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# Photodissociation and photoionization of molecules of astronomical interest

H. Hrodmarsson, E. van Dishoeck

► To cite this version:

H. Hrodmarsson, E. van Dishoeck. Photodissociation and photoionization of molecules of astronomical interest. Astronomy and Astrophysics - A&A, 2023, 675, pp.A25. 10.1051/0004-6361/202346645. hal-04568712

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# Photodissociation and photoionization of molecules of astronomical interest

## Updates to the Leiden photodissociation and photoionization cross section database*

H. R. Hrodmarsson<sup>1,2</sup> and E. F. van Dishoeck<sup>3,4</sup>

Received 13 April 2023 / Accepted 16 May 2023

## ABSTRACT

*Context.* Vacuum-ultraviolet (VUV) photons are important drivers of chemical processes in space. Thus, it is important to accurately characterize and constrain photorates in different radiation fields, via the photodissociation and photoionization cross sections of individual atoms and molecules. These have been available in the Leiden VUV photodissociation and photoionization cross section database.

*Aims.* Experimental and theoretical advances in the past decade or so have allowed multiple new cross sections to be obtained, particularly photoionization cross sections of radicals. The database is hereby updated by including these more recent cross sections and is also expanded with several astronomically relevant species.

*Methods.* The cross sections have been used to calculate photodissociation and photoionization rates in several different radiation fields as well as from cosmic-ray-induced VUV fluxes. The reduction of rates in shielded regions was calculated as a function of dust, molecular and atomic hydrogen, atomic carbon, and self-shielding column densities. The relative importance of these shielding types is molecule and atom dependent, as well as the assumed dust absorbance. All the data are publicly available from the Leiden VUV cross section database.

*Results.* The Leiden VUV cross section database has been updated with 14 new astrophysically relevant molecular species and 16 updates to previous entries. The database update is accompanied by a brief review of the basic physical processes, particularly photoionization processes which have not been reviewed in the context of previous database updates.

**Key words.** molecular data – ISM: molecules – photon-dominated region (PDR) – cosmic rays – dust, extinction – ultraviolet: ISM

## 1. Introduction

At the time of writing, almost a century has passed since the first propositions that atomic and molecular abundances in interstellar environments are governed by photodissociation and photoionization processes (Eddington 1928). Today it is indeed apparent that vacuum-ultraviolet (VUV) radiation is undeni- ably an important driver of chemical reactions in space. The VUV regime is characterized by photons with wavelengths in the 10–200 nm range which can only propagate under vacuum (hence the name); however more importantly, VUV photons pos- sess the unique energetic quanta capable of breaking molecular bonds and/or ionizing atoms and molecules. These characteris- tic photodissociations and photoionizations are both species- and

wavelength-dependent, and hence, VUV-driven photodissocia- tion and photoionization processes have been accumulated and database-formatted for wide usage in the astrochemical com- munity. These are the principle parameters when it comes to quantifying photodestruction rates (or photorates) of molecules in different interstellar or galactic environments, which makes their implementation crucial not only in astrochemical model- ing (van Dishoeck 1988; Gredel et al. 1989; Roberge et al. 1991; van Dishoeck et al. 2006; van Dishoeck & Visser 2015; Heays et al. 2017), but in combustion science as well where on average larger molecules such as hydrocarbons and complex organic molecules are typically implemented (Kameta et al. 2002; Yang et al. 2012; Keller-Rudek et al. 2013).

Recent advances in the field of astrochemistry, molecular astrophysics, and atmospheric science have allowed our under- standing of molecular complexity in space to reach a veritable golden age. These fields are currently flourishing as the rate

<footnote n="1">¹ LISA UMR 7583 Université Paris-Est Créteil and Université de Paris, Institut Pierre et Simon Laplace, 61 Avenue du Général de Gaulle, 94010 Créteil, France
e-mail: hhrodmarsson@lisa.ipsl.fr</footnote>

<footnote n="2">² Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: hrodmarsson@strw.leidenuniv.nl</footnote>

<footnote n="3">³ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: ewine@strw.leidenuniv.nl</footnote>

<footnote n="4">⁴ Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany</footnote>

<footnote>* Leiden photodissociation and photoionization cross section database: https://home.strw.leidenuniv.nl/~ewine/photo/</footnote>
# Photodissociation and photoionization of molecules of astronomical interest

## Updates to the Leiden photodissociation and photoionization cross section database*

H. R. Hrodmarsson<sup>1,2</sup> and E. F. van Dishoeck<sup>3,4</sup>

Received 13 April 2023 / Accepted 16 May 2023

## ABSTRACT

*Context.* Vacuum-ultraviolet (VUV) photons are important drivers of chemical processes in space. Thus, it is important to accurately characterize and constrain photorates in different radiation fields, via the photodissociation and photoionization cross sections of individual atoms and molecules. These have been available in the Leiden VUV photodissociation and photoionization cross section database.

*Aims.* Experimental and theoretical advances in the past decade or so have allowed multiple new cross sections to be obtained, particularly photoionization cross sections of radicals. The database is hereby updated by including these more recent cross sections and is also expanded with several astronomically relevant species.

*Methods.* The cross sections have been used to calculate photodissociation and photoionization rates in several different radiation fields as well as from cosmic-ray-induced VUV fluxes. The reduction of rates in shielded regions was calculated as a function of dust, molecular and atomic hydrogen, atomic carbon, and self-shielding column densities. The relative importance of these shielding types is molecule and atom dependent, as well as the assumed dust absorbance. All the data are publicly available from the Leiden VUV cross section database.

*Results.* The Leiden VUV cross section database has been updated with 14 new astrophysically relevant molecular species and 16 updates to previous entries. The database update is accompanied by a brief review of the basic physical processes, particularly photoionization processes which have not been reviewed in the context of previous database updates.

**Key words.** molecular data – ISM: molecules – photon-dominated region (PDR) – cosmic rays – dust, extinction – ultraviolet: ISM

## 1. Introduction

At the time of writing, almost a century has passed since the first propositions that atomic and molecular abundances in interstellar environments are governed by photodissociation and photoionization processes (Eddington 1928). Today it is indeed apparent that vacuum-ultraviolet (VUV) radiation is undeni- ably an important driver of chemical reactions in space. The VUV regime is characterized by photons with wavelengths in the 10–200 nm range which can only propagate under vacuum (hence the name); however more importantly, VUV photons pos- sess the unique energetic quanta capable of breaking molecular bonds and/or ionizing atoms and molecules. These characteris- tic photodissociations and photoionizations are both species- and

wavelength-dependent, and hence, VUV-driven photodissocia- tion and photoionization processes have been accumulated and database-formatted for wide usage in the astrochemical com- munity. These are the principle parameters when it comes to quantifying photodestruction rates (or photorates) of molecules in different interstellar or galactic environments, which makes their implementation crucial not only in astrochemical model- ing (van Dishoeck 1988; Gredel et al. 1989; Roberge et al. 1991; van Dishoeck et al. 2006; van Dishoeck & Visser 2015; Heays et al. 2017), but in combustion science as well where on average larger molecules such as hydrocarbons and complex organic molecules are typically implemented (Kameta et al. 2002; Yang et al. 2012; Keller-Rudek et al. 2013).

Recent advances in the field of astrochemistry, molecular astrophysics, and atmospheric science have allowed our under- standing of molecular complexity in space to reach a veritable golden age. These fields are currently flourishing as the rate

<footnote n="1">¹ LISA UMR 7583 Université Paris-Est Créteil and Université de Paris, Institut Pierre et Simon Laplace, 61 Avenue du Général de Gaulle, 94010 Créteil, France
e-mail: hhrodmarsson@lisa.ipsl.fr</footnote>

<footnote n="2">² Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: hrodmarsson@strw.leidenuniv.nl</footnote>

<footnote n="3">³ Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
e-mail: ewine@strw.leidenuniv.nl</footnote>

<footnote n="4">⁴ Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany</footnote>

<footnote>* Leiden photodissociation and photoionization cross section database: https://home.strw.leidenuniv.nl/~ewine/photo/</footnote>
of new molecule detections has been accelerating for the past few years where a few new annual detections in the 2000s and 2010s have ballooned to tens of new detections annually in the 2020s (McGuire 2022). Thanks to dedicated large-scale facilities such as the Large Atacama Millimeter/submillimeter Array (ALMA), improvements in data treatments such as spectral stacking methods (Loomis et al. 2021), and dedicated deep surveys at long wavelengths such as GOTHAM (McGuire et al. 2020) and QUIJOTE (Agúndez et al. 2015; Cernicharo et al. 2021a), the previously large thresholds that were required to be overcome in order to detect a molecule have been significantly decreased.

Accommodating new molecules in astrochemical models is a titanic task requiring an enormous amount of reaction rates. The previous update of the Leiden VUV cross section database (Heays et al. 2017) collected photodissociation and photoionization cross sections for 102 atoms and molecules of astronomical interest. These were used to calculate dissociation and ionization rates under different radiation fields (including cosmic-rays) both with and without dust attenuation. An update to the database is timely to meet the data needs of the ever-growing astrochemical user community, which also presents an opportunity to highlight recent experimental and theoretical advances that have allowed cross sections of (in particular) radicals to be measured in absolute terms and will continue to produce datasets relevant to interstellar photoprocesses.

Experimental and theoretical advances have allowed cross sections of challenging species to have been measured and computed. New developments at large-scale synchrotron facilities such as SOLEIL (Nahon et al. 2012), Swiss Light Source (SLS; Johnson et al. 2009), and the Advanced Light Source (ALS; Heimann et al. 1997) in double-imaging photoelectron photoion coincidence (i²PEPICO) spectroscopy (Garcia et al. 2013; Tang et al. 2015b; Baer & Tuckett 2017), coupled with the facile production of radicals using flow tubes (Garcia et al. 2015), pyrolysis sources (Hemberger et al. 2021, 2022), and reaction chambers (Osborn et al. 2008; Taatjes et al. 2008), have allowed the measurements of wavelength-dependent absolute photoionization cross sections of radicals (Dyke 2019), and recent theoretical advances have allowed photodissociation cross sections of diatomics to be computed at high temperatures (Pezzella et al. 2021).

Ultraviolet (UV) radiation is mostly produced by very hot objects in our Universe, principally stars in various stages of their lifespan. While dark clouds efficiently shield the material therein, cosmic-ray impacts still penetrate the opaque clouds and induce VUV photon emission from electronically excited atomic and molecular hydrogen (Prasad & Tarafdar 1983; Gredel et al. 1989; Caselli & Walmsley 2001). The cloud edges, however, are subject to irradiation by far-UV (FUV) photons with energies of 6–13.6 eV (91–207 nm) as photons with energies above 13.6 eV (the ionization threshold of hydrogen) are quickly scavenged.

In more general terms, clouds of gas and dust in which photodissociation and photoionization are the dominant destruction pathways are collectively termed photon-dominated or photodissociation regions (PDRs; Tielens & Hollenbach 1985; Wolfire et al. 2022). Therein, the formation and destruction of a large family of molecules is governed by VUV-driven photoprocesses. Chemistry is expedited by the formation of reactive radicals and ions in photodissociation and photoionization processes, respectively (Tielens 2013; van Dishoeck 2014). Thus, PDRs offer a dynamic interstellar laboratory where VUV radiation acts as the ultimate destroyer and creator; breaking down molecules but

simultaneously chemically replenishing the region with reactive species.

In giant molecular clouds, EUV photons (with energies above 13.6 eV) can ionize hydrogen and create H II regions such as Eta Carinae and the Tarantula nebulae (Larsson et al. 2012). PDRs surround the H II gas, especially in active star-forming regions whose relatively short lifetimes mean that the embedded chemistry is continually reignited by UV radiation (Harada et al. 2019). These PDRs display a layered structure which manifests as a hot interface between the H II region and PDR where the strong photon flux creates highly reactive ions such as CO⁺ and HOC⁺ which are generally good tracers of these environments (Sternberg & Dalgarno 1995; Armijos-Abendaño et al. 2020), as well as OH⁺, NH⁺, and CH⁺ (Bruderer et al. 2010; Benz et al. 2011). Other species such as c-C₃H₂ and C₂H can also be found at these interfaces (Rizzo et al. 2005) but they are also reliable tracers of outflow cavity walls (Tychoniec et al. 2021), and the upper atmosphere of the outer disk beyond the edge of the pebble disk of protoplanetary disks where they become more stratified and thus more permeable for UV photons (Bergin et al. 2016).

We are now better equipped than ever before to use chemistry as a tool to understand and trace the multiple stages of star and planet formation, particularly in heavily processed regions such as the so-called Central Molecular Zone (CMZ) where molecules are exposed to energetic phenomena such as shock waves due to the high level of turbulence, intense UV radiation fields from nearby massive stellar clusters, X rays from the central black hole, and are even further enhanced by cosmic ray ionization rates. Some such clouds in CMZ have now been found to be a prolific repository of complex organic molecules (COMs) in the Galaxy (Zeng et al. 2020).

Protoplanetary disks themselves experience strong radiation fields which can be seven orders of magnitude stronger than the interstellar field. This invariably influences the chemical structure of disks, and particularly at high vertical heights, the principle carbon bearer becomes C⁺ while in the cold midplane, molecules tend to be frozen onto dust grains (Aikawa et al. 2002; Öberg & Bergin 2021).

It is well known that employing accurate photorates significantly affects the chemical structure of disks (Walsh et al. 2012). Recent synergies of models and observations have shown, for example, that HCN and CN are not as good tracers of UV fields and photodissociation-initiated chemistry in disks as previously assumed (Cazzoletti et al. 2018; Bergner et al. 2021), high UV fluxes appear to be required to replicate C₂H emission features in several disks (Bergner et al. 2019; Bosman et al. 2021), and that many COMs can survive the passage through disks intact but this requires their photoprocesses to be well constrained (Bergner et al. 2021; Booth et al. 2021). Different stellar types at the respective centers of disks have also been shown to influence the disk chemistry where molecules such as HC₃N have been suggested to trace the extent by which the UV field may play an important role in catalyzing the disk chemistry (Bergner et al. 2018).

On the other hand, molecules (and chemistry) can be used to constrain the UV fields in particular regions. For instance, observations of water and other hydrides in high-mass star-forming regions allow us to put constraints on the UV flux from the incumbent protostar, which can be up to a few hundred times the strength of the ISRF (Benz et al. 2016). This is important for constraining the amount of FUV and X rays across the protostellar envelope to trace the full water chemistry. Water chemistry can already be heavily impacted by UV photodissociation in bow-shocks (Tabone et al. 2021) and X-rays have also been
of new molecule detections has been accelerating for the past few years where a few new annual detections in the 2000s and 2010s have ballooned to tens of new detections annually in the 2020s (McGuire 2022). Thanks to dedicated large-scale facilities such as the Large Atacama Millimeter/submillimeter Array (ALMA), improvements in data treatments such as spectral stacking methods (Loomis et al. 2021), and dedicated deep surveys at long wavelengths such as GOTHAM (McGuire et al. 2020) and QUIJOTE (Agúndez et al. 2015; Cernicharo et al. 2021a), the previously large thresholds that were required to be overcome in order to detect a molecule have been significantly decreased.

Accommodating new molecules in astrochemical models is a titanic task requiring an enormous amount of reaction rates. The previous update of the Leiden VUV cross section database (Heays et al. 2017) collected photodissociation and photoionization cross sections for 102 atoms and molecules of astronomical interest. These were used to calculate dissociation and ionization rates under different radiation fields (including cosmic-rays) both with and without dust attenuation. An update to the database is timely to meet the data needs of the ever-growing astrochemical user community, which also presents an opportunity to highlight recent experimental and theoretical advances that have allowed cross sections of (in particular) radicals to be measured in absolute terms and will continue to produce datasets relevant to interstellar photoprocesses.

Experimental and theoretical advances have allowed cross sections of challenging species to have been measured and computed. New developments at large-scale synchrotron facilities such as SOLEIL (Nahon et al. 2012), Swiss Light Source (SLS; Johnson et al. 2009), and the Advanced Light Source (ALS; Heimann et al. 1997) in double-imaging photoelectron photoion coincidence (i²PEPICO) spectroscopy (Garcia et al. 2013; Tang et al. 2015b; Baer & Tuckett 2017), coupled with the facile production of radicals using flow tubes (Garcia et al. 2015), pyrolysis sources (Hemberger et al. 2021, 2022), and reaction chambers (Osborn et al. 2008; Taatjes et al. 2008), have allowed the measurements of wavelength-dependent absolute photoionization cross sections of radicals (Dyke 2019), and recent theoretical advances have allowed photodissociation cross sections of diatomics to be computed at high temperatures (Pezzella et al. 2021).

Ultraviolet (UV) radiation is mostly produced by very hot objects in our Universe, principally stars in various stages of their lifespan. While dark clouds efficiently shield the material therein, cosmic-ray impacts still penetrate the opaque clouds and induce VUV photon emission from electronically excited atomic and molecular hydrogen (Prasad & Tarafdar 1983; Gredel et al. 1989; Caselli & Walmsley 2001). The cloud edges, however, are subject to irradiation by far-UV (FUV) photons with energies of 6–13.6 eV (91–207 nm) as photons with energies above 13.6 eV (the ionization threshold of hydrogen) are quickly scavenged.

In more general terms, clouds of gas and dust in which photodissociation and photoionization are the dominant destruction pathways are collectively termed photon-dominated or photodissociation regions (PDRs; Tielens & Hollenbach 1985; Wolfire et al. 2022). Therein, the formation and destruction of a large family of molecules is governed by VUV-driven photoprocesses. Chemistry is expedited by the formation of reactive radicals and ions in photodissociation and photoionization processes, respectively (Tielens 2013; van Dishoeck 2014). Thus, PDRs offer a dynamic interstellar laboratory where VUV radiation acts as the ultimate destroyer and creator; breaking down molecules but

simultaneously chemically replenishing the region with reactive species.

In giant molecular clouds, EUV photons (with energies above 13.6 eV) can ionize hydrogen and create H II regions such as Eta Carinae and the Tarantula nebulae (Larsson et al. 2012). PDRs surround the H II gas, especially in active star-forming regions whose relatively short lifetimes mean that the embedded chemistry is continually reignited by UV radiation (Harada et al. 2019). These PDRs display a layered structure which manifests as a hot interface between the H II region and PDR where the strong photon flux creates highly reactive ions such as CO⁺ and HOC⁺ which are generally good tracers of these environments (Sternberg & Dalgarno 1995; Armijos-Abendaño et al. 2020), as well as OH⁺, NH⁺, and CH⁺ (Bruderer et al. 2010; Benz et al. 2011). Other species such as c-C₃H₂ and C₂H can also be found at these interfaces (Rizzo et al. 2005) but they are also reliable tracers of outflow cavity walls (Tychoniec et al. 2021), and the upper atmosphere of the outer disk beyond the edge of the pebble disk of protoplanetary disks where they become more stratified and thus more permeable for UV photons (Bergin et al. 2016).

We are now better equipped than ever before to use chemistry as a tool to understand and trace the multiple stages of star and planet formation, particularly in heavily processed regions such as the so-called Central Molecular Zone (CMZ) where molecules are exposed to energetic phenomena such as shock waves due to the high level of turbulence, intense UV radiation fields from nearby massive stellar clusters, X rays from the central black hole, and are even further enhanced by cosmic ray ionization rates. Some such clouds in CMZ have now been found to be a prolific repository of complex organic molecules (COMs) in the Galaxy (Zeng et al. 2020).

Protoplanetary disks themselves experience strong radiation fields which can be seven orders of magnitude stronger than the interstellar field. This invariably influences the chemical structure of disks, and particularly at high vertical heights, the principle carbon bearer becomes C⁺ while in the cold midplane, molecules tend to be frozen onto dust grains (Aikawa et al. 2002; Öberg & Bergin 2021).

It is well known that employing accurate photorates significantly affects the chemical structure of disks (Walsh et al. 2012). Recent synergies of models and observations have shown, for example, that HCN and CN are not as good tracers of UV fields and photodissociation-initiated chemistry in disks as previously assumed (Cazzoletti et al. 2018; Bergner et al. 2021), high UV fluxes appear to be required to replicate C₂H emission features in several disks (Bergner et al. 2019; Bosman et al. 2021), and that many COMs can survive the passage through disks intact but this requires their photoprocesses to be well constrained (Bergner et al. 2021; Booth et al. 2021). Different stellar types at the respective centers of disks have also been shown to influence the disk chemistry where molecules such as HC₃N have been suggested to trace the extent by which the UV field may play an important role in catalyzing the disk chemistry (Bergner et al. 2018).

On the other hand, molecules (and chemistry) can be used to constrain the UV fields in particular regions. For instance, observations of water and other hydrides in high-mass star-forming regions allow us to put constraints on the UV flux from the incumbent protostar, which can be up to a few hundred times the strength of the ISRF (Benz et al. 2016). This is important for constraining the amount of FUV and X rays across the protostellar envelope to trace the full water chemistry. Water chemistry can already be heavily impacted by UV photodissociation in bow-shocks (Tabone et al. 2021) and X-rays have also been
shown to impact interstellar water chemistry (Notsu et al. 2021). The UV chemistry is also an important parameter to trace the chemical evolution of methanol in comet-forming zones around low-mass protostars (Drozdovskaya et al. 2014) and unknown or missing UV chemistry has been invoked to account for H, N, O radical species that models cannot account for (Coutens et al. 2019).

Circumstellar envelopes also possess UV-driven chemistry that originates from asymptotic giant branch (AGB), red giant branch (RGB), and supergiant stars that are subject to large mass loss through their stellar wind. The envelope is irradiated both from the central star and the interstellar radiation field, similar to protoplanetary disks, and at larger radii the shielding from dust and molecules gets less effective leading to greater intensity in photoprocesses (Cernicharo et al. 2001; Woods et al. 2003; Li et al. 2016; Decin 2021). The effect depends mainly on the extinction experienced by the UV radiation which is set by the outflow density and its structure, onset of dust extinction, and the intensity of the radiation governed by the stellar radius and blackbody temperature. In high UV outflows, photodissociation and photoionization are faster than two-body reactions which reduces the outflow to a mostly atomic and ionized state. UV photons from stellar or even planetary companions of AGB outflows have furthermore been shown to be capable of influencing the chemistry deep inside their circumstellar envelopes at low mass-loss rates in a clumpy circumstellar medium (as is observed for several AGB stars). These effects become more significant with increased effective temperatures and lower mass-loss rates (Van de Sande & Millar 2022).

UV photons from our Sun are also important to the atmospheres of the planets and moons in the Solar System. Solar photons are responsible for ionizing molecules such as CO₂, N₂, CO, and O₂ in the upper atmosphere of Mars (Haider et al. 2009). On Venus, the UV radiation from the Sun leads to photoionization that is sufficient to create an ionosphere capable of fending off the solar wind (Russell et al. 2006). In the higher layers of Titan's atmosphere, photoionization produces N⁺, CH₃⁺ (x = 1–4), H⁺ and most abundantly, N₂⁺, which requires more energetic photons to produce than are available in the ISM. Photoionization processes are the principal ion generation process on Titan's dayside and a good agreement is found between data recorded on board the Cassini orbiter and purely photochemical ion chemistry models (Robertson et al. 2009).

In the upper atmospheres of exoplanets such as hot Jupiters, photochemical reactions dominate the upper atmosphere where the UV flux is high and the densities are too low for thermochemical reactions to dominate (Madhusudhan 2019). The UV flux from the host star may also significantly affect thermal inversions in the atmospheres and it is suggested that high stellar UV fluxes may destroy the molecules responsible for the temperature inversions (Knutson et al. 2010). The chemistry in exoplanetary atmospheres is multiplexed and dependent on multiple other factors besides UV-flux such as pressure, temperature and composition (Madhusudhan et al. 2016; Tinetti et al. 2018; Venot et al. 2018a,b).

This paper is structured as follows. Section 2 provides background for the wavelength-dependent cross sections and photoprocesses and give an account of recent experimental and theoretical advancements that have allowed recent cross sections to be determined. Section 2 also gives an account of the radiation fields utilized to compute photodestruction rates in this work and a brief description of the dust and molecular line shielding components utilized to derive shielding functions of the computed photorates. Section 2 concludes with a description of the

cosmic-ray ionization derived photorates and a brief account of the effects of temperature on cross sections and caveats concerning the applicability of the cross sections for exoplanet atmospheres. Section 3 gives an overview of all the updated cross sections in the database. And Sect. 4 is devoted to a discussion of the updates and prospects for the future.

## 2. Methods

### 2.1. Cross sections

The wavelength-dependent photoabsorption cross section, $\sigma(\lambda)$, describes the expected rate of photoabsorption per spectral unit of an isolated molecule or atom in a photon-intensity normalized radiation field. Effectively, the cross section is a descriptor of the complex photoexcitation dynamics in molecules that are accessed via electronically excited states. Having the dimension of an area (frequently in the units of $cm^2$ or Mb which equals $10^{-18} cm^2$), the cross section can be related to the optical depth ($\tau$) via $\tau = N\sigma$, where N is the column density.

After absorbing a VUV photon, a molecule in an electronically excited state may decay by several channels, each of which needs to be accounted for and quantified for an appropriate description of the VUV-induced photodynamics. For an electronically excited polyatomic molecule ABC*, the different processes include: (i) photodissociation (ABC* $\rightarrow$ A + BC/AB + C/AC + B), photoionization (ABC* $\rightarrow$ ABC⁺ + e⁻), and nondestructive emission (ABC* $\rightarrow$ ABC + hν). Photodissociation processes relevant to astrophysics and astrochemistry have been outlined in detail previously and we refer the reader to previous overviews and reviews (van Dishoeck 1988; Kirby & Van Dishoeck 1989; van Dishoeck & Visser 2015; Heays et al. 2017).

Briefly, photodissociation processes are split into the following: (i) direct dissociation which generally yields a broad absorption cross section, typically peaking at values of $10^{-18}$–$10^{-17} cm^2$; as well as (ii) direct and (iii) indirect predissociation, which typically yield more structured cross sections typifying the vibrational profiles of the electronically (bound) excited states which decay via state interactions with dissociative states. Typical intensities of predissociative states are usually higher than that of (directly) dissociative states and typical values are around $10^{-16} cm^2$, but these are significantly varied. Finally, (iv) spontaneous radiative dissociation is where a bound state radiates back into the vibrational continuum of a lower state with line-dependent probability. For H₂, this is the dominant photodissociation pathway (Stecher & Williams 1967) and peak cross sections may reach $10^{-14} cm^2$ over a width of less than 0.1 nm, making the cross section highly structured.

Since many of the database updates outlined below concern new photoionization cross sections, it is worth formulating valence photoionization processes a bit further noting that several literature reviews of valence photoionization processes are available (Hatano 1999a,b, 2001; Dyke 2019). The excitation processes that are most relevant above the ionization energy (IE) of a molecule AB can be summarized as follows:

$$AB + h\nu \rightarrow AB^{+} + e^{-} \quad (i) \text{ Direct ionization}$$

$$AB + h\nu \rightarrow A^{+} + B + e^{-} \quad (ii) \text{ Dissociative ionization}$$

$$AB + h\nu \rightarrow AB^{**} \quad (iii) \text{ Superexcitation}$$

$$AB^{**} \rightarrow AB^{+} + e^{-} \quad (iv) \text{ Autoionization}$$

$$AB^{**} \rightarrow A + B \quad (v) \text{ Dissociation}$$

$$AB^{**} \rightarrow \dots \quad (vi) \text{ Others.}$$

When a molecule AB receives energy which is larger than its IE, AB may be directly ionized (AB⁺) or it could be excited to form (AB**) which was named by Platzman as a
shown to impact interstellar water chemistry (Notsu et al. 2021). The UV chemistry is also an important parameter to trace the chemical evolution of methanol in comet-forming zones around low-mass protostars (Drozdovskaya et al. 2014) and unknown or missing UV chemistry has been invoked to account for H, N, O radical species that models cannot account for (Coutens et al. 2019).

Circumstellar envelopes also possess UV-driven chemistry that originates from asymptotic giant branch (AGB), red giant branch (RGB), and supergiant stars that are subject to large mass loss through their stellar wind. The envelope is irradiated both from the central star and the interstellar radiation field, similar to protoplanetary disks, and at larger radii the shielding from dust and molecules gets less effective leading to greater intensity in photoprocesses (Cernicharo et al. 2001; Woods et al. 2003; Li et al. 2016; Decin 2021). The effect depends mainly on the extinction experienced by the UV radiation which is set by the outflow density and its structure, onset of dust extinction, and the intensity of the radiation governed by the stellar radius and blackbody temperature. In high UV outflows, photodissociation and photoionization are faster than two-body reactions which reduces the outflow to a mostly atomic and ionized state. UV photons from stellar or even planetary companions of AGB outflows have furthermore been shown to be capable of influencing the chemistry deep inside their circumstellar envelopes at low mass-loss rates in a clumpy circumstellar medium (as is observed for several AGB stars). These effects become more significant with increased effective temperatures and lower mass-loss rates (Van de Sande & Millar 2022).

UV photons from our Sun are also important to the atmospheres of the planets and moons in the Solar System. Solar photons are responsible for ionizing molecules such as CO₂, N₂, CO, and O₂ in the upper atmosphere of Mars (Haider et al. 2009). On Venus, the UV radiation from the Sun leads to photoionization that is sufficient to create an ionosphere capable of fending off the solar wind (Russell et al. 2006). In the higher layers of Titan's atmosphere, photoionization produces N⁺, CH₃⁺ (x = 1–4), H⁺ and most abundantly, N₂⁺, which requires more energetic photons to produce than are available in the ISM. Photoionization processes are the principal ion generation process on Titan's dayside and a good agreement is found between data recorded on board the Cassini orbiter and purely photochemical ion chemistry models (Robertson et al. 2009).

In the upper atmospheres of exoplanets such as hot Jupiters, photochemical reactions dominate the upper atmosphere where the UV flux is high and the densities are too low for thermochemical reactions to dominate (Madhusudhan 2019). The UV flux from the host star may also significantly affect thermal inversions in the atmospheres and it is suggested that high stellar UV fluxes may destroy the molecules responsible for the temperature inversions (Knutson et al. 2010). The chemistry in exoplanetary atmospheres is multiplexed and dependent on multiple other factors besides UV-flux such as pressure, temperature and composition (Madhusudhan et al. 2016; Tinetti et al. 2018; Venot et al. 2018a,b).

This paper is structured as follows. Section 2 provides background for the wavelength-dependent cross sections and photoprocesses and give an account of recent experimental and theoretical advancements that have allowed recent cross sections to be determined. Section 2 also gives an account of the radiation fields utilized to compute photodestruction rates in this work and a brief description of the dust and molecular line shielding components utilized to derive shielding functions of the computed photorates. Section 2 concludes with a description of the

cosmic-ray ionization derived photorates and a brief account of the effects of temperature on cross sections and caveats concerning the applicability of the cross sections for exoplanet atmospheres. Section 3 gives an overview of all the updated cross sections in the database. And Sect. 4 is devoted to a discussion of the updates and prospects for the future.

## 2. Methods

### 2.1. Cross sections

The wavelength-dependent photoabsorption cross section, $\sigma(\lambda)$, describes the expected rate of photoabsorption per spectral unit of an isolated molecule or atom in a photon-intensity normalized radiation field. Effectively, the cross section is a descriptor of the complex photoexcitation dynamics in molecules that are accessed via electronically excited states. Having the dimension of an area (frequently in the units of $cm^2$ or Mb which equals $10^{-18} cm^2$), the cross section can be related to the optical depth ($\tau$) via $\tau = N\sigma$, where N is the column density.

After absorbing a VUV photon, a molecule in an electronically excited state may decay by several channels, each of which needs to be accounted for and quantified for an appropriate description of the VUV-induced photodynamics. For an electronically excited polyatomic molecule ABC*, the different processes include: (i) photodissociation (ABC* $\rightarrow$ A + BC/AB + C/AC + B), photoionization (ABC* $\rightarrow$ ABC⁺ + e⁻), and nondestructive emission (ABC* $\rightarrow$ ABC + hν). Photodissociation processes relevant to astrophysics and astrochemistry have been outlined in detail previously and we refer the reader to previous overviews and reviews (van Dishoeck 1988; Kirby & Van Dishoeck 1989; van Dishoeck & Visser 2015; Heays et al. 2017).

Briefly, photodissociation processes are split into the following: (i) direct dissociation which generally yields a broad absorption cross section, typically peaking at values of $10^{-18}$–$10^{-17} cm^2$; as well as (ii) direct and (iii) indirect predissociation, which typically yield more structured cross sections typifying the vibrational profiles of the electronically (bound) excited states which decay via state interactions with dissociative states. Typical intensities of predissociative states are usually higher than that of (directly) dissociative states and typical values are around $10^{-16} cm^2$, but these are significantly varied. Finally, (iv) spontaneous radiative dissociation is where a bound state radiates back into the vibrational continuum of a lower state with line-dependent probability. For H₂, this is the dominant photodissociation pathway (Stecher & Williams 1967) and peak cross sections may reach $10^{-14} cm^2$ over a width of less than 0.1 nm, making the cross section highly structured.

Since many of the database updates outlined below concern new photoionization cross sections, it is worth calculating valence photoionization processes a bit further noting that several literature reviews of valence photoionization processes are available (Hatano 1999a,b, 2001; Dyke 2019). The excitation processes that are most relevant above the ionization energy (IE) of a molecule AB can be summarized as follows:

$$AB + h\nu \rightarrow AB^{+} + e^{-} \quad (i) \text{ Direct ionization}$$

$$AB + h\nu \rightarrow A^{+} + B + e^{-} \quad (ii) \text{ Dissociative ionization}$$

$$AB + h\nu \rightarrow AB^{**} \quad (iii) \text{ Superexcitation}$$

$$AB^{**} \rightarrow AB^{+} + e^{-} \quad (iv) \text{ Autoionization}$$

$$AB^{**} \rightarrow A + B \quad (v) \text{ Dissociation}$$

$$AB^{**} \rightarrow \dots \quad (vi) \text{ Others.}$$

When a molecule AB receives energy which is larger than its IE, AB may be directly ionized (AB⁺) or it could be excited to form (AB**) which was named by Platzman as a
superexcited molecule (Platzman 1962). If the absorbed photon energy exceeds the sum of the IE and the dissociation threshold of the ion, the molecule can undergo dissociative photoionization ($A^+ + B$).

The superexcited molecule (AB**) can ionize (AB** → AB⁺ + e⁻), which gives rise to autoionizing resonances which typically manifest as strong and discrete peaks in photoionization cross sections. Most superexcited states are assigned to high Rydberg states which are vibrationally (and/or rotationally), doubly, or inner-core excited, and converge to each of the electronically excited states of the ion. Superexcited states can also lead to neutral dissociation (AB** → A + B) as well as ion-pair formation (AB** → A⁺ + B⁻). It should be noted that extensive studies of ion-pair formation have revealed that its cross sections are much smaller than those of photodissociation and (dissociative) photoionization (Mitsuke et al. 1993a,b; Yoshida & Mitsuke 1994, 1996). Dissociation into neutral fragments is competing with autoionization, however, and is of great importance in the observed decay of each state-assigned superexcited molecule (Hatano 1999b).

This competition can be quantified by the photoionization efficiency parameter (or ionization quantum yield), η(λ), which serves as an index for the degree of competition between ionization and dissociation. The η(λ) parameter is often assumed to be unity above the IE threshold but this is demonstrably not the case as it often does not reach unity as high as 10 eV above the first ionization potential (Hatano 2001). Secondly, η(λ) displays significant wavelength-dependent variations which depend on the molecule's electronic structure (Hatano 1999a, 2001).

## 2.2. Experimental advances: Photoionization cross sections

During the past decade or so, some significant experimental developments have been successfully utilized to characterize physical chemical characteristics of astronomically relevant molecules, in particular open-shell radical species. In many cases, these instrumental advances have been achieved at (or in collaboration with) synchrotron facilities where a high flux, variable polarization, and tunable wavelengths are accessible in the VUV range. While recent advances with tunable VUV table top light sources have also been spearheaded in recording VUV photodissociation branching ratios (Gao & Ng 2019) and zero-kinetic energy electron (ZEKE) spectroscopy (Harper et al. 2022), the bandwidth achieved with lasers is still too narrow to record absolute cross sections, and their use is better suited at discrete wavelengths to obtain single absolute points which can be used to normalize synchrotron yields.

Studying such reactive species with photoelectron spectroscopy using VUV radiation from an inert gas low-pressure discharge photon source used to be an industry standard (Dyke 1987, 2019). However, using monochromized synchrotron radiation as the photon source allows more information to be obtained on molecular ionic states and the associated photoionization dynamics. Hence it is possible to identify autoionizing resonances, perform angularly resolved photoelectron measurements, and relative band intensities as a function of wavelength, and threshold (or slow) photoelectron spectra (TPES/SPES), can be obtained which involve collecting the near-zero kinetic energy electrons, thus uncovering the spectral fingerprints of cationic states in high resolution (Poully et al. 2010). Among the most prominent experimental techniques employing these state-of-the-art techniques is the double-imaging photoelectron photoion coincidence (i²PEPICO) spectroscopic method (Baer & Tuckett 2017; Hochlaf 2017). This technique involves photoionization of

molecules and the acceleration of nascent photoelectrons and photoions in opposite directions with a DC electric field. The photoelectrons pass through a set of lenses for velocity map imaging (VMI; Eppink & Parker 1997), while the photoions pass through a mass spectrometer and both sets of ions are detected with imaging plates where the electrons and ions are detected in coincidence (Continetti 2001), meaning that for each electron signal detected on the electron side, there is a corresponding cation signal detected on the MS-TOF side where both particles originated from the same photoionization event (Osborn et al. 2008; Taatjes et al. 2008; Garcia et al. 2013).

The i²PEPICO technique allows for multiplex detection schemes and the separation of structural isomers by investigating the TPES/SPES that are obtained by integrating the generated photoelectrons with the lowest kinetic energies (Wu et al. 2019). While this isomer separation is expansively applicable to molecular spectra and has been utilized in the detection of multiple molecular species of a particular mass in complex combustion mixtures (Krueger et al. 2014; Felsmann et al. 2015, 2016; Pieper et al. 2018; Hemberger et al. 2020, 2022), including the formation of two- and three-ringed polycyclic aromatic hydrocarbons (PAHs; Mercier et al. 2020; Hemberger et al. 2021), there is a caveat. Namely, the ultimate resolution of TPES/SPES, in general, does not always allow for isomeric discrimination owing to the similar potential energy surfaces between the neutral and cationic forms of some molecules, which leads to similarities in the recorded TPES/SPES of some isomers. Hence, there are larger molecules that may have to be disentangled through the excited cationic states. Examples include the anilino and 4-picolyl radicals which are isomers with the same molecular formula (C₆H₆N) but different geometries (Reusch et al. 2017; Hrodmarsson et al. 2019b). However, these instances of similarities in the TPES/SPES of isomers are very rare in the literature so far.

To record the absolute photoionization cross sections of radicals with the i²PEPICO technique there are a few methods available that have been successfully employed at the DESIRS beamline at the SOLEIL synchrotron (Nahon et al. 2012; Garcia et al. 2013; Tang et al. 2015b), the Chemical Dynamics beamline at the ALS (Heimann et al. 1997), and the Vacuum Ultraviolet Beamline at the SLS (Johnson et al. 2009; Bodi et al. 2012). On the DESIRS beamline at SOLEIL, a flow-tube reactor has been coupled to the on-site i²PEPICO instrument (Garcia et al. 2015) while both at the Chemical Dynamics beamline at ALS and the Vacuum Ultraviolet Beamline at SLS, different types of reactors or pyrolysis sources employing a series of gas phase reaction schemes have allowed the recording of absolute photoionization cross sections of multiple species (Taatjes et al. 2008; Osborn et al. 2008; Holzmeier et al. 2016; Rosch et al. 2021; Pan et al. 2022).

The flow-tube contraption at DESIRS employs a MW discharge to create reactive F radicals that effectively abstract H-atoms from appropriate precursors to form the radicals of interest. The photoionization efficiency (or the total ion yield) is then measured by collecting all the coincident ion events for a particular mass species and is integrated as a function of photon energy or wavelength. To obtain the absolute photoionization cross section, a series of measurements are performed where the decrease in the mass signal of a parent species is monitored as well as the mass peak increase in the radical species resulting from the H-abstraction. This allows us to write the ratio of the photoionization cross section of the parent and radical as the ratio of the mass decrease of the parent and the mass increase of the radical (Hrodmarsson et al. 2019b). Thus, the absolute
superexcited molecule (Platzman 1962). If the absorbed photon energy exceeds the sum of the IE and the dissociation threshold of the ion, the molecule can undergo dissociative photoionization ($A^+ + B$).

The superexcited molecule (AB**) can ionize (AB** → AB⁺ + e⁻), which gives rise to autoionizing resonances which typically manifest as strong and discrete peaks in photoionization cross sections. Most superexcited states are assigned to high Rydberg states which are vibrationally (and/or rotationally), doubly, or inner-core excited, and converge to each of the electronically excited states of the ion. Superexcited states can also lead to neutral dissociation (AB** → A + B) as well as ion-pair formation (AB** → A⁺ + B⁻). It should be noted that extensive studies of ion-pair formation have revealed that its cross sections are much smaller than those of photodissociation and (dissociative) photoionization (Mitsuke et al. 1993a,b; Yoshida & Mitsuke 1994, 1996). Dissociation into neutral fragments is competing with autoionization, however, and is of great importance in the observed decay of each state-assigned superexcited molecule (Hatano 1999b).

This competition can be quantified by the photoionization efficiency parameter (or ionization quantum yield), η(λ), which serves as an index for the degree of competition between ionization and dissociation. The η(λ) parameter is often assumed to be unity above the IE threshold but this is demonstrably not the case as it often does not reach unity as high as 10 eV above the first ionization potential (Hatano 2001). Secondly, η(λ) displays significant wavelength-dependent variations which depend on the molecule's electronic structure (Hatano 1999a, 2001).

## 2.2. Experimental advances: Photoionization cross sections

During the past decade or so, some significant experimental developments have been successfully utilized to characterize physical chemical characteristics of astronomically relevant molecules, in particular open-shell radical species. In many cases, these instrumental advances have been achieved at (or in collaboration with) synchrotron facilities where a high flux, variable polarization, and tunable wavelengths are accessible in the VUV range. While recent advances with tunable VUV table top light sources have also been spearheaded in recording VUV photodissociation branching ratios (Gao & Ng 2019) and zero-kinetic energy electron (ZEKE) spectroscopy (Harper et al. 2022), the bandwidth achieved with lasers is still too narrow to record absolute cross sections, and their use is better suited at discrete wavelengths to obtain single absolute points which can be used to normalize synchrotron yields.

Studying such reactive species with photoelectron spectroscopy using VUV radiation from an inert gas low-pressure discharge photon source used to be an industry standard (Dyke 1987, 2019). However, using monochromized synchrotron radiation as the photon source allows more information to be obtained on molecular ionic states and the associated photoionization dynamics. Hence it is possible to identify autoionizing resonances, perform angularly resolved photoelectron measurements, and relative band intensities as a function of wavelength, and threshold (or slow) photoelectron spectra (TPES/SPES), can be obtained which involve collecting the near-zero kinetic energy electrons, thus uncovering the spectral fingerprints of cationic states in high resolution (Pouilly et al. 2010). Among the most prominent experimental techniques employing these state-of-the-art techniques is the double-imaging photoelectron photoion coincidence (i²PEPICO) spectroscopic method (Baer & Tuckett 2017; Hochlaf 2017). This technique involves photoionization of

molecules and the acceleration of nascent photoelectrons and photoions in opposite directions with a DC electric field. The photoelectrons pass through a set of lenses for velocity map imaging (VMI; Eppink & Parker 1997), while the photoions pass through a mass spectrometer and both sets of ions are detected with imaging plates where the electrons and ions are detected in coincidence (Continetti 2001), meaning that for each electron signal detected on the electron side, there is a corresponding cation signal detected on the MS-TOF side where both particles originated from the same photoionization event (Osborn et al. 2008; Taatjes et al. 2008; Garcia et al. 2013).

The i²PEPICO technique allows for multiplex detection schemes and the separation of structural isomers by investigating the TPES/SPES that are obtained by integrating the generated photoelectrons with the lowest kinetic energies (Wu et al. 2019). While this isomer separation is expansively applicable to molecular spectra and has been utilized in the detection of multiple molecular species of a particular mass in complex combustion mixtures (Krueger et al. 2014; Felsmann et al. 2015, 2016; Pieper et al. 2018; Hemberger et al. 2020, 2022), including the formation of two- and three-ringed polycyclic aromatic hydrocarbons (PAHs; Mercier et al. 2020; Hemberger et al. 2021), there is a caveat. Namely, the ultimate resolution of TPES/SPES, in general, does not always allow for isomeric discrimination owing to the similar potential energy surfaces between the neutral and cationic forms of some molecules, which leads to similarities in the recorded TPES/SPES of some isomers. Hence, there are larger molecules that may have to be disentangled through the excited cationic states. Examples include the anilino and 4-picolyl radicals which are isomers with the same molecular formula (C₆H₆N) but different geometries (Reusch et al. 2017; Hrodmarsson et al. 2019b). However, these instances of similarities in the TPES/SPES of isomers are very rare in the literature so far.

To record the absolute photoionization cross sections of radicals with the i²PEPICO technique there are a few methods available that have been successfully employed at the DESIRS beamline at the SOLEIL synchrotron (Nahon et al. 2012; Garcia et al. 2013; Tang et al. 2015b), the Chemical Dynamics beamline at the ALS (Heimann et al. 1997), and the Vacuum Ultraviolet Beamline at the SLS (Johnson et al. 2009; Bodi et al. 2012). On the DESIRS beamline at SOLEIL, a flow-tube reactor has been coupled to the on-site i²PEPICO instrument (Garcia et al. 2015) while both at the Chemical Dynamics beamline at ALS and the Vacuum Ultraviolet Beamline at SLS, different types of reactors or pyrolysis sources employing a series of gas phase reaction schemes have allowed the recording of absolute photoionization cross sections of multiple species (Taatjes et al. 2008; Osborn et al. 2008; Holzmeier et al. 2016; Rosch et al. 2021; Pan et al. 2022).

The flow-tube contraption at DESIRS employs a MW discharge to create reactive F radicals that effectively abstract H-atoms from appropriate precursors to form the radicals of interest. The photoionization efficiency (or the total ion yield) is then measured by collecting all the coincident ion events for a particular mass species and is integrated as a function of photon energy or wavelength. To obtain the absolute photoionization cross section, a series of measurements are performed where the decrease in the mass signal of a parent species is monitored as well as the mass peak increase in the radical species resulting from the H-abstraction. This allows us to write the ratio of the photoionization cross section of the parent and radical as the ratio of the mass decrease of the parent and the mass increase of the radical (Hrodmarsson et al. 2019b). Thus, the absolute
photoionization cross section of the radical can be isolated with the caveat that the accuracy of that cross section is (mostly) limited to that of the parent.

The real breakthrough from coupling the flow-tube to the i²PEPICO scheme to study radicals was twofold. Firstly, ion imaging allows not only the detection of dissociative ionization, but also filtering out the background when using a molecular beam (Tang et al. 2015b). Secondly, the issue of dissociative ionization of the precursor can be circumvented to a larger degree in comparison to using pyrolysis and photolysis to produce the radicals from suitable precursors, for instance, halogenated carbohydrates such as fluoro-, chloro-, bromo-, or iodo-hydrocarbons to produce hydrocarbon radicals with either pyrolysis or photolysis (for example, see Robinson et al. 2003; Gans et al. 2010, and references therein). For instance, the appearance energy of the dissociative ionization of CH₄ to produce CH₃⁺ is around 14.3 eV in comparison to 9.8 eV which is the ionization energy of the methyl radical (CH₃). That means that there is a window spanning over 4 eV where the ionization cross section of CH₃ can be recorded without interference from the dissociative ionization of the CH₄ precursor. In comparison to the aforementioned halomethanes, only a less than 2 eV window is available to study the photoionization of CH₃ before CH₃⁺ signals from the dissociative ionization of the parent, CH₃X (X = F, Cl, Br, I), start mixing with the CH₃ signals (Gans et al. 2010; Tang et al. 2014, 2015a, 2016).

At the Chemical Dynamics beamline at the ALS, the preferred method of forming the radicals of interest involves laser flash photolysis of appropriate precursors in a slow flow reactor. Photolysis is achieved with an excimer laser propagated along the reactor axis, collinear with the gas flow. Products are analyzed with a Multiplexed Photoionization Mass Spectrometer (MPIMS). The absolute photoionization cross sections can then be obtained relative to a reference species using gas mixtures with known concentrations of both species (Dodson et al. 2015).

### 2.3. Theoretical advances: Photodissociation cross sections

All the fundamental information about a molecule's photodestruction can be revealed by the molecule's wavefunction, $\psi$, which is the solution of the time-independent Schrödinger equation

$$H\Psi(x, R) = E\Psi(x, R), \quad (1)$$

where $x$ denotes the spatial and spin coordinates of the $n$ electrons in the molecule and $R$ denotes the positions of all $N$ nuclei in the molecule. The total Hamiltonian, $H$, consists of the sum of the kinetic energy operators of the nuclei $\alpha$ and the electrons and all their potential energies due to mutual interactions. As the mass of atomic nuclei is much larger than that of electrons, the Born-Oppenheimer (BO) approximation is frequently used which assumes that the movement of the nuclei with respect to the electrons is negligible. This leads to the separation of nuclear and electronic coordinates:

$$\Psi(x, R) = \Psi^{\text{el}}(x, R)\Psi^{\text{nuc}}(x, R). \quad (2)$$

This separation allows the electronic eigenvalues to be extracted via:

$$H^{\text{el}}(x, R)\Psi^{\text{el}}(x, R) = E^{\text{el}}(x, R)\Psi^{\text{el}}(x, R), \quad (3)$$

where the electronic energies ($E^{\text{el}}$) represent the potential energy curves or surfaces of the molecular system. When rovibrational energy levels of a diatomic molecule in a $^1\Sigma^±$ electronic state

are treated, the solution represents a well-studied mathematical problem (Simon 2000) for which many efficient numerical methods are available (Yurchenko et al. 2016 and references therein), most notably the iterative Cooley-Numerov method (Numerov 1924; Cooley 1961; Cashion 1963) which is used in the program LEVEL from Le Roy (2017).

The situation is, however, usually much more complicated. When multiple excited states of varying symmetries are present, there are several sources of angular momentum couplings that need to be considered, such as electronic spin, electron orbital momentum, and molecular rotational motion. Additionally, effects due to hyperfine structure caused by nuclear spin angular momentum and external fields, either electric or magnetic, must be accounted for (Qu et al. 2022) as well as some additional consideration in the case of open shell (radical) diatomics that include transition metal atoms (Tennyson et al. 2016a). These multitudes of state interactions cause the BO approximation to break down and it becomes impossible to treat each electronic state in isolation. A multitude of studies investigating rovibrational electronic state-to-state interactions in diatomics and how they influence the photodissociation dynamics exist and have been compiled in various books (see, for instance, the works of Herzberg 1950; Lefebvre-Brion & Field 1986, 2004; and Brown & Carrington 2003).

Recently a new program, DUO, was developed to solve the coupled nuclear motion problem for diatomic molecules (Yurchenko et al. 2016). The main method of solving the radial equation is called discrete variable representation (DVR) which has been independently applied to the one-dimensional Schrödinger equation (Guardiola & Ros 1982b,a). In this method the R coordinate is truncated to an interval and discretized in a grid of $N_p$ uniformly spaced points. This transforms the Schrödinger equation to an ordinary matrix eigenvalue problem where the $N_p \times N_p$ real symmetric Hamiltonian matrix is diagonalized. This method gives a very fast convergence of the calculated energies and wave functions with respect to the number of grid points $N_p$.

By coupling the potential energy curves from DUO with another program developed by the same group, ExoCross (Yurchenko et al. 2018), photodissociation cross sections at various temperatures can be obtained (Pezzella et al. 2021). This methodology has been applied to HF and HCl to obtain high-temperature VUV photodissociation cross sections (Pezzella et al. 2022). This work was very quickly revisited by a different group who used a different transition dipole moment in dealing with one of the electronic transitions in HCl which led to significant differences in the cross sections at high temperatures toward longer wavelengths (Qin et al. 2022). The reasoning behind this choice is that in the work by Pezzella et al., they used a tabulated TDM value published previously (Engin et al. 2012) which appears to have a typographical error. Overall, the results are consistent with what was previously included in the database.

Other notable results making use of DUO include the updated photodissociation cross sections of CS (Xu et al. 2019). In this work, the authors used a coupled-channel Schrödinger equation (CSE) to investigate the predissociation mechanisms of CS where over twenty electronic states were accounted for, but special attention was paid to the $B^1\Sigma^+$ and $C^1\Sigma^+$ states which are found to be strongly predissociative. To calculate the photodissociation cross section they employed the program PyDiatomic (Gibson 2016) which also uses the Numerov method (Johnson 1978).

It is worth briefly noting some recent advances concerning photoionization cross sections. Provided that the electronic
photoionization cross section of the radical can be isolated with the caveat that the accuracy of that cross section is (mostly) limited to that of the parent.

The real breakthrough from coupling the flow-tube to the i²PEPICO scheme to study radicals was twofold. Firstly, ion imaging allows not only the detection of dissociative ionization, but also filtering out the background when using a molecular beam (Tang et al. 2015b). Secondly, the issue of dissociative ionization of the precursor can be circumvented to a larger degree in comparison to using pyrolysis and photolysis to produce the radicals from suitable precursors, for instance, halogenated carbohydrates such as fluoro-, chloro-, bromo-, or iodo-hydrocarbons to produce hydrocarbon radicals with either pyrolysis or photolysis (for example, see Robinson et al. 2003; Gans et al. 2010, and references therein). For instance, the appearance energy of the dissociative ionization of CH₄ to produce CH₃⁺ is around 14.3 eV in comparison to 9.8 eV which is the ionization energy of the methyl radical (CH₃). That means that there is a window spanning over 4 eV where the ionization cross section of CH₃ can be recorded without interference from the dissociative ionization of the CH₄ precursor. In comparison to the aforementioned halomethanes, only a less than 2 eV window is available to study the photoionization of CH₃ before CH₃⁺ signals from the dissociative ionization of the parent, CH₃X (X = F, Cl, Br, I), start mixing with the CH₃ signals (Gans et al. 2010; Tang et al. 2014, 2015a, 2016).

At the Chemical Dynamics beamline at the ALS, the preferred method of forming the radicals of interest involves laser flash photolysis of appropriate precursors in a slow flow reactor. Photolysis is achieved with an excimer laser propagated along the reactor axis, collinear with the gas flow. Products are analyzed with a Multiplexed Photoionization Mass Spectrometer (MPIMS). The absolute photoionization cross sections can then be obtained relative to a reference species using gas mixtures with known concentrations of both species (Dodson et al. 2015).

## 2.3. Theoretical advances: Photodissociation cross sections

All the fundamental information about a molecule's photodestruction can be revealed by the molecule's wavefunction, $\psi$, which is the solution of the time-independent Schrödinger equation

$$H\Psi(x, R) = E\Psi(x, R), \qquad (1)$$

where $x$ denotes the spatial and spin coordinates of the $n$ electrons in the molecule and $R$ denotes the positions of all $N$ nuclei in the molecule. The total Hamiltonian, $H$, consists of the sum of the kinetic energy operators of the nuclei $\alpha$ and the electrons and all their potential energies due to mutual interactions. As the mass of atomic nuclei is much larger than that of electrons, the Born-Oppenheimer (BO) approximation is frequently used which assumes that the movement of the nuclei with respect to the electrons is negligible. This leads to the separation of nuclear and electronic coordinates:

$$\Psi(x, R) = \Psi^{\text{el}}(x, R)\Psi^{\text{nuc}}(x, R). \qquad (2)$$

This separation allows the electronic eigenvalues to be extracted via:

$$H^{\text{el}}(x, R)\Psi^{\text{el}}(x, R) = E^{\text{el}}(x, R)\Psi^{\text{el}}(x, R), \qquad (3)$$

where the electronic energies ($E^{\text{el}}$) represent the potential energy curves or surfaces of the molecular system. When rovibrational energy levels of a diatomic molecule in a $^1\Sigma^±$ electronic state

are treated, the solution represents a well-studied mathematical problem (Simon 2000) for which many efficient numerical methods are available (Yurchenko et al. 2016 and references therein), most notably the iterative Cooley-Numerov method (Numerov 1924; Cooley 1961; Cashion 1963) which is used in the program LEVEL from Le Roy (2017).

The situation is, however, usually much more complicated. When multiple excited states of varying symmetries are present, there are several sources of angular momentum couplings that need to be considered, such as electronic spin, electron orbital momentum, and molecular rotational motion. Additionally, effects due to hyperfine structure caused by nuclear spin angular momentum and external fields, either electric or magnetic, must be accounted for (Qu et al. 2022) as well as some additional consideration in the case of open shell (radical) diatomics that include transition metal atoms (Tennyson et al. 2016a). These multitudes of state interactions cause the BO approximation to break down and it becomes impossible to treat each electronic state in isolation. A multitude of studies investigating rovibrational electronic state-to-state interactions in diatomics and how they influence the photodissociation dynamics exist and have been compiled in various books (see, for instance, the works of Herzberg 1950; Lefebvre-Brion & Field 1986, 2004; and Brown & Carrington 2003).

Recently a new program, DUO, was developed to solve the coupled nuclear motion problem for diatomic molecules (Yurchenko et al. 2016). The main method of solving the radial equation is called discrete variable representation (DVR) which has been independently applied to the one-dimensional Schrödinger equation (Guardiola & Ros 1982b,a). In this method the R coordinate is truncated to an interval and discretized in a grid of $N_p$ uniformly spaced points. This transforms the Schrödinger equation to an ordinary matrix eigenvalue problem where the $N_p \times N_p$ real symmetric Hamiltonian matrix is diagonalized. This method gives a very fast convergence of the calculated energies and wave functions with respect to the number of grid points $N_p$.

By coupling the potential energy curves from DUO with another program developed by the same group, ExoCross (Yurchenko et al. 2018), photodissociation cross sections at various temperatures can be obtained (Pezzella et al. 2021). This methodology has been applied to HF and HCl to obtain high-temperature VUV photodissociation cross sections (Pezzella et al. 2022). This work was very quickly revisited by a different group who used a different transition dipole moment in dealing with one of the electronic transitions in HCl which led to significant differences in the cross sections at high temperatures toward longer wavelengths (Qin et al. 2022). The reasoning behind this choice is that in the work by Pezzella et al., they used a tabulated TDM value published previously (Engin et al. 2012) which appears to have a typographical error. Overall, the results are consistent with what was previously included in the database.

Other notable results making use of DUO include the updated photodissociation cross sections of CS (Xu et al. 2019). In this work, the authors used a coupled-channel Schrödinger equation (CSE) to investigate the predissociation mechanisms of CS where over twenty electronic states were accounted for, but special attention was paid to the $B^1\Sigma^+$ and $C^1\Sigma^+$ states which are found to be strongly predissociative. To calculate the photodissociation cross section they employed the program PyDiatomic (Gibson 2016) which also uses the Numerov method (Johnson 1978).

It is worth briefly noting some recent advances concerning photoionization cross sections. Provided that the electronic
structure is known exactly, molecular cross sections can be calculated as described above, but this is only the case for atoms and diatomics. For larger molecules, other approximating methods are required. At photon energies below 30 eV (or above 41 nm), the additivity of atomic photoionization cross sections overestimates the molecular ionization cross sections considerably. Previously, a model inspired by the classical and quantum mechanical sum rules of oscillator strengths has been used to describe photoabsorption and photoionization cross sections which were accurate to 20% on average, for a number of (closed-shell) molecules (Bobeldijk et al. 1994).

More recently, advances using the XCHEM methodology (Marante et al. 2017a,b; González-Vázquez et al. 2023) have not only provided great accuracy in the calculation of total and partial photoionization cross sections, but also photoelectron angular distributions and asymmetry parameters. The basic concept of XCHEM involves using a hybrid Gaussian-B-spline basis (GABS; Marante et al. 2014) combining the usual basis used in bound state calculations, but unsuited to describe the continuum, with a B-spline basis that provides a good description of the highly oscillating continuum wave functions. Besides applications to atomic and diatomic species, it has now been successfully applied to a triatomic molecule, namely H₂O (Fernández-Milán et al. 2023).

An interesting future avenue that could expedite experimentally and theoretically obtained cross sections is the use of machine learning algorithms. Recently, machine learning methods were used in combination with differential absorption spectroscopic methods in the VUV to develop predictive capabilities for inferring molecular structure from absorption spectra (Doner et al. 2022). By analyzing 102 absorption spectra of organic molecules such as alkanes, alkenes, ethers, and alcohols, the authors found that optimal determination of molecular structure using machine learning methods is strongly dependent on the absorption region in question. The work provides separate learning models for each molecular classification scheme which enables the identification of multifunctional species with isomer-resolved speciation. The application of procedures such as these could significantly expediate cross section data for the dozens of new molecules that are detected annually in space at the time of writing.

## 2.4. Radiation fields

The rate of photodissociation and photoionization (s⁻¹) per molecule or atom which is exposed to a radiation field of UV radiation is calculated thusly:

$$ \int \sigma(\lambda)I(\lambda)d\lambda \qquad (4) $$

where σ(λ) is the wavelength-dependent cross section in question, and I(λ) is the wavelength-dependent UV radiation field intensity summed over all coincidence angles. The radiation fields used are identical to those used previously (Heays et al. 2017) so only a brief summary follows here.

A total of nine different radiation fields have been used with the updated cross sections to calculate photorates to exemplify the variability in photodestruction in differing interstellar environs. The radiation fields utilized are the interstellar radiation field (ISRF) of Draine (1978), the Galactic radiation field estimate of Mathis et al. (1983), blackbody emission spectra at 4000 K, 10 000 K and 20 000 K, the Lyman-α line, the solar emission spectrum (Woods et al. 1996; Curdt et al. 2001),

the TW Hya radiation field (France et al. 2014), and a cosmic ray induced UV radiation field which is described in detail below. All radiation fields are normalized to match the energy intensity ($\int hcI(\lambda)d\lambda/\lambda$) of the Draine field integrated between 91.2 and 200 nm, that is, $2.6 \times 10^{-10} \text{ W cm}^{-2}$. The integrated fluxes of the radiation fields used to compute the photorates when using a 0.001 nm grid are provided in Table A.1 along with the normalization factors required.

## 2.5. Dust and line shielding

The last database update included shielding functions and gave a detailed overview of the formulations accounting for dust and line shielding (Heays et al. 2017). These calculations are also performed for the updated cross sections, and we present a brief overview of the calculations but refer to the previous work by Heays et al. for a more detailed discussion.

Molecules embedded inside interstellar clouds, protoplanetary disks or other such objects with large densities and a high dust content, are at least partially shielded from VUV radiation. Equation (4) gave the unattenuated photodestruction rate and so to account for the shielding materials in these objects we recalculate the rate as:

$$ \int \sigma^{pd}(\lambda) \exp[-\tau_{\text{dust}}(\lambda, N_{\text{H}+2\text{H}_2}) - \sum_{x=\text{H},\text{H}_2,\text{self}} N_X \sigma_X^{\text{abs}}(\lambda)] I(\lambda) d\lambda. \qquad (5) $$

Here, the first exponential term models the VUV absorption by dust as a function of wavelength and the column density of H nuclei (assuming it is proportional to the dust column density). The second exponential term is a summation of the shielding by atomic and molecular species (denoted by X with column density N_X) where the most important cases are photoabsorption by H, H₂, and self-shielding in the cases of other abundant molecules such as CO and N₂.

The rate reduction due to shielding is characterized by the shielding function:

$$ \theta = k/k_0 \qquad (6) $$

where k₀ is the photodestruction rate at the irradiated edge of the shielding region. The calculations here are appropriate for an infinite-slab geometry where the incident (isotropic) radiation is restricted to 2π sr and back-scattered radiation from the shielded region. Modeling dust shielding in other geometries will require more specific radiative transfer calculations than those used here. Shielding functions for photodissociation and photoionization have been calculated for all the species in the database and are available online in tabulated form.

The shielding functions are often plotted as a function of the visual extinction (A_V) in an interstellar cloud for simpler use. These can be formulated as one-parameter exponential curves (van Dishoeck et al. 2006):

$$ \theta(A_V) = \exp(-\gamma_{\text{exp}}A_V) \qquad (7) $$

or second order exponential integrals (Neufeld & Wolfire 2009; Roueff et al. 2014):

$$ \theta(A_V) = E_2(-\gamma_{E_2} A_V). \qquad (8) $$

A further reduction of the shielding function can be accomplished by introducing an exponential-decay parameter (γ_{fit}) and
structure is known exactly, molecular cross sections can be calculated as described above, but this is only the case for atoms and diatomics. For larger molecules, other approximating methods are required. At photon energies below 30 eV (or above 41 nm), the additivity of atomic photoionization cross sections overestimates the molecular ionization cross sections considerably. Previously, a model inspired by the classical and quantum mechanical sum rules of oscillator strengths has been used to describe photoabsorption and photoionization cross sections which were accurate to 20% on average, for a number of (closed-shell) molecules (Bobeldijk et al. 1994).

More recently, advances using the XCHEM methodology (Marante et al. 2017a,b; González-Vázquez et al. 2023) have not only provided great accuracy in the calculation of total and partial photoionization cross sections, but also photoelectron angular distributions and asymmetry parameters. The basic concept of XCHEM involves using a hybrid Gaussian-B-spline basis (GABS; Marante et al. 2014) combining the usual basis used in bound state calculations, but unsuited to describe the continuum, with a B-spline basis that provides a good description of the highly oscillating continuum wave functions. Besides applications to atomic and diatomic species, it has now been successfully applied to a triatomic molecule, namely H₂O (Fernández-Milán et al. 2023).

An interesting future avenue that could expedite experimentally and theoretically obtained cross sections is the use of machine learning algorithms. Recently, machine learning methods were used in combination with differential absorption spectroscopic methods in the VUV to develop predictive capabilities for inferring molecular structure from absorption spectra (Doner et al. 2022). By analyzing 102 absorption spectra of organic molecules such as alkanes, alkenes, ethers, and alcohols, the authors found that optimal determination of molecular structure using machine learning methods is strongly dependent on the absorption region in question. The work provides separate learning models for each molecular classification scheme which enables the identification of multifunctional species with isomer-resolved speciation. The application of procedures such as these could significantly expediate cross section data for the dozens of new molecules that are detected annually in space at the time of writing.

## 2.4. Radiation fields

The rate of photodissociation and photoionization (s⁻¹) per molecule or atom which is exposed to a radiation field of UV radiation is calculated thusly:

$$ \int \sigma(\lambda)I(\lambda)d\lambda \qquad (4) $$

where σ(λ) is the wavelength-dependent cross section in question, and I(λ) is the wavelength-dependent UV radiation field intensity summed over all coincidence angles. The radiation fields used are identical to those used previously (Heays et al. 2017) so only a brief summary follows here.

A total of nine different radiation fields have been used with the updated cross sections to calculate photorates to exemplify the variability in photodestruction in differing interstellar environs. The radiation fields utilized are the interstellar radiation field (ISRF) of Draine (1978), the Galactic radiation field estimate of Mathis et al. (1983), blackbody emission spectra at 4000 K, 10 000 K and 20 000 K, the Lyman-α line, the solar emission spectrum (Woods et al. 1996; Curdt et al. 2001),

the TW Hya radiation field (France et al. 2014), and a cosmic ray induced UV radiation field which is described in detail below. All radiation fields are normalized to match the energy intensity ($\int hcI(\lambda)d\lambda/\lambda$) of the Draine field integrated between 91.2 and 200 nm, that is, $2.6 \times 10^{-10} \text{ W cm}^{-2}$. The integrated fluxes of the radiation fields used to compute the photorates when using a 0.001 nm grid are provided in Table A.1 along with the normalization factors required.

## 2.5. Dust and line shielding

The last database update included shielding functions and gave a detailed overview of the formulations accounting for dust and line shielding (Heays et al. 2017). These calculations are also performed for the updated cross sections, and we present a brief overview of the calculations but refer to the previous work by Heays et al. for a more detailed discussion.

Molecules embedded inside interstellar clouds, protoplanetary disks or other such objects with large densities and a high dust content, are at least partially shielded from VUV radiation. Equation (4) gave the unattenuated photodestruction rate and so to account for the shielding materials in these objects we recalculate the rate as:

$$ \int \sigma^{pd}(\lambda) \exp[-\tau_{\text{dust}}(\lambda, N_{\text{H}+2\text{H}_2}) - \sum_{x=\text{H},\text{H}_2,\text{self}} N_X \sigma_X^{\text{abs}}(\lambda)] I(\lambda) d\lambda. \qquad (5) $$

Here, the first exponential term models the VUV absorption by dust as a function of wavelength and the column density of H nuclei (assuming it is proportional to the dust column density). The second exponential term is a summation of the shielding by atomic and molecular species (denoted by X with column density N_X) where the most important cases are photoabsorption by H, H₂, and self-shielding in the cases of other abundant molecules such as CO and N₂.

The rate reduction due to shielding is characterized by the shielding function:

$$ \theta = k/k_0 \qquad (6) $$

where k₀ is the photodestruction rate at the irradiated edge of the shielding region. The calculations here are appropriate for an infinite-slab geometry where the incident (isotropic) radiation is restricted to 2π sr and back-scattered radiation from the shielded region. Modeling dust shielding in other geometries will require more specific radiative transfer calculations than those used here. Shielding functions for photodissociation and photoionization have been calculated for all the species in the database and are available online in tabulated form.

The shielding functions are often plotted as a function of the visual extinction (A_V) in an interstellar cloud for simpler use. These can be formulated as one-parameter exponential curves (van Dishoeck et al. 2006):

$$ \theta(A_V) = \exp(-\gamma_{\text{exp}}A_V) \qquad (7) $$

or second order exponential integrals (Neufeld & Wolfire 2009; Roueff et al. 2014):

$$ \theta(A_V) = E_2(-\gamma_{E_2}A_V). \qquad (8) $$

A further reduction of the shielding function can be accomplished by introducing an exponential-decay parameter (γ_{fit}) and
an effective unshielded rate ($k_0^{fit}$) so that the depth-dependent photodestruction rate is:

$$k = k_0^{fit} \exp(-\gamma_{fit} A_V) \qquad (9)$$

which leads to the shielding function:

$$\theta(A_V) = k_0^{fit} / k_0 = \exp(-\gamma_{fit} A_V). \qquad (10)$$

The values of $\gamma_{E_2}$, $\gamma_{exp}$, $\gamma_{fit}$, and $k_0^{fit}$, for both photodissociation and photoionization are tabulated for each updated or added cross section in the database and can be downloaded online.

The dust-shielding-dependent photodissociation and photoionization rates were calculated using the optical properties of a dust population assuming one particular composition and size distribution which were obtained from the mixed grain-size and composition model built, developed and tested by Draine et al. (Draine & Lee 1984; Li & Draine 2001; Weingartner & Draine 2001a,b,c,d; Draine 2003a,b,c; Draine & Tan 2003), specifically their “RV = 3.1” model published online.

The additional terms due to atom and molecule shielding (including self-shielding) are also included. The importance of these shielding parameters were discussed in detail previously (Heays et al. 2017), but notable molecules whose self-shielding effects may have some significant astronomical relevance include $N_2$ (Li et al. 2013), CO (Visser et al. 2009), and $H_2$ (Wolcott-Green & Haiman 2019). $H_2$ shielding is particularly important at atomic-to-molecular transitions in cool low-metallicity, dust-free gas (Sternberg et al. 2021), in alleviating the effect of Lyman-Werner radiation background allowing $H_2$ formation and gas cooling (Nickerson et al. 2018; Skinner & Wise 2020), and it is crucial to accurately estimate the amount of cold dense gas that is available for star formation (Latif & Khochfar 2019). It is also cosmologically relevant to include self-shielding of $H_2$ in simulations of supermassive black hole collapses (Luo et al. 2020).

Atomic shielding is also important, for instance, neutral atomic carbon (C I) can shield and prevent CO photodissociation, thus allowing CO gas content to build up in dust-free disks (Kral et al. 2019; Cataldi et al. 2020) and can also suppress radiation pressure (Kral et al. 2017). In such gas-rich debris disks, CO self-shielding plays an important role as well (Moor et al. 2019). Attenuation of radiation fields by C, Si, and S self-shielding has also been shown to ensure efficient formation of species such as CO, OH, SiO, and $H_2O$ in dust-free winds or jets (Tabone et al. 2020).

In and of itself, $H_2O$ self-shielding has been shown to be an important component in the ubiquity of water vapor during the early stages of terrestrial planet formation (Bethell & Bergin 2009). More recently, the importance of self-shielding by $H_2O$ has been demonstrated to enhance the abundances of species such as $C_2H_2$, $CH_4$, HCN, $CH_3CN$ and $NH_3$ by over 3 orders of magnitude within the inner 5 AU of disks which could have significant implications for prebiotic chemistry on nascent planets (Duval et al. 2022). Water self-shielding could also enhance the $H_2^{18}O$ content high up in the molecular layer of protoplanetary disks which could make $H_2^{18}O$ observable with James Webb Space Telescope (Calahan et al. 2022).

Self-shielding is also found to play an important role in fractionation. In the case of CO, inefficient self-shielding affects CO isotopologue intensity profiles in the disk outer regions (Miotello et al. 2018). In the case of $N_2$, fractionation can be completely dominated by isotope-selective photodissociation

(Heays et al. 2014), which impacts the subsequent fractionation of HCN as HCN formation is closely coupled to the UV irradiated surface layers of protoplanetary disks. This leads to the column density ratio of HCN over $HC^{15}N$ in the disk’s inner 100 AU being sensitive to the grain size distribution where for larger grains, self-shielding of $N_2$ becomes more important relative to dust extinction, leading to stronger isotope fractionation (Visser et al. 2018).

Self-shielding has also been theorized to contribute to the ortho-to-para ratio of $H_2CO$ observed in proto-brown dwarfs as the two spin isomers display different photodissociation yields. However, this is not confirmed and is considered speculative (Riaz et al. 2019).

## 2.6. Cosmic ray ionization rates

The astrochemical importance of cosmic rays cannot be overstated (Dalgarno 2006a,b). Cosmic rays penetrate deeper than photons into interstellar clouds, protostellar envelopes, protoplanetary disks, and planetary atmospheres, where they ionize $H_2$ molecules. This ignites a cascade of rescattered electrons which further excite $H_2$ and generate excited H atoms that radiatively decay (Cravens & Dalgarno 1978; Gredel & Dalgarno 1995). Additionally, in dark clouds, cosmic rays are solely responsible for producing atomic hydrogen (Padovani et al. 2018a). This cosmic-ray-triggered photolysis of molecular hydrogen seeds more shaded regions in the universe with smaller bubbles of VUV photons which are absorbed by the embedded material. This UV flux is highly structured with thousands of discrete emission lines between 80 and 170 nm along with continuum emission between 122 and 300 nm (Prasad & Tarafdar 1983; Gredel et al. 1987; Cecchi-Pestellini & Aiello 1992). Approximately 15% of the integrated flux is due to Lyman-$\alpha$ emission. This flux has been quantified and here, we compute the cosmic ray ionization-driven photorates of the newly updated cross sections.

The cosmic ray induced UV flux is modeled as a rate of photons generated per unit spectral density per hydrogen nucleus

$$R(\lambda) = \xi_{H_2} x_{H_2} P(\lambda) \qquad (11)$$

with

$$x_{\lambda} = \frac{n(X)}{n(H) + 2n(H_2)} \qquad (12)$$

as the relative abundance of species X with respect to total hydrogen nuclei, $\xi_{H_2}$ is the rate at which a $H_2$ molecule is ionized by cosmic ray collisions, and, as previously (Heays et al. 2017), $P(\lambda)$, denotes the wavelength-dependent probability distribution of generated photons adopted from the work of Gredel et al. (1989).

The value of $\xi_{H_2}$ is highly uncertain given the “average” rate of cosmic-ray ionization in the ISM (Indriolo & McCall 2012), as well as the fact that it can be very strongly enhanced close to protostars (Ceccarelli et al. 2014; Podio et al. 2014) and supernova remnants (Vaupre et al. 2014). In molecular clouds, it is suggested that the cosmic-ray ionization rate decreases with increasing column densities of the cloud and so can vary from $10^{-16}$ for diffuse clouds down to $10^{-17}$ s$^{-1}$ for dense clouds (Padovani et al. 2009; Indriolo & McCall 2012).

However, modeling of the chemistry of the prestellar core L1544 suggests a $\xi_{H_2}$ value as high as $10^{-16}$ s$^{-1}$, which is an order of magnitude higher than what was previously thought (Ivlev et al. 2019). It has also been found that the cosmic ray
an effective unshielded rate ($k_0^{fit}$) so that the depth-dependent photodestruction rate is:

$$k = k_0^{fit} \exp(-\gamma_{fit} A_V) \qquad (9)$$

which leads to the shielding function:

$$\theta(A_V) = k_0^{fit} / k_0 = \exp(-\gamma_{fit} A_V). \qquad (10)$$

The values of $\gamma_{E_2}$, $\gamma_{exp}$, $\gamma_{fit}$, and $k_0^{fit}$, for both photodissociation and photoionization are tabulated for each updated or added cross section in the database and can be downloaded online.

The dust-shielding-dependent photodissociation and photoionization rates were calculated using the optical properties of a dust population assuming one particular composition and size distribution which were obtained from the mixed grain-size and composition model built, developed and tested by Draine et al. (Draine & Lee 1984; Li & Draine 2001; Weingartner & Draine 2001a,b,c,d; Draine 2003a,b,c; Draine & Tan 2003), specifically their “RV = 3.1” model published online.

The additional terms due to atom and molecule shielding (including self-shielding) are also included. The importance of these shielding parameters were discussed in detail previously (Heays et al. 2017), but notable molecules whose self-shielding effects may have some significant astronomical relevance include N₂ (Li et al. 2013), CO (Visser et al. 2009), and H₂ (Wolcott-Green & Haiman 2019). H₂ shielding is particularly important at atomic-to-molecular transitions in cool low-metallicity, dust-free gas (Sternberg et al. 2021), in alleviating the effect of Lyman-Werner radiation background allowing H₂ formation and gas cooling (Nickerson et al. 2018; Skinner & Wise 2020), and it is crucial to accurately estimate the amount of cold dense gas that is available for star formation (Latif & Khochfar 2019). It is also cosmologically relevant to include self-shielding of H₂ in simulations of supermassive black hole collapses (Luo et al. 2020).

Atomic shielding is also important, for instance, neutral atomic carbon (C I) can shield and prevent CO photodissociation, thus allowing CO gas content to build up in dust-free disks (Kral et al. 2019; Cataldi et al. 2020) and can also suppress radiation pressure (Kral et al. 2017). In such gas-rich debris disks, CO self-shielding plays an important role as well (Moor et al. 2019). Attenuation of radiation fields by C, Si, and S self-shielding has also been shown to ensure efficient formation of species such as CO, OH, SiO, and H₂O in dust-free winds or jets (Tabone et al. 2020).

In and of itself, H₂O self-shielding has been shown to be an important component in the ubiquity of water vapor during the early stages of terrestrial planet formation (Bethell & Bergin 2009). More recently, the importance of self-shielding by H₂O has been demonstrated to enhance the abundances of species such as C₂H₂, CH₄, HCN, CH₃CN and NH₃ by over 3 orders of magnitude within the inner 5 AU of disks which could have significant implications for prebiotic chemistry on nascent planets (Duval et al. 2022). Water self-shielding could also enhance the H₂¹⁸O content high up in the molecular layer of protoplanetary disks which could make H₂¹⁸O observable with James Webb Space Telescope (Calahan et al. 2022).

Self-shielding is also found to play an important role in fractionation. In the case of CO, inefficient self-shielding affects CO isotopologue intensity profiles in the disk outer regions (Miotello et al. 2018). In the case of N₂, fractionation can be completely dominated by isotope-selective photodissociation

(Heays et al. 2014), which impacts the subsequent fractionation of HCN as HCN formation is closely coupled to the UV irradiated surface layers of protoplanetary disks. This leads to the column density ratio of HCN over HC¹⁵N in the disk's inner 100 AU being sensitive to the grain size distribution where for larger grains, self-shielding of N₂ becomes more important relative to dust extinction, leading to stronger isotope fractionation (Visser et al. 2018).

Self-shielding has also been theorized to contribute to the ortho-to-para ratio of H₂CO observed in proto-brown dwarfs as the two spin isomers display different photodissociation yields. However, this is not confirmed and is considered speculative (Riaz et al. 2019).

## 2.6. Cosmic ray ionization rates

The astrochemical importance of cosmic rays cannot be overstated (Dalgarno 2006a,b). Cosmic rays penetrate deeper than photons into interstellar clouds, protostellar envelopes, protoplanetary disks, and planetary atmospheres, where they ionize H₂ molecules. This ignites a cascade of rescattered electrons which further excite H₂ and generate excited H atoms that radiatively decay (Cravens & Dalgarno 1978; Gredel & Dalgarno 1995). Additionally, in dark clouds, cosmic rays are solely responsible for producing atomic hydrogen (Padovani et al. 2018a). This cosmic-ray-triggered photolysis of molecular hydrogen seeds more shaded regions in the universe with smaller bubbles of VUV photons which are absorbed by the embedded material. This UV flux is highly structured with thousands of discrete emission lines between 80 and 170 nm along with continuum emission between 122 and 300 nm (Prasad & Tarafdar 1983; Gredel et al. 1987; Cecchi-Pestellini & Aiello 1992). Approximately 15% of the integrated flux is due to Lyman-α emission. This flux has been quantified and here, we compute the cosmic ray ionization-driven photorates of the newly updated cross sections.

The cosmic ray induced UV flux is modeled as a rate of photons generated per unit spectral density per hydrogen nucleus

$$R(\lambda) = \xi_{H_2} x_{H_2} P(\lambda) \qquad (11)$$

with

$$x_{\lambda} = \frac{n(X)}{n(H) + 2n(H_2)} \qquad (12)$$

as the relative abundance of species X with respect to total hydrogen nuclei, $\xi_{H_2}$ is the rate at which a H₂ molecule is ionized by cosmic ray collisions, and, as previously (Heays et al. 2017), $P(\lambda)$, denotes the wavelength-dependent probability distribution of generated photons adopted from the work of Gredel et al. (1989).

The value of $\xi_{H_2}$ is highly uncertain given the “average” rate of cosmic-ray ionization in the ISM (Indriolo & McCall 2012), as well as the fact that it can be very strongly enhanced close to protostars (Ceccarelli et al. 2014; Podio et al. 2014) and supernova remnants (Vaupre et al. 2014). In molecular clouds, it is suggested that the cosmic-ray ionization rate decreases with increasing column densities of the cloud and so can vary from $10^{-16}$ for diffuse clouds down to $10^{-17}$ s⁻¹ for dense clouds (Padovani et al. 2009; Indriolo & McCall 2012).

However, modeling of the chemistry of the prestellar core L1544 suggests a $\xi_{H_2}$ value as high as $10^{-16}$ s⁻¹, which is an order of magnitude higher than what was previously thought (Ivlev et al. 2019). It has also been found that the cosmic ray
ionization rate in high-density environments such as in the inner parts of collapsing molecular clouds or the midplanes of circumstellar disks have higher rates than previously assumed. Tangentially it is important to note that some processes such as stellar winds, the magnetic field structure, and even the chemical make-up can modulate cosmic ray ionization (Cleeves et al. 2013, 2014) and a sub-interstellar cosmic ray ionization rate has been observed in the disk midplane of TW Hya (Cleeves et al. 2015).

The cosmic ray ionization rate does not decline exponentially with increasing column density but follows a more complex behavior because of the interplay of different processes governing the generation and propagation of secondary particles (Padovani et al. 2018b). The same can be said of massive hot cores where the models predict significantly elevated values of $\xi_{H_2}$ (Barger & Garrod 2020).

Meanwhile, molecular ions such as $H_3^+$ (Indriolo 2012), $OH^+$ (Bacalla et al. 2019), $H_2O^+$ (Indriolo et al. 2015), and $ArH^+$ (Neufeld & Wolfire 2016) are being used to constrain the cosmic ray ionization rate which can yield values up to $10^{-15} \text{ s}^{-1}$. At higher densities typical of starless cores, observations of $HCO^+$, $DCO^+$, and CO show that the cosmic ray ionization rate decreases but still displays a spread of two orders of magnitude ($5 \times 10^{-18} \text{ s}^{-1} \le \xi_{H_2} \le 4 \times 10^{-16} \text{ s}^{-1}$) (Caselli et al. 1998; Maret & Bergin 2007; Fuente et al. 2016). Such a spread could be due to incompleteness of chemical models and the configuration of the magnetic field lines (Padovani & Galli 2011; Padovani et al. 2013; Silsbee et al. 2018). More recently, models have been developed estimating the cosmic ray ionization rate using observations of $H_2D^+$ and other higher deuterations of $H_3^+$ (Bovino et al. 2020) which have yielded values between $7 \times 10^{-18} \text{ s}^{-1} \le \xi_{H_2} \le 6 \times 10^{-17} \text{ s}^{-1}$ (Sabatini et al. 2020).

Harmonizing all the variables observed in cosmic-ray ionization rates has led to a surge in our understanding the underlying astrophysical processes governing the origins and propagation of cosmic rays. As an example, it has been found that ionization rates measured inside molecular clouds could not be solely due to background cosmic rays, and if the cosmic ray spectrum measured by Voyager 1 is representative of the whole Galaxy, the predicted ionization rate in diffuse clouds fails to reproduce data by 1–2 orders of magnitude (Recchia et al. 2019). This has led researchers to suggest other possibilities that would have to be invoked such as inhomogeneous distribution of cosmic rays in the ISM, cosmic ray sources inside clouds, and others (Phan et al. 2018). Cosmic rays from supernova remnants have also been invoked to be important as they would be discrete sources of cosmic rays so that local spectra of MeV cosmic rays would generally not be representative for spectra elsewhere in the Galaxy (Phan et al. 2021). Other factors may be important for the cosmic ray ionization rate such as how cosmic ray diffusion operates in molecular clouds; through free-streaming or diffusive propagation (Silsbee & Ivlev 2019), and how diffusive shock acceleration can drive high ionization rates and synchrotron emissions toward protostellar sources (Padovani et al. 2016). These and other recent advances and current open questions concerning cosmic rays have recently been reviewed (Padovani et al. 2020; Gabici 2022).

The cosmic ray ionization rate adopted in the database is $\xi_{H_2} = 10^{-16} \text{ s}^{-1} \text{H}_2^{-1}$. All cosmic ray induced photodestruction rates can be adapted to other values of $\xi_{H_2}$ by simple scaling. Other relevant parameters that were assumed are the following: $x(H) = 10^{-4}$, $x(N_2) = x(CO) = 10^{-5}$, ortho-$H_2$:para-$H_2$ = 0:1. These are equivalent to those used in the previous database update.

Although most cosmic ray generated photons are absorbed by dust grains, there is a fraction that drives photodissociation and photoionization of atoms or molecules, X. This fraction is given by:

$$p_X(\lambda) = \frac{x_X \sigma_X^{\text{diss/ion}}}{x_{\text{dust}} \sigma_{\text{dust}}^{\text{abs}}(\lambda) + \sum_j x_j \sigma_j^{\text{abs}}(\lambda)} \quad (13)$$

Here, $\sigma_X^{\text{diss/ion}}$ is the photodissociation or photoionization cross section of species X, and the denominator sums the photoabsorption cross sections of all dust and gas species. The probability of a cosmic-ray-generated UV photon being absorbed by a dust grain or any gaseous molecule is wavelength-dependent through the relevant cross sections utilized in Eq. (13).

The rate of a particular photodestruction process for species X due to cosmic ray ionization produced photons is then:

$$k_X = \frac{1}{x_X} \int R(\lambda) p_X(\lambda) d\lambda. \quad (14)$$

The integration was carried out on a 0.001 nm wavelength grid which sufficiently captures the full details of the cross sections included in the database.

## 2.7. Temperature effects

The original objective of the database was to provide cross sections to accurately simulate UV-driven photoprocesses in the interstellar medium where temperature effects are negligible. As such, it is worth briefly addressing limitations of the applicability of the data in this database. These concern high-temperatures in certain radiation fields, but these effects are usually molecule dependent and should be assessed on a molecule-to-molecule basis.

As shown in the works of both Pezzella et al. (2022) and Qin et al. (2022), photodissociation rates of HF and HCl under ISRF conditions are negligibly affected by the high-temperature cross sections in comparison to colder temperatures in molecular clouds. As the effects of high temperatures are principally observed as large increases in the cross sections toward longer wavelengths, the photodissociation rates are particularly temperature-sensitive in radiation fields with greater intensities toward longer wavelengths. For instance, under a 4000 K black-body radiation field, the photodissociation rates of HF and HCl derived at excitation temperatures between 0 K and 10 000 K are found to increase negligibly between 0 K and 2000 K, but by two orders of magnitude between 2000 K and 10 000 K (Qin et al. 2022).

In the cases of high-temperature exoplanet atmosphere, a caveat is therefore warranted in using the data from this database. Currently, high-temperature photodissociation cross sections are being computed and compiled in the EXOMOL database (Tennyson et al. 2016b) and UV absorption cross sections at various temperature ranges are being compiled in the HITRAN database (Gordon et al. 2022), but at the time of writing only a handful of high-temperature cross section are available. These temperature dependent limitations have also been discussed in Sect. 8.2 of Heays et al. (2017).

## 3. Cross section database update

All cross sections that have been added to the database (or updated) are presented. They are plotted in Figs. 1–4 and in
ionization rate in high-density environments such as in the inner parts of collapsing molecular clouds or the midplanes of circumstellar disks have higher rates than previously assumed. Tangentially it is important to note that some processes such as stellar winds, the magnetic field structure, and even the chemical make-up can modulate cosmic ray ionization (Cleeves et al. 2013, 2014) and a sub-interstellar cosmic ray ionization rate has been observed in the disk midplane of TW Hya (Cleeves et al. 2015).

The cosmic ray ionization rate does not decline exponentially with increasing column density but follows a more complex behavior because of the interplay of different processes governing the generation and propagation of secondary particles (Padovani et al. 2018b). The same can be said of massive hot cores where the models predict significantly elevated values of $\xi_{H_2}$ (Barger & Garrod 2020).

Meanwhile, molecular ions such as $H_3^+$ (Indriolo 2012), $OH^+$ (Bacalla et al. 2019), $H_2O^+$ (Indriolo et al. 2015), and $ArH^+$ (Neufeld & Wolfire 2016) are being used to constrain the cosmic ray ionization rate which can yield values up to $10^{-15} \text{ s}^{-1}$. At higher densities typical of starless cores, observations of $HCO^+$, $DCO^+$, and CO show that the cosmic ray ionization rate decreases but still displays a spread of two orders of magnitude ($5 \times 10^{-18} \text{ s}^{-1} \le \xi_{H_2} \le 4 \times 10^{-16} \text{ s}^{-1}$) (Caselli et al. 1998; Maret & Bergin 2007; Fuente et al. 2016). Such a spread could be due to incompleteness of chemical models and the configuration of the magnetic field lines (Padovani & Galli 2011; Padovani et al. 2013; Silsbee et al. 2018). More recently, models have been developed estimating the cosmic ray ionization rate using observations of $H_2D^+$ and other higher deuterations of $H_3^+$ (Bovino et al. 2020) which have yielded values between $7 \times 10^{-18} \text{ s}^{-1} \le \xi_{H_2} \le 6 \times 10^{-17} \text{ s}^{-1}$ (Sabatini et al. 2020).

Harmonizing all the variabilities observed in cosmic-ray ionization rates has led to a surge in our understanding the underlying astrophysical processes governing the origins and propagation of cosmic rays. As an example, it has been found that ionization rates measured inside molecular clouds could not be solely due to background cosmic rays, and if the cosmic ray spectrum measured by Voyager 1 is representative of the whole Galaxy, the predicted ionization rate in diffuse clouds fails to reproduce data by 1–2 orders of magnitude (Recchia et al. 2019). This has led researchers to suggest other possibilities that would have to be invoked such as inhomogeneous distribution of cosmic rays in the ISM, cosmic ray sources inside clouds, and others (Phan et al. 2018). Cosmic rays from supernova remnants have also been invoked to be important as they would be discrete sources of cosmic rays so that local spectra of MeV cosmic rays would generally not be representative for spectra elsewhere in the Galaxy (Phan et al. 2021). Other factors may be important for the cosmic ray ionization rate such as how cosmic ray diffusion operates in molecular clouds; through free-streaming or diffusive propagation (Silsbee & Ivlev 2019), and how diffusive shock acceleration can drive high ionization rates and synchrotron emissions toward protostellar sources (Padovani et al. 2016). These and other recent advances and current open questions concerning cosmic rays have recently been reviewed (Padovani et al. 2020; Gabici 2022).

The cosmic ray ionization rate adopted in the database is $\xi_{H_2} = 10^{-16} \text{ s}^{-1} \text{H}_2^{-1}$. All cosmic ray induced photodestruction rates can be adapted to other values of $\xi_{H_2}$ by simple scaling. Other relevant parameters that were assumed are the following: $x(H) = 10^{-4}$, $x(N_2) = x(CO) = 10^{-5}$, ortho-$H_2$:para-$H_2$ = 0:1. These are equivalent to those used in the previous database update.

Although most cosmic ray generated photons are absorbed by dust grains, there is a fraction that drives photodissociation and photoionization of atoms or molecules, X. This fraction is given by:

$$p_X(\lambda) = \frac{x_X \sigma_X^{\text{diss/ion}}}{x_{\text{dust}} \sigma_{\text{dust}}^{\text{abs}}(\lambda) + \sum_j x_j \sigma_j^{\text{abs}}(\lambda)} \quad (13)$$

Here, $\sigma_X^{\text{diss/ion}}$ is the photodissociation or photoionization cross section of species X, and the denominator sums the photoabsorption cross sections of all dust and gas species. The probability of a cosmic-ray-generated UV photon being absorbed by a dust grain or any gaseous molecule is wavelength-dependent through the relevant cross sections utilized in Eq. (13).

The rate of a particular photodestruction process for species X due to cosmic ray ionization produced photons is then:

$$k_X = \frac{1}{x_X} \int R(\lambda) p_X(\lambda) d\lambda. \quad (14)$$

The integration was carried out on a 0.001 nm wavelength grid which sufficiently captures the full details of the cross sections included in the database.

## 2.7. Temperature effects

The original objective of the database was to provide cross sections to accurately simulate UV-driven photoprocesses in the interstellar medium where temperature effects are negligible. As such, it is worth briefly addressing limitations of the applicability of the data in this database. These concern high-temperatures in certain radiation fields, but these effects are usually molecule dependent and should be assessed on a molecule-to-molecule basis.

As shown in the works of both Pezzella et al. (2022) and Qin et al. (2022), photodissociation rates of HF and HCl under ISRF conditions are negligibly affected by the high-temperature cross sections in comparison to colder temperatures in molecular clouds. As the effects of high temperatures are principally observed as large increases in the cross sections toward longer wavelengths, the photodissociation rates are particularly temperature-sensitive in radiation fields with greater intensities toward longer wavelengths. For instance, under a 4000 K black-body radiation field, the photodissociation rates of HF and HCl derived at excitation temperatures between 0 K and 10 000 K are found to increase negligibly between 0 K and 2000 K, but by two orders of magnitude between 2000 K and 10 000 K (Qin et al. 2022).

In the cases of high-temperature exoplanet atmosphere, a caveat is therefore warranted in using the data from this database. Currently, high-temperature photodissociation cross sections are being computed and compiled in the EXOMOL database (Tennyson et al. 2016b) and UV absorption cross sections at various temperature ranges are being compiled in the HITRAN database (Gordon et al. 2022), but at the time of writing only a handful of high-temperature cross section are available. These temperature dependent limitations have also been discussed in Sect. 8.2 of Heays et al. (2017).

## 3. Cross section database update

All cross sections that have been added to the database (or updated) are presented. They are plotted in Figs. 1–4 and in
<figure><img src="image_1.png" /><figcaption>**Fig. 1.** Cross sections of $H_3^+$, CH, $C_2$, $C_2H$, $C_2H^-$, $C_2H_3$, $C_2H_5$, and $l-C_3H$. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken grey lines.</figcaption></figure>
<figure><img src="image_3.png" /><figcaption>**Fig. 1.** Cross sections of H⁺, CH, C₂, C₂H, C₂H⁻, C₂H₃, C₂H₅, and I-C₃H. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken grey lines.</figcaption></figure>
<figure><img src="image_2.png" /><figcaption>**Fig. 2.** Cross sections of c-C<sub>3</sub>H and HC<sub>3</sub>H, c-C<sub>3</sub>H<sub>2</sub>, C<sub>3</sub>H<sub>3</sub>, C<sub>4</sub>H<sup>-</sup>, C<sub>6</sub>H<sup>-</sup>, OH, and HO<sub>2</sub>. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>
<figure><img src="image_4.png" /><figcaption>**Fig. 2.** Cross sections of c-C<sub>3</sub>H and HC<sub>3</sub>H, c-C<sub>3</sub>H<sub>2</sub>, C<sub>3</sub>H<sub>3</sub>, C<sub>4</sub>H<sup>-</sup>, C<sub>6</sub>H<sup>-</sup>, OH, and HO<sub>2</sub>. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>
<figure><img src="image_3.png" /><figcaption>**Fig. 3.** Cross sections of HCO, HCOOH, NH₂, HNC, HNCO, CH₃CHO, CH₃OCH₃, and CH₃OCHO. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>
<figure><img src="image_5.png" /><figcaption>**Fig. 3.** Cross sections of HCO, HCOOH, NH₂, HNC, HNCO, CH₃CHO, CH₃OCH₃, and CH₃OCHO. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>
<figure><img src="image_4.png" /><figcaption>**Fig. 4.** Cross sections of SH, CS, H₂CS, S₂, SiH, HF. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>

each section their newly computed photorates are tabulated for each molecule along with comparisons to older values where applicable in Tables 1–33. In Table 34, an overview of the database updates is presented along with an estimated rating of the uncertainty of the cross sections. We give four ratings: A+, A, B, and C, which correspond to accuracy within 20%, 30%, a factor of 2 and an order of magnitude, respectively. The new cross sections are presented in the same logical order as presented in the previous database update (Heays et al. 2017).

### 3.1. $H_3^+$

The VUV photodissociation of $H_3^+$ has been investigated recently using three-dimensional imaging of the dissociation products (Urbain et al. 2019). The potential energy surfaces of $H_3^+$ exhibit a rich topology which results from the high degree of symmetry

imposed by the indiscernibility of the protons, and the asymptotic degeneracy of its fragmentation channels which stems from it. In their seminal work on time-dependent wavepacket propagation, Kulander & Heller computed the photodissociation cross section of $H_3^+$ in its absolute ground state (Kulander & Heller 1978) in which they found a maximum around 21 eV that starts growing in above 14 eV. This cross section is currently implemented in the database.

The experimental dissociation threshold of $H_3^+$ has, however, been measured to be 4.373 eV (283.5 nm) (Cosby & Helm 1988), calculated as 4.349 eV (285.1 nm) (Mizus et al. 2019), and photodissociation of the $H_3^+$ ion has been observed up to 1 eV below the previously obtained thresholds using an ion storage ring (Petrignani et al. 2010). This work by Petrignani et al. (2010) found a photodissociation cross section of $7 \times 10^{-20} \text{ cm}^2$ at 4.9 eV. If such a cross section is considered
<figure><img src="image_6.png" /><figcaption>**Fig. 4.** Cross sections of SH, CS, H₂CS, S₂, SiH, HF. Photodissociation is presented in red. Photoionization is presented in green. Dissociation and ionization thresholds are shown with broken gray lines.</figcaption></figure>

each section their newly computed photorates are tabulated for each molecule along with comparisons to older values where applicable in Tables 1–33. In Table 34, an overview of the database updates is presented along with an estimated rating of the uncertainty of the cross sections. We give four ratings: A+, A, B, and C, which correspond to accuracy within 20%, 30%, a factor of 2 and an order of magnitude, respectively. The new cross sections are presented in the same logical order as presented in the previous database update (Heays et al. 2017).

### 3.1. $H_3^+$

The VUV photodissociation of $H_3^+$ has been investigated recently using three-dimensional imaging of the dissociation products (Urbain et al. 2019). The potential energy surfaces of $H_3^+$ exhibit a rich topology which results from the high degree of symmetry

imposed by the indiscernibility of the protons, and the asymptotic degeneracy of its fragmentation channels which stems from it. In their seminal work on time-dependent wavepacket propagation, Kulander & Heller computed the photodissociation cross section of $H_3^+$ in its absolute ground state (Kulander & Heller 1978) in which they found a maximum around 21 eV that starts growing in above 14 eV. This cross section is currently implemented in the database.

The experimental dissociation threshold of $H_3^+$ has, however, been measured to be 4.373 eV (283.5 nm) (Cosby & Helm 1988), calculated as 4.349 eV (285.1 nm) (Mizus et al. 2019), and photodissociation of the $H_3^+$ ion has been observed up to 1 eV below the previously obtained thresholds using an ion storage ring (Petrignani et al. 2010). This work by Petrignani et al. (2010) found a photodissociation cross section of $7 \times 10^{-20} \text{ cm}^2$ at 4.9 eV. If such a cross section is considered
<table><caption>**Table 1.** Calculated photodissociation rates of $H_3^+$ and comparisons to current entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.95E-11</td><td>—</td><td>—</td></tr><tr><td>Mathis '83</td><td>3.29E-11</td><td>—</td><td>—</td></tr><tr><td>4000 K</td><td>5.33E-08</td><td>—</td><td>—</td></tr><tr><td>10 000 K</td><td>1.80E-10</td><td>—</td><td>—</td></tr><tr><td>20 000 K</td><td>3.39E-11</td><td>—</td><td>—</td></tr><tr><td>Lyman-α</td><td>1.10E-11</td><td>—</td><td>—</td></tr><tr><td>Solar</td><td>3.11E-08</td><td>3.88E-13</td><td>8.02E+04</td></tr><tr><td>TW-Hya</td><td>1.17E-10</td><td>3.67E-12</td><td>31.9</td></tr><tr><td>Cosmic-ray UV</td><td>1.36E-15</td><td>2.33E-17</td><td>58.4</td></tr></tbody></table>

<table><caption>**Table 2.** Calculated photoionization rates of CH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.51E-10</td><td>7.63E-10</td><td>0.329</td></tr><tr><td>Mathis '83</td><td>1.93E-10</td><td>5.59E-10</td><td>0.345</td></tr><tr><td>4000 K</td><td>9.93E-15</td><td>2.26E-14</td><td>0.439</td></tr><tr><td>10 000 K</td><td>2.30E-11</td><td>6.82E-11</td><td>0.337</td></tr><tr><td>20 000 K</td><td>2.22E-10</td><td>6.42E-10</td><td>0.346</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>—</td></tr><tr><td>Solar</td><td>4.57E-12</td><td>9.64E-12</td><td>0.474</td></tr><tr><td>TW-Hya</td><td>5.09E-11</td><td>1.38E-10</td><td>0.369</td></tr><tr><td>Cosmic-ray UV</td><td>1.74E-14</td><td>5.78E-14</td><td>0.301</td></tr></tbody></table>

<table><caption>**Table 3.** Calculated photoionization rates of $C_2$ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.46E-10</td><td>4.09E-10</td><td>0.846</td></tr><tr><td>Mathis '83</td><td>2.98E-10</td><td>3.42E-10</td><td>0.871</td></tr><tr><td>4000 K</td><td>1.58E-15</td><td>1.39E-15</td><td>1.14</td></tr><tr><td>10 000 K</td><td>2.36E-11</td><td>2.75E-11</td><td>0.858</td></tr><tr><td>20 000 K</td><td>3.54E-10</td><td>4.18E-10</td><td>0.847</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>—</td></tr><tr><td>Solar</td><td>7.34E-12</td><td>6.71E-12</td><td>1.09</td></tr><tr><td>TW-Hya</td><td>8.04E-11</td><td>8.75E-11</td><td>0.919</td></tr><tr><td>Cosmic-ray UV</td><td>2.11E-14</td><td>2.46E-14</td><td>0.858</td></tr></tbody></table>

<table><caption>**Table 4.** Calculated photoionization rates of $C_2H$.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>6.20E-10</td></tr><tr><td>Mathis '83</td><td>4.12E-10</td></tr><tr><td>4000 K</td><td>4.39E-15</td></tr><tr><td>10 000 K</td><td>4.52E-11</td></tr><tr><td>20 000 K</td><td>5.83E-10</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>1.40E-11</td></tr><tr><td>TW-Hya</td><td>1.48E-10</td></tr><tr><td>Cosmic-ray UV</td><td>4.09E-14</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

by introducing a $7 \times 10^{-20}$ cm$^2$ baseline to the down the dissociation limit of 283.5 nm and from those thresholds assuming that the cross section drops linearly down to 500 nm where a

<table><caption>**Table 5.** Calculated photodetachment rates of $C_2H^-$.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.92E-09</td></tr><tr><td>Mathis '83</td><td>2.18E-09</td></tr><tr><td>4000 K</td><td>1.77E-06</td></tr><tr><td>10 000 K</td><td>1.16E-08</td></tr><tr><td>20 000 K</td><td>2.77E-09</td></tr><tr><td>Lyman-α</td><td>1.16E-09</td></tr><tr><td>Solar</td><td>1.76E-09</td></tr><tr><td>TW-Hya</td><td>5.45E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.32E-13</td></tr></tbody></table>

**Notes.** No previous photodetachment rates were included in the database.

cross section of approximately $3 \times 10^{-21}$ cm$^2$ was measured (Petrignani et al. 2010), this would yield significantly increased photorates as presented in Table 1.
<table><caption>**Table 1.** Calculated photodissociation rates of $H_3^+$ and comparisons to current entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.95E-11</td><td>–</td><td>–</td></tr><tr><td>Mathis '83</td><td>3.29E-11</td><td>–</td><td>–</td></tr><tr><td>4000 K</td><td>5.33E-08</td><td>–</td><td>–</td></tr><tr><td>10 000 K</td><td>1.80E-10</td><td>–</td><td>–</td></tr><tr><td>20 000 K</td><td>3.39E-11</td><td>–</td><td>–</td></tr><tr><td>Lyman-α</td><td>1.10E-11</td><td>–</td><td>–</td></tr><tr><td>Solar</td><td>3.11E-08</td><td>3.88E-13</td><td>8.02E+04</td></tr><tr><td>TW-Hya</td><td>1.17E-10</td><td>3.67E-12</td><td>31.9</td></tr><tr><td>Cosmic-ray UV</td><td>1.36E-15</td><td>2.33E-17</td><td>58.4</td></tr></tbody></table>

<table><caption>**Table 2.** Calculated photoionization rates of CH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.51E-10</td><td>7.63E-10</td><td>0.329</td></tr><tr><td>Mathis '83</td><td>1.93E-10</td><td>5.59E-10</td><td>0.345</td></tr><tr><td>4000 K</td><td>9.93E-15</td><td>2.26E-14</td><td>0.439</td></tr><tr><td>10 000 K</td><td>2.30E-11</td><td>6.82E-11</td><td>0.337</td></tr><tr><td>20 000 K</td><td>2.22E-10</td><td>6.42E-10</td><td>0.346</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>4.57E-12</td><td>9.64E-12</td><td>0.474</td></tr><tr><td>TW-Hya</td><td>5.09E-11</td><td>1.38E-10</td><td>0.369</td></tr><tr><td>Cosmic-ray UV</td><td>1.74E-14</td><td>5.78E-14</td><td>0.301</td></tr></tbody></table>

<table><caption>**Table 3.** Calculated photoionization rates of $C_2$ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.46E-10</td><td>4.09E-10</td><td>0.846</td></tr><tr><td>Mathis '83</td><td>2.98E-10</td><td>3.42E-10</td><td>0.871</td></tr><tr><td>4000 K</td><td>1.58E-15</td><td>1.39E-15</td><td>1.14</td></tr><tr><td>10 000 K</td><td>2.36E-11</td><td>2.75E-11</td><td>0.858</td></tr><tr><td>20 000 K</td><td>3.54E-10</td><td>4.18E-10</td><td>0.847</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>7.34E-12</td><td>6.71E-12</td><td>1.09</td></tr><tr><td>TW-Hya</td><td>8.04E-11</td><td>8.75E-11</td><td>0.919</td></tr><tr><td>Cosmic-ray UV</td><td>2.11E-14</td><td>2.46E-14</td><td>0.858</td></tr></tbody></table>

<table><caption>**Table 4.** Calculated photoionization rates of $C_2H$.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>6.20E-10</td></tr><tr><td>Mathis '83</td><td>4.12E-10</td></tr><tr><td>4000 K</td><td>4.39E-15</td></tr><tr><td>10 000 K</td><td>4.52E-11</td></tr><tr><td>20 000 K</td><td>5.83E-10</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>1.40E-11</td></tr><tr><td>TW-Hya</td><td>1.48E-10</td></tr><tr><td>Cosmic-ray UV</td><td>4.09E-14</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

by introducing a $7 \times 10^{-20}$ cm$^2$ baseline to the down the dissociation limit of 283.5 nm and from those thresholds assuming that the cross section drops linearly down to 500 nm where a

<table><caption>**Table 5.** Calculated photodetachment rates of $C_2H^-$.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.92E-09</td></tr><tr><td>Mathis '83</td><td>2.18E-09</td></tr><tr><td>4000 K</td><td>1.77E-06</td></tr><tr><td>10 000 K</td><td>1.16E-08</td></tr><tr><td>20 000 K</td><td>2.77E-09</td></tr><tr><td>Lyman-α</td><td>1.16E-09</td></tr><tr><td>Solar</td><td>1.76E-09</td></tr><tr><td>TW-Hya</td><td>5.45E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.32E-13</td></tr></tbody></table>

**Notes.** No previous photodetachment rates were included in the database.

cross section of approximately $3 \times 10^{-21}$ cm$^2$ was measured (Petrignani et al. 2010), this would yield significantly increased photorates as presented in Table 1.
<table><caption>**Table 6.** Calculated photodissociation & photoionization rates of C₂H₃.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>3.04E-09</td><td>2.01E-09</td></tr><tr><td>Mathis '83</td><td>2.56E-09</td><td>1.43E-09</td></tr><tr><td>4000 K</td><td>3.68E-06</td><td>2.08E-12</td></tr><tr><td>10 000 K</td><td>1.38E-08</td><td>3.28E-10</td></tr><tr><td>20 000 K</td><td>3.44E-09</td><td>1.67E-09</td></tr><tr><td>Lyman-α</td><td>7.87E-12</td><td>4.19E-09</td></tr><tr><td>Solar</td><td>1.68E-06</td><td>1.77E-09</td></tr><tr><td>TW-Hya</td><td>7.76E-09</td><td>2.74E-09</td></tr><tr><td>Cosmic-ray UV</td><td>4.81E-14</td><td>2.09E-13</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 7.** Calculated photodissociation & photoionization rates of C₂H₅.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.55E-09</td><td>4.08E-10</td></tr><tr><td>Mathis '83</td><td>9.98E-10</td><td>2.82E-10</td></tr><tr><td>4000 K</td><td>6.42E-08</td><td>1.54E-12</td></tr><tr><td>10 000 K</td><td>5.86E-09</td><td>9.81E-11</td></tr><tr><td>20 000 K</td><td>1.96E-09</td><td>3.37E-10</td></tr><tr><td>Lyman-α</td><td>7.87E-12</td><td>8.69E-10</td></tr><tr><td>Solar</td><td>6.60E-08</td><td>3.65E-11</td></tr><tr><td>TW-Hya</td><td>1.43E-09</td><td>5.79E-10</td></tr><tr><td>Cosmic-ray UV</td><td>6.26E-14</td><td>4.19E-14</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 8.** Calculated photoionization rates of I-C₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.37E-09</td></tr><tr><td>Mathis '83</td><td>9.79E-10</td></tr><tr><td>4000 K</td><td>3.41E-13</td></tr><tr><td>10 000 K</td><td>1.88E-10</td></tr><tr><td>20 000 K</td><td>1.11E-09</td></tr><tr><td>Lyman-α</td><td>3.83E-09</td></tr><tr><td>Solar</td><td>1.53E-10</td></tr><tr><td>TW-Hya</td><td>2.56E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.63E-13</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

<table><caption>**Table 10.** Calculated photoionization rates of HC₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.09E-09</td></tr><tr><td>Mathis '83</td><td>1.45E-09</td></tr><tr><td>4000 K</td><td>3.57E-12</td></tr><tr><td>10 000 K</td><td>4.41E-10</td></tr><tr><td>20 000 K</td><td>1.70E-09</td></tr><tr><td>Lyman-α</td><td>4.72E-09</td></tr><tr><td>Solar</td><td>1.96E-10</td></tr><tr><td>TW-Hya</td><td>3.13E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.19E-13</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

<table><caption>**Table 9.** Calculated photoionization rates of c-C₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.33E-09</td></tr><tr><td>Mathis '83</td><td>9.55E-10</td></tr><tr><td>4000 K</td><td>2.98E-13</td></tr><tr><td>10 000 K</td><td>1.78E-10</td></tr><tr><td>20 000 K</td><td>1.08E-09</td></tr><tr><td>Lyman-α</td><td>4.19E-09</td></tr><tr><td>Solar</td><td>1.65E-10</td></tr><tr><td>TW-Hya</td><td>2.66E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.65E-13</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

<table><caption>**Table 11.** Calculated photoionization rates of c-C₃H₂.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.80E-09</td></tr><tr><td>Mathis '83</td><td>1.26E-09</td></tr><tr><td>4000 K</td><td>1.46E-12</td></tr><tr><td>10 000 K</td><td>3.19E-10</td></tr><tr><td>20 000 K</td><td>1.45E-09</td></tr><tr><td>Lyman-α</td><td>4.72E-09</td></tr><tr><td>Solar</td><td>1.90E-10</td></tr><tr><td>TW-Hya</td><td>3.06E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.03E-13</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.
<table><caption>**Table 6.** Calculated photodissociation & photoionization rates of C₂H₃.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>3.04E-09</td><td>2.01E-09</td></tr><tr><td>Mathis '83</td><td>2.56E-09</td><td>1.43E-09</td></tr><tr><td>4000 K</td><td>3.68E-06</td><td>2.08E-12</td></tr><tr><td>10 000 K</td><td>1.38E-08</td><td>3.28E-10</td></tr><tr><td>20 000 K</td><td>3.44E-09</td><td>1.67E-09</td></tr><tr><td>Lyman-α</td><td>7.87E-12</td><td>4.19E-09</td></tr><tr><td>Solar</td><td>1.68E-06</td><td>1.77E-09</td></tr><tr><td>TW-Hya</td><td>7.76E-09</td><td>2.74E-09</td></tr><tr><td>Cosmic-ray UV</td><td>4.81E-14</td><td>2.09E-13</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 7.** Calculated photodissociation & photoionization rates of C₂H₅.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.55E-09</td><td>4.08E-10</td></tr><tr><td>Mathis '83</td><td>9.98E-10</td><td>2.82E-10</td></tr><tr><td>4000 K</td><td>6.42E-08</td><td>1.54E-12</td></tr><tr><td>10 000 K</td><td>5.86E-09</td><td>9.81E-11</td></tr><tr><td>20 000 K</td><td>1.96E-09</td><td>3.37E-10</td></tr><tr><td>Lyman-α</td><td>7.87E-12</td><td>8.69E-10</td></tr><tr><td>Solar</td><td>6.60E-08</td><td>3.65E-11</td></tr><tr><td>TW-Hya</td><td>1.43E-09</td><td>5.79E-10</td></tr><tr><td>Cosmic-ray UV</td><td>6.26E-14</td><td>4.19E-14</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 8.** Calculated photoionization rates of l-C₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.37E-09</td></tr><tr><td>Mathis '83</td><td>9.79E-10</td></tr><tr><td>4000 K</td><td>3.41E-13</td></tr><tr><td>10 000 K</td><td>1.88E-10</td></tr><tr><td>20 000 K</td><td>1.11E-09</td></tr><tr><td>Lyman-α</td><td>3.83E-09</td></tr><tr><td>Solar</td><td>1.53E-10</td></tr><tr><td>TW-Hya</td><td>2.56E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.63E-13</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

<table><caption>**Table 10.** Calculated photoionization rates of HC₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.09E-09</td></tr><tr><td>Mathis '83</td><td>1.45E-09</td></tr><tr><td>4000 K</td><td>3.57E-12</td></tr><tr><td>10 000 K</td><td>4.41E-10</td></tr><tr><td>20 000 K</td><td>1.70E-09</td></tr><tr><td>Lyman-α</td><td>4.72E-09</td></tr><tr><td>Solar</td><td>1.96E-10</td></tr><tr><td>TW-Hya</td><td>3.13E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.19E-13</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

<table><caption>**Table 9.** Calculated photoionization rates of c-C₃H.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.33E-09</td></tr><tr><td>Mathis '83</td><td>9.55E-10</td></tr><tr><td>4000 K</td><td>2.98E-13</td></tr><tr><td>10 000 K</td><td>1.78E-10</td></tr><tr><td>20 000 K</td><td>1.08E-09</td></tr><tr><td>Lyman-α</td><td>4.19E-09</td></tr><tr><td>Solar</td><td>1.65E-10</td></tr><tr><td>TW-Hya</td><td>2.66E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.65E-13</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

<table><caption>**Table 11.** Calculated photoionization rates of c-C₃H₂.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.80E-09</td></tr><tr><td>Mathis '83</td><td>1.26E-09</td></tr><tr><td>4000 K</td><td>1.46E-12</td></tr><tr><td>10 000 K</td><td>3.19E-10</td></tr><tr><td>20 000 K</td><td>1.45E-09</td></tr><tr><td>Lyman-α</td><td>4.72E-09</td></tr><tr><td>Solar</td><td>1.90E-10</td></tr><tr><td>TW-Hya</td><td>3.06E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.03E-13</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.
<table><caption>**Table 12.** Calculated photoionization rates of C<sub>3</sub>H<sub>3</sub>.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>6.30E-10</td><td>1.84E-09</td></tr><tr><td>Mathis '83</td><td>4.55E-10</td><td>1.27E-09</td></tr><tr><td>4000 K</td><td>3.28E-07</td><td>5.86E-12</td></tr><tr><td>10 000 K</td><td>3.35E-09</td><td>4.55E-10</td></tr><tr><td>20 000 K</td><td>7.52E-09</td><td>1.52E-09</td></tr><tr><td>Lyman-α</td><td>0</td><td>3.64E-09</td></tr><tr><td>Solar</td><td>2.78E-07</td><td>1.57E-10</td></tr><tr><td>TW-Hya</td><td>1.08E-09</td><td>2.49E-09</td></tr><tr><td>Cosmic-ray UV</td><td>8.62E-15</td><td>1.79E-13</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 13.** Calculated photodetachment rates of C<sub>4</sub>H<sup>-</sup>.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.93E-09</td></tr><tr><td>Mathis '83</td><td>1.31E-09</td></tr><tr><td>4000 K</td><td>3.97E-07</td></tr><tr><td>10 000 K</td><td>6.44E-09</td></tr><tr><td>20 000 K</td><td>1.99E-09</td></tr><tr><td>Lyman-α</td><td>9.77E-10</td></tr><tr><td>Solar</td><td>4.95E-07</td></tr><tr><td>TW-Hya</td><td>2.52E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.09E-13</td></tr></tbody></table>

Notes. No previous photodetachment rates were included in the database.

<table><caption>**Table 14.** Calculated photodetachment rates of C<sub>6</sub>H<sup>-</sup>.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.08E-09</td></tr><tr><td>Mathis '83</td><td>7.14E-10</td></tr><tr><td>4000 K</td><td>1.36E-07</td></tr><tr><td>10 000 K</td><td>3.27E-09</td></tr><tr><td>20 000 K</td><td>1.13E-09</td></tr><tr><td>Lyman-α</td><td>5.98E-10</td></tr><tr><td>Solar</td><td>1.67E-07</td></tr><tr><td>TW-Hya</td><td>1.28E-09</td></tr><tr><td>Cosmic-ray UV</td><td>6.59E-14</td></tr></tbody></table>

Notes. No previous photodetachment rates were included in the database.

### 3.2. CH (methylidyne)

In the original publication of the database, an absorption/dissociation cross section of CH is included along with a tentative photoionization cross section. The photodissociation cross section is based on ab initio calculations (van Dishoeck 1987) and the included photoionization cross section was based on a photoelectron spectrum (Barsuhn & Nesbet 1978).

Recently, the photoion efficiency curve of CH was measured by mixing a CH<sub>4</sub> precursor diluted in He with F radicals to abstract the H atoms (Gans et al. 2016). As CH was produced by means of a series of exothermic H-abstractions, some of the excess energy populated the v = 1, 2 levels of the neutral

ground state, but these contribute negligibly to the measured total ion yield above the ionization threshold which is measured at 10.640 eV (or 116.53 nm).

Recent theoretical calculations on the absolute photoionization cross section have recently been performed (Wang et al. 2021) and these are used to scale the total ion yield measured by Gans et al. Their measurements reach 103.3 nm but display a linear increase in their total ion yields. Here we extrapolate this linear trend upward to 91.2 nm.

### 3.3. C<sub>2</sub> (dicarbon, carbon dimer)

As was the case with methylidyne, the photodissociation cross section of the dicarbon molecule has been computed as the molecule's absorption spectrum is extremely difficult to measure due to its radical nature. Cross sections were previously computed by Pouilly et al. (1983) but the dissociation energy has been recently been experimentally determined as 50 390.5 cm<sup>-1</sup> (198.45 nm) (Borsovszky et al. 2021). The ionization energy from the X<sup>1</sup>Σ<sup>+</sup> ground state is 11.866 eV (104.49 nm) and from the first excited (a<sup>3</sup>Π<sub>u</sub>) state it is 11.790 eV (105.16 nm).

The total ion yield has been recorded by Harper et al. (2020a). It has been scaled so its intensity matches the computed cross section of C<sub>2</sub> from the ground state where a maximum of 50 Mb at 14.5 eV (85.5 nm) was found (Toffoli & Lucchese 2004) which is on par with previous calculations (Padial et al. 1985).

### 3.4. C<sub>2</sub>H (ethynyl)

The photodissociation cross section of the ethynyl radical was calculated in the work of van Hemert & van Dishoeck (2008). More recently, the ionization threshold of C<sub>2</sub>H (IE = 11.641 eV = 106.50 nm) and the total ion yield have both been measured from just above threshold up to 12 eV (Gans et al. 2017). Akin to the cross section of CH<sub>3</sub>, the total ion yield is extended up to 90 nm and scaled to 50 Mb which is comparable to both C<sub>2</sub> and C<sub>2</sub>H<sub>2</sub>.

### 3.5. C<sub>2</sub>H<sup>-</sup>

Inclusion of anions in astrochemical models has been done by adopting an empirical formula for the photodetachment cross sections which is dependent on the electron affinity of the neutral and the absolute cross section at large photon energies (Millar et al. 2007). The absolute photodetachment cross section of C<sub>2</sub>H<sup>-</sup> has been measured with 22-pole ion trap technology
<table><caption>**Table 12.** Calculated photoionization rates of C<sub>3</sub>H<sub>3</sub>.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>6.30E-10</td><td>1.84E-09</td></tr><tr><td>Mathis '83</td><td>4.55E-10</td><td>1.27E-09</td></tr><tr><td>4000 K</td><td>3.28E-07</td><td>5.86E-12</td></tr><tr><td>10 000 K</td><td>3.35E-09</td><td>4.55E-10</td></tr><tr><td>20 000 K</td><td>7.52E-09</td><td>1.52E-09</td></tr><tr><td>Lyman-α</td><td>0</td><td>3.64E-09</td></tr><tr><td>Solar</td><td>2.78E-07</td><td>1.57E-10</td></tr><tr><td>TW-Hya</td><td>1.08E-09</td><td>2.49E-09</td></tr><tr><td>Cosmic-ray UV</td><td>8.62E-15</td><td>1.79E-13</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 13.** Calculated photodetachment rates of C<sub>4</sub>H<sup>-</sup>.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.93E-09</td></tr><tr><td>Mathis '83</td><td>1.31E-09</td></tr><tr><td>4000 K</td><td>3.97E-07</td></tr><tr><td>10 000 K</td><td>6.44E-09</td></tr><tr><td>20 000 K</td><td>1.99E-09</td></tr><tr><td>Lyman-α</td><td>9.77E-10</td></tr><tr><td>Solar</td><td>4.95E-07</td></tr><tr><td>TW-Hya</td><td>2.52E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.09E-13</td></tr></tbody></table>

**Notes.** No previous photodetachment rates were included in the database.

<table><caption>**Table 14.** Calculated photodetachment rates of C<sub>6</sub>H<sup>-</sup>.</caption><thead><tr><th>Radiation field</th><th>Photodetachment (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.08E-09</td></tr><tr><td>Mathis '83</td><td>7.14E-10</td></tr><tr><td>4000 K</td><td>1.36E-07</td></tr><tr><td>10 000 K</td><td>3.27E-09</td></tr><tr><td>20 000 K</td><td>1.13E-09</td></tr><tr><td>Lyman-α</td><td>5.98E-10</td></tr><tr><td>Solar</td><td>1.67E-07</td></tr><tr><td>TW-Hya</td><td>1.28E-09</td></tr><tr><td>Cosmic-ray UV</td><td>6.59E-14</td></tr></tbody></table>

**Notes.** No previous photodetachment rates were included in the database.

### 3.2. CH (methylidyne)

In the original publication of the database, an absorption/dissociation cross section of CH is included along with a tentative photoionization cross section. The photodissociation cross section is based on ab initio calculations (van Dishoeck 1987) and the included photoionization cross section was based on a photoelectron spectrum (Barsuhn & Nesbet 1978).

Recently, the photoion efficiency curve of CH was measured by mixing a CH<sub>4</sub> precursor diluted in He with F radicals to abstract the H atoms (Gans et al. 2016). As CH was produced by means of a series of exothermic H-abstractions, some of the excess energy populated the v = 1, 2 levels of the neutral

ground state, but these contribute negligibly to the measured total ion yield above the ionization threshold which is measured at 10.640 eV (or 116.53 nm).

Recent theoretical calculations on the absolute photoionization cross section have recently been performed (Wang et al. 2021) and these are used to scale the total ion yield measured by Gans et al. Their measurements reach 103.3 nm but display a linear increase in their total ion yields. Here we extrapolate this linear trend upward to 91.2 nm.

### 3.3. C<sub>2</sub> (dicarbon, carbon dimer)

As was the case with methylidyne, the photodissociation cross section of the dicarbon molecule has been computed as the molecule's absorption spectrum is extremely difficult to measure due to its radical nature. Cross sections were previously computed by Pouilly et al. (1983) but the dissociation energy has been recently been experimentally determined as 50 390.5 cm<sup>-1</sup> (198.45 nm) (Borsovszky et al. 2021). The ionization energy from the X<sup>1</sup>Σ<sup>+</sup> ground state is 11.866 eV (104.49 nm) and from the first excited (α<sup>3</sup>Π<sub>u</sub>) state it is 11.790 eV (105.16 nm).

The total ion yield has been recorded by Harper et al. (2020a). It has been scaled so its intensity matches the computed cross section of C<sub>2</sub> from the ground state where a maximum of 50 Mb at 14.5 eV (85.5 nm) was found (Toffoli & Lucchese 2004) which is on par with previous calculations (Padial et al. 1985).

### 3.4. C<sub>2</sub>H (ethynyl)

The photodissociation cross section of the ethynyl radical was calculated in the work of van Hemert & van Dishoeck (2008). More recently, the ionization threshold of C<sub>2</sub>H (IE = 11.641 eV = 106.50 nm) and the total ion yield have both been measured from just above threshold up to 12 eV (Gans et al. 2017). Akin to the cross section of CH<sub>3</sub>, the total ion yield is extended up to 90 nm and scaled to 50 Mb which is comparable to both C<sub>2</sub> and C<sub>2</sub>H<sub>2</sub>.

### 3.5. C<sub>2</sub>H<sup>-</sup>

Inclusion of anions in astrochemical models has been done by adopting an empirical formula for the photodetachment cross sections which is dependent on the electron affinity of the neutral and the absolute cross section at large photon energies (Millar et al. 2007). The absolute photodetachment cross section of C<sub>2</sub>H<sup>-</sup> has been measured with 22-pole ion trap technology
<table><caption>**Table 15.** Calculated photodissociation rates of OH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.78E-10</td><td>4.26E-10</td><td>1.13</td></tr><tr><td>Mathis '83</td><td>2.73E-10</td><td>2.86E-10</td><td>1.05</td></tr><tr><td>4000 K</td><td>1.91E-10</td><td>2.14E-10</td><td>1.12</td></tr><tr><td>10 000 K</td><td>2.02E-10</td><td>2.27E-10</td><td>1.12</td></tr><tr><td>20 000 K</td><td>3.50E-10</td><td>3.75E-10</td><td>1.07</td></tr><tr><td>Lyman-α</td><td>6.40E-10</td><td>7.20E-10</td><td>1.13</td></tr><tr><td>Solar</td><td>1.73E-10</td><td>1.92E-10</td><td>1.11</td></tr><tr><td>TW-Hya</td><td>5.15E-10</td><td>5.68E-10</td><td>1.10</td></tr><tr><td>Cosmic-ray UV</td><td>4.75E-14</td><td>5.34E-14</td><td>1.12</td></tr></tbody></table>

<table><caption>**Table 16.** Calculated photoionization rates of OH.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.59E-11</td></tr><tr><td>Mathis '83</td><td>1.86E-11</td></tr><tr><td>4000 K</td><td>1.50E-17</td></tr><tr><td>10 000 K</td><td>8.23E-13</td></tr><tr><td>20 000 K</td><td>1.65E-11</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>2.87E-12</td></tr><tr><td>TW-Hya</td><td>1.01E-11</td></tr><tr><td>Cosmic-ray UV</td><td>1.65E-15</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

<table><caption>**Table 17.** Calculated photoionization rates of HO₂.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>8.39E-11</td></tr><tr><td>Mathis '83</td><td>6.51E-11</td></tr><tr><td>4000 K</td><td>7.88E-16</td></tr><tr><td>10 000 K</td><td>6.35E-12</td></tr><tr><td>20 000 K</td><td>7.73E-11</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>1.51E-12</td></tr><tr><td>TW-Hya</td><td>1.85E-11</td></tr><tr><td>Cosmic-ray UV</td><td>5.58E-15</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

<table><caption>**Table 18.** Calculated photoionization rates of HCO.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>8.79E-10</td></tr><tr><td>Mathis '83</td><td>6.33E-10</td></tr><tr><td>4000 K</td><td>7.63E-13</td></tr><tr><td>10 000 K</td><td>1.27E-10</td></tr><tr><td>20 000 K</td><td>7.31E-10</td></tr><tr><td>Lyman-α</td><td>1.11E-09</td></tr><tr><td>Solar</td><td>5.11E-11</td></tr><tr><td>TW-Hya</td><td>8.03E-10</td></tr><tr><td>Cosmic-ray UV</td><td>8.16E-14</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

at several photon energies which allows the construction of the cross sections based on the aforementioned empirical formulas with greater than 10% accuracy (Best et al. 2011).

### 3.6. C₂H₃ (vinyl)

The absorption cross section of the vinyl radical between 225 and 238 nm has been measured by Fahr et al. (1998) who obtain a maximum absorbance of 10 Mb at 225 nm. This is the only recorded cross section of the vinyl radical but an older absorption spectrum of the C₂H₃ radical was recorded between 360 and 500 nm (Hunziker et al. 1983). Their absorption spectrum has been fitted with several Gaussians and the highest peaks scaled to 10 Mb. The curve measured by Fahr et al. (1998), however, resembles the onset of a Gaussian peak and the curve steepness also compares well with the total ion yield recorded by Garcia et al. (2021). Here we simulate an absorption with a Gaussian using the measurements by Fahr et al. which yields a maximum at 40 Mb around 200 nm. This intensity is comparable to other hydrocarbons in the database although further calculations and measurements of this radical would be of great interest.

Other work relevant to the photodissociation of C₂H₃ includes a photodissociation study by Ahmed et al. (1999) who found the threshold for photodissociation of C₂H₃ just above 1 eV (1240 nm). Up to 6 eV (207 nm) they find that the fragments formed involve a H atom and various electronically excited states of the C₂H₃ planar form or the H₂CC molecule. As with other photodissociation cross sections in the database that have been obtained by calculations, a baseline absorption of 0.05 Mb from the dissociation threshold up to the Lyman-α limit at 91.2 nm is added to the simulated cross section.

The adiabatic ionization energy of the vinyl radical has been measured as 8.462 eV (146.5 nm) (Wu et al. 2019). The photoionization of vinyl has been studied to include its first two excited states (ā⁺³A'' & Ā⁺¹A'') and its total ion yield was measured up to 12 eV (103 nm) (Garcia et al. 2021). This total ion yield has been scaled to match the intensity of the cross sections of C₂H₂, and C₂H₆ (Cooper et al. 1995; Kameta et al. 1996; Toffoli & Lucchese 2004).

### 3.7. C₂H₅ (ethyl)

The ethyl cation, C₂H₅⁺ has been detected with the ROSINA probe on 67P along with C₂H₄⁺, C₂H₃⁺, C₂H₂⁺, and many others (Beth et al. 2020) and is included here in the database for the first time.

While no absolute photodissociation cross section has been recorded for the ethyl radical, its absorption spectrum was recorded by Munk et al. (1986). They observed a broad absorption centered around 245 nm which originates from an excitation
<table><caption>**Table 15.** Calculated photodissociation rates of OH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>3.78E-10</td><td>4.26E-10</td><td>1.13</td></tr><tr><td>Mathis '83</td><td>2.73E-10</td><td>2.86E-10</td><td>1.05</td></tr><tr><td>4000 K</td><td>1.91E-10</td><td>2.14E-10</td><td>1.12</td></tr><tr><td>10 000 K</td><td>2.02E-10</td><td>2.27E-10</td><td>1.12</td></tr><tr><td>20 000 K</td><td>3.50E-10</td><td>3.75E-10</td><td>1.07</td></tr><tr><td>Lyman-α</td><td>6.40E-10</td><td>7.20E-10</td><td>1.13</td></tr><tr><td>Solar</td><td>1.73E-10</td><td>1.92E-10</td><td>1.11</td></tr><tr><td>TW-Hya</td><td>5.15E-10</td><td>5.68E-10</td><td>1.10</td></tr><tr><td>Cosmic-ray UV</td><td>4.75E-14</td><td>5.34E-14</td><td>1.12</td></tr></tbody></table>

<table><caption>**Table 16.** Calculated photoionization rates of OH.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.59E-11</td></tr><tr><td>Mathis '83</td><td>1.86E-11</td></tr><tr><td>4000 K</td><td>1.50E-17</td></tr><tr><td>10 000 K</td><td>8.23E-13</td></tr><tr><td>20 000 K</td><td>1.65E-11</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>2.87E-12</td></tr><tr><td>TW-Hya</td><td>1.01E-11</td></tr><tr><td>Cosmic-ray UV</td><td>1.65E-15</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

<table><caption>**Table 17.** Calculated photoionization rates of HO₂.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>8.39E-11</td></tr><tr><td>Mathis '83</td><td>6.51E-11</td></tr><tr><td>4000 K</td><td>7.88E-16</td></tr><tr><td>10 000 K</td><td>6.35E-12</td></tr><tr><td>20 000 K</td><td>7.73E-11</td></tr><tr><td>Lyman-α</td><td>0</td></tr><tr><td>Solar</td><td>1.51E-12</td></tr><tr><td>TW-Hya</td><td>1.85E-11</td></tr><tr><td>Cosmic-ray UV</td><td>5.58E-15</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

<table><caption>**Table 18.** Calculated photoionization rates of HCO.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>8.79E-10</td></tr><tr><td>Mathis '83</td><td>6.33E-10</td></tr><tr><td>4000 K</td><td>7.63E-13</td></tr><tr><td>10 000 K</td><td>1.27E-10</td></tr><tr><td>20 000 K</td><td>7.31E-10</td></tr><tr><td>Lyman-α</td><td>1.11E-09</td></tr><tr><td>Solar</td><td>5.11E-11</td></tr><tr><td>TW-Hya</td><td>8.03E-10</td></tr><tr><td>Cosmic-ray UV</td><td>8.16E-14</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

at several photon energies which allows the construction of the cross sections based on the aforementioned empirical formulas with greater than 10% accuracy (Best et al. 2011).

### 3.6. C₂H₃ (vinyl)

The absorption cross section of the vinyl radical between 225 and 238 nm has been measured by Fahr et al. (1998) who obtain a maximum absorbance of 10 Mb at 225 nm. This is the only recorded cross section of the vinyl radical but an older absorption spectrum of the C₂H₃ radical was recorded between 360 and 500 nm (Hunziker et al. 1983). Their absorption spectrum has been fitted with several Gaussians and the highest peaks scaled to 10 Mb. The curve measured by Fahr et al. (1998), however, resembles the onset of a Gaussian peak and the curve steepness also compares well with the total ion yield recorded by Garcia et al. (2021). Here we simulate an absorption with a Gaussian using the measurements by Fahr et al. which yields a maximum at 40 Mb around 200 nm. This intensity is comparable to other hydrocarbons in the database although further calculations and measurements of this radical would be of great interest.

Other work relevant to the photodissociation of C₂H₃ includes a photodissociation study by Ahmed et al. (1999) who found the threshold for photodissociation of C₂H₃ just above 1 eV (1240 nm). Up to 6 eV (207 nm) they find that the fragments formed involve a H atom and various electronically excited states of the C₂H₃ planar form or the H₂CC molecule. As with other photodissociation cross sections in the database that have been obtained by calculations, a baseline absorption of 0.05 Mb from the dissociation threshold up to the Lyman-α limit at 91.2 nm is added to the simulated cross section.

The adiabatic ionization energy of the vinyl radical has been measured as 8.462 eV (146.5 nm) (Wu et al. 2019). The photoionization of vinyl has been studied to include its first two excited states (ā⁺³A'' & Ā⁺¹A'') and its total ion yield was measured up to 12 eV (103 nm) (Garcia et al. 2021). This total ion yield has been scaled to match the intensity of the cross sections of C₂H₂, and C₂H₆ (Cooper et al. 1995; Kameta et al. 1996; Toffoli & Lucchese 2004).

### 3.7. C₂H₅ (ethyl)

The ethyl cation, C₂H₅⁺ has been detected with the ROSINA probe on 67P along with C₂H₄⁺, C₂H₃⁺, C₂H₂⁺, and many others (Beth et al. 2020) and is included here in the database for the first time.

While no absolute photodissociation cross section has been recorded for the ethyl radical, its absorption spectrum was recorded by Munk et al. (1986). They observed a broad absorption centered around 245 nm which originates from an excitation
<table><caption>**Table 19.** Calculated photodissociation & photoionization rates of HCOOH.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.03E-09</td><td>2.78E-10</td></tr><tr><td>Mathis '83</td><td>1.35E-09</td><td>2.18E-10</td></tr><tr><td>4000 K</td><td>1.20E-08</td><td>2.74E-15</td></tr><tr><td>10 000 K</td><td>1.28E-09</td><td>2.11E-11</td></tr><tr><td>20 000 K</td><td>1.84E-09</td><td>2.57E-10</td></tr><tr><td>Lyman-α</td><td>1.79E-09</td><td>0</td></tr><tr><td>Solar</td><td>1.41E-08</td><td>1.50E-11</td></tr><tr><td>TW-Hya</td><td>1.77E-09</td><td>9.92E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.04E-13</td><td>2.05E-14</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 20.** Calculated photoionization rates of NH₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>8.96E-11</td><td>1.90E-10</td><td>0.472</td></tr><tr><td>Mathis '83</td><td>7.12E-11</td><td>1.51E-10</td><td>0.472</td></tr><tr><td>4000 K</td><td>7.26E-16</td><td>1.66E-15</td><td>0.437</td></tr><tr><td>10 000 K</td><td>6.59E-12</td><td>1.41E-11</td><td>0.467</td></tr><tr><td>20 000 K</td><td>8.54E-11</td><td>1.80E-10</td><td>0.474</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>—</td></tr><tr><td>Solar</td><td>4.00E-12</td><td>8.71E-12</td><td>0.459</td></tr><tr><td>TW-Hya</td><td>2.70E-11</td><td>5.79E-11</td><td>0.466</td></tr><tr><td>Cosmic-ray UV</td><td>6.31E-15</td><td>1.35E-14</td><td>0.467</td></tr></tbody></table>

<table><caption>**Table 21.** Calculated photodissociation & photoionization rates of HNC.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.70E-09</td><td>1.91E-10</td></tr><tr><td>Mathis '83</td><td>1.13E-09</td><td>1.57E-10</td></tr><tr><td>4000 K</td><td>4.33E-11</td><td>7.85E-16</td></tr><tr><td>10 000 K</td><td>7.07E-10</td><td>1.30E-11</td></tr><tr><td>20 000 K</td><td>1.48E-09</td><td>1.91E-10</td></tr><tr><td>Lyman-α</td><td>1.38E-09</td><td>0</td></tr><tr><td>Solar</td><td>1.04E-10</td><td>1.45E-11</td></tr><tr><td>TW-Hya</td><td>1.75E-09</td><td>7.52E-11</td></tr><tr><td>Cosmic-ray UV</td><td>1.43E-13</td><td>1.49E-14</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

to the 3s Rydberg orbital whilst at smaller wavelengths, the 3p manifold is populated. No VUV absorption measurements have been recorded below 200 nm, but several studies on the photodissociation of C₂H₅ have been reported which showcase the main dissociation pathway to be the loss of H and then different rearrangements of the C₂H₄ moiety that are energy-dependent, for instance, the 3s manifold appears to produce ethene whilst the 3p manifold produces CH₃CH (Chicharro et al. 2019; Marggi Poullain et al. 2019). In the work of Marggi Poullain et al., they also calculate two more excited states contributing between 200 and 160 nm, namely the Ĉ²A'' and Ī²A' states which are expected to have onsets at approximately 6.8 eV (182 nm) and 7.2 eV (172 nm), respectively. Two absorption peaks are simulated for these states with Gaussians to bridge the gap between the absorption spectrum from Munk et al. and the absolute photoionization cross section of C₂H₅ which was

measured by Gans et al. (2011b). Further measurements and calculations of the photodissociation characteristics of the ethyl radical would be highly valued to validate the modest scaling of the intensity of our simulated photodissociation cross section which reaches 20 Mb at its maximum for dissociation via the Ĉ²A'' and Ī²A' states.

### 3.8. I-C₃H and c-C₃H

The photoionization dynamics of C₃Hₓ (x = 0–3) isomers were recently investigated by Garcia et al. (2018) where C₃H isomers were produced by means of H abstraction from propyne (CH₃CCH) with F radicals. A total ion yield was obtained of C₃H isomers, whose signal consisted both of ions of linear and cyclic C₃H geometries. By using the slow photoelectron spectrum methodology, the vertical ionization energies of I-C₃H
<table><caption>**Table 19.** Calculated photodissociation & photoionization rates of HCOOH.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.03E-09</td><td>2.78E-10</td></tr><tr><td>Mathis '83</td><td>1.35E-09</td><td>2.18E-10</td></tr><tr><td>4000 K</td><td>1.20E-08</td><td>2.74E-15</td></tr><tr><td>10 000 K</td><td>1.28E-09</td><td>2.11E-11</td></tr><tr><td>20 000 K</td><td>1.84E-09</td><td>2.57E-10</td></tr><tr><td>Lyman-α</td><td>1.79E-09</td><td>0</td></tr><tr><td>Solar</td><td>1.41E-08</td><td>1.50E-11</td></tr><tr><td>TW-Hya</td><td>1.77E-09</td><td>9.92E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.04E-13</td><td>2.05E-14</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 20.** Calculated photoionization rates of NH₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>8.96E-11</td><td>1.90E-10</td><td>0.472</td></tr><tr><td>Mathis '83</td><td>7.12E-11</td><td>1.51E-10</td><td>0.472</td></tr><tr><td>4000 K</td><td>7.26E-16</td><td>1.66E-15</td><td>0.437</td></tr><tr><td>10 000 K</td><td>6.59E-12</td><td>1.41E-11</td><td>0.467</td></tr><tr><td>20 000 K</td><td>8.54E-11</td><td>1.80E-10</td><td>0.474</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>4.00E-12</td><td>8.71E-12</td><td>0.459</td></tr><tr><td>TW-Hya</td><td>2.70E-11</td><td>5.79E-11</td><td>0.466</td></tr><tr><td>Cosmic-ray UV</td><td>6.31E-15</td><td>1.35E-14</td><td>0.467</td></tr></tbody></table>

<table><caption>**Table 21.** Calculated photodissociation & photoionization rates of HNC.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.70E-09</td><td>1.91E-10</td></tr><tr><td>Mathis '83</td><td>1.13E-09</td><td>1.57E-10</td></tr><tr><td>4000 K</td><td>4.33E-11</td><td>7.85E-16</td></tr><tr><td>10 000 K</td><td>7.07E-10</td><td>1.30E-11</td></tr><tr><td>20 000 K</td><td>1.48E-09</td><td>1.91E-10</td></tr><tr><td>Lyman-α</td><td>1.38E-09</td><td>0</td></tr><tr><td>Solar</td><td>1.04E-10</td><td>1.45E-11</td></tr><tr><td>TW-Hya</td><td>1.75E-09</td><td>7.52E-11</td></tr><tr><td>Cosmic-ray UV</td><td>1.43E-13</td><td>1.49E-14</td></tr></tbody></table>

Notes. No rates were previously included in the database.

to the 3s Rydberg orbital whilst at smaller wavelengths, the 3p manifold is populated. No VUV absorption measurements have been recorded below 200 nm, but several studies on the photodissociation of C₂H₅ have been reported which showcase the main dissociation pathway to be the loss of H and then different rearrangements of the C₂H₄ moiety that are energy-dependent, for instance, the 3s manifold appears to produce ethene whilst the 3p manifold produces CH₃CH (Chicharro et al. 2019; Marggi Poullain et al. 2019). In the work of Marggi Poullain et al., they also calculate two more excited states contributing between 200 and 160 nm, namely the Ĉ²A'' and Ī²A' states which are expected to have onsets at approximately 6.8 eV (182 nm) and 7.2 eV (172 nm), respectively. Two absorption peaks are simulated for these states with Gaussians to bridge the gap between the absorption spectrum from Munk et al. and the absolute photoionization cross section of C₂H₅ which was

measured by Gans et al. (2011b). Further measurements and calculations of the photodissociation characteristics of the ethyl radical would be highly valued to validate the modest scaling of the intensity of our simulated photodissociation cross section which reaches 20 Mb at its maximum for dissociation via the Ĉ²A'' and Ī²A' states.

### 3.8. I-C₃H and c-C₃H

The photoionization dynamics of C₃Hₓ (x = 0–3) isomers were recently investigated by Garcia et al. (2018) where C₃H isomers were produced by means of H abstraction from propyne (CH₃CCH) with F radicals. A total ion yield was obtained of C₃H isomers, whose signal consisted both of ions of linear and cyclic C₃H geometries. By using the slow photoelectron spectrum methodology, the vertical ionization energies of I-C₃H
<table><caption>**Table 22.** Calculated photodissociation & photoionization rates of HNCO.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.56E-09</td><td>1.03E-10</td></tr><tr><td>Mathis '83</td><td>1.72E-09</td><td>8.43E-11</td></tr><tr><td>4000 K</td><td>7.47E-09</td><td>6.18E-16</td></tr><tr><td>10 000 K</td><td>1.18E-09</td><td>7.29E-12</td></tr><tr><td>20 000 K</td><td>2.17E-09</td><td>1.01E-10</td></tr><tr><td>Lyman-α</td><td>4.65E-09</td><td>0</td></tr><tr><td>Solar</td><td>9.94E-09</td><td>6.89E-12</td></tr><tr><td>TW-Hya</td><td>3.39E-09</td><td>4.49E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.66E-13</td><td>7.43E-15</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 23.** Calculated photoionization rates of CH<sub>3</sub>CHO and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>8.37E-10</td><td>8.34E-10</td><td>1.00</td></tr><tr><td>Mathis '83</td><td>5.93E-10</td><td>6.05E-10</td><td>0.98</td></tr><tr><td>4000 K</td><td>1.33E-13</td><td>8.25E-14</td><td>1.61</td></tr><tr><td>10 000 K</td><td>1.11E-10</td><td>9.37E-11</td><td>1.18</td></tr><tr><td>20 000 K</td><td>6.47E-10</td><td>6.83E-10</td><td>0.95</td></tr><tr><td>Lyman-α</td><td>1.95E-10</td><td>1.93E-10</td><td>1.01</td></tr><tr><td>Solar</td><td>2.66E-11</td><td>2.36E-11</td><td>1.13</td></tr><tr><td>TW-Hya</td><td>3.60E-10</td><td>2.92E-10</td><td>1.23</td></tr><tr><td>Cosmic-ray UV</td><td>7.28E-14</td><td>6.92E-14</td><td>1.05</td></tr></tbody></table>

<table><caption>**Table 24.** Calculated photodissociation & photoionization rates of CH<sub>3</sub>OCH<sub>3</sub>.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.04E-09</td><td>1.15E-09</td></tr><tr><td>Mathis '83</td><td>1.39E-09</td><td>8.45E-10</td></tr><tr><td>4000 K</td><td>6.91E-10</td><td>1.93E-13</td></tr><tr><td>10 000 K</td><td>1.31E-09</td><td>1.41E-10</td></tr><tr><td>20 000 K</td><td>1.90E-09</td><td>9.60E-10</td></tr><tr><td>Lyman-α</td><td>1.19E-09</td><td>3.00E-09</td></tr><tr><td>Solar</td><td>7.21E-10</td><td>1.42E-10</td></tr><tr><td>TW-Hya</td><td>1.37E-09</td><td>2.02E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.76E-13</td><td>1.35E-13</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

and c-C<sub>3</sub>H were found to be 9.118 eV (136.0 nm) and 9.830 eV (126.1 nm), respectively. Since there are no strong autoionizing resonances present in the combined ionization efficiency spectra of the isomers, the total ion yield of the individual isomers can be convincingly synthesized by integrating over the fitted TPES of the two contributing isomers. This gives the two total ion yields simple step functions which are scaled to 30 Mb. The reasoning for this is the following. Total photoabsorption cross sections of neutral alkanes appear to follow a simple trend where the maxima of the cross sections in the VUV range scales approximately linearly with the number of carbon atoms (Kameta et al. 1992). Such a trend would predict approximately 70 Mb maximum considering the cross sections of CH and C<sub>2</sub>H. This is, however not as straight-forward when it comes to radical species as other radicals including three and four carbon atoms, for instance,

propargyl (Savee et al. 2012) and 2-butyne-1-yl (Hrodmarsson et al. 2019b), have significantly smaller cross sections (between 10 and 25 Mb) in comparison to their closed-shell alkane counterparts. There are also discrepancies between calculations and measurements of the absolute maxima of the cross sections of hydrocarbon radicals (Huang et al. 2018; Hartweg et al. 2020). Hence, we cautiously give a scaling of the order 30 Mb with the caveat that the error is likely within an order of magnitude.

### 3.9. HC<sub>3</sub>H (t-C<sub>3</sub>H<sub>2</sub>) and c-C<sub>3</sub>H<sub>2</sub>

The total ion yields of both HC<sub>3</sub>H and c-C<sub>3</sub>H<sub>2</sub> have been recorded by Garcia et al. (2018). In a manner similar to the C<sub>3</sub>H isomers, both isomers were identified in the same mass channel. Again, by integrating the calculated TPES of the
<table><caption>**Table 22.** Calculated photodissociation & photoionization rates of HNCO.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.56E-09</td><td>1.03E-10</td></tr><tr><td>Mathis '83</td><td>1.72E-09</td><td>8.43E-11</td></tr><tr><td>4000 K</td><td>7.47E-09</td><td>6.18E-16</td></tr><tr><td>10 000 K</td><td>1.18E-09</td><td>7.29E-12</td></tr><tr><td>20 000 K</td><td>2.17E-09</td><td>1.01E-10</td></tr><tr><td>Lyman-α</td><td>4.65E-09</td><td>0</td></tr><tr><td>Solar</td><td>9.94E-09</td><td>6.89E-12</td></tr><tr><td>TW-Hya</td><td>3.39E-09</td><td>4.49E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.66E-13</td><td>7.43E-15</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 23.** Calculated photoionization rates of CH<sub>3</sub>CHO and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>8.37E-10</td><td>8.34E-10</td><td>1.00</td></tr><tr><td>Mathis '83</td><td>5.93E-10</td><td>6.05E-10</td><td>0.98</td></tr><tr><td>4000 K</td><td>1.33E-13</td><td>8.25E-14</td><td>1.61</td></tr><tr><td>10 000 K</td><td>1.11E-10</td><td>9.37E-11</td><td>1.18</td></tr><tr><td>20 000 K</td><td>6.47E-10</td><td>6.83E-10</td><td>0.95</td></tr><tr><td>Lyman-α</td><td>1.95E-10</td><td>1.93E-10</td><td>1.01</td></tr><tr><td>Solar</td><td>2.66E-11</td><td>2.36E-11</td><td>1.13</td></tr><tr><td>TW-Hya</td><td>3.60E-10</td><td>2.92E-10</td><td>1.23</td></tr><tr><td>Cosmic-ray UV</td><td>7.28E-14</td><td>6.92E-14</td><td>1.05</td></tr></tbody></table>

<table><caption>**Table 24.** Calculated photodissociation & photoionization rates of CH<sub>3</sub>OCH<sub>3</sub>.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.04E-09</td><td>1.15E-09</td></tr><tr><td>Mathis '83</td><td>1.39E-09</td><td>8.45E-10</td></tr><tr><td>4000 K</td><td>6.91E-10</td><td>1.93E-13</td></tr><tr><td>10 000 K</td><td>1.31E-09</td><td>1.41E-10</td></tr><tr><td>20 000 K</td><td>1.90E-09</td><td>9.60E-10</td></tr><tr><td>Lyman-α</td><td>1.19E-09</td><td>3.00E-09</td></tr><tr><td>Solar</td><td>7.21E-10</td><td>1.42E-10</td></tr><tr><td>TW-Hya</td><td>1.37E-09</td><td>2.02E-09</td></tr><tr><td>Cosmic-ray UV</td><td>1.76E-13</td><td>1.35E-13</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

and c-C<sub>3</sub>H were found to be 9.118 eV (136.0 nm) and 9.830 eV (126.1 nm), respectively. Since there are no strong autoionizing resonances present in the combined ionization efficiency spectra of the isomers, the total ion yield of the individual isomers can be convincingly synthesized by integrating over the fitted TPES of the two contributing isomers. This gives the two total ion yields simple step functions which are scaled to 30 Mb. The reasoning for this is the following. Total photoabsorption cross sections of neutral alkanes appear to follow a simple trend where the maxima of the cross sections in the VUV range scales approximately linearly with the number of carbon atoms (Kameta et al. 1992). Such a trend would predict approximately 70 Mb maximum considering the cross sections of CH and C<sub>2</sub>H. This is, however not as straight-forward when it comes to radical species as other radicals including three and four carbon atoms, for instance,

propargyl (Savee et al. 2012) and 2-butyne-1-yl (Hrodmarsson et al. 2019b), have significantly smaller cross sections (between 10 and 25 Mb) in comparison to their closed-shell alkane counterparts. There are also discrepancies between calculations and measurements of the absolute maxima of the cross sections of hydrocarbon radicals (Huang et al. 2018; Hartweg et al. 2020). Hence, we cautiously give a scaling of the order 30 Mb with the caveat that the error is likely within an order of magnitude.

### 3.9. HC<sub>3</sub>H (t-C<sub>3</sub>H<sub>2</sub>) and c-C<sub>3</sub>H<sub>2</sub>

The total ion yields of both HC<sub>3</sub>H and c-C<sub>3</sub>H<sub>2</sub> have been recorded by Garcia et al. (2018). In a manner similar to the C<sub>3</sub>H isomers, both isomers were identified in the same mass channel. Again, by integrating the calculated TPES of the
<table><caption>**Table 25.** Calculated photodissociation & photoionization rates of CH<sub>3</sub>OCHO.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.25E-09</td><td>2.90E-10</td></tr><tr><td>Mathis '83</td><td>1.48E-09</td><td>2.27E-10</td></tr><tr><td>4000 K</td><td>9.53E-10</td><td>1.85E-10</td></tr><tr><td>10 000 K</td><td>7.04E-10</td><td>4.83E-15</td></tr><tr><td>20 000 K</td><td>1.38E-09</td><td>2.33E-11</td></tr><tr><td>Lyman-α</td><td>2.02E-09</td><td>2.64E-10</td></tr><tr><td>Solar</td><td>3.79E-09</td><td>0</td></tr><tr><td>TW-Hya</td><td>1.01E-09</td><td>1.63E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.61E-13</td><td>2.44E-14</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 26.** Calculated photoionization rates of SH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>1.26E-09</td><td>5.02E-11</td><td>25</td></tr><tr><td>Mathis '83</td><td>9.40E-10</td><td>3.71E-11</td><td>25</td></tr><tr><td>4000 K</td><td>1.11E-13</td><td>5.30E-16</td><td>210</td></tr><tr><td>10 000 K</td><td>1.37E-10</td><td>3.86E-12</td><td>36</td></tr><tr><td>20 000 K</td><td>1.07E-09</td><td>4.50E-11</td><td>24</td></tr><tr><td>Lyman-α</td><td>3.18E-11</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>3.00E-11</td><td>8.86E-13</td><td>34</td></tr><tr><td>TW-Hya</td><td>2.89E-10</td><td>1.10E-11</td><td>26</td></tr><tr><td>Cosmic-ray UV</td><td>1.00E-13</td><td>3.36E-15</td><td>30</td></tr></tbody></table>

<table><caption>**Table 27.** Calculated photodissociation rates of CS and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.69E-09</td><td>9.49E-10</td><td>2.83</td></tr><tr><td>Mathis '83</td><td>1.73E-09</td><td>6.29E-10</td><td>2.75</td></tr><tr><td>4000 K</td><td>6.31E-11</td><td>5.20E-12</td><td>12.1</td></tr><tr><td>10 000 K</td><td>1.37E-09</td><td>2.90E-10</td><td>4.72</td></tr><tr><td>20 000 K</td><td>2.38E-09</td><td>7.64E-10</td><td>3.12</td></tr><tr><td>Lyman-α</td><td>1.34E-09</td><td>8.42E-09</td><td>0.159</td></tr><tr><td>Solar</td><td>1.17E-10</td><td>3.09E-10</td><td>0.379</td></tr><tr><td>TW-Hya</td><td>1.47E-09</td><td>4.95E-09</td><td>0.297</td></tr><tr><td>Cosmic-ray UV</td><td>1.51E-13</td><td>1.93E-13</td><td>0.782</td></tr></tbody></table>

<table><caption>**Table 28.** Calculated photoionization rates of CS and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>1.10E-10</td><td>2.60E-11</td><td>4.23</td></tr><tr><td>Mathis '83</td><td>8.38E-11</td><td>1.84E-11</td><td>4.55</td></tr><tr><td>4000 K</td><td>1.70E-15</td><td>7.27E-16</td><td>2.34</td></tr><tr><td>10 000 K</td><td>9.01E-12</td><td>2.41E-12</td><td>3.74</td></tr><tr><td>20 000 K</td><td>9.77E-11</td><td>2.10E-11</td><td>4.65</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>3.47E-12</td><td>1.89E-13</td><td>18.4</td></tr><tr><td>TW-Hya</td><td>2.72E-11</td><td>3.62E-12</td><td>7.51</td></tr><tr><td>Cosmic-ray UV</td><td>7.63E-15</td><td>2.04E-15</td><td>3.74</td></tr></tbody></table>
<table><caption>**Table 25.** Calculated photodissociation & photoionization rates of CH<sub>3</sub>OCHO.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.25E-09</td><td>2.90E-10</td></tr><tr><td>Mathis '83</td><td>1.48E-09</td><td>2.27E-10</td></tr><tr><td>4000 K</td><td>9.53E-10</td><td>1.85E-10</td></tr><tr><td>10 000 K</td><td>7.04E-10</td><td>4.83E-15</td></tr><tr><td>20 000 K</td><td>1.38E-09</td><td>2.33E-11</td></tr><tr><td>Lyman-α</td><td>2.02E-09</td><td>2.64E-10</td></tr><tr><td>Solar</td><td>3.79E-09</td><td>0</td></tr><tr><td>TW-Hya</td><td>1.01E-09</td><td>1.63E-11</td></tr><tr><td>Cosmic-ray UV</td><td>2.61E-13</td><td>2.44E-14</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 26.** Calculated photoionization rates of SH and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>1.26E-09</td><td>5.02E-11</td><td>25</td></tr><tr><td>Mathis '83</td><td>9.40E-10</td><td>3.71E-11</td><td>25</td></tr><tr><td>4000 K</td><td>1.11E-13</td><td>5.30E-16</td><td>210</td></tr><tr><td>10 000 K</td><td>1.37E-10</td><td>3.86E-12</td><td>36</td></tr><tr><td>20 000 K</td><td>1.07E-09</td><td>4.50E-11</td><td>24</td></tr><tr><td>Lyman-α</td><td>3.18E-11</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>3.00E-11</td><td>8.86E-13</td><td>34</td></tr><tr><td>TW-Hya</td><td>2.89E-10</td><td>1.10E-11</td><td>26</td></tr><tr><td>Cosmic-ray UV</td><td>1.00E-13</td><td>3.36E-15</td><td>30</td></tr></tbody></table>

<table><caption>**Table 27.** Calculated photodissociation rates of CS and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.69E-09</td><td>9.49E-10</td><td>2.83</td></tr><tr><td>Mathis '83</td><td>1.73E-09</td><td>6.29E-10</td><td>2.75</td></tr><tr><td>4000 K</td><td>6.31E-11</td><td>5.20E-12</td><td>12.1</td></tr><tr><td>10 000 K</td><td>1.37E-09</td><td>2.90E-10</td><td>4.72</td></tr><tr><td>20 000 K</td><td>2.38E-09</td><td>7.64E-10</td><td>3.12</td></tr><tr><td>Lyman-α</td><td>1.34E-09</td><td>8.42E-09</td><td>0.159</td></tr><tr><td>Solar</td><td>1.17E-10</td><td>3.09E-10</td><td>0.379</td></tr><tr><td>TW-Hya</td><td>1.47E-09</td><td>4.95E-09</td><td>0.297</td></tr><tr><td>Cosmic-ray UV</td><td>1.51E-13</td><td>1.93E-13</td><td>0.782</td></tr></tbody></table>

<table><caption>**Table 28.** Calculated photoionization rates of CS and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>1.10E-10</td><td>2.60E-11</td><td>4.23</td></tr><tr><td>Mathis '83</td><td>8.38E-11</td><td>1.84E-11</td><td>4.55</td></tr><tr><td>4000 K</td><td>1.70E-15</td><td>7.27E-16</td><td>2.34</td></tr><tr><td>10 000 K</td><td>9.01E-12</td><td>2.41E-12</td><td>3.74</td></tr><tr><td>20 000 K</td><td>9.77E-11</td><td>2.10E-11</td><td>4.65</td></tr><tr><td>Lyman-α</td><td>0</td><td>0</td><td>–</td></tr><tr><td>Solar</td><td>3.47E-12</td><td>1.89E-13</td><td>18.4</td></tr><tr><td>TW-Hya</td><td>2.72E-11</td><td>3.62E-12</td><td>7.51</td></tr><tr><td>Cosmic-ray UV</td><td>7.63E-15</td><td>2.04E-15</td><td>3.74</td></tr></tbody></table>
<table><caption>**Table 29.** Calculated photodissociation & photoionization rates of H₂CS.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.28E-09</td><td>1.55E-09</td></tr><tr><td>Mathis '83</td><td>1.53E-09</td><td>1.11E-09</td></tr><tr><td>4000 K</td><td>1.10E-08</td><td>1.13E-12</td></tr><tr><td>10 000 K</td><td>2.56E-09</td><td>2.55E-10</td></tr><tr><td>20 000 K</td><td>2.25E-09</td><td>1.29E-09</td></tr><tr><td>Lyman-α</td><td>2.63E-09</td><td>3.36E-09</td></tr><tr><td>Solar</td><td>1.30E-08</td><td>4.95E-08</td></tr><tr><td>TW-Hya</td><td>2.47E-09</td><td>1.83E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.05E-13</td><td>1.64E-13</td></tr></tbody></table>

Notes. No rates were previously included in the database.

<table><caption>**Table 30.** Calculated photodissociation rates of S₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>4.94E-10</td><td>6.56E-10</td><td>0.753</td></tr><tr><td>Mathis '83</td><td>2.87E-10</td><td>3.74E-10</td><td>0.767</td></tr><tr><td>4000 K</td><td>1.63E-07</td><td>1.98E-07</td><td>0.823</td></tr><tr><td>10 000 K</td><td>3.24E-09</td><td>4.27E-09</td><td>0.759</td></tr><tr><td>20 000 K</td><td>4.94E-10</td><td>6.66E-10</td><td>0.742</td></tr><tr><td>Lyman-α</td><td>–</td><td>–</td><td>–</td></tr><tr><td>Solar</td><td>1.62E-07</td><td>2.07E-07</td><td>0.783</td></tr><tr><td>TW-Hya</td><td>7.79E-10</td><td>1.01E-09</td><td>0.771</td></tr><tr><td>Cosmic-ray UV</td><td>6.55E-15</td><td>8.85E-15</td><td>0.740</td></tr></tbody></table>

<table><caption>**Table 31.** Calculated photoionization rates of S₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.30E-09</td><td>1.28E-10</td><td>18</td></tr><tr><td>Mathis '83</td><td>1.62E-09</td><td>9.25E-11</td><td>18</td></tr><tr><td>4000 K</td><td>2.18E-12</td><td>6.46E-14</td><td>34</td></tr><tr><td>10 000 K</td><td>3.82E-10</td><td>1.76E-11</td><td>22</td></tr><tr><td>20 000 K</td><td>1.86E-09</td><td>1.06E-10</td><td>18</td></tr><tr><td>Lyman-α</td><td>8.52E-09</td><td>2.83E-10</td><td>30</td></tr><tr><td>Solar</td><td>3.41E-10</td><td>1.33E-11</td><td>26</td></tr><tr><td>TW-Hya</td><td>5.22E-09</td><td>1.98E-10</td><td>26</td></tr><tr><td>Cosmic-ray UV</td><td>3.01E-13</td><td>1.40E-14</td><td>22</td></tr></tbody></table>

<table><caption>**Table 32.** Calculated photoionization rates of SiH.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>5.34E-09</td></tr><tr><td>Mathis '83</td><td>3.72E-09</td></tr><tr><td>4000 K</td><td>1.22E-10</td></tr><tr><td>10 000 K</td><td>1.55E-09</td></tr><tr><td>20 000 K</td><td>4.56E-09</td></tr><tr><td>Lyman-α</td><td>5.36E-09</td></tr><tr><td>Solar</td><td>3.40E-10</td></tr><tr><td>TW-Hya</td><td>4.41E-09</td></tr><tr><td>Cosmic-ray UV</td><td>4.97E-13</td></tr></tbody></table>

Notes. No previous photoionization rates were included in the database.

individual isomers, we can disentangle them and cautiously scale the photoionization efficiency maxima to 30 Mb.

### 3.10. C₃H₃

An important intermediate in combustion chemistry, the resonantly stabilized propargyl radical is included in the database. The absolute photoionization cross section of propargyl was measured by Savee et al. (2012) and the ionization energy has been measured as 8.70053 eV (142.502 nm) (Jacovella et al. 2013). The photoionization cross section measurements by Savee were significantly larger than a previous measurements (Robinson et al. 2003), but were subsequently replicated and verified (Xu & Pratt 2013).

The photodissociation cross section of propargyl has been pieced together from several studies both experimental and theoretical. An absorption cross section was recorded which peaks around 12 Mb (Fahr et al. 1997). The absorption spectrum of C₃H₃ was also calculated by Eisfeld (2006) who found much stronger absorption features toward longer wavelengths. Experiments have not found these absorption features,
<table><caption>**Table 29.** Calculated photodissociation & photoionization rates of H₂CS.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>2.28E-09</td><td>1.55E-09</td></tr><tr><td>Mathis '83</td><td>1.53E-09</td><td>1.11E-09</td></tr><tr><td>4000 K</td><td>1.10E-08</td><td>1.13E-12</td></tr><tr><td>10 000 K</td><td>2.56E-09</td><td>2.55E-10</td></tr><tr><td>20 000 K</td><td>2.25E-09</td><td>1.29E-09</td></tr><tr><td>Lyman-α</td><td>2.63E-09</td><td>3.36E-09</td></tr><tr><td>Solar</td><td>1.30E-08</td><td>4.95E-08</td></tr><tr><td>TW-Hya</td><td>2.47E-09</td><td>1.83E-09</td></tr><tr><td>Cosmic-ray UV</td><td>2.05E-13</td><td>1.64E-13</td></tr></tbody></table>

**Notes.** No rates were previously included in the database.

<table><caption>**Table 30.** Calculated photodissociation rates of S₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>4.94E-10</td><td>6.56E-10</td><td>0.753</td></tr><tr><td>Mathis '83</td><td>2.87E-10</td><td>3.74E-10</td><td>0.767</td></tr><tr><td>4000 K</td><td>1.63E-07</td><td>1.98E-07</td><td>0.823</td></tr><tr><td>10 000 K</td><td>3.24E-09</td><td>4.27E-09</td><td>0.759</td></tr><tr><td>20 000 K</td><td>4.94E-10</td><td>6.66E-10</td><td>0.742</td></tr><tr><td>Lyman-α</td><td>–</td><td>–</td><td>–</td></tr><tr><td>Solar</td><td>1.62E-07</td><td>2.07E-07</td><td>0.783</td></tr><tr><td>TW-Hya</td><td>7.79E-10</td><td>1.01E-09</td><td>0.771</td></tr><tr><td>Cosmic-ray UV</td><td>6.55E-15</td><td>8.85E-15</td><td>0.740</td></tr></tbody></table>

<table><caption>**Table 31.** Calculated photoionization rates of S₂ and comparisons to previous entries in the database.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th><th>Previous rate (s<sup>-1</sup>)</th><th>This work/previous rate</th></tr></thead><tbody><tr><td>ISRF</td><td>2.30E-09</td><td>1.28E-10</td><td>18</td></tr><tr><td>Mathis '83</td><td>1.62E-09</td><td>9.25E-11</td><td>18</td></tr><tr><td>4000 K</td><td>2.18E-12</td><td>6.46E-14</td><td>34</td></tr><tr><td>10 000 K</td><td>3.82E-10</td><td>1.76E-11</td><td>22</td></tr><tr><td>20 000 K</td><td>1.86E-09</td><td>1.06E-10</td><td>18</td></tr><tr><td>Lyman-α</td><td>8.52E-09</td><td>2.83E-10</td><td>30</td></tr><tr><td>Solar</td><td>3.41E-10</td><td>1.33E-11</td><td>26</td></tr><tr><td>TW-Hya</td><td>5.22E-09</td><td>1.98E-10</td><td>26</td></tr><tr><td>Cosmic-ray UV</td><td>3.01E-13</td><td>1.40E-14</td><td>22</td></tr></tbody></table>

<table><caption>**Table 32.** Calculated photoionization rates of SiH.</caption><thead><tr><th>Radiation field</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>5.34E-09</td></tr><tr><td>Mathis '83</td><td>3.72E-09</td></tr><tr><td>4000 K</td><td>1.22E-10</td></tr><tr><td>10 000 K</td><td>1.55E-09</td></tr><tr><td>20 000 K</td><td>4.56E-09</td></tr><tr><td>Lyman-α</td><td>5.36E-09</td></tr><tr><td>Solar</td><td>3.40E-10</td></tr><tr><td>TW-Hya</td><td>4.41E-09</td></tr><tr><td>Cosmic-ray UV</td><td>4.97E-13</td></tr></tbody></table>

**Notes.** No previous photoionization rates were included in the database.

individual isomers, we can disentangle them and cautiously scale the photoionization efficiency maxima to 30 Mb.

### 3.10. C₃H₃

An important intermediate in combustion chemistry, the resonantly stabilized propargyl radical is included in the database. The absolute photoionization cross section of propargyl was measured by Savee et al. (2012) and the ionization energy has been measured as 8.70053 eV (142.502 nm) (Jacovella et al. 2013). The photoionization cross section measurements by Savee were significantly larger than a previous measurements (Robinson et al. 2003), but were subsequently replicated and verified (Xu & Pratt 2013).

The photodissociation cross section of propargyl has been pieced together from several studies both experimental and theoretical. An absorption cross section was recorded which peaks around 12 Mb (Fahr et al. 1997). The absorption spectrum of C₃H₃ was also calculated by Eisfeld (2006) who found much stronger absorption features toward longer wavelengths. Experiments have not found these absorption features,
<table><caption>**Table 33.** Calculated photodissociation & photoionization rates of HF.</caption><thead><tr><th>Radiation field</th><th>Photodissociation (s<sup>-1</sup>) – this work</th><th>Photoionization (s<sup>-1</sup>) – this work</th></tr></thead><tbody><tr><td>ISRF</td><td>1.38E-10</td><td>0</td></tr><tr><td>Mathis '83</td><td>9.85E-11</td><td>0</td></tr><tr><td>4000 K</td><td>5.31E-13</td><td>0</td></tr><tr><td>10 000 K</td><td>2.88E-11</td><td>0</td></tr><tr><td>20 000 K</td><td>1.17E-10</td><td>0</td></tr><tr><td>Lyman-α</td><td>4.93E-10</td><td>0</td></tr><tr><td>Solar</td><td>2.18E-11</td><td>2.45E-13</td></tr><tr><td>TW-Hya</td><td>3.19E-10</td><td>2.13E-12</td></tr><tr><td>Cosmic-ray UV</td><td>1.93E-13</td><td>2.04E-15</td></tr></tbody></table>

<table><caption>**Table 34.** Summary of all updates and new species added to the database.</caption><thead><tr><th>Species</th><th>Thresh. dissoc. prod.</th><th>Dissoc. thresh. (nm)</th><th>Ioniz./photodet.</th><th>Uncert. dissoc.</th><th>Uncert. ioniz./photodet.</th></tr></thead><tbody><tr><td>H<sub>3</sub><sup>+</sup></td><td>H<sup>+</sup> + H<sub>2</sub></td><td>282</td><td>–</td><td>A</td><td>–</td></tr><tr><td>CH</td><td>C + H</td><td>358</td><td>117</td><td>C</td><td>A</td></tr><tr><td>C<sub>2</sub></td><td>C + C</td><td>193</td><td>102</td><td>B</td><td>B</td></tr><tr><td>C<sub>2</sub>H</td><td>C<sub>2</sub> + H</td><td>253</td><td>107</td><td>B</td><td>B</td></tr><tr><td>C<sub>2</sub>H<sup>-</sup></td><td>–</td><td>–</td><td>412</td><td>–</td><td>A+</td></tr><tr><td>C<sub>2</sub>H<sub>3</sub></td><td>H<sub>2</sub>CC + H</td><td>1240</td><td>147</td><td>C</td><td>C</td></tr><tr><td>C<sub>2</sub>H<sub>5</sub></td><td>C<sub>2</sub>H<sub>4</sub> + H</td><td>260</td><td>153</td><td>C</td><td>A+</td></tr><tr><td>l-C<sub>3</sub>H</td><td>C<sub>3</sub> + H</td><td>379</td><td>136</td><td>B</td><td>B</td></tr><tr><td>c-C<sub>3</sub>H</td><td>C<sub>3</sub> + H</td><td>289</td><td>126</td><td>B</td><td>B</td></tr><tr><td>HC<sub>3</sub>H</td><td>l-C<sub>3</sub>H + H</td><td>400</td><td>139</td><td>B</td><td>B</td></tr><tr><td>c-C<sub>3</sub>H<sub>2</sub></td><td>c-C<sub>3</sub>H + H</td><td>284</td><td>136</td><td>B</td><td>B</td></tr><tr><td>C<sub>3</sub>H<sub>3</sub></td><td>C<sub>3</sub>H<sub>2</sub> + H/C<sub>3</sub>H + H<sub>2</sub></td><td>300</td><td>143</td><td>C</td><td>A+</td></tr><tr><td>C<sub>4</sub>H<sup>-</sup></td><td>–</td><td>–</td><td>348</td><td>–</td><td>A+</td></tr><tr><td>C<sub>6</sub>H<sup>-</sup></td><td>–</td><td>–</td><td>327</td><td>–</td><td>A+</td></tr><tr><td>OH</td><td>O + H</td><td>279</td><td>95</td><td>A+</td><td>A+</td></tr><tr><td>HO<sub>2</sub></td><td>H + O<sub>2</sub></td><td>476</td><td>109</td><td>C</td><td>A+</td></tr><tr><td>HCO</td><td>H + CO</td><td>2037</td><td>152</td><td>C</td><td>A+</td></tr><tr><td>HCOOH</td><td>H + HCOO</td><td>333</td><td>110</td><td>A+</td><td>A+</td></tr><tr><td>NH<sub>2</sub></td><td>NH + H</td><td>314</td><td>111</td><td>C</td><td>A+</td></tr><tr><td>HNC</td><td>H + NC</td><td>165</td><td>103</td><td>B</td><td>B</td></tr><tr><td>HNCO</td><td>NH + CO</td><td>333</td><td>108</td><td>A</td><td>B</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>HCO + CH<sub>3</sub></td><td>342</td><td>121</td><td>A</td><td>A</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>CH<sub>3</sub>O + CH<sub>3</sub></td><td>196</td><td>127</td><td>A+</td><td>A+</td></tr><tr><td>CH<sub>3</sub>OCHO</td><td>CH<sub>3</sub>O + CHO</td><td>248</td><td>113</td><td>A+</td><td>A+</td></tr><tr><td>SH</td><td>S + H</td><td>345</td><td>119</td><td>B</td><td>A+</td></tr><tr><td>CS</td><td>C + S</td><td>168</td><td>110</td><td>A+</td><td>A</td></tr><tr><td>H<sub>2</sub>CS</td><td>H<sub>2</sub> + CS</td><td>313</td><td>135</td><td>A</td><td>B</td></tr><tr><td>S<sub>2</sub></td><td>S + S</td><td>280.6</td><td>133</td><td>A+</td><td>B</td></tr><tr><td>SiH</td><td>Si + H</td><td>417</td><td>156</td><td>B</td><td>B</td></tr><tr><td>HF</td><td>H + F</td><td>140</td><td>78</td><td>A+</td><td>B</td></tr></tbody></table>

however, or photodissociation products in this wavelength range (Deyerl et al. 1999; Nguyen et al. 2001a,b; Zheng et al. 2009). The photodissociation cross section included here is, therefore, a scaled combination of the two transitions from the Eisfeld spectra which agree with experiments, and are absolutely scaled to the cross section measured previously (Fahr et al. 1997).

### 3.11. C<sub>4</sub>H<sup>-</sup> and C<sub>6</sub>H<sup>-</sup>

As with C<sub>2</sub>H<sup>-</sup>, the absolute photodetachment cross sections of both C<sub>4</sub>H<sup>-</sup> and C<sub>6</sub>H<sup>-</sup> have been measured with 22-pole ion

trap technology at several photon energies which allows the construction of the cross sections (Best et al. 2011). Their cross sections are included in this database now for the first time.

### 3.12. OH (hydroxyl)

Previously, the photodissociation cross section of OH is based on the theoretical work by van Dishoeck & Dalgarno (van Dishoeck et al. 1984; van Dishoeck & Dalgarno 1984a,b). More recently, the VUV photoabsorption spectra of the A<sup>2</sup>Σ<sup>+</sup> (ν' = 0) and D<sup>2</sup>Σ<sup>-</sup> (ν' = 0, 1) bands of OH (and OD) were