M dwarf stars make up over 70% of stars by number in the Milky Way Galaxy and are known to host at least two exoplanets per star on average. Using mutually eclipsing double-lined spectroscopic binary stars (SB2 EBs), astronomers can empirically measure stellar properties of M dwarf stars including mass and radius. However, empirical measurements systematically differ from the predictions of stellar evolutionary models and show large scatter. Some M dwarf stars are outliers, with radii that are a factor of 2-to-3 larger than model predictions, assuming they were measured accurately. In this dissertation, I investigated whether the outliers, systematic offset, and the scatter seen in the mass-radius diagram are physical, using SB2 EBs with photometry from NASA's Kepler Mission and high-resolution near-infrared ground-based spectroscopy. Empirical measurements using space-based photometry and high-resolution near-infrared ground-based spectroscopy, together with Bayesian model-fitting techniques, provide significant advancements over previous measurements. For this dissertation work, a sample of Kepler EBs were carefully chosen to be detached and non-interacting. I conducted a radial velocity survey of the sample using Immersion GRating INfrared Spectrometer (IGRINS) with the Discovery Channel Telescope (DCT) and iSHELL with NASA's Infrared Telescope Facility (IRTF). Combined with high-precision Kepler data, I determined the masses and radii of the component stars in the sample. I also determined a new mass-radius relationship of M dwarf stars using the sample of Kepler EB systems. My investigation showed that the outliers in the mass-radius diagram of M dwarf stars are not physical and they are due to the quality of data and from analysis using different pipelines. I also showed that the offset and scatter in the mass-radius diagram are persistent, which are not from the measurement uncertainties. This suggests the need for an extra degree of freedom to accurately capture the discrepancies between the empirical measurements and model predictions. Lastly, I showed that reduced convective heat flow due to enhanced magnetic fields from rapid stellar rotation can account for the offset and scatter in the measurements.

We carried out a near-infrared radial velocity search for Jupiter-mass planets around 36 late M dwarfs. This survey was the first of its kind undertaken to monitor radial velocity variability of these faint dwarfs. For this unique survey we employed the 10-m Keck II on Mauna Kea in Hawaii. With a resolution of 20,000 on the near-infrared spectrograph, NIRSPEC, we monitored these stars over four epochs in 2007. In addition to the measurement of relative radial velocity we established physical properties of these stars. The physical properties of M dwarfs we determined included the identification of neutral atomic lines, the measurement of pseudo-equivalent widths, masses, surface gravity, effective temperature, absolute radial velocities, rotational velocities and rotation periods. The identification of neutral atomic lines was carried out using the Vienna Atomic line Database. We were able to confirm these lines that were previously identified. We also found that some of the lines observed in the K-type stars, such as Mg I though weak, still persist in late M dwarfs. Using the measurement of pseudo-equivalent widths (p-EW) of 13 neutral atomic lines, we have established relations between p-EW and spectral type. Such relations serve as a tool in determining the spectral type of an unknown dwarf star by means of measuring its p-EW. We employed the mass-luminosity relation to compute the masses of M dwarfs. Our calculations indicate these dwarfs to be in the range of 0.1 to 0.07 solar masses. This suggests that some of the late M dwarfs appear to be in the Brown dwarf regime. Assuming their radii of 0.1 solar radii, we calculated their surface gravity. The mean surface gravity is, log g = 5.38. Finally their effective temperature was determined by using the spectral-type iii temperature relationship. Our calculations show effective temperatures in the range of 3000 2300 K. Comparison of these values with models in literature show a good agreement. The absolute radial and rotational velocities of our targets were also calculated. Values of rotational velocities indicate that M dwarfs are, in general, slow rotators. Using our result and that from literature, we extended our study of rotational velocities to L dwarfs. Our observations show an increase in rotational velocities from late M to L dwarfs. We also find that the mean periods of M dwarfs are less than 10 hours. In order to improve our precision in measuring relative radial velocity (RV), we employed the use of deconvolution method. With this method we were able to ameliorate relative RV precision from 300 m/s to 200 m/s. This was a substantial improvement in our ability to detect gas-giant planets. However none of the 15 dwarfs we monitored indicate a presence of companions. This null result was then used to compute the upper limit to the binary frequency and close-in Jupiter mass planetary frequency. We find the binary frequency to be 11% while the planetary frequency was 1.20%.

A trend in polarization as predicted by theoretical models was validated, and atmospheric dust grain sizes and projected rotational velocities for these objects were estimated. Comprehensive studies of UDs are proving to be crucial not only in our understanding of UDs but also for star and planet formation as brown dwarfs represent their lower and upper mass boundaries, respectively. Brown dwarfs (BD) were mere theoretical astrophysical objects for more than three decades (Kumar (1962)) till their first observational detection in 1995 (Rebolo et al. (1995), Nakajima et al. (1995)). These objects are intermediate in mass between stars and planets. Since their observational discovery these objects have been studied thoroughly and holistically.Various methods for searching and characterizing these objects in different regions of the sky have been put forward and tested with great success. Theoretical models describing their physical, atmospheric and chemical processes and properties have been proposed and have been validated with a large number of observational results. The work presented in this dissertation is a compilation of synoptic studies of ultracool dwarfs(UDs)¹. [Footnote 1:]. [bullet] A search for wide binaries around solar type stars in upper scorpio OB association (Upper Sco) do indicate (the survey is not yet complete) a deficit of BD binaries at these large separations ([less than] 5AU). [bullet] Twenty six new UDs were discovered at low galactic latitudes in our survey from archival data and a novel technique using reduced proper motion. [bullet] Six field UDs were discovered by spectroscopic follow-up of the candidates selected from a deep survey. [bullet] Optical interferometry was used to independently determine the orbit of the companion of HD33636 which was initially determined using Hubble Space Telescope(HST)astrometry and radial velocity found. Some inconsistency in the HST determined orbit and mass. [bullet] Optical linear polarization in UDs was used to investigate the dust propertied in their atmospheres. Footnote 1: We use the term "ultracool dwarfs" as the mass of most of the objects mentioned is unknown, which is required to classify an object as a brown dwarf. We define objects later than M7 as ultra cool dwarfs.

Brown dwarfs are substellar objects that fall in-between the smallest stars and largest planets in size and temperature. Due to their relatively cool temperatures, the atmospheres of these 'failed stars' have been shown to exhibit interesting properties such as iron, silicate, and salt clouds. Theoretical atmospheric models based on known physics and chemistry can be used as tools to interpret and understand our observations of brown dwarfs. I have fit archival and new infrared spectra of over 300 brown dwarfs with atmospheric models. Using the parameters of the best-fit models as estimates for the physical properties of the brown dwarfs in my sample, I have performed a survey of how brown dwarfs evolve with spectral type and temperature. I present my fit results and observed trends. I use these fit results to note where current atmospheric models are able to well-replicate the data and where the models and data conflict.

M dwarfs have been the subject of renewed interest as potential habitable planet hosts and have increasingly become the targets of planet detection surveys. Currently, however, the number of detections of transiting M dwarf planets remain low. The characterisation of M dwarf activity is an important consideration for such surveys, and provides constraints on the modelling of magnetically active low mass stars. Currently the spottedness of M dwarfs is not well understood owing to their intrinsic faintness and the lack of diagnostics for assessing starspot morphologies and distributions. The WFCAM Transit Survey (WTS) contains long term observations of M dwarfs in the near infra-red and presents an opportunity to study the long term variability of M dwarfs. The M dwarfs in the WTS are identified by use of colour-spectral type relations, and the periodically variable M dwarfs in the sample are detected using a Lomb-Scargle periodogram analysis. A total of 72 periodically variable M dwarfs are found with periods ranging from 0.16 to 90.33 days. The relations between the spectral subtypes, amplitudes and periods are studied and comparisons to earlier works studying M dwarf rotation are made. A number of examples of significant spot evolution are found, which exhibit complex light curve morphologies that vary in form and amplitude over periods of months to years. This provides an indication as to the nature of the spottedness of these stars. Simulations are performed to probe the connection between spot coverage, temperature and light curve amplitude. Using the results from these simulations, the spot coverage fractions of the WTS M dwarfs are estimated and they are found to be heavily spotted. Dynamic models with spots evolving at various average rates are used to explore how spot evolution can drive increased dispersion in the light curves, and to what extent this affects the detectability of periodicity by the method used. It is found that spot evolution can invoke significant noise in an M dwarf light curve, and in combination with photon noise, can in some instances inhibit the detection of a period. In reflection of the results, the relation between the light curve dispersion and spot coverage of the WTS M dwarfs is considered and it is found that more heavily spotted M dwarfs have intrinsically noisier light curves. The morphologies of the light curves produced by the simulations, and the manner in which they evolve, are qualitatively similar to the real M dwarfs in the WTS sample and indicate how models extrapolated from sunspot distributions can explain behaviour seen in active M dwarf light curves.

Les naines brunes sont des astres incapables de déclencher et soutenir des réactions nucléaires dans leur cœur. En l’absence de cette source d’énergie, leur luminosité diminue avec le temps jusqu’à leur extinction complète. Leur flux aux longueurs d’onde de 0,8 à 2,35 μm est particulièrement altéré par l’humidité contenue dans l’atmosphère terrestre, ce qui complique l’étude de ces astres. Le but de la présente recherche est de vérifier si la division par un spectre d’étoile A0 est un moyen de corriger l’altération causée par l’atmosphère terrestre sur cette partie de leur spectre. Tout d’abord, des notions, pertinentes à la compréhension de ce travail, sont abordées. L’introduction présente quelques notions sur les naines brunes et sur l’atmosphère terrestre. Le deuxième chapitre concerne le traitement des données. Il traite de la calibration, de la mise en évidence du problème de non-répétabilité de la position de la fente du spectromètre SIMON ainsi que de ses causes. Il porte aussi sur l’uniformisation de la réponse des pixels et de la soustraction du ciel pour extraire les spectres. La méthode employée pour étudier l’effet de l’atmosphère terrestre sur les spectres de naines brunes y est présentée. Le troisième chapitre analyse les résultats obtenus par l’utilisation de l’étoile de référence de type A0 comme calibration pour corriger le spectre de naine brune, en assumant un même effet de l’atmosphère terrestre sur les deux types d’astres. Nous ne pouvons conclure, avec certitude, que l’absorption tellurique affecte de la même façon les deux spectres ni de quelle façon exactement ils sont affectés. Une recherche supplémentaire nécessitant de nouvelles prises de données à des masses d’air et à des taux d’humidité variés est requise. / Brown dwarfs are celestial bodies unable to sustain nuclear reactions. For this reason their luminosity declines until complete extinction. Their flux, particularly in the band between 0,8 and 2,35 μm, is absorbed by the water vapor in the terrestrial atmosphere. The goal of this research is to find a way to correct this part of their spectra affected by this effect. First, general notions needed to understand the project are exposed. The second chapter concerns the data reduction. The calibration, the problem of the position repeatability of the slit of the spectrometer SIMON and his cause are exposed. It discusses techniques to even up the pixels’ response and the substraction of the sky from the spectra. The method used to study the atmosphere effect on brown dwarf spectra is presented. The third chapter analyses the results that use the A0 reference star to correct the brown dwarf spectrum. We cannot conclude that the A0 spectrum is affected in the same way as the brown dwarf spectrum by the terrestrial atmosphere. The data from a single night do not allow a good analysis of this effect as a function of air mass and humidity level. Others missions are needed.

L'outil développé dans le cadre de cette thèse est disponible à l'adresse suivante: www.astro.umontreal.ca/~malo/banyan.php / Près de 70% des étoiles de la Galaxie ont une masse inférieure à ~0.8 Msun. Cependant, étant donné que ces étoiles sont plus difficilement observables en raison de leur plus faible luminosité, cette statistique ne reflète pas le recensement actuel de la population d'étoiles de faible masse dans le voisinage solaire, ni dans les groupes cinématiques d'étoiles jeunes. Cette population a une grande importance pour contraindre la forme de la fonction de masse Galactique, et aussi pour contraindre les modèles évolutifs. Les étoiles de faible masse sont aussi d'excellentes cibles pour la recherche d'exoplanètes avec des techniques variées (imagerie directe, vitesse radiale, transit). La caractérisation des exoplanètes autour de ces étoiles est tributaire des connaissances fondamentales sur celles-ci, c'est-à-dire de leur luminosité bolométrique, température effective, rayon et âge. Dans la présente thèse, dont le but est d'identifier et caractériser les étoiles de faible masse, une méthode statistique a été développée afin d'établir quantitativement l'appartenance d'une étoile à un groupe en dérivant une probabilité d'association. Cette méthode combine l'inférence Bayesienne et des modèles empiriques de plusieurs observables, dont la luminosité, vitesse spatiale et position galactique, de membres confirmés de 7 groupes d'étoiles jeunes (8-120 Mans) ainsi que d'étoiles vieilles du champ. Les étoiles ayant une probabilité d'association minimale de 90% sont considérées comme des candidates. L'analyse développée prédit aussi la vitesse radiale et la distance trigonométrique qu'une étoile aurait dans une association donnée. L'analyse a montré, pour les 177 membres confirmés, un excellent accord entre les paramètres prédits et observés, soit de 1.9 km/s et 10% respectivement, pour la vitesse radiale et la parallaxe. La mesure de ces paramètres pour les candidates est donc une bonne manière de confirmer leur appartenance à l'association. Cette méthode robuste a été appliquée sur un échantillon de 758 étoiles montrant des signes de jeunesse (émission H$\alpha$ et rayons X). L'analyse a permis d'identifier 214 candidates hautement probables, et le suivi spectroscopique de ces étoiles a permis, jusqu'à présent, de confirmer la justesse de la prédiction en vitesse radiale pour 130 étoiles. Ces observations spectroscopiques ont aussi permis de mesurer leur vitesse de rotation, qui s'est avérée élevée comparativement aux étoiles vieilles du champs. La mesure de la distance trigonométrique était aussi en accord avec la prédiction pour 18 candidates jeunes. Grâce aux membres dont l'appartenance à un groupe jeune a été confirmée, un modèle empirique de la luminosité en rayon X des étoiles a pu être établi. Cette luminosité s'est avérée significativement plus élevée (environ 4 fois plus) pour les étoiles des groupes les plus jeunes (~8-12 Mans) que pour celles des groupes plus vieux (~120 Mans). Cet observable constitue donc un bon indicateur d'âge. La comparaison des spectres de 59 candidates à des modèles d'atmosphère a permis de déterminer trois paramètres fondamentaux: la luminosité bolométrique, la température effective et le rayon. Globalement, les candidates jeunes ont une luminosité plus élevée et un rayon plus grand que les étoiles vieilles. De récents modèles évolutifs incluant le traitement d'une dynamo de type rotationnel et générant un champ magnétique de surface de 1 à 2.5 kGauss ont été utilisés pour déterminer l'âge isochronal de ces étoiles. Les âges ainsi déterminés pour les étoiles de l'association \beta Pictoris en utilisant des étoiles de types spectraux différents sont davantage cohérents (types K5V-M0V: 24 Mans, types M1V-M4V: 14 Mans) et sont aussi cohérents avec l'âge déterminé indépendamment pour le groupe en utilisant l'abondance du lithium des membres de faible masse (26 Mans). / About 70% of the stars in the Galaxy have a mass inferior than ~0.8 Msun. However, this statistic does not reflect the current census population of low mass in the solar neighborhood and in young kinematic groups, since their low luminosity make their observation more difficult. This population is of great interest to check the validity of the Galactic mass function, and also to constraint evolutionary models. The low-mass stars are also excellent targets for the search for exoplanets using various techniques (direct imaging, radial velocity, transit). The characterization of the exoplanets orbiting these stars depends mostly on our basic knowledge of the host star, that is their bolometric luminosity, effective temperature, radius and age. The present thesis aim to identify and characterize low-mass stars. Toward that end, a statistical method has been developed to determine quantitatively the membership probability of a star to a young kinematic group. This method combines the Bayesian inference and empirical models of several observables such as the brightness, Galactic space velocity and position of bona fide members of 7 young stars groups (8-120 Mans), as well as old field stars. Stars with a membership probability greater than 90% are considered candidate members. The analysis also predicts the radial velocity and distance that a star would have if it was an actual member. For the 177 previously-known members, an excellent agreement was found between the predicted and observed parameters (1.9 km/s and 10% for the radial velocity and parallax, respectively). Measuring these observables for the candidates stars is thus a good way to confirm their membership. This robust method was applied to a sample of 758 stars which showed signs of youth (H$\alpha$ and X-ray emission). It allowed to identify 214 highly probable candidates. The spectroscopic follow-up yields a radial velocity in agreement with predictions for 130 stars. These spectroscopic observations also allowed to measure their projected rotational velocity, which turned out to be higher than that of the old population of stars. Trigonometric distance measurements were also obtained and were coherent with predictions for 18 young candidates. Using the confirmed members, a new empirical model of the X-ray luminosity was developed. The X-ray luminosity was found to be about 4 times higher for stars around ~8-12Myr than for older, ~120Myr stars, thus, this observable is a good age indicator in this range. Comparing the spectra of 59 young candidate members to atmosphere models allowed to determine three basic parameters: the bolometric luminosity, the effective temperature and the radius. Overall, these candidates are more luminous and have a greater radius than old stars. Recent evolutionary models that include the rotational dynamo-type treatment and produce magnetic field strength of 1 to 2.5 kGauss were used to derive an isochronal age for each star. The ages determined for \beta Pictoris moving group members using stars of different spectral types are coherent with one another (types K5V-M0V: 24 Mans, types M1V-M4V: 14 Mans) and are also coherent with age determined independently using lithium abundance of the low-mass members (26 Mans).

Les naines brunes sont des astres incapables de déclencher et soutenir des réactions nucléaires dans leur cœur. En l’absence de cette source d’énergie, leur luminosité diminue avec le temps jusqu’à leur extinction complète. Leur flux aux longueurs d’onde de 0,8 à 2,35 μm est particulièrement altéré par l’humidité contenue dans l’atmosphère terrestre, ce qui complique l’étude de ces astres. Le but de la présente recherche est de vérifier si la division par un spectre d’étoile A0 est un moyen de corriger l’altération causée par l’atmosphère terrestre sur cette partie de leur spectre. Tout d’abord, des notions, pertinentes à la compréhension de ce travail, sont abordées. L’introduction présente quelques notions sur les naines brunes et sur l’atmosphère terrestre. Le deuxième chapitre concerne le traitement des données. Il traite de la calibration, de la mise en évidence du problème de non-répétabilité de la position de la fente du spectromètre SIMON ainsi que de ses causes. Il porte aussi sur l’uniformisation de la réponse des pixels et de la soustraction du ciel pour extraire les spectres. La méthode employée pour étudier l’effet de l’atmosphère terrestre sur les spectres de naines brunes y est présentée. Le troisième chapitre analyse les résultats obtenus par l’utilisation de l’étoile de référence de type A0 comme calibration pour corriger le spectre de naine brune, en assumant un même effet de l’atmosphère terrestre sur les deux types d’astres. Nous ne pouvons conclure, avec certitude, que l’absorption tellurique affecte de la même façon les deux spectres ni de quelle façon exactement ils sont affectés. Une recherche supplémentaire nécessitant de nouvelles prises de données à des masses d’air et à des taux d’humidité variés est requise. / Brown dwarfs are celestial bodies unable to sustain nuclear reactions. For this reason their luminosity declines until complete extinction. Their flux, particularly in the band between 0,8 and 2,35 μm, is absorbed by the water vapor in the terrestrial atmosphere. The goal of this research is to find a way to correct this part of their spectra affected by this effect. First, general notions needed to understand the project are exposed. The second chapter concerns the data reduction. The calibration, the problem of the position repeatability of the slit of the spectrometer SIMON and his cause are exposed. It discusses techniques to even up the pixels’ response and the substraction of the sky from the spectra. The method used to study the atmosphere effect on brown dwarf spectra is presented. The third chapter analyses the results that use the A0 reference star to correct the brown dwarf spectrum. We cannot conclude that the A0 spectrum is affected in the same way as the brown dwarf spectrum by the terrestrial atmosphere. The data from a single night do not allow a good analysis of this effect as a function of air mass and humidity level. Others missions are needed.

I present the development of two near infrared proper motion pipelines for high resolution near infrared data from UKIDSS and the VISTA VVV survey. The UKIDSS pipeline is capable of accuracies of order 5-10 mas yr⁻¹ for bright sources with the largest epoch baselines (~ 8 years). The VVV pipeline reaches 1-2 mas yr⁻¹ proper motion precision at the bright end and parallax measurements at ~ 1 mas precision. It will be possible to improve upon the VVV astrometric precision due to increases in data volume and further pipeline development. I have used the proper motion pipelines to generate three near infrared proper motion catalogues of the UKIDSS LAS and GPS and the VVV survey. The LAS proper motion catalogue covers 1500 deg2 at high Galactic latitudes and contains approximately 15 million sources with two J band epochs. The GPS proper motion catalogue covers 1500 deg2 of the northern Galactic plane and contains approximately 400 million sources with two K band epochs. The VVV proper motion catalogue covers 560 deg2 of the Galactic bulge and disc and contains approximately 200 million sources with between 50 and 150 Ks band epochs. I have also produced a preliminary 5σ parallax catalogue containing 3403 VVV sources. The LAS and GPS proper motion catalogues have been used by myself and other authors to identify and study many new examples of high proper motion stars, brown dwarfs, ul-tracool dwarf benchmark candidates, cool white dwarfs, substellar subdwarfs and nearby sources within < 25 pc. These catalogues remain far from fully exploited and will be a useful resource for future research by the astronomical community. Exploitation of the VVV proper motion catalogue is still in its infancy, yet it has already generated large numbers of new high proper motion sources. These include new brown dwarf candi-dates, important benchmark objects, and nearby sources which have previously avoided detection. Parallax results from the VVV pipeline will be useful to improve low mass star/ultracool dwarf luminosity functions, significantly increasing the numbers of brown dwarfs with known parallaxes and illustrates how general purpose multi-epoch wide area surveys can generate parallaxes. Finally, I discuss the long term usefulness of such catalogues in the Gaia era and how they might be exploited in the future.

M dwarfs constitute around 70% of all stars in the local Galaxy. Their multitude together with their long main-sequence lifetimes make them important for studies of global properties of the Galaxy such as the initial mass function or the structure and kinematics of stellar populations. In addition, the exoplanet community is showing an increasing interest for those small, cold stars. However, very few M dwarfs are well characterized, and in the case of exoplanetary systems the stellar parameters have a direct influence on the derived planet properties. Stellar parameters of M dwarfs are difficult to determine because of their low surface temperatures that result in an optical spectrum dominated by molecular lines. Most previous works have therefore relied on empirical calibrations. High-resolution spectrographs operating in the infrared, a wavelength region less affected by molecular lines, have recently opened up a new window for the investigation of M dwarfs. In the two first papers of this thesis we have shown that we can determine the metallicity, and in some cases the effective temperature, using synthetic spectral fitting with improved accuracy. This method is time consuming and therefore not practical or even feasible for studies of large samples of M dwarfs. When comparing our results from the high-resolution studies with available photometric calibrations we find systematic differences. In the third paper we therefore used our sample to determine a new photometric metallicity calibration. Compared to previous calibrations our new photometric calibration shows improved statistical characteristics, and our calibration gives similar results as spectroscopic calibrations. In a comparison with theoretical calculations we find a good agreement of the shapes and slopes of iso-metallicity lines with our empirical relation. Applying the photometric calibration to a sample of M dwarfs with confirmed exoplanets we find a possible giant planet-metallicity correlation for M dwarfs.