The travel that came with the science, including an overview of the talks I have given can be found on the old travel page. Most of the information here assumes some kind of knowledge already. I'm sorry about that for those who do not fully understand what I've written down. If you have any question, please don't hestitate to ask me! First there are some placeholders, for which I need to write some content soon...

Click to jump directly to Observing simulated galaxies The environment of galaxies/halos, Stochastic star formation and consequences thereof, The OWLS simulations and galaxies therein, My thesis

Self-regulated galaxy formation

From the simulations described below, and work by others, insights have emerged about how galaxies form and evolve. The build-up of stellar mass inside them is regulated on the large scales, through a balance of inflow of gas (which is determined by the cosmology and the cooling properties of gas) and outflows (which are the result of massive stars and Active Galactic Nuclei). This implies that what happens deep inside the dense gaseous regions of the galaxy, including the star formation process itself (!) is to a large extent irrelevant for the star formation properties of the galaxy as a whole. There are some important implications of this picture. Even though self-regulation is becoming widely accepted, these implications are often overlooked. As such, observations and simulations are often interpreted erroneously.

Translating simulations into observations

An artist impression of JWST in space, in front of a fake Milky Way. It won't get that far.... In the work started at STScI I mainly focus on making mock observations from different inds of simulations. We use semi-analytic models as well as hydrodynamic simulations. We simulate deep images and analyze these as if they were real images to find back the properties of the galaxies on the images. We then compare the resulting galaxy population with the galaxy population in the input models and investigate how different they are and why. This is very useful when planning future observations (e.g. with JWST) and for interpreting current observations of Hubble and other large observatories.

The environment of galaxies and their host dark matter halos

For now, just a link to the website corresponding to a paper.

Stochastic star formation and its influence on galaxies

Most, or at least many, stars are formed in clusters. Stars in star forming regions and in star clusters follow a certain mass distribution that is fairly well known. As stars of different masses create different elements and put different amounts of energy in the gas surrounding them, the precise, galaxy wide distribution of stellar masses is an important quantity for galaxy evolution. Now the clusters in which these stars form themselves follow a mass distribution that strongly favours low mass clusters. In the lowest mass clusters the largest possible stellar masses cannot exist (the most massive star would be more massive than its hosting cluster!), so once all stars in all clusters are taken together, there are less massive stars than you would guess from the (universal) mass distribution in the star clusters.

The OverWhelmingly Large Simulations Project

The project for my PhD is part of the OverWhelmingly Large Simulations project. OWLS consists of a large suite of cosmological N-body/SPH simulations, using a modified version of Volker Springel's Gadget code. The power of the projects lies in the large variation of subgrid models for the unresolved physics. For the non-experts: simulations have a limited mass resolution (and a limited spatial resolution). Therefore, many processes that are important in the formation of galaxies (e.g. forming stars, growing a supermassive black hole in the center, exploding supernovae, ...) can not be followed explicitly. Therefore one makes assumptions about how these processes work out on the larger scales that can be resolved. These models are called subgrid models, and the most important aspect of OWLS is the large variation in these models.

The density of gas in the universe now

In particular, the following parameters are varied:

  • Size of the box (mainly 25 and 100 Mpc/h, comoving)
  • Mass resolution
  • Cosmological parameters
  • Star formation law
  • The effective equation of state for high density gas
  • The way supernova feedback works
  • The way (and also whether at all) supermassive black holes grow and feed energy back into the galaxy
  • The cooling function of the gas
  • The reionization of the universe at high redshift
  • A list of OWLS related papers with more (technical) information can be found in the links section.

    My project within OWLS: The Galaxies

    A galaxy in a high resolution simulation

    My project focuses mainly on the galaxies that form inside a the simulation box, a beautiful example of which you see depicted here (click on it to see it from three sides). Selecting these galaxies automatically is not as trivial as it may seem, as a computer cannot look at such images as we can.

    A part of my topic is to select groups of particles that make up something together that an observer might call a galaxy. A comparison of several of these methods, from very easy (by linking particles that are close enough together), along physically motivated (group together gravitationally bound structures) all the way to creating mock observations of the simulation (and selecting galaxies with the tools observers would use for the same purpose) is an important part of my project.

    Once the galaxies are identified I try to explain their physical properties (total mass, mass in stars, ages, metallicity, star formation rate, luminosity, etc...) and relate them to the input physics of the specific run. Example questions are "How is the star formation rate of a galaxy related to the wind velocity due to supernova explosions?" and "What kind of processes do we need to explain the observed, red and dead (no star formation) elliptical galaxies?"

    Getting observables (magnitude, color, reddening due to dust) for galaxies is also something of my concern. I implemented an adapted version of the Bruzual and Charlot (2003) population synthesis code to determine the luminosity of the stellar component of the simulated universe. This light then travels towards us and encounters gas and dust. What this gas and dust do to the light is vaguely known and I am now trying to consistently model effects, in order to come up with realistic luminosities and colors of the galaxies.

    My thesis

    Thesis Marcel Haas


    My thesis, that resulted from this research, and a bit more, can be found on the thesis website!










    Other OWLS Projects

    There is quite a big list of people working with the OWLS simulations. Some of them may be found in my links section. If they alread published a paper, that can probably be found in the list of papers about OWLS on the links section.

    This is actually a bit outdated by now...

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    Contact details

    Marcel R. Haas

    Leiderdorp, Schiedam

    The Netherlands

    Telephone:

    +31 - 6 1151 5535

    E-mail: mail_at_marcelhaas_dot_com