Department of Astronomy,
University of California, Berkeley,
C-207 Hearst Field Annex,
Berkeley, CA 94720 USA
E-mail: feldmann -at- berkeley.edu
I am interested in understanding how galaxies and many of their properties evolve over cosmic history: Which processes determine their sizes, regulate their star formation rates, or shape their morphology? In fact, nobody really knows. However, compared with just 10 years ago, we are now much closer to answering those questions. This remarkable development is largely a result of two major advances. First, with the advent of large scale digital galaxy surveys the quantitative analysis of millions of galaxies became possible -- a development that is still revolutionizing our understanding of galaxy evolution. Secondly, the continuous increase in computing power enables astrophysicists like myself to develop and evaluate increasingly sophisticated theoretical models. This is required because galaxy evolution is an inherently complex problem and requires numerical models of high dynamical range. In my work I often rely on state-of-the-art hydrodynamics and gravity solvers such as the SPH-code GASOLINE or the AMR-code ART to study how galaxies evolve in a cosmological setting.
||PhD in Physics, Institute of
Astronomy, ETH Zürich, Switzerland
|Title: "The Evolution of
Massive Galaxies - A numerical perspective"
|06/2005||Diploma degree (equiv. M.Sc.) in Computer
|Title: "Planning with preferences - Solving partial satisfaction problems"|
|09/2004||Diploma degree (equiv. M.Sc.) in Physics,
|Title: "Phase structure and
photon propagator in 3D abelian lattice
|09/2012 - present
||Hubble fellow at the Department of Astronomy, University of California, Berkeley|
|08/2010 - 08/2012
Kavli Institute for
Astrophysics Group at the Fermi National Accelerator
Laboratory, IL, U.S.A.
|09/2009 - 10/2009||Institute of Astronomy, ETH
|2008 - 2009
||Dep. Physics, ETH
Zürich, Supervision of several undergraduate
projects in astrophysics
|2005 - 2008
||Dep. Physics, ETH
Zürich, Teaching assistant for several courses in
physics and astrophysics
||Associate Fellowship of
the Kavli Institute for Cosmological Physics
||ETH Extragalactic Astrophysics Excellence Award|
|2004-2008||PhD fellowship from the Studienstiftung des deutschen Volkes|
|2001-2004||Scholarship from the Studienstiftung
des deutschen Volkes
|Link to the full
list of ADS published papers
Interactions of cosmic rays with the interstellar gas and radiation fields of the Milky Way provide the majority of the gamma rays observed by the Fermi Gamma Ray Space Telescope. In addition to the gas which is densely concentrated along the Galactic Disk, hydrodynamical simulations and observational evidence favor the presence of a halo of hot (T~10^6 K) ionized hydrogen, extending with non-negligible densities out to the virial radius of the Milky Way. We show that cosmic ray collisions with this circum-galactic gas should be expected to provide a significant flux of gamma rays, on the order of 10% of the observed isotopic gamma ray background at energies above 1 GeV. In addition, gamma rays originating from the extended halos of other galaxies along a given line-of-sight should contribute to this background at a similar level.
|The density profile of
ionized hydrogen in a simulated Milky-Way
halo and comparison with
The total matter density (solid
blue line) is well approximated by an NFW
profile, except in the central region of the halo (<
20 kpc), where cooling and adiabatic contraction lead to
a density enhancement. The density
profile of ionized hydrogen that our
simulation predicts (solid red line)
is in good agreement with observations (symbols) and can
be fit with a
beta-profile (dotted red line). Cosmic
rays that originate in the disk of the Milky Way, but diffuse outward, interact
with this extended halo
of hydrogen and produce
a diffuse and highly isotropic background of
|Characterizing the conversion factor between CO emission and column density of molecular hydrogen, X_CO, is crucial in studying the gaseous content of galaxies, its evolution, and relation to star formation. In most cases the conversion factor is assumed to be close to that of giant molecular clouds in the Milky Way, except possibly in mergers and star-bursting galaxies. However, there are physical grounds to expect that it should also depend on the gas metallicity, surface density, and strength of the interstellar radiation field. We study the dependence of X_CO on such gas properties and on spatial resolution using a model that is based on a combination of results of sub-parsec scale magnetohydrodynamic simulations and on the gas distribution from self-consistent cosmological simulations of galaxy formation. We show that neglecting these dependencies can strongly bias the inferred distribution of column densities of molecular clouds to have a narrower and offset range compared to the true distribution. We further show that observations of molecular gas based on CO emission can result in a biased slope of the star formation -- gas relation. Specifically, our model predicts that this relation appears to steepens at high surface densities as a result of the gas surface density dependence of X_CO. Finally, we show that on sub-kpc scales most of the scatter of the star formation -- gas relation is a consequence of discreteness effects of the star formation process. In contrast, we expect variations of X_CO to be responsible for most of the scatter measured on super-kpc scales.|
|The relation between the
surface density of the star
formation rate and the molecular
hydrogen surface density. The relation used in the
simulation is perfectly linear
(dashed black line). However, the relation
inferred from CO data (blue solid
curve) deviates from the actual relation at high surface densities, similar to
indicate (grey dashed line).
A star formation efficiency per free fall time that evolves over the life time of giant molecular clouds (GMCs) may have important implications for models of supersonic turbulence in molecular clouds or for the relation between star formation rate and H2 surface density. In the paper we discuss observational data that could be interpreted as evidence of such a time variability. In particular, we investigate a recent claim based on measurements of H2 and stellar masses in individual GMCs. We show that this claim depends crucially on the assumption that H2 masses do not evolve over the life times of GMCs. We exemplify our findings with a simple toy model that uses a constant star formation efficiency and, yet, is able to explain the observational data.
|The estimator ηGMC of the
star formation efficiency vs. mass of the GMC.
Empty Squares and triangles are observational
data. Overplotted are solid and dot-dashed lines that
refer to the predictions of the our model. Filled
circles and filled stars indicate when the age of the
modeled GMC is half its total life time or when the
cloud is 1 Myr away from the end of its life,
respectively. The diagonal dashed line indicates a slope
of -0.75, which is approximatively the slope predicted
by our model. The observed data is consistent with this
slope. The horizontal line denotes the value of the
actual (time-independent) star formation efficiency of
the GMC that entered into our model.
Many physical processes may be responsible for making elliptical morphologies and quenching star formation, but the mainly responsible mechanisms, and the epochs and timescales at/on which they operate have not been yet identified. In this paper we use a simulation of the formation of a group of galaxies with sufficient resolution to track the evolution of gas and stars of about a dozen galaxy group members over cosmic history. Ellipticals form, as suspected, through galaxy mergers. In contrast with what has often been speculated, however, these mergers occur at z>1, before the merging progenitors enter the virial radius of the group and before the group is fully assembled. Quenching of star formation in the still star-forming elliptical galaxies lags behind their morphological transformation, but, once started, is taking less than a billion years to complete.
|Assembly histories since z =
2 of the z ∼ 0 group satellites. Red solid (blue
dashed) lines show the stellar mass of z ∼ 0 elliptical
(disk) satellites as function of time (bottom axis) and
redshift (top axis). Filled (empty) symbols indicate the
time when the progenitor of a z ∼ 0 gas-poor (gas-rich)
satellite enters the virial radius of the group. Sudden
increases in stellar mass are caused by merger events,
often before infall into the group, while close
pericentric passages that lead to tidal stripping reveal
themselves through a step-wise stellar mass loss occurring
after their entrance in the group. The gas-poor disk
satellites do not grow significant stellar mass after they
enter the group, due to quenching of their star formation.
In this paper we trace the evolution of central galaxies in three ~10^13 M_sun galaxy groups simulated at high resolution in cosmological hydrodynamical simulations. The evolution in the group potential leads, at z=0, to central galaxies that are massive, gas-poor early-type systems supported by stellar velocity dispersion resembling either elliptical or S0 galaxies. Their central stellar densities stay approximately constant from z~1.5 down to z=0. Instead, the galaxies grow inside-out, by acquiring a stellar envelope outside the innermost ~2 kpc. Consequently the density within the effective radius decreases by up to two orders of magnitude. Both major and minor mergers contribute to most of the mass accreted outside the effective radius and thus drive the evolution of the half-mass radii. Our simulations demonstrate that, in galaxy groups, the interplay between halo mass assembly, galaxy merging and gas accretion has a substantial influence on the star formation histories and z=0 morphologies of central galaxies.
galaxy groups at different redshifts. The size
of each image is 1.2 Mpc × 1.2 Mpc. The four
columns correspond to z = 2.5, z = 1.5, z = 0.6 and z =
0. Each row corresponds to a different galaxy group.
Color coded are dark matter in blue (from 3.6 to 1460 M⊙
/ pc^2), cold gas (here the gas with T < 2.5 ×
10^5 K) in green, stellar matter in yellow (both from
0.9 to 365 M⊙ / pc^2), and hot gas (here the gas with T
≥ 2.5 × 10^5 K) as red surface mass isocontours (3
contour lines at 1, 4.5 and 20 M⊙ / pc^2). The white
circle shows the virial radius of the group at the each
We use a set of high-resolution N-body simulations of binary galaxy mergers to show that the morphologies of the tidal features that are seen around a large fraction of nearby, massive ellipticals in the field cannot be reproduced by equal-mass dissipationless mergers; rather, they are well explained by the accretion of disk-dominated galaxies. The minor cold-accretion events that explain the presence, brightness, and structural and color properties of the tidal debris cause only a modest mass and luminosity increase in the accreting massive elliptical. These results, coupled with the relative statistical frequencies of disk- and bulge-dominated galaxies in the field, suggest that massive ellipticals assemble most of their mass well before their tidal debris forms through the accretion of relatively little, kinematically cold material rather than in very recent, dissipationless major mergers.
Morphological signatures of mergers. (a) Observed image of an elliptical galaxy that shows tidal tails at large galactocentric distances; (b-d) Mock images of: a simulated 1:4 merger between an elliptical galaxy and a disk+bulge system 600 Myrs after the merger; a simulated 1:10 merger between an elliptical galaxy and a disk 500 Myrs after the merger; a simulated 1:4 merger between elliptical galaxies 380 Myrs after the merger. The tidal features originating in mergers between ellipticals and those involving a disk-dominated companion are strikingly different, independent of the mass ratio and orbit characteristics. While all mergers can lead to shells and diffuse features, only the mergers involving disks show strong tidal arms and loops, similar to the observed features around bright ellipticals.
Observational studies of galaxy evolution are increasingly dependent on accurate photometric redshifts. As part of my PhD program I designed and implemented ZEBRA, the Zurich Extragalactic Bayesian Redshift Analyzer. ZEBRA is a publicly available software package that allows to compute photometric redshifts with outstanding accuracy and has been successfully used by many research groups. You can find more information about ZEBRA on its dedicated website.
|A simple Maximum-Likelihood estimate of redshifts: (top) spectroscopic vs. photometric redshifts; (bottom) the error in the redshift estimation as function of spectroscopic redshift for different template types; The standard deviation of dz/1+z is ~ 0.043 and the outlier fraction ~ 2.1 %. Systematic biases at z~1 are visible.||ZEBRA's Bayesian estimate of redshifts with template optimization. Top and bottom panels as in a). Both the standard deviation of dz/1+z ~ 0.027 and the outlier fraction ~ 0.8 % are improved. Systematic biases are minimized.|