WST Operations

The WST science drivers encompass a very broad range of areas, across the full electromagnetic spectrum and beyond. The WST will be pivotal, in synergy with other major astronomical facilities in the 2040s, to tackle some of the key open questions in modern astrophysics:

What are the extreme physical conditions that govern transient events (explosions, eruptions, and disruptions)?

The WST will uniquely combine spectroscopic and time-domain capabilities, including both repeated and target-of-opportunity (ToO) observations. This will enable the exploration of unprecedented numbers of faint sources while combining strong statistical power with detailed spectroscopy.
The dynamical UniverseMulti-messengerStars
Read more

Was the Universe re-ionized by few very highly star-forming galaxies or from a larger population of galaxies with more modest rate of star-formation?

The WST will uniquely combine the required panoramic coverage and sensitivity with the ability to characterise the galaxies’ ionising capability. By cross-correlating the fluctuating 21 cm signal with the large-scale galaxy distribution in the same cosmic volumes, it will test whether rare luminous or abundant sub-luminous sources drive reionisation.

Origins

What is the interplay between dark, stellar, and gaseous material in galaxies, and how does primordial and metal-enriched gas flow in and out of galaxies at various scales during different epochs?

Understanding the interplay between galaxies, their dark matter haloes, and the large-scale structures has long been limited by observational gaps across these regimes. The WST will bridge these scales with unprecedented accuracy and statistical power, offering a unified view of galaxy evolution.

Galaxy assembly

How do black holes form and grow over cosmic time?

The statistical power of the WST, combined with its operational approach, will be key in investigating intermediate mass black holes and constrain the whole range of black hole population and their influence on galaxies.

Black holes

What is the origin of the chemical elements that are crucial to trace the evolution of galaxies?

The WST will uniquely address key questions in stellar physics and evolution by measuring the chemistry, motions, and properties of vast stellar populations across galaxies.
StarsMulti-messenger
Read more

Is the accelerated expansion of the Universe due to an unknown form of energy or to a modification of General Relativity on large scales?

The WST will provide this essential multiprobe view, combining local and high redshift galaxy surveys, cosmic web mapping, and gravitational wave counterparts to reveal deviations from standard cosmology.

New frontiers in cosmology

How do environmental conditions affect the formation and evolution of stars and planets?

The WST will perform a large-scale, high-resolution spectroscopic survey of planet-host stars and white dwarfs, spanning a broad range of Galactic environments.

Star and planet formation

What can we learn from multi-messenger observations (e.g., gravitational waves and photons) about the nature of compact objects? How can the extreme conditions during mergers of such objects test the laws of physics?

The wide field of view and high multiplexing of WST are ideal for pinpointing the electromagnetic counterparts of gravitational wave events, which can have initial localization uncertainties of several square degrees.

Multi-messenger

What are the extreme physical conditions that govern transient events (explosions, eruptions, and disruptions)?

The WST will uniquely combine spectroscopic and time-domain capabilities, including both repeated and target-of-opportunity (ToO) observations. This will enable the exploration of unprecedented numbers of faint sources while combining strong statistical power with detailed spectroscopy.
The dynamical UniverseMulti-messengerStars
Read more

Was the Universe re-ionized by few very highly star-forming galaxies or from a larger population of galaxies with more modest rate of star-formation?

The WST will uniquely combine the required panoramic coverage and sensitivity with the ability to characterise the galaxies’ ionising capability. By cross-correlating the fluctuating 21 cm signal with the large-scale galaxy distribution in the same cosmic volumes, it will test whether rare luminous or abundant sub-luminous sources drive reionisation.

Origins

What is the interplay between dark, stellar, and gaseous material in galaxies, and how does primordial and metal-enriched gas flow in and out of galaxies at various scales during different epochs?

Understanding the interplay between galaxies, their dark matter haloes, and the large-scale structures has long been limited by observational gaps across these regimes. The WST will bridge these scales with unprecedented accuracy and statistical power, offering a unified view of galaxy evolution.

Galaxy assembly

How do black holes form and grow over cosmic time?

The statistical power of the WST, combined with its operational approach, will be key in investigating intermediate mass black holes and constrain the whole range of black hole population and their influence on galaxies.

Black holes

What is the origin of the chemical elements that are crucial to trace the evolution of galaxies?

The WST will uniquely address key questions in stellar physics and evolution by measuring the chemistry, motions, and properties of vast stellar populations across galaxies.
StarsMulti-messenger
Read more

Is the accelerated expansion of the Universe due to an unknown form of energy or to a modification of General Relativity on large scales?

The WST will provide this essential multiprobe view, combining local and high redshift galaxy surveys, cosmic web mapping, and gravitational wave counterparts to reveal deviations from standard cosmology.

New frontiers in cosmology

How do environmental conditions affect the formation and evolution of stars and planets?

The WST will perform a large-scale, high-resolution spectroscopic survey of planet-host stars and white dwarfs, spanning a broad range of Galactic environments.

Star and planet formation

What can we learn from multi-messenger observations (e.g., gravitational waves and photons) about the nature of compact objects? How can the extreme conditions during mergers of such objects test the laws of physics?

The wide field of view and high multiplexing of WST are ideal for pinpointing the electromagnetic counterparts of gravitational wave events, which can have initial localization uncertainties of several square degrees.

Multi-messenger

What are the extreme physical conditions that govern transient events (explosions, eruptions, and disruptions)?

The WST will uniquely combine spectroscopic and time-domain capabilities, including both repeated and target-of-opportunity (ToO) observations. This will enable the exploration of unprecedented numbers of faint sources while combining strong statistical power with detailed spectroscopy. The dynamical universeMulti-messengerStars
Read more

Was the Universe re-ionized from few very highly star-forming galaxies or from a larger population of galaxies with more modest rate of star-formation?

The WST will uniquely combine the required panoramic coverage and sensitivity with the ability to characterise the galaxies’ ionising capability. By cross-correlating the fluctuating 21 cm signal with the large-scale galaxy distribution in the same cosmic volumes, it will test whether rare luminous or abundant sub-luminous sources drive reionisation.

Read more

What is the interplay between dark, stellar, and gaseous material in galaxies, and how does primordial and metal-enriched gas flow in and out of galaxies at various scales during different epochs?

Understanding the interplay between galaxies, their dark matter haloes, and the large-scale structures has long been limited by observational gaps across these regimes. The WST will bridge these scales with unprecedented accuracy and statistical power, offering a unified view of galaxy evolution.

Read more

How do black holes form and grow over cosmic time?

The statistical power of the WST, combined with its operational approach, will be key in investigating intermediate mass black holes and constrain the whole range of black hole population and their influence on galaxies.

Read more

What is the origin of the chemical elements that are crucial to trace the evolution of galaxies?

The WST will uniquely address key questions in stellar physics and evolution by measuring the chemistry, motions, and properties of vast stellar populations across galaxies.
StarsMulti-messenger
Read more

Is the accelerated expansion of the Universe due to an unknown form of energy or to a modification of General Relativity on large scales?

The WST will provide this essential multiprobe view, combining local and high redshift galaxy surveys, cosmic web mapping, and gravitational wave counterparts to reveal deviations from standard cosmology.

Read more

How do the environment conditions affect the formation and evolution of stars and planets?

The WST will perform a large-scale, high-resolution spectroscopic survey of planet-host stars and white dwarfs, spanning a broad range of Galactic environments.

Read more

What multiple messengers (e.g. gravitational waves, photons) tell us on the nature of compact objects and the extreme physics at play during their merging?

The wide field of view and high multiplexing of WST is ideally suited to the several square degrees uncertainty on the location on sky of the electromagnetic counterpart of gravitational waves events.

Read more

Is the accelerated expansion of the Universe due to an unknown form of energy or to a modification of General Relativity on large scales?

What signatures of new physics from inflation and the early Universe are present in the clustering of high redshift galaxies?

How do black holes form and grow over cosmic time?

What is the interplay between dark, stellar, and gaseous material in galaxies, and how does primordial and metal-enriched gas flow in and out of galaxies at various scales during different epochs?

What is the detailed formation and accretion history of the Milky Way, its populations, and its satellites?

What is the origin of the chemical elements that are crucial to trace the evolution of galaxies?

How do the environment conditions affect the formation and evolution of stars and planets?

What are the extreme physical conditions that govern transient events (explosions, eruptions, and disruptions)?

What multiple messengers (e.g. gravitational waves, photons) tell us on the nature of compact objects and the extreme physics at play during their merging?

Synergies

The WST will fill a critical gap in the global astronomical infrastructure of the 2040s.

Next section

History of the project

The WST was conceived to transform our understanding of the Universe through large-scale spectroscopy.

Acronyms

TECHNICAL

WST: Wide-field Spectroscopic Telescope

FoV: Field-of-View

IFS: Integral Field Spectrograph

IFU: Integral Field Unit

MOS: Multi-Object Spectrograph

MOS-HR: High-resolution Multi-Object Spectrograph

MOS-LR: Low-resolution Multi-Object Spectrograph

ToO: Targets of Opportunity

INSTITUTES & UNIVERSITIES

AIP: Leibniz Institute for Astrophysics Potsdam

ANU/Astralis: The Australian National University / Astralis

CRAL/CNRS: Centre de Recherche Astrophysique de Lyon / French National Centre for Scientific Research

EPFL: Swiss Federal Institute of Technology in Lausanne

ESO: European Southern Observatory

IA/CAUP: Institute of Astrophysics and Space Sciences / Centre for Astrophysics of the University of Porto

IASF-MI/INAF: Institute for Space Astrophysics and Cosmic Physics of Milan / National Institute for Astrophysics

IP2I/CNRS: Institute of Physics of the Two Infinities of Lyon / French National Centre for Scientific Research

IRFU/CEA: Institute for Research into the Fundamental Laws of the Universe / French Alternative Energies and Atomic Energy Commission

Lagrange/CNRS: Lagrange Laboratory / French National Centre for Scientific Research

LAM/CNRS: Marseille Astrophysics Laboratory / French National Centre for Scientific Research

MAQC/Astralis: Macquarie University / Astralis

NCAC: Nicolaus Copernicus Astronomical Center

OAArcetri/INAF: Arcetri Astrophysical Observatory / National Institute for Astrophysics

OABrera/INAF:Brera Astronomical Observatory / National Institute for Astrophysics

OACapodimonte/INAF: Capodimonte Astronomical Observatory / National Institute for Astrophysics

OASBologna/INAF:Bologna Observatory of Astrophysics and Space Science / National Institute for Astrophysics

UKRI: UK Research and Innovation

UNIBO: University of Bologna

UNIGRO/NOVA: University of Groningen / The Netherlands Research School for Astronomy

UNISYD: The University of Sydney

UNIVIE: University of Vienna

UWA: The University of Western Australia

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Join the community

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This project has received funding from the European Union Horizon Europe Research and Innovation Action under grant agreement no. 101183153 -WST.
Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or European Research Executive Agency (REA). Neither the European Union nor the granting authority can be held responsible for them.

Acronyms

TECHNICAL

WST: Wide-field Spectroscopic Telescope

FoV: Field-of-View

IFS: Integral Field Spectrograph

IFU: Integral Field Unit

MOS: Multi-Object Spectrograph

MOS-HR: High-resolution Multi-Object Spectrograph

MOS-LR: Low-resolution Multi-Object Spectrograph

ToO: Targets of Opportunity

INSTITUTES & UNIVERSITIES

AIP: Leibniz Institute for Astrophysics Potsdam

ANU/Astralis: The Australian National University / Astralis

CRAL/CNRS: Centre de Recherche Astrophysique de Lyon / French National Centre for Scientific Research

EPFL: Swiss Federal Institute of Technology in Lausanne

ESO: European Southern Observatory

IA/CAUP: Institute of Astrophysics and Space Sciences / Centre for Astrophysics of the University of Porto

IASF-MI/INAF: Institute for Space Astrophysics and Cosmic Physics of Milan / National Institute for Astrophysics

IP2I/CNRS: Institute of Physics of the Two Infinities of Lyon / French National Centre for Scientific Research

IRFU/CEA: Institute for Research into the Fundamental Laws of the Universe / French Alternative Energies and Atomic Energy Commission

Lagrange/CNRS: Lagrange Laboratory / French National Centre for Scientific Research

LAM/CNRS: Marseille Astrophysics Laboratory / French National Centre for Scientific Research

MAQC/Astralis: Macquarie University / Astralis

NCAC: Nicolaus Copernicus Astronomical Center

OAArcetri/INAF: Arcetri Astrophysical Observatory / National Institute for Astrophysics

OABrera/INAF:Brera Astronomical Observatory / National Institute for Astrophysics

OACapodimonte/INAF: Capodimonte Astronomical Observatory / National Institute for Astrophysics

OASBologna/INAF:Bologna Observatory of Astrophysics and Space Science / National Institute for Astrophysics

UKRI: UK Research and Innovation

UNIBO: University of Bologna

UNIGRO/NOVA: University of Groningen / The Netherlands Research School for Astronomy

UNISYD: The University of Sydney

UNIVIE: University of Vienna

UWA: The University of Western Australia

Edit Template
ue-logo-h
This project has received funding from the European Union Horizon Europe Research and Innovation Action under grant agreement no. 101183153 -WST.
Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or European Research Executive Agency (REA). Neither the European Union nor the granting authority can be held responsible for them.