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The formation of globular clusters at high and low redshift
16.07.2018 - 20.07.2018
Haus Sexten - Via Dolomiti 45, 39030, Sexten
Conferences 2018


Tracing star and cluster formation across cosmic times

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Conference Rational

Globular clusters (GCs) are among the first baryonic structures to form at high redshift and they are intimately linked with the formation and earliest phases of galaxy evolution. The metal-poor GCs probe the dark matter of their host galaxy and a tight scaling relation between the mass of the central super-massive black hole and the number of GCs hold over many orders of magnitude. Despite their importance for our understanding of the stellar initial mass function, star formation and chemical evolution of the Universe, their origin and exact role in galaxy formation is still shrouded in mystery.

Thanks to recent observational advances, largely driven by the Hubble Space Telescope (HST), young star clusters have been found in local star-forming galaxies. However, only in extreme star bursts the conditions are met to form young massive clusters (YMCs) with masses comparable to old GCs. The change in the properties of the resulting stellar cluster populations in galaxies at high and low redshift may suggest a change in the gas physical conditions. On the other hand, the formation of YMCs has led to the exciting possibility that local starburst galaxies are windows to star formation at high redshift.

In parallel to the discoveries of YMCs, detailed photometric and spectroscopic studies of the stellar populations of old GCs have revealed an unanticipated complexity of the stellar population and despite various attempts, no signs of such complexities have been found in YMCs. Did old GCs form in a different formation mechanism?

Old GCs have a typical mass of a few 105 solar masses, while YMCs appear to form with a scale-free power-law mass function, with indications for an environmentally dependent truncation at high masses. Reconciling these different mass distributions by different formation mechanism and/or dynamical evolution (i.e. the preferential disruption of low-mass GCs) is a topic of an ongoing debate. Understanding the relative contribution of “nature” and “nurture” is vital to understand the similarities between these two types of objects.

The frequency of GCs relative to field stars increases when considering lower metallicities, reaching near 100% at metallicities of [Fe/H] ~ -2. But there are no GCs known below [Fe/H] ~ -2.5, raising the question whether this absence is a physical limit, or is because there are simply not enough low-metallicity stars to expect at least 1 GC in the Milky Way. The ages of metal-poor GCs are consistent with them having formed soon after or even before the start of reionisation of the Universe, implying that they formed near the transition of PopIII to PopII star formation. It is still an open question what was their exact role in the early stage of chemical enrichment and evolution of galaxies.

In light of the advancement coming from both observational (ground-based facilities like ALMA, MUSE, and space missions like HST, JWST, GAIA) and numerical, this workshop aims to tie the formation of GCs in the early Universe to observational constraints coming from YMCs in nearby starburst environments. Specific questions addressed in this symposium are: Is there a common formation scenario for YMCs and GCs? Where do GCs fall in the transition from PopIII to PopII star formation? What is the origin of the anomalous chemical abundances in old GCs? The workshop has the goal of bringing together experts from different fields to understand the similarities and differences between YMCs and GCs.
Short information

The conference will be held from 16-20 July 2018 in Sexten, Italy and will be limited to about 60 participants. Each day will feature a few keynote talks to set the stage and a small number of long talks to present key results relevant for the meeting as well as a number of contributed talks. There will be chance for discussion in small groups and in a few plenary sections. The main topics to be covered are:

(i) Clumpy star formation from high to low redshift; how conditions for star formation change across time 

(ii) Stellar populations in globular clusters, chemical complexity and link with field stars

(iii) Globular cluster formation, scaling relations, evolution observational constraints and theoretical predictions. 

(iv) Young star clusters in local galaxies: formation, scaling relations, evolutions. Are young massive clusters analogs of GCs?
Angela Adamo (chair)
Mark Gieles (co-chair)
Linda Smith 
Nate Bastian 
Oscar Agertz
Confirmed Speakers 
Oscar Agertz (Lund University)
Nicola Amorisco (Institute for Theory and Computation, Cambridge)
Jean Brodie (UC Observatories/Lick Observatory)
Miroslava Dessauges-Zavadsky (Geneva Observatory)
Bruce Elmegreen (IBM, New York)
Annette Ferguson (University of Edinburgh)
Oleg Gnedin (University of Michigan)
Mike Grudich (Caltech)
Cliff Johnson (Northwestern University)
Ralf Klessen (Institute of Theoretical Astrophysics, Heidelberg)
Diederik Kruijssen (University of Heidelberg) -
Carmela Lardo (Geneva Observatory)
Sarah Martell (UNSW Sydney)
Joel Pfeffer (Liverpool John Moores University)
Eric Peng (Kavli Institute for Astronomy and Astrophysics)
Else Starkenburg (Leibniz-Institut für Astrophysik, Potsdam)
Glenn van de Ven (ESO, Garching)
Fee: 300 Eur (250 Eur for PhD students)
Contact email This e-mail address is being protected from spambots. You need JavaScript enabled to view it
Please DO NOT use online payment for this workshop: payments will be collected onsite.

**** Deadlines ****
Abstract for Contributed Talk: April, 15th
Abstract for Poster submission: June, 15h

Please check the payment options
Please remind our bus transfers:
Marco Polo Venice - Sesto Airport; Sunday 15 Jul 2018, 3.30 pm and 7.30 pm (cost € 50.00)
Sesto - Marco Polo Venice Airport; Friday, July 20, 1:00 pm / Saturday, July 21, 8:00 am (cost € 50.00)


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