Influence des fractions hydrophobique et hydrophilique de la matière organique dissoute sur la sorption de Cd, Cu et Pb dans l'horizon B de Podzol

Mémoire numérisé par la Direction des bibliothèques de l'Université de Montréal

Near Infrared Observations of GQ Lup b Using the Gemini Integral Field Spectrograph NIFS

We present new JHK spectroscopy (R ~ 5000) of GQ Lup b, acquired with the near-infrared integral field spectrograph NIFS and the adaptive optics system ALTAIR at the Gemini North telescope. Angular differential imaging was used in the J and H bands to suppress the speckle noise from GQ Lup A; we show that this approach can provide improvements in signal-to-noise ratio (S/N) by a factor of 2 - 6 for companions located at subarcsecond separations. Based on high quality observations and GAIA synthetic spectra, we estimate the companion effective temperature to Teff = 2400 +/- 100 K, its gravity to log g = 4.0 +/- 0.5, and its luminosity to log(L/L_s) = -2.47 +/- 0.28. Comparisons with the predictions of the DUSTY evolutionary tracks allow us to constrain the mass of GQ Lup b to 8 - 60 MJup, most likely in the brown dwarf regime. Compared with the spectra published by Seifahrt and collaborators, our spectra of GQ Lup b are significantly redder (by 15 - 50%) and do not show important Pa\beta emission. Our spectra are in excellent agreement with the lower S/N spectra previously published by McElwain and collaborators.Comment: 34 pages, 10 figures, accepted for publication in Ap

Utilisation de facteurs motogéniques afin d'améliorer le succès de la thérapie cellulaire pour le traitement de la dystrophie musculaire de Duchenne

À cause de l’absence de dystrophine, les fibres musculaires d’un enfant atteint de la Dystrophie Musculaire de Duchenne (DMD) sont fragiles et leurs ruptures fréquentes entraînent une dégénérescence progressive du tissu musculaire. Basée sur les mécanismes de la régénérescence musculaire, la transplantation de myoblastes consiste à fournir des précurseurs myogéniques sains afin que ces derniers participent à la réparation du tissu musculaire dystrophique. Bien que cette approche ait permis de restaurer l’expression de dystrophine lors d’études cliniques menées auprès de patients DMD, la faible dispersion des fibres exprimant la dystrophine s’est révélée un problème majeur requérant que des injections de myoblastes soient effectuées à tous les millimètres afin d’obtenir un succès de greffe optimal. Une faible migration des cellules greffées à l’extérieur des sites d’injection étant suspectée comme principale cause de la restriction des fibres hybrides au niveau des sites d’injections, l’objectif de nos travaux fut d’établir que l’IGF-1, le bFGF et l’interleukine-4 présentent des propriétés chémokinésiques et que leur co-injection avec les cellules greffées est une approche physiologique et efficace pour favoriser la migration intramusculaire des myoblastes squelettiques humains ou de singe. Bien que la co-injection de facteurs de croissance fût envisagée dans l’espoir que les cellules ayant migré puissent fusionner avec les fibres retrouvées à l’extérieur de la trajectoire d’injection, les résultats de transplantation obtenus chez le primate suggèrent que l’augmentation du potentiel migratoire n’est pas, à elle seule, une approche suffisante pour accroître la quantité et la dispersion des fibres hybrides. Globalement, nos travaux ont permis de mieux comprendre et de redéfinir les facteurs limitant le succès de la transplantation de myoblastes. Bien que les cellules myogéniques aient effectivement un potentiel migratoire limité, l’absence de fusion entre les cellules greffées et les fibres non endommagées est sans doute la cause réelle de la restriction des fibres hybrides. Tant que ce problème subsistera, toutes les approches permettant d’améliorer la migration des cellules greffées ne pourront se révéler efficaces pour améliorer la dispersion des fibres et pour réduire la quantité d’injections requises pour le traitement d’un patient dystrophique.Due to the absence of dystrophin, muscle fibers of Duchenne Muscular Dystrophy (DMD) patients are fragile and their constant ruptures induce a progressive lost of muscular tissues. Myoblast transplantation (MT) is an experimental treatment for DMD. Following their intramuscular injection, healthy myogenic precursor cells are able to fuse with host fibers and restore dystrophin expression. Although MT had efficiently restore dystrophin expression in DMD patients; transplantation success following a single injection is limited. The low dispersion of dystrophin expressing fibers is a major problem that requires myoblast injections every millimetre to obtain an optimal graft success. Since poor transplanted cell migration outside the injection sites has been proposed to explain the restriction of hybrid myofibers, motogenic factors were tested to verify whether their co-injection with transplanted myoblasts is a physiological and effective approach to stimulate proteolytic activity as well as myoblast intramuscular migration. Results demonstrated that insulin growth factor-1, basic fibroblast growth factor and interleukin-4 show strong chemokinetic potential for human skeletal myoblasts and increase the migration distances reached by transplanted cells. By improving cell migration through muscular tissue, we hoped that growth factors co-injection would help transplanted cells to fuse with myofibers located outside the injection sites. However, experiments conducted in monkeys suggest that improvement of transplanted cell migration is not, per se, a sufficient approach to increase the quantity and dispersion of hybrid fibers. Generally, our work helped to clarify and redefine a major problem, which limits graft success. Even if short-term observations suggest that transplanted cells are not always trapped inside the injection sites, myofibers including grafted cell nuclei remain restricted to the injection trajectories one month post transplantation. Lack of fusion with undamaged myofibers located outside the injection sites will probably have to be resolved to improve dispersion of hybrid myofibers and thus reduce the number of injections required for the treatment of DMD patients. As long as this fusion problem remains, all approaches, which increase transplanted cell migration, will not be sufficient to increase MT success

Characterization of Low-mass, Wide-separation Substellar Companions to Stars in Upper Scorpius: Near-infrared Photometry and Spectroscopy

We present new 0.9-2.45 $\mu$m spectroscopy ($R \sim 1000$), and $Y$, $J$, $H$, $K_s$, $L^\prime$ photometry, obtained at Gemini North, of three low-mass brown dwarf companions on wide orbits around young stars of the Upper Scorpius OB association: HIP 78530 B, [PGZ2001] J161031.9-191305 B, and GSC 06214-00210 B. We use these data to assess the companions' spectral type, temperature, surface gravity and mass, as well as the ability of the BT-Settl and Drift-Phoenix atmosphere models to reproduce the spectral features of young substellar objects. For completeness, we also analyze the archival spectroscopy and photometry of the Upper Scorpius planetary mass companion 1RXS J160929.1-210524 b. Based on a comparison with model spectra we find that the companions, in the above order, have effective temperatures of 2700, 2500, 2300 and 1700 K. These temperatures are consistent with our inferred spectral types, respectively M7 $\beta$, M9 $\gamma$, M9 $\gamma$, and L4 $\gamma$. From bolometric luminosities estimated from atmosphere model spectra adjusted to our photometry, and using evolution models at 5-10 Myr, we estimate masses of 21-25, 28-70, 14-17 and 7-12 $M_{\rm Jup}$, respectively. J1610-1913 B appears significantly over-luminous for its inferred temperature, which explains its higher mass estimate. Synthetic spectra based on the BT-Settl and Drift-Phoenix atmosphere models generally offer a good fit to our observed spectra, although our analysis has highlighted a few problems. For example, the best fits in the individual near-infrared bands occur at different model temperatures. Also, temperature estimates based on a comparison of the broadband magnitudes and colors of the companions to synthetic magnitudes from the models are systematically lower than the temperature estimates based on a comparison with synthetic spectra.Comment: 16 pages, 8 figures, published in the Astrophysical Journa

Comprehensive High-resolution Chemical Spectroscopy of Barnard's Star with SPIRou

Determination of fundamental parameters of stars impacts all fields of astrophysics, from galaxy evolution to constraining the internal structure of exoplanets. This paper presents a detailed spectroscopic analysis of Barnard's star that compares an exceptionally high-quality (signal-to-noise ratio of $>$2500 in the $H$ band), high-resolution NIR spectrum taken with CFHT/SPIRou to PHOENIX-ACES stellar atmosphere models. The observed spectrum shows thousands of lines not identified in the models with a similar large number of lines present in the model but not in the observed data. We also identify several other caveats such as continuum mismatch, unresolved contamination and spectral lines significantly shifted from their expected wavelengths, all of these can be a source of bias for abundance determination. Out of $>10^4$ observed lines in the NIR that could be used for chemical spectroscopy, we identify a short list of a few hundred lines that are reliable. We present a novel method for determining the effective temperature and overall metallicity of slowly-rotating M dwarfs that uses several groups of lines as opposed to bulk spectral fitting methods. With this method, we infer $T_{\rm eff}$ = 3231 $\pm$ 21 K for Barnard's star, consistent with the value of 3238 $\pm$ 11 K inferred from the interferometric method. We also provide abundance measurements of 15 different elements for Barnard's star, including the abundances of four elements (K, O, Y, Th) never reported before for this star. This work emphasizes the need to improve current atmosphere models to fully exploit the NIR domain for chemical spectroscopy analysis.Comment: 24 pages, 18 figures, submitted to Ap

CO or no CO? Narrowing the CO abundance constraint and recovering the H2O detection in the atmosphere of WASP-127 b using SPIRou

Precise measurements of chemical abundances in planetary atmospheres are necessary to constrain the formation histories of exoplanets. A recent study of WASP-127b, a close-in puffy sub-Saturn orbiting its solar-type host star in 4.2 d, using HST and Spitzer revealed a feature-rich transmission spectrum with strong excess absorption at 4.5 um. However, the limited spectral resolution and coverage of these instruments could not distinguish between CO and/or CO2 absorption causing this signal, with both low and high C/O ratio scenarios being possible. Here we present near-infrared (0.9--2.5 um) transit observations of WASP-127 b using the high-resolution SPIRou spectrograph, with the goal to disentangle CO from CO2 through the 2.3 um CO band. With SPIRou, we detect H2O at a t-test significance of 5.3 sigma and observe a tentative (3 sigma) signal consistent with OH absorption. From a joint SPIRou + HST + Spitzer retrieval analysis, we rule out a CO-rich scenario by placing an upper limit on the CO abundance of log10[CO]<-4.0, and estimate a log10[CO2] of -3.7^(+0.8)_(-0.6), which is the level needed to match the excess absorption seen at 4.5um. We also set abundance constraints on other major C-, O-, and N-bearing molecules, with our results favoring low C/O (0.10^(+0.10)_(-0.06)), disequilibrium chemistry scenarios. We further discuss the implications of our results in the context of planet formation. Additional observations at high and low-resolution will be needed to confirm these results and better our understanding of this unusual world.Comment: 23 pages, 13 figures, Submitted for publication in the Monthly Notice of the Royal Astronomical Societ

New Mass and Radius Constraints on the LHS 1140 Planets -- LHS 1140 b is Either a Temperate Mini-Neptune or a Water World

The two-planet transiting system LHS 1140 has been extensively observed since its discovery in 2017, notably with $Spitzer$, HST, TESS, and ESPRESSO, placing strong constraints on the parameters of the M4.5 host star and its small temperate exoplanets, LHS 1140 b and c. Here, we reanalyse the ESPRESSO observations of LHS 1140 with the novel line-by-line framework designed to fully exploit the radial velocity content of a stellar spectrum while being resilient to outlier measurements. The improved radial velocities, combined with updated stellar parameters, consolidate our knowledge on the mass of LHS 1140 b (5.60$\pm$0.19 M$_{\oplus}$) and LHS 1140 c (1.91$\pm$0.06 M$_{\oplus}$) with unprecedented precision of 3%. Transits from $Spitzer$, HST, and TESS are jointly analysed for the first time, allowing us to refine the planetary radii of b (1.730$\pm$0.025 R$_{\oplus}$) and c (1.272$\pm$0.026 R$_{\oplus}$). Stellar abundance measurements of refractory elements (Fe, Mg and Si) obtained with NIRPS are used to constrain the internal structure of LHS 1140 b. This planet is unlikely to be a rocky super-Earth as previously reported, but rather a mini-Neptune with a $\sim$0.1% H/He envelope by mass or a water world with a water-mass fraction between 9 and 19% depending on the atmospheric composition and relative abundance of Fe and Mg. While the mini-Neptune case would not be habitable, a water-abundant LHS 1140 b potentially has habitable surface conditions according to 3D global climate models, suggesting liquid water at the substellar point for atmospheres with relatively low CO$_2$ concentration, from Earth-like to a few bars.Comment: 31 pages, 18 figures, accepted for publication in ApJ

Osteocrin is a specific ligand of the natriuretic peptide clearance receptor that modulates bone growth

Osteocrin (Ostn) is a recently discovered secreted protein produced by cells of the osteoblast lineage that shows a well conserved homology with members of the natriuretic peptide (NP) family. We hypothesized that Ostn could interact with the NP receptors, thereby modulating NP actions on the skeleton. Ostn binds specifically and saturably to the NP peptide receptor-C (NPR-C) receptor with a K-d of similar to 5 nM with no binding to the GC-A or GC-B receptors. Deletion of several of the residues deemed important for NP binding to NPR-C led to abolition of Ostn binding, confirming the presence of a "natriuretic motif." Functionally, Ostn was able to augment C-type natriuretic peptide-stimulated cGMP production in both pre-chondrocytic (ATDC5) and osteoblastic (UMR106) cells, suggesting increased NP levels due to attenuation of NPR-C associated NP clearance. Ostn-transgenic mice displayed elongated bones and a marked kyphosis associated with elevated bone cGMP levels, suggesting that elevated natriuretic peptide activity contributed to the increased bone length possibly through an increase in growth plate chondrocyte proliferation. Thus, we have demonstrated that Ostn is a naturally occurring ligand of the NPR-C clearance receptor and may act to locally modulate the actions of the natriuretic system in bone by blocking the clearance action of NPR-C, thus locally elevating levels of C-type natriuretic peptide