This field of the sky in this image is a small fraction of the field targeted by the Hawaii Two-0 survey. The field of view is 1×3 square arcminutes, corresponding roughly to three times the size of Jupiter viewed from Earth.
Two of the dots are stars in our Sun's neighborhood — the remaining ~300 are galaxies, billions of lightyears away. The full survey covers a field of view which is 24,000 times larger.
Credit: H2O/Conor McPartland.
The Cosmic Dawn Center is involved in a number of observational surveys, dedicated to unraveling the mysteries of the Cosmic Dawn. Below is an overview of these surveys.
For a more general overview of our research, as well as the instruments and methods that we use, click here:
Cosmic Dawn Survey
The Cosmic Dawn Survey is a 50 square degree multi-wavelength survey of the Euclid Deep and Calibration fields.
The scientific aim is to understand the co-evolution of galaxies, black holes, and the dark matter haloes that host them from reonization (z ~ 12, about 500 million years after the Big Bang) to the present (z ~ 0).
The fields are some of the darkest and most observable fields on the sky and have existing multi-wavelength data that will enable immediate science. The survey parameters are designed to enable stellar mass measurement at 3 < z < 12 (2 billion years of Cosmic time, starting 500 million years after the Big Bang), to probe the large scale structure of reionization in the early Universe, and find luminous quasars to the highest redshifts where they exist.
Cosmic Evolution Survey (COSMOS)
COSMOS is an astronomical survey designed to probe the formation and evolution of galaxies as a function of both cosmic time (redshift) and the local galaxy environment.
The survey covers a 2 square degree equatorial field with spectroscopy and X-ray to radio imaging by most of the major space-based telescopes and a number of large ground based telescopes.
Over 2 million galaxies are detected, spanning 75% of the age of the Universe.
Resolving QUIEscent Magnified (REQUIEM) Galaxies
A unique sample of ten strongly lensed high-redshift (1.6<z<3.2), massive (10.5<logM*<11.7) quiescent galaxies, this survey includes new HST WFC3/G141 grism spectroscopy to measure age gradients in the inner cores (<1kpc) of the to-date most comprehensive sample of strongly lensed massive quiescent galaxies.
The analysis will combine deep G141 grism spectroscopy with a wealth of existing rest-frame FUV-optical HST and Spitzer/IRAC imaging. Additionally, ultra-deep dust continuum imaging will be added from a Cycle 6 and 7 REQUIEM-ALMA program.
Beyond Ultra-deep Frontier Fields And Legacy Observations (BUFFALO)
BUFFALO is an astronomical survey built around the six Hubble Space Telescope (HST) Frontier Fields clusters designed to learn about early galactic assembly and clustering and prepare targets for observations with the James Webb Space Telescope.
BUFFALO will place significant new constraints on how and when the most massive and luminous galaxies in the universe formed and how early galaxy formation is linked to dark matter assembly.
Hawaii Two-0 Survey (H20)
The H20 survey is a 20 deg2 deep Subaru Hyper-SuprimeCam (HSC) imaging and Keck DEIMOS + MOSFIRE spectroscopic survey of the two primary Euclid Deep Calibration Fields (NEP and CDFS).
The survey will give insight into galaxy formation, evolution, and quenching, as well as stellar mass functions and dark energy.
Ultra Deep Survey with the VISTA telescope (UltraVISTA)
UltraVISTA is an Ultra Deep, near-infrared survey with the new VISTA surveys telescope of the European Southern Observatory (ESO). Over the course of 5 years, UltraVISTA will repeatedly image the COSMOS field in 5 bands resulting in three key surveys:
Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS)
The Spitzer Matching Survey of the Ultra-VISTA Deep Stripes (SMUVS) consists of deep 3.6 and 4.5 imaging of three Ultra-VISTA near-infrared survey stripes in the COSMOS field.
SMUVS reaches point-source sensitivities of about 25.0 AB mag at both 3.6 and 4.5 microns with a significance of 4 sigma, accounting for both survey sensitivity and source confusion. To this limit, the SMUVS catalogs contain a total of ~350,000 sources, each of which is detected significantly in at least one IRAC band.
Because of its uniform and high sensitivity, relatively large area coverage, and the wide array of ancillary data available in COSMOS, the SMUVS survey will be useful for a large number of cosmological investigations.
The ALMA Large Program to Investigate C+ at Early Times (ALPINE)
ALPINE is an ALMA program that studies the gas and dust properties of young galaxies at redshifts z = 4-6. ALPINE observes a total of 118 main-sequence galaxies in spectroscopic redshifts between 4.4 and 5.9 in the COSMOS field and GOODS-S/ECDFS at a rest wavelength of 159 micrometers. ALPINE focusses on galaxies that are characteristic of these redshifts, therefore its results paint a representative picture of the physical properties of early galaxies
The main science questions addressed with ALPINE are:
- What are the mechanisms that fuel the initial growth of galaxies? - ALPINE gives accurate measurements of the gas properties and gas fractions of galaxies at z>4.
- What are the ISM properties of galaxies in the early Universe and how do they compare to the present day galaxies? - ALPINE accurately constrains the dust properties of these galaxies.
Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH)
The Spitzer Large Area Survey with Hyper-Suprime-Cam (SPLASH) is an astronomical survey to investigate the co-evolution of cosmic large-scale structure, dark matter and the assembly and growth of galaxies as well as supernovae in the early Universe through transient studies.
The survey covers two 1.8 square degree fields (COSMOS and SXDS) and provides optical (from the Hyper-Suprime-Cam on the Subaru telescope) and mid-infrared (from the Spitzer Space telescope) imaging at an unprecedented depth over this area.
The major science enabled by SPLASH includes:
- Investigation of the co-evolution of cosmic large-scale structure, dark matter and the assembly and growth of galaxies and AGN.
- Physics of supernova at high redshifts through transient studies and constraints on the initial mass function.
- Understanding the importance of smooth gas accretion vs. mergers for galaxy growth.
- Probing re-ionization through infrared background fluctuations.
3D-HST is a near-infrared spectroscopic survey with the Hubble Space Telescope designed to study the physical processes that shape galaxies in the distant Universe.
3D-HST is surveying ~600 square arcminutes of well-studied extragalactic survey fields (AEGIS, COSMOS, GOODS-S, UKIDSS-UDS), and now provides the critical third dimension — redshift — for ~10,000 galaxies at z > 1.
This is the epoch when ~60% of the star formation in the Universe took place, the number density of quasars peaked, the first galaxies stopped forming stars and the structural regularity that we see in galaxies today emerged.