Science Cases
HARMONI is conceived as a workhorse instrument that will exploit the ELT scientific potential in its early years, starting at first light. HARMONI covers the visible and near-infrared (0.46 to 2.46 μm) spectral ranges with resolving powers, R, from 3000 to 17000 and a field-of-view from 6"×9" in the coarsest spaxel scale (30 mas × 60 mas) to 0.6"×0.8" in the finest spaxel scale (4 mas × 4 mas) which Nyquist samples the diffraction limit of the ELT at near-infrared wavelengths (about 10 mas FWHM). It also provides a high-contrast mode. Thanks to these characteristics, HARMONI will address many of the ELT key science cases.
Planetary science and exoplanets - Simulated Science Cases
Solar system bodies
It will be possible to study the atmosphere of outer planets and their moons (e.g., Titan, Io, Europa) getting the spectra of individual "storms", hot spots and volcanoes. As well as to study the geology and composition of small Solar system bodies by spectroscopically mapping their surfaces.
High-contrast spectroscopy of exoplanets in nearby stars
Using the high-contrast mode, HARMONI will produce direct images and spectra of extrasolar planets which will enable the chemical characterization of their atmospheres.
Evolution of planetary-mass objects
HARMONI can determine the dynamical mass of brown dwarfs and planetary-mass objects in various stages of evolution. The fundamental relation between mass, luminosity, temperature, and age, which is key to understanding the evolution of substellar objects, will be established.
The Milky Way and nearby galaxies - Simulated Science Cases
Intermediate mass black holes
The existence of intermediate mass black holes at the center of stellar clusters will be investigated using HARMONI by tracing the gravitational potential through the measurement of the spatially resolved stellar kinematics.
Dynamical masses of stellar-mass black holes
Low-Mass X-ray Binaries (LMXBs) represent the end-points of the most massive stars and are important for our understanding of stellar evolution. HARMONI will measure the mass of the compact object, neutron star or black hole, of the binary system which is needed to to determine its Equation of State.
Ultra-compact binaries and the progenitors of Type Ia supernovae
Ultra-Compact Binaries (UCBs) are important sources for gravitational waves. They represent one of most extremes physical environments known. HARMONI will determine their dynamical masses and allow us to distinguish between various formation mechanisms.
Stellar populations in nearby galaxies
HARMONI will obtain the resolved spectra of individual stars in nearby galaxies to measure their age, composition, and kinematics. This will determine the chemo-dynamical properties of galaxies and constrain their star-formation history and evolution.
Galaxy Cores, Black Holes, and AGN Physics
HHARMONI will help us to understand the large scale feedback of the AGN into the host galaxy. The gas at the vicinity of the accretion disk will be spatially resolved and the relevant physical processes characterized.
Cosmology and high-z Universe - Simulated Science Cases
The evolution of M bulge-sigma relations using QSOs
HARMONI will make stellar-velocity dispersion measurements in the host-galaxies of QSO. This will enable us to monitor the build-up of black holes, the stellar mass and their total halo masses and provide the crucial information with which to understand their co-evolution.
High-z type Ia SNe
SNe Ia are a fundamental tool for cosmology as distance indicators. HARMONI will provide accurate redshift measurements and a secure classification of the SNe as type Ia up to z about 4.
Gamma-Ray Bursts and their Hosts
HARMONI will be able to provide sensitive spectroscopic follow-up of the GRB hosts. This will permit detailed analysis of the chemical composition and precise measurements of the redshift of the hosts. GRB hosts can help us to map the ionization history of the Universe.
High-z Luminous and Ultraluminous Infrared Galaxies
Infrared bright galaxies are important contributors to the total star-formation of the Universe. HARMONI will characterize their evolution, feedback, and dynamical masses at the Cosmic noon (z ~ 1-3).
The Physics of High Redshift Galaxies
HARMONI will measure the gas and stellar spatially resolved kinematics of galaxies up to z ~ 2-5. The analysis of the rotation curves will reveal the dark matter distribution. The metal abundances and AGN impact on their evolution will be studied too.
From first light to the earliest galaxies
HARMONI will yield detailed kinematic and composition information from the very earliest galaxies (z~10) ionising their immediate environments in a largely neutral intergalactic medium.
Black hole masses of lensed QSO
The rotation of the gas in the broad line region (BLR) of lensed QSO can be used to determine their black hole masses. Using spectroastrometry, it will be possible to measure the BLR size and kinematics even if it is not spatially resolved.