August 3, 2015
August 6, 2015
Division J Galaxies and Cosmology
NOTE: exact dates to be announced later
Co-Chairs of SOC:
Sugata Kaviraj (Uni. of Hertfordshire)
Henry Ferguson (STScI)
- Properties of emergent galaxies in the early Universe (e.g. star-formation rates, stellar ages, metallicities, masses, sizes)
- Interplay between gas inflows, star formation and outflows at z>1
- Growth of black holes at z>1, feeding processes (and are they different at low and high z), interaction of AGN with the interstellar medium
- Origin of the Hubble sequence and evolution of galaxy morphology
- Confrontation of observations and galaxy-formation models (e.g. hydro- cosmological simulations, semi-analytical models) in the early Universe
- Linking studies of high-redshift galaxies with the existing literature at z<1, to construct a coherent picture of galaxy evolution over ~90% of cosmic time
- Exploitation of new and future facilities, e.g. multi-object spectrographs (KMOS, MUSE, etc.), ALMA and SKA precursors (LOFAR, e-MERLIN, etc.), JWST, ELTs
- Key post-2015 goals and challenges, in the context of future instrumentation
- The role of citizen-science projects (e.g. Galaxy Zoo) in widening the scientific impact of large astronomical datasets
Coordinating Division: Division J (Galaxies and Cosmology)
Divisions with an interest in the themes of this meeting (in alphabetical order):
Division B: Facilities, Technologies and Data Science
Division C: Education, Outreach and Heritage
Division D: High-Energy Phenomena and Fundamental Physics
Division G: Stars and Stellar physicsDivision H: Inter-stellar matter and Local Universe
Over the last two decades, a convergence of powerful observational facilities and high-performance computing has significantly advanced our understanding of galaxy evolution. Detailed empirical studies have quantified the evolution of galaxy properties (particularly over the latter half of cosmic time) and theoretical models, within the framework of the LCDM paradigm, have met with significant success in reproducing these properties.
While our knowledge is still dominated by work in the nearby (z<1) Universe, an explosion of multi-wavelength data at high redshift is revolutionising our understanding of emergent galaxies at z>1. Since the bulk of the cosmic stellar-mass assembly and black-hole growth takes place at these redshifts (both peaking around z~2), answers to basic questions at these epochs are central to a complete understanding of galaxy evolution. For example, what processes drove the growth of early stellar populations and black holes? How did interactions between galaxies and their constituent black holes shape the Universe we see today? How did the morphological mix of the visible Universe evolve into today’s Hubble sequence? How well do our current theoretical models reproduce the properties of galaxies in the early Universe?
Recent and ongoing studies are delivering a dramatic improvement in our understanding of these fundamental questions. HST surveys like CANDELS, combined with facilities like Spitzer and Herschel, are now constraining galaxy parameters, such as star-formation rates, ages, metallicities, masses and sizes, to z~2 and beyond. Together with deep Chandra observations, these data are probing the co-evolution of young galaxies and their black holes, and the critical role of AGN-driven jets in producing negative feedback, that quenches star formation and influences the morphology of galaxies at early epochs. High-resolution near-infrared imaging from the HST is quantifying the origin and evolution of the Hubble sequence in the early Universe, allowing us to probe the evolving morphological mix of the visible Universe over cosmic time. In parallel, near-infrared integral-field spectrographs on 10m class telescopes such as SINFONI and OSIRIS, together with facilities like IRAM, are enabling detailed spatially-resolved studies of the kinematics, star formation and molecular gas in significant samples of early galaxies, yielding crucial insights into what drives the assembly of the stellar populations that dominate our Universe today. This growing empirical literature is motivating an array of theoretical work, in particular high-resolution hydro-simulations, which are elucidating the cosmic drivers of stellar-mass buildup, black-hole growth and morphological transformations with unprecedented accuracy.
Our current understanding of galaxy evolution will shortly be bolstered by new instruments with multiplexing capabilities, such as KMOS, MUSE and MOSFIRE, and those that offer high-resolution imaging in the long-wavelength regime, such as ALMA and the SKA precursors (e-MERLIN, LOFAR, etc.). These will enable unprecedented studies of stellar and gas kinematics at high redshift, and allow us to investigate the poorly-understood interplay between gas and star formation in the early Universe. In addition, the unprecedented depth and resolution of the e-ROSITA X-ray mission will offer transformational insights into large-scale structure and AGN across cosmic time. Looking further ahead to the turn of the decade, the field is poised for yet another revolution, both in terms of the ground-breaking depth and area offered by future imaging and spectroscopic surveys (e.g. LSST, Euclid, 4MOST, MOONS), and our ability to comprehensively probe galaxy evolution all the way up to the epoch of reionization, using instruments like the JWST and the ELTs.
The time will be ripe in 2015 for bringing together the wealth of empirical and theoretical studies that are leveraging today’s instruments, and setting the stage for the exploitation of new and forthcoming facilities. For example, the interpretation of current multi-wavelength survey data (e.g HST programmes like CANDELS, Herschel programmes like HerMES, etc.) will be mature, and large sets of data will be available from new instruments such as KMOS, ALMA and e-MERLIN. In the same vein, while theoretical simulations are just starting to produce realistic assembly histories for galaxies in the early Universe, more accurate analyses are expected between now and 2015 (possibly revealing new questions and challenges).
The large spectrum of key topics spanned by this Symposium is particularly suited to the large audiences expected at IAU General Assemblies, that are diverse both geographically and in the specialities of the attending researchers. As noted above, 2015 is a particularly opportune time for this meeting, given the maturing literature from current datasets and the expected influx of data from new facilities. The IAU General Assembly in 2015 is, therefore, the ideal location for a conference that critically reviews our current and ongoing studies of the early Universe and identifies the community’s key challenges and goals in the context of future instrumentation. The overall aim of the proposed Symposium is to bring together theorists, observers and instrumentalists to (1) showcase the community’s accumulating knowledge of the early Universe, (2) connect these high-redshift studies to the past literature to construct a coherent picture of galaxy evolution over ~90% of cosmic time and (3) lay the groundwork for the exploitation of future instruments that will become available post-2015.
The themes of this Symposium are strongly aligned with several IAU Divisions, spanning the full spectrum of topics that constitute the IAU’s scientific mission. The proposed coordinating Division is Division J (Galaxies and Cosmology). The principal topics of this meeting include high-energy phenomena like AGN (Division D), star formation (Division G) and inter-stellar matter (Division H), the exploitation of current and future facilities (Division B) and the role of citizen-science projects such as Galaxy Zoo in widening the scientific impact of large astronomical datasets (Division C).