Thank you for visiting nature.com. You are using a browser version with limited support for CSS. To obtain the best experience, we recommend you use a more up to date browser (or turn off compatibility mode in Internet Explorer). In the meantime, to ensure continued support, we are displaying the site without styles and JavaScript.

# Vibrationally excited molecular hydrogen production from the water photochemistry

## Abstract

Vibrationally excited molecular hydrogen has been commonly observed in the dense photo-dominated regions (PDRs). It plays an important role in understanding the chemical evolution in the interstellar medium. Until recently, it was widely accepted that vibrational excitation of interstellar H2 was achieved by shock wave or far-ultraviolet fluorescence pumping. Here we show a further pathway to produce vibrationally excited H2 via the water photochemistry. The results indicate that the H2 fragments identified in the O(1S) + H2(X1Σg+) channel following vacuum ultraviolet (VUV) photodissociation of H2O in the wavelength range of λ = ~100-112 nm are vibrationally excited. In particular, more than 90% of H2(X) fragments populate in a vibrational state v = 3 at λ~112.81 nm. The abundance of water and VUV photons in the interstellar space suggests that the contributions of these vibrationally excited H2 from the water photochemistry could be significant and should be recognized in appropriate interstellar chemistry models.

## Introduction

Vibrationally excited molecular hydrogen (H2(v > 0)) is a key species in the interstellar medium (ISM)1. The internal energy available in vibrationally excited H2 can be used to overcome or diminish the activation barrier of various chemical reactions of interest for molecular astrochemistry. The enhancement in the reactivity of H2 when it is in a vibrationally excited state has solved several puzzling problems, e.g., the formation of the methylidine cation (CH+) in the ISM2,3,4. CH+ was one of the first molecules observed in space, its ubiquity and high abundance have been a longstanding problem for more than 70 years5. The reaction that forms the CH+ molecule is endothermic (with a barrier of ~0.37 eV). Such endothermicity could be overcome by the C+ reacting with the vibrationally excited H26,7. Therefore, the excitation of interstellar H2 is an essential prerequisite for determining the chemical composition in the ISM.

Recent astronomical observations have illustrated that conspicuous emissions from vibrationally excited H2 exist in the photo-dominated regions (PDRs) and shocks8. The first ultraviolet detection of vibrational excited interstellar H2 was performed by Federman et al. using the Hubble Space Telescope toward the star ζ Ophiuchi9, and then detected by Jensen et al. toward HD 38087 and HD 19957910, Gnacinski et al. towards HD 14788811, and Racheford et al. near Herschel 3612. In particular, over 500 interstellar H2 absorption lines from excited vibrational levels v = 1–14 were reported by Meyer et al. toward HD 37903, one of the hot stars located in the NGC 2023 reflection nebula13.

It was widely accepted that two major sources were responsible for the excitation of H2 in the ISM, i.e., shock waves and far-ultraviolet (FUV) fluorescence14,15. For shocks, the H2 molecules were collisionally excited from the ground state in shock-heated gases; whereas for fluorescence they were populated by radiative decay of electronically excited states, which were pumped through the absorption of FUV photons. Though there was general agreement between the main characteristics of models and observations for H2 excitation, some discrepancies are yet to be unraveled. For instance, the observations showed that the v = 4 lines are significantly stronger than the predictions16. A possible explanation for an excess in v = 4 was that H2 formation is occurring directly into this level, which inspired the scientists to look for processes other than collisions and fluorescence excitation in PDRs. In this work, we demonstrated that vibrationally excited H2 can be directly produced from the water photochemistry in the vacuum UV (VUV) region, via a new discovered fragmentation channel O(1S) + H2.

Water photochemistry has been of great interest to chemists since it represents a prototype system for the photodissociation of triatomic molecules, as well as an important process occurring in planetary atmospheres, interstellar clouds, and comet coma17,18,19,20. The electronic spectrum of H2O displays two continuous absorption bands with their maxima at λ ~ 167 nm and ~128 nm respectively, and stronger absorption features at λ < 124 nm associated with excitations to Rydberg states (Supplementary Fig. 1). Various photon-induced fragmentation processes of H2O have been studied previously20:

$${{{{{{\rm{H}}}}}}}_{2}{{{{{\rm{O}}}}}}({\tilde{X}}^{1}{{{{{{\rm{A}}}}}}}_{1})+hv\to {{{{{\rm{H}}}}}}+{{{{{\rm{OH}}}}}}({{{{{{\rm{X}}}}}}}^{2}\varPi )\,({D}_{th}=5.102\,{{{{{\rm{eV}}}}}})$$
(1)
$$\to {{{{{\rm{H}}}}}}+{{{{{\rm{OH}}}}}}({{{{{{\rm{A}}}}}}}^{2}{\Sigma }^{+})\,({D}_{th}=9.124\,{{{{{\rm{eV}}}}}})$$
(2)
$$\to {{{{{\rm{O}}}}}}({\,\,}{\!\!}^{3}{{{{{\rm{P}}}}}})+{{{{{\rm{H}}}}}}+{{{{{\rm{H}}}}}}\,({D}_{th}=9.513\,{{{{{\rm{eV}}}}}})$$
(3)
$$\hskip6pt\to {{{{{\rm{O}}}}}}({\,\,}{\!\!}^{1}{{{{{\rm{D}}}}}})+{{{{{\rm{H}}}}}}+{{{{{\rm{H}}}}}}\,({D}_{th}=11.480\,{{{{{\rm{eV}}}}}})$$
(4)

where the threshold energies (Dth) for these fragmentation channels are given in parentheses21,22 (Some are on the basis of thermodynamic calculations with the data available from the thermochemical network) (https://atct.anl.gov). Photodissociation studies at both 193 nm23 and 157.6 nm24,25,26,27, which excite H2O to the $${\tilde{A}}^{1}{{{{{{\rm{B}}}}}}}_{1}$$ state, reveal prompt O-H bond fission and formation of ground-state OH(X2Π) radical with little internal excitation. In contrast, photodissociation of H2O in its second ($${\tilde{B}}^{1}{{{{{{\rm{A}}}}}}}_{1}{\leftarrow }\tilde{X}^{1}{{{{{{\rm{A}}}}}}}_{1}$$) absorption band is much more complicated. This dissociation proceeds via two main pathways: one leading to the OH(A2Σ+) + H products when the dissociation energy is above the threshold for this channel; the other to OH(X2Π) + H through two conical intersections (CIs) between the $$\tilde{B}$$ state and the ground state ($$\tilde{X}$$1A1) at the linear geometries HOH and OHH28,29,30,31,32,33,34. At shorter wavelengths, three body channels (3) and (4) can be reached. Recent photofragment translational spectroscopy (PTS) measurements of the H atoms from H2O photolysis in the wavelength range of 90 ≤ λ ≤ 110 nm revealed the dominated production of channels (3) and (4)35. Of particular astrochemical significance, the PTS study showed that ~20% of H2O photoexcitation events induced by the solar photons yield O atoms via the three-body channels.

The competing H2 elimination channels following VUV photoexcitation of H2O should also be thermodynamically accessible,

$${{{{{{\rm{H}}}}}}}_{2}{{{{{\rm{O}}}}}}({\tilde{X}}^{2}{{{{{{\rm{A}}}}}}}_{1})+hv\to {{{{{\rm{O}}}}}}({\,\,}{\!\!}^{1}{{{{{\rm{D}}}}}})+{{{{{{\rm{H}}}}}}}_{2}({{{{{{\rm{X}}}}}}}^{1}{\Sigma }_{{{{{{\rm{g}}}}}}}^{+})\,({D}_{th}=6.983\,{{{{{\rm{eV}}}}}})$$
(5)
$$\to {{{{{\rm{O}}}}}}({\,\,}{\!\!}^{1}{{{{{\rm{S}}}}}})+{{{{{{\rm{H}}}}}}}_{2}({{{{{{\rm{X}}}}}}}^{1}{\Sigma }_{{{{{{\rm{g}}}}}}}^{+})\,({D}_{th}=9.206\,{{{{{\rm{eV}}}}}})$$
(6)

To date, only the branching ratio for the channel (5) has been measured a long time ago by Slanger and Black36. Whereas the possible fragmentation channel (6) has yet to be identified in any detail. Recent development of the intense VUV free-electron laser (FEL), at the Dalian Coherent Light Source, has provided a unique tool for studying the state-of-the-art molecular fragmentation dynamics in the VUV range37,38.

Here, we present the experimental verification of O(1S) + H2(X1Σg+) fragments based on VUV-pump and VUV-probe time-sliced velocity-map imaging (TSVMI) measurements of O(1S) atoms (Fig. 1). The results indicate that all of the H2 fragments identified following VUV photodissociation of H2O in the wavelength range of λ = ~100–112 nm are vibrationally excited. In particular, more than 90% of H2(X) fragments populate in a single vibrational state v = 3 at λ ~ 112.81 nm, representing an alternative source of vibrationally excited H2 in the ISM.

## Results and discussion

### Observation of vibrationally excited H2 from H2O photolysis

The present experimental studies were performed on the recently constructed VUV FEL-TSVMI apparatus which equips with two independently tunable VUV laser radiation sources (Fig. 1b). The VUV FEL output (Fig. 1a) was used to directly excite H2O molecules to a dissociative rovibronic state. The subsequent O(1S) fragments were then resonantly ionized at λ = 121.7 nm, which was generated by a table-top VUV source from the four-wave mixing scheme (see Method section for more details). A pulsed supersonic molecular beam of 3% H2O/Ar was crossed by the two counter-propagating VUV beams in the interaction region of the TSVMI setup, as shown schematically in Fig. 1.

Figure 2 displays time-sliced ion images of the O(1S) photofragments recorded following photolysis of H2O at λ = 102.67, 105.52, 107.65, 109.12, 111.48, and 112.81 nm, respectively. These wavelengths locate in the central of the sharp features in the absorption spectrum (Supplementary Fig. 1), which are attributed to nd ← 1b1 (n ≥ 3) Rydberg transitions. The double-headed red arrows in the image figures stand for the polarization direction of photolysis lasers. At all six photolysis wavelengths, well-resolved concentric ring structures with different intensities are clearly observed in the experimental images, which can be directly attributed to different vibrational states of H2(X) coproducts. It is noted that these structures cannot arise from the other O(1S) elimination process, i.e., the O(1S) + H + H channel, because of the insufficient photolysis photon energy (Dth ≥ 13.703eV22). In addition, an off-axis biconvex LiF lens was used to disperse the 212.55 nm and 835.66 nm lights from the photodissociation/photoionization region, ensuring no secondary dissociation (e.g., the primary OH(X/A) fragment subsequently absorbs another UV photons and dissociates) takes place. The two-photon excitation process is also not possible by applying the extremely low intensity of the VUV light.

The velocity distributions of the O(1S) fragments were determined from the radii of the resolved ring structures in the VMI images, from which the total kinetic energy release distributions (ET) were derived and shown in Fig. 3. In this photodissociation experiments, the available energy (the photoexcitation energy subtracts the threshold energy (hv−Dth)) is distributed between the O(1S) and H2(X) product kinetic energy and the internal energy (Eint). Then the internal energy distributions of H2(X) fragments can be deduced from the ET spectra by using the law of energy conservation,

$$hv({\lambda }_{{{{{{\rm{VUV}}}}}}{{{{{\rm{FEL}}}}}}})\mbox{--}{D}_{th}={E}_{int}[{{{{{\rm{O}}}}}}({\,\,}{\!\!}^{1}{{{{{\rm{S}}}}}})]+{E}_{int}[{{{{{{\rm{H}}}}}}}_{2}(X)]+{E}_{T}[{{{{{\rm{O}}}}}}({\,\,}{\!\!}^{1}{{{{{\rm{S}}}}}})+{{{{{{\rm{H}}}}}}}_{2}({{{{{\rm{X}}}}}})]$$
(7)

The energy combs representing the vibrational quantum numbers of H2(X) fragments were labeled in Fig. 3. The structures provide H2 vibrational distributions with vibrational and partially rotational resolution. Best-fit simulations of these spectra return H2(X, v) population distributions (Fig. 4 and Table 1). It is notable that all of the H2 fragments formed at the six photolysis wavelengths are vibrationally excited with cold rotational excitation (J < 9, Supplementary Fig. 2), and the inverted vibrational state population distributions mainly span vibrational levels of 1 ≤ v ≤ 5, peaking at v = 4 at 109.12 nm and 107.65 nm, and v = 3 at other wavelengths. The most striking finding is that more than 90% of H2(X) fragments populate to a single excited vibrational state v = 3 at 111.48 and 112.81 nm, suggesting peculiar dissociation dynamics. This phenomenon has a little similarity with the previously reported ClO vibrational distribution from OClO photodissociation39 and the OD rotational distribution from HOD photodissociation40. Further Analysis (Supplementary note 1) reveals that about 80% of the available energy, or 11,450 cm−1, is released in vibration of H2 at 112.81 nm photolysis, the rest of the energy is partitioned in translation (~18%) and rotation (~2%). As the photoexcitation energy increases, however, almost the same energy ~11,100 cm−1 is released in vibration, e.g., at 102.67 nm, implying the dissociation undergoes the same transition state. The excess of the available energy tends to depositing in translation (~47% at 102.67 nm).

To further reveal this dissociation process, photodissociation of D2O has also been investigated using the same strategy. Supplementary Fig. S3 shows time-sliced velocity map images of the O(1S) fragments following photoexcitation of D2O at λ = 98.80, 100.36, 102.65, 105.21, 108.29, 111.29, and 112.71 nm, respectively. Image analysis yields the corresponding P(ET) distributions (Supplementary Fig. S4), and best-fit simulations of these spectra return D2(X, v) population distributions (Supplementary Fig. S5 and Table 1). In similarity with the H2 fragments from H2O photolysis, the D2 fragment vibrational state population distributions mainly possess vibrational levels of 2 ≤ v ≤ 7, peaking at v = 4 at 112.71 nm, and v = 5 at other wavelengths. The single v propensity has also been observed, with 95% of D2(X) fragments populating to a single excited vibrational state v = 4 at 112.71 nm, which means ~11,108 cm−1 of the available energy is released in vibration of D2.

The O(1S) ion image measurements reveal not only the ET distribution of the photo-product channels, but also the angular distribution of the photo-fragments, which is characterized by the anisotropy β parameter. The O(1S) ion images display near isotropic distributions with average parameters β = ~0–0.2 at these photolysis wavelengths, indicating that the dissociation process should be quite slow. All of these observations could be accounted for qualitatively by a transition state structure in which both hydrogen atoms are on the same side of the O atom, or the two hydrogen atoms are close enough ensuring two O-H bonds simultaneously break and two H atoms recombine to form H2, as illustrated in CO2 dissociation41.

The calculated energy diagram for the vertical excitation of H2O and the subsequent pathways for the O + H2 dissociation channels obtained from the potential energy surfaces (PESs) are shown in Fig. 5, and in Supplementary note 2. According to the previous studies35, photoexcitation at λ~100–112 nm which populates the nd Rydberg states can undergo efficient nonadiabatic coupling to the $$\tilde{E}{'}$$ and $$\tilde{D}$$ electronic states. There are two pathways leading to the O(1S) + H2 (X1Σg+) fragments. One is an adiabatic pathway via the $$\tilde{E}{'}$$ state. An extremely high barrier of 13.25 eV, however, prevents the direct dissociation from this state. Meanwhile, the PESs present a nonadiabatic pathway through an avoided crossing between the $$\tilde{D}$$ and $$\tilde{E}{'}$$ states, and this pathway has a much lower barrier of 11.55 eV, as shown in Fig. 5b. The avoided crossing between the two states is located where the energy difference is minimal and the wavefunctions are strongly mixed. This transition state has a geometry with the H-H bond distance shorter than 1.1 Å and the two O-H bond lengths around 1.8 Å. The calculated energies and average bond distances of vibrational states for H2(X)/D2(X) are shown in Table 2. When the H-H bond lengthens to ~1.1 Å, the vibrational excitation level of H2 can be up to 5, which is inconsistent with the vibrational state population distributions of v ≤ 5 observed in experiments. Similarly, the transition state with the D-D bond distance (~1.1 Å) leads to the vibrational excitation of D2 fragments spanning v ≤ 7, which is also in accord with the experimental observation. For the photoexcitation energy being lower than 11.55 eV, the water molecule can further transfer to the $$\tilde{B}$$ state through an avoid crossing between the $$\tilde{D}$$ and $$\tilde{B}$$ states28, and then return to the transition state around the $$\tilde{D}/\tilde{E}{'}$$ coupling. It is noted that this central atom elimination channel has also been observed previously in the photodissociation of OCS42, CO243, and CS244, where the dissociation mechanism has been illustrated as the molecular isomerization with one side atom moving to the other side via a nonadiabatic transition or a roaming process. In comparison, the O(1S) + H2 channel mainly proceeds to the transition state with the two H atom being close, and the dissociation process involves the O-H bonds breaking and H-H bond forming. This dissociation process undergoes several internal conversions with the more scrambling that leads to near isotropic anisotropy.

### Implications for vibrationally excited H2 in the ISM

Since the rate constant enhancement when H2 goes from the ground to an excited vibrational state gets larger at low temperature, the chemistry of vibrationally excited H2 has been considered, not merely in the context of trying to explain the longstanding problem of CH+ formation in diffuse clouds, but also in the determination of the global chemical composition in dense PDRs1. In addition, the vibrationally excited H2 in the ground electronic state formed in rarefied interstellar environments can survive in several days (it decays radiatively with Einstein A-coefficient A ~10−6 s−1)45, making them a key species in the ISM. Vibrationally excited H2 has been commonly observed in the interstellar circumstances, as in PDRs where the H2 (v > 0) molecules are considered to be produced by FUV fluorescence, and in shocked gas where the excitation is mainly collisional. Astronomical observations, however, displayed that the H2 molecules have significant populations in high excitation levels8,11. These high-excitation populations may arise from other non-thermal pumping processes. Burton et al. suggested that H2 formation might be responsible for an apparent excess in the v = 4 levels observed in the NGC2023 PDR16. In this work, the vibrationally excited H2 formation has been clearly observed in the H2O photodissociation via the O(1S) + H2 channel. These H2 fragments have strongly inverted vibrational state population distributions with peaking at v = 3 or 4, suggesting an additional source of vibrationally excited H2 in the ISM.

The quantitative determination of the quantum yields of dissociation channels (1)–(6) is needed to assess the importance of both the H2O photolysis in the VUV region and the role of H2(v > 0) formation in the interstellar space. This is out of scope in this study. From the references, the quantum yield of the O(1D) + H2 channel has been measured by Slanger et al.36 to be 0.1 at around 121.6 nm, whereas McNesby et al.36,46 reported a yield of 0.14 by detection of H2 from H2O photolysis. The subtle difference between the two measurements may arise from the contribution of the O(1S) + H2 channel. Given this assumption, the quantum yield of 0.04 for the O(1S) + H2 channel can be as the lower limit since this channel should be more and more important as the photoexcitation energy increases. Recent measurements of the H atom PTS35 and the O(1D)/O(1S) fragment ion images are achieved at the photolysis wavelengths of 107.5 nm in our lab. The analysis of these features provides the quantum yield of the O(1S) + H2 channel to be ~16 ± 8% at 107.5 nm. The large uncertainty comes from the calibration of the detection efficiency of the O(1S) and O(1D) atoms (Supplementary Fig. 6 and Supplementary note 3). The average absorption cross-section of H2O at λ = 100–112 nm is σH2O ~ 2 × 10−17  cm247, enabling estimation of the cross-section for forming H2(v > 0) fragments at λ = 107.5 nm: σ~3.2 × 10−18 cm2. The abundance of water and VUV photons48,49 in interstellar space suggests that the contributions of these H2(v > 0) sources could be significant and thus should be recognized in appropriate interstellar chemistry models.

In summary, the present study provides a benchmark illustration of the use of a FEL-based VUV light source combined with the ion imaging detection methods to exploit the dissociation processes at the state-to-state level, and thereby demonstrates the exclusive production of vibrationally excited H2 fragments from H2O photolysis. The single v propensity, accounting for >90% of the total H2(X) product yield at the photolysis wavelength λ~112.8 nm, has been observed. This process represents a further source of vibrationally excited H2 observed in the ISM.

## Methods

The vacuum ultraviolet free-electron laser (VUV FEL) has been constructed recently50. The VUV FEL facility runs in the high gain harmonic generation mode, in which the seed laser is injected to interact with the electron beam in the modulator. The seeding pulse (λ ~ 240–360 nm), is generated from a Ti:sapphire laser system. The electron beam is generated from a photocathode RF gun, and accelerated to the beam energy of ~300 MeV by 7 S-band accelerator structures, with a bunch charge of 500 pC. The micro-bunched beam is then sent through the radiator, which is tuned to the nth harmonic of the seed wavelength, and coherent FEL radiation with wavelength λ/n is emitted. Optimization of the linear accelerator yields a high-quality light beam with emittance of ~1.5 mm·mrad, energy spread of ~1‰, and pulse duration of ~1.5 ps. In this work, the VUV-FEL operates at 10 Hz, and the maximum pulse energy is >100 μJ/pulse. The output wavelength is continuously tunable in the range 50–150 nm.

The VUV FEL-TSVMI experiment involves a molecular beam, photolysis and probe lasers and the detection system, and is summarized in Fig. 1. The pulsed supersonic beam was generated by expanding a mixture of 3% H2O and Ar at a backing pressure of 1 bar into the source chamber where it was skimmed before entering the ion optics assembly (IOA, 23-plate ion optics51) mounted in the differentially pumped reaction chamber. The beam passed through a 2 mm hole in the first electrode and propagates along the center axis of the IOA towards the center of the front face of the detector. The molecular beam was intersected at 90o angles by the counter-propagating photolysis and probe laser beams between the second and the third plates of the IOA. The photolysis photons were provided by the FEL, operating at 10 Hz with εpump fixed in the horizontal plane and thus parallel to the front face of the detector. The O(1S) photoproducts were probed by one-photon excitation at λ = 121.7 nm via the autoionization transition of O*[2s22p3(2P0)3 s(1P01)]←O(1S). The 121.7 nm probe photons were generated by four-wave difference frequency mixing (DFWM) using two 212.55 nm photons and one 835.66 nm photon in a cell filled with an Ar/Kr mixture (3:1 mixing ratio). The laser light at 212.55 nm was produced by doubling the output of a 355 nm pumped dye laser operating at ~425 nm. A portion of 532 nm output of the same Nd:YAG laser was used to pump another dye laser which operated at ~835 nm. To eliminate background signals arising from the secondary photolysis of H2O in the interaction region, the 121.7, 212.55, and 835.66 nm beams were passed through a biconvex LiF lens positioned off-axis at the exit of the Ar/Kr gas cell so as to ensure that only the VUV beam was dispersed through the interaction region.

The resulting O+ (1S) ions were then accelerated through the remainder of the IOA and passed through a 740 mm long field-free region before impacting on a 75 mm-diameter chevron double MCP detector coupled with a P43 phosphor screen. Transient images on the phosphor screen were recorded by a charge-coupled device (CCD) camera (Imager pro plus 2M, La Vision), using a 30 ns gate pulse voltage in order to acquire time-sliced images. Images were taken under different experimental conditions to confirm that the signal was from the intended two-color VUV pump-probe scheme. Specifically, images were recorded: (i) with both pump (VUV FEL) and probe (VUV DFWM) beams present in the interaction region; (ii) with the pump beam present but the probe beam blocked, and (iii) with the pump beam blocked and the probe beam present. The one-color background images recorded under conditions (ii) and (iii), which were very weak compared to the image measured with both beams present, were subtracted from the two-color image recorded under condition (i). Converting the radius of any given feature in the measured images to the corresponding O(1S) atom velocity relied on calibration factors derived from imaging O+ ions from the one color multiphoton excitation of O2 at λ = 225.00 nm52.

## Data availability

The source data underlying Figs. 3 and 4 are provided as a Source Data file. All other data supporting this study are available from the authors upon request. Source data are provided with this paper.

## References

1. 1.

Agúndez, M., Goicoechea, J. R., Cernicharo, J., Faure, A. & Roueff, E. The chemistry of vibrationally excited H2 in the interstellar medium. Astrophys. J. 713, 662–670 (2010).

2. 2.

Stecher, T. P. & Williams, D. A. CH and CH+ formation in ion-molecule reactions. Astrophys. J. 177, L141 (1972).

3. 3.

Freeman, A. & Williams, D. A. Vibrationally excited molecular hydrogen in circumstellar clouds and the interstellar CH+ abundance. Astrophys. Space Sci. 83, 417–422 (1982).

4. 4.

Garrod, R. T., Rawlings, J. M. C. & Williams, D. A. Chemical effects of H2 formation excitation. Astrophys. Space Sci. 286, 487–499 (2003).

5. 5.

Douglas, A. E. & Herzberg, G. Note on CH+ in interstellar space and in the laboratory. Astrophys. J. 94, 381–381 (1941).

6. 6.

Hierl, P. M., Morris, R. A. & Viggiano, A. A. Rate coefficients for the endothermic reactions C+(2P) + H2(D2) → CH+(CD+) + H(D) as functions of temperature from 400–1300 K. J. Chem. Phys. 106, 10145–10152 (1997).

7. 7.

Jones, M. E., Barlow, S. E., Ellison, G. B. & Ferguson, E. E. Reactions of C+, He+, and Ne+ with vibrationally excited H2 and D2. Chem. Phys. Lett. 130, 218–223 (1986).

8. 8.

Williams, D.A. Astrochemistry: from molecular clouds to planetary systems; conference summary. IAU Symposium, 197, 549–554 (2000).

9. 9.

Federman, S. R., Cardell, J. A., van Dishoeck, E. F., Lambert, D. L. & Black, J. H. Vibrationally excited H2, HCl, and NO+ in the diffuse clouds toward ζ Ophiuchi. Astrophys. J. 445, 325–329 (1995).

10. 10.

Jensen, A. G., Snow, T. P., Sonneborn, G. & Rachford, B. L. Observational properties of rotationally excited molecular hydrogen in translucent lines of sight. Astrophys. J. 711, 1236–1256 (2010).

11. 11.

Gnaciński, P. Interstellar H2 toward HD 147888. Astron. Astrophys. 549, A37 (2012).

12. 12.

Rachford, B. L., Snow, T. P. & Ross, T. L. Vibrationally excited molecular hydrogen near Herschel 36. Astrophys. J. 786, 159 (2014).

13. 13.

Meyer, D. M., Lauroesch, J. T., Sofia, U. J., Draine, B. T. & Bertoldi, F. The rich ultraviolet spectrum of vibrationally excited interstellar H2 toward HD 37903. Astrophys. J. 553, L59–L62 (2001).

14. 14.

Beckwith, S., Persson, S. E., Neugebauer, G. & Becklin, E. E. Observations of the molecular hydrogen emission from the Orion Nebula. Astrophys. J. 223, 464–470 (1978).

15. 15.

Gatley, I. et al. Fluorescent molecular hydrogen emission from the reflection nebula NGC 2023. Astrophys. J. 318, L73–L76 (1987).

16. 16.

Burton, M. G., Bulmer, M., Moorhouse, A., Geballe, T. R. & Brand, P. W. J. L. Fluorescent molecular hydrogen line emission in the far-red. Mon. Not. R. Astron. Soc. 257, 1P–6P (1992).

17. 17.

Yuan, K., Dixon, R. N. & Yang, X. Photochemistry of the water molecule: adiabatic versus nonadiabatic dynamics. Acc. Chem. Res. 44, 369–378 (2011).

18. 18.

Yuan, K. et al. Nonadiabatic dissociation dynamics in H2O: competition between rotationally and nonrotationally mediated pathways. Proc. Natl Acad. Sci. U.S.A. 105, 19148–19153 (2008).

19. 19.

Chang, Y. et al. Water photolysis and its contributions to the hydroxyl dayglow emissions in the atmospheres of Earth and Mars. J. Phys. Chem. Lett. 11, 9086–9092 (2020).

20. 20.

Chang, Y. et al. Electronically excited OH super-rotors from water photodissociation by using vacuum ultraviolet free-electron laser pulses. J. Phys. Chem. Lett. 11, 7617–7623 (2020).

21. 21.

Boyarkin, O. V. et al. Accurate bond dissociation energy of water determined by triple-resonance vibrational spectroscopy and ab initio calculations. Chem. Phys. Lett. 568, 14–20 (2013).

22. 22.

Harich, S. A. et al. Photodissociation of H2O at 121.6 nm: a state-to-state dynamical picture. J. Chem. Phys. 113, 10073–10090 (2000).

23. 23.

Plusquellic, D. F., Votava, O. & Nesbitt, D. J. Bond-selective photofragmentation of jet-cooled HOD at 193 nm: vibrationally mediated photochemistry with zero-point excitation. J. Chem. Phys. 109, 6631–6640 (1998).

24. 24.

Yang, X. F., Hwang, D. W., Lin, J. J. & Yang, X. Dissociation dynamics of the water molecule on the Ã 1B1 electronic surface. J. Chem. Phys. 113, 10597–10604 (2000).

25. 25.

Zhou, L., Xie, D., Sun, Z. & Guo, H. Product fine-structure resolved photodissociation dynamics: the A band of H2O. J. Chem. Phys. 140, 024310 (2014).

26. 26.

Lu, I. C., Wang, F., Yuan, K., Cheng, Y. & Yang, X. Nonstatistical spin dynamics in photodissociation of H2O at 157 nm. J. Chem. Phys. 128, 066101 (2008).

27. 27.

Engel, V. et al. Photodissociation of water in the first absorption band: a prototype for dissociation on a repulsive potential energy surface. J. Phys. Chem. 96, 3201–3213 (1992).

28. 28.

van Harrevelt, R. & van Hemert, M. C. Photodissociation of water. I. Electronic structure calculations for the excited states. J. Chem. Phys. 112, 5777–5786 (2000).

29. 29.

Dixon, R. N. et al. Chemical “double slits”: dynamical interference of photodissociation pathways in water. Science 285, 1249–1253 (1999).

30. 30.

Fillion, J. H. et al. Photodissociation of H2O and D2O in B̃, C̃, and D̃ states (134−119 nm). comparison between experiment and ab initio calculations. J. Phys. Chem. A 105, 11414–11424 (2001).

31. 31.

Mordaunt, D. H., Ashfold, M. N. R. & Dixon, R. N. Dissociation dynamics of H2O(D2O) following photoexcitation at the Lyman‐α wavelength (121.6 nm). J. Chem. Phys. 100, 7360–7375 (1994).

32. 32.

Zhou, L., Jiang, B., Xie, D. & Guo, H. State-to-state photodissociation dynamics of H2O in the B-band: competition between two coexisting nonadiabatic pathways. J. Phys. Chem. A 117, 6940–6947 (2013).

33. 33.

Jiang, B., Xie, D. & Guo, H. State-to-state photodissociation dynamics of triatomic molecules: H2O in the B band. J. Chem. Phys. 136, 034302 (2012).

34. 34.

Su, S. et al. Photodissociation dynamics of HOD via the (1A1) electronic state. J. Chem. Phys. 143, 184302 (2015).

35. 35.

Chang, Y. et al. Three-body photodissociation of the water molecule and its implications for prebiotic oxygen production. Nat. Commun. 12, 2476 (2021).

36. 36.

Slanger, T. G. & Black, G. Photodissociative channels at 1216 Å for H2O, NH3, and CH4. J. Chem. Phys. 77, 2432–2437 (1982).

37. 37.

Wang, H. et al. Photodissociation dynamics of H2O at 111.5 nm by a vacuum ultraviolet free-electron laser. J. Chem. Phys. 148, 124301 (2018).

38. 38.

Zhou, J. et al. Ultraviolet photolysis of H2S and its implications for SH radical production in the interstellar medium. Nat. Commun. 11, 1547 (2020).

39. 39.

Delmdahl, R. F., Bakker, B. L. G. & Parker, D. H. Completely inverted ClO vibrational distribution from OClO(2A2 24, 0, 0). J. Chem. Phys. 112, 5298–5300 (2000).

40. 40.

Luo, Z. et al. Strong isotope effect in the VUV photodissociation of HOD: a possible origin of D/H isotope heterogeneity in the solar nebula. Sci. Adv. 7, eabg7775 (2021).

41. 41.

Wang, X. D., Gao, X. F., Xuan, C. J. & Tian, S. X. Dissociative electron attachment to CO2 produces molecular oxygen. Nat. Chem. 8, 258–263 (2016).

42. 42.

Chen, W. et al. Observation of the carbon elimination channel in vacuum ultraviolet photodissociation of OCS. J. Phys. Chem. Lett. 10, 4783–4787 (2019).

43. 43.

Lu, Z., Chang, Y. C., Yin, Q. Z., Ng, C. Y. & Jackson, W. M. Evidence for direct molecular oxygen production in CO2 photodissociation. Science 346, 61–64 (2014).

44. 44.

Li, Z. et al. Direct observation of the C + S2 channel in CS2 photodissociation. J. Phys. Chem. Lett. 12, 844–849 (2021).

45. 45.

Cravens, T. E. Vibrationally excited molecular hydrogen in the upper atmosphere of Jupiter. J. Geophys. Res. 92, 11083–11100 (1987).

46. 46.

McNesby, J. R., Tanaka, I. & Okabe, H. Vacuum ultraviolet photochemistry. III. Primary processes in the vacuum ultraviolet photolysis of water and ammonia. J. Chem. Phys. 36, 605–607 (1962).

47. 47.

Lee, L. C. & Suto, M. Quantitative photoabsorption and fluorescence study of H2O and D2O at 50-190nm. Chem. Phys. 110, 161–169 (1986).

48. 48.

Bethell, T. & Bergin, E. Formation and survival of water vapor in the terrestrial planet-forming region. Science 326, 1675–1677 (2009).

49. 49.

Claire, M. W. et al. The evolution of solar flux from 0.1 nm to 160 μm: quantitative estimates for planetary studies. Astrophys. J. 757, 95 (2012).

50. 50.

Chang, Y. et al. Hydroxyl super rotors from vacuum ultraviolet photodissociation of water. Nat. Commun. 10, 1250 (2019).

51. 51.

Lin, J. J., Zhou, J., Shiu, W. & Liu, K. Application of time-sliced ion velocity imaging to crossed molecular beam experiments. Rev. Sci. Instrum. 74, 2495–2500 (2003).

52. 52.

Parker, D. H. & Eppink, A. T. J. B. Photoelectron and photofragment velocity map imaging of state-selected molecular oxygen dissociation/ionization dynamics. J. Chem. Phys. 107, 2357–2362 (1997).

## Acknowledgements

The experimental work was supported by the National Natural Science Foundation of China (Grant Nos. 21922306, 21873099), the National Natural Science Foundation of China (NSFC Center for Chemical Dynamics (Grant No. 21688102)), the Key Technology Team of the Chinese Academy of Sciences (Grant No. GJJSTD20190002), the Liaoning Revitalization Talents Program (XLYC1907154). and the international partnership program of Chinese Academy of Sciences (No. 121421KYSB20170012). The theoretical work was supported by the National Natural Science Foundation of China (Grant Nos. 21733006, 22073042, 22122302, and 12047532).

## Author information

Authors

### Contributions

K.J.Y. designed the experiments. Y.C., Z.J.L., Y.R.Z., and J.Y.Y. performed the experiments. K.J.Y. and Y.C. analyzed the data. K.J.Y., Z.C.C., W.Q.Z., G.R.W., and X.M.Y. discussed the experimental results. F.A., X.X.H., and D.Q.X. performed the theoretical calculation. K.J.Y., Y.C., and X.X.H prepared the manuscript.

### Corresponding authors

Correspondence to Xixi Hu or Kaijun Yuan.

## Ethics declarations

### Competing interests

The authors declare no competing interests.

Peer review information Nature Communications thanks Paul Houston and the other anonymous reviewer for their contribution to the peer review of this work. Peer reviewer reports are available.

Publisher’s note Springer Nature remains neutral with regard to jurisdictional claims in published maps and institutional affiliations.

## Rights and permissions

Reprints and Permissions

Chang, Y., An, F., Chen, Z. et al. Vibrationally excited molecular hydrogen production from the water photochemistry. Nat Commun 12, 6303 (2021). https://doi.org/10.1038/s41467-021-26599-9

• Accepted:

• Published:

• DOI: https://doi.org/10.1038/s41467-021-26599-9