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Stellar Composite Spectrum

A composite spectrum using all publicly available low-resolution multi-object spectra with redshifts above 5.

A composite stellar spectrum (2-D above, 1-D below) using all publicly available low-resolution multi-object spectra with redshifts above 5. The observations make are a plethora of intergalactic medium (IGM), stellar, and interstellar medium (ISM) features visible. Indeed, amongst these are the Lyman break/Balmer break at short wavelengths (where radiation is absorbed by neutral gas), rest-frame ultraviolet emission lines (that probe electron densities, gas-phase abundances, metallicities, and ionisation parameters of the emitting star-forming galaxies and their environments), and optical line emission. Moreover, this plethora of features allows for characterisations of IGM opacity, stellar ages and masses, and gas-phase metallicities, to only name a few. Dashed vertical lines represent the positions of all detected emission (grey) and absorption (black) lines. The individual spectra are all obtained by the Near Infrared Spectrograph (NIRSpec), an instrument on the James Webb Space Telescope with unprecedented sensitivity and wavelength coverage. The plot is adapted from Roberts-Borsani et al. (2024).

This graphic was developed during the breakthrough workshop ‘The Chronology of the Very Early Universe According to JWST: The First Billion Years‘ at the International Space Science Institute (ISSI) in Bern, Switzerland.

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Earliest galaxies distribution

Spectroscopically-confirmed early galaxies and the cosmic star formation rate before and after the first observations with the James Webb Space Telescope (JWST).

Spectroscopically-confirmed early galaxies and the cosmic star formation rate before and after the first observations with the James Webb Space Telescope (JWST). The individual timing of the galaxies since the Big Bang is measured by their redshifts.

a.) The distribution of pre-JWST candidates (dots) and public JWST data sets (squares) over absolute magnitude (MUV) and time, highlighting the power of JWST to detect galaxies beyond a redshift of 6. The latter include compilations (Roberts-Borsani et al. 2024) and single targets (Castellano et al. 2024; Carniani et al. 2024) observed with NIRSpec MSA observations, as well as NIRCam grism (FRESCO and EIGER; Oesch et al., 2023 and Kashino et al., 2023b, respectively).

b.) The cosmic Star-Formation-Rate (SFR) density over the first Billion years (adapted from Figure 17 of Harikane et al., 2024), as seen from HST/WFC3 samples (circles) and JWST/NIRCam estimates (squares). A model of constant star formation (SF) efficiency is plotted as grey line, for comparison. The model and all literature points are derived from Harikane et al., 2024 (and references therein). The literature points are integrated down to an absolute magnitude of MUV = −18 mag. 

This graphic was developed during the breakthrough workshop ‘The Chronology of the Very Early Universe According to JWST: The First Billion Years‘ at the International Space Science Institute (ISSI) in Bern, Switzerland.

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Earliest galaxies morphologies

Resolved morphologies of the early galaxies (with redshift > 6) observed with the James Webb Space Telescope (JWST).


Resolved morphologies of the early galaxies (with redshift > 6) observed with the James Webb Space Telescope (JWST) (using the Near-InfraRed Camera, NIRCam, instrument unless otherwise specified). Galaxies in the field (top row) show clumpy and dense structures (Kartaltepe et al. 2023). Thanks to gravitational lensing, the light from these compact galaxies is resolved into several stellar clumps down to small sizes on the scale of tens of parsecs (“The Cosmic Grapes”; Fujimoto et al. 2024). In some cases, these clumps show strong emission lines as showcased for M1149-JD1 observed with NIRISS and NIRCam (Bradač et al. 2024), MIRI imaging and integral field spectroscopy (Álvarez-Márquez et al. 2023), and NIRSpec (GA-NIFS collab. in prep.) suggesting that intense episodes of star formation are concentrated within them. Near the critical lines, the galaxy light is stretched into long arcs revealing bright compact bound star clusters, with intrinsic sizes smaller than 10 parsecs such as for the “Cosmic Gems arc”, “Firefly Sparkle”, and “Sunrise arc” (Adamo et al. 2024; Mowla et al. 2024; Vanzella et al. 2023a, respectively) and single stars such as “Earendel” (Welch et al. 2022). These stellar systems dominate the light of their galaxies, suggesting that star cluster might be a dominant star formation mode for young galaxies.

This graphic was developed during the breakthrough workshop ‘The Chronology of the Very Early Universe According to JWST: The First Billion Years‘ at the International Space Science Institute (ISSI) in Bern, Switzerland.

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Cosmic Timeline

The cosmic timeline, from the origin of the known Universe in the Big Bang, 13.8 Billion years ago, until present day.

The cosmic timeline, from the origin of the known Universe in the Big Bang, 13.8 Billion years ago, until present day. Shown are major events based on the current standard picture. After the Big Bang, the Universe underwent “Inflation”, a period of accelerated expansion that expanded the Universe by around 60 orders of magnitude. The Universe then kept expanding and cooling until the next major epoch of “Recombination”, when the first hydrogen atoms formed about 400’000 years later. After the subsequent “Dark ages” of the Universe that lasted for a few hundred Million years, the emergence of the earliest galaxies marked the start of the era of “Cosmic dawn”. Within the first galaxies, the first photons were produced and were capable of ionising the neutral hydrogen atoms permeating space. This then started the Epoch of Reionisation (EoR), the most recent major phase transition in the Universe. Isolated galaxies (light dots) produced ionised regions (roundish patches) in the initial stages of reionisation that grew and merged until the Universe was fully re-ionised. 

A graphic by the DELPHI project (ERC 717001) is included in the current illustration. The final graphic was developed during the breakthrough workshop ‘The Chronology of the Very Early Universe According to JWST: The First Billion Years‘ at the International Space Science Institute (ISSI) in Bern, Switzerland.

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Antarctica topography

The ice surface- and bed topography of Antarctica.

The ice surface- and bed topography of Antarctica with elevations relative to present-day global mean sea-level. Almost 98% of the Antarctic continent surface is covered by ice and its weight is pushing down the rocky crust below it. If the continental ice sheet would melt, isostatic post-glacial rebound would cause an uplift of the rocky surface of Antarctica. Elevations are taken from the BedMachine compilations (Morlighem et al., 2020) and the Scientific colour map ‚oleron‘ is used to represent bed topography accurately and to all readers.

  • Creator: Guy Paxman
  • This version: 25.06.2024
  • License: Attribution-ShareAlike 4.0 International (CC BY-SA 4.0)
  • Specific citation: These graphics by Guy Paxman are available via the open-access s-ink.org repository.
  • Related references:
    Morlighem, M., Rignot, E., Binder, T. et al. Deep glacial troughs and stabilizing ridges unveiled beneath the margins of the Antarctic ice sheet. Nature Geoscience 13, 132–137 (2020)

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Greenland topography

The ice surface- and bed topography of Greenland.

The ice surface- and bed topography of Greenland with elevations relative to present-day global mean sea-level. Almost 80% of Greenland’s surface is covered by ice and its weight is pushing down the rocky crust below it. If the ice sheet would melt, post-glacial rebound would cause an uplift of the rocky surface of Greenland. Elevations are taken from the BedMachine compilations (Morlighem et al., 2017) and the Scientific colour map ‚oleron‘ is used to represent bed topography accurately and to all readers.

  • Creator: Guy Paxman
  • This version: 23.06.2024
  • License: Attribution-ShareAlike 4.0 International (CC BY-SA 4.0)
  • Specific citation: These graphics by Guy Paxman are available via the open-access s-ink.org repository.
  • Related references:
    Morlighem, M., Williams, C. N., Rignot, E. et al. BedMachine v3: Complete bed topography and ocean bathymetry mapping of Greenland from multibeam echo sounding combined with mass conservation. Geophysical Research Letters, 44(21), 11-051 (2017)

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Colour-blind friendly palettes

Visually accessible colour palettes for inclusive graphic design contain only colours that are also discernible when converted to grey-scale.

Visually accessible colour palettes for inclusive graphic design contain only colours that are also discernible when converted to grey-scale. The simulated colour-blind appearance of the individual colours is presented at the bottom portions of the coloured arcs. The open-access Scientific colour maps (Crameri, 2018) are colour-blind friendly colour palettes that are suitable for data visualisation and more general graphic applications, such as web design.

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Perceptually-uniform colour gradients

Accurate colour scales for data visualisation have a constant local colour contrast between neighbouring colour values along the individual gradients.

Accurate colour scales for data visualisation have a constant local colour contrast between neighbouring colour values along the individual gradients. The open-access Scientific colour maps (Crameri, 2018) are perceptually-uniform and also colour-blind friendly colour gradients that are suitable for mapping data with colour in any type of science graph.

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Continental rift evolution (animation)

Continental rift evolution—from inception to breakup—accounting for surface processes and tectonic deformation.

Continental rift evolution—from inception to breakup—accounting for surface processes and tectonic deformation. Shown is the rifting evolution of a regional 3-D model covering upper crust, lower crust, and mantle lithosphere atop an asthenospheric layer. The rift fault network evolves through five major phases: (a) distributed deformation and coalescence, (b) fault system growth, (c) fault system decline and basinward localization, (d) rift migration, and (e) breakup. Sediments not only interact with tectonic deformation but they also record subsidence, block rotation, and rift migration. The visualisation is based on coupled numerical models of geodynamics (ASPECT) and landscape evolution (FastScape). The animation is based on the reference model of Neuharth et al., 2022.

  • Creator: Sascha Brune and Derek Neuharth
  • Original version: 26.05.2024
  • This version: 27.11.2024
  • License: Attribution-ShareAlike 4.0 International (CC BY-SA 4.0)
  • Specific citation: These animation Sascha Brune and Derek Neuharth is based on Neuharth et al. (2022) and available via the open-access s-ink.org repository.
  • Related reference: Neuharth, D., Brune, S., Wrona, T., Glerum, A., Braun, J., & Yuan, X. (2022). Evolution of Rift Systems and Their Fault Networks in Response to Surface Processes. Tectonics, 41(3), e2021TC007166. https://doi.org/10.1029/2021TC007166

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