object merger, was co-PI of the _Chandra_ observations, and contributed to
analysis and writing. OS contributed to afterglow and kilonova modelling and
led the writing of these sections. MB was involved in kilonova modelling, EB
contributed to interpretation, placing the burst in context and high energy
properties. KH was involved in kilonova spectral modelling and identified the
2.15 micron feature. LI reduced VLT/MUSE and X-shooter observations and led
the host analysis. GPL contributed to afterglow and kilonova modelling. ARE
analysed the Chandra observations, BS reduced and analysed VLT observations.
NS contributed to afterglow and kilonova modelling. SS was responsible for
placing the burst afterglow in context and demonstrating its faintness. NRT
contributed to analysis, interpretation and writing. KA was involved in the
ULTRACAM observations and interpretation. GA led the ATCA observations. GB
reduced the JWST NIRCAM data. LC processed and analysed the MUSE observations.
VSD is the ULTRACAM PI. JPUF contributed to the interpretation. WF was the PI
on the Chandra observations and contributed to discussion. CF contributed to
the theoretical interpretation. NG was involved in host analysis. KEH, GP, AR,
SDV, SC, PDA, DH, MDP, CCT, AdUP and DA contributed to ESO observations and
discussion. DW contributed to spectral and progenitor modelling and
discussion. MJD, PK, SP, JM, SGP, IP, DIS contributed to the ULTRACAM
observations. GL investigated potential similarities with other transients.
AT, PAE, BS and JAK contributed to the Swift observations. MF extracted and
flux-calibrated the TESS light curve. SJS analysed the JWST spectral lines,
and contributed to interpretation and writing. HFS performed the BPASS-hoki-
ppxf fits to the integrated MUSE flux and contributed the associate figure and
text. All authors contributed to manuscript preparation through contributions
to concept development, discussion and text.

## Acknowledgements

We dedicate this paper to David Alexander Kann, who passed on March 10. The
final messages he sent were regarding follow-up of GRB 230307A, and we hope it
would satisfy his curiosity to know the final conclusions.

This work is based on observations made with the NASA/ESA/CSA James Webb Space
Telescope. The data were obtained from the Mikulski Archive for Space
Telescopes at the Space Telescope Science Institute, which is operated by the
Association of Universities for Research in Astronomy, Inc., under NASA
contract NAS 5-03127 for JWST. These observations are associated with program
#4434 and 4445. Support for Program numbers 4434 and 4445 was provided through
grants from the STScI under NASA contract NAS5- 03127.

This paper is partly based on observations collected at the European Southern
Observatory under ESO programme 110.24CF (PI Tanvir), and on observations
obtained at the international Gemini Observatory (program IDs
GS-2023A-DD-106), a program of NOIRLab, which is managed by the Association of
Universities for Research in Astronomy (AURA) under a cooperative agreement
with the National Science Foundation on behalf of the Gemini Observatory
partnership: the National Science Foundation (United States), National
Research Council (Canada), Agencia Nacional de Investigación y Desarrollo
(Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina),
Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and
Korea Astronomy and Space Science Institute (Republic of Korea). Processed
using the Gemini IRAF package and DRAGONS (Data Reduction for Astronomy from
Gemini Observatory North and South).

AJL, DBM and NRT were supported by the European Research Council (ERC) under
the European Union’s Horizon 2020 research and innovation programme (grant
agreement No. 725246).

N. Sarin is supported by a Nordita fellowship. Nordita is supported in part by
NordForsk. B. Metzger is supported in part by the NSF (grant AST-2002577).
J.H. and D.L. were supported by a VILLUM FONDEN Investigator grant (project
number 16599). G.P.L. is supported by a Royal Society Dorothy Hodgkin
Fellowship (grant Nos. DHF-R1-221175 and DHF-ERE-221005). G.L. was supported
by a research grant (19054) from VILLUM FONDEN. K. H. is supported by JST
FOREST Program (JPMJFR2136) and the JSPS Grant-in-Aid for Scientific Research
(20H05639, 20H00158, 23H01169, 20K14513). KEH acknowledges support from the
Carlsberg Foundation Reintegration Fellowship Grant CF21-0103. S. Schulze
acknowledges support from the G.R.E.A.T. research environment, funded by
Vetenskapsrådet, the Swedish Research Council, project number 2016-06012. The
Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation
under grant No. 140. JPUF is supported by the Independent Research Fund
Denmark (DFF–4090-00079) and thanks the Carlsberg Foundation for support. SJS
acknowledges funding from STFC Grant ST/X006506/1 and ST/T000198/1. VSD and
ULTRACAM are funded by STFC grant ST/V000853/1 AAB acknowledges funding from
the UK Space Agency. MN is supported by the European Research Council (ERC)
under the European Union’s Horizon 2020 research and innovation programme
(grant agreement No. 948381) and by UK Space Agency Grant No. ST/Y000692/1.
H.F.S is supported by the Eric and Wendy Schmidt AI in Science Postdoctoral
Fellowship, a Schmidt Futures program. DS acknowledges funding from STFC
grants ST/T000406/1, ST/T003103/1, ST/X001121/1. MER acknowledges support from
the research programme Athena with project number 184.034.002, which is
financed by the Dutch Research Council (NWO). POB acknowledges funding from
STFC grant ST/W000857/1. D.K.G acknowledges support from the Australian
Research Council Centre of Excellence for Gravitational Wave Discovery
(OzGrav), through project number CE170100004.

## Data availability

JWST data are directly available from the MAST archive. Chandra and Swift data
are also in the public domain. ESO and Gemini data are stored in their
respective archives and will be available to all once the proprietary period
expires. Data can be obtained from the corresponding author between the date
of publication and the end of the proprietary period. This research has made
use of _Fermi_ data which are publicly available and can be obtained through
the High Energy Astrophysics Science Archive Research Center (HEASARC) website
at https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html

## Code availability

Much analysis for this paper has been undertaken with publically available
codes and the details required to reproduce the analysis are contained within
the manuscript.

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