Academic literature on the topic 'Red clump'
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Journal articles on the topic "Red clump"
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Girardi, Léo. "Red Clump Stars." Annual Review of Astronomy and Astrophysics 54, no. 1 (September 19, 2016): 95–133. http://dx.doi.org/10.1146/annurev-astro-081915-023354.
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Kamiński, T. "Massive dust clumps in the envelope of the red supergiant VY Canis Majoris." Astronomy & Astrophysics 627 (July 2019): A114. http://dx.doi.org/10.1051/0004-6361/201935408.
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The envelope of the red supergiant VY CMa has long been considered an extreme example of episodic mass loss that is possibly taking place in other cool and massive evolved stars. Recent (sub-)millimeter observations of the envelope revealed the presence of massive dusty clumps within 800 mas of the star and reinforce the picture of drastic mass-loss phenomena in VY CMa. We present new ALMA observations at an angular resolution of 0.1″ and at an unprecedented sensitivity that reveal further details about the dusty clumps. We resolve more discrete features and identify a submillimeter counterpart of a more distant Southwest (SW) Clump known from visual observations. The brightest clump, named C, is marginally resolved in the observations. Gas seen against the resolved continuum emission of clump C produces a molecular spectrum in absorption, in lines of mainly sulfur-bearing species. Except for SW Clump, no molecular emission is found to be associated with the dusty clumps and we propose that the dusty structures have an atypically low gas content. We attempt to reproduce the properties of the dusty clumps through 3D radiative transfer modeling. Although a clump configuration explaining the observations is found, it is not unique. A very high optical depth of all clumps to the stellar radiation makes the modeling very challenging, and requires an unrealistically high dust mass for one of the clumps. We suggest that the dusty features have substructures (e.g., porosity) that allow deeper penetration of stellar photons within the clumps than in a homogeneous configuration. A comparison of the estimated clump ages to variations in the stellar visual flux for over a century suggests that the mechanism responsible for their formation is not uniquely manifested by enhanced or strongly diminished visual light. The study demonstrates that the dusty mass-loss episodes of VY CMa are indeed unparalleled among all known non-explosive stars. The origin of these episodes remains an unsolved problem.
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Lucey, Madeline, Yuan-Sen Ting, Nesar S. Ramachandra, and Keith Hawkins. "From the inner to outer Milky Way: a photometric sample of 2.6 million red clump stars." Monthly Notices of the Royal Astronomical Society 495, no. 3 (January 2020): 3087–103. http://dx.doi.org/10.1093/mnras/staa1226.
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ABSTRACT Large pristine samples of red clump stars are highly sought after given that they are standard candles and give precise distances even at large distances. However, it is difficult to cleanly select red clumps stars because they can have the same Teff and log g as red giant branch stars. Recently, it was shown that the asteroseismic parameters, $\rm {\Delta }$P and $\rm {\Delta \nu }$, which are used to accurately select red clump stars, can be derived from spectra using the change in the surface carbon to nitrogen ratio ([C/N]) caused by mixing during the red giant branch. This change in [C/N] can also impact the spectral energy distribution. In this study, we predict the $\rm {\Delta }$P, $\rm {\Delta \nu }$, Teff, and log g using 2MASS, AllWISE, Gaia, and Pan-STARRS data in order to select a clean sample of red clump stars. We achieve a contamination rate of ∼20 per cent, equivalent to what is achieved when selecting from Teff and log g derived from low-resolution spectra. Finally, we present two red clump samples. One sample has a contamination rate of ∼20 per cent and ∼405 000 red clump stars. The other has a contamination of ∼33 per cent and ∼2.6 million red clump stars that includes ∼75 000 stars at distances >10 kpc. For |b| > 30 deg, we find ∼15 000 stars with contamination rate of ∼9 per cent. The scientific potential of this catalogue for studying the structure and formation history of the Galaxy is vast, given that it includes millions of precise distances to stars in the inner bulge and distant halo where astrometric distances are imprecise.
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López-Corredoira, M., Y. W. Lee, F. Garzón, and D. Lim. "Distribution of red clump stars does not support the X-shaped Galactic bulge." Astronomy & Astrophysics 627 (June 25, 2019): A3. http://dx.doi.org/10.1051/0004-6361/201935571.
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Context. Claims of an X-shaped Galactic bulge were based on the assumption of red clump stars as standard candles in some lines of sight crossing the off-plane bulge. However, some doubts have been cast on whether the two peaks in star counts along the line of sight really represent a double peak in the density distribution, or whether there is something wrong with the assumption of a unique constant absolute magnitude for all of these stars. Aims. With the advent of Gaia-DR2 parallaxes in combination with near-infrared VISTA-VVV data, we are able to check which of the hypotheses is correct. Methods. We calculated the median absolute magnitude MK corresponding to both peaks of putative red clumps in seven lines of sight with the lowest extinction in the interesting coordinates’ range. Results. The difference between the absolute magnitude of the bright and the faint peak is ΔMK ≈ 0.4. The selected stars in both peaks cannot be represented by the same red clump giants with constant MK ≈ −1.6. Conclusions. The hypothesis that the bulge contains an X-shape is based on the assumption that the faint and bright peaks of the density distribution towards the bulge are dominated by standard red clump stars. However, we show that both the faint and bright peaks cannot be dominated by standard red clump stars simultaneously.
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Ruiz-Dern, L., C. Babusiaux, F. Arenou, and C. Turon. "Characterisation of the Gaia Red Clump." EAS Publications Series 67-68 (2014): 395–96. http://dx.doi.org/10.1051/eas/1567084.
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Buldgen, Gaël, B. Rendle, T. Sonoi, G. R. Davies, A. Miglio, S. J. A. J. Salmon, D. R. Reese, et al. "Mean density inversions for red giants and red clump stars." Monthly Notices of the Royal Astronomical Society 482, no. 2 (August 27, 2018): 2305–19. http://dx.doi.org/10.1093/mnras/sty2346.
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Karaali, S., S. Bilir, and E. Yaz Gökçe. "Absolute magnitude calibration for red clump stars." Astrophysics and Space Science 346, no. 1 (April 20, 2013): 89–104. http://dx.doi.org/10.1007/s10509-013-1449-7.
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Garnavich, P. M., and K. Stanek. "Red Clump Stars – Further Improved Distance Indicator." Highlights of Astronomy 12 (2002): 688. http://dx.doi.org/10.1017/s1539299600014672.
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AbstractThe ideal distance indicator would be a standard candle abundant enough to provide many examples within reach of parallax measurements and sufficiently bright to be seen out to Local Group galaxies. The red clump stars closely match this description. These are the metal rich equivalent of the better known horizontal branch stars, and their brightness dispersion is only 0.2 mag (one sigma) in the Solar neighborhood. Using Hipparcos to calibrate a large, local sample, the red clump method has been used to measure accurate distances to the Galactic center (Paczyński & Stanek 1998), M31 (Stanek & Garnavich 1998), LMC (Udalski et al. 1998; Stanek et al. 1998; Udalski 1999) and some clusters in our Galaxy (e.g. 47Tuc: Kaluzny et al. 1998). As with all the distance indicators, the main worry lies in the possible systematics of the method, in particular, the brightness dependence on the stellar metallicity and age. These dependences have come under close scrutiny and, indeed, the population effects on the red clump brightness appear small and calibratable. Perhaps the most controversial result from the red clump method is the estimation of a “short” distance to the Large Magellanic Cloud (Udalski et al. 1998; Stanek, Zaritsky & Harris 1998; Udalski 2000). This distance to the LMC is shorter by 12% than the “standard” value, and has very important implications for the Cepheid distance scale and the determination of the Hubble constant.
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Abedigamba, O. P., L. A. Balona, and T. R. Medupe. "Red Clump stars inKepleropen cluster NGC 6819." EPJ Web of Conferences 101 (2015): 06001. http://dx.doi.org/10.1051/epjconf/201510106001.
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Liu, Y. J., G. Zhao, J. R. Shi, G. Pietrzyński, and W. Gieren. "The abundances of nearby red clump giants*." Monthly Notices of the Royal Astronomical Society 382, no. 2 (November 7, 2007): 553–66. http://dx.doi.org/10.1111/j.1365-2966.2007.11852.x.
Full textDissertations / Theses on the topic "Red clump"
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Ruiz-Dern, Laura. "Gaia : de la validation des données aux paramètres du Red Clump." Thesis, Paris Sciences et Lettres (ComUE), 2016. http://www.theses.fr/2016PSLEO014/document.
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La mission Gaia de l'Agence Spatiale Européenne (ESA) a pour objectif de cartographier notre galaxie avec une précision astrométrique jamais atteinte auparavant. Il est donc particulièrement important que les données qui seront publiées soient rigoureusement validées afin d'assurer une qualité optimum au Catalogue. Ces validations sont faites par l'une des équipes de l'unité de coordination CU9 du Consortium Gaia DPAC (Data Processing and Analys Consortium) chargé par l'ESA de la production du Catalogue Gaia. Dans le cadre de cette thèse, nous avons mis en place toute l’infrastructure nécessaire à la validation du catalogue Gaia par comparaison avec des catalogues externes. Celle-ci gère toutes les interactions avec l'environnement global des validations et avec la base de données Gaia. Ensuite nous avons développé un ensemble de tests statistiques pour valider les données du premier catalogue Gaia (DR1). Ces tests concernent notamment l’homogénéité des données sur le ciel, la qualité des positions et de la photométrie de l'ensemble des étoiles de DR1 (plus d'un milliard d'étoiles, $V<20$) ainsi que celle des parallaxes et mouvements propres des étoiles de textit{Tycho-Gaia} Astrometric Solution (TGAS), environ deux millions d'étoiles communes aux catalogues Gaia et Tycho-2 ($V<12$). Ces tests statistiques sur la DR1 sont opérationnels et ont déjà été appliqués très récemment sur des données préliminaires. Cela a déjà permis d'améliorer ces données (donc la qualité du catalogue), et d'en caractériser les propriétés statistiques. Cette caractérisation est essentielle à une exploitation scientifique correcte des données. Le premier catalogue Gaia sera publié à la fin de l’été 2016. Parmi les objets observés par Gaia, il y a une population d'étoiles particulièrement intéressantes, les étoiles du Red Clump (RC), très utilisées comme étalons de distance. Nous avons développé et testé deux méthodes pour modéliser les relations couleur-couleur (CC) et température effective - couleur dans toutes les bandes photométriques, de l'ultraviolet au proche-infrarouge. Elles permettront de caractériser le RC dans la bande G de Gaia dès la publication du catalogue: 1. en utilisant des modèles théoriques, et 2. empiriquement, en se basant sur une méthode Monte Carlo Markov Chain (MCMC). Pour cela nous avons très rigoureusement sélectionné des échantillons d'étoiles avec une bonne qualité photométrique, une bonne métallicité, déterminée par spectroscopie, une température effective homogène et une faible extinction interstellaire. À partir de ces calibrations CC et température-couleur, nous avons ensuite développé une méthode par Maximum de Vraisemblance qui permet de déterminer les magnitudes absolues, les températures et les extinctions des étoiles du RC. Les couleurs et extinctions ainsi obtenues ont été testées sur des étoiles avec des températures effectives mesurées spectroscopiquement et une extinction déterminée par la mesure des Bandes Diffuses Interstellaires (DIB). Ces propriétés intrinsèques des étoiles du RC vont permettre de caractériser le Red Clump Gaia et de calibrer, dans la bande Gaia, la magnitude absolue de cet étalon de distance, premier échelon essentiel de la détermination des distances dans l'UniversThe Gaia mission of the European Space Agency (ESA) aims to map our galaxy with an unprecedented astrometric precision. It is therefore very important that the data that will be published be rigorously validated to ensure an optimal quality in the Catalogue. These validations are done by one of the teams of the coordination unit CU9 of the Gaia DPAC Consortium (Data Processing and Analysis Consortium) commissioned by ESA of the Gaia catalogue production. As part of this thesis, we implemented all the necessary infrastructure to validate the Gaia catalogue by comparison with external catalogues. This last manages all the interactions with the global environment of validations and with the Gaia database. Then we developed a set of statistical tests to validate the data from the first Gaia catalogue (DR1). These tests relate in particular to the homogeneity of data on the sky, the quality of the positions and of photometry of all the stars of DR1 (more than a billion stars, $V <20$) as well as that of the parallaxes and proper motions for textit{Tycho-Gaia} Astrometric Solution (TGAS) stars, around two million stars in common in Gaia and Tycho-2 catalogues ($V <12$).These DR1 statistical tests are operational and were already applied very recently on preliminary data. This has improved the data (thus the quality of the catalog) as well as allowed to characterize the statistical properties. This characterisation is essential for a correct scientific exploitation of the data. The first Gaia catalogue will be released in late summer 2016.Among the objects that Gaia observes, there is a population of stars particularly interesting, the Red Clump (RC) stars, widely used for distance indicators. We developed and tested two methods to model the colour-colour (CC) and effective temperature - colour relations in all photometric bands, from the ultraviolet to the near infrared. They will allow us to characterize the RC in the Gaia G band upon publication of the catalogue: 1. using theoretical models, and 2. empirically, based on a Monte Carlo Markov Chain (MCMC) method. For this we have very carefully selected samples of stars with a good photometric quality, good metallicity determined by spectroscopy, an homogeneous effective temperature and a low interstellar extinction.From these CC and temperature-colour calibrations, we then developed a Maximum Likelihood method that allows to derive absolute magnitudes, temperatures and extinctions of the RC stars. Estimates of colours and extinctions are tested on stars with spectroscopically measured effective temperatures and an extinction determined by the measurement of Diffuse Interstellar Bands (DIB). These intrinsic properties of RC stars will allow to characterize the Gaia RC and calibrate, within the Gaia G band, the absolute magnitude of this standard candle, first essential step of determining distances in the Univers
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Peter, Camaren. "The red clump stars as a distance indicator : review and application." Master's thesis, University of Cape Town, 2002. http://hdl.handle.net/11427/7411.
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Bibliography: leaves 76-81.The intention of this project was primarily to determine the distance to the Galactic Centre using a new technique pioneered by Paczynski and Stanek (1998) that uses the red clump stars as a standard candle. This was made possible by the large number of stars simultaneously observed by the OGLE microlensing project which yields well-defined red clump structures in their colour magnitude diagrams. We have used data obtained at Sutherland in July 1997, in collaboration with the PLANET microlensing project. It was hoped that the observation of a number of lensing events occurring in fields in the Galactic Bulge region would reveal information about the Galactic structure in that region and perhaps yield information about the lens masses. The red clump technique is reviewed and applied to several 3x 3 arcminfields observed at low galactic latitude and longitude in the Galactic Bulge. The derived distances to the fields show consistency with the E2 bar model proposed by Stanek, and indicate that the distance from our sun to the Galactic Centre is 7.97± 0.4 kpc. Furthermore, an attempt is made to apply the derived individual distance to each field to calculate the possible lens mass associated with each event.
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Percival, Susan M. "Calibration of the Red Clump distance scale and its application to the LMC." Thesis, Liverpool John Moores University, 2003. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.400586.
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Tatton, Benjamin. "The structure of the Magellanic Clouds traced by red clump stars at near-infrared wavelengths." Thesis, Keele University, 2018. http://eprints.keele.ac.uk/5587/.
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This thesis is about the Red Clump (RC) star population within the Magellanic Clouds. These are observed in the near-infrared Y JKs wavelengths using data obtained by the ESO public VMC survey. These were studied to shed more light on the internal structure and past and current evolution of this interacting system of dwarf irregular galaxies. RC stars were selected from the colour magnitude diagram (CMD) using a contour method to assign the selection box and reddening vector. The J − Ks vs Ks CMD of the central 30 Doradus region of the Large Magellanic Cloud (LMC) region was analysed to determine the extinction content there, producing a reddening map. This was compared with other works including an optical reddening map which also used RC stars. The reddening map also proved to be a useful tool as a tracer of ISM features including the identification of molecular clouds. The extinction maps were made in the Y − Ks colours for the whole LMC and whole SMC. These were then used to deredden the populations. These populations had their distribution examined in a number of ways including line of sight depth and residuals derived from least-squares plane fitting. The distorted structures found appear to be the product of interactions between the LMC and SMC. RC content was also studied in the Magellanic Bridge region (lying between the LMC and SMC) where a RC population was found throughout the Bridge, mainly at LMC distance and mostly towards the LMC and SMC showing evidence of a tidally stripped SMC population. Maps were created showing this. This thesis thus presents an unprecedented, global view of the stellar and interstellar structure of the interacting Magellanic Cloud, using an intermediate-age stellar tracer, piercing through and using dust.
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Ekanayake, Gemunu. "Determination of Stellar Parameters through the Use of All Available Flux Data and Model Spectral Energy Distributions." UKnowledge, 2017. http://uknowledge.uky.edu/physastron_etds/44.
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Basic stellar atmospheric parameters, such as effective temperature, surface gravity, and metallicity plays a vital role in the characterization of various stellar populations in the Milky Way. The Stellar parameters can be measured by adopting one or more observational techniques, such as spectroscopy, photometry, interferometry, etc. Finding new and innovative ways to combine these observational data to derive reliable stellar parameters and to use them to characterize some of the stellar populations in our galaxy is the main goal of this thesis.
Our initial work, based on the spectroscopic and photometric data available in literature, had the objective of calibrating the stellar parameters from a range of available flux observations from far-UV to far-IR. Much effort has been made to estimate probability distributions of the stellar parameters using Bayesian inference, rather than point estimates.
We applied these techniques to blue straggler stars (BSSs) in the galactic field, which are thought to be a product of mass transfer mechanism associated with binary stars. Using photometry available in SDSS and GALEX surveys we identified 85 stars with UV excess in their spectral energy distribution (SED) : indication of a hot white dwarf companion to BSS. To determine the parameter distributions (mass, temperature and age) of the WD companions, we developed algorithms that could fit binary model atmospheres to the observed SED. The WD mass distribution peaks at 0.4M , suggests the primary formation channel of field BSSs is Case-B mass transfer, i.e. when the donor star is in red giant phase of its evolution. Based on stellar evolutionary models, we estimate the lower limit of binary mass transfer efficiency β ~ 0.5.
Next, we have focused on the Canis Major overdensity (CMO), a substructure located at low galactic latitude in the Milky Way, where the interstellar reddening (E(B-V )) due to dust is significantly high. In this study we estimated the reddening, metallicity distribution and kinematics of the CMO using a sample of red clump (RC) stars. The averageE(B-V)(~0.19)is consistent with that measured from Schlegel maps (Schlegal et.al. 1998). The overall metallicity and kinematic distribution is in agreement with the previous estimates of the disk stars. But the measured mean alpha element abundance is relatively larger with respect to the expected value for disk stars.
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Dyrda, Agnieszka. "Dynamical behavior of the human red blood cell ionic channels." Rennes 1, 2009. http://www.theses.fr/2009REN1S139.
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Erythrocytes are one of the cellular models frequently used to decipher the physiology of membrane transport. However, if pumps, antiporters and cotransporters are now well defined, the molecular identity and the physiological role of the conductive pathways present in the membrane of red blood cell (RBC) is still elusive albeit the growing evidences of their role in physiological and pathological conditions. The present work, using the patch clamp technique and biophysical studies, shows that: 1) The changes in osmotic fragility observed after Gardos channel dependent dehydration is mainly not due to rehydration of the cell via membrane transporters but rather due to change in membrane properties elicited by the Ca2+ loading. It reflects a specific calcium-induced lytic vulnerability of the membrane leading to rupture before the cells attain their maximal spherical volumes. 2) The Gardos channel can be transiently activated when seal formation induces membrane deformation. This phenomenon can result only from activation of a permeability pathway with a finite Ca2+ conductance. This transient activity generates secondary transient anionic channel activity that has been studied further. 3) The diversity of anionic channel activities recorded in normal human RBCs, as well as in P. Falciparum-infected RBCs, corresponds to different kinetic modalities of a unique type of maxi anion channel with multiple conductance levels, gating properties and pharmacology. Finally, the present work contributes to the understanding of the role of ion channels in RBCs and opens questions on the contribution of ion channels in the rheological properties of RBCs. Keywords: erythrocyte, ionic channels, osmotic fragility, patch clamp techniqueLes érythrocytes sont un des modèles pour l’étude des voies de transport membranaire. Si les pompes, les antiports et les cotransports sont bien définis, l’identité moléculaire et le rôle physiologique des voies de conductances du globule rouge restent méconnus. Le présent travail réalisé à l’aide des techniques de patch-clamp montre que : 1) Les changements de fragilité osmotique observés lors d’une déhydratation des cellules après stimulation du canal Gardos, ne sont pas dus à une réhydration des cellules via l’activation de transporteurs, mais à des changements de propriétés de la membrane liées à l’augmentation du [Ca2+]i. Elle reflète une vulnérabilité spécifique de la membrane au Ca2+, induisant la rupture de la membrane avant que la cellule n’ait atteint son volume critique. 2) Le canal Gardos peut-être activé transitoirement lors d’épisode de déformation de la membrane. Ce phénomène ne peut être que le résultat de l’activation d’une voie de perméabilité au Ca2+ ayant une conductance déterminée. 3) L’activité transitoire du canal Gardos active secondairement une voie de conductance anionique. La diversité des canaux anioniques précédemment décrits dans la membrane des érythrocytes humains correspond à l’activité d’un unique canal anionique de type maxi-chlorure ayant des modalités d’activation et de fonctionnement (état d’ouverture multiple, cinétique, pharmacologie…) différentes en fonction des conditions expérimentales. Ce travail contribue à une meilleure compréhension des canaux ioniques présents dans la membrane du globule rouge et permet d’envisager la participation de ces canaux dans la régulation des propriétés rhéologiques des globules rouges. Mots clés: érythrocyte, canaux ioniques, fragilité osmotique, patch clamp
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Morgan, Brittany. "Development of Micro Volume DNA and RNA Profiling Assays to Identify the Donor and Tissue Source of Origin of Trace Forensic Biological Evidence." Master's thesis, University of Central Florida, 2013. http://digital.library.ucf.edu/cdm/ref/collection/ETD/id/6326.
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In forensic casework analysis it is necessary to obtain genetic profiles from increasingly smaller amounts of biological material left behind by perpetrators of crime. The ability to obtain profiles from trace biological evidence is demonstrated with so-called 'touch DNA evidence' which is perceived to be the result of DNA obtained from shed skin cells transferred from donor to an object or person during physical contact. However, the current method of recovery of trace DNA involves cotton swabs or adhesive tape to sample an area of interest. This "blind-swabbing" approach may result in the recovery of biological material from different individuals resulting in admixed DNA profiles which are often difficult to interpret.
Profiles recovered from these samples are reported to be from shed skin cells with no biological basis for that determination. A specialized approach for the isolation of single or few cells from 'touch DNA evidence' is necessary to improve the analysis and interpretation of recovered profiles. Here we describe the development of optimized and robust micro volume PCR reactions (1-5 uL) to improve the sensitivity and efficiency of 'touch DNA' analysis. These methods will permit not only the recovery of the genetic profile of the donor of the biological material, but permit an identification of the tissue source of origin using mRNA profiling.
Results showed that the 3.5 uL amplification volume, a fraction of the standard 25 uL amplification volume, was the most ideal volume for the DNA assay, as it had very minimal evaporation with a 50% profile recovery rate at a single cell equivalent input (~5 pg) with reducing amplification volume alone. Findings for RNA showed that by reducing both amplification steps, reverse transcriptase PCR (20 uL) and body fluid multiplex PCR (25 uL), to 5 uL, ideal results were obtained with an increase in sensitivity and detection of six different body fluids down to 50 pg.
Once optimized at the trace level, the assays were applied to the collection of single and few cells. DNA findings showed that about 40% of a full profile could be recovered from a single buccal cell, with nearly 80% of a full profile recovered from only two cells. RNA findings from collected skin particles of "touched" surfaces showed accurate skin detection down to 25 particles and detection in one clump of particles. The profiles recovered were of high quality and similar results were able to be replicated through subsequent experiments.
More studies are currently underway to optimize these developed assays to increase profile recovery at the single cell level. Methods of doing so include comparing different locations on touched surfaces for highest bio-particle recovery and the development of physical characteristics of bio-particles that would provide the most ideal results.M.S.
Masters
Chemistry
Sciences
Forensic Science; Forensic Biochemistry Track
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Górski, Marek. "Precyzyjne wyznaczenia odległości do wybranych galaktyk Grupy Lokalnej." Doctoral thesis, 2014. https://depotuw.ceon.pl/handle/item/1118.
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Wyznaczenia odległości należą do najważniejszych, a jednocześnie najtrudniejszych pomiarów astronomicznych. Pozwalają określić strukturę Wszechświata, skalę energetyczną zjawisk astrofizycznych oraz wartości stałych fizycznych -- w szczególności stałej Hubble'a.Porównanie wyników pomiaru odległości do szeregu galaktyk Grupy Lokalnej pokazuje, że istnieją duże rozbieżności pomiędzy wynikami uzyskanymi przy pomocy różnych metod. Stosowane metody zdominowane są przez błędy systematyczne, z których największe znaczenie ma wpływ poczerwienienia, efekty populacyjne oraz kalibracja punktu zerowego.W mojej pracy badam wpływ błędów systematycznych na trzy wskaźniki odległości: jasność cefeid, jasność wierzchołka gałęzi czerwonych olbrzymów oraz średnią jasność gwiazd Red Clump. W pierwszej części pracy przedstawiam pomiar odległość do galaktyki M33, dla której rozbieżność wyznaczeń wynosi aż 30%. W oparciu o podczerwoną oraz optyczną fotometrię 26 cefeid uzyskałem odległość 24.62 +/- 0.03 (stat.) +/- 0.06 (syst.) mag. Wartośc ta jest zgodna ze współczesnymi wyznaczeniami opartymi o optyczne pomiary jasności cefeid, jednak jest mniejsza o około 0.2-0.3 mag w stosunku do takich metod jak FGLR lub gwiazdy zaćmieniowe. Dzięki wykorzystaniu pasm optycznych oraz podczerwonych, wyznaczyłem dokładną wartość poczerwienienia (E(B-V) = 0.19 +/- 0.02 mag). Otrzymana odległość jest w niewielkim stopniu zależna od wartości ekstynkcji, prawa poczerwienienia, metaliczności oraz efektów populacyjnych.W dalszej części pracy badam wpływ błędów systematycznych na jasność wierzchołka gałęzi czerwonych olbrzymów (z ang. Tip of the Red Giant Branch, TRGB) w pasmach optycznych oraz podczerwonych. Na podstawie pomiaru jasności TRGB wyznaczyłem odległości do czterech galaktyk Grupy Lokalnej: LMC, SMC, WLM oraz IC 1613. Odległość do Wielkiego Obłoku Magellana wyznaczona przy pomocy jasności TRGB w paśmie K jest większa o 0.2 mag w stosunku do ,,klasycznej odległości'' (18.50 mag). Natomiast w paśmie I jest od niej mniejsza o 0.2 mag. Są to różnice dużo większe niż statystyczna niepewność pomiaru (0.04 mag), co świadczy o istnieniu błędu systematycznego przewidzianego przez syntetyczne modele populacji gwiazdowych. Efekt ten związany jest z obecnością stosunkowo młodych gwiazd na gałęzi czerwonych olbrzymów. Odległości wyznaczone do pozostałych trzech galaktyk potwierdzają istnienie tego efektu populacyjnego.Odległości względne między LMC a poszczególnymi galaktykami mają taka samą wartość w pasmach J, K oraz dla jasności bolometrycznej, są one również zgodne z odległościami względnymi wyznaczonymi przy pomocy innych metod -- podczerwonej jasności cefeid, oraz gwiazd podwójnych. Wyznaczenie odległości oparte o jasność bolometryczną TRGB i kolor gwiazd gałęzi czerwonych olbrzymów prowadzi do wyniku, który jest zgodny z cefeidami oraz gwiazdami podwójnymi i w niewielkim stopniu zależy od opisanych powyżej efektów populacyjnych. W ostatniej części pracy badam wpływ efektów populacyjnych na jasność gwiazd Red Clump. Na podstawie fotometrii Kosmicznego Teleskopu Hubble'a zmierzyłem średnią jasność gwiazd RC w 15 pobliskich galaktykach. Jasność tą porównałem z bolometryczną jasnością wierzchołka gałęzi czerwonych olbrzymów (TRGB) w tych galaktykach, która jest w bardzo małym stopniu zależna od metaliczności i innych efektów populacyjnych. Jasność absolutna gwiazd RC jest różna dla poszczególnych galaktyk i w skrajnym przypadku może być większa o 0.4 mag w stosunku do średniej jasności gwiazd RC w Drodze Mlecznej. Efekt ten jest zgodny z przewidywaniami opartymi o syntetyczne modele populacji gwiazdowych.Distance determinations are one of the most important and difficult measurements in astronomy.They allow us to set the structure of the Universe, energy scale of astrophysical phenomena, and value of the physical constants -- in particular Hubble'a constant. Comparison of measurement results for numerous galaxies shows discrepancy between different methods. Distance determinations are dominated by different systematic errors, of which the most important are reddening, population effects and zero point calibration.In my thesis I investigate the impact of systematic errors on three distance indicators: the brightness of Cepheids, brightness of the Tip of the Red Giant Branch, and the mean magnitude of the Red Clump.In first part of my thesis I present distance measurement to the M33 galaxy, for which the discrepancy of the distance measurements is up to 30 %. Based on infrared and optical photometry of 26 Cepheid I have obtained the distance moduli of 24.62 +/- 0.03 (rand.) +/- 0.06 (syst.) mag. The value is consistent with contemporary designations based on optical measurements of the brightness of Cepheids, but is smaller by about 0.2-0.3 mag in relation to such methods as FGLR or eclipsing binaries. By using optical and infrared bands, I have obtained accurate value of reddening (E(B-V) = 0.19 +/- 0.02 mag). The resulting distance is slightly dependent on the value of the extinction law, reddening, metallicity and population effects.In the following part of the thesis I investigate the impact of systematic errors on the brightness of the Tip of the Red Giant Branch in the optical and infrared bands. On the basis of TRGB brightness I have obtained distance to four Local Group galaxies: LMC, SMC, WLM and IC 1613.The distance to the Large Magellanic Cloud determined in the K-band TRGB brightness is higher by 0.2 mag compared to the "classic distance" (18.50 mag). However, in the I band it is smaller by 0.2 mag. Those differences are much larger than the statistical measurement uncertainty (0.04 mag), which proves the existence of a systematic error predicted by the synthetic stellar population models. This effect is associated with the presence of relatively young stars on the red giant branch.Distances derived for other three galaxies confirm the existence of this population effect. The relative distance between the LMC and the individual galaxies have the same value in the bands J, K and in the bolometric brightness, they are also consistent with the relative distances derived with other methods -- infrared brightness of Cepheid variable stars and eclipsing binaries.Determination of the distance based on the TRGB bolometric luminosity and color of red giant branch leads to a result which is consistent with Cepheides and eclipsing binaries and hardly depends on the population effects described above.In the last part of the thesis I analyze impact of the population effects on the brightness of the Red Clump stars. Based on the photometry of the Hubble Space Telescope I have measured the average brightness of RC stars in the 15 nearby galaxies. I compared mean RC brightness with the bolometric brightness of the tip of the red giant branch (TRGB) in those galaxies, which is a very small dependent on the metallicity and other population effects. RC absolute magnitude of stars is different for different galaxies and in extreme cases can be up to 0.4 mag in comparison to the average RC brightness in the Milky Way. This effect is consistent with expectations based on synthetic stellar population models.
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Chamberlain, S. E., I. M. Gonzàlez-Gonzàlez, K. A. Wilkinson, F. A. Konopacki, Sriharsha Kantamneni, J. M. Henley, and J. R. Mellor. "SUMOylation and phosphorylation of GluK2 regulate kainate receptor trafficking and synaptic plasticity." 2012. http://hdl.handle.net/10454/5911.
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NoPhosphorylation or SUMOylation of the kainate receptor (KAR) subunit GluK2 have both individually been shown to regulate KAR surface expression. However, it is unknown whether phosphorylation and SUMOylation of GluK2 are important for activity-dependent KAR synaptic plasticity. We found that protein kinase C-mediated phosphorylation of GluK2 at serine 868 promotes GluK2 SUMOylation at lysine 886 and that both of these events are necessary for the internalization of GluK2-containing KARs that occurs during long-term depression of KAR-mediated synaptic transmission at rat hippocampal mossy fiber synapses. Conversely, phosphorylation of GluK2 at serine 868 in the absence of SUMOylation led to an increase in KAR surface expression by facilitating receptor recycling between endosomal compartments and the plasma membrane. Our results suggest a role for the dynamic control of synaptic SUMOylation in the regulation of KAR synaptic transmission and plasticity.
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Corrêa, Sonia A. L., C. J. Hunter, O. Palygin, S. C. Wauters, K. J. Martin, C. McKenzie, K. McKelvey, et al. "MSK1 regulates homeostatic and experience-dependent synaptic plasticity." 2012. http://hdl.handle.net/10454/5942.
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NoThe ability of neurons to modulate synaptic strength underpins synaptic plasticity, learning and memory, and adaptation to sensory experience. Despite the importance of synaptic adaptation in directing, reinforcing, and revising the behavioral response to environmental influences, the cellular and molecular mechanisms underlying synaptic adaptation are far from clear. Brain-derived neurotrophic factor (BDNF) is a prime initiator of structural and functional synaptic adaptation. However, the signaling cascade activated by BDNF to initiate these adaptive changes has not been elucidated. We have previously shown that BDNF activates mitogen- and stress-activated kinase 1 (MSK1), which regulates gene transcription via the phosphorylation of both CREB and histone H3. Using mice with a kinase-dead knock-in mutation of MSK1, we now show that MSK1 is necessary for the upregulation of synaptic strength in response to environmental enrichment in vivo. Furthermore, neurons from MSK1 kinase-dead mice failed to show scaling of synaptic transmission in response to activity deprivation in vitro, a deficit that could be rescued by reintroduction of wild-type MSK1. We also show that MSK1 forms part of a BDNF- and MAPK-dependent signaling cascade required for homeostatic synaptic scaling, which likely resides in the ability of MSK1 to regulate cell surface GluA1 expression via the induction of Arc/Arg3.1. These results demonstrate that MSK1 is an integral part of a signaling pathway that underlies the adaptive response to synaptic and environmental experience. MSK1 may thus act as a key homeostat in the activity- and experience-dependent regulation of synaptic strength.
Book chapters on the topic "Red clump"
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Puzeras, Eduardas, and Gražina Tautvaišienė. "Chemical Properties of the Hipparcos Red Clump." In Star Clusters in the Era of Large Surveys, 221–22. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-22113-2_35.
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Ribas, Salvador J., Francesca Figueras, and Jordi Torra. "A Kinematical Study of the Galactic Disk Using Red Clump Stars." In Astrophysics and Space Science Proceedings, 433. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-642-11250-8_115.
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Tautvaišienė, Gražina, and Šarūnas Mikolaitis. "Carbon and Nitrogen As Tracers of Stellar Evolution in Red Clump Stars of Open Clusters." In Star Clusters in the Era of Large Surveys, 229–30. Berlin, Heidelberg: Springer Berlin Heidelberg, 2011. http://dx.doi.org/10.1007/978-3-642-22113-2_39.
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Mateo, Mario, and Despina Hatzidimitriou. "The Evolution of the Red Giant Clump and the Structure of the Small Magellanic Cloud." In The Stellar Populations of Galaxies, 454. Dordrecht: Springer Netherlands, 1992. http://dx.doi.org/10.1007/978-94-011-2434-8_121.
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Stanek, K. Z., M. Mateo, A. Udalski, M. Szymański, J. Kałużny, M. Kubiak, and W. Krzemiński. "Evidence for the Galactic Bar from the Two Color Photometry of the Bulge Red Clump Stars." In Unsolved Problems of the Milky Way, 103–9. Dordrecht: Springer Netherlands, 1996. http://dx.doi.org/10.1007/978-94-009-1687-6_13.
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"Horizontal Branch and Red Clump." In Old Stellar Populations, 163–230. Weinheim, Germany: Wiley-VCH Verlag GmbH & Co. KGaA, 2013. http://dx.doi.org/10.1002/9783527665518.ch4.
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"4896 reed clump [n]." In Encyclopedic Dictionary of Landscape and Urban Planning, 803. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-540-76435-9_11215.
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"planting [n], reed rhizome and shoot clumps." In Encyclopedic Dictionary of Landscape and Urban Planning, 713. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-540-76435-9_9993.
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"reed rhizome and shoot clumps planting [n]." In Encyclopedic Dictionary of Landscape and Urban Planning, 803. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-540-76435-9_11222.
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"4373 planting [n] of reed rhizome clumps." In Encyclopedic Dictionary of Landscape and Urban Planning, 715. Berlin, Heidelberg: Springer Berlin Heidelberg, 2010. http://dx.doi.org/10.1007/978-3-540-76435-9_10035.
Full textConference papers on the topic "Red clump"
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Miglio, A., J. Montalbán, P. Eggenberger, S. Hekker, A. Noels, Joyce Ann Guzik, and Paul A. Bradley. "Asteroseismology of red-clump stars with CoRoT and Kepler." In STELLAR PULSATION: CHALLENGES FOR THEORY AND OBSERVATION: Proceedings of the International Conference. AIP, 2009. http://dx.doi.org/10.1063/1.3246424.
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Dintenfass, L. "VERY LARGE AND COMPACT AGGREGATES OF RED CELLS IN HEART DISEASE AND CANCER: POSSIBLY AN ANALOGOUS ROLE IN THE MICROCIRCULATION AS PLATELET AGGREGATES." In XIth International Congress on Thrombosis and Haemostasis. Schattauer GmbH, 1987. http://dx.doi.org/10.1055/s-0038-1644213.
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Very large aggregates of red blood cells, showing compact morphology, are easily observed in vitro, and might be of importance in the in vivo microcirculation. Blood from patients with myocardial infarction, WaldenstrBm1s macroglobulinaemia, or varoous carcinomas. etc., was anticoagulated with EDTA, and adjusted to haematocrit of 0.30, using native plasma. All tests were carried out in the slit-capillary photoviscometer, at temp, of 22°C. Micro and macrophotographs were taken during flow and stasis, using slits of 12.5 and 50 micron gaps. Studies showed that very large (two-dimensional) red cell aggregates are formed, such aggregates (clumps) containing up to 50,000 red cells in a single clump. The architecture of such aggregates differed according to the origin of blood: both rouleaux type and random / compact type of aggregates were observed; in principle, a spectrum of morphologies can be seen. These observations form a link between the earlier work of FAHRAEUS, on the one hand, and that of KNISELY, on the other; whic works appeared at the time to be contradictory and irreconcilable.
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Richards, Anita, Khudhair Assaf, Alain Baudry, R. J. Davis, Leen Decin, Moshe Elitzur, Sandra Etoka, et al. "What causes clumps in winds from red supergiants and asymptotic giant branch stars?" In 11th European VLBI Network Symposium & Users Meeting. Trieste, Italy: Sissa Medialab, 2016. http://dx.doi.org/10.22323/1.178.0046.
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Milanovic, M., J. Korelic, A. Hren, F. Mihalic, and P. Slibar. "The RC-RCD clamp circuit for fly-back converter." In Proceedings of the IEEE International Symposium on Industrial Electronics. IEEE, 2005. http://dx.doi.org/10.1109/isie.2005.1528976.
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Igland, Ragnar T., and Tore So̸reide. "Advanced Pipeline Trawl Gear Impact Design." In ASME 2008 27th International Conference on Offshore Mechanics and Arctic Engineering. ASMEDC, 2008. http://dx.doi.org/10.1115/omae2008-57354.
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Non-linear dynamic finite element analysis for the interference between clump weight and pipeline on seabed is performed using ANSYS software package, Ref /1/. Output from the analysis is the pull-over force magnitude, as well as shape and duration of impact on pipeline from the clump weight. Two pipelines sizes are analysed for trawl pull-over, the 10" and 12" pipelines laying on seabed. Small scale tests have been used to verify the FE model. The dynamic behaviour during impact testing is fairly well simulated by FE analysis scheme chosen. The results from the FE analysis are compared with the recommended practise outlined by DNV-RP-F111. Realistic trawl pull-over loads are established using actual stiffness of the pipeline and the pipe-soil interaction. The reduced trawl loads and the effect of pipe-soil interaction lead to reduced load effects and will avoid a conservative design and reduce the intervention costs.
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Wuti, Virot, Amata Luangpol, Kaweewat Tattiwong, Anan Sopin, Phaophak Sirisuk, and Chanin Bunlaksananusorn. "Performance Comparison between a two-switch and RCD clamp forward converters." In 2019 5th International conference on Engineering, Applied Sciences and Technology (ICEAST). IEEE, 2019. http://dx.doi.org/10.1109/iceast.2019.8802553.
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Alleman, Neil. "Increasing the Safety and Efficiency of Completions with the Utilization of Remote Manipulation Systems and Elimination of Hanging Sheaves." In Offshore Technology Conference Asia. OTC, 2022. http://dx.doi.org/10.4043/31464-ms.
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Abstract The process of running completions typically involves an increased complexity of systems and setups. The running of control lines and umbilicals have historically used hanging sheaves to route the lines from the spoolers to well center and require increased number of personnel in the red zone during operations. These complexities introduce many risks and potential incidents that operators aim to eliminate. Typical procedures for running completions require man-riding operations to hang sheaves in the derrick. Once the control lines or umbilicals are routed through these sheaves, they become overhead loaded objects and subsequently increase the risk of incident to personnel working on the rig floor. Other operational steps include the manual manipulation of lines to clamp the lines/umbilical to the tubular. This traditional clamping procedure not only requires an increased number of personnel in the red zone, but it also introduces inefficiencies to the operation. Through planning and the use of specialized remote manipulation technologies, operators can remove the need for overhead control line/umbilical sheaves and the manual handling of lines in the red zone. Although risks do not always result in incidents, organizations still strive to eliminate risks throughout their operations. By using remote manipulation technologies that eliminate control line/umbilical hanging sheaves, the operators benefit from the following: – Eliminating working at height for sheave installation – Eliminating overhead loaded components and increasing safety of personnel working on the rig floor – Decreasing the number of personnel required in the red zone and reducing manual handling – Increasing the efficiency of the operation By using systems like these, operators have been able to increase average running speeds, improving from 8.8 to 5.9 minutes per joint, as well as eliminate potentially fatal incidents that have occurred during the completions running process.
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Lakshmi, D., A. Usha, Pramod Kumar Rampelli, D. Sreenivasa Reddy, Bhoopendra Kumar Singh, and Vinod Chippalkatti. "Design and development of high frequency 360Watt RCD clamp forward converter for radar applications." In 2014 International Conference on Advances in Electronics, Computers and Communications (ICAECC). IEEE, 2014. http://dx.doi.org/10.1109/icaecc.2014.7002468.
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Igland, Ragnar T., and Trond Lamvik. "Using ECA in Structural Integrity of Submarine Pipelines for Optimalization of Intervention Work." In ASME 2010 29th International Conference on Ocean, Offshore and Arctic Engineering. ASMEDC, 2010. http://dx.doi.org/10.1115/omae2010-20349.
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The paper deals with the design methodology to define the design loads and determine the maximum allowable size of girth weld defects. The motivation for this work is reduced intervention costs obtained by opening all free spans as these are governing for rock infill volumes. 20–30% reduction of the intervention work is obtained. Structural integrity of the pipeline related to the interference with fishing gear is an important design scenario. Trawling in free span, pull-over loads with clump weight as an ALS condition is the main issue. REINERTSEN observed during detail design a lack of acceptance criteria for ALS conditions in the DNV OS-F101 design code, Ref. [1] for interference between trawl gear and subsea pipelines with low D/t ratio. Curvature in the trawl pull-over point as a function of time is found approximately constant while trawl load is increasing. The membrane forces carry most of the trawl load a few seconds after the trawl impact while bending moment decreases. This is in accordance to the philosophy that the strain and the curvature will be nearly constant for increased loading. The global load bearing mechanism is membrane and less bending. This means that we have control on the strain and that the pipeline system maintains its stiffness against loading for this high axial capacity of the flowline. These observations leads to a deformation controlled trawl load approach where an ECA of the flowline can be used to document structural integrity. Engineering Criticality Assessment (ECA) analysis is applied to evaluate the integrity of the flowlines with respect to risk for unstable fracture in girth welds due to impact from trawl equipment. The fatigue load effects from installation, temporary and operational phases are included in the ECA analysis. Geometric effects and external/internal pressure are included using the tailormade softwares LINKpipe, Ref. [7] and Crackwise4, Ref. [8]. The residual capacity of the flowlines is calculated with emphasis on fatigue during operation after the trawl pull-over. The fatigue life should be within the inspection interval, reflecting the Integrity Management Scheme.
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Chong, W. W. F., M. Teodorescu, and H. Rahnejat. "Influence of Ultra-Thin Film Tribology on Hard Disk Areal Storage Capacity." In STLE/ASME 2010 International Joint Tribology Conference. ASMEDC, 2010. http://dx.doi.org/10.1115/ijtc2010-41128.
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In most industrial applications, a thin film of lubricant improves the tribological behaviour of the load carrying conjunctions. Modern hard disk drives are no exception, where one of the challenges is the progressive demand for higher data storage capacity, while decreasing the physical size of the device. This paper investigates the load carrying capacity of an ultra thin lubricant film formed between the hard disk drive platter and its flying read-write head slider. Hydrodynamic wedge action is responsible for the entrainment of a film of perfluoropolyether into the conjunction, but does not account for the main share of the load carrying capacity of the very thin discretized film, several molecular diameters of the fluid in thickness. It is shown that the main mechanism of pressure generation is in fact the solvation effect. Additionally, starvation of contact may well occur, further exacerbating the thinness of a lubricant film. There is often a cavitation region at the contact exit, which is followed by film reformation, changing the density distribution of lubricant on the surface and consequently the attainable data storage density. This is caused by the observed clumps of lubricant in the reformation zones (a phenomenon referred to as lubricant mogul) which can also cause transient motions of the read-write head.
Reports on the topic "Red clump"
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Moran, Nava, Richard Crain, and Wolf-Dieter Reiter. Regulation by Light of Plant Potassium Uptake through K Channels: Biochemical, Physiological and Biophysical Study. United States Department of Agriculture, September 1995. http://dx.doi.org/10.32747/1995.7571356.bard.
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The swelling of plant motor cells is regulated by various signals with almost unknown mediators. One of the obligatory steps in the signaling cascade is the activation of K+-influx channels -K+ channels activated by hyperpolarization (KH channels). We thus explored the regulation of these channels in our model system, motor cell protoplasts from Samanea saman, using patch-clamp in the "whole cell" configuration. (a) The most novel finding was that the activity of KH channels in situ varied with the time of the day, in positive correlation with cell swelling: in Extensor cells KH channels were active in the earlier part of the day, while in Flexor cells only during the later part of the day; (b) High internal pH promoted the activity of these channels in Extensor cells, opposite to the behavior of the equivalent channels in guard cells, but in conformity with the predicted behavior of the putative KH channel, cloned from S. saman recently; (c) HIgh external K+ concentration increased (KH channel currents in Flexor cells. BL depolarized the Flexor cells, as detected in cell-attached patch-clamp recording, using KD channels (the K+-efflux channels) as "voltage-sensing devices". Subsequent Red-Light (RL) pulse followed by Darkness, hyperpolarized the cell. We attribute these changes to the inhibition of the H+-pump by BL and its reactivation by RL, as they were abolished by an H+-pump inhibitor. BL increased also the activity KD channels, in a voltage-independent manner - in all probability by an independent signaling pathway. Blue-Light (BL), which stimulates shrinking of Flexor cells, evoked the IP3 signaling cascade (detected directly by IP3 binding assay), known to mobilize cytosolic Ca2+. Nevertheless, cytosolic Ca2+ . did not activate the KD channel in excised, inside-out patches. In this study we established a close functional similarity of the KD channels between Flexor and Extensior cells. Thus the differences in their responses must stem from different links to signaling in both cell types.