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BEGIN:VEVENT
DTSTART;TZID=Atlantic/Canary:20230302T123000
DTEND;TZID=Atlantic/Canary:20230302T133000
UID:iactalks-1664
X-WR-CALNAME: IAC Talks: Open Astronomy Seminars
X-ORIGINAL-URL: /Talks/view/1664
CREATED:2023-03-02T12:30:00+00:00
X-WR-CALDESC: IAC Talks upcomming talks
SUMMARY:Early-type galaxies: instructions to build them through mergers
DESCRIPTION:Early-type galaxies: instructions to build them through mergers
 \nDr. Carlo Cannarozzo\n\n \nEarly-type galaxies: instructions to bui
 ld them through mergers\nMassive  early-type galaxies (ETGs) are "red and 
 dead" systems mainly composed  of old and metal-rich stellar populations. 
 In a cosmological context,  present-day ETGs are believed to be the remnan
 ts of a complex stellar  mass assembly history marked by several mergers, 
 which are the  consequence of the underlying hierarchical assembly of thei
 r host dark  matter halos. In this  talk, I will deal mainly with the
  merger-driven evolution of ETGs.  Firstly, I will illustrate a compa
 rison between observed ETGs from the  MaNGA survey and simulated galaxies 
 from the IllustrisTNG cosmological  simulation suite. The aim of this stud
 y is to provide an interpretative  scenario of the stellar mass assembly h
 istory of observed present-day  ETGs, comparing the radial distributions o
 f their stellar properties  with those of simulated galaxies, in which it 
 is possible to disentangle  the contribution of stars formed in situ (i.e.
  within the main  progenitor galaxy) and stars formed ex situ (i.e. in oth
 er galaxies) and  then accreted through mergers. Then, I will describ
 e how the  scaling relation between the stellar mass and stellar velocity 
  dispersion in ETGs evolves across cosmic time. Specifically, by  extendin
 g the results of Cannnarozzo, Sonnenfeld & Nipoti (2020), I  model the
  aforementioned relation through a Bayesian hierarchical  approach, consid
 ering ETGs with log(M∗/M⊙) > 9 over the redshift  range 0 ≲ 
 z ≲ 4. Together with a new characterisation of the relation,  I rec
 onstruct the back-in-time evolutionary pathways of individual ETGs  on the
  stellar mass-velocity dispersion plane to answer the question  “how
  did high-redshift ETGs assemble through cosmic time to reach the  functio
 nal form of the relation in the present-day Universe?“.\nAfter  the 
 main topic, if time permits, I would like to spend a few minutes  presenti
 ng another extra content (below you can find the title and a  brief abstra
 ct of this further content). Feel free to include it or not  in the announ
 cement mail.\nEXTRA - Inferring the Dark Matter halo mass in galaxies
  from other observables with Machine Learning\nIn  the context of the gala
 xy-halo connection, it is widely known that the  Dark Matter (DM) halos sh
 ow correlations with some physical properties  of the hosted galaxy: the m
 ost well-known relation is the so-called  Stellar-to-Halo-Mass Relation. H
 owever, we know that there are several  other empirical relations among ga
 laxy properties, involving, for  example, the stellar mass, the gas and st
 ellar metallicities, the black  hole mass, etc. Given the complexity of th
 e problem and the high number  of galaxy properties that might be related 
 to DM halos, the study of the  galaxy-halo connection can be approached by
  relying on machine learning  techniques to shed light on this intricate n
 etwork of relations. With  the aim of inferring the DM halo mass and then 
 finding a unique  functional form able to link the halo mass to other obse
 rvables in real  galaxies, I rely on the state-of-the-art Explainable Boos
 ting Machine, a  novel implementation of generalised additive models with 
 pairwise  interactions, training a model on the IllustrisTNG simulation su
 ite at  different redshift.\n \n \n \nYoutube933518
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