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Laboratory We Astrophysics Newsletter, whose goal is to enhance communication and interactions between experi- mentalists, theoreticians, modelers, and observers in the fields of Astrophysics and Planetary Science around the world. This newsletter was initiated by the led at Cold Solar System Objects (CSSO) project NASA Ames Research Center (ARC) and in collaboration with NASA Goddard Space Flight Center (GSFC). The overarching goal of the CSSO to investigate and understand the project composition, chemical processes occurring on the surfaces and in the atmospheres of cold Solar System objects using unique facilities and expertise at NASA ARC and GSFC.

evolution,

origin,

and

Michel Nuevo

Ella Sciamma-O’Brien

This newsletter is intended to be released quarterly. Each issue will focus on a particular theme in the Laboratory Astrophysics field and include sections such as a cover interview, a description of facilities, recent publications in the field, and/or announcements for upcoming meetings.

image, a scientist

Partha Bera

Lora Jovanovic

Laboratory

the Astrophysics The of theme issue is Cold Solar System Newsletter’s first Objects. We present an interview of Dr. Farid Salama, a leader in Laboratory Astrophysics research at NASA ARC and has advocated for the field for decades. The laboratory facilities presented in this issue are the 5 facilities of the CSSO project team and include: the Ices, Ice Irradiation, and Organics Laboratory for Astrobiology (I3OLAB), the COsmic the Optical SImulation Chamber Constants Facility (OCF), and the Matrix Isolation/ Optical Constants of Ices (MIOCI), at NASA ARC, as well as the Cosmic Ice Laboratory at NASA GSFC. The long list of recent publications in this first issue covers work published since the beginning of 2025 and demonstrates the abundance and productivity of research conducted in the field of Laboratory Astrophysics within the Planetary Science commu- nity. Finally, several upcoming meetings relevant to the field of Planetary Science and Astrochemistry are listed in this issue.

(COSmIC),

Joseph Roser

Aaron McKinnon

In future issues, we look forward to featuring various Laboratory Astrophysics themes and include inter- views of scientists and presentations of facilities around the world.

Visit our newsletter website for current and past issues here.

We welcome contributions to the newsletter. You can share publications and announcements through our contribution form here, and join our mailing list or contact us at labastronewsletter@mail.nasa.gov.

We publish quarterly! Keep an eye out for our next issue. Welcome to the Lab Astro newsletter!

The Editorial Team

NASA.gov/ames/science/lab-astro-newsletter

December 2025

Interview with Dr. Farid Salama Astrophysicist at NASA Ames Research Center

use of laser reaction excitation spectroscopy as a tool to locate extremely weak vibronic transitions that can be activated by near-infrared photons. The goal of the research project was to identify molecules that can offer a way to accomplish new chemical synthesis with long-wavelength near-infrared solar photons.

The second offer was a National Research Council (NRC) fellowship to work at NASA Ames with Lou Allamandola who was just setting up a new IR Lab Astro Laboratory in the Space Science Division to support the NASA Kuiper Airborne Observatory (KAO). This is where I got exposed to Laboratory Astrophysics for the first time with the opportunity to work on Jupiter’s moon, Io. My core project, however, was to set up a Lab Astro Laboratory in the UV-visible range using my experience with MIS and VUV spectroscopy. found this multidisciplinary work fascinating, and I decided to continue working in this field. In addition, having built and set up a new experimental system I was keen to work and perform research with this new tool close to my heart.

Briefly, my career path is as follows: graduate student and PhD in molecular physics at the University of Paris-Orsay and the Pierre & Marie Curie Institute in Paris, followed as postdoc at the LBL, UC Berkeley, and, since then, worked in the Astrophysics branch of the Space Science Division at NASA Ames first as a NRC fellow, then as a UC Berkeley Astronomy research assistant, SETI PI and finally as a NASA civil servant. I’m currently the Director of the COSmIC Facility where I have had the pleasure to work with a fantastic team of young and seasoned scientists and engineering technicians over the past years who helped make it possible to build this truly unique laboratory facility.

What inspired you to become a scientist? Which scientist had the largest impact on your research or inspired you?

I was initially not considering going into research and becoming a scientist. I was advised and encouraged by my university Professors to go beyond the Master and try a one-year postgraduate degree for advanced studies

Farid Salama is an Astrophysicist in the Space Science and Astrobiology Division at NASA Ames Research Center. His current research is centered around the study of interstellar, planetary and exoplanetary molecules and ions in the laboratory and the formation of grains and aerosols from molecular precursors in astrophysically relevant environments.

How did you get into Lab Astro research? Can you tell us about your career path?

I got into lab astro research by coincidence. I had not been involved in astronomy and astrophysics before. My background was in Molecular Physics and Physical Chemistry working on molecules and I molecular ions. After I graduated from my PhD, applied for a postdoc and received two offers for positions in Northern California.

the Lawrence One offer was in UC Berkeley, at Berkeley Lab (LBL) in the laboratory of Prof. Pimentel who had developed the technique of Matrix Isolation Spectroscopy (MIS) to work with Heinz Frei on the useo

studies (DEA in France). I ended up selecting a project, among the many I had been presented with, that was based on molecular spectroscopy using the time I was MIS technique. This was the first confronted with research, and I I was actually very interested in continuing in this direction.

found that

Many scientists I met during my career had a large impact on my research and inspired me. In science we build ourselves on the knowledge and experience the scientists who preceded us. As the saying of goes: “We stand on the shoulders of the giants that preceded us”. To cite a few, these include my thesis adviser, Janine Fournier, who guided me in my first exposure to a research lab, Antoine Fournier, the Director of the Lab, who was an unconventional scientist who taught me a lot too. The discussions I had with Sidney Leach who was leading the Molecular Photophysics Laboratory in Orsay had also a strong impact on my career choices. When I moved to the US and started my career as a researcher, the in UC Berkeley, and Lou late George Pimentel Allamandola and Xander Tielens at NASA Ames are among the researchers who inspired me a lot.

I was also quite inspired by the late Giacinto Scoles, a Professor in Princeton and a pioneer in the study of intermolecular forces whom I met as a PhD student visiting the University of Waterloo in Canada in 1985 during my postgraduate studies. I happened to attend the university where he a seminar he gave at encouraged young students and early career scientists to choose a topic that attracted them its current popularity or conceived regardless of importance and to work hard until becoming a world expert in the subject topic. His advice was that this approach helped science. His advice struck me as worth following and my career and experience showed me how correct his advice was.

What is your current research about? What motivates you in your research? What do you enjoy the most about your research?

My research centers on molecular spectroscopy and mass spectrometry in the areas of laboratory astrophysics and astrochemistry in conjunction with ground-based and space-based ultraviolet, optical and infrared astronomy (Diffuse Interstellar Bands (DIBs) and Aromatic Infrared Bands (AIBs) in galactic and extragalactic environments; planetary ices; planetary and exoplanetary atmospheres, etc.).

What motivates me in my research is to increase our knowledge and strengthen our understanding of the composition of the materials that surround us (inter- stellar clouds, circumstellar environments, planets, planetary atmospheres, exoplanets, comets, etc.). I’m also driven by the curiosity of identifying elements that are ubiquitous in space such as the hundreds of absorption bands in the visible and the emission bands in the IR.

The COSmIC Team: Farid Salama, with, from left to right, Lora Jovanovic, Ella Sciamma-O’Brien, David Dubois, Salma Bejaoui, and Claire Ricketts.

What do you consider to be your greatest achievement in your research? What impact has your research had in the field?

(COSmIC) interstellar,

I consider the design and development of the Cosmic to Simulation Chamber generate laboratory analogs of circumstellar, ions and planetary and exoplanetary molecules, grains as my greatest achievement. This unique facility has had a strong impact in interstellar and exo- circumstellar planetary studies and has allowed breakthroughs such as the first survey of DIBs in translucent clouds for PAH signatures, the formation of circumstellar grain analogs in the laboratory, and the measure- ments of planetary and exoplanetary haze molecules and aerosols.

astrophysics,

planetary

and

The COSmIC Facility impact was recognized with a NASA Award for the unique and “recognition of exceptional contribution to astrophysics and planetary advances (image on next page).

In 2022, Farid Salama was named a fellow of the AAS in recognition of his significant advances in astrophysics and astrochemistry, and for his service to the community through the creation of the Lab Astro Division of the AAS.

I contributed to a Regarding the science aspect, better knowledge of the spectra of PAH ions by providing the first spectroscopic data on the electronic isolated PAHs molecules and ions spectra of measured with COSmIC under astrophysically relevant conditions that led to the first survey of PAHs in the search of Diffuse Interstellar Bands in galactic and extragalactic environments. I also contributed to the formation of laboratory analogs of circumstellar carbon grain with COSmIC. I also contributed to the first results on planetary ices on Io (Jupiter’s moon) for comparison with infrared airborne data as well as the formation of laboratory analogs of planetary aerosols with COSmIC for a better understanding of Titan’s (Saturn/s moon) and other planetary hazes. I also participated to the ORGANIC experiments on the facility EXPOSE-R on the International multi-user investigated the chemical Space Station where I chemical and evolution, modification of PAHs and fullerenes in space.

destruction,

survival,

Regarding the science advocacy aspect, I played a laboratory astro- key role in the establishment of physics as a recognized and vital field of science. I am a co-founder of the Laboratory Astrophysics Division of the American Astronomical Society (AAS) launched in 2012, and I helped found the the American Astrochemistry sub-commission of Chemical Society subsequently launched. I also founded the International Astronomical Union (IAU) Laboratory Astrophysics Commission. In both cases, I played a leading role, as Chair of the AAS LAD Division and first President of the IAU Commission.

Which open question in Lab Astro would you like to see answered in the near future?

I would like to see a full identification and charac- ions, grains) the species (molecules, terization of responsible for the DIBs seen all over the universe, in galactic

Top: In 2003, G. Scott Hubbard, NASA Ames Research Center’s director awarded Farid Salama the NASA Exceptional Achievement Medal for developing a unique experimental facility in laboratory astrophysics and for innovative research on diffuse interstellar bands. Bottom: A picture of the plasma produced in the COSmIC chamber to simulate astrophysical environments.

How has the field evolved since you started your career in Lab Astro? What role did you play in it?

The field of Lab Astro has largely evolved since I started my career and continues to evolve at an impressive pace. Because of its multidisciplinary aspect and the requirement to address problems and issues that are beyond the current level of knowledge in fundamental science (physics, chemistry, etc.), Laboratory Astrophysics is continuously challenged to push the limits of science. The discovery of a new form of carbon (fullerene C60) that resulted from a laboratory study of potential carriers of the Diffuse Interstellar Bands led to a Nobel prize for the researchers and is a testimony to the strong impact of Laboratory Astrophysics on basic sciences.

The role I have been playing in Lab Astro has had various components: direct contribution to science leadership and mentorship as laboratory results, director and advocacy for the field.

galactic and extragalactic environments. Identifying the DIBs is a key open question for astrophysics and astronomy. Identifying the carriers of the DIBs has various from probing the Galactic structure and evolution to unraveling interstellar chemistry and answering fundamental questions in astrobiology.

implications

What was the most important advice somebody gave you?

Most important advice: choose a topic that attracts you (see Giacinto Scoles above) and believe in and advocate your research.

Do you have some advice for early career scientists?

My advice: choose a science field that you like/enjoy, make sure to work in a friendly environment with a friendly team (teamwork is essential), although research is competitive, try to always work with an open team spirit. Stay motivated, curious and, most of all, modest. Learn to open up to other fields and activities and look to each for the values they provide to our global knowledge. Most importantly, work hard, do not get discouraged and stay patient; remember that research is more than often a long and hard endeavor that always brings results if you believe in your work. Always keep in mind the high ethical requirements in research: honesty and fairness.

What are the top books that you recommend reading to get started in the field of Lab Astro?

There are a large number of publications that have been published in the past two or three decades that have witnessed the evolution of the field of Laboratory Astrophysics. Some examples include proceedings from Laboratory Astrophysics workshops and confe- rences.

A non-exhaustive list of books is provided below:

● Proceedings of Laboratory Astrophysics

workshops and conferences:

● NASA LAW books (1990, 1998, 2002, 2006, etc.); ● ECLA 2020;

● IAU Proceedings (IAU 371, IAU 350, IAU 280); ● Molecular Spectroscopy in Astrophysics,

Spectrochimica Acta, Part A: Molecular and Biomolecular Spectroscopy, Elsevier, Vol. 57, 613– 958 (2001).

How do you balance your professional and personal life?

I strongly believe that

I have always tried to balance my professional and life as well as I could. It is not always an personal easy thing to do but is essential to have a balanced life. Outside of work I spend most, if not all, my time with my family (and my dog). I very much enjoy walking or hiking with my family and my friends. I also spend time reading and/or watching movies or listening to music. I also enjoy traveling, and discovering and exploring new places for the first time.

Farid’s family: Amira, Farid, Josie, Maissa, and Milou.

Section header image credits: NASA, ESA, Hubble Heritage

Laboratory Astrophysics Facilities:

The Cold Solar System Objects ISFM Project Facilities

In this first issue of the Laboratory Astrophysics Newsletter, we will present the 5 laboratory facilities that are used to carry out the experimental work of the Cold Solar System Objects (CSSO) Internal Scientist Funding Model (ISFM) project. These 5 laboratory facilities are: the Ices, Ice Irradiation, and Organics Laboratory for Astrobiology (I3OLAB), the Optical Constants Facility (OCF), and the Matrix Isolation/Optical Constants of Ices (MIOCI) at NASA Ames Research Center, as well as the Cosmic Ice Laboratory at NASA Goddard Space Flight Center.

the COsmic SImulation Chamber (COSmIC),

I3OLAB Facility at NASA Ames Michel Nuevo (michel.nuevo@nasa.gov), Scott Sandford https://www.nasa.gov/ices-ice-irradiation-and-organics-laboratory-for-astrobiology/ https://www.astrochem.org/fac/ice_lab.php

COSmIC at NASA Ames Farid Salama (farid.salama@nasa.gov), Ella Sciamma-O’Brien, Salma Bejaoui, David Dubois, Lora Jovanovic, Claire Ricketts https://www.nasa.gov/cosmic-facility/

Optical Constants Facility at NASA Ames Ella Sciamma-O’Brien (ella.m.sciammaobrien@nasa.gov), Farid Salama, Claire Ricketts, Lora Jovanovic, Diane Wooden https://www.nasa.gov/space-science-and-astrobiology-at-ames/research-teams/all-research-teams/optical-constant-facility/

Matrix Isolation/Optical Constants of Ices at NASA Ames Joseph Roser (joseph.e.roser@nasa.gov), Lora Jovanovic, Diane Wooden, Claire Ricketts https://www.nasa.gov/space-science-and-astrobiology-at-ames/research-teams/all-research-teams/matrix-isolation-optical- constants-of-ices-laboratory/

Cosmic Ice Laboratory at NASA Goddard Christopher Materese (christopher.k.materese@nasa.gov), Reggie Hudson, Perry Gerakines, Patrick Tribbett, Yukiko Yarnall https://science.gsfc.nasa.gov/691/cosmicice/

Identify, characterize, and study the evolution of ices in astrophysical environments

ice analogs simu- Various astrophysically relevant lating interstellar dense molecular clouds, protostellar disks (PPDs), and outer Solar System objects are simulated in cryo-vacuum systems, charactered with infrared (IR) spectroscopy, and compared to mission data for the detection of specific compounds and families of compounds, e.g., astronomical data obtained by NASA, ESA, and JAXA missions and IR observatories (Spitzer, JWST, ISO, SOFIA, IRTF).

Study chemical processes occurring when ices and organics are exposed to ionizing radiation and subsequent formation of complex organic materials

Astrophysically relevant ices are irradiated with ultra- violet (UV) photons or energetic electrons and monitored with IR spectroscopy to study their chemical evolution and the formation of new species upon irradiation, with an emphasis on investigation of astro-biologically relevant compounds, such as amino acids, sugar derivatives, nucleobases, and amphi- philes. The organics residues resulting from the warm-up of the ices to room temperature are also analyzed to determine their molecular and elemental compositions using IR spectroscopy, gas chromato- graphy coupled to mass spectrometry (GC-MS), and X-ray absorption near-edge structure (XANES) spec- troscopy.

Study chemical processes when organic residues are exposed to further ionizing radiation, and subsequent formation of insoluble materials that resemble insoluble organic matter in extraterrestrial materials

Ice-covered dust grains and more complex organics are believed to experience high doses of ionizing radiation in PPDs, resulting in the formation of a very refractory, insoluble material whose composition resembles that of insoluble organic matter (IOM) in meteorites, interplanetary dust particles (IDPs), and asteroid materials from Ryugu (Hayabusa2) and Bennu (OSIRIS-REx).

Exposing organic residues to additional high-energy radiation results in changes in their chemical and elemental compositions, which can be studied as a function of the radiation dose.

Study extraterrestrial materials from comets and asteroids and support sample return missions

I3OLAB also characterizes organics in extraterrestrial samples (meteorites, their chemical and elemental compositions to understand the processes and conditions in which those materials formed and evolved.

IDPs, asteroids)

for

Laboratory equipment

Cryovacuum systems. The I3OLAB facility has cryo- vacuum systems (see photo above) that typically operate in the 10-8 torr range and are equipped with closed-cycle He cryocoolers to perform experiments below 20 K. Ices are made by depositing pre-mixed gases onto a cold substrate (aluminum foil or IR- transparent window) and are simultaneously irra- diated with UV photons from a microwave-powered H2 lamp or 1.2-keV electrons from an electron gun. UV lamps emit primarily Lyman-α photons (121.6 nm) in addition to a continuum centered at 160 nm, with a flux of about 1014 photons cm–2 s–1. Photon total doses

doses in those experiments are equivalent to about 105 years in the diffuse interstellar medium (ISM) and 108 years in the dense ISM.

FTIR spectroscopy. One of the cryovacuum systems is equipped with a Thermo Fisher iS50 Fourier- transform infrared (FTIR) spectrometer. Samples are deposited on an IR-transparent window, allowing for real-time collection of transmission IR spectra during ice deposition, irradiation, and thermal cycling. The spectrometer can measure spectra in the near-IR (NIR; 10000–4000 cm−1) and mid-IR (MIR; 5000–600 cm−1) ranges with a spectral resolution ≥0.09 cm−1, using different beamsplitters and a liquid nitrogen (MCT) (LN2)-cooled mercury–cadmium–telluride detector.

FTIR microscopy. A Thermo Fisher Nicolet iN10 MX FTIR microscope is used to analyze a wide variety of samples, including organic residues produced from the UV irradiation of astrophysical ice analogs and extraterrestrial samples including meteorites (e.g., Sutter’s Mill) and samples from asteroids Ryugu and Bennu, with a ≥5-μm spatial resolution down to and a ≥4-cm-1 spectral resolution by collecting transmission or reflection spectra in the MIR (4000‒675 cm–1) and thanks to an LN2- NIR (7000‒4000 cm–1) ranges, cooled MCT detector and a KBr beamsplitter.

GC-MS. The gas chromatography coupled to mass spectrometry (GC-MS) device at I3OLAB combines a Thermo Trace gas chromatograph with a Thermo DSQ II mass spectrometer, which can record mass spectra in the 50–650 Da mass range. Using a variety of GC columns (Rxi-5ms, Rtx-200MS, DB-17HT, etc.), derivatization techniques (BSTFA, MTBSTFA, etc.), and temperature gradients, GC-MS separates organic components of complex mixtures from samples produced in the laboratory or extraterrestrial materials. Compound identification is made by comparison of retention times and mass spectra of GC peaks in samples with commercial standards prepared in the same manner as the samples. In the absence of relevant standards, mass fragmentation spectra can provide constraints on the structure of unidentified compounds. GC-MS analysis of residues produced from the UV irradiation of ices of astrophysical interest have shown that astrobio- logically relevant molecules such as amino acids, nucleobases, and sugar derivatives (see figure) can be made under abiotic conditions.

Gas handling system. Ice samples are condensed from pre-mixed gas mixtures whose compositions ISM clouds, simulate various environments (e.g.,

GC-MS data showing the detection of 2-deoxyribose in a residue produced from the UV irradiation of an H2O:CH3OH ice mixture (from Nuevo et al. 2018).

PPDs, comets, icy satellites). Mixtures are made from gases (lecture bottles) and vapors (from liquids) of simple molecules (e.g., H2O, CH3OH, CO, CO2, NH3, CH4, N2) which are prepared in a gas handling system that operates with a background pressure of about 10–6 mbar. The composition of each mixture is determined by the partial pressures of individual components. The resulting mixtures are transferred to glass bulbs that are then interfaced with the cryovacuum systems, and from which ices can be deposited on cold substrates.

COSmIC at NASA Ames Farid Salama (farid.salama@nasa.gov), Ella Sciamma-O’Brien, Salma Bejaoui, David Dubois, Lora Jovanovic, Claire Ricketts https://www.nasa.gov/cosmic-facility/

Overview

COSmIC stands for “Cosmic Simulation Chamber” and was developed to generate, process and analyze interstellar, circumstellar, and (exo)planetary analogs in the laboratory. COSmIC is used to study neutral and ionized molecules and nanoparticles and grains under temperature and vacuum conditions that are representative of space environments.

Laboratory equipment

COSmIC, depicted below, consists of a pulsed discharge nozzle (PDN) mounted on a vacuum chamber and coupled to a cavity ringdown spectro- meter (CRDS) and a quadrupole mass spectrometer (QMS). An RF/DC Plasma Static Langmuir Probe can also be connected to the chamber.

Pictures of the COSmIC facility. Left inserts: the PDN slit and images of an argon-based (blue) and a nitrogen-based (pink) plasma. Left: the CRDS system coupled to the COSmIC chamber. Right: The QMS coupled to COSmIC.

The PDN is used to generate a free supersonic expansion by injecting a gas mixture into the vacuum chamber through a very thin slit (127 µm ´ 10 cm). A reservoir with heating plates (up to 300°C) allows to mix precursors into a carrier gas before expansion through the slit. The expansion lowers the gas temperature (50–150 K) and the pressure (0.1–30 mbar). A cold plasma discharge (1–2 eV energy) can the expansion by be generated in the stream of applying a high voltage (600–1000 V) onto elec- trodes placed along the slit (see schematic). This plasma discharge then generates cold isolated neutral, ions, radicals in the gas phase, as well as solid particles in a setting that realistically simulates astrophysical and (exo)planetary environments.

(a) Schematic of the pulse discharge nozzle (PDN). (b) Gas temperature before the plasma is turned on. (c) Gas temperature after the plasma is turned on.

Cavity Ringdown Spectroscopy (CRDS) is an ultra- sensitive direct absorption technique based on the measurement of the lifetime of probe photons trapped into an optical cavity formed by two high reflectivity (>99.99%) mirrors facing each other. On COSmIC, a laser and several sets of mirrors allow measuring the absorption spectra of neutral and ionized molecules (with and without plasma) in the ultraviolet to near infrared spectral range from 300 to 900 nm. An IR CRDS system (2.7–4.0 under development. These measured absorption spectra can then be directly compared to observational data for their interpretation.

also

µm)

Mass spectrometry is another in situ, non-intrusive technique that allows monitoring the neutral and ionized species produced in the plasma expansion on COSmIC. The first mass spectrometer installed on COSmIC was a time-of-flight mass spectrometer that enabled studying the chemical pathways leading to the formation of heavier molecular species precursors of solid particles analogs of cosmic dust grains and planetary aerosols. Recently a new quadrupole mass spectrometer was installed on COSmIC that will enable not only the detection of positive ions and neutrals in the plasma expansion but also negative ions. A Langmuir probe can also be coupled to the COSmIC chamber to characterize the plasma parameters (e.g., pressure, temperature).

Simulating Interstellar Environments (gas phase)

and

CRDS can be used on COSmIC to measure the absorption spectra in the NUV-NIR range of ionized PAHs nitrogen-contained PAH molecules (PANHs) isolated in a cold free jet expansion of argon (Ar) carrier gas. These high-resolution experimental spectra can then be compared to the observations and the upper limits for the column densities of the PAHs and PANHs molecular carrier can be derived. A first quantitative survey of neutral and ionized PAHs in the optical range, and in particular a comparison of CRDS experimental absorption spectra of pentacene to ISO interstellar observations opened the way for unambiguous quantitative searches of PAHs in a variety of interstellar and circumstellar environments.

Experimental gas-phase CRDS absorption spectrum of phenanthrene compared to solid matrix isolation spectroscopy spectrum demonstrating the high- resolution capability of the CRDS technique (from Bejaoui & Salama 2019).

Simulating Circumstellar Environments (gas and solid phases)

In COSmIC, simple hydrocarbons (e.g., CH4, C2H2) and PAHs seeded in Ar gas can be used as precursors to study grain formation in the gas phase. The plasma chemistry induced in the PDN produces more complex molecular species, that can then be directly detected in situ by mass spectrometry, and that can be collected on solid phase materials, substrates and analyzed ex situ, with high-resolution mass spectrometry, scanning electron microscopy, and spectrally with the Optical Constants Facility (OCF).

High-resolution laser desorption mass spectra of grains formed by plasma chemistry from aromatic precursors seeded in Ar gas (Gavilan et al. 2020).

Simulating (Exo)Planetary Environments (gas and solid phases)

The COSmIC facility can also be used to simulate the chemistry occurring in the upper layers of planetary (e.g., Titan, Pluto, Triton, Jupiter) and exoplanetary atmospheres. Different gas mixtures (e.g., N2:CH4, N2:CH4:C2H2, N2:CH4:C6H6, N2:CH4:CO, Ar:NH3:CH4, Ar:NH3:C2H2, Ar:CH4:CO, Ar:CH4:CO2) be in order to investigate the injected in the plasma, chemical pathways leading to the formation of aerosols, via in situ mass spectrometry, and produce aerosol analogs for further ex situ analysis (Scanning electron microscopy, X-ray absorption spectroscopy, high resolution mass spectrometry, optical properties with OCF.

can

Left: Time-of-flight mass spectra of Titan-simulated N2:CH4-based atmosphere with and without the addition of heavier gas-phase precursors (C2H2, C6H6). Right: Scanning electron microscope images of the resulting solid grains (from Sciamma-O’Brien et al. 2015).

Overview

The NASA Ames Optical Constants Facility (OCF) was recently developed to characterize the spectral properties of non-homogeneous refractory solid samples, using transmission and reflection measure- ments, and determine their optical constants, from the near ultraviolet (NUV) to far infrared (FIR).

Optical constants are the real and imaginary parts of the complex refractive index, respectively n and k, of a material: N = n + ik. They describe how a material interacts with incident including transmission, light, reflection, refraction, absorption, and scattering. Both real and imaginary indices vary with wavelength.

Optical constants are fundamental input parameters for models (e.g., radiative transfer, atmospheric, and reflectance spectral models) used to interpret observational data returned from space missions and ground-based observatories. They support strategic research activities recommended by the "Origins, Worlds and Life" Planetary Science and Astrobiology Decadal Survey 2023–2032.

thus

Laboratory equipment

The OCF is composed of a Filmetrics-KLA F40-UVX reflectance microscope, a Thermo Fisher iS50 Fourier-transform Infrared (FTIR) spectrometer, and two Harrick Scientific variable angle transmission (VATA) and reflection (SEAGULL) accessories.

The reflectance microscope allows characterization of the optical properties of samples deposited on single- polished silicon (Si) substrates from 200 nm to 1.7 µm. This instrument is equipped with a ´10 objective, and different apertures (50, 100, 250, and 500 µm) that allow conducting measurements on spots as small as 5 µm diameter, hence enabling the characterization of spectral properties of both homo- geneous and inhomogeneous samples.

The Fourier-Transform InfraRed (FTIR) spectrometer allows characterization of the spectral properties of samples deposited on different types of substrates (e.g., magnesium fluoride MgF2, cesium iodide CsI, potassium bromide KBr, double-polished silicon, Si) from 0.6 to 200 µm (17,000–50 cm–1). This wide wavelength range is made possible by the availability (visible, Vis), TEC- of InGaAs (near (mid- infrared, MIR), DLaTGS-Polyethylene (far infrared, FIR)] and four different beamsplitters [Quartz (Vis), CaF2 (NIR), KBr (MIR), Solid Substrate (FIR)]. An automated exchanger allows full spectral coverage without breaking purge. The spectra can be measured with a resolution as low as 0.5 cm-1 .

infrared, NIR), DLaTGS-KBr

four different detectors [Si

The Variable Angle Transmission Accessory (VATA) and the SEAGULL variable angle reflectance acces- sory can be coupled to the FTIR spectrometer. They allow the characterization of the optical properties of solid samples, over a broad range of incidence and emittance angles, the VATA accessory, and from 5° to 85° for the SEAGULL accessory. The VATA and SEAGULL accessories enable the characterization of light distribution in both transmission and reflection measurements.

from 0° to 90° for

the angular

Optical constant determination

using

codes

the Cauchy

equation, Inversion Swanepoel method, and subtractive Kramers–Kronig relations have been developed to determine the thickness and both n and k indices by fitting inter- ference fringes observed in spectral measurements.

By combining optical constants determined from reflection measurements in the NUV-NIR range and from transmission measurements in the Vis-FIR the OCF provides refractive indices of range, refractory solid samples over a wide wavelength range. Below are examples of optical constants of analogs produced with the COSmIC and determined with OCF:

Optical constants n and k determined for aerosol analogs produced by plasma chemistry in Ar:CH4, N2:CH4, and N2:CH4:C2H2 gas mixtures (adapted from Sciamma-O’Brien et al. 2023). This comparison in the solid shows that higher nitrogen content samples (from elemental composition determined by Nuevo et al. 2022) results in higher n and k.

Example of Planetary Application: Titan

The optical constants of COSmIC N2:CH4 aerosol analogs shown above were used in a radiative transfer model to interpret Cassini VIMS (Visible and Infrared Mapping Spectrometer) observations of Titan (T-79 flyby).

Radiance factor observed with VIMS between 0.4 and 1.6 µm during the T-79 flyby (in red) compared to best fits calculated with optical constants determined for Titan aerosol analogs produced with the COSmIC facility, considering different surface albedos As (adapted from Sciamma-O’Brien et al. 2023).

The analysis of Cassini VIMS observations showed that aerosol analogs, which contain more nitrogen and are more absorbing, have a spectral behavior that is more representative of Titan’s aerosols.

Optical Constants database (OCdb)

The NASA Ames Optical Constants database (OCdb) was launched in January 2023. It is a data repository developed to provide published, peer-reviewed optical constants of organic refractory materials and ices relevant to (exo)planetary and astrophysical envi- ronments.

The goal of OCdb is to centralize published optical constants data to facilitate both their access by the scientific community and the analysis and inter- pretation of observational data returned by ground- and space-based telescopes and space missions. are Laboratories encouraged to contribute their data in order to increase their visibility and availability.

generating

constants

optical

For now, the Optical Constants database provides data sets for ice samples (pure and mixtures), and organic refractory materials produced from irra- diation of ice samples (also called “ice tholins” or “ice residues”) or gas precursors (also called “gas tholins”). We plan to expand the types of materials in the future.

Isolation/Optical Constants of

Ices The Matrix (MIOCI) vacuum system supports infrared trans- mittance spectroscopy of ices with vacuum deposition in a high vacuum (10–8 torr) environment and at deposition temperatures as low as 5 K.

The original MIOCI vacuum system was designed to investigate carbonaceous molecules that may be present in the interstellar medium, and in particular, the class of molecules known as polycyclic aromatic hydrocarbons or PAHs. These molecules have long in the interstellar been theorized to be present medium as the emitters of well-known infrared emission bands interstellar environments. With the MIOCI system, the infrared absorption spectra of isolated PAH molecules can be measured by co-depositing the PAH species of interest with argon ice. The argon matrix (thus "matrix isolation spectroscopy") serves as a relatively non- perturbing medium for producing a solid-state infrared transmittance measurement that resembles a gas- phase measurement.

seen in numerous

If the PAH molecules are not completely isolated from one another within the argon matrix, their mutual interactions could appear in the transmission spectra. It was also observed that the probability of two PAH molecules being embedded within the argon matrix should increase as the PAH/argon ratio increases. This led to a series of publications investigating small molecular (or "clusters") in the infrared by repeating the matrix isolation experiments as a function of PAH/argon ratio and identifying changes in the spectra as the PAH/argon ratio increases.

of PAH molecules

aggregates

The transmission spectra measured by MIOCI can also be used to calculate the complex index of refraction (also known as "optical constants") of cryogenic ices in the mid-infrared. The Kramers– Kronig relation provides a relation linking the real and imaginary parts of the complex index of refraction that allows both quantities to be determined using transmission measurements. This led to a publication describing the complex index of refraction of ammonia ice deposited at 40 K, a temperature representative of the temperatures of icy outer Solar System bodies such as Pluto.

Surface ammonia ice detections on these bodies are particularly interesting since the ammonia ice could be rapidly destroyed by radiation exposure. Surface ammonia ice can therefore be indicative of cryo- volcanism occurring within these outer Solar System bodies.

The MIOCI system is nearing completion of a system redesign that added a new capability for molecular beam deposition to the experiments that can be performed. In this new system, a microwave discharge source will produce a beam of molecular fragments — for example, hydrogen atoms from dissociation of molecular hydrogen — that can be co- deposited along with other ices onto the cryogenic substrate window. This will allow low-energy chemical reactions of the deposited ices to be studied without the need for energetic processing to drive the experiments.

Overview

For over 40 years, the Cosmic Ice Laboratory at NASA Goddard Space Flight Center has researched icy Solar System and interstellar environments. Our laboratory specializes in molecular spectroscopy, obtaining fundamental physical properties of ices, low temperature chemistry, radiation chemistry, and reaction kinetics. Our work has a wide range of applications from astronomy to astrobiology. This includes identifying and quantifying infrared bands in observational data, making predictions about the chemical composition of Solar System and interstellar ices, interpreting the origins of molecules detected in extraterrestrial samples, and determining the lifetimes of molecules in an extraterrestrial environment. Our data benefit all phases of NASA missions from planning to final analysis by providing fundamental data about what might be detected, how long it might last, how much of it there is, and what its presence could imply about the environment.

Research topics

spectra

infrared

to measure

Molecular spectroscopy: We use laboratory expe- riments of the compounds that are known or predicted to exist in icy Solar System and interstellar environments. These measurements can then be used to identify specific molecules or classes of molecules in spectra obtained from samples, missions, and ground and space telescopes. Our laboratory spectral data also provide information about the ices (e.g., amorphous or crystalline). We also specialize in obtaining optical constants of ices which can be used to quantify the abundance of specific compounds in target objects of interest. The data we generate are critical for the interpretation of observations.

the structure of

Fundamental physical properties of ices: We use experiments to measure the fundamental physical ices including their densities, indices of properties of vapor pressures, and enthalpies of refraction, vaporization, among other things. These important fundamental properties are important to predict the behavior of molecules in icy environments and are often essential to fully quantify their abundance and chemical reactivities.

Radiation Chemistry: We use a combination of infrared spectroscopy and p+ radiolysis to simulate a range of Solar System and interstellar radiation environments and monitor chemical changes in sample ices in situ. These experiments allow us to track the radiolytic destruction of reactant compounds and the formation of new products as a function of radiation dose. These measurements are quantitative and can be applied to the interpretation of different space environments. The destruction and formation kinetics of reactants and products allow us to make predictions about their relative abundances, and expected lifetimes in different icy environments. These experiments also help interpret the origins of compounds detected in extraterrestrial samples.

the presence of molecules,

form within an ice at

Low temperature chemistry: We perform low tempe- rature thermochemistry experiments to observe the reactivities of compounds in the solid phase. These experiments involve reactive species that can be low collected together or temperatures and become able to react as the ice is warmed. Such experiments include solid phase acid– base reactions and oxidation–reduction reactions. These reactions are especially relevant to icy objects that undergo seasonal or periodic temperature changes. Additionally, of importance to sample return missions significant where the sample undergoes significant temperature changes between collection and analysis.

reactions

these

are

Laboratory Equipment

Van de Graaff Accelerator (above): This accelerator is located at NASA Goddard's Radiation Facility. It has been used by our lab since the 1980s and has played a role in ~75% of our papers. It delivers ~0.9-MeV protons with an incident flux sufficient to provide a 200 MGy (20000 Mrad) dose to ice samples over 1–2 days, with pauses to record IR spectra. To determine doses, we measure the beam current on the ice's underlying metal substrate, biased at +50 V to prevent the emission of secondary electrons. We can vary the incident flux by an order of magnitude or more to check for non-linear effects. The doses available are sufficient to replicate radiation chemistry for many astronomical environments.

Cryovacuum systems coupled with integrated FTIR spectrometers: Four cryovacuum systems (~10 to 300 K temperature range, ~10–8 torr operating pressure) are dedicated to the IR spectroscopy of ices. Each system has a dedicated manifold with calibrated leak valves allowing us to control the deposition rate and create ice mixtures without premixing gases. Two of the chambers are interfaced with the Van de Graaff accelerator for our ice radiolysis studies.

The cold end of each cryostat is interfaced with a multi-port sample chamber so that IR measurements can be made in situ during thermal annealing, and before and after irradiations of ices. Infrared spectra can be collected either in transmission (KBr, ZnSe reflection (polished windows as a substrate) or aluminum mirror substrate) and diode lasers (670 nm) are used for interferometry to measure sample thicknesses. If desired, samples can be collected after warming for ex situ analyses such as GC-MS or LC-MS or for use in aqueous chemistry experiments.

Ultra-high vacuum system: This cryovacuum system torr (~10 to 300 K temperature range, ~10–10 operating pressure) is equipped with a quartz-crystal microbalance, a two-laser interferometer, a quadru- pole mass spectrometer and is interfaced to an IR spectrometer. This system is primarily used to measure physical properties of ices including indices of refraction and densities.

Recent Sources of Funding: NASA’s Solar System Workings Program, NASA’s Emerging Worlds Program, NASA’s Astrophysics Research and Analysis Program, FLaRe ISFM, NASA Astrobiology Institute.

Recent Publications From the Laboratory Astrophysics Community January–November 2025

Optical diagnostics applications to laboratory astrophysical research Sun, W., Yuan, D., Zhang, Z., et al. Lights, 1, 3 (2025) https://doi.org/10.3390/lights1010003

Nature of adsorption of amino acids and precursors on interstellar amorphous solid water Watanabe, N., Hori, Y., Okazawa, K., et al. Monthly Notices of the Royal Astronomical Society, 544, 3173 (2025) https://doi.org/10.1093/mnras/staf1913

Thermochemical and kinetic investigation of CH3NH2 production in Titan’s atmosphere Mayr, G. L., Vieira, I. S., Spada, R. F. K. ACS Omega, 10, 56597 (2025) https://doi.org/10.1021/acsomega.5c09060

Microstructure controls sublimation timescales of exposed salt-rich ices on icy worlds Chinnery, H. E., Fox-Powell, M. G. Journal of Geophysical Research: Planets, 130, e2025JE009236 (2025) https://doi.org/10.1029/2025JE009236

Spectroscopic investigation of insoluble organic matter in aubrites and enstatite chondrites Neha, Natrajan, S., Marhas, K. K. Journal of Geophysical Research: Planets, 130, e2025JE009101 (2025) https://doi.org/10.1029/2025JE009101

Sample preparation for MALDI-TOF mass spectrometry of model prebiotic reactions in simulated ocean world environments Dzurilla, K. A., Herndon, E. C., Barge, L. M., Forsythe, J. G. ACS Omega, 10, 51709 (2025) https://doi.org/10.1021/acsomega.5c07633

Interstellar formation of 1,2-propanediol (CH3CH(OH)CH2OH) and 1,2-ethenediol (HOCHCHOH) — Key precursors to sugars and sugar derivatives Wang, J., Zhang, C., Eckhardt, A. K., Kaiser, R. I. Chemical Science, 16, 21111 (2025) https://doi.org/10.1039/D5SC05315C

Formation of polyoxymethylenes in extraterrestrial ice analogs of formaldehyde exposed to ionizing radiation Gong, Q., Bai, X., Lu, J., et al. The Astrophysical Journal, 994, 70 (2025) https://doi.org/10.3847/1538-4357/ae0cb7

Cryogenic infrared action spectroscopy of [H2NCO]+ and [H2NCS]+, protonated forms of interstellar HNCO and HNCS Gerlach, M., Schneider, N. R., Petrić, S., et al. The Journal of Physical Chemistry A, 129, 10339 (2025) https://doi.org/10.1021/acs.jpca.5c04708

Multiscale perspectives on solid-phase astrochemistry: Laboratory, computation, and open questions Dickers, M. D., Mifsud, D. V., Mason, N. J., Fantuzzi, F. Space Science Reviews, 221, 106 (2025) https://doi.org/10.1007/s11214-025-01228-9

Bennu and Ryugu constituents from samples IR analyses and potential source of terrestrial planets’ ingredients Pilorget, C., Okada, T., Bibring, J.-P., et al. Nature Communications, 16, 9532 (2025) https://doi.org/10.1038/s41467-025-65438-z

Cosmic ray interactions with indene and adamantane seeded water ice mantles Abdo, E., Dartois, E., Chabot, M., et al. Astronomy & Astrophysics, 703, A246 (2025) https://doi.org/10.1051/0004-6361/202556030

Detection of organic compounds in freshly ejected ice grains from Enceladus’s ocean Khawaja, N., Postberg, F., O’Sullivan, T. R., et al. Nature Astronomy, 9, 1662 (2025) https://doi.org/10.1038/s41550-025-02655-y

Interstellar formation of the elusive phosphanyloxyphosphane (H2POPH2) and phosphanylphosphinous acid (H2PPHOH) via nonequilibrium chemistry: Precursors to the phosphate backbone of nucleotides Wang, J., Sun, B.-J., Bergantini, A., et al. Journal of the American Chemical Society, 147, 38987 (2025) https://doi.org/10.1021/jacs.5c12481

Characterization of the chemical evolution of CH4 ices under processing by cosmic ray analogues with the procoda code – I. Effective reaction rate coefficients and chemical equilibrium phase Gerasimenko, S., Carvalho, G. A., Zanatto, F., et al. Monthly Notices of the Royal Astronomical Society, 544, 855 (2025) https://doi.org/10.1093/mnras/staf1738

The formation of organic macromolecular matter from the electron irradiation of simple carbon-containing ices Kipfer, K. A., Ligterink, N. F. W., Riebe, M. E. I., et al. Astronomy & Astrophysics, 702, A123 (2025) https://doi.org/10.1051/0004-6361/202555840

Modeling low-temperature plasmas simulating Titan’s atmosphere Dubois, D., Raymond, A. W., Sciamma-O’Brien, E., Salama, F. Planetary Science Journal, 6, 241 (2025) https://doi.org/10.3847/PSJ/ae0296

Differential partitioning behavior of chondritic organics in Enceladus analog ices Vu, T. H., Phillips-Lander, C. M., Czaplinski, E. C., et al. ACS Earth and Space Chemistry, 9, 2354 (2025) https://doi.org/10.1021/acsearthspacechem.5c00041

Laboratory study of amino acids on amorphous Mg-silicate using infrared spectroscopy and X-ray diffraction – Implications for the survival and delivery of interstellar organics to the solar nebula and early Earth Thompson, S. P., Day, S. J. Monthly Notices of the Royal Astronomical Society, 543, 951 (2025) https://doi.org/10.1093/mnras/staf1457

Molecular mobility of extraterrestrial ices: surface diffusion in astrochemistry and planetary science Ligterink, N. F. W., Walsh, C., Cuppen, H. M., et al. Physical Chemistry Chemical Physics, 27, 19630 (2025) https://doi.org/10.1039/D5CP02278A

Amides from the carbonaceous asteroid (162173) Ryugu: Nanoscale spectral and isotopic characterizations Vacher, L. G., Phan, V. T. H., Bonal, L., et al. Meteoritics & Planetary Science, 60, 2033 (2025) https://doi.org/10.1111/maps.70019

Formation of thiocarbonic acid (H2CS3) – the sulfur counterpart of carbonic acid (H2CO3) – in interstellar analog ices Coulaud, L., Wang, J., Herath, A., et al. Physical Chemistry Chemical Physics, 27, 19324 (2025) https://doi.org/10.1039/D5CP02478A

Photo-chemical processing of CH4:O2 ices Ge, Y., Zhang, C., Zhen, J., Wang, Y. Monthly Notices of the Royal Astronomical Society, 542, 2363 (2025) https://doi.org/10.1093/mnras/staf1383

Formation of hydrogen trioxide (HOOOH) in extraterrestrial ice analogs and its role as an oxidizer in prebiotic chemistry Bai, X., Li, C., Luo, Y., et al. Science Advances, 11, eadw5720 (2025) https://doi.org/10.1126/sciadv.adw5720

X-ray induced photochemistry of hydrocarbons: Implications for the formation of organic haze in (exo)planetary atmospheres Bejaoui, S., Dubois, D., Nemsak, S., Salama, F. The Planetary Science Journal, 6, 203 (2025) https://doi.org/10.3847/PSJ/adf4d3

Gas and aqueous phase computations on the keto-enol tautomerization of pyruvic and zymonic acids: Implications for prebiotic enol phosphates Bera, P. P., Wilson, M., Pohorille, A., et al. The Journal of Physical Chemistry A, 129, 7287 (2025) https://doi.org/10.1021/acs.jpca.5c01351

Oxygen isotopic heterogeneities in refractory inclusions in the ungrouped carbonaceous chondrite Acfer 094 Fagan, T. J., Kobayashi, S., Krot, A. N., Yurimoto, H. Meteoritics & Planetary Science, 60, 1734 (2025) https://doi.org/10.1111/maps.70003

Na,Ca carbonates in OSIRIS-REx samples: Evidence for low-temperature, Na-bearing brines on Bennu’s parent body Singerling, S.A., Brenker, F.E., Tkalcec, B., et al. Geochimica et Cosmochimica Acta, 404, 86 (2025) https://doi.org/10.1016/j.gca.2025.06.028

Laboratory infrared spectra and band strengths of carbonyl sulfide (OCS) in CH3OH- and CO-rich ice mixtures for analyzing interstellar ice observations Slavicinska, K., Coone, C., Benz, B., et al. ACS Earth and Space Chemistry, 9, 2148 (2025) https://doi.org/10.1021/acsearthspacechem.5c00134

Physicochemical properties of α-pinene in water ice analogs under energetic heavy-ion irradiation de Barros, A. L. F., Doreste, D. V., Ricca, A., et al. ACS Earth and Space Chemistry, 9, 2180 (2025) https://doi.org/10.1021/acsearthspacechem.5c00152

Formation of lactic acid (CH3CH(OH)COOH), a metabolic keystone for the molecular origins of life, in interstellar ice analogues Wang, J., Zhang, C., Bergantini, A., et al. Journal of the American Chemical Society, 147, 29088 (2025) https://doi.org/10.1021/jacs.5c07637

Photochemical haze formation on Titan and Uranus: A comparative review Dubois, D. International Journal of Molecular Sciences, 26, 7531 (2025) https://doi.org/10.3390/ijms26157531

Vacuum ultraviolet photoabsorption spectroscopy of space-related ices: Formation of (cyano)polyynes in 1 keV electron irradiated hydrocarbon-rich ices Kaňuchová, Z., Borchert, L. E., Mifsud, D. V., et al. Astronomy & Astrophysics, 700, A115 (2025) https://doi.org/10.1051/0004-6361/202554933

Water-group ion irradiation studies of Enceladus ice analogues: Can radiolysis account for material in and around the south polar plume? Richards, G., Richárd Rácz, R., Kovács, S. T. S., et al. Planetary and Space Science, 266, 106179 (2025) https://doi.org/10.1016/j.pss.2025.106179

Crystallization and isotopic exchange in water + ethylene glycol ices Hudson, R. L. Monthly Notices of the Royal Astronomical Society, 542, 96 (2025) https://doi.org/10.1093/mnras/staf1199

Photodesorption of SO2 and SO from UV-irradiated SO2 ices Martín-Doménech, R., Escribano, B., Navarro-Alamida, D., et al. Monthly Notices of the Royal Astronomical Society, 541, 2992 (2025) https://doi.org/10.1093/mnras/staf1126

Photochemistry of interstellar ice forming complex organic molecules Muñoz Caro, G. M., Carrascosa de Lucas, H., Martín-Doménech, R. Nature Reviews Chemistry, 9, 537 (2025) https://doi.org/10.1038/s41570-025-00729-z

Experimental constraints on the shock history of CI chondrites and Ryugu grains Nakahashi, T., Miyahara, M., Yamaguchi, A., et al. Earth and Planetary Science Letters, 668, 119559 (2025) https://doi.org/10.1016/j.epsl.2025.119559

Solar System’s earliest solids as tracers of the accretion region of Ryugu and Ivuna-type carbonaceous chondrites Kawasaki, N., Arakawa, S., Miyamoto, Y., et al. Communications Earth & Environment, 6, 537 (2025) https://doi.org/10.1038/s43247-025-02511-x

Cryogenic differential calorimetry: Exothermicity of amorphous-to-crystalline phase transitions (ACPT) in astrophysical and cometary ice analogs Kushwaha, R. K., Gudipati, M. S., Henderson, B. L. The Astrophysical Journal, 987, 190 (2025) https://doi.org/10.3847/1538-4357/addc68

Experimental and theoretical porosity determination for ices of astrophysical interest: CH4, C2H4, C2H6, CH3OH, N2, NH3, CO, and CO2 Millán, C., Luna, R., Domingo, M., et al. Icarus, 441, 116710 (2025) https://doi.org/10.1016/j.icarus.2025.116710

Gas-phase formation and photochemistry of large amino-containing PAH clusters. Wu, X., Wu, Y., Hua, L., et al. Monthly Notices of the Royal Astronomical Society, 541, 1241 (2025) https://doi.org/10.1093/mnras/staf1062

Co-evolution of organics and water in experimentally shocked Murchison and EET 90628 chondrites Quirico, E., Yabuta, H., Beck, P., et al. Geochimica et Cosmochimica Acta, 402, 316 (2025). https://doi.org/10.1016/j.gca.2025.05.046

Interstellar water ice analogue properties as a function of temperature: Updated density, porosity, and infrared band strength Escribano, B., del Burgo Olivares, C., Carrascosa, H., et al. Astronomy & Astrophysics, 699, A79 (2025) https://doi.org/10.1051/0004-6361/202555090

Missing interstellar sulfur in inventories of polysulfanes and molecular octasulfur crowns Herath, A., McAnally, M., Turner, A. M., et al. Nature Communications, 16, 5571 (2025) https://doi.org/10.1038/s41467-025-61259-2

Synthesis of new hexamethylenetetramine-based products (HMT-R) in UV-irradiated pre-cometary ice analogues del Burgo Olivares, C., Carrascosa, H., Muñoz Caro, G. M., et al. Astronomy & Astrophysics, 698, A285 (2025) https://doi.org/10.1051/0004-6361/202554613

H2S ice sublimation dynamics: Experimentally constrained binding energies, entrapment efficiencies, and snowlines Santos, J.C., Piacentino, E. L., Bergner, J. B., et al. Astronomy & Astrophysics, 698, A254 (2025) https://doi.org/10.1051/0004-6361/202554068

On the darkness of Ryugu and other dark small bodies Beck, P., Quirico, E., Poch, O., Schmitt, B. Nature Astronomy, 9, 793 (2025) https://doi.org/10.1038/s41550-025-02557-z

Spectroscopic study of ice analogs of trans-Neptunian objects exposed to ionizing radiation. II. Infrared spectra and functional groups Zhang, C., Wang, J., Turner, A. M., et al. The Astrophysical Journal Supplement Series, 279, 1 (2025) https://doi.org/10.3847/1538-4365/add144

Photolysis and sublimation chemistry of ammonium cyanide with relevance to cometary environments Wilkins, O. H., Yocum, K. M., Esposito, V. J., et al. The Planetary Science Journal, 6, 10 (2025) https://doi.org/10.3847/PSJ/ad9a67

Establishing an accurate infrared band strength for the cyanate ion in interstellar ices Gerakines, P. A., Materese, C. K., Hudson, R. L. Monthly Notices of the Royal Astronomical Society, 537, 2918 (2025) https://doi.org/10.1093/mnras/staf192

Exploring the formation and alteration of organics in ice: experimental insights for astrochemistry and space missions Hofmann, F., Asanova, N., Urso, R. G., Elsaesser, A. Earth, Planets and Space, 77, 70 (2025) https://doi.org/10.1186/s40623-025-02207-8

Cosmic-ray induced sputtering of interstellar formaldehyde ices Faure, M., Bacmann, A., Faure, A., et al. Astronomy & Astrophysics, 693, A30 (2025) https://doi.org/10.1051/0004-6361/202449937

Infrared spectroscopy of astrophysical ice analogues at oblique angles González Díaz, C., Carrascosa, H., Muñoz Caro, G. M. Monthly Notices of the Royal Astronomical Society, 538, 1906 (2025) https://doi.org/10.1093/mnras/staf338

Predicting the detectability of sulphur-bearing molecules in the solid phase with simulated spectra of JWST instruments Taillard, A., Martín-Doménech, R., Carrascosa, H., et al. Astronomy & Astrophysics, 694, A263 (2025) https://doi.org/10.1051/0004-6361/202452900

Characterization of amino acid nanolayers and their interactions under simulated planetary conditions Gonçalves, D., Hofmann, F., Drauschke, J., et al. ACS Earth and Space Chemistry, 9, 356 (2025) https://doi.org/10.1021/acsearthspacechem.4c00334

The photochemistry of amino acids produced on the polar cryovolcanic regions of Titan Gonçalves, D., Hofmann, F., Wipf, S., et al. ACS Earth and Space Chemistry, 9, 715 (2025) https://doi.org/10.1021/acsearthspacechem.4c00376

VIS-to-MIR reflectance and Raman spectroscopy of the CM2 NWA 12184 carbonaceous chondrite Galiano, A., Dirri, F., Ferrari, M., et al. Meteoritics & Planetary Science, 60, 570 (2025) https://doi.org/10.1111/maps.14315

Sample return missions: Rosetta Stones returned from the first small bodies in the Solar System Nakamura, T., Engrand, C., Zolensky, M., et al. Space Science Reviews, 221, 44 (2025) https://doi.org/10.1007/s11214-025-01168-4

Thermal desorption kinetics, binding energies, and entrapment of methyl mercaptan ices Narayanan, S., Piacentino, E. L., Öberg, K. I., Rajappan, M. The Astrophysical Journal, 986, 10 (2025) https://doi.org/10.3847/1538-4357/adc7b6

Characterization of H2O:N2 ice under bombardment by cosmic rays – I. Reaction rates and chemical equilibrium Queiroz, L. M. S. V., Silva, J. R. C., Ferrão, L. F. A., Pilling, S. Monthly Notices of the Royal Astronomical Society, 537, 3100 (2025) https://doi.org/10.1093/mnras/staf225

Light element isotopic heterogeneities in organic residues that formed by the ion irradiation of ices Rojas, J., Duprat, J., Dartois, E., et al. Astronomy & Astrophysics, 698, A34 (2025) https://doi.org/10.1051/0004-6361/202451601

Formation of ammonium nitrate particles in CO2-rich atmospheres Jiménez-Escobar, A., Ciaravella, A., Mangione, A., et al. The Planetary Science Journal, 6, 135 (2025) https://doi.org/10.3847/PSJ/add730

Photochemistry of benzene (C6H6) hydrogen cyanide (HCN) co-condensed ices part 2: Formation of aerosols analogues of Titan's atmosphere Couturier-Tamburelli, I., Danger, G., Mouzay, J., Piétri, N. Icarus, 438, 116626 (2025) https://doi.org/10.1016/j.icarus.2025.116626

Experimental investigations of mineral-organic chondritic analogs under hydrothermal conditions: Implications for carbonaceous asteroids Serra, C., Grauby, O., Ferry, D., et al. Geochimica et Cosmochimica Acta, 398, 29 (2025) https://doi.org/10.1016/j.gca.2025.04.018

Mid-infrared detection and characterization of refractory inclusions in CM and CO chondrites: A non-destructive approach for returned space samples Charlier, J., Aléon-Toppani, A., Brunetto, R., et al. Meteoritics & Planetary Science, 60, 544 (2025) https://doi.org/10.1111/maps.14314

Water in Ryugu as a property of processes in its parent body Le Pivert-Jolivet, T., Brunetto, R., Pilorget, C., et al. Astronomy & Astrophysics, 695, A168 (2025) https://doi.org/10.1051/0004-6361/202453270

Methylene-to-methyl ratio variability in Ryugu samples: Clues to a heterogeneous aqueous alteration Dionnet, Z., Djouadi, Z., Delaye, L., et al. Meteoritics & Planetary Science, 60, 273 (2025) https://doi.org/10.1111/maps.14304

Irradiation origin and stability of CO on trans-Neptunian objects: Laboratory constraints and observational evidence from JWST/DiSCo-TNOs Hénault, E., Brunetto, R., Pinilla-Alonso, N., et al. Astronomy & Astrophysics, 694, A126 (2025) https://10.1051/0004-6361/202452321

Molecular evolution of H2O:O2 ices at different temperatures in simulated space environments. I. Chemical kinetics and equilibrium Silva, J. R. C., Queiroz, L. M. S. V., Ferrão, L. F. A., Pilling, S. The Astrophysical Journal, 985 (2), 254 (2025) https://doi.org/10.3847/1538-4357/adc924

Tholin formation and accumulation due to hypersonic high-temperature flows in methane-containing atmospheres Lappa, M., Esposito, A., Russo, C., Apicella, B. Icarus, 439, 116649 (2025) https://doi.org/10.1016/j.icarus.2025.116649

Elemental and isotopic signatures of asteroid Ryugu support three early Solar System reservoirs Shollenberger, Q. R., Render, J., Wimpenny, J., et al. Earth and Planetary Science Letters, 664, 119443 (2025) https://doi.org/10.1016/j.epsl.2025.119443

Challenges and opportunities in using amino acids to decode carbonaceous chondrite and asteroid parent body processes Aponte, J. C., McLain, H. L., Saeedi, D., et al. Astrobiology, 25, 437 (2025) https://doi.org/10.1089/ast.2025.0017

Measurement of photochemical haze refractive indices and hygroscopicity: Influence of CO2 in CH4/H2S/N2 mixtures Jansen, K. T., Reed, N. W., Browne, E. C., Tolbert, M. A. Astrobiology, 25, 395 (2025) https://doi.org/10.1089/ast.2024.0142

Abundant ammonia and nitrogen-rich organic matter in samples from the B-type carbonaceous asteroid Bennu Glavin, D. P., Dworkin, J. P., Alexander, C. M. O’D., et al. Nature Astronomy, 9, 199 (2025) https://doi.org/10.1038/s41550-024-02472-9

Section header image credits: NASA, ESA, CSA, STScI, J. Jencson (Caltech/IPAC)

Community Announcements Upcoming Conferences, Meetings, and Workshops Relevant to Laboratory Astrophysics

American Geophysical Union Fall meeting (AGU25) 15‒19 December 2025 New Orleans, LA, USA https://www.agu.org/annual-meeting Abstract submission deadline: Closed Registration deadline: 15 December 2025

Pacifichem 2025 15‒20 December 2025 Honolulu, HI, USA https://pacifichem.org/ Abstract submission deadline: Closed Registration deadline: 20 December 2025

American Physical Society (APS) Global Physics Summit Symposium: “Chemical Physics in Astrophysical Environments” 15‒20 March 2026 Denver, CO, USA https://summit.aps.org/ Abstract submission deadline: Closed Registration deadlines: 29 January 2026 (Early bird), 5 March 2026 (Regular)

American Chemical Society (ACS) Spring Meeting 2026 Astrochemistry Subdivision Symposium: “The Icy Universe Revealed by JWST” 22‒26 March 2026 Atlanta, GA, USA http://astro.phys-acs.org/symposia/Spring2026.html Abstract submission deadline: Closed Registration dates: 10 December 2025–22 March 2026

Astrobiobiology Science Conference (AbSciCon) 2026 17‒22 May 2026 Madison, WI, USA https://www.agu.org/abscicon Abstract submission deadline: 14 January 2026 Registration dates: Not posted yet

International Astronomical Union (IAU) Symposium 407: Origins 2026 6–11 July 2026 Paris, France https://www.iau.org/Iau/Iau/Science/Scientific-Meetings/IAUM2026/IAUS407.aspx Abstract submission dates: Not posted yet Registration dates: Not posted yet

COSPAR 2026 46th General Assembly 1‒9 August 2026 Florence, Italy https://cospar2026.org/ Abstract submission deadline: 13 February 2026 Registration deadlines: 17 May 2026 (Early bird), 15 July 2026 (Regular), 1 August 2026 (Onsite)

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