Made-to measure galaxy models - I Methodology

We re-derive the made-to-measure method of Syer and Tremaine 1996, for modelling stellar systems and individual galaxies, and demonstrate how extensions to the made-to-measure method may be implemented and used. We illustrate the enhanced made-to-measure method by determining the mass-to-light ratio of a galaxy modelled as a Plummer sphere. From the standard galactic observables of surface brightness and line-of-sight velocity dispersion together with the h_4 Gauss-Hermite coefficient of the line-of-sight velocity distribution, we successfully recover the true mass-to-light ratio of our toy galaxy. Using kinematic data from Kleyna et al 2002, we then estimate the mass-to-light ratio of the dwarf spheroidal galaxy Draco achieving a V-band value of 539 \pm 136 M_{\odot} / L_{\odot}. We describe the main aspects of creating a made-to-measure galaxy model and show how the key modelling parameters may be determined.Comment: 18 pages, 15 figure

Made-to-measure galaxy models - II Elliptical and Lenticular Galaxies

We take a sample of 24 elliptical and lenticular galaxies previously analysed by the SAURON project using three-integral dynamical models created with Schwarzschild's method, and re-analyse them using the made-to-measure (M2M) method of dynamical modelling. We obtain good agreement between the two methods in determining the dynamical mass-to-light (M/L) ratios for the galaxies with over 80% of ratios differing by < 10% and over 95% differing by < 20%. We show that (M/L)_M2M is approximately equal to (M/L)_Sch. For the global velocity dispersion anisotropy parameter delta, we find similar values but with fewer of the made-to-measure models tangentially anisotropic by comparison with their SAURON Schwarzschild counterparts. Our investigation is the largest comparative application of the made-to-measure method to date.Comment: 14 pages, 8 figures and 5 table

Made-to-measure galaxy models - III Modelling with Milky Way observations

We demonstrate how the Syer & Tremaine made-to-measure method of stellar dynamical modelling can be adapted to model a rotating galactic bar. We validate our made-to-measure changes using observations constructed from the existing Shen et al. (2010) N-body model of the Milky Way bar, together with kinematic observations of the Milky Way bulge and bar taken by the Bulge Radial Velocity Assay (BRAVA). Our results for a combined determination of the bar angle and bar pattern speed (~30 degrees and ~40 km/s/kpc) are consistent with those determined by the N-body model. Whilst the made-to-measure techniques we have developed are applied using a particular N-body model and observational data set, they are in fact general and could be applied to other Milky Way modelling scenarios utilising different N-body models and data sets. Additionally, we use the exercise as a vehicle for illustrating how N-body and made-to-measure methods might be combined into a more effective method.Comment: Accepted for publication, 10 pages, 7 figure

Zmym4 is required for early cranial gene expression and craniofacial cartilage formation

The Six1 transcription factor plays important roles in the development of cranial sensory organs, and point mutations underlie craniofacial birth defects. Because Six1’s transcriptional activity can be modulated by interacting proteins, we previously screened for candidate interactors and identified zinc-finger MYM-containing protein 4 (Zmym4) by its inclusion of a few domains with a bona fide cofactor, Sine oculis binding protein (Sobp). Although Zmym4 has been implicated in regulating early brain development and certain cancers, its role in craniofacial development has not previously been described

N-corps évolutif pour la modélisation photométrique et dynamique des galaxies de type précoce

Early type galaxies present a large sample of photometric and dynamical structures. These signatures are fossil records of their formation and evolution processes. Their study helps us to retrace their formation and past evolution history. In order to understand their structures, models reproducing observations are built. The developed method is a generalisation of the one introduced by Syer and Tremaine (1996), consisting in a N-body, the particles' weights of which are changing along time. The presented code is adapted for integral field spectroscopy data, and is able to reproduce luminosities as well as dynamics of observed galaxies. These models are based on SAURON data obtained on early type galaxies. Preliminary results have been obtained on M 87 and NGC 3377. An appendix is presenting observations of the galaxy NGC 936.Les galaxies de type précoce présentent un large éventail de structures photométriques et dynamiques. Ces structures sont autant de signatures fossiles des processus de formation et d'évolution de ces galaxies. Leur étude nous permet de remonter à l'histoire de leur formation et de leur évolution. Dans le but de comprendre les structures observées, des modèles reproduisant des observations sont construits. La méthode développée est une généralisation de celle introduite par Syer & Tremaine (1996), consistant en un N-corps dont le poids des particules varie au cours du temps. Le code présenté est adapté à des données de spectroscopie intégrale de champ, et est à-même de reproduire la photométrie ainsi que la dynamique des galaxies observées. Ces modèles sont basés sur des données SAURON obtenues sur des galaxies de type précoce. Des modèles préliminaires ont été obtenus pour les galaxies M 87 et NGC 3377. Une annexe présente en outre des observations menées sur NGC 936

Modeling the color diversity of Kuiper Belt Objets : Cometary Activity as an alternative rejuvenating process.

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Modeling the color diversity of Kuiper Belt Objets : Cometary Activity as an alternative rejuvenating process.

International audienc

MBOSS Color Evolution Tracks: A Simple Empirical Model

International audienc