Interstellar Archives

Schematic diagram demonstrating interstellar ices within dark clouds made of molecular hydrogen being processed by photochemistry involving the production of electronically excited water and radiation chemistry involving the production of ionized water and secondary electrons. This work focuses on the interaction depicted in the second of the two CRs (blue lines) in which a CR interacts in the ice mantle to produce secondary electrons. Reproduced from Ref. 4. Copyright 2019, The Royal Society of Chemistry. -- astro-ph.HE

The Role of Low-energy (< 20 eV) Secondary Electrons in the Extraterrestrial Synthesis of Prebiotic Molecules

by Keith CowingDecember 6, 2023December 6, 2023

We demonstrate for the first time that Galactic cosmic rays with energies as high as 1e10 eV can trigger a cascade of low-energy (< 20 eV) secondary electrons that could […]

Tentative detection of oxalic acid (HOOC-COOH) during warm-up of an UV-irradiated CH3COOH:H2O ice sample (Exp. 11). Left panel: QMS signal for 𝑚 𝑧 = 44, 45 and 46. These fragments are representative of the oxalic acid, while 𝑚 𝑧 = 21 is not expected to correspond to any molecule and is used as a reference. Centre panel: mass spectrum of oxalic acid taken from NIST database. Right panel: scheme to form oxalic acid via radical-radical reaction from photon and thermal processing of acetic acid-containing ices. The formation temperature of oxalic acid could not be determined, since oxalic acid was only detected from QMS data in the gas phase during thermal desorption. -- astro-ph.IM

Astrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Imaging & Spectroscopy, Interstellar, Status Report

UV-photoprocessing Of Acetic Acid (CH3COOH)-bearing Interstellar Ice Analogs

by Keith CowingDecember 6, 2023December 6, 2023

Acetic acid (CH3COOH) was detected in the gas toward interstellar clouds, hot cores, protostars and comets. Its formation in ice mantles was proposed and acetic acid awaits detection in the […]

NH3-H2O co-deposition experiments. All experiments have been performed on a gold substrate. The TPDs have a ramp of 0.2K/s. The solid lines represent the desorption of NH3 while the dashed-dotted lines represent the desorption of water. Lines of the same colour belong to the same set of experiments. Inset: TPD of NH3 from a gold surface used to calibrate all the consequent experiments. -- astro-ph.SR

Astrochemistry, Astrogeology, Biochemistry & Organic Chemistry, Comets and Asteroids, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Interstellar, Status Report

Experimental Study Of The Binding Energy Of NH3 On Different Types Of Ice And Its Impact On The Snow Line Of NH3 And H2O

by Keith CowingDecember 3, 2023December 2, 2023

N-bearing molecules (like N2H+ or NH3) are excellent tracers of high-density, low-temperature regions like dense cloud cores and could shed light into snowlines in protoplanetary disks and the chemical evolution […]

This is an artist's concept depicting the presence of buckyballs in space. Buckyballs, which consist of 60 carbon atoms arranged like soccer balls, have been detected in space before by scientists using NASA's Spitzer Space Telescope. The new result is the first time an electrically charged (ionized) version has been found in the interstellar medium. NASA/JPL-Caltech

Astrochemistry, Astrogeology, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biophysics, Imaging & Spectroscopy, Press Release

Hubble Detected C60 Molecules aka Buckyballs

by Keith CowingNovember 25, 2023November 25, 2023

Scientists using NASA’s Hubble Space Telescope have confirmed the presence of electrically-charged molecules in space shaped like soccer balls, shedding light on the mysterious contents of the interstellar medium (ISM) […]

Emission of SO, SiS, and SO2 integrated in velocity. Upper panels: velocity-integrated emission of, from left to right, SO N = 3 − 2, N = 2 − 1(2), N = 2 − 1(3), and N = 4 − 4 (see Table 1 for the spectral parameters). The integration velocity range is 85.7–105.8 km s−1 in all images to match the velocity interval where the PN emission is detected. The black contours start from the 3σ rms level of the integrated maps, which is, from left to right: 4.8 × 10−2 Jy beam−1 km s−1 ; 2.5 × 10−2 Jy beam−1 km s−1 ; 3.6 × 10−2 Jy beam−1 km s−1 ; 2.7 × 10−2 Jy beam−1 km s−1 , and the step is of 10σ rms. The white contour corresponds to the PN integrated emission, and the numbered regions "1" and "2" are those defined in Fig. 1. The synthesised beam is illustrated in the lower-left corner. To the right of the quantum numbers, we indicate the Eup of the transition. Lower panels: same as the upper panels for the SiS J = 5 − 4 and J = 6 − 5 lines, and the SO2 JKa,Kb = 31,3 − 20,2 and JKa,Kb = 101,9 − 100,10 lines. The 3σ rms level is: 2.9 × 10−2 Jy beam−1 km s−1 for SiS J = 5 − 4; 2.3 × 10−2 Jy beam−1 km s−1 for SiS J = 6 − 5; 2.95 × 10−3 Jy beam−1 km s−1 for SO2 JKa,Kb = 31,3 − 30,2; 1 × 10−2 Jy beam−1 km s−1 for SO2 JKa,Kb = 101,9 − 100,10. -- astro-ph.GA

Astrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Imaging & Spectroscopy, Status Report

The GUAPOS Project: G31.41+0.31 Unbiased ALMA Spectral Observational Survey. IV. Phosphorus-bearing Molecules And Their Relation With Shock Tracers

by Keith CowingNovember 24, 2023November 24, 2023

The astrochemistry of the important biogenic element phosphorus (P) is still poorly understood, but observational evidence indicates that P-bearing molecules are likely associated with shocks.

A graphic illustrating the Galactic distribution of phosphorus in the range 0–25 kpc from the Galactic Centre, as identified from stellar and interstellar observations. Detections by atomic transitions in stellar photospheres are denoted by green stars (from ref. 2 and references therein), in diffuse clouds by purple circles (ref. 16 and those therein17,18,19), and in planetary nebulae by blue triangles, while magenta circles and cyan diamonds mark the identifications in molecular clouds and circumstellar envelopes from molecular lines. The red square shows the position of WB89-621. The orange X indicates the solar system. The APOGEE survey detections are not shown per possible contamination. WB89-621 is the only known source of phosphorus in any form beyond 12 kpc.

Astrochemistry, Astronomy & Telescopes, Biosignatures & Paleobiology, Imaging & Spectroscopy, Status Report

Phosphorous Has Been Discovered In The Outer Reaches Of The Milky Way

by Keith CowingNovember 16, 2023November 16, 2023

Despite its importance in planet formation and biology, phosphorus has been identified only in the inner 12 kpc of the Galaxy2-19. The study of this element has been hindered in […]

Taurus Magnetic Cloud viewed by Herschel and Planck -- ESA

AI - Data - Apps - Cybernetics, Astrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Imaging & Spectroscopy, Status Report

The UMIST Database For Astrochemistry 2022

by Keith CowingNovember 8, 2023November 8, 2023

Detailed astrochemical models are a key component to interpret the observations of interstellar and circumstellar molecules since they allow important physical properties of the gas and its evolutionary history to […]

Scanning electron microscope images of the original carbon material (left) and after ice deposition and subsequent irradiation with X-rays (right). The original thickness of a-13C dust is ∼300 nm. Left: the carbon grains are 3–5 nm in size and form fractal entities that finally produce a very porous, three-dimensional layer. Right: the erosion of carbon is clearly visible by a strong flattening of the carbon structure. -- astro-ph.SR

Astrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Biosignatures & Paleobiology, Icy Worlds, Interstellar, Status Report

Interstellar Carbonaceous Dust Erosion Induced By X-ray Irradiation Of Water Ice In Star-forming Regions

by Keith CowingNovember 1, 2023November 1, 2023

The chemical inventory of protoplanetary midplanes is the basis for forming planetesimals. Among them, solid-state reactions based on CO/CO2 toward molecular complexity on interstellar dust grains have been studied in […]

The (H2O)20 cluster model used in this work, optimised at ωB97X-V/def2-TZVP, which also shows the size dimensions. The different positions in which the C atom has been adsorbed (Pos1, Pos2, and Pos3) are also shown. -- astro-ph.GA

Astrochemistry, Astronomy & Telescopes, Biochemistry & Organic Chemistry, Interstellar, Status Report

Formation Of Interstellar Complex Organic Molecules On Water-rich Ices Triggered By Atomic Carbon Freezing

by Keith CowingOctober 27, 2023October 27, 2023

The reactivity of interstellar carbon atoms (C) on the water-dominated ices is one of the possible ways to form interstellar complex organic molecules (iCOMs).

‘Oumuamua -- Illustration by Samuel Cabot

Astrochemistry, Astrogeology, Astronomy & Telescopes, Comets and Asteroids, Interstellar, Meteorites & Asteroids, Panspermia, Press Release, Space Weather & Heliophysics

X-rays May Tell Us More About The Origins Of Visiting Space Rocks

by Keith CowingOctober 14, 2023October 14, 2023

A research team led by a Yale astronomer has some advice for our next close encounter with a wandering, interstellar object. Check its X-rays on the way out. Since 2017, […]

Interstellar

The Role of Low-energy (< 20 eV) Secondary Electrons in the Extraterrestrial Synthesis of Prebiotic Molecules

UV-photoprocessing Of Acetic Acid (CH3COOH)-bearing Interstellar Ice Analogs

Experimental Study Of The Binding Energy Of NH3 On Different Types Of Ice And Its Impact On The Snow Line Of NH3 And H2O

Hubble Detected C60 Molecules aka Buckyballs

The GUAPOS Project: G31.41+0.31 Unbiased ALMA Spectral Observational Survey. IV. Phosphorus-bearing Molecules And Their Relation With Shock Tracers

Phosphorous Has Been Discovered In The Outer Reaches Of The Milky Way

The UMIST Database For Astrochemistry 2022

Interstellar Carbonaceous Dust Erosion Induced By X-ray Irradiation Of Water Ice In Star-forming Regions

Formation Of Interstellar Complex Organic Molecules On Water-rich Ices Triggered By Atomic Carbon Freezing

X-rays May Tell Us More About The Origins Of Visiting Space Rocks

Relevance of the Avalon Assemblage as an Astrobiological Analog for Icy Ocean Worlds

The Climate and Potential Habitability of a Warm and Oxygenated Mars

Variable X-ray flux May Explain Variable Helium Escape From The Habitable-zone Exoplanet LHS 1140b

Spacetime Contactability in Galactic Civilization Networks: Contact Counts and Percolation

Surprisingly Enriched CO and CH4 in Halley-type Comet 13P/Olbers: Clues to Its Interstellar Heritage