On the Luminous and Dark Matter Distribution in Early-Type Galaxies

The way mass is distributed in galaxies plays a major role in shaping their evolution across cosmic time. The galaxy's total mass is usually determined by tracing the motion of stars in its potential, which can be probed observationally by measuring stellar spectra at different distances from the galactic centre, whose kinematics is used to constrain dynamical models. A class of such models, commonly used to accurately determine the distribution of luminous and dark matter in galaxies, is that of equilibrium models. In this Thesis, a novel approach to the design of equilibrium dynamical models, in which the distribution function is an analytic function of the action integrals, is presented. Axisymmetric and rotating models are used to explain observations of a sample of nearby early-type galaxies in the Calar Alto Legacy Integral Field Area survey. Photometric and spectroscopic data for round and flattened galaxies are well fitted by the models, which are then used to get the galaxies' total mass distribution and orbital anisotropy. The time evolution of massive early-type galaxies is also investigated with numerical models. Their structural properties (mass, size, velocity dispersion) are observed to evolve, on average, with redshift. In particular, they appear to be significantly more compact at higher redshift, at fixed stellar mass, so it is interesting to investigate what drives such evolution. This Thesis focuses on the role played by dark-matter haloes: their mass-size and mass-velocity dispersion correlations evolve similarly to the analogous correlations of ellipticals; at fixed halo mass, the haloes are more compact at higher redshift, similarly to massive galaxies; a simple model, in which all the galaxy's size and velocity-dispersion evolution is due to the cosmological evolution of the underlying halo population, reproduces the observed size and velocity-dispersion of massive compact early-type galaxies up to redshift of about 2.

Poly(lactide): from hyperbranched copolyesters to new block copolymers with functional methacrylates

The prologue of this thesis (Chapter 1.0) gives a general overview on lactone based poly(ester) chemistry with a focus on advanced synthetic strategies for ring-opening polymerization, including the emerging field of organo catalysis. This section is followed by a presentation of the state-of the art regarding the two central fields of the thesis: (i) polyfunctional and branched poly(ester)s in Chapter 1.1 as well as (ii) the development of new poly(ester) based block copolymers with functional methacrylates (Chapter 1.2). Chapter 2 deals with the synthesis of new, non-linear poly(ester) structures. In Chapter 2.1, the synthesis of poly(lactide)-based multiarm stars, prepared via a grafting-from method, is described. The hyperbranched poly(ether)-poly(ol) poly(glycerol) is employed as a hydrophilic core molecule. The resulting star block copolymers exhibit potential as phase transfer agents and can stabilize hydrophilic dyes in a hydrophobic environment. In Chapter 2.2, this approach is expanded to poly(glycolide) multiarm star polymers. The problem of the poor solubility of linear poly(glycolide)s in common organic solvents combined with an improvement of the thermal properties has been approached by the reduction of the total chain length. In Chapter 2.3, the first successful synthesis of hyperbranched poly(lactide)s is presented. The ring-opening, multibranching copolymerization of lactide with the “inimer” 5HDON (a hydroxyl-functional lactone monomer) was carefully examined. Besides a precise molecular characterization involving the determination of the degree of branching, we were able to put forward a reaction model for the formation of branching during polymerization. Several innovative approaches to amphiphilic poly(ester)/poly(methacrylate)-based block copolymers are presented in the third part of the thesis (Chapter 3). Block copolymer build-up especially relies on the combination of ring-opening and living radical polymerization. Atom transfer radical polymerization has been successfully combined with lactide ring-opening, using a “double headed” initiator. This strategy allowed for the realization of poly(lactide)-block-poly(2-hydroxyethyl methacrylate) copolymers, which represent promising materials for tissue engineering scaffolds with anti-fouling properties (Chapter 3.1). The two-step/one-pot approach forgoes the use of protecting groups for HEMA by a careful selection of the reaction conditions. A series of potentially biocompatible and partially biodegradable homo- and block copolymers is described in Chapter 3.2. In order to create a block copolymer with a comparably strong hydrophilic character, a new acetal-protected glycerol monomethacrylate monomer (cis-1,3- benzylidene glycerol methacrylate/BGMA) was designed. The hydrophobic poly(BGMA) could be readily transformed into the hydrophilic and water-soluble poly(iso-glycerol methacrylate) (PIGMA) by mild acidic hydrolysis. Block copolymers of PIGMA and poly(lactide) exhibited interesting spherical aggregates in aqueous environment which could be significantly influenced by variation of the poly(lactide)s stereo-structure. In Chapter 3.3, pH-sensitive poly(ethylene glycol)-b-PBGMA copolymers are described. At slightly acidic pH values (pH 4/37°C), they decompose due to a polarity change of the BGMA block caused by progressing acetal cleavage. This stimuli-responsive behavior renders the system highly attractive for the targeted delivery of anti-cancer drugs. In Chapter 3.4, which was realized in cooperation, the concept of biocompatible, amphiphilic poly(lactide) based polymer drug conjugates, was pursued. This was accomplished in the form of fluorescently labeled poly(HPMA)-b-poly(lactide) copolymers. Fluorescence correlation spectroscopy (FCS) of partially biodegradable block copolymer aggregates exhibited fast cellular uptake by human cervix adenocarcinoma cells without showing toxic effects in the examined concentration range (Chapter 4.1). The current state of further projects which will be pursued in future studies is addressed in Chapter 4. This covers the synthesis of biocompatible star block copolymers (Chapter 4.2) and the development of new methacrylate monomers for biomedical applications (Chapters 4.3 and 4.4). Finally, the further investigation of hydroxyl-functional lactones and carbonates which are promising candidates for the synthesis of new hydrophilic linear or hyperbranched biopolymers, is addressed in Chapter 4.5.

Physiologie eines erlernten Körpermodells in Drosophila melanogaster

In der vorliegenden Dissertation wird ein Körpergrößengedächtnis untersucht. Es wird dargestellt, wie diese Information über die Reichweite der Fliege beim Lückenklettern unter kotrollierten Umweltbedingungen erworben und prozessiert wird. Zusätzlich wird geklärt, welche biochemischen Signale benötigt werden, um daraus ein lang anhalten-des Gedächtnis zu formen. Adulte Fliegen sind in der Lage, ihre Körperreichweite zu lernen. Naive Fliegen, die in der Dunkelheit gehalten wurden, versuchen erfolglos, zu breite Lücken zu überqueren, während visuell erfahrene Fliegen die Kletterversuche an ihre Körpergröße anpassen. Erfahrene kleine Fliegen scheinen Kenntnis ihres Nachteils zu haben. Sie kehren an Lückenbreiten um, welche ihre größeren Artgenos-sen durchaus noch versuchen. Die Taufliegen lernen die größenabhängige Reichweite über die visuelle Rückmeldung während des Laufens (aus Parallaxenbewegung). Da-bei reichen 15 min in strukturierter, heller Umgebung aus. Es gibt keinen festgelegten Beginn der sensiblen Phase. Nach 2 h ist das Gedächtnis jedoch konsolidiert und kann durch Stress nicht mehr zerstört oder durch sensorische Eingänge verändert werden. Dunkel aufgezogene Fliegen wurden ausgewählten Streifenmustern mit spezifischen Raumfrequenzen ausgesetzt. Nur die Insekten, welche mit einem als „optimal“ klassi-fizierten Muster visuell stimuliert wurden, sind in der Lage, die Körperreichweite einzu-schätzen, indem die durchschnittliche Schrittlänge in Verbindung mit der visuellen Wahrnehmung gebracht wird. Überraschenderweise ist es sogar mittels partieller Kompensation der Parallaxen möglich, naive Fliegen so zu trainieren, dass sie sich wie kleinere Exemplare verhalten. Da die Experimente ein Erlernen der Körperreich-weite vermuten lassen, wurden lernmutante Stämme beim Lückenüberwinden getes-tet. Sowohl die Ergebnisse von rut1- und dnc1-Mutanten, als auch das defizitäre Klet-tern von oc1-Fliegen ließ eine Beteiligung der cAMP-abhängigen Lernkaskade in der Protocerebralbrücke (PB) vermuten. Rettungsexperimente der rut1- und dnc1-Hinter-gründe kartierten das Gedächtnis in unterschiedliche Neuronengruppen der PB, wel-che auch für die visuelle Ausrichtung des Kletterns benötigt werden. Erstaunlicher-weise haben laterale lokale PB-Neurone und PFN-Neurone (Projektion von der PB über den fächerförmigen Körper zu den Noduli) verschiedene Erfordernisse für cAMP-Signale. Zusammenfassend weisen die Ergebnisse darauf hin, dass hohe Mengen an cAMP/PKA-Signalen in den latero-lateralen Elementen der PB benötigt werden, wäh-rend kolumnäre PFN-Neurone geringe oder keine Mengen an cAMP/PKA erfordern. Das Körperreichweitengedächtnis ist vermutlich das am längsten andauernde Ge-dächtnis in Drosophila. Wenn es erst einmal konsolidiert ist hält es länger als drei Wo-chen.rnAußerdem kann die Fruchtliege Drosophila melanogaster trainiert werden, die kom-plexe motorische Aufgabe des Lückenkletterns zu optimieren. Die trainierten Fliegen werden erfolgreicher und schneller beim Überqueren von Lücken, welche größer sind als sie selbst. Dabei existiert eine Kurzeitkomponente (STM), die 40 min nach dem ersten Training anhält. Nach weiteren vier Trainingsdurchläufen im Abstand von 20 min wird ein Langzeitgedächtnis (LTM) zum Folgetag geformt. Analysen mit Mutati-onslinien wiesen eine Beteiligung der cAMP-abhängigen Lernkaskade an dieser Ge-dächtnisform auf. Rettungsexperimente des rut2080-Hintergrunds kartierten sowohl das STM, als auch das LTM in PFN-Neuronen. Das STM kann aber ebenso in den alpha- und beta- Loben der Pilzkörper gerettet werden.rnLetztendlich sind wildtypische Fliegen sogar in der Lage, sich an einen Verlust eines Mittelbeintarsuses und dem einhergehenden Fehlen des Adhäsionsorgans am Tarsusende anzupassen. Das Klettern wird zwar sofort schlechter, erholt sich aber bis zum Folgetag wieder auf ein normales Niveau. Dieser neue Zustand erfordert ein Ge-dächtnis für die physischen Möglichkeiten, die nur durch plastische Veränderungen im Nervensystem des Insekts erreicht werden können.

Un nuovo indicatore di segregazione radiale delle blue stragglers

Le blue straggler stars (BSS) sono un importante strumento osservativo per gli studi mirati alla determinazione dell'evoluzione dinamica degli ammassi globulari. La loro distribuzione radiale, influenzata dal fenomeno di segregazione di massa, costituisce un efficace strumento per la determinazione dello stato di rilassamento del sistema. In questo lavoro di tesi sono esplorate le potenzialità di un nuovo indicatore di segregazione centrale delle BSS: la cosiddetta "Area Positiva (A+)", definita come la differenza tra l'area sottesa dalla distribuzione radiale cumulativa delle BSS e quella di una popolazione di riferimento. Per costruzione, questo parametro e` indicatore sensibile del livello di segregazione delle BSS. Il campione di ammassi e` costituito da 18 oggetti di bassa densità e concentrazione recentemente osservati nell'ambito di una survey ultravioletta con la camera WFC3/UVIS (Piotto et al. 2015) e 8 sistemi di densità più elevata, analizzati in lavori precedenti. Per ciascun ammasso sono state selezionate le popolazioni di BSS e di stelle di riferimento lungo la sequenza principale o il ramo delle giganti e sono state costruite le rispettive distribuzioni radiali cumulative, da cui e` stata poi determinata l'Area Positiva. Sono state infine individuate forti correlazioni tra A+ e alcuni parametri strutturali/dinamici degli ammassi, in particolare col tempo di rilassamento e la densita` centrali. Questi risultati dimostrano che il parametro A+ e` un buon misuratore del grado di evoluzione dinamica degli ammassi globulari.

Clues on the frequency of giant planets in wide orbits

The available results of deep imaging searches for planetary companions around nearby stars provide us useful constraints on the frequencies of giant planets in very wide orbits. Here we present some preliminary results of the Monte Carlo simulation which compare the published detection limits with the generated planetary masses and orbital parameters. This allow us to consider the impications of the null detection, which comes from the direct imaging techniques, on the distributions of mass and semimajor axis derived from the results of the other search techniques and also to check the agreement of the observations with the available planetary formation models.

Brown Dwarf Binaries

Nearly 500 brown dwarfs have been discovered in recent years. The majority of these brown dwarfs exist in the solar neighborhood, yet determining their fundamental properties (mass, age, temperature & metallicity) has proved to be quite difficult, with current estimates relying heavily on theoretical models. Binary brown dwarfs provide a unique opportunity to empirically determine fundamental properties, which can then be used to test model predictions. In addition, the observed binary fractions, separations, mass ratios, & orbital eccentricities can provide insight into the formation mechanism of these low-mass objects. I will review the results of various brown dwarf multiplicity studies, and will discuss what we have learned about the formation and evolution of brown dwarfs by examining their binary properties as a function of age and mass.

Infrared Parallaxes of Young Field Brown Dwarfs and Connections to Directly Imaged Gas-Giant Exoplanets

We have measured high-precision infrared parallaxes with the Canada-France-Hawaii Telescope for a large sample of candidate young (approximate to 10-100 Myr) and intermediate-age (approximate to 100-600 Myr) ultracool dwarfs, with spectral types ranging from M8 to T2.5. These objects are compelling benchmarks for substellar evolution and ultracool atmospheres at lower surface gravities (i.e., masses) than most of the field population. We find that the absolute magnitudes of our young sample can be systematically offset from ordinary (older) field dwarfs, with the young late-M objects being brighter and the young/dusty mid-L (L3-L6.5) objects being fainter, especially at J band. Thus, we conclude the "underluminosity" of the young planetary-mass companions HR 8799b and 2MASS J1207-39b compared to field dwarfs is also manifested in young free-floating brown dwarfs, though the effect is not as extreme. At the same time, some young objects over the full spectral type range of our sample are similar to field objects, and thus a simple correspondence between youth and magnitude offset relative to the field population appears to be lacking. Comparing the kinematics of our sample to nearby stellar associations and moving groups, we identify several new moving group members, including the first free-floating L dwarf in the AB Dor moving group, 2MASS J0355+11. Altogether, the effects of surface gravity (age) and dust content on the magnitudes and colors of substellar objects appear to be degenerate. (C) 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim

A Near-Infrared Spectroscopic Study of Young Field Ultracool Dwarfs

We present a near-infrared (0.9-2.4 mu m) spectroscopic study of 73 field ultracool dwarfs having spectroscopic and/or kinematic evidence of youth (approximate to 10-300 Myr). Our sample is composed of 48 low-resolution (R approximate to 100) spectra and 41 moderate-resolution spectra (R greater than or similar to 750-2000). First, we establish a method for spectral typing M5-L7 dwarfs at near-IR wavelengths that is independent of gravity. We find that both visual and index-based classification in the near-IR provides consistent spectral types with optical spectral types, though with a small systematic offset in the case of visual classification at J and K band. Second, we examine features in the spectra of similar to 10 Myr ultracool dwarfs to define a set of gravity-sensitive indices based on FeH, VO, Ki, Nai, and H-band continuum shape. We then create an index-based method for classifying the gravities of M6-L5 dwarfs that provides consistent results with gravity classifications from optical spectroscopy. Our index-based classification can distinguish between young and dusty objects. Guided by the resulting classifications, we propose a set of low-gravity spectral standards for the near-IR. Finally, we estimate the ages corresponding to our gravity classifications.

Rwandan youth in the development of music industry

In this days for ever, the Rwandan youth are more active in the development of music industry, the recording studio are created every day, and the number of musician is increasing from one day to another day, it is too early to get the statistic; some of the youth are dropped out their studies to develop their career of music; the question was how many of them are developing their career to become the Professional? WHY IN THESE DAYS, RWANDAN YOUTH ARE WORKING HARDLY IN THE DEVELOPMENT OF MUSIC INDUSTRY?” it was not easy for me to get the accurate answers; some questions remains in my mind like -Are they working for money-music as a job (professional)? -Are they willing to become célèbre-stars? -Is it for the entertainment/Relaxing? -Is it because they love music? -Are they escaping the problems-Music as an escape domain? -Are they exploring their free time? -Are they using the music as the way of expressing their views? Those questions require analysing each question deeply, and getting the answers from the singers and listeners of music or DJ, in order to confirm the causes of being more active in music industry for the Rwandan youth. I am not interesting to make a deep research but to analyze and I hope this article will help the students and many researchers to develop and find out the exact causes. As my aim is to open the door for the researchers, briefly let us analyze all those above questions one to one based on the main causes as the motivation of forcing the Rwandan youth to be in the industry music.

A Stellar Census of the Tucana-Horologium Moving Group

We report the selection and spectroscopic confirmation of 129 new late-type (SpT = K3-M6) members of the Tucana-Horologium moving group, a nearby (d similar to 40 pc), young (tau similar to 40 Myr) population of comoving stars. We also report observations for 13 of the 17 known Tuc-Hor members in this spectral type range, and that 62 additional candidates are likely to be unassociated field stars; the confirmation frequency for new candidates is therefore 129/191 = 67%. We have used radial velocities, Ha emission, and Li-6708 absorption to distinguish between contaminants and bona fide members. Our expanded census of Tuc-Hor increases the known population by a factor of similar to 3 in total and by a factor of similar to 8 for members with SpT >= K3, but even so, the K-M dwarf population of Tuc-Hor is still markedly incomplete. Our expanded census allows for a much more detailed study of Tuc-Hor than was previously feasible. The spatial distribution of members appears to trace a two-dimensional sheet, with a broad distribution in X and Y, but a very narrow distribution (+/- 5 pc) in Z. The corresponding velocity distribution is very small, with a scatter of +/- 1.1 km s(-1) about the mean UVW velocity for stars spanning the entire 50 pc extent of Tuc-Hor. We also show that the isochronal age (tau similar to 20-30 Myr) and the lithium depletion boundary age (tau similar to 40 Myr) disagree, following the trend in other pre-main-sequence populations for isochrones to yield systematically younger ages. The H alpha emission line strength follows a trend of increasing equivalent width with later spectral type, as is seen for young clusters. We find that moving group members have been depleted of measurable lithium for spectral types of K7.0-M4.5. None of our targets have significant infrared excesses in the WISE W3 band, yielding an upper limit on warm debris disks of F < 0.7%. Finally, our purely kinematic and color-magnitude selection procedure allows us to test the efficiency and completeness for activity-based selection of young stars. We find that 60% of K-M dwarfs in Tuc-Hor do not have ROSAT counterparts and would have been omitted in X-ray-selected samples. In contrast, GALEX UV-selected samples using a previously suggested criterion for youth achieve completeness of 77% and purity of 78%, and we suggest new SpT-dependent selection criteria that will yield > 95% completeness for tau similar to 40 Myr populations with GALEX data available.

Quantification of relativistic perturbation forces on spacecraft trajectories

The intent of the work presented in this thesis is to show that relativistic perturbations should be considered in the same manner as well known perturbations currently taken into account in planet-satellite systems. It is also the aim of this research to show that relativistic perturbations are comparable to standard perturbations in speciffc force magnitude and effects. This work would have been regarded as little more then a curiosity to most engineers until recent advancements in space propulsion methods { e.g. the creation of a artiffcial neutron stars, light sails, and continuous propulsion techniques. These cutting-edge technologies have the potential to thrust the human race into interstellar, and hopefully intergalactic, travel in the not so distant future. The relativistic perturbations were simulated on two orbit cases: (1) a general orbit and (2) a Molniya type orbit. The simulations were completed using Matlab's ODE45 integration scheme. The methods used to organize, execute, and analyze these simulations are explained in detail. The results of the simulations are presented in graphical and statistical form. The simulation data reveals that the speciffc forces that arise from the relativistic perturbations do manifest as variations in the classical orbital elements. It is also apparent from the simulated data that the speciffc forces do exhibit similar magnitudes and effects that materialize from commonly considered perturbations that are used in trajectory design, optimization, and maintenance. Due to the similarities in behavior of relativistic versus non-relativistic perturbations, a case is made for the development of a fully relativistic formulation for the trajectory design and trajectory optimization problems. This new framework would afford the possibility of illuminating new more optimal solutions to the aforementioned problems that do not arise in current formulations. This type of reformulation has already showed promise when the previously unknown Space Superhighways arose as a optimal solution when classical astrodynamics was reformulated using geometric mechanics.

Evidence for distinct modes of solar activity

The Sun shows strong variability in its magnetic activity, from Grand minima to Grand maxima, but the nature of the variability is not fully understood, mostly because of the insufficient length of the directly observed solar activity records and of uncertainties related to long-term reconstructions. Here we present a new adjustment-free reconstruction of solar activity over three millennia and study its different modes. Methods. We present a new adjustment-free, physical reconstruction of solar activity over the past three millennia, using the latest verified carbon cycle, 14C production, and archeomagnetic field models. This great improvement allowed us to study different modes of solar activity at an unprecedented level of details. Results. The distribution of solar activity is clearly bi-modal, implying the existence of distinct modes of activity. The main regular activity mode corresponds to moderate activity that varies in a relatively narrow band between sunspot numbers 20 and 67. The existence of a separate Grand minimum mode with reduced solar activity, which cannot be explained by random fluctuations of the regular mode, is confirmed at a high confidence level. The possible existence of a separate Grand maximum mode is also suggested, but the statistics is too low to reach a confident conclusion. Conclusions. The Sun is shown to operate in distinct modes – a main general mode, a Grand minimum mode corresponding to an inactive Sun, and a possible Grand maximum mode corresponding to an unusually active Sun. These results provide important constraints for both dynamo models of Sun-like stars and investigations of possible solar influence on Earth’s climate.

Predictive Margins and Marginal Effects in Stata

Tables of estimated regression coefficients, usually accompanied by additional information such as standard errors, t-statistics, p-values, confidence intervals or significance stars, have long been the preferred way of communicating results from statistical models. In recent years, however, the limits of this form of exposition have been increasingly recognized. For example, interpretation of regression tables can be very challenging in the presence of complications such as interaction effects, categorical variables, or nonlinear functional forms. Furthermore, while these issues might still be manageable in the case of linear regression, interpretational difficulties can be overwhelming in nonlinear models such as logistic regression. To facilitate sensible interpretation of such models it is often necessary to compute additional results such as marginal effects, predictive margins, or contrasts. Moreover, smart graphical displays of results can be very valuable in making complex relations accessible. A number of helpful commands geared at supporting these tasks have been recently introduced in Stata, making elaborate interpretation and communication of regression results possible without much extra effort. Examples of such commands are -margins-, -contrasts-, and -marginsplot-. In my talk, I will discuss the capabilities of these commands and present a range of examples illustrating their use.

The HARPS search for southern extra-solar planets

The meter-per-second precision achieved by today’s velocimeters enables us to search for 1−10 M⊕ planets in the habitable zone of cool stars. This paper reports on the detection of three planets orbiting GJ 163 (HIP 19394), a M3 dwarf monitored by our ESO/HARPS search for planets. We made use of the HARPS spectrograph to collect 150 radial velocities of GJ 163 over a period of eight years. We searched the radial-velocity time series for coherent signals and found five distinct periodic variabilities. We investigated the stellar activity and called into question the planetary interpretation for two signals. Before more data can be acquired we concluded that at least three planets are orbiting GJ 163. They have orbital periods of Pb = 8.632 ± 0.002, Pc = 25.63 ± 0.03, and Pd = 604 ± 8 days and minimum masses msini = 10.6 ± 0.6, 6.8 ± 0.9, and 29 ± 3 M⊕, respectively. We hold our interpretations for the two additional signals with periods P(e) = 19.4 and P(f) = 108 days. The inner pair presents an orbital period ratio of 2.97, but a dynamical analysis of the system shows that it lays outside the 3:1 mean motion resonance. The planet GJ 163c, in particular, is a super-Earth with an equilibrium temperature of Teq = (302 ± 10)(1 − A)1/4 K and may lie in the so-called habitable zone for albedo values (A = 0.34 − 0.89) moderately higher than that of Earth (A⊕ = 0.2−0.3).

The HARPS search for southern extra-solar planets

The vast diversity of planetary systems detected to date is defying our capability of understanding their formation and evolution. Well-defined volume-limited surveys are the best tool at our disposal to tackle the problem, via the acquisition of robust statistics of the orbital elements. We are using the HARPS spectrograph to conduct our survey of ≈850 nearby solar-type stars, and in the course of the past nine years we have monitored the radial velocity of HD 103774, HD 109271, and BD-061339. In this work we present the detection of five planets orbiting these stars, with msin   (i) between 0.6 and 7 Neptune masses, four of which are in two multiple systems, comprising one super-Earth and one planet within the habitable zone of a late-type dwarf. Although for strategic reasons we chose efficiency over precision in this survey, we have the capability to detect planets down to the Neptune and super-Earth mass range as well as multiple systems, provided that enough data points are made available.