaging (with TRACE 4 ), very high precision time-resolvedradiometry (with ACRIMSAT 5 ), and ground-based lunar reflectance differential spectroscopy, andnarrow-band imaging from a variety of telescopes, inferences for the detectability and possibilitiesfor characterization of extra-solar planets by space-transit measurements are being assessed. Thisstudy is partially funded by the National Geographic Society Committee for Research andExploration.3 [##]: See Publication List for cited references (indicated [##])4 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/TRANSIT_04/TRACE/TOV_TRACE.html5 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/TRANSIT_04/ACRIMSAT/ACRIMSAT_TOV.html

Glenn Schneider – Curriculum Vita/Resume Page: 13/21 11/29/04Galaxy Evolution and Origins Probe (GEOP): Future mission concept study, co-proposed (asdeputy PI) with R. Thompson (PI), selected by NASA 6 . Rodger Thompson, University of Arizona.GEOP will observe more than five million galaxies to study the mass assembly of galaxies, theglobal history of star formation, and the change of galaxy size and brightness over a volume of theuniverse large enough to determine the fluctuations of these processes.Other Research Activities - PreviousLunar Occultations & Stellar Diameters (Dissertation Research, Department ofAstronomy, University of Florida): The observation and analysis of lunar occultations. Asystematic program of fast photometric observations of lunar occultations was carried out tomeasure stellar diameters, obtain better astrometric positions of stars, search for previouslyunsuspected stellar duplicity and provide fundamental data for the determination of time based oncorrections and checks to the lunar theory. Fast photometric data acquisition instrumentation wasdesigned and developed to carry out a systematic study of selected stellar targets which wereocculted by the moon. New numerical techniques for data reduction and analysis, including theintroduction of probabilistic constraints into a non-linear least-squares differential-correction modelfitting process, were investigated and implemented. Physical parameters (including diameters) formany stars and stellar systems were successfully determined. Chairman: Dr. John P. Oliver. (e.g.,see: Ph. D. Thesis [3O] or Program Summary [8R]) .Asteroidal Photometry: Initiated a collaborative program of multi-color asteroidal photometryand fast photometric observations of asteroidal occultations of stars to determine the size, shape anddensity of selected minor planets, and to search for asteroidal duplicity. Designed and constructedportable photoelectric photometers, electrometer amplifiers, time-code converters and digital dataacquisition electronics for remote-site observations. Deployable field stations were used forindependent observations, and in conjunction with observations made at Rosemary Hill Observatory(RHO) and other fixed observatory sites. Profiles, diameters, and densities, as well as other physicaland photometric properties of many asteroids were determined, including Nemausa, Pallas, andCeres. This program was conducted under a grant from the University of Florida's Division ofSponsored Research. (e.g., see papers on Nemausa [3R], Ceres, [4R], and Pallas [7R]).Numerical Modeling of White Dwarf Stars: Developed a computational model for investigatingdynamical instabilities in the structure of white dwarf stars of varying chemical compositions, ionicpartitions and central densities, applicable over a wide range of partial and total degeneracy regimes.The model included such affects as Coulomb interactions between electrons and nucleons, inversebeta decays, the effects of the general theory of relativity on the condition on hydrostaticequilibrium (local and global), stellar rotation, mass accretion in binary systems and interactionswith external magnetic fields. This work was supported by a grant from Warner ComputerSystems, Inc. (e.g., see ACM paper "Astrophysical APL - Diamonds in the Sky" [2P]).Polar Atmospheric / Climatological Research: The integrity of the synoptic meteorologicalrecord of the South Pole is important both to the continuing effort to understand the climatology ofthe Antarctic Plateau, and to a number of interdisciplinary studies aimed at discovering the details ofthe mechanism responsible for the depletion of upper atmospheric ozone. An analysis of thenighttime synoptic meteorological record from the South Pole station was undertaken, and asystematic error in the sky cover observations was discovered. As a result it was determined that theseasonal variations in sky cover, as inferred from these observations, are not nearly as significant aspreviously believed. This project was partially supported under National Science Foundation grantDPP 86-14550. (e.g., see JOC paper [6R])6http://www.nasa.gov/home/hqnews/2004/jul/HQ_04246_mission_concepts.html

Glenn Schneider – Curriculum Vita/Resume Page: 14/21 11/29/04Total Solar EclipsesDr. Schneider is a member of the International Astronomical Union’s Division II Working Groupon Solar Eclipses. He is recognized as a leading expert in the high-precision numerical calculationof eclipse circumstances and the application of those computations in planning and carrying outobservations of total solar eclipses. For more than three decades, Dr. Schneider has leadexpeditionary groups and conducted such observations on land, sea and air of twenty-five (of thetwenty-six) total solar eclipses occurring since 7 March 1970 from remote locations across theglobe conducting direct, polarimetric, and spectrophotometric imaging programs. Additionally, hehas executed three, and planned five, high-altitude eclipse intercepts with jet aircraft:•Planned and Executed: A 44,000 ft very highly technically challenging and navigationallycritical intercept using a Citation II over the North Atlantic on 03 October 1986 7 .•Planned and Executed: A 41,000 ft intercept over the South Atlantic, working in situ onthe flight deck of a VASP airlines DC-10, extending the duration of totality to 6m 15s 8 .•Planned: A supersonic one-hour totality at 60,000 ft intercept over the South Atlanticusing an Air France Concorde 9 . Very sadly, this was cancelled due to the grounding ofthe Concorde fleet following the horrific crash of AF 4590 outside of Paris on 25 July2000 10 .•Planned and Executed: The QANTAS 2901 / 23 November 2003 Antarctic eclipse flight.(see [34P]).•Planned and Executed: The Lan Chile 8001 / 23 November 2003 Antarctic eclipseflight 11 .The planning of the above airborne observations was rooted in the use of the EFLIGHT S/W,created by Dr. Schneider, specifically to address the problem and optimization of intercepting themoon's shadow from a moving aircraft. The core algorithms were developed for the highlytechnically challenging 1986 eclipse intercept and were augmented for the 1992 eclipse flight toprovide greater flexibility for real-time use on the DC-10 flight deck. The S/W was modified inpreparation for the 2001 Concorde eclipse flight, for consideration of an intercept in the supersonicregime where the instantaneous speed of the aircraft was greater than that of the lunar umbra giventhe geometrical circumstances of that eclipse. Most recently, EFLIGHT was again modifiedspecifically for the “over the pole” approach geometry of the lunar shadow for the 23 Nov 2003eclipse and tailored for real-time use given the manual input requirements of the Boeing 747-400ER FMS, to enable an observational program 12 in co-ordination with contemporaneousobservations of the LASCO/C2 coronagraph on the SOHO spacecraft.7 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_86/ECLIPSE_86.html8 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_92/ECLIPSE92_REPORT.9 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_01/CONCORDE_ECLIPSE.html10 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_01/ECLIPSE_2001_REPORT.html#MEMORIUM11 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_03/ECLIPSE_03.html12 http://nicmosis.as.arizona.edu:8000/ECLIPSE_WEB/ECLIPSE_03/QF2901_IMAGING/TSE2003_REPORT.html

Glenn Schneider – Curriculum Vita/Resume Page: 15/21 11/29/04Previous Employment/PositionsComputer Sciences Corporation - Space Telescope Science Institute(1985-1994) Ending Annual Salary: $--,---Appointment/Functional Responsibility: Served for nine years as an Operations Astronomerin the Operations, and Science and Engineering Support Divisions at STScI.General Responsibilities: Appointed as a member of the Instruction Management (ScienceInstrument Commanding) Task Group. Designed, implemented, and tested science commandinginstructions (for the Science Planning and Scheduling System (SPSS) /Science CommandingSubsystem of the Hubble Space Telescope Science Operations Ground System (SOGS)).Developed operational procedures, science instrument command groups and supportive filestructures for inclusion in the HST Project Data Base (PDB) for operating the WideField/Planetary Camera (WFPC), Fine Guidance Sensors (for astrometric science), WideField/Planetary Camera-2 (WFPC-2), as well as other Science Instruments and spacecraftsubsystems. Participated in the validation of low-level and atomic command constructs testedduring Assembly and Verification for all HST Science Instruments. Adapted these for use in theSOGS and Payload Operations Control Center/Applications Support Software (PASS) groundsystems. Designed and built higher-level logic to control the use of these command structures.Developed requirements and software interfaces for driving flow-down control logic from astructured Proposal Management Data Base (PMDB) and calendars of time-ordered events.Developed and implemented reconfiguration instructions and associated table driven logic to allowfor automatic setup and transitioning of the science instruments to/from various defined operationalstates. Generated detailed requirements for the proposal Transformation software. Contributed tothe Proposal Instructions and Instrument Handbooks.WFPC-2: In preparation for the on-orbit installation of WFPC-2 was responsible for working withthe WFPC-2 Science, Instrument Development, and Integration & Test teams in both pre-launchtesting of the hardware and ground system software. This effort engendered gaining specific firsthandknowledge of the workings of the instrument by participating a series of ground system,thermal vacuum, hardware, and system functional tests. This also encompassed participation in theSMOV Proposal Implementation Team. Assisted in defining the overall implementationrequirements for WFPC-2 SMOV and performed detailed reviews of those proposals,implementation plans, calendars and SMSs. Supported the HST servicing mission by firstparticipating in a number of pre-launch simulation and training exercises, and later performing realtimemonitoring, data collection and evaluation during the servicing mission itself.* Command Development: Developed ground system command constructs which were requiredfor testing and operating the WFPC-2, both pre-launch and on-orbit. The scope of this activity wassufficiently broad so involvement went beyond just creating executable procedures and software,but lent itself to active participation in and contributing to development efforts across many groupsat STScI, MOSES, JPL and the WFPC-2 Science team. The need to be responsive to ever changingdemands and requirements were met as the operational methodologies and instrumentcharacteristics evolved and/or solidified during the long series of ground tests which occurredduring this period.* SLTV: Actively participated in the WFPC-2 System Level Thermal Vacuum Test and InstrumentCalibration as the STScI/Science Commanding on-site representative at JPL. Worked closelyduring round-the-clock shifts with JPL hardware, S/W, instrument and science team personnel.Defined, modified, executed and analyzed real-time tests designed to explore and evaluate theoperating characteristics of the WFPC-2. Investigated anomalous behaviors which led to both abetter understanding of the instrument, and to changes in the methods of operating andcommanding it. Information and knowledge that was acquired during SLTV was transferred toother STScI and WFPC-2 project personnel and incorporated in the implementation of the WFPC-

Glenn Schneider – Curriculum Vita/Resume Page: 16/21 11/29/042 stored command instructions. Worked with the ESB WFPC-2 engineer on obtaining the SLTVengineering data in a timely manner from JPL and porting it to a data archive at STScI.* Tests and Simulations: The exercise of pre-deployment validation of a new science instrumentrequired extensive sub-system and integrated tests to be run both ground and flight hardware andsoftware. Supported this effort by contributing to, and participating in the various ground systemand functional tests, discrete simulations, and joint integrated simulations. In particular, to validatethe command generation capability of the ground system for the WFPC-2, and the response tothose command requests by the instrument created test proposals, calendars, and SMS's used inthese series of tests. Worked with the MOSES SI personnel in reviewing new Real-Time commandprocedures that were needed in support of these tests, and the servicing mission. Monitored theground system and instrument behavior during execution, and participated in real-time hardwareand software anomaly analysis and resolution. Worked with other members of flight team, throughthe real-time simulations, to define and improve procedures to be used during the servicing mission.* Servicing Mission: Assisted in preparing and configuring the ESB/commanding work site atthe OSS facility by setting up the hardware and S/W interfaces to permit real-time analysis on theengineering data. Developed adjunct data collection and analysis tools, and set up automated datareduction and network transfer processes. During the Servicing mission participated in the 24-hourcommanding shift coverage - monitoring instrument and spacecraft sub-system changeouts. Keysubsystem parameters were watched and trended and, for the WFPC-1 and 2 in particular, thermalconsiderations were constantly addressed and discussed with other project elements - as werecontaminant and other issues of real-time concern.* Serving Mission Observatory Verification: Served as a member of the SMOV ProposalImplementation Team. Worked on the development and implementation of engineering, calibration,and ERO proposals for the SMOV program in consultation and association with the WFPC-2 IDTand I&T teams. Identified the need for special commanding and/or structuring of the PMDBthrough a series of proposal implementation meetings and reviews. Built, tested, and delivered nonstandardcommanding for early operations of the WFPC-2. Test, and later flight, calendars andSMS's were microscopically reviewed for any deficiencies - and proposals reworked as neededwhen problems were found. During execution monitored all first-time operations, and was preparedto responded to unanticipated anomalies. Throughout this era worked with the WFPC-2engineering and science teams (JPL and SIB) to evaluate the instrument's performance andprovided information on commanding related activities to these groups through regular calibrationand team meetings. Worked with the with the WFPC-2 science team to develop a coherenttransition plan to the Cycle 4 calibration program. Currently working with both the IDT andSTScI/SIB on defining additional on-orbit and laboratory tests to better characterize and calibratethe photometric performance of the instrument, based upon on-orbit data.WFPC-1: Participated in the planning and implementation of all ground system simulation,throughput, and vehicle tests. Prepared special commanding instructions and structured inputs forthe WFPC-1. Worked on the production, and reviewed the content, of the WFPC-1 commandingon Calendars, Science Mission Specifications (SMS's) and command loads used in all GroundSystem Tests (GST's). Supported real-time monitoring of the use of the WFPC-1 during integratedsystem GST's. Participated in the development and implementation of many special WFPCengineering operations, procedures, and instructions including the implementation and redefinitionof the UV Flood, CCD decontamination procedures, integration of the NASA Standard SpacecraftComputer-1 (NSSC-1) soft safing capability and Real Time safing recovery plans. Worked withGSFC Flight Software Group (Code 512) in defining special executive flight softwarerequirements, and WFPC/NSSC-1 command interfaces for special operations. Provided"emergency" support for unplanned safing events, WFPC instrument anomalies and unforeseenTarget of Opportunity observations. Worked with WFPC engineers (both contractor and in-house)and representatives of the Telescope Instrument Branch in assessing general post-launch instrumentperformance, operational use trending, and in response to directed technical inquiries. Worked with

Glenn Schneider – Curriculum Vita/Resume Page: 17/21 11/29/04the WFPC on-site Instrument Development Team (IDT) representative to help assure that newWFPC command capabilities (not originally specified by the IDT) were implemented andassimilated into the ground systems in a faithful and efficient manner. Created new instructions,data base definitions, and supported ground testing and validation of these capabilities, whichincluded: the on-board WFPC Idle checking (and bay 5 temperature regulation) software;suppression of CCD erasure following preflashes; issuance of autoerase commands followingpyramid rotations; allowing Kspot, Bias, Dark and exposures to be preflashed and CR-Splitting ofthe latter two; and permitting subsetted CCD reads with efficient use of the onboard tape recorderand/or communications downlink.Observatory Verification: Member of the Orbital Verification (OV) Planning/ImplementationTeam. Reviewed and identified technical problems in OV proposals. Developed solutions to theseproblems and worked with the IDTs to reach closure on those items. Wrote detailed implementationplans used by personnel involved in defining science and engineering objectives, planning andscheduling of activities, developing, testing, and implementing special science instrument andspacecraft subsystem commanding, identifying required real-time support, and supplying specificdatabase constructs and entries needed to carry out these proposals.FGS/Astrometry: Served, for two years, as the STScI Operation Division's technical representativeto the Space Telescope Astrometry Team. Worked with the team on defining baseline functionalastrometric requirements. Developed command constructs and procedural logic for using the HSTFine Guidance Sensors (FGS's) to carry out astrometric science observations, and special OrbitalVerification focus and alignment tests. Oversaw the creation of test calendars, and SMS's used tovalidate FGS commanding. Participated in ground-system simulation, unit level hardware, andvehicle testing of Fine Guidance Electroncs/FGS commanding. Developed and provided software toassist in the Real-Time analysis of FGS, Pointing Control System and Optical Telescope Assemblytelemetry during early on-orbit operations.Operations Support: Reviewed proposals scheduled for execution and resulting commanding onflight SMS's. Participated in iterative SMS analysis/rerun cycling during the OV, SMOV, ScienceVerification epochs, and Science Assessment and Early Return Observations. Uncovered andreported numerous problems, developed and offered solutions to SPSS, User Support and SciencePlanning Branches (SPB) as appropriate. Worked with SPSS personnel on fixing many problemsrelated to improper PMDB population or proposal structure, and interpreting PASS missionscheduler and command loader products. Often consulted with the proposer (directly or throughSPB) to recommend proposal changes to enable his/her scientific or engineering goals to beaccomplished when the proposal itself was improperly or incompletely specified. Developed manysoftware tools which were provided to various branches of the Operations and Systems Engineeringdivisions to assist in validating the integrity of transformation products, the PMDB, and flightSMS's and to facilitate engineering data analysis.HST/WFPC (1 & 2) Instrument Calibration and Engineering ProgramsWFPC-2 SOFA Partial Stepping Test, Co-InvestigatorWFPC K-Spot Reflectivity Test, Principle InvestigatorWFPC Calibration: UV Flood Test, Co-InvestigatorWFPC Calibration: UV Grism Test, Co-InvestigatorWFPC Light-Pipe Throughput Test, Co-Investigator

Glenn Schneider – Curriculum Vita/Resume Page: 18/21 11/29/04Catonsville Community College (1987-1989)Appointment: Adjunct Faculty in AstronomyGeneral Responsibilities: Taught laboratory and lecture sessions of introductory astronomy forundergraduate, associate degree candidate, and "nontraditional (returning) students. Planned andexecuted curricula, lesson plans and in-class observing exercises. Developed planetarium based andaugmented education program.Department of Astronomy - University of Florida (1978-1982, 1984-1985)South Pole Telescope: Designed, implemented and tested the firmware program for the automatedoperation of the University of Florida's multi-color photometric South Pole Telescope. Developedprocess control, data acquisition and calibration management software. Assisted in telescope,photometer, and control system mechanical and electronic design, fabrication, and telescopecalibration. Performed instrument installation, photometric calibration and operational field check atthe Amundsen-Scott South Pole Station. Performed instrument anomaly analysis during observingseason. Returned to the South Pole for post-season instrument performance evaluation andengineering diagnostics. Reduced and analyzed photometric data as part of a quantitative site surveyprogram, as well as astronomical studies of γ 2 Velorum and HR 2554. This work was supported byNational Science Foundation grants DPP 82-17830 and DPP 84-14128.Additional Instrumental Work: Designed, fabricated, and installed a new Cassagrain light baffleand offset guiding systems for the RHO 76 cm. telescope. Designed and built a multi-channeldigital data acquisition system to be used by several photometric instruments. Redesigned and putinto working service a 3-color flare star photometer. Designed and constructed coelostat fed flashspectrograph employing a U.T.-synchronous high speed camera used for obtaining time resolvedspectra of the solar chromosphere and inner corona during the inner tangential contacts of solareclipses. Interfaced an Ebert-Faste scanning spectrograph to a microprocessor based controlsystem, and used this system to determine the size of the Hα emission region of several B-emission(shell) stars, including Zeta Tauri. Performed maintenance and repairs on Alvin Clark 20 cm.refractor and Celestron telescopes at UF's student observatory.Teaching Responsibilities & Experience: Taught laboratory and lecture sections ofintroductory general undergraduate astronomy, astronomy for astronomy majors, astronomical(observing and data analysis) techniques, and digital electronics. Planned, supervised and evaluatedin class exercises in astronomy, data manipulation and analysis, instrumentation. Taught and trainedstudents in observational methods in photographic and photoelectric photometry at Rosemary HillObservatory (76 cm telescope) and on-campus student observatory. Maintained and rebuilt facilitiesand telescopes at on-campus student observatory. Taught seminar series on APL programming forphysical sciences and computer programming with APL.Space Astronomy Laboratory - University of Florida (1982-1984)Giotto/Halley Optical Probe Experiment: Ground System data acquisition and real-timeanalysis S/W lead for (multi-channel photo-polarimeter employing a MAMA detector) flown on theEuropean Space Agency's Giotto Mission to Halley's Comet. Designed, developed andprogrammed ground support equipment and real-time spacecraft simulator. Assisted in opticalcalibration, electronic circuit board design, fabrication, and calibration of engineering and flightmodel units. Performed flight unit engineering checkout during spacecraft/payload Assembly &Verification at British Aerospace. Worked with project mission planners and scientists at the

Glenn Schneider – Curriculum Vita/Resume Page: 19/21 11/29/04European Space Agency (Noordwijc, Netherlands) and Service d'Aeronomie-Centre National de laRecherche Scientifique (Paris, France) on many payload interface and operational issues.Additional Instrumental Work: Specified, designed, and programmed a microcomputerinterface for an optical vignetting table for photometric and radiometric calibration of spacecraftinstrumentation as part of a collaborative project between the Space Astronomy Laboratory andRuhr-Universitat, Bereich Extraterrestrische Physik (Bochum, W. Germany).Warner Computer Systems, Inc. (1976-1980)APL Technical Consultant: Maintained public and development system workspace libraries.Wrote system specific application functions and integrated them into the libraries. Developedplotting/graphics display software for Tektronix, Versatek, and Diablo/Spintronic devices.Supervised creation of documentation of APL software libraries by technical writing staff.APL Technical Analyst: Developed turn-key end-user directed software systems. Productscreated included software for econometrics forecasting, statistical analysis, laser/resonant-cavitydesign, message and packet switching, and inventory and process control. Conducted APLprogramming classes and handled technical inquires from time-sharing clients.Observing ExperienceHubble Space Telescope: Near Infrared Camera & Multi-Object Spectrometer, WideField/Planetary Cameras (1 & 2), Fine Guidance Sensors (astrometric interferometry), SpaceTelescope Imaging Spectrograph, Advanced Camera for SurveysTransition Region Coronal Explorer (TRACE)Heinrick Hertz Sub-Millimeter TelescopePalomar/PHARO Adaptive Optics SystemData Analysis/Reduction from Keck-II and Lick {NGS+LGS} AO Systems and IRTFSolar chromospheric/inner coronal spectroscopy and polarimetrySpace Radiometry (ACRIMSAT)A wide range of small fixed, and portable optical telescopes and CCD imaging systems.Multi-color differential photometry of eclipsing and intrinsic variablesFast photometry of lunar and asteroidal occultationsPhotography with hyersensitized platesPlate reduction with iris photometer and microdensitometerComputer ExperienceHardware, Mainframes/WorkStations Operating Systems: VAX 11/750,11/780, 8600, 8800,Alphas (VMS); Sun SparcStations (Solaris 2.4+); Apple Macintosh G4 & G5 (OS X); Xerox6/7/9 and 560 systems (CP-V, UTS, BPM); IBM 360, 370, 3033N, 3081, 3094 and 4341 (OS/VS,MVS); DEC 20 (TOPS); Ahmdal 470/V6; Harris 500; PDP-11/34; Data General Nova

Glenn Schneider – Curriculum Vita/Resume Page: 20/21 11/29/04Hardware, Micros/PC's: Rockwell AIM-65 and RM-65 systems; Apple Macintosh (MacOS, allflavors 6.0—10.3.1); Apple II, II+, IIe; HP-85a; MCM 700; Commodore Pet, SX-64, and SP-9000; IBM 5100, 5110, and PcSoftware: Programming environments: APL, IDL, FORTH, BASIC, 6502, 6800 and RCA 1802machine and assembly languages. Special Purpose Application Programs: numerous for dataanalysis packages, graphics and image display (e.g., TRANSFORM, KALEIDAGRAPH,PHOTOSHOP, CANVAS) Systems utility functions and development s S/W: MacOS and VMS.Professional Society MembershipInternational Astronomical Union (division DII working group on solar eclipses 2003-2006)American Astronomical SocietySPIE (International Society for Optical Engineering)American Association for the Advancement of ScienceAssociation for Computing Machinery (SIGAPL)International Occultation Timers AssociationHonors and AwardsASP - Maria and Eric Muhlmann Award for 2003 (NICMOS IDT)NASA/GSFC - Science Leadership AwardSPACE TELESCOPE SCIENCE INSTITUTE - Individual Achievement AwardNASA - Public Service Achievement Award: HST Orbital VerificationNASA - Achievement Award: WFPC-2 Science TeamNASA - Project Award: HST ProgramNASA - Project Award: HST 1st Servicing MissionJET PROPULSION LABORATORY - WF/PC II Project Award: SLTV and CalibrationNASA/GSFC - Achievement Award: HST 1st SM WFPC-2 Development and DeliveryNASA/GSFC - Achievement Award: HST 1st Servicing Mission Integration & TestNASA/GSFC - Achievement Award: HST 1st Servicing Mission Observatory VerificationNASA/GSFC - Achievement Award: HST NSSC-1 FSW, Mission Ops, Engineering Support, IDTNASA/GSFC - "Special Act" Award (HST Continuous Process Improvement Team)NASA/GSFC - Certificate of Recognition (HST Program)NYIT - Physics Research AwardNYIT - Silver Medal for Physics ResearchMember: Sigma Pi Sigma (National Physics Honor Society)

Glenn Schneider – Curriculum Vita/Resume Page: 21/21 11/29/04Recent Public/Community ServiceHubble Space Telescope Post-SM4 Scientific Review Panel (D. Black, Chair)Independent Report to STScI: HST/NICMOS & Ground-Based/AO Capabilities(NASA/GSFC) NICMOS Dewar Anomaly Review Board (G. Morrow, Chair)PublicationsRefereed Publications (44), Conference Proceedings (36), Meeting Abstracts/Presentations (71),Special/Solicited Reports (8), Others (5). See separate Publication List.