Bibliographies thématiques / NGC 6810

Littérature scientifique sur le sujet « NGC 6810 »

Auteur : Grafiati
Publié le 10 mars 2023

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Articles de revues sur le sujet "NGC 6810"

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Strickland, David K. « A new superwind galaxy : XMM–Newton observations of NGC 6810 ». Monthly Notices of the Royal Astronomical Society 376, no 2 (avril 2007) : 523–33. http://dx.doi.org/10.1111/j.1365-2966.2007.11478.x.

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Hekker, S., S. Basu, D. Stello, T. Kallinger, F. Grundahl, S. Mathur, R. A. García et al. « Asteroseismic inferences on red giants in open clusters NGC 6791, NGC 6819, and NGC 6811 usingKepler ». Astronomy & ; Astrophysics 530 (18 mai 2011) : A100. http://dx.doi.org/10.1051/0004-6361/201016303.

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Corsaro, Enrico, Dennis Stello, Daniel Huber, Timothy R. Bedding, Alfio Bonanno, Karsten Brogaard, Thomas Kallinger et al. « ASTEROSEISMOLOGY OF THE OPEN CLUSTERS NGC 6791, NGC 6811, AND NGC 6819 FROM 19 MONTHS OFKEPLERPHOTOMETRY ». Astrophysical Journal 757, no 2 (17 septembre 2012) : 190. http://dx.doi.org/10.1088/0004-637x/757/2/190.

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Stello, Dennis, Søren Meibom, Ronald L. Gilliland, Frank Grundahl, Saskia Hekker, Benoît Mosser, Thomas Kallinger et al. « AN ASTEROSEISMIC MEMBERSHIP STUDY OF THE RED GIANTS IN THREE OPEN CLUSTERS OBSERVED BYKEPLER : NGC 6791, NGC 6819, AND NGC 6811 ». Astrophysical Journal 739, no 1 (30 août 2011) : 13. http://dx.doi.org/10.1088/0004-637x/739/1/13.

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Bellamy, B., et D. Stello. « New Seismic Members in NGC 6791 and NGC 6819 ». EPJ Web of Conferences 101 (2015) : 06007. http://dx.doi.org/10.1051/epjconf/201510106007.

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Madejski, Greg M., Chris Done, T. Jane Turner, Richard F. Mushotzky, Peter Serlemitsos, Fabrizio Fiore, Marek Sikora et Mitchell C. Begelman. « Solving the Mystery of the Periodicity in the Seyfert Galaxy NGC 6814 ». Symposium - International Astronomical Union 159 (1994) : 127–30. http://dx.doi.org/10.1017/s0074180900174911.

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The reports of periodic X–ray emission from the Seyfert galaxy NGC 6814 have motivated a number of exotic models for the active nucleus. Our ROSAT observation shows that while the nucleus of NGC 6814 is indeed an X–ray emitter, the periodicity is due to another source, most likely a Galactic accreting binary system, ∼ 37 arc min away.
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Ананьевская, Ю. К., В. Н. Фролов et Е. В. Поляков. « Исследование рассеянного звездного скопления NGC 6800 ». Письма в астрономический журнал : Астрономия и космическая астрофизика 41, no 07 (2015) : 367–76. http://dx.doi.org/10.7868/s0320010815060017.

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Yontan, T., S. Bilir, Z. F. Bostancı, T. Ak, S. Karaali, T. Güver, S. Ak, Ş. Duran et E. Paunzen. « CCD UBVRI photometry of NGC 6811 ». Astrophysics and Space Science 355, no 2 (29 janvier 2015) : 267–81. http://dx.doi.org/10.1007/s10509-014-2175-5.

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Kuehn, Charles A., Jason A. Drury, Beau R. Bellamy, Dennis Stello, Timothy R. Bedding, Mike Reed et Breanna Quick. « Photometry UsingKepler“Superstamps” of Open Clusters NGC 6791 & ; NGC 6819 ». EPJ Web of Conferences 101 (2015) : 06040. http://dx.doi.org/10.1051/epjconf/201510106040.

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Pottasch, S. R., D. A. Beintema et W. A. Feibelman. « Abundances of planetary nebulae NGC 2022, NGC 6818 and IC 4191 ». Astronomy & ; Astrophysics 436, no 3 (juin 2005) : 953–65. http://dx.doi.org/10.1051/0004-6361:20042627.

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Thèses sur le sujet "NGC 6810"

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Street, Rachel. « A search for extra-solar planetary transits in the field of open cluster NGC 6819 ». Thesis, University of St Andrews, 2002. http://hdl.handle.net/10023/12939.

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The technique of searching for extra-solar planetary transits is investigated. This technique, which relies on detecting the brief, shallow eclipses caused by planets passing across the line of sight to the primary star, requires high-precision time-series photometry of large numbers of stars in order to detect these statistically rare events. Observations of ~ 18000 stars in the field including the intermediate-age open cluster NGC 6819 are presented. This target field contrasts with the stellar environment surveyed by the radial velocity technique, which concentrates on the Solar neighbourhood. I present the data-reduction techniques used to obtain high-precision photometry in a semi-automated fashion for tens of thousands of stars at a time, together with an algorithm designed to search the resulting lightcurves for the transit signatures of hot Jupiter type planets. I describe simulations designed to test the detection efficiency of this algorithm and, for comparison, predict the number of transits expected from this data, assuming that hot Jupiter planets similar to HD 209458 are as common in the field of NGC 6819 as they are in the Solar neighbourhood. While no planetary transits have yet been identified, the detection of several very low amplitude eclipses by stellar companions demonstrates the effectiveness of the method. This study also indicates that stellar activity and particularly blending are significant causes of false detections. A useful additional consequence of studying this time-series photometry is the census it provides of some of the variable stars in the field. I report on the discovery of a variety of newly-discovered variables, including Algol-type detached eclipsing binaries which are likely to consist of M-dwarf stars. Further study of these stars is strongly recommended in order to help constrain models of stellar structure at the very low mass end. I conclude with a summary of this work in the context of other efforts being made in this field and recommend promising avenues of further study.
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Venturi, Giacomo. « The impact of galactic outflows on their host galaxies through spatially resolved spectroscopy ». Doctoral thesis, 2019. http://hdl.handle.net/2158/1160629.

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The observed properties of galaxies and supermassive black holes (BH) at their centers suggest that there must be a non-gravitational feedback mechanism regulating their evolution. These are the discrepancy at low and high masses between the observed stellar mass function of galaxies and that predicted by ΛCDM models, the scaling relations between the mass of BHs and the velocity dispersion, mass and luminosity of the host galaxy spheroid and the similarity between BH growth and star formation cosmic histories. Models of galaxy formation and evolution in fact routinely include feedback from active galactic nuclei (AGN) and supernovae (SNe), which can successfully reproduce the observed properties cited above. Models consider the following two types of AGN feedback: the radiative mode (or quasar mode), that operates during a luminous AGN phase through winds powered by radiation pressure, and the kinetic (or radio) mode, in which kinetic energy is released by the AGN on longer timescales through relativistic jets, which heat the surrounding halo in galaxy clusters, thus preventing cooling and further accretion on the central galaxy, and consequently further star formation. So far, the clearest observational evidence of AGN feedback comes from the kinetic mode in massive central cluster galaxies. Radiative feedback is instead more elusive, and has been recently revealed in action only in a few luminous quasars around the peak of AGN activity history (z~2), where most powerful outflows are observed. However, it is not possible to study high-z quasar outflows on small spatial scales (<100 pc), being poorly-resolved or even unresolved in observations, due to their large distances. This can lead to systematics and uncertainties in the determination of outflow properties and forces to make some assumptions on them, which further increases the uncertainties on the outflow energetics and complicates the evaluation of the impact of outflows on host galaxies and the comparison with models. On the contrary, due to their vicinity, nearby active galaxies are ideal laboratories to explore in detail outflow properties, their formation and acceleration mechanisms, as well as the effects of AGN activity on host galaxies. This work focuses on investigating the properties of outflows in nearby Seyfert galaxies, the physical conditions of the ionized gas and the interplay between nuclear activity and star formation in the galaxy, thanks to the unprecedented combination of spatial and spectral coverage provided by the integral field spectrograph MUSE at the Very Large Telescope (VLT). We introduce our optically- and X-ray selected sample of nearby Seyferts, called MAGNUM survey. We present our MUSE emission-line flux and kinematic maps of the 10 objects we have analyzed so far, including a star-forming galaxy, NGC 6810, to study the properties of a starburst outflow for comparison as well. We map the ionized gas down to spatial scales as low as ~10 pc. We find ubiquitous ionization cones and outflows with various morphologies and extensions, from a few hundred pc to several kpc. We detect peculiar kinematic features suggestive of outflows with hollow-conical structures. We also identify enhanced linewidths perpendicular to radio jets, which point to a correlation between the presence of jets and perpendicular turbulent or outflowing gas motions. We then focus on a detailed multi-wavelength study of the ionized gas and outflow, in terms of physical properties, kinematics, and ionization mechanisms, in one specific galaxy of our sample, NGC 1365, from MUSE in optical band and Chandra satellite in X-rays. Here we map a kpc-scale biconical outflow ionized by the AGN prominent in [O III], while Hα emission traces star formation in a circumnuclear ring and along the bar of the galaxy. Soft X-rays are mostly due to thermal emission from the star-forming regions, but we manage to isolate the AGN photoionized component which matches the [O III] emission from MUSE. We map the mass outflow rate of the galactic ionized outflow, which matches that of the nuclear X-ray wind and then decreases with radius. The integrated mass outflow rate, kinetic energy rate, and outflow velocity are broadly consistent with the typical relations observed in more luminous AGN. We extend our analysis to the nearby star-forming galaxy NGC 6810, whose bipolar galactic ionized outflow we map with MUSE. We determine the dominant ionization mechanism in the outflow, its density and ionization parameter, discovering the first case of star formation occurring within an outflow in an unambiguously star-forming galaxy. We finally investigate with MUSE also the kinetic AGN feedback, by studying the ionized gas enshrouding the X-ray cavity inflated by radio jets around the massive radio-galaxy 3C 317 at the center of the local cluster Abell 2052. Thanks to MUSE capabilities, by mapping the warm gas filaments enshrouding the bubble we are able to directly measure the expansion velocity of the cavity, which usually is instead assumed or derived from indirect and model-dependent methods.
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Manne-Nicholas, Emily Rachel. « Determining the Mass of the Supermassive Black Hole in NGC 6814 ». 2017. http://scholarworks.gsu.edu/phy_astr_diss/94.

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Supermassive black holes (SMBH) are now thought to exist at the center nearly all massive galaxies. Not only are they thought to be ubiquitous, but it was also discovered nearly two decades ago that the mass of these SMBHs correlate strongly with properties of their host galaxies including bulge stellar velocity dispersion (MBH-sigma) and bulge luminosity (MBH-Lbulge). This correlation was not expected due to the tiny size of the SMBH gravitational sphere of influence compared to the size of the host galaxy, and imply a connection between the two, but this connection is still not well-understood. One step toward understanding this connection is to accurately measure the masses of these black holes. Two of the most common direct SMBH mass measurement techniques are stellar dynamical modeling (SDM), which generally only applies to quiescent galaxies, and reverberation mapping (RM), which can only be applied to active galactic nuclei (AGN) that exhibit broadened emission lines. Due to the unknown geometry of the region that produces these broad lines, the whole RM sample of black hole masses generally needs to be multiplied by a constant called the f-factor to bring it into agreement with the SDM sample on the MBH-sigma relation. It is unknown how well this f-factor, being a population average, applies to individual RM masses. It would therefore be useful to measure an SMBH mass with both methods simultaneously to test whether they produce the same black hole mass. However, because the RM and SDM techniques usually apply to galaxies that are not possible for both, this has only been attempted twice before (NGC 3227 and NGC 4151). The purpose of this dissertation is to apply SDM to the SMBH at the center of NGC 6814 for which there already exists an RM mass. This makes it only the third broad-lined AGN for which an SDM mass has been derived. In order to perform SDM accurately, the distance to the galaxy needs to be well-constrained as the error in the SDM mass scales linearly with distance. Because no adequate distance measurements already exist, the first half of this dissertation is devoted to deriving a Cepheid distance to NGC 6814 from V- and I-band HST WFC3 time series photometry. We measure the distance to NGC 6814 to be 17.54 +1.44/-1.33 Mpc. In the second half, we incorporate that distance measurement into our stellar dynamical modeling on Gemini NIFS+Altair IFU data of NGC 6814's central 1.55''x1.55''. We derive a mass of 1.19 +37.57/-1.17 x108 solar masses, and best fit mass-to-light ratio of 0.948 +0.032/-0.208 in solar units. This mass is nearly an order of magnitude larger than the RM mass but has a 3-sigma range spanning nearly three orders of magnitude. We describe possible reasons for our larger-than-expected mass value, such as the existence of a bar, which would not be well-modeled by an axisymmetric dynamical code. Finally, we describe future steps that may be taken to better constrain the mass, such as creating more models to further explore parameter space.
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Chapitres de livres sur le sujet "NGC 6810"

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Wallinder, F. « A Single Variability Model for NGC 6814 and NGC 5548 ». Dans Theory of Accretion Disks — 2, 287–91. Dordrecht : Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4_29.

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Bash, F. N., J. H. Davis, D. T. Jaffe, W. F. Wall et E. C. Sutton. « CO 3-2 Observations of NGC 253 ». Dans Submillimetre Astronomy, 227–28. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_85.

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Abramowicz, M. A., G. Bao, V. Karas et A. Lanza. « Periodic X-Ray Variability of the Seyfert Galaxy NGC 6814 ». Dans Theory of Accretion Disks — 2, 213–21. Dordrecht : Springer Netherlands, 1994. http://dx.doi.org/10.1007/978-94-011-0858-4_19.

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Tacconi, Linda J. « The Azimuthal Distribution of the ISM in NGC 6946 ». Dans Submillimetre Astronomy, 243–44. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_93.

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Moriarty-Schieven, G. H., V. A. Hughes et R. L. Snell. « NGC 2071 : A Twin for L1551, and Evidence for Backflow ? » Dans Submillimetre Astronomy, 37–38. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_11.

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Kameya, Osamu. « Millimeter and Submillimeter Observations of the NGC 7538 Molecular Cloud ». Dans Submillimetre Astronomy, 181–82. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_67.

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Rosenthal, E., S. Eales, S. Stephens et K. Y. Lo. « CO (3-2) Emission from the Nucleus of NGC 6946 ». Dans Submillimetre Astronomy, 241–42. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_92.

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Levi-Montalcini, Rita. « NGF : An Uncharted Route ». Dans The Neurosciences : Paths of Discovery, I, 245–65. Boston, MA : Birkhäuser Boston, 1992. http://dx.doi.org/10.1007/978-1-4684-6817-5_14.

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Howe, J. E., N. Geis, R. Genzel, D. T. Jaffe, A. Poglitsch et G. J. Stacey. « Extensive C+ 158 µm Line Mapping of W3 and NGC 1977 ». Dans Submillimetre Astronomy, 285–86. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_109.

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Dupraz, C., F. Casoli, F. Combes et M. Gerin. « CO(1-0) in a Newly-Born Elliptical Galaxy : NGC 7252 ». Dans Submillimetre Astronomy, 249–50. Dordrecht : Springer Netherlands, 1990. http://dx.doi.org/10.1007/978-94-015-6850-0_96.

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Actes de conférences sur le sujet "NGC 6810"

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Abramowicz, Marek A. « Orbital models for the periodic X-ray flares of NGC 6814 ». Dans Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42222.

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Madejski, G., C. Done, T. J. Turner, R. F. Mushotzky, P. Serlemitsos, F. Fiore, M. Sikora et M. Begelman. « Solving the mystery of the periodicity in the Seyfert galaxy NGC 6814 ». Dans The soft x-ray cosmos : ROSAT science symposium and data analysis workshop. AIP, 1994. http://dx.doi.org/10.1063/1.46743.

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Leighly, Karen, Hideyo Kunieda et Sachiko Tsuruta. « Temporal and spectral X-ray variability from the Seyfert 1 galaxy NGC 6814 ». Dans Testing the AGN paradigm diagnostics. AIP, 1992. http://dx.doi.org/10.1063/1.42224.

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Zhou, Jianhua, Tingting Xia, Mian Li et Min Xu. « A Normalized Circle Intersection Method for Bi-Objective Optimization Programming ». Dans ASME 2017 International Design Engineering Technical Conferences and Computers and Information in Engineering Conference. American Society of Mechanical Engineers, 2017. http://dx.doi.org/10.1115/detc2017-68101.

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Multi-objective optimization (MOO) problems are encountered in many applications and a number of approaches have been proposed to deal with this kind of problems. Despite the computational efforts, the quality of the Pareto front is also a considerable issue. An evenly distributed Pareto front is desirable for developing analytical expressions. In this paper, a brand new approach called Normalized Circle Intersection (NCI) is proposed, which is able to efficiently generate a Pareto front with evenly-distributed Pareto points for bi-objective problems, no matter the feasible boundary is convex or not. Firstly, the anchor points are computed using an existing sequential MOO (SMOO) approach. Then in the normalized objective space, a circle with a radius of r centering at one of the anchor points or the latest obtained Pareto point is drawn. The intersection of the circle and the feasible boundary, which exists for sure, can be determined whether it is a Pareto point or not. For a convex or concave feasible boundary, the intersection is exactly the Pareto point to be found, while for a non-convex boundary the intersection can provide useful information for searching the true Pareto point even if it self is not a Pareto point. A novel MOO formulation is proposed for NCI correspondingly. Four examples, including two numerical and two engineering examples, are provided to demonstrate the applicability of the proposed method. Comparison of the computational results with WS, NNC and SMOO shows the effectiveness of the proposed method.
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Rapports d'organisations sur le sujet "NGC 6810"

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Madejski, Grzegorz. X-ray Variability of the Magnetic Cataclysmic Variable V1432 Aql and the Seyfert Galaxy NGC 6814. Office of Scientific and Technical Information (OSTI), juillet 2003. http://dx.doi.org/10.2172/813321.

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