q11/random_k4/random_4.md

LABORATORY ASTROPHYSICS
Newsletter

DECEMber 2025 | Issue 1

Cold Solar System Objects

Interview with Dr. Farid Salama

Presentation of the Cold Solar System Objects (CSSO) ISFM Project Facilities

Recent publications (January–November 2025)

Upcoming conferences

Letter from the
Editors

to

the

are

excited

present

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

is

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.

I

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.

it

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/

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

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)

is

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).

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/

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.

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/

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.

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/

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
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Astronomy & Astrophysics, 699, A79 (2025)
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Missing interstellar sulfur in inventories of polysulfanes and molecular octasulfur crowns
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Synthesis of new hexamethylenetetramine-based products (HMT-R) in UV-irradiated pre-cometary ice analogues
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H2S ice sublimation dynamics: Experimentally constrained binding energies, entrapment efficiencies, and
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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)
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Photolysis and sublimation chemistry of ammonium cyanide with relevance to cometary environments
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Establishing an accurate infrared band strength for the cyanate ion in interstellar ices
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Monthly Notices of the Royal Astronomical Society, 537, 2918 (2025)
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Exploring the formation and alteration of organics in ice: experimental insights for astrochemistry and space
missions
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Earth, Planets and Space, 77, 70 (2025)
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Cosmic-ray induced sputtering of interstellar formaldehyde ices
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https://doi.org/10.1051/0004-6361/202449937

Infrared spectroscopy of astrophysical ice analogues at oblique angles
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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
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Astronomy & Astrophysics, 694, A263 (2025)
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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
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ACS Earth and Space Chemistry, 9, 715 (2025)
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VIS-to-MIR reflectance and Raman spectroscopy of the CM2 NWA 12184 carbonaceous chondrite
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Meteoritics & Planetary Science, 60, 570 (2025)
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Sample return missions: Rosetta Stones returned from the first small bodies in the Solar System Nakamura, T.,
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Space Science Reviews, 221, 44 (2025)
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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)
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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)
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Formation of ammonium nitrate particles in CO2-rich atmospheres
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The Planetary Science Journal, 6, 135 (2025)
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Photochemistry of benzene (C6H6) hydrogen cyanide (HCN) co-condensed ices part 2: Formation of aerosols
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Experimental investigations of mineral-organic chondritic analogs under hydrothermal conditions: Implications for
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Geochimica et Cosmochimica Acta, 398, 29 (2025)
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Mid-infrared detection and characterization of refractory inclusions in CM and CO chondrites: A non-destructive
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Meteoritics & Planetary Science, 60, 544 (2025)
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Water in Ryugu as a property of processes in its parent body
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Methylene-to-methyl ratio variability in Ryugu samples: Clues to a heterogeneous aqueous alteration
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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
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Astronomy & Astrophysics, 694, A126 (2025)
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Molecular evolution of H2O:O2 ices at different temperatures in simulated space environments. I. Chemical
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Tholin formation and accumulation due to hypersonic high-temperature flows in methane-containing atmospheres
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Icarus, 439, 116649 (2025)
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Elemental and isotopic signatures of asteroid Ryugu support three early Solar System reservoirs
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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
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Measurement of photochemical haze refractive indices and hygroscopicity: Influence of CO2 in
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Astrobiology, 25, 395 (2025)
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Abundant ammonia and nitrogen-rich organic matter in samples from the B-type carbonaceous asteroid Bennu
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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
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Registration deadline: 15 December 2025

Pacifichem 2025
15‒20 December 2025
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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
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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)

Section header image credits: NASA/JPL-Caltech/STScI