Efficient surface formation route of interstellar hydroxylamine through NO hydrogenation. II. The multilayer regime in interstellar relevant ices

Water Complex of Imidogen

Imidogen (NH) is the simplest nitrogen hydride that plays an important role in combustion and interstellar chemistry, and its combination with H₂O is the prototypical amidation reaction of O-H bonds involving a nitrene intermediate. Herein, we report the observation of the elusive water complex of NH, a prereaction complex associated with the amidation reaction in a solid N₂ matrix at 10 K. The hydrogen-bonded structure of NH···OH₂ (versus HN···HOH) is confirmed via IR spectroscopy with comprehensive isotope labeling (D, ¹⁸O, and ¹⁵N) and quantum chemical calculations at the UCCSD(T)/aug-cc-pVQZ level of theory. In line with the observed absorption at 350 nm, irradiation of the complex at 365 nm leads to O-H bond insertion, yielding hydroxylamine NH₂OH.

Infrared Spectroscopic Study on Swift-Ion Irradiation of Solid N2O-H2O Samples: Synthesis of N-O Bearing Species in Astrophysical Ices

As of early 2022, only six species bearing an N-O bond have been detected toward cold molecular clouds and regions of star formation. It is not clear yet if the small number of N-O bond species found in the interstellar medium so far stems from physical and technological limitations of astronomical detection techniques, or whether in fact molecules that bear an N-O bond are for some reason rare in these objects of the interstellar medium. Astronomical N-O bearing molecules are important because they are part of astrochemical models which propose that they are precursors of hydroxylamine (NH₂OH), a species linked to the formation of prebiotic amino acids in space. The aim of this study is the better understanding of the open question of the interstellar synthesis of N-O bearing species. We have analyzed by infrared spectroscopy an astrophysically relevant polar ice mixture of N₂O:H₂O processed by 90 MeV ¹³⁶Xe²³⁺ ions, which can mimic the physicochemical processes triggered by cosmic rays in water-covered interstellar ice grains. The results show the formation of N₂O₃ and of H₂O₂, but no HN-O species of any kind were detected. Such findings are discussed in light of recent studies from our group and from the literature.

Cysteine 343 in the substrate binding domain is the primary S-Nitrosylated site in protein disulfide isomerase

Abnormal protein accumulations are typical pathological features for neurodegenerative diseases. Protein disulfide isomerase (PDI) is a critical enzyme in oxidative protein folding. S-nitrosylated PDI has been detected in the postmortem brain in neurodegenerative disease patients, but the effect of S-nitrosylation on PDI function and developing neurodegeneration was not clarified in detail. In this study, we identified that in vitro and in vivo S-nitrosylation of C343 in the b' domain of PDI occurs. Reduced recombinant human PDI (hPDI) reacted quickly with S-nitrosocompounds, with an observed increase in the expected S-nitrosylated species and the appearance of the disulfide state of the active sites. Both Mononitrosylated and dinitrosylated were observed from the S-nitrosylation of hPDI. Dinitrosylated species were S-nitrosylated both cysteines at active site. But, at least in part, mononitrosylated species were S-nitrosylated on cysteine 343 in the substrate binding b' domain. Although active site S-nitrosylation is reversible by reduced glutathione, S-nitrosylation of C343 is comparative stable. S-nitrosylation of PDI in SH-SY5Y cells was observed after the S-nitrosocysteine (SNOC) treatment and S-nitrosylated PDI was still detected 24 h after removing SNOC. While wild-type PDI was S-nitrosylated, the level of S-nitrosylation of the C343S mutant in over-expressed cells was substantially lower and only wild-type PDI of S-nitrosylation remained 24 h after removing SNOC in over-expressed cells. Both of in vitro and in vivo results suggested that S-nitrosylation of C343 in PDI may be the causative effect on physiological changes in neurodegerenative disease patients, and may be useful for the drug development for neurodegenerative diseases.

Spectroscopy of prospective interstellar ions and radicals isolated in para-hydrogen matrices

The p-H₂ matrix-isolation technique coupled with photolysis in situ or electron bombardment produces protonated or hydrogenated species important in astrochemistry.

Radiolysis of N2-rich astrophysical ice by swift oxygen ions: implication for space weathering of outer solar system bodies

In order to investigate the role of medium mass cosmic rays and energetic solar particles in the processing of N₂-rich ice on frozen moons and cold objects in the outer solar system, the bombardment of an N₂ : H₂O : NH₃ : CO₂ (98.2 : 1.5 : 0.2 : 0.1) ice mixture at 16 K employing 15.7 MeV ¹⁶O⁵⁺ was performed. The changes in the ice chemistry were monitored and quantified by Fourier transformed infrared spectroscopy (FTIR). The results indicate the formation of azide radicals (N₃), and nitrogen oxides, such as NO, NO₂, and N₂O, as well as the production of CO, HNCO, and OCN^-. The effective formation and destruction cross-sections are roughly on the order of 10^-12 cm² and 10^-13 cm², respectively. From laboratory molecular analyses, we estimated the destruction yields for the parent species and the formation yields for the daughter species. For N₂, this value was 9.8 × 10⁵ molecules per impact of ions, and for the most abundant new species (N₃), it was 1.1 × 10⁵ molecules per impact of ions. From these yields, an estimation of how many species are destroyed or formed in a given timescale (10⁸ years) in icy bodies in the outer solar system was calculated. This work reinforces the idea that such physicochemical processes triggered by cosmic rays, solar wind, and magnetospheric particles (medium-mass ions) in nitrogen-rich ices may play an important role in the formation of molecules (including pre-biotic species precursors such as amino acids and other "CHON" molecules) in very cold astrophysical environments, such as those in the outer region of the solar system (e.g. Titan, Triton, Pluto, and other KBOs).

Reaction of H + HONO in solid para-hydrogen: infrared spectrum of ˙ONH(OH)

Hydrogenation reactions in the N/O chemical network are important for an understanding of the mechanism of formation of organic molecules in dark interstellar clouds, but many reactions remain unknown.

Dynamic nitroxyl formation in the ammonia oxidation on platinum via Eley–Rideal reactions

Simultaneous production of HNO, NO, and OH via Eley–Rideal reactions during the dynamic oxidation of ammonia on Pt surfaces.

Polymer amide as an early topology

Hydrophobic polymer amide (HPA) could have been one of the first normal density materials to accrete in space. We present ab initio calculations of the energetics of amino acid polymerization via gas phase collisions. The initial hydrogen-bonded di-peptide is sufficiently stable to proceed in many cases via a transition state into a di-peptide with an associated bound water molecule of condensation. The energetics of polymerization are only favorable when the water remains bound. Further polymerization leads to a hydrophobic surface that is phase-separated from, but hydrogen bonded to, a small bulk water complex. The kinetics of the collision and subsequent polymerization are discussed for the low-density conditions of a molecular cloud. This polymer in the gas phase has the properties to make a topology, viz. hydrophobicity allowing phase separation from bulk water, capability to withstand large temperature ranges, versatility of form and charge separation. Its flexible tetrahedral carbon atoms that alternate with more rigid amide groups allow it to deform and reform in hazardous conditions and its density of hydrogen bonds provides adhesion that would support accretion to it of silicon and metal elements to form a stellar dust material.

Solid state chemistry of nitrogen oxides – Part II: surface consumption of NO2

Efficient surface destruction mechanisms (NO₂ + H/O/N), leading to solid H₂O, NH₂OH, and N₂O, can explain the non-detection of NO₂ in space.

THz and mid-IR spectroscopy of interstellar ice analogs: methyl and carboxylic acid groups

A fundamental problem in astrochemistry concerns the synthesis and survival of complex organic molecules (COMs) throughout the process of star and planet formation. While it is generally accepted that most complex molecules and prebiotic species form in the solid phase on icy grain particles, a complete understanding of the formation pathways is still largely lacking. To take full advantage of the enormous number of available THz observations (e.g.,Herschel Space Observatory, SOFIA, and ALMA), laboratory analogs must be studied systematically. Here, we present the THz (0.3–7.5 THz; 10–250 cm⁻¹) and mid–IR (400–4000 cm⁻¹) spectra of astrophysically-relevant species that share the same functional groups, including formic acid (HCOOH) and acetic acid (CH₃COOH), and acetaldehyde (CH₃CHO) and acetone ((CH₃)₂CO), compared to more abundant interstellar molecules such as water (H₂O), methanol (CH₃OH), and carbon monoxide (CO). A suite of pure and mixed binary ices are discussed. The effects on the spectra due to the composition and the structure of the ice at different temperatures are shown. Our results demonstrate that THz spectra are sensitive to reversible and irreversible transformations within the ice caused by thermal processing, suggesting that THz spectra can be used to study the composition, structure, and thermal history of interstellar ices. Moreover, the THz spectrum of an individual species depends on the functional group(s) within that molecule. Thus, future THz studies of different functional groups will help in characterizing the chemistry and physics of the interstellar medium (ISM).

Solid state chemistry of nitrogen oxides – Part I: surface consumption of NO

NO₂ is efficiently formed in the solid state via NO + O/O₂/O₃ reactions.

Efficient diffusive mechanisms of O atoms at very low temperatures on surfaces of astrophysical interest

At the low temperatures of interstellar dust grains, it is well established that surface chemistry proceeds via diffusive mechanisms of H atoms weakly bound (physisorbed) to the surface. Until recently, however, it was unknown whether atoms heavier than hydrogen could diffuse rapidly enough on interstellar grains to react with other accreted species. In addition, models still require simple reduction as well as oxidation reactions to occur on grains to explain the abundances of various molecules. In this paper we investigate O-atom diffusion and reactivity on a variety of astrophysically relevant surfaces (water ice of three different morphologies, silicate, and graphite) in the 6.5–25 K temperature range. Experimental values were used to derive a diffusion law that emphasizes that O atoms diffuse by quantum mechanical tunnelling at temperatures as low as 6.5 K. The rates of diffusion on each surface, based on modelling results, were calculated and an empirical law is given as a function of the surface temperature. The relative diffusion rates are k_H2Oice > k_sil > k_graph ≫ k_expected. The implications of efficient O-atom diffusion over astrophysically relevant time-scales are discussed. Our findings show that O atoms can scan any available reaction partners (e.g., either another H atom, if available, or a surface radical like O or OH) at a faster rate than that of accretion. Also, as dense clouds mature, H₂ becomes far more abundant than H and the O : H ratio grows, and the reactivity of O atoms on grains is such that O becomes one of the dominant reactive partners together with H.

Astrochemistry of transition metals? The selected cases of [FeN]+, [FeNH]+ and [(CO)2FeN]+: pathways toward CH3NH2 and HNCO

Transition metals are proposed to play an active role in the synthesis of organic compounds containing heteroatoms in astrochemistry.

Hydrogenation processes from hydrogen peroxide: an investigation in Ne matrix for astrochemical purposes

Hydrogenation processes of hydrogen peroxide leading to the formation of water.

SURFRESIDE(2): an ultrahigh vacuum system for the investigation of surface reaction routes of interstellar interest

A new ultrahigh vacuum experiment is described to study atom and radical addition reactions in interstellar ice analogues for astronomically relevant temperatures. The new setup - SURFace REaction SImulation DEvice (SURFRESIDE(2)) - allows a systematic investigation of solid state pathways resulting in the formation of molecules of astrophysical interest. The implementation of a double beam line makes it possible to expose deposited ice molecules to different atoms and/or radicals sequentially or at the same time. Special efforts are made to perform experiments under fully controlled laboratory conditions, including precise atom flux determinations, in order to characterize reaction channels quantitatively. In this way, we can compare and combine different surface reaction channels with the aim to unravel the solid state processes at play in space. Results are constrained in situ by means of a Fourier transform infrared spectrometer and a quadrupole mass spectrometer using reflection absorption infrared spectroscopy and temperature programmed desorption, respectively. The performance of the new setup is demonstrated on the example of carbon dioxide formation by comparing the efficiency through two different solid state channels (CO + OH → CO2 + H and CO + O → CO2) for which different addition products are needed. The potential of SURFRESIDE(2) to study complex molecule formation, including nitrogen containing (prebiotic) compounds, is discussed.