About

Timothy Glotch is a planetary geologist and the Department Chair at the Department of Geosciences at Stony Brook University. His research interests include quantitative remote sensing at infrared wavelengths of the surfaces of Mars, the Moon, Earth, and small bodies, laboratory spectroscopic measurements of minerals, extraterrestrial samples, and their analogs under simulated lunar or asteroid environments, as well as micro-Raman and nano-infrared spectroscopy of terrestrial and extraterrestrial samples. He is the principal investigator of the RISE2 node of NASA’s Solar System Exploration Research Virtual Institute and a co-investigator on the Lunar Reconnaissance Orbiter Diviner Lunar Radiometer science team. Additionally, he was a Participating Scientist for the remote sensing portion of NASA’s OSIRIS-REx sample return mission to the near-Earth asteroid Bennu. His recent research involves detailed micro- and nano-spectroscopic analyses of samples from near-Earth asteroids Ryugu and Bennu to uncover the history of early geochemical reactions in our Solar System, as well as analyses of lunar samples returned by Apollo missions to understand the genesis of unusual lunar rock types. He collaborates with teams at Brookhaven National Laboratory to identify signatures of uranium mining and milling activities from orbital hyperspectral imagers, supporting the Department of Energy's nuclear nonproliferation efforts.

Research topics

• Geology
• Astrobiology
• Physics
• Paleontology
• Geochemistry
• Mineralogy
• Astronomy
• Materials science
• Chemistry
• Mathematics
• Organic chemistry
• Remote sensing
• Earth science
• Statistics
• Astrophysics
• Environmental chemistry

Selected publications

• Supplement Materials: Effects of Particle Size, Temperature, and Metal Content on VNIR Spectra of Ordinary Chondrite Meteorites in a Simulated Asteroid Environment

  2026-01-01

  report

  Laboratory spectral analysis of well-characterized meteorite samples can be employed to more quantitatively analyze asteroid remote sensing data in conjunction with returned extraterrestrial samples. In this work, we examine the combined effects of physical (temperature, particle size) and chemical (petrologic type, metal fraction) variables on VNIR spectra of ordinary chondrite meteorite powders. Six equilibrated ordinary chondrite meteorite falls were prepared at a variety of particle sizes to capture the spectral diversity associated with asteroid regoliths dominated by various grain sizes. Mineral compositions and abundance were determined from electron microprobe analysis of meteorite thick sections to precisely characterize changes in spectral features due to variations in mineralogy. VNIR spectra of the ordinary chondrite material were measured under simulated asteroid surface conditions at a series of temperatures chosen to mimic near-Earth asteroid surfaces. The resulting spectra show minimal variation in both major absorption bands across the simulated near-Earth asteroid temperature regime. Changes in particle size result in variations in band centers and band area ratios for material of the same composition, two key parameters typically used to derive asteroid composition. Unlike previous spectral investigations of ordinary chondrites, we retained the metal fraction in our powders instead of analyzing the silicate fraction only. Metal has a subtle but non-negligible effect on the VNIR spectra of ordinary chondrites. The more petrologically pristine samples from each ordinary chondrite group display relatively weaker absorption bands than their more thermally altered counterparts. The band centers shift to longer wavelengths as temperature, grain size, and petrologic type increase.

  PublisherDOI

• Nanoscale infrared spectroscopy reveals complex organic–mineral assemblages in asteroid Bennu

  Proceedings of the National Academy of Sciences · 2026-03-30

  articleOpen access

  Asteroid Bennu preserves primitive material from the early solar system, and returned samples allow direct examination of how organics and minerals were assembled and altered. We applied nanoscale infrared spectroscopy together with Raman spectroscopy to the Bennu sample OREX-800066-3 to characterize chemical variability at ~20 nm scales. Analysis of nano-Fourier-transform infrared spectroscopy spectra identifies three recurring compositional domains; aliphatic-rich, carbonate-rich, and nitrogen-bearing organic-rich regions. Statistical evaluation shows that these domains are compositionally and spatially distinct at the nanoscale, with strong negative correlations between aliphatic signatures and both carbonates and N-bearing organics, and negligible correlation between carbonates and N-bearing organics. Organosulfur compounds are spatially restricted to carbonate-rich regions, indicating organic-sulfate interactions during late-stage brine evolution. Raman spectra indicate highly disordered, thermally minimally metamorphosed carbonaceous matter, consistent with preservation of labile functional groups. These results demonstrate that Bennu's angular lithology (characterized by planar facets and sharp edges) is not chemically uniform and records heterogeneous aqueous alteration rather than pervasive uniform processing. N-bearing organic functional groups are widely preserved despite extensive alteration, and carbonate-rich areas show intimate nanoscale mixing of different carbonate species. The coexistence of distinct organic- and carbonate-rich domains suggests contributions from both primordial compositional diversity and subsequent rock-fluid interaction. Comparison with Ryugu samples highlights shared features but key differences in organic-carbonate associations and carbonate distributions. Overall, Bennu's nanoscale heterogeneity provides constraints on organic preservation, carbonate formation, organic-sulfate chemistry, and parent-body evolution in volatile-rich early solar system materials.

  PublisherDOI

• Geomorphological Analysis of Martian Chloride Salt-Bearing Deposits

  2026-02-20

  articleOpen accessSenior author

  Remote sensing data have identified numerous chloride salt-bearing deposits across the Martian southern highlands. Due to the high solubility of chloride salts, these deposits may indicate the last stable liquid water on the Martian surface. Analyses of the deposits’ morphologies, ages, and surrounding topographies may provide crucial clues for understanding the hydrologic past of Mars. Many hypotheses regarding the formation of these deposits have been proposed (for example, ponding and evaporation of upwelled groundwater, surface runoff, or formation in shallow lacustrine environments), but no consensus has yet been reached, and it is possible that multiple formation pathways resulted in chloride salt deposition. In this work, we use salt map/digital terrain model (DTM) overlays to perform geomorphological analyses of chloride depositional environments. A Hapke-based abundance estimation technique was used to create salt abundance maps from Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) imagery that overlies chloride-bearing deposits. We used Context Camera (CTX), High Resolution Imaging Science Experiment (HiRISE), and High Resolution Stereo Camera (HRSC) datasets to create DTMs. We have identified 4 target regions (Terra Sirenum, N-NE Noachis Terra, W of Hesperia Planum, and E of Hesperia Planum to Terra Cimmeria) in the southern highlands and focused our analyses on ~4-5 deposit clusters within each target region, forming a representative sample of deposit variability. We have selected clusters based on diversities in how chloride deposits map with elevation, underlying deposit age (ranging from late Noachian to early/mid Amazonian), valley network density, and surrounding geologic features such as channels or flat expanses. The combination of elevation data from DTMs, high resolution imagery for surrounding context, and CRISM salt abundance maps enables us to place constraints on deposit thickness and extent, chloride salt volume, and brine-forming pond/lake volumes if applicable. Studying variability among deposits will assist in determining if chlorides formed from a universal process or multiple, localized processes. The chloride salt map/DTM overlays created in this work will enhance understanding of these deposits and assist in the determination of their origin.

  PublisherOA PDFDOI

• Paragenetic Formation of Aqueous Alteration Minerals: Thermodynamic Modeling of Basalt Weathering on Early Mars

  2026-05-15

  articleOpen access

  Basalt preferentially produces Fe(III) nontronite and Fe(II)/Mg saponite-rich assemblages in open and closed system weathering, respectively. Formation of non-evaporative sulfates and carbonates require geochemically distinct conditions.

  PublisherOA PDFDOI

• Effects of Particle Size, Temperature, and Metal Content on VNIR Spectra of Ordinary Chondrite Meteorites in a Simulated Asteroid Environment

  Journal of Geophysical Research Planets · 2026-03-01

  article

  Abstract Laboratory spectral analysis of well‐characterized meteorite samples can be employed to more quantitatively analyze asteroid remote sensing data in conjunction with returned extraterrestrial samples. In this work, we examine the combined effects of physical (temperature, particle size) and chemical (petrologic type, metal fraction) variables on visible and near‐infrared (VNIR) spectra of ordinary chondrite meteorite powders. Six equilibrated ordinary chondrite meteorite falls were prepared at a variety of particle sizes to capture the spectral diversity associated with asteroid regoliths dominated by various grain sizes. Mineral compositions and abundance were determined from electron microprobe analysis of meteorite thick sections to precisely characterize changes in spectral features due to variations in mineralogy. VNIR spectra of the ordinary chondrites were measured under simulated asteroid surface conditions at a series of temperatures chosen to mimic near‐Earth asteroid surfaces. The resulting spectra show minimal variation in both major absorption bands across the simulated near‐Earth asteroid temperature regime. Changes in particle size result in variations in band centers and band area ratios for material of the same composition, two key parameters typically used to derive asteroid composition. Unlike previous spectral investigations of ordinary chondrites, we retained the metal fraction in our powders instead of analyzing only the silicate fraction. Metal has a subtle but non‐negligible effect on the VNIR spectra of ordinary chondrites. The more petrologically pristine samples from each ordinary chondrite group display relatively weaker absorption bands than their more thermally altered counterparts. The band centers shift to longer wavelengths as grain size and petrologic type increase.

  PublisherDOI

• Reflectance spectroscopy (200-4200 nm) of the red-sloped C2 carbonaceous chondrites MET 00432, Tagish Lake, Tarda, and WIS 91600 (“CT” grouplet)

  Icarus · 2026-01-22

  article
  PublisherDOI

• Geomorphological Analysis of Martian Chloride Salt-Bearing Deposits

  2025-12-26

  articleOpen accessSenior author

  Remote sensing data have identified numerous chloride salt-bearing deposits across the Martian southern highlands. Due to the high solubility of chloride salts, these deposits may indicate the last stable liquid water on the Martian surface. Analyses of the deposits’ morphologies, ages, and surrounding topographies may provide crucial clues for understanding the hydrologic past of Mars. Many hypotheses regarding the formation of these deposits have been proposed (for example, ponding and evaporation of upwelled groundwater, surface runoff, or formation in shallow lacustrine environments), but no consensus has yet been reached, and it is possible that multiple formation pathways resulted in chloride salt deposition. In this work, we use salt map/digital terrain model (DTM) overlays to perform geomorphological analyses of chloride depositional environments. A Hapke-based abundance estimation technique was used to create salt abundance maps from Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) imagery that overlies chloride-bearing deposits. We used Context Camera (CTX), High Resolution Imaging Science Experiment (HiRISE), and High Resolution Stereo Camera (HRSC) datasets to create DTMs. We have identified 4 target regions (Terra Sirenum, N-NE Noachis Terra, W of Hesperia Planum, and E of Hesperia Planum to Terra Cimmeria) in the southern highlands and focused our analyses on ~4-5 deposit clusters within each target region, forming a representative sample of deposit variability. We have selected clusters based on diversities in how chloride deposits map with elevation, underlying deposit age (ranging from late Noachian to early/mid Amazonian), valley network density, and surrounding geologic features such as channels or flat expanses. The combination of elevation data from DTMs, high resolution imagery for surrounding context, and CRISM salt abundance maps enables us to place constraints on deposit thickness and extent, chloride salt volume, and brine-forming pond/lake volumes if applicable. Studying variability among deposits will assist in determining if chlorides formed from a universal process or multiple, localized processes. The chloride salt map/DTM overlays created in this work will enhance understanding of these deposits and assist in the determination of their origin.

  PublisherOA PDFDOI

• The Utility of a Hyperspectral Infrared Imager for Crewed Exploration of Planetary Bodies

  Earth and Space Science · 2025-10-01 · 1 citations

  articleOpen accessSenior author

  Abstract Planetary analog simulations are a powerful exercise for understanding the utility of deployable instruments, their operational protocols, and the visualization of data products during ExtraVehicular Activities (EVAs). This paper presents results of a field campaign by the NASA Solar System Exploration Research Virtual Institute (SSERVI) Remote, In Situ and Synchrotron Studies for Science and Exploration‐2 (RISE2) team to Kilbourne Hole, New Mexico in March/April 2023 to test the utility of a portable thermal infrared (TIR) hyperspectral imager (HSI) during four EVA simulations. The HSI provides emitted radiance spectra from 7 to 14 μm to map spectral variations likely caused by composition and physical properties, which allows HSI data products to aid in sample selection and site documentation. Four pairs of analog astronauts performed a mock EVA at three stations with field deployable instruments including an HSI. The HSI was found to be a useful tool for performing reconnaissance observations, field site documentation, and sample selection for visibly indistinct materials. From these analog simulations we prioritize two recommendations for use of HSI's in crewed missions. First, HSI‐derived data products should be tailored for the specific science objectives and/or sampling objectives of the mission to expedite interpretation and decision‐making. Second, the HSI instrument would ideally have a wide field‐of‐view/panoramic capability to reduce crew time selecting sites to image. Additionally, pre‐EVA reconnaissance from a remotely operated rover could be conducted with an HSI to collect data prior to disturbance and again post human activity.

  PublisherOA PDFDOI

• Mineralogy and Geochemistry of Xenoliths and Phreatomagmatic Deposits in Potrillo Volcanic Field, New Mexico, Determined from Portable Instruments: Applications to Surface Exploration of the Moon and Mars

  The Planetary Science Journal · 2025-10-01

  articleOpen access

  Abstract Instruments that yield information about the mineralogy and chemistry of surface materials will be part of future robotic and human exploration of the Moon and Mars. Accurate interpretation of such data can be informed by coordinated analyses of relevant materials in terrestrial analog terrains. We used a suite of portable instrumentation—visible-to-shortwave infrared (VSWIR) spectroscopy, thermal infrared (TIR) spectroscopy, and X-ray fluorescence—to conduct coordinated mineralogical, geochemical, and visual characterization of a suite of outcrops and loose rocks in Kilbourne Hole and Hunts Hole, New Mexico. A variety of textures, particle sizes, and petrogenetic origins were examined. Data were interpreted using spectral models, spectral library comparisons, and chemical calibration curves and compared to mineralogical information derived from X-ray diffraction. Insights and limitations for each technique are presented in terms of surface type; for example, both the VSWIR and TIR instruments exhibited limitations in discerning the full mineralogy of the fine-grained tuff beds. The diverse suite of xenoliths was apparent in TIR spectral images, and the dominant mineral component was identifiable through linear unmixing of TIR spectra. However, inaccuracies in mineral abundance were also observed, highlighting the need for use of more advanced analysis methods. Known lithological diversity was less apparent in VSWIR spectra, which were dominated by minor amounts of phyllosilicates within or coating the rocks. Finally, based on the dearth of mafic minerals and the abundance of quartz, we infer that the Kilbourne/Hunts tuff beds are dominated by fragments of country rock (“accidentals”) rather than juvenile magmatic materials.

  PublisherDOI

• Compositional and Morphological Variations of Effusive Lava Flows and Explosive Pyroclastic Deposits at the Caldera‐Forming Gardner Shield Volcano on the Moon

  Journal of Geophysical Research Planets · 2025-05-01

  article

  Abstract We identified a ∼31 km diameter caldera with a well‐developed ring fault and ring dike structure at the Gardner shield volcano. Using Chandrayaan‐1 Moon Mineralogy Mapper (M 3 ) and Lunar Reconnaissance Orbiter (LRO) Diviner data, we investigated 15 effusive flow units and an explosive unit. Spectral analysis revealed compositional similarities between effusive and explosive eruptions, indicating a single sourced magmatic eruption. Detailed hyperspectral and multispectral analyses (visible, near‐infrared, thermal infrared, and radar) indicate the presence of explosive pyroclastic material in the central part of the shield. We identified key morphological structures at the Gardner shield, including three major faults, the caldera's ring fault and ring dike structure, subsidence and resurgence crustal blocks, a graben, a parasitic cone, and extended lineaments beyond the previous work. Our analysis indicates that the well‐developed Gardner caldera exhibits lower subsidence compared to Earth's calderas, likely due to the Moon's lower gravity and lower crustal density. These surficial structures preserve the evidence of subsurface magmatic chamber dynamics, making the Gardner shield a unique location for understanding the thermophysical evolution of a central vent shield regime on the Moon. We describe six evolutionary stages, evidenced by multiple volcano‐tectonic structures, two distinct eruption styles, and the shield's relationship with the subsurface magmatic chamber, revealing a thermophysical evolution of a central‐vent polygenetic shield volcano on the Moon, following a formation mechanism similar to those observed in the shield volcanoes on Earth and Mars.

  PublisherDOI

Recent grants

• CAREER: Fundamental Measurements of Mineral Optical Properties and Theoretical Treatment of Light Scattering at Infrared Wavelengths

  NSF · $494k · 2012–2018

Frequent coauthors

• P. R. Christensen

  Arizona State University

  333 shared

• M. A. Barucci

  Sorbonne Paris Cité

  243 shared

• J. R. Brucato

  Arcetri Astrophysical Observatory

  204 shared

• Joshua P. Emery

  204 shared

• Salvatore Ferrone

  Observatoire de Paris

  203 shared

• B. E. Clark

  Radiology Associates of Albuquerque

  203 shared

• M. Pajola

  Osservatorio Astronomico di Padova

  203 shared

• Marco Delbó

  University of Leicester

  203 shared

Education

• B.A.

  Colgate University

  1999

• Ph.D., Geological Sciences

  Arizona State University

  2004

Awards & honors

• NASA’s Solar System Exploration Research Virtual Institute (…
• Participating Scientist for NASA’s OSIRIS-REx sample return…