Tracing the Mass-Assembly History of Galaxies with Deep Surveys

We use the optical and near-infrared galaxy samples from the Munich Near-Infrared Cluster Survey (MUNICS), the FORS Deep Field (FDF) and GOODS-S to probe the stellar mass assembly history of field galaxies out to z ~ 5. Combining information on the galaxies' stellar mass with their star-formation rate and the age of the stellar population, we can draw important conclusions on the assembly of the most massive galaxies in the universe: These objects contain the oldest stellar populations at all redshifts probed. Furthermore, we show that with increasing redshift the contribution of star-formation to the mass assembly for massive galaxies increases dramatically, reaching the era of their formation at z ~ 2 and beyond. These findings can be interpreted as evidence for an early epoch of star formation in the most massive galaxies in the universe.Comment: 3 pages, 2 figures; published in B. Aschenbach, V. Burwitz, G. Hasinger, B. Leibundgut (eds.): "Relativistic Astrophysics and Cosmology - Einstein's Legacy. Proceedings of the Conference held in Munich, 2006", ESO Astrophysics Symposia, Springer Verlag, 2007, p. 310. Replaced to match final published versio

Reply to the Comment of G. Feulner

In my reply I present a re-analysis of the data of the Smithsonian Astrophysical Observatory (SAO). For this, a new data reduction method is introduced, allowing a drastic lowering of data scatter, so that the time series of the reduced data clearly shows the ≈ 1% variation of the terrestric solar irradiance in parallel with solar activity. The implications are discussed

The Smithsonian solar constant data revisited: No evidence for a strong effect of solar activity in ground-based insolation data

Apparent evidence for a strong signature of solar activity in ground-based insolation data was recently reported. In particular, a strong increase of the irradiance of the direct solar beam with sunspot number as well as a decline of the brightness of the solar aureole and the measured precipitable water content of the atmosphere with solar activity were presented. The latter effect was interpreted as evidence for cosmic-ray-induced aerosol formation. Here I show that these spurious results are due to a failure to correct for seasonal variations and the effects of volcanic eruptions and local pollution in the data. After correcting for these biases, neither the atmospheric water content nor the brightness of the solar aureole show any significant change with solar activity, and the variations of the solar-beam irradiance with sunspot number are in agreement with previous estimates. Hence there is no evidence for the influence of solar activity on the climate being stronger than currently thought

Magnon heralding in cavity optomagnonics

In the emerging field of cavity optomagnonics, photons are coupled coherently to magnons in solid-state systems. These new systems are promising for implementing hybrid quantum technologies. Being able to prepare Fock states in such platforms is an essential step towards the implementation of quantum information schemes. We propose a magnon-heralding protocol to generate a magnon Fock state by detecting an optical cavity photon. Due to the peculiarities of the optomagnonic coupling, the protocol involves two distinct cavity photon modes. Solving the quantum Langevin equations of the coupled system, we show that the temporal scale of the heralding is governed by the magnon-photon cooperativity and derive the requirements for generating high fidelity magnon Fock states. We show that the nonclassical character of the heralded state, which is imprinted in the autocorrelation of an optical "read" mode, is only limited by the magnon lifetime for small enough temperatures. We address the detrimental effects of nonvacuum initial states, showing that high fidelity Fock states can be achieved by actively cooling the system prior to the protocol.Comment: 17 pages, 14 figures. Correction of typos, version as publishe

Neural principles underlying motor learning and adaptation

Animals, and especially humans, can learn to flexibly adjust their movements to changing environments. The neural principles underlying this remarkable capability are still not fully understood. Among the most prominent brain regions controlling movement is primary motor cortex (M1). Adapted motor behaviour can be related to a change in neural activity within this region. Yet, the rules guiding this activity change, and thus behavioural adaptation, remain unclear. The overall aim of this thesis is to investigate the learning process(es) governing the described change in activity in M1 and, with that, the change in behaviour. Computational modelling is used to study three specific aspects of learning: 1. What constrains learning to favour some neural activity patterns over others? 2. Can we identify where in a hierarchical pathway learning is happening? 3. How can sensory feedback guide the learning process? We start by investigating what kind of biological constraints differentially affect learning of new neural activity that either preserves coactivation patterns between neurons (within-manifold learning), or requires learning of new coactivation patterns (outside-manifold learning). We propose a new explanation - the learnability of feedback signals - for why within-manifold activity patterns can be easier learned than outside-manifold activity patterns. In the second part we develop a hierarchical model of the motor system to investigate whether we can derive where learning has happened from only measuring neural activity. Lastly, we investigate how the brain could implement a biologically plausible learning rule which allows it to correctly assign errors and update recurrent connectivity in a goal-driven manner. Overall, our work offers new perspectives on the role of M1 for motor learning and adaptation, challenges current beliefs, and puts a focus on the role of feedback signals for local plasticity in M1.Open Acces

The connection between star formation and stellar mass: Specific star formation rates to redshift one

We investigate the contribution of star formation to the growth of stellar mass in galaxies over the redshift range 0.5 < z < 1.1 by studying the redshift evolution of the specific star formation rate (SSFR), defined as the star formation rate per unit stellar mass. We use an I-band selected sample of 6180 field galaxies from the Munich Near-Infrared Cluster Survey (MUNICS) with spectroscopically calibrated photometric redshifts. The SSFR decreases with stellar mass at all redshifts. The low SSFRs of massive galaxies indicates that star formation does not significantly change their stellar mass over this redshift range: The majority of massive galaxies have assembled the bulk of their mass before redshift unity. Furthermore, these highest mass galaxies contain the oldest stellar populations at all redshifts. The line of maximum SSFR runs parallel to lines of constant star formation rate. With increasing redshift, the maximum SFR is generally increasing for all stellar masses, from SFR ~ 5 M_sun/yr at z = 0.5 to SFR ~ 10 M_sun/yr at z = 1.1. We also show that the large SSFRs of low-mass galaxies cannot be sustained over extended periods of time. Finally, our results do not require a substantial contribution of merging to the growth of stellar mass in massive galaxies over the redshift range probed. We note that highly obscured galaxies which remain undetected in our sample do not affect these findings for the bulk of the field galaxy population.Comment: 5 pages, 3 colour figures, accepted for publication in MNRAS Letter