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Littérature scientifique sur le sujet « Astronomical spectroscopy »

Auteur : Grafiati

Publié le 4 juin 2021

Mis à jour le 29 juillet 2024

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Articles de revues sur le sujet "Astronomical spectroscopy"

1

Bhattacharyya, J. C. « Astronomical spectroscopy ». Resonance 3, n^o 5 (mai 1998) : 24–29. http://dx.doi.org/10.1007/bf02838839.

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Bhattacharyya, J. C. « Astronomical spectroscopy ». Resonance 3, n^o 6 (juin 1998) : 16–24. http://dx.doi.org/10.1007/bf02836981.

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Miller, David J. « Astronomical spectroscopy : an introduction to the atomic and molecular physics of astronomical spectroscopy ». Contemporary Physics 61, n^o 4 (1 octobre 2020) : 304. http://dx.doi.org/10.1080/00107514.2020.1853241.

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Panchuk, V. E., M. E. Sachkov, M. V. Yushkin et M. V. Yakopov. « Integral methods in astronomical spectroscopy ». Astrophysical Bulletin 65, n^o 1 (janvier 2010) : 75–94. http://dx.doi.org/10.1134/s1990341310010074.

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Allamandola, L. J. « Grain Spectroscopy ». Symposium - International Astronomical Union 150 (1992) : 65–72. http://dx.doi.org/10.1017/s0074180900089725.

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Our fundamental knowledge of interstellar grain composition has grown substantially during the past two decades thanks to significant advances in two areas: astronomical infrared spectroscopy and laboratory astrophysics. The opening of the mid-infrared, the spectral range from 4000-400 cm−1 (2.5-25 μm), to spectroscopic study has been critical to this progress because spectroscopy in this region reveals more about a material's molecular composition and structure than any other physical property.

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Odeh, Mohammad Sh. « Low cost equipment for astronomical spectroscopy ». Journal of Instrumentation 16, n^o 12 (1 décembre 2021) : T12009. http://dx.doi.org/10.1088/1748-0221/16/12/t12009.

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Abstract The purpose of this paper is to show how we can obtain spectra for different astronomical objects using low coat equipment. Where a high-efficiency diffraction grating named “The Star Analyzer” was used by the International Astronomical Center (IAC) in Abu Dhabi, UAE to get the spectrum of different astronomical objects. Balmer series was readily visible when observing an “A” type star. TiO absorptions lines were distinguished by observing an “M” type star. Methane absorption lines were visible by observing Uranus and Neptune. Whereas HI and HeI emission lines were detected by observing a blue hypergiant. In addition, C2 Swan band absorption lines were identified by observing a red giant carbon star. This type of observation is very interesting for public outreach as well as university students, because it shows astrophysical principles for public and students practically and by using low cost equipment.

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Hentschel, Klaus. « Updating a handbook on astronomical spectroscopy ». Journal for the History of Astronomy 46, n^o 2 (mai 2015) : 242–43. http://dx.doi.org/10.1177/0021828614552243.

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Glaspey, John W., et Ian Powell. « A camera for astronomical CCD spectroscopy ». Publications of the Astronomical Society of the Pacific 100 (octobre 1988) : 1282. http://dx.doi.org/10.1086/132317.

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DEVORKIN, D. « Astronomical Spectroscopy : The Analysis of Starlight. » Science 237, n^o 4816 (14 août 1987) : 783–84. http://dx.doi.org/10.1126/science.237.4816.783-a.

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Martin-Drumel, M. A., K. L. K. Lee, A. Belloche, O. Zingsheim, S. Thorwirth, H. S. P. Müller, F. Lewen et al. « Submillimeter spectroscopy and astronomical searches of vinyl mercaptan, C2H3SH ». Astronomy & ; Astrophysics 623 (mars 2019) : A167. http://dx.doi.org/10.1051/0004-6361/201935032.

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Context. New laboratory investigations of the rotational spectrum of postulated astronomical species are essential to support the assignment and analysis of current astronomical surveys. In particular, considerable interest surrounds sulfur analogs of oxygen-containing interstellar molecules and their isomers. Aims. To enable reliable interstellar searches of vinyl mercaptan, the sulfur-containing analog to the astronomical species vinyl alcohol, we investigated its pure rotational spectrum at millimeter wavelengths. Methods. We extended the pure rotational investigation of the two isomers syn and anti vinyl mercaptan to the millimeter domain using a frequency-multiplication spectrometer. The species were produced by a radiofrequency discharge in 1,2-ethanedithiol. Additional transitions were remeasured in the centimeter band using Fourier-transform microwave spectroscopy to better determine rest frequencies of transitions with low-J and low-Ka values. Experimental investigations were supported by quantum chemical calculations on the energetics of both the [C2,H4,S] and [C2,H4,O] isomeric families. Interstellar searches for both syn and anti vinyl mercaptan as well as vinyl alcohol were performed in the EMoCA spectral line survey carried out toward Sgr B2(N2) with ALMA. Results. Highly accurate experimental frequencies (to better than 100 kHz accuracy) for both syn and anti isomers of vinyl mercaptan are measured up to 250 GHz; these deviate considerably from predictions based on extrapolation of previous microwave measurements. Reliable frequency predictions of the astronomically most interesting millimeter-wave lines for these two species can now be derived from the best-fit spectroscopic constants. From the energetic investigations, the four lowest singlet isomers of the [C2,H4,S] family are calculated to be nearly isoenergetic, which makes this family a fairly unique test bed for assessing possible reaction pathways. Upper limits for the column density of syn and anti vinyl mercaptan are derived toward the extremely molecule-rich star-forming region Sgr B2(N2) enabling comparison with selected complex organic molecules.

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Thèses sur le sujet "Astronomical spectroscopy"

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Tulloch, Simon. « Astronomical spectroscopy with electron multiplying CCDs ». Thesis, University of Sheffield, 2010. http://ethos.bl.uk/OrderDetails.do?uin=uk.bl.ethos.522382.

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Shaw, Graham David. « New techniques in astronomical multi-slit spectroscopy ». Thesis, Durham University, 1993. http://etheses.dur.ac.uk/5643/.

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LDSS-2 is a low dispersion survey spectrograph for the William Herschel Telescope. It was constructed to meet an increasing demand for large scale statistical surveys of stellar and galactic populations. This thesis describes its design, construction and installation, together with additional research concerning the fabrication of multi-slit aperture masks.LDSS-2 has a similar optical system to its predecessor LDSS-1, but it can hold greater numbers of aperture masks, filters and grisms, and its control system is fully automated. This is expected to improve its observing efficiency and allow LDSS-2 to be run as a common-user instrument. A range of instrument characterisation tests were performed, and they confirmed that LDSS-2 is capable of meeting its astronomical objectives. Its peak efficiency with the medium-blue grism was found to be 20.4% at 5915A with half-power points at 4135A and 7225A.Six different types of aperture mask were investigated, of which two (photochemically etched and mechanically milled) were tested using LDSS- 2. Work was begun towards the development of laser-cut masks, including the procurement of a 16W carbon dioxide laser and a motorised X-Y table. At present, mechanically milled masks offer the best compromise between cost, lead time, flexibility and quality for an instrument such as LDSS-2. Movable-slit masks may be preferred if access to the focal plane is restricted, but at present they are limited to lower multiplex gains. Laser-cut masks appear to offer the most potential for development in the immediate future, but liquid crystal masks may also become competitive in the longer term.

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Watson, Frederick Garnett. « Multi-object astronomical spectroscopy with optical fibres ». Thesis, University of Edinburgh, 1987. http://hdl.handle.net/1842/27619.

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A full account is given of the relatively new astronomical technique of multi- object spectroscopy with optical fibre lightguides. The thesis begins with a survey of the number densities of a wide range of astronomi- cal object classes, and, after comparing the merits of the various techniques for multi- object spectroscopy, shows (by defining the "effective aperture" of a multiple fibre - coupled telescope) that the multi -fibre tech- nique is very well- suited to the real distribution of celestial objects. A review of the properties of optical fibres is given, together with an exposition of the important considerations in the design of fibre feeds for astronomy. This is followed by a description of the requirements in the design of telescopes, spectrographs and detectors to render them suitable for the multi -fibre technique. Equations are derived for the performance of these systems in terms of signal -to -noise ratio, and an example is given. A survey of the equipment that has been built for multi -fibre spectroscopy at observatories throughout the world is presented, and special attention is paid to the FOCAP fibre system at the 3.9 -metre Anglo- Australian tele- scope. The thesis gives an example of the use of FOCAP in work carried out by the writer to investigate the kinematics of RR Lyrae variables in the nuclear bulge of the Galaxy. Evidence is found in the preliminary results for the existence of non -circular motions along the galactic centre line -of- sight. A description is then given of the FLAIR wide -field fibre -coupled multi- object spectroscopy system built by the writer for the 1.2 -metre UK Schmidt Telescope. Reports are presented on a series of observational pro- grammes designed to test the system, including the classification of stars in the Chamaeleon dark cloud, spectroscopy of Orion cluster flare stars, spectroscopy of objects in the Large Magellanic Cloud, the measurement of galaxy redshifts, and the observation of quasar candidates. An experiment in time -resolved multi- object photometry is also described. It is shown that for spectroscopy, the prototype system will perform well on stellar targets to V "16 -17, but, although galaxy redshifts have been obtained, its usefulness for the systematic measurement of redshifts is hampered by its low sensitivity in the blue region of the spectrum. An account is then given of the relatively simple steps needed to rectify this, together with a brief description of a proposed, fully- optimised FLAIR system. Finally, the future prospects for multi -fibre astronomical spectroscopy are briefly reviewed, from the point of view of the new instrumentation becoming available, and the astronomical results that will be produced.

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Haynes, Roger. « Infrared fibres in astronomical instrumentation ». Thesis, Durham University, 1995. http://etheses.dur.ac.uk/5402/.

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For several years multi-object spectroscopy systems have been available for carrying out survey work in the visible region, but until very recently there has not been a system for the near infrared region. This thesis describes the design, manufacture and commissioning of the first multi-object fibre system for near infrared spectroscopy. SMIRFS (Spectroscopic Multi-object Infrared Fibre System) is a prototype system that has been designed at the Department of Physics in Durham to couple the Cassegrain focus of the United Kingdom InfraRed Telescope (UKIRT) to a cooled long slit infrared spectrograph (CGS4). Two different fibre bundles are available, each containing 14 fibres. One bundle is made from zirconium fluoride fibres, for K band spectroscopy and the second bundle is made from silica fibres, for J and H band spectroscopy. During the design process of SMIRFS a number of issues were addressed. These included; the characteristics of infrared fibres, in particular their throughput and FRD, atmospheric features in the near infra-red and suitable sky subtraction techniques, fibre preparation and evaluation, the use of microlenses for coupling slow focal ratio beams with fibres, and the thermal emissions from the warm material of the instrument. These, along with the design, manufacture and testing of the SMIRFS are described in detail, including the fibre evaluation results and estimates for throughput, instrument thermal background derived from the commissioning run data. Finally, there is a brief discussion on the development of infrared fibre system for astronomy.

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Porter, Martin John. « A CCD camera system for use in echelle spectroscopy / ». St. Lucia, Qld, 2004. http://www.library.uq.edu.au/pdfserve.php?image=thesisabs/absthe17953.pdf.

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Carrasco, Bertha Esperanza. « Further developments of optical fibre techniques for astronomical spectroscopy ». Thesis, Durham University, 1992. http://etheses.dur.ac.uk/6029/.

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This thesis describes instrumental techniques pursued to optimise the quality of the spectroscopic data which will be obtained via the new generation of multifibre systems. The technical aspects discussed include the instrumental sources of systematic errors on sky subtraction and new methods to evaluate the fibre performance in terms of throughput and preservation of the input focal ratio. The limiting factor in faint multifibre spectroscopy is the accuracy and reliability of sky subtraction. Instrumentality the precision to which sky subtraction can be done is limited by systematic errors. The conditions that have to be satisfied to subtract the sky properly at faint levels, the sources of errors and possible ways of eliminating them are analysed. A comprehensive discussion of the effect of deficient wavelength sampling and of poor fibre flatfield calibration on sky subtraction is provided via computer simulations of fibre data. Several laboratory fibre evaluation techniques and data processing software packages have been developed. These techniques have been used to measure the through put of silica fibres at optical wavelengths. Also presented in this thesis are preliminary results obtained from a series of experiments implemented at infrared wavelengths. As a result of these developments a new method for determining the focal ratio degradation (FRD), based on a known theoretical model for microbending induced beam- spreading is proposed. This theory characterises the FRD by a single parameter which can be determined by a very simple experiment. The model successfully predicts real experimental results. This new technique will allows us to accurately model the complete performance of any fibre. Such modelling can include complicated phenomena such as tilted input beams and central obstructions without the need to setup experiments for specific cases. Furthermore, it can be used to evaluate the performance of infrared fibres. Finally, the results of an exhaustive laboratory evaluation of the Autofib-1.5 fibre bundle are presented. The evaluation was carried out after a multiway fibre connector prototype was incorporated into the Autofib-1.5 fibre bundle, with the emphasis being placed on the performance of the connector.

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Lee, David. « New techniques in astronomical spectroscopy for 8-m telescopes ». Thesis, Durham University, 1998. http://etheses.dur.ac.uk/4847/.

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The purpose of this thesis is to investigate new instrument technology to enhance the capabilities of 8-m telescopes. This thesis first describes the theory, design, construction, and testing of an immersed grating. Immersed gratings can be used to provide R≥ 10(^4) with a multi-object and/or integral field spectrograph on an 8-m telescope. Immersed gratings allow high resolution to be achieved whilst maintaining the required pupil size at a level similar to that on 4-m telescopes. This thesis describes laboratory tests which verify that immersed gratings provide high resolution. The throughput penalty in using an immersed grating is shown to be small with losses due to air-glass reflections, which can be eliminated with antireflection coatings, and metal-dielectric losses. This work demonstrates that immersed gratings provide a good method to reach R=10(^4) (and above) with a multi-aperture spectrograph on an 8-m telescope. The second part of this thesis describes the construction of a microlens-fibre based integral field unit (IFU): the SMIRFS-IFU. This instrument provides a unique J and H-band integral field capability for use with the CGS4 spectrograph at UKIRT. The optical design, assembly, laboratory testing, and telescope commissioning of the SMIRFS-IFU are described. The microlens arrays for use with SMIRFS-IFU were tested in detail and found to provide excellent image quality but with some scattered light. The assembly of the SMIRFS-IFU was achieved with high precision. The overall performance of the SMIRFS-IFU was found to be high and close to theoretical expectations. This instrument demonstrates that the technology of microlenses linked to fibres does provide a means of constructing high performance (i.e. high throughput, high spatial and spectral resolution) IFUs. Integral field spectroscopy is even more important for 8-m telescopes to take advantage of their enormous fight gathering power. The SMIRFS-IFU is an important upgrade to CGS4 to perform high spatial resolution integral field spectroscopy.

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Clampin, Mark. « Investigation of a resistive anode detector for astronomical spectroscopy ». Thesis, University of St Andrews, 1986. http://hdl.handle.net/10023/7110.

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A large format two dimensional photon counting detector has been evaluated as a detector for astronomical spectroscopy. The design comprises an 320 photocathode, a tandem MCP gain stage and a circular arc terminated resisitive anode to provide pOSitional coordinates of detected events. The system is run from an LSI 11/23 computer operating under FORTH control. The micro-channel plate operating characteristics and the detector's resolution, quantum efficiency and imaging performance have been studied. The principal areas requiring design improvement are found to be the micro-channel plate gain, processing and photocathode quality. electronic signal The detector has been employed in a observing program on a 0.5 m telescope. Spectra of IAU faint radial velocity standards and the eclipsing binary system s-l Cam have been obtained and analysed to assess the system's performance.

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Oates, Anthony Patrick. « A technique for astronomical spectroscopy with a multi-aperture telescope ». Thesis, University of Central Lancashire, 1985. http://clok.uclan.ac.uk/19078/.

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A technique for acquiring spectral line data using a multi-aperture telescope is described. The multi-aperture principle and the criteria which led to the selection of a dispersive spectrometer are discussed. The problem of linking telescope and spectrometer has been solved by incorporating low loss optical fibres and this is also discussed. The problems of automatic data collection, its manipulation, display and storage presented a major research effort which were largely overcome by the use of cheap, digital micro-computers. To achieve rapid and flexible data handling the i.E.E.E. bus was used as the communication medium between control and data collecting micro-computers. In particular a non-standard approach was adopted when implementing specialised interrupt handling routines to deal with data communication, an aspect which forms the central theme of this thesis and is described in chapters three to five inclusive. A discussion relating to data obtained using the system in single fibre mode and to RPCS data obtained at intermediate resolution is presented in chapters six and seven respectively. The former permitted a preliminary determination to be made of both system resolution and the approximate integration times required to undertake a program of stellar emission line work. This is complimentary to that described in the final chapter which discusses the spectra of emission line stars, some of which are accompanied by circumstellar 'shells'. For pre-main sequence stars these shells may ultimately provide conditions favourable for the formation of planetary systems. There are examples of these types of stars to be found in the Northern hemisphere and which are within the detection limit of the system described in this thesis.

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Bounissou, Sophie. « ”On-chip” astronomical instrumentation : bringing polarimetric and spectroscopic capabilities to the detector level ». Thesis, Université Paris-Saclay (ComUE), 2019. http://www.theses.fr/2019SACLS400.

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Cette thèse étudie la possibilité d'intégrer plusieurs fonctions instrumentales au sein de la matrice de bolomètres pour les observations dans le domaine du sub-millimétrique. Ceci est désormais envisageable grâce aux progrès des micro-technologies.Dans un premier temps, nous avons optimisé le design des pixels polarimétriques inventés pour l'instrument B-BOP du futur observatoire spatial SPICA. Ce travail a notamment permis de quantifier la cross-polarisation (1/1000) et de repenser la géométrie des pixels afin d'obtenir des détecteurs mieux adaptés au rayonnement incident.Cette thèse a également été l'occasion, et ce de manière indépendante à la polarimétrie, de réfléchir à l'intégration de la spectroscopie au sein du plan focal. Pour cela, nous nous sommes orientés vers de l'interférométrie de type Fabry Pérot (FP). Un FP dans un faisceau collimaté présente l'avantage d'être très facilement compatible avec l'imagerie. Toutefois, nous avons choisi d'intégrer le spectromètre au plus près du détecteur (et donc dans le faisceau convergent). Nous avons également initié le développement de FP tout silicium (Si) à haute résistivité afin de réduire les pertes dûes aux miroirs métalliques, conventionnellement utilisés dans nos gammes de longueurs d'onde. Afin d'améliorer les performances spectrales du FP, les miroirs sont fabriqués via un empilement de couches de silicium interposés de vide tels des miroirs de Bragg. Cela permet d'augmenter rapidement le coefficient de réflexion des miroirs sans toutefois en augmenter trop la complexité: une finesse de 215 est, par exemple, attendue à 320 µm pour un FP utilisant des miroirs Si/vide/Si. Ensuite, nous avons étudié le couplage détecteur/FP qui se voit renforcé par la résonance des deux cavités optiques formées par le système complet. Enfin, des calculs ont montré qu'un FP avec une finesse raisonnable (150) mis dans le plan focal ne dégrade que très peu l'imagerie et la spectroscopie.A la fin de cette thèse, plusieurs étalons FP ont été réalisés et ont déjà démontré des propriétés intéressantes: une résolution spectrale de 180 a notamment été obtenue. En plus de cela, les mesures ont montré que le silicium avait une absorption négligeable à 77 K
This thesis assesses the potential of gathering several instrumental functions into a bolometer array for sub-millimetric astronomical observations. This possibility is now conceivable thanks to the recent progress made in micro-technologies.First, we optimized the design of polarimetric pixels invented for the B-BOP instrument of the future space observatory SPICA. This work enabled the quantification of the cross-polarization (1/1000) and to rethink the geometry of the pixels in order to obtain detectors better matched to incident radiation.This thesis has also been an opportunity to deal with the integration of spectroscopy within the focal plane, independently from the polarimetry aspect. We accordingly focused on Fabry-Pérot (FP) interferometry, as an FP in a collimated beam can well-suited for imaging. Nonetheless, we chose to integrate the spectrometer closer to the detector (and thus in the convergent beam). We also initiated the development of an FP made from high-resistivity silicon in order to lower the losses due to metallic mirrors, generally used in this range of wavelengths. With the objective to enhance the spectral capabilities of the FP, mirrors are built as a stack of silicon layers, separated by vacuum (Bragg mirrors). This increases the reflectivity of the mirrors while keeping the complexity to a reasonable level : a finesse of 215, for instance, is expected at 320 µm for a FP using Si/vacuum/Si mirrors. As a next step, we studied the detector/FP coupling which is enhanced by the resonance of two optical cavities formed by the whole system. Eventually, calculations showed that an FP with a moderate finesse (150) put in the focal plane barely deteriorates imaging or spectroscopy.By the end of this thesis, several FP etalons have been built and have already demonstrated favorable properties: we obtained a spectral resolution of 180. Moreover, measurements showed that silicon has a negligible absorption at a temperature of 77 K

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Livres sur le sujet "Astronomical spectroscopy"

1

Kitchin, C. R. Optical astronomical spectroscopy. Bristol : Institute of Physics Pub., 1995.

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2

Harrison, Ken M. Astronomical Spectroscopy for Amateurs. New York, NY : Springer New York, 2011. http://dx.doi.org/10.1007/978-1-4419-7239-2.

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3

David, Emerson. Interpreting astronomical spectra. Chichester : J. Wiley & Sons, 1996.

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4

Hadrava, Petr. Stellar spectroscopy at Ondřejov Observatory. Ondřejov : Astronomical Institute of the Academy of Sciences of the Czech Republic, 2004.

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5

S, Kwok, dir. Astronomical infrared spectroscopy : Future observational directions. San Francisco, Calif : Astronomical Society of the Pacific, 1993.

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6

Derviz, T. E. Astronomicheskie spektrografy : Uchebnoe posobie. Leningrad : Leningradskiĭ universitet, 1985.

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7

D, Garmany C., Joint Institute for Laboratory Astrophysics, University of Colorado, Boulder. Dept. of Astrophysical, Planetary, and Atmospheric Sciences et United States. National Aeronautics and Space Administration, dir. Spectroscopic observations of selected stellar systems. Boulder, Colo : Joint Institute for Laboratory Astrophysics, 1985.

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8

Torres, Rafael Escribano. Spectroscopy of the atmospheres. Madrid : Consejo Superior de Investigaciones Científicas, 2010.

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9

A, Dalgarno, et Layzer David, dir. Spectroscopy of astrophysical plasmas. Cambridge, CB : Cambridge University Press, 1987.

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10

Observatory, Anglo-Australian, dir. The UCL Echelle spectograph. Epping, N.S.W : Anglo-Australian Observatory, Epping Laboratory, 1989.

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Chapitres de livres sur le sujet "Astronomical spectroscopy"

1

Lawrence, Andy. « Spectroscopy ». Dans Astronomical Measurement, 121–44. Berlin, Heidelberg : Springer Berlin Heidelberg, 2013. http://dx.doi.org/10.1007/978-3-642-39835-3_5.

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Massey, Philip, et Margaret M. Hanson. « Astronomical Spectroscopy ». Dans Planets, Stars and Stellar Systems, 35–98. Dordrecht : Springer Netherlands, 2013. http://dx.doi.org/10.1007/978-94-007-5618-2_2.

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Ade, Peter A. R., Griffin Matthew J. et Carole E. Tucker. « Astronomical Spectroscopy ». Dans Physical Principles of Astronomical Instrumentation, 123–54. Boca Raton : CRC Press, 2021. http://dx.doi.org/10.1201/9781315374659-7.

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Schmidt, Timothy W. « Astronomical Molecular Spectroscopy ». Dans Computational Spectroscopy, 377–98. Weinheim, Germany : Wiley-VCH Verlag GmbH & Co. KGaA, 2010. http://dx.doi.org/10.1002/9783527633272.ch13.

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Mertz, Lawrence. « Spectroscopy ». Dans Excursions in Astronomical Optics, 95–107. New York, NY : Springer New York, 1996. http://dx.doi.org/10.1007/978-1-4612-2386-3_5.

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Hopkins, Jeffrey L. « Amateur Astronomical Spectroscopy ». Dans The Patrick Moore Practical Astronomy Series, 45–73. Cham : Springer International Publishing, 2013. http://dx.doi.org/10.1007/978-3-319-01442-5_2.

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Hopkins, Jeffrey L. « Astronomical Spectroscopy Projects ». Dans The Patrick Moore Practical Astronomy Series, 233–51. Cham : Springer International Publishing, 2013. http://dx.doi.org/10.1007/978-3-319-01442-5_8.

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Harrison, Ken M. « A History of Astronomical Spectroscopy ». Dans Patrick Moore's Practical Astronomy Series, 9–14. New York, NY : Springer New York, 2010. http://dx.doi.org/10.1007/978-1-4419-7239-2_2.

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Escribano, Rafael, et Guillermo M. Muñoz Caro. « Introduction to Spectroscopy and Astronomical Observations ». Dans Laboratory Astrophysics, 27–47. Cham : Springer International Publishing, 2018. http://dx.doi.org/10.1007/978-3-319-90020-9_3.

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Maillard, J. P. « Astronomical Fourier-Transform Spectroscopy of the 1990s ». Dans Progress in Fourier Transform Spectroscopy, 133–41. Vienna : Springer Vienna, 1997. http://dx.doi.org/10.1007/978-3-7091-6840-0_16.

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Actes de conférences sur le sujet "Astronomical spectroscopy"

1

HOLT, STEPHEN S. « X-RAY ASTRONOMICAL SPECTROSCOPY ». Dans A Festschrift in Honor of Ricardo Giacconi. WORLD SCIENTIFIC, 2000. http://dx.doi.org/10.1142/9789812792174_0006.

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2

Serabyn, E., et E. Weisstein. « Submillimeter Fourier Transform Spectroscopy of Astronomical Sources ». Dans Fourier Transform Spectroscopy. Washington, D.C. : Optica Publishing Group, 1995. http://dx.doi.org/10.1364/fts.1995.ffd14.

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From the 4000 m altitude of Mauna Kea, submillimeter wavelength astronomical observations are often possible at frequencies up to nearly 1 THz. To measure broadband astronomical and atmospheric spectra in the available atmospheric transmission windows between 150 GHz and 1 THz, we have built a moderate resolution (λ/Δλ < 5000) Fourier Transform Spectrometer for use at the Caltech Submillimeter Observatory (CSO). The instrument is a dielectric-beamsplitter rapid-scan FTS which uses the CSO’s facility bolometer as its single detecting element. Five bandpass filters are used to match to the available atmospheric transmission windows, in order to limit the background flux on the detector. The maximum path difference is 45 cm, yielding a spectral resolution of 200 MHz. The instrumental field of view is defined by a Winston cone light concentrator. Observations with this instrument have now begun to yield high quality astronomical spectra, several of which are described in the following.

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3

Dallier, Richard, et Jean Gabriel Cuby. « Noncooled near-infrared spectroscopy ». Dans Astronomical Telescopes & Instrumentation, sous la direction de Albert M. Fowler. SPIE, 1998. http://dx.doi.org/10.1117/12.317246.

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4

Serabyn, Eugene. « Submillimeter Fourier transform spectroscopy ». Dans Astronomical Telescopes & Instrumentation, sous la direction de Thomas G. Phillips. SPIE, 1998. http://dx.doi.org/10.1117/12.317347.

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5

Serabyn, E., et J. R. Pardo. « Astronomical and Atmospheric Fourier Transform Spectroscopy at Submillimeter Wavelengths ». Dans Fourier Transform Spectroscopy. Washington, D.C. : OSA, 2001. http://dx.doi.org/10.1364/fts.2001.fmb1.

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6

Naylor, D. A., et B. G. Gom. « FTS-2 : A Submillimetre Astronomical Imaging Fourier Transform Spectrometer ». Dans Fourier Transform Spectroscopy. Washington, D.C. : OSA, 2007. http://dx.doi.org/10.1364/fts.2007.fwa1.

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7

Stern, R. A., R. C. Catura, M. M. Blouke et M. Winzenread. « EUV Astronomical Spectroscopy With CCD Detectors ». Dans 1986 Astronomy Conferences, sous la direction de David L. Crawford. SPIE, 1986. http://dx.doi.org/10.1117/12.968135.

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8

Joyce, Richard R., Kenneth H. Hinkle, Michael R. Meyer et Michael F. Skrutskie. « Infrared astronomical spectroscopy with a noncryogenic spectrograph ». Dans Astronomical Telescopes & Instrumentation, sous la direction de Albert M. Fowler. SPIE, 1998. http://dx.doi.org/10.1117/12.317339.

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9

Burgarella, Denis, Kjetil Dohlen, Veronique Buat, Gerard R. Lemaitre et Annie Perez. « Multi-object spectroscopy in space ». Dans Astronomical Telescopes & Instrumentation, sous la direction de Pierre Y. Bely et James B. Breckinridge. SPIE, 1998. http://dx.doi.org/10.1117/12.324436.

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10

Smith, Erin C., et Ian S. McLean. « Grism spectroscopy with FLITECAM ». Dans SPIE Astronomical Telescopes + Instrumentation, sous la direction de Ian S. McLean et Masanori Iye. SPIE, 2006. http://dx.doi.org/10.1117/12.672174.

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