Relevant bibliographies by topics / Interferometers telescopes stars

Academic literature on the topic 'Interferometers telescopes stars'

Author: Grafiati
Published: 4 June 2021
Last updated: 20 February 2023

Create a spot-on reference in APA, MLA, Chicago, Harvard, and other styles

Select a source type:

Contents

Consult the lists of relevant articles, books, theses, conference reports, and other scholarly sources on the topic 'Interferometers telescopes stars.'

Next to every source in the list of references, there is an 'Add to bibliography' button. Press on it, and we will generate automatically the bibliographic reference to the chosen work in the citation style you need: APA, MLA, Harvard, Chicago, Vancouver, etc.

You can also download the full text of the academic publication as pdf and read online its abstract whenever available in the metadata.

Journal articles on the topic "Interferometers telescopes stars"

1

McAlister, Harold A. "Overview of Multiple–Aperture Interferometry Binary Star Results from the Northern Hemisphere." Proceedings of the International Astronomical Union 2, S240 (August 2006): 35–44. http://dx.doi.org/10.1017/s1743921307003778.

Full text
Abstract:
AbstractLong-baseline optical interferometry (LBI) can nearly close the gap in selection space between astrometric and spectroscopic detection of binary star systems, bringing the complementary powers of astrometry and spectroscopy to bear on a complete dynamical understanding of such systems, particularly including the determination of the masses of the individual stellar components. In the case of double-lined spectroscopic systems, their resolution by long-baseline interferometry also yields the orbital parallax and hence the luminosities of the individual stars. In some of these cases, the angular diameters of one or more components are accessible, and so a complete specification of a star in terms of its mass, radius and luminosity is made.The northern hemisphere is now equipped with several interferometers of unprecedented capability in terms of their baseline sizes, numbers of telescopes and telescope apertures. These instruments, most notably the Palomar Testbed Interferometer at Mt. Palomar Observatory, have produced very significant results of a number of interesting systems fulfilling interferometry's promise to produce fundamental astrophysical data at levels of accuracy that challenge or confirm astrophysical theory.This paper presents basic principles of long-baseline interferometric study of binary stars and summarizes results from northern interferometers with specific examples of their broad impact on binary star astronomy.
APA, Harvard, Vancouver, ISO, and other styles
2

Defrère, D., P. Hinz, B. Mennesson, R. Millan-Gabet, A. Skemer, V. Bailey, and T. J. Rodigas. "Searching for Faint Exozodiacal Disks: Keck Results and LBTI Status." Proceedings of the International Astronomical Union 8, S299 (June 2013): 332–33. http://dx.doi.org/10.1017/s1743921313008818.

Full text
Abstract:
AbstractThe possible presence of dust in the habitable zone around nearby main-sequence stars is considered as a major hurdle toward the direct imaging of Earth-like extrasolar planets with future dedicated space-based telescopes (e.g., Roberge et al. 2012). In this context, NASA has funded two ground-based mid-infrared nulling interferometers to combine the large apertures available at the Keck Observatory and the Large Binocular Telescope (LBT). In this poster, we present the preliminary results of the extended survey carried out with the Keck Interferometer Nuller (KIN) between 2008 and 2011 and describe the forthcoming LBTI survey.
APA, Harvard, Vancouver, ISO, and other styles
3

Guinan, Edward F., Scott Engle, and Edward J. Devinney. "Advances in Telescope and Detector Technologies – Impacts on the Study and Understanding of Binary Star and Exoplanet Systems." Proceedings of the International Astronomical Union 7, S282 (July 2011): 11–20. http://dx.doi.org/10.1017/s1743921311026792.

Full text
Abstract:
AbstractCurrent and planned telescope systems (both on the ground and in space) as well as new technologies will be discussed with emphasis on their impact on the studies of binary star and exoplanet systems. Although no telescopes or space missions are primarily designed to study binary stars (what a pity!), several are available (or will be shortly) to study exoplanet systems. Nonetheless those telescopes and instruments can also be powerful tools for studying binary and variable stars. For example, early microlensing missions (mid-1990s) such as EROS, MACHO and OGLE were initially designed for probing dark matter in the halos of galaxies but, serendipitously, these programs turned out to be a bonanza for the studies of eclipsing binaries and variable stars in the Magellanic Clouds and in the Galactic Bulge. A more recent example of this kind of serendipity is the Kepler Mission. Although Kepler was designed to discover exoplanet transits (and so far has been very successful, returning many planetary candidates), Kepler is turning out to be a “stealth” stellar astrophysics mission returning fundamentally important and new information on eclipsing binaries, variable stars and, in particular, providing a treasure trove of data of all types of pulsating stars suitable for detailed Asteroseismology studies. With this in mind, current and planned telescopes and networks, new instruments and techniques (including interferometers) are discussed that can play important roles in our understanding of both binary star and exoplanet systems. Recent advances in detectors (e.g. laser frequency comb spectrographs), telescope networks (both small and large – e.g. Super-WASP, HAT-net, RoboNet, Las Combres Observatory Global Telescope (LCOGT) Network), wide field (panoramic) telescope systems (e.g. Large Synoptic Survey Telescope (LSST) and Pan-Starrs), huge telescopes (e.g. the Thirty Meter Telescope (TMT), the Overwhelming Large Telescope (OWL) and the Extremely Large Telescope (ELT)), and space missions, such as the James Webb Space Telescope (JWST), the possible NASA Explorer Transiting Exoplanet Survey Satellite (TESS – recently approved for further study) and Gaia (due for launch during 2013) will all be discussed. Also highlighted are advances in interferometers (both on the ground and from space) and imaging now possible at sub-millimeter wavelengths from the Extremely Long Array (ELVA) and Atacama Large Millimeter Array (ALMA). High precision Doppler spectroscopy, for example with HARPS, HIRES and more recently the Carnegie Planet Finder Spectrograph, are currently returning RVs typically better than ~2-m/s for some brighter exoplanet systems. But soon it should be possible to measure Doppler shifts as small as ~10-cm/s – sufficiently sensitive for detecting Earth-size planets. Also briefly discussed is the impact these instruments will have on the study of eclipsing binaries, along with future possibilities of utilizing methods from the emerging field of Astroinformatics, including: the Virtual Observatory (VO) and the possibilities of analyzing these huge datasets using Neural Network (NN) and Artificial Intelligence (AI) technologies.
APA, Harvard, Vancouver, ISO, and other styles
4

Horch, Elliott P., Samuel A. Weiss, Paul M. Klaucke, Richard A. Pellegrino, and Justin D. Rupert. "Observations with the Southern Connecticut Stellar Interferometer. I. Instrument Description and First Results." Astronomical Journal 163, no. 2 (January 26, 2022): 92. http://dx.doi.org/10.3847/1538-3881/ac43bb.

Full text
Abstract:
Abstract We discuss the design, construction, and operation of a new intensity interferometer, based on the campus of Southern Connecticut State University in New Haven, Connecticut. While this paper will focus on observations taken with an original two-telescope configuration, the current instrumentation consists of three portable 0.6 m Dobsonian telescopes with single-photon avalanche diode detectors located at the Newtonian focus of each telescope. Photons detected at each station are time stamped and read out with timing correlators that can give cross-correlations in timing to a precision of 48 ps. We detail our observations to date with the system, which has now been successfully used at our university in 16 nights of observing. Components of the instrument were also deployed on one occasion at Lowell Observatory, where the Perkins and Hall telescopes were made to function as an intensity interferometer. We characterize the performance of the instrument in detail. In total, the observations indicate the detection of a correlation peak at the level of 6.76σ when observing unresolved stars, and consistency with partial or no detection when observing at a baseline sufficient to resolve the star. Using these measurements, we conclude that the angular diameter of Arcturus is larger than 15 mas and that of Vega is between 0.8 and 17 mas. While the uncertainties are large at this point, both results are consistent with measures from amplitude-based long baseline optical interferometers.
APA, Harvard, Vancouver, ISO, and other styles
5

Gies, D. R. "O and B-star surface mapping." Symposium - International Astronomical Union 176 (1996): 121–28. http://dx.doi.org/10.1017/s0074180900083157.

Full text
Abstract:
The massive O and B-type stars will be among the first targets of the new generation of long baseline optical interferometers (such as the CHARA Array, a 400-m diameter distributed array of five 1-m telescopes). Many of these objects are binary stars for which joint astrometric and spectroscopic observations will provide masses and distances (e.g., 15 Mon; Gies et al. 1993), but there is also great interest in resolving disks of single stars. Early interferometric observations have already resolved the flattened circumstellar disks around some Be stars (Quirrenbach et al. 1994).
APA, Harvard, Vancouver, ISO, and other styles
6

Serabyn, Eugene. "Observing Faint Companions Close to Bright Stars." Proceedings of the International Astronomical Union 7, S282 (July 2011): 163–66. http://dx.doi.org/10.1017/s1743921311027268.

Full text
Abstract:
AbstractProgress in a number of technical areas is enabling imaging and interferometric observations at both smaller angular separations from bright stars and at deeper relative contrast levels. Here we discuss recent progress in several ongoing projects at the Jet Propulsion Laboratory. First, extreme adaptive optics wavefront correction has recently enabled the use of very short (i.e., blue) wavelengths to resolve close binaries. Second, phase-based coronagraphy has recently allowed observations of faint companions to within nearly one diffraction beam width of bright stars. Finally, rotating interferometers that can observe inside the diffraction beam of single aperture telescopes are being developed to detect close-in companions and bright exozodiacal dust. This paper presents a very brief summary of the techniques involved, along with some illustrative results.
APA, Harvard, Vancouver, ISO, and other styles
7

Zuckerman, B. "Radio and Millimeter Observations of Circumstellar Envelopes." Symposium - International Astronomical Union 120 (1987): 345–55. http://dx.doi.org/10.1017/s0074180900154300.

Full text
Abstract:
Circumstellar chemistry has been confined largely to analysis of a few dozen molecules in the envelope of one carbon-rich star, IRC+10216. A new generation of large millimeter wavelength telescopes promises to broaden the data base to include many other stars and additional molecules. Carbon-monoxide emission has already been detected from approximately 130 stars and many of these are prime candidates for chemical studies. The detection of HCN emission in a few oxygen-rich stars was quite unexpected and indicates that nonequilibrium chemical processes are important in at least some circumstellar envelopes. New millimeter wavelength interferometers can measure the spatial distribution of various molecules for comparison with predictions of models for photodissociation, freeze-out on grains, self-shielding, and nonspherical outflow.
APA, Harvard, Vancouver, ISO, and other styles
8

Pietraszewski, K. A. R. B., C. R. Bell, J. Ring, N. K. Reay, and M. Leeper. "Multiplexed interferometric stellar oscillation spectrometry - MISOS." Symposium - International Astronomical Union 123 (1988): 517–20. http://dx.doi.org/10.1017/s0074180900158620.

Full text
Abstract:
Interferometric spectrometry techniques for measuring stellar oscillations have been developed at Imperial College, resulting in two separate interferometers, the Michelson and the Fabry-Perot based instruments. They have both been used on large telescopes; the Michelson instrument to search for oscillations in solar-type stars and the Fabry-Perot instrument to measure oscillations in δScuti-type stars. So far there has been only marginal evidence for solar-type oscillations, including our observations of εCyg with ~1ms−1 precision. In order to increase the significance of future observations we are currently improving both instruments and aim to achieve a ten-fold increase in precision, i.e. ~10cms−1, by using up to 100 separate spectral lines simultaneously. Such an improvement will allow us to continue the search for solar-type oscillations.
APA, Harvard, Vancouver, ISO, and other styles
9

Davis, John. "Combining High Angular Resolution Interferometry and Spectroscopy in Studies of Stars and Stellar Systems." International Astronomical Union Colloquium 170 (1999): 390–400. http://dx.doi.org/10.1017/s025292110004882x.

Full text
Abstract:
AbstractA number of long baseline optical/infrared interferometers have commenced their scientific programs or are under development. These instruments will provide accurate measurements of the angular sizes of single stars and the angular separations of binary systems at resolutions impossible with conventional telescopes. The combination of interferometric data with the results of high-resolution spectroscopy will, for many classes of objects, provide a powerful method for studying them that neither technique can do alone. Examples include the combination of interferometric and spectroscopic data for spectroscopic binaries and, in particular, for double-lined binaries, and single-lined binaries of known parallax, to determine fundamental stellar quantities. Another example concerns the study of Cepheid variables, where the combination of the data can provide an independent calibration of the zero point of the luminosity scale. The requirements and potential of these combined interferometric-spectroscopic studies are discussed.
APA, Harvard, Vancouver, ISO, and other styles
10

Anthonioz, Fabien, F. Ménard, C. Pinte, W.-F. Thi, J. B. Lebouquin, J. P. Berger, M. Benisty, et al. "The VLTi/PIONIER survey of southern TTauri disks." Proceedings of the International Astronomical Union 8, S299 (June 2013): 94–98. http://dx.doi.org/10.1017/s1743921313007990.

Full text
Abstract:
AbstractStudying the inner regions of protoplanetary disks (1-10 AU) is of importance to understand the formation of planets and the accretion process feeding the forming central star. Herbig AeBe stars are bright enough to be routinely observed by Near IR interferometers. The data for the fainter T Tauri stars is much more sparse. In this contribution we present the results of our ongoing survey at the VLTI. We used the PIONIER combiner that allows the simultaneous use of 4 telescopes, yielding 6 baselines and 3 independent closure phases at once. PIONIER's integrated optics technology makes it a sensitive instrument. We have observed 22 T Tauri stars so far, the largest survey for T Tauri stars to this date.Our results demonstrate the very significant contribution of an extended component to the interferometric signal. The extended component is different from source to source and the data, with several baselines, offer a way to improve our knowledge of the disk geometry and/or composition. These results validate an earlier study by Pinte et al. 2008 and show that the dust inner radii of T Tauri disks now appear to be in better agreement with the expected position of the dust sublimation radius, contrary to previous claims.
APA, Harvard, Vancouver, ISO, and other styles
More sources

Dissertations / Theses on the topic "Interferometers telescopes stars"

1

Bock, Douglas Carl-Johan. "Wide Field Aperture Synthesis Radio Astronomy." University of Sydney. Physics, 1998. http://hdl.handle.net/2123/377.

Full text
Abstract:
This thesis is focussed on the Molonglo Observatory Synthesis Telescope (MOST), reporting on two primary areas of investigation. Firstly, it describes the recent upgrade of the MOST to perform an imaging survey of the southern sky. Secondly, it presents a MOST survey of the Vela supernova remnant and follow-up multiwavelength studies. The MOST Wide Field upgrade is the most significant instrumental upgrade of the telescope since observations began in 1981. It has made possible the nightly observation of fields with area ~5 square degrees, while retaining the operating frequency of 843 MHz and the pre-existing sensitivity to point sources and extended structure. The MOST will now be used to make a sensitive (rms approximately 1 mJy/beam) imaging survey of the sky south of declination -30°. This survey consists of two components: an extragalactic survey, which will begin in the south polar region, and a Galactic survey of latitudes |b| < 10°. These are expected to take about ten years. The upgrade has necessitated the installation of 352 new preamplifiers and phasing circuits which are controlled by 88 distributed microcontrollers, networked using optic fibre. The thesis documents the upgrade and describes the new systems, including associated testing, installation and commissioning. The thesis continues by presenting a new high-resolution radio continuum survey of the Vela supernova remnant (SNR), made with the MOST before the completion of the Wide Field upgrade. This remnant is the closest and one of the brightest SNRs. The contrast between the structures in the central pulsar-powered nebula and the synchrotron radiation shell allows the remnant to be identified morphologically as a member of the composite class. The data are the first of a composite remnant at spatial scales comparable with those available for the Cygnus Loop and the Crab Nebula, and make possible a comparison of radio, optical and soft X-ray emission from the resolved shell filaments. The survey covers an area of 50 square degrees at a resolution of 43" x 60", while imaging structures on scales up to 30'. It has been used for comparison with Wide Field observations to evaluate the performance of the upgraded MOST. The central plerion of the Vela SNR (Vela X) contains a network of complex filamentary structures. The validity of the imaging of these filaments has been confirmed with Very Large Array (VLA) observations at 1.4 GHz. Unlike the situation in the Crab Nebula, the filaments are not well correlated with H-alpha emission. Within a few parsec of the Vela pulsar the emission is much more complex than previously seen: both very sharp edges and more diffuse emission are present. It has been postulated that one of the brightest filaments in Vela X is associated with the X-ray feature (called a `jet') which appears to be emanating from the region of the pulsar. However, an analysis of the MOST and VLA data shows that this radio filament has a flat spectral index similar to another more distant filament within the plerion, indicating that it is probably unrelated to the X-ray feature.
APA, Harvard, Vancouver, ISO, and other styles
2

Bock, Douglas Carl-Johan. "Wide Field Aperture Synthesis Radio Astronomy." Thesis, The University of Sydney, 1997. http://hdl.handle.net/2123/377.

Full text
Abstract:
This thesis is focussed on the Molonglo Observatory Synthesis Telescope (MOST), reporting on two primary areas of investigation. Firstly, it describes the recent upgrade of the MOST to perform an imaging survey of the southern sky. Secondly, it presents a MOST survey of the Vela supernova remnant and follow-up multiwavelength studies. The MOST Wide Field upgrade is the most significant instrumental upgrade of the telescope since observations began in 1981. It has made possible the nightly observation of fields with area ~5 square degrees, while retaining the operating frequency of 843 MHz and the pre-existing sensitivity to point sources and extended structure. The MOST will now be used to make a sensitive (rms approximately 1 mJy/beam) imaging survey of the sky south of declination -30°. This survey consists of two components: an extragalactic survey, which will begin in the south polar region, and a Galactic survey of latitudes |b| < 10°. These are expected to take about ten years. The upgrade has necessitated the installation of 352 new preamplifiers and phasing circuits which are controlled by 88 distributed microcontrollers, networked using optic fibre. The thesis documents the upgrade and describes the new systems, including associated testing, installation and commissioning. The thesis continues by presenting a new high-resolution radio continuum survey of the Vela supernova remnant (SNR), made with the MOST before the completion of the Wide Field upgrade. This remnant is the closest and one of the brightest SNRs. The contrast between the structures in the central pulsar-powered nebula and the synchrotron radiation shell allows the remnant to be identified morphologically as a member of the composite class. The data are the first of a composite remnant at spatial scales comparable with those available for the Cygnus Loop and the Crab Nebula, and make possible a comparison of radio, optical and soft X-ray emission from the resolved shell filaments. The survey covers an area of 50 square degrees at a resolution of 43" x 60", while imaging structures on scales up to 30'. It has been used for comparison with Wide Field observations to evaluate the performance of the upgraded MOST. The central plerion of the Vela SNR (Vela X) contains a network of complex filamentary structures. The validity of the imaging of these filaments has been confirmed with Very Large Array (VLA) observations at 1.4 GHz. Unlike the situation in the Crab Nebula, the filaments are not well correlated with H-alpha emission. Within a few parsec of the Vela pulsar the emission is much more complex than previously seen: both very sharp edges and more diffuse emission are present. It has been postulated that one of the brightest filaments in Vela X is associated with the X-ray feature (called a `jet') which appears to be emanating from the region of the pulsar. However, an analysis of the MOST and VLA data shows that this radio filament has a flat spectral index similar to another more distant filament within the plerion, indicating that it is probably unrelated to the X-ray feature.
APA, Harvard, Vancouver, ISO, and other styles
3

Christou, J. C., G. Brusa, A. Conrad, S. Esposito, T. Herbst, P. Hinz, J. M. Hill, et al. "Adaptive optics capabilities at the Large Binocular Telescope Observatory." SPIE-INT SOC OPTICAL ENGINEERING, 2016. http://hdl.handle.net/10150/622008.

Full text
Abstract:
We present an overview of the current and future adaptive optics systems at the LBTO along with the current and planned science instruments they feed. All the AO systems make use of the two 672 actuator adaptive secondary mirrors. They are (1) FLAO (NGS/SCAO) feeding the LUCI NIR imagers/spectrographs; (2) LBTI/AO (NGS/SCAO) feeding the NIR/MIR imagers and LBTI beam combiner; (3) the ARGOS LGS GLAO system feeding LUCIs; and (4) LINO-NIRVANA - an NGS/MCAO imager and interferometer system. AO performance of the current systems is presented along with proposed performances for the newer systems taking into account the future instrumentation.
APA, Harvard, Vancouver, ISO, and other styles
4

De, Witt Aletha. "Radio astronomy techniques : the use of radio instruments from single dish radio telescopes to radio interferometers." Thesis, 2012. http://hdl.handle.net/10500/7046.

Full text
Abstract:
New radio telescopes under development, will significantly enhance the capabilities of radio astronomy in the Southern Hemisphere. South Africa, in particular, is actively involved in the development of a new array (MeerKAT) as well as in the expansion of existing very long baseline interferometer arrays in the south. Participation in these new developments demands a thorough understanding of radio astronomy techniques, and data analysis, and this thesis focusses on two projects with the aim of gaining such experience. The Southern Hemisphere very long baselines array is not well served with calibrator sources and there are significant gaps in the present calibrator distribution on the sky. An adequately dense, well distributed, set of strong, compact calibrator or reference sources is needed. With this in mind, observations using the Southern Hemisphere long baseline array were conducted to investigate a sample of candidate calibrator sources. The compactness of the sources was investigated and new potential calibrators have been identified. Single antenna radio spectroscopy of OH masers has identified sources of 1720 MHz emission associated with supernova remnants at the shock interface between the expanding supernova remnant and a molecular cloud. Models indicate that these masers are shock excited and can only be produced under tight physical constraints. Out ows from newly-formed stars create nebulous regions known as Herbig-Haro objects when they interact with the surrounding medium, and these regions are potentially similar to those seen in supernova remnants. If conditions behind the shock fronts of Herbig-Haro objects are able to support 1720-MHz OH masers they could be a useful diagnostic tool for star formation. A survey toward Herbig-Haro objects using a single-dish radio telescope did detect 1720-MHz OH lines in emission, but neither their spectral signature nor follow-up observations with the Very Large Array showed evidence of maser emission.
Mathematical Sciences
Ph.D. (Astronomy)
APA, Harvard, Vancouver, ISO, and other styles
5

Rodríguez, Kamenetzky Adriana Raquel. "Emisión no térmica y aceleración de partículas en jets protoestelares." Bachelor's thesis, 2018. http://hdl.handle.net/11086/11763.

Full text
Abstract:
Tesis (Doctor en Astronomía)--Universidad Nacional de Córdoba, Facultad de Matemática, Astronomía, Física y Computación, 2018.
Desde los primeros estudios realizados en radiofrecuencias en regiones de formación estelar, la emisión de jets de objetos estelares jóvenes (YSOs, por sus siglas en inglés) ha sido considerada exclusivamente de origen térmico. La presencia de una componente de emisión no térmica en jets protoestelares, constituye un descubrimiento reciente y sin dudas excepcional, que implica la existencia de partículas con velocidades relativistas en interacción con campos magnéticos. Explicar la presencia de tales partículas en estos sistemas, requiere la acción de un mecanismo responsable de incrementar eficientemente su energía cinética. El principal objetivo de esta Tesis es profundizar en la investigación de este interesante tópico. Para ello se estudió la emisión continua en radio de dos YSOs con distinta masa: (1) La fuente triple en radio continuo en Serpens (masa intermedia), el primer YSO para el cual ha sido propuesta la presencia de emisión sincrotrón y que, morfológicamente, puede considerarse el prototipo de jet protoestelar no térmico; (2) El sistema HH 80-81 (alta masa), uno de los jets protoestelares más potentes conocidos, y el único (hasta el momento) en que se ha detectado emisión centimétrica linealmente polarizada, confirmando el origen sincrotrónico de la radiación. En ambos casos, se realizaron estudios para caracterizar la naturaleza de la emisión en radio en distintas regiones del jet. Los resultados fueron analizados en el contexto de aceleración de partículas en choques del jet con el medio ambiente, explorando los posibles escenarios en que éstas podrían ser eficientemente aceleradas a energías relativistas. El estudio de estos objetos fue abordado en un amplio rango de longitudes de onda de radio, mediante el análisis de nuevos datos de alta sensitividad obtenidos con interferómetro Karl G. Jansky Very Large Array (VLA) del National Radio Astronomy Observatory (NRAO).
Since the first studies of star formation regions at radio frequencies, the emission of jets powered by young stellar objects (YSOs) has been exclusively considered of thermal origin. The presence of a non thermal component in the radio emission of these jets constitutes a recent discovery with very importan implications, such as the existence of particles with relativistic velocity interacting with magnetic fields. The existence of relativistic particles in these low energy systems requires the action of a mechanism able to efficiently increase their kinetic energy. The main goal of this Thesis is to deepen the study of this interesting topic. For this purpose we studied the radio continuum emission of two representative YSOs having different masses: (1) The triple source in Serpens (intermediate mass), known to be first YSO for which the presence of synchrotron radiation has been proposed, and morphologically considered as a prototype of non-thermal jets; (2) The system HH 80-81 (high mass), being one of the most powerful protostellar jets known, and the only one (to date) for which linearly polarized centimeter emission has been detected, thus confirming the synchrotronic origin of the radiation. In both cases, studies were conducted to characterize the nature of the radio emission in different regions of the jet. The results were analyzed in the context of particle acceleration in the shocks of the jet with the environment, exploring possible scenarios to accelerate particles up to relativistic energies. We addressed the study of these objects through the analysis of new high sensitivity data obtained with the Karl G. Jansky Very Large Array (VLA) interferometer from the National Radio Astronomy Observatory (NRAO), in a wide range of radio wavelengths.
APA, Harvard, Vancouver, ISO, and other styles

Books on the topic "Interferometers telescopes stars"

1

Gladis, Magris, Bruzual-Alfonzo Gustavo Ramon, Carigi Leticia, and International Astronomical Union, eds. XII IAU Regional Latin American Meeting: Isla Margarita, Venezuela, octubre 22-26, 2007. México, D.F: Instituto de Astronomía, UNAM, 2009.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
2

Latin American Regional Meeting of Astronomy (12th 2007 Margarita Island, Venezuela). XII IAU Regional Latin American Meeting: Isla Margarita, Venezuela, octubre 22-26, 2007. Edited by Magris Gladis, Bruzual-Alfonzo Gustavo Ramon, Carigi Leticia, and International Astronomical Union. México, D.F: Instituto de Astronomía, UNAM, 2009.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
3

1940-, Paresce Francesco, ed. Science with the VLT Interferometer: Proceedings of the ESO workshop held at Garching, Germany, 18-21 June 1996. Berlin: Springer, 1997.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
4

Magnetic fields in the universe II: From laboratory and stars to the primordial universe : Cozumel, Quintana Roo, México, enero 28-febrero 1, 2008. México, D. F: Instituto de Astronomía, Universidad Nacional Autónoma de México, 2009.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
5

A, Esquivel, and Universidad Nacional Autónoma de México. Instituto de Astronomía., eds. Magnetic fields in the universe II: From laboratory and stars to the primordial universe : Cozumel, Quintana Roo, México, enero 28-febrero 1, 2008. México, D. F: Instituto de Astronomía, Universidad Nacional Autónoma de México, 2009.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
6

Erika, Benítez, Cruz-Gonzalez Irene, Krongold Yair, and Universidad Nacional Autónoma de México. Instituto de Astronomía., eds. The nuclear region, host galaxy and environment of active galaxies: Huatulco, Oaxaca, México, abril 18-20, 2007. México, D.F: Instituto de Astronomí́a, Universidad Nacional Autónoma de México, 2008.

Find full text
APA, Harvard, Vancouver, ISO, and other styles
7

Paula, Benaglia, Bosch Guillermo 1968-, Cappa Cristina, Niemela Virpi, and Universidad Nacional Autónoma de México. Instituto de Astronomía., eds. Massive stars: Fundamental parameters and circumstellar interactions : Cariló, Buenos Aires, Argentina, diciembre 11-14, 2006. México, D.F: Instituto de Astronomía, Universidad Nacional Autónoma de México, 2008.

Find full text
APA, Harvard, Vancouver, ISO, and other styles

Book chapters on the topic "Interferometers telescopes stars"

1

Lane, Benjamin F. "Pulsating Stars." In The Very Large Telescope Interferometer Challenges for the Future, 177–83. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_20.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Richichi, Andrea, and Markus Wittkowski. "First VLTI Observations of Mira Stars." In The Very Large Telescope Interferometer Challenges for the Future, 219–24. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_25.

Full text
APA, Harvard, Vancouver, ISO, and other styles
3

Haniff, Christopher. "Imaging Stars and Their Environments with the VLTI." In The Very Large Telescope Interferometer Challenges for the Future, 163–70. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_18.

Full text
APA, Harvard, Vancouver, ISO, and other styles
4

Niedzielski, A. "The Wolf-Rayet Stars at High (Spatial) Resolution." In The Very Large Telescope Interferometer Challenges for the Future, 237–44. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_27.

Full text
APA, Harvard, Vancouver, ISO, and other styles
5

Dougados, C., J. Bouvier, G. Duvert, P. J. V. Garcia, and D. F. M. Folha. "Probing the Magnetosphere in Young Stars with AMBER/VLTI." In The Very Large Telescope Interferometer Challenges for the Future, 151–56. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_16.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Perrin, Guy. "Interferometry: The Tool to Study Giant, Supergiant and Mira Stars." In The Very Large Telescope Interferometer Challenges for the Future, 197–212. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_23.

Full text
APA, Harvard, Vancouver, ISO, and other styles
7

Correia, S., A. Richichi, and M. Schöller. "Prospects of High Angular Resolution Measurements of Binary Stars Properties with VLTI." In The Very Large Telescope Interferometer Challenges for the Future, 191–96. Dordrecht: Springer Netherlands, 2003. http://dx.doi.org/10.1007/978-94-017-0157-0_22.

Full text
APA, Harvard, Vancouver, ISO, and other styles
8

Cottrell, Geoff. "7. The radio sky." In Telescopes: A Very Short Introduction, 77–95. Oxford University Press, 2016. http://dx.doi.org/10.1093/actrade/9780198745860.003.0007.

Full text
Abstract:
‘The radio sky’ considers radio telescopes that can see much longer wavelengths. Cosmic radio waves were first discovered in 1932 by Karl Jansky, with the first radio telescope built in 1937. Technology for radar systems advanced during World War II and then after the war scientists, such as Bernard Lovell and Martin Ryle, made use of the advances in electronics, radio technology, and digital computers, to found radio astronomy. Single-dish antennas—including the Lovell Telescope at Jodrell Bank Observatory—continue to play important roles. To improve angular resolution two antennas need to be operated as an interferometer. These are described along with the discovery of quasars, supermassive black holes, pulsars, and neutron stars.
APA, Harvard, Vancouver, ISO, and other styles
9

Breckinridge, James B., Alec M. Pridgeon, and Donald E. Osborn. "In Space at Last." In With Stars in Their Eyes, 407–46. Oxford University Press, 2022. http://dx.doi.org/10.1093/oso/9780190915674.003.0012.

Full text
Abstract:
This chapter discusses how Aden and Marjorie Meinel were hired at NASA/JPL and their contributions in six major areas: (1) the large deployable reflector system study to create technology fundamental to the James Webb Space Telescope; (2) the Thousand Astronomical Unit (TAU) mission to make high-precision, fundamental measurements of the distance from Earth to most objects in this galaxy; (3) space optical systems for the detection and characterization of exoplanets; (4) interferometry to recover images across the surface of stars, measure precision stellar motions, and reveal details of planetary formation and evolution; (5) repair of the Hubble Space Telescope; and (6) the ground-based Advanced Electro Optical System (AEOS) telescope of the Air Force. The chapter ends with the awards Aden and Marjorie both received and their deaths in 2011 and 2008, respectively.
APA, Harvard, Vancouver, ISO, and other styles
10

Moffat, John W. "Origins of Gravitational Waves and Detectors." In The Shadow of the Black Hole, 88–107. Oxford University Press, 2020. http://dx.doi.org/10.1093/oso/9780190650728.003.0006.

Full text
Abstract:
Civita criticized Einstein’s papers on gravitational waves: their energy momentum is frame dependent and therefore does not fit the covariance of Einstein’s gravity theory. Infeld and Rosen did not believe gravitational waves existed, and Einstein changed his mind on their existence repeatedly. Others did believe in them, such as Fock and Feynman. Weber constructed his “Weber bar” to detect gravitational waves, but when he claimed success, he was criticized. He then proposed using a Michelson-Morley type of interferometer with lasers to detect gravitational waves, as did Weiss. Merging black holes and neutron stars were proposed as detectable sources of gravitational waves. Taylor and Hulse, using the large Arecibo radio telescope, indirectly detected gravitational waves from inspiraling neutron stars. Primordial gravitational waves, still emanating from the Big Bang, were claimed to have been detected by BICEP2, but the waves were eventually shown to be a result of foreground dust.
APA, Harvard, Vancouver, ISO, and other styles

Conference papers on the topic "Interferometers telescopes stars"

1

Shulyak, D., K. Perraut, Claudia Paladini, G. Li Causi, Stephane Sacuto, and O. Kochukhov. "Analysis of surface structures of chemically peculiar stars with modern and future interferometers." In SPIE Astronomical Telescopes + Instrumentation, edited by Jayadev K. Rajagopal, Michelle J. Creech-Eakman, and Fabien Malbet. SPIE, 2014. http://dx.doi.org/10.1117/12.2055555.

Full text
APA, Harvard, Vancouver, ISO, and other styles
2

Loos, G. C. "On The Implementation Of Adaptive Optics For Improving Broadband Spectral Response In Michelson Interferometry." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.atub2.

Full text
Abstract:
Beginning with the experiments by Michelson in the 1920's and continuing with more recent research activities around the world Michelson interferometry has evolved into a powerful tool for measuring the diameters of giant stars and separations and orbits of multiple star systems. This paper offers calculations of the wavelength dependent limiting sensitivity achievable using a two aperture interferometer, without or with partial adaptive optics corrections, based upon realistic assumptions in regard to system noise sources. Results are presented for the case of observing resolved stars characterized as spectral type G2V, the spectral classification of the sun.
APA, Harvard, Vancouver, ISO, and other styles
3

Greenaway, A. H. "The role of adaptive optics in long-baseline interferometry." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.atua5.

Full text
Abstract:
To obtain, at optical frequencies, even crude images of some stars of most spectral types an instrument of several hundred metres in diameter is required [1]. A single optical telescope of this diameter is unlikely to be constructed in the foreseeable future, either on the ground or in space. Thus to obtain images of the surfaces of a significant number of stars other than the sun an interferometric instrument, consisting of several separate telescopes, will need to be used. The processes by means of which an image may be synthesized from such an instrument have been reviewed recently [2]. Here the use of adaptive optics to improve the sensitivity of such an array will be considered.
APA, Harvard, Vancouver, ISO, and other styles
4

Wizinowich, P., D. S. Acton, A. Gleckler, T. Gregory, P. Stomski, K. Avicola, J. Brase, H. Friedman, D. Gavel, and C. Max. "W.M. Keck Observatory Adaptive Optics Facility." In Adaptive Optics. Washington, D.C.: Optica Publishing Group, 1996. http://dx.doi.org/10.1364/adop.1996.amb.1.

Full text
Abstract:
The W.M. Keck Observatory, in collaboration with Lawrence Livermore National Laboratory (LLNL), is currently in the critical design phase of a natural guide star (NGS) and single laser guide star (LGS) adaptive optics (AO) user facility for the Nasmyth platform of the Keck II 10-m telescope.1 Two science instruments will accompany the AO facility: a near infrared camera (NIRC-2) being built at Caltech, and a near infrared spectrometer (NIRSPEC) being built at UCLA. NASA is planning to fund an interferometer between the Keck telescopes which will require a second NGS AO facility on Keck I.
APA, Harvard, Vancouver, ISO, and other styles
5

Hofmann, Karl-Heinz, Udo Beckmann, Thomas Bloecker, Vincent Coude du Foresto, Marc G. Lacasse, Rafael Millan-Gabet, Sebastien Morel, et al. "Observations of MIRA stars with the IOTA/FLUOR interferometer and comparison with MIRA star models." In Astronomical Telescopes and Instrumentation, edited by Pierre J. Lena and Andreas Quirrenbach. SPIE, 2000. http://dx.doi.org/10.1117/12.390270.

Full text
APA, Harvard, Vancouver, ISO, and other styles
6

Kervella, Pierre, Frederic Thevenin, Damien Segransan, and Emmanuel Di Folco. "Main sequence stars as calibrators for interferometry." In SPIE Astronomical Telescopes + Instrumentation, edited by Wesley A. Traub. SPIE, 2004. http://dx.doi.org/10.1117/12.550793.

Full text
APA, Harvard, Vancouver, ISO, and other styles
7

Gavel, Donald T., Herbert W. Friedman, and Scot S. Olivier. "Wide-baseline optical interferometry with laser guide stars." In Astronomical Telescopes & Instrumentation, edited by Robert D. Reasenberg. SPIE, 1998. http://dx.doi.org/10.1117/12.317147.

Full text
APA, Harvard, Vancouver, ISO, and other styles
8

Horch, Elliott P., Nicole M. Hess, Patrick R. Thayer, James W. Davidson, Brian W. Baptista, Mark E. Everett, and Steve B. Howell. "Speckle imaging of KOI binary stars with the WIYN telescope." In Optical and Infrared Interferometry and Imaging VI, edited by Antoine Mérand, Michelle J. Creech-Eakman, and Peter G. Tuthill. SPIE, 2018. http://dx.doi.org/10.1117/12.2313008.

Full text
APA, Harvard, Vancouver, ISO, and other styles
9

Andersen, Johannes. "Binary star science with interferometry." In Astronomical Telescopes and Instrumentation, edited by Wesley A. Traub. SPIE, 2003. http://dx.doi.org/10.1117/12.456749.

Full text
APA, Harvard, Vancouver, ISO, and other styles
10

Vernon, R. G. "Real-Time Corrected Long Baseline Interferometer System Concept." In Adaptive Optics for Large Telescopes. Washington, D.C.: Optica Publishing Group, 1992. http://dx.doi.org/10.1364/aolt.1992.pd10.

Full text
Abstract:
A design concept and analyis for a long baseline interferometer imaging system that uses real-time higher order wavefront control, tilt and piston control has been developed to: (1) stabilize the fringe field associated with the visibility phases, (2) measure visibility amplitudes and closure phase, and (3) allow investigation of celestial sources beyond 15th magnitude. Pupil plane phase difference control and closure phase measurement on three telescopes is accomplished simultaneously using differential phase modulation and Fourier de composition. Atmospheric wavefromt sensing is accomplished in all three telescopes using Rayleigh scattered 15 watt laser guide stars focused at 20 km. Tilt sensing and correction is accomplished using the imaged source field. A method for obtaining good pupil plane coverage using only three 1 meter apertures is presented. Analysis is performed on the adaptive optics assemblies to trade-off laser guide star power requirements, optical train efficiency, wavefront sensor measuring accuracy, track sensor accuracy, number of wavefront sensor subapertures, deformable mirror actuators and servo bandwidth requirements. Analysis is performed on the piston control subsystem to optimize the measurement of closure phase and visibility amplitude over a narrow spectral bandwidth, to trade-off source irradiance requirements, piston measuring accuracy, and visibility amplitude accuracy.
APA, Harvard, Vancouver, ISO, and other styles
You might also be interested in the extended bibliographies on the topic 'Interferometers telescopes stars' for particular source types:
Journal articles
We offer discounts on all premium plans for authors whose works are included in thematic literature selections. Contact us to get a unique promo code!

To the bibliography