Atlas of UV spectra of supernovae

Publisher: European Space Agency, Publisher: Distributed by ESA Scientific & Technical Publications Branch in Paris, France, Noordwijk, The Netherlands

Written in English
Published: Pages: 224 Downloads: 312
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  • Stars, Variable -- Spectra.,
  • Supernovae.

Edition Notes

Includes bibliographical references.

StatementP. Benvenuti ... (et al.).
SeriesESA SP -- 1046
ContributionsBenvenuti, P., European Space Agency.
The Physical Object
Pagination224 p. :
Number of Pages224
ID Numbers
Open LibraryOL20314044M

THE ULTRAVIOLET PROPERTIES OF SUPERNOVAE A Dissertation in Astronomy and Astrophysics by Peter J. Brown c Peter J. Brown Submitted in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy August Key words: cosmology: observations – infrared: general – line: identification – supernovae: general Online-only material: color figures 1. INTRODUCTION This sample of 41 near-infrared (NIR, – μm) spectra from Type Ia supernovae (SNe Ia) provides the first opportunity to study NIR spectral evolution in a large number of SNe Ia. in the ultraviolet (UV) to μm in the near-infrared (NIR). Optical spectra provide line profiles and velocity measurements of Hi,Hei,Caii, and Feii that trace the composition and kinematics of the supernova (SN). NIR spectra show that helium is present in the atmosphere as early as 11 days after the explosion. A UV spectrum. The Sadtler Handbook of Ultraviolet Spectra by Sadtler Research Laboratories (Author) ISBN ISBN Why is ISBN important? ISBN. This bar-code number lets you verify that you're getting exactly the right version or edition of a book.

Studying the Ultraviolet Spectrum of the First Spectroscopically Confirmed Supernova at Redshift Two distance scale – supernovae: general – supernovae: individual (DES16C2nm) – surveys prominent in the UV spectra of SLSNe-I, with a characteristic turnover at . We present 41 near-infrared (NIR, mu m) spectra from normal Type Ia supernovae (SNe Ia) obtained at epochs ranging from 14 days before to 75 days with respect to the maximum light date in the V band. All data were obtained at the Infrared Telescope Facility using the SpeX by: mass loss history. This early detection of supernovae (SNe) allows spectra and luminosity observations to be made during the rising phase of the light curve as well as the decline. Shock breakout was predicted nearly 40 years ago [1,2], but has only recently been observed as an . Maurice Gavin (lots of spectra of variables, supernovae, Wolf-Rayet stars, ) Ernst Pollmann (observation of Be-stars, VVCep and many hints for beginners) Sylvain and André Rondi (fines spectrograph constructions and many tips) Dale Mais (SBIG spectrograph - numerous informations).

Although supernovae are rare within our galaxy, they are sufficiently bright to be seen in very distant galaxies. These distant supernovae are classified according to their spectra. There are two basic types of supernova, called (boringly enough) ``Type I'' and ``Type II''. Type I: supernovae WITHOUT hydrogen absorption lines in their spectrum.   Ultraviolet and Visible Absorption Spectra, Index for is a reference volume listing of ultraviolet and visible absorption spectra in the literature. This book contains ab references to published absorption spectra in 27 important American and European journals and one Edition: 1. Supernova explosions are not only important to the ecology of the universe, seeding it, among other things, with the heavy elements necessary for the existence of life, but they are also a natural laboratory in which a host of unique physical phenomena occur. While still far from a complete.   spectra of “normal” SNe Ia 17,18,19,20,21 (the spectrum of SN O was provided courtesy of the Cal´an/Tololo Supernova Survey), as they would appear redshifted to z = The spectra show the evolution of spectral features between 7 restframe days before and 2 days after restframe B-band maximum light.

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Atlas of UV spectra of supernovae. Paris, France: European Space Agency ; Noordwijk, the Netherlands: Distributed by ESA Scientific & Technical Publications Branch, © (OCoLC) Document Type: Book: All Authors / Contributors: P Benvenuti; European Space Agency.

adshelp[at] The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement NNX16AC86ACited by: 3. The MPI-Mainz UV/VIS Spectral Atlas is a comprehensive collection of cross sections for gaseous molecules and radicals, primarily relevant to atmospheric research.

The individual data sets were collected from the original publications, either copied from tabulations, or read from figures in those cases where numerical data could no longer be.

Solar EUV and UV spectral atlases online. SOHOSUMER EUV Solar Spectral Atlas The first EUV spectral atlas obtained with SUMER has been made available on the Web.

The atlas covers the spectral range - Å ( - Å in 2nd order). The SUMER spectrum, with all its details, clearly demonstrates the strength of this instrument. The temporal evolution of the optical spectra of various types of supernovae (SNe) is illustrated, in part to aid observers classifying supernova candidates.

Type II SNe are defined by the presence of hydrogen, and they exhibit a very wide variety of photometric and spectroscopic properties. Among hydrogen-deficient SNe (Type I), three subclasses are now known: those whose early-time spectra Cited by: But the spectra of supernovae resisted interpretation for a very long time.

The outstanding obstacle was the great characteristic width of the spectral features— Å—corresponding to Doppler broadening velocities of –10, km s − by: 5.

Type Ib Supernova Spectra Beforesupernovae were classified as either Type I or Type II depending on whether hydrogen was present in their spectra. Through mostly serendipitous discoveries, it became clear that Type I supernovae should be divided into at.

Abstract. Model atmospheres for supernovae of type II have been calculated taking into account the effects of sphericity and velocity fields. We obtain a good fit for the energy distribution of the recent supernovae SN K and SN : W. Spies, P. Hauschildt, R.

Wehrse, B. Baschek, G. Shaviv. It also presents integrated spectra of stellar clusters, galaxies and quasars, and the reference spectra of some terrestrial light sources, for calibration purposes. Whether used as the principal reference for comparing with your recorded spectra or for inspiring independent observing projects, this atlas provides a breathtaking view into our.

The MPI-Mainz UV/VIS spectral atlas of gaseous molecules of atmospheric interest, Earth Syst. Sci. Data, 5, –, (), DOI: /essd Cross Sections The molecular species included in the database are classified in the categories listed below.

Many of the categories contain a number of subcategories, which appear after. OPTICAL SPECTRA OF SUPERNOVAE Figure 2 Spectra of SNe, showing late-time distinctions between various types and subtypes.

Notation is the same as in Figure 1. The parent galaxy of SN L is NGC (cz D km s−1); others are listed in the caption of Figure 1. At even later phases, SN A was dominatedCited by: We present the entire sample of ultraviolet (UV) spectra of supernovae (SNe) obtained with the Ultraviolet/ Optical Telescope (UVOT) on board the Swift satellite during the first two years of observations (/).

A total of 29 UV-grism and 22 V-grism spectra of nine SNe have been collected, of which six are thermonuclear. A supernova (/ ˌ s uː p ər ˈ n oʊ v ə / plural: supernovae / ˌ s uː p ər ˈ n oʊ v iː / or supernovas, abbreviations: SN and SNe) is a powerful and luminous stellar transient astronomical event occurs during the last evolutionary stages of a massive star or when a white dwarf is triggered into runaway nuclear fusion.

The original object, called the progenitor, either. An Atlas of Stellar Spectra Astrophys. monographs, Univ. Chicago Press () AN ATLAS OF STELLAR SPECTRA WITH AN OUTLINE OF SPECTRAL CLASSIFICATION Morgan * Keenan * Kellman Table of Contents INTRODUCTION THE O5-F2 STARS The O Stars O B0 B B1 B2 B3 B5 B8 The Spectrum of Draconis The A Stars B9 A0 A1 A2 A3 A5 A7 F0 F2 The Peculiar A StarsFile Size: 4MB.

ATLAS is an asteroid impact early warning system being developed by the University of Hawaii and funded by NASA. It consists of two telescopes, miles apart, which automatically scan the whole sky several times every night looking for moving objects.

ATLAS will provide one day's warning for a kiloton "town killer," a week for a 5-megaton "city killer," and three weeks for a megaton. A Type Ia supernova occurs when a white dwarf star accretes material from a companion.

Astronomers have completed the first thorough study of the. Here we present a detailed analysis of Hubble Space Telescope ultraviolet (UV) and ground-based optical spectra and light curves of the SN Ia SN jn (PTF10ygu).

SN jn was discovered by the Palomar Transient Factory (PTF) 15 days before maximum light, allowing us to secure a time-series of four UV spectra at epochs from to +5 days Cited by: UV-VIS Spectroscopy - Chemical Analysis Chemical Analysis Solutions Unit SiRS PhDSonia R.

Sousa PhD Marketing Manager - Spectroscopy 21 January Group/Presentation Title Agilent Restricted Page 1 Month ##, X. Type Ib/Ic supernovae are distinguished from Type Ia by the lack of an absorption line of singly ionized silicon at a wavelength of nanometres. As Type Ib and Ic supernovae age, they also display lines from elements such as oxygen, calcium and magnesium.

In contrast, Type. SN jn was discovered by the Palomar Transient Factory (PTF) 15 d before maximum light, allowing us to secure a time series of four near-UV spectra at epochs from − to + d relative to.

Type Ia supernovae 1 are destructive explosions of carbon-oxygen white dwarfs 2,gh they are used empirically to measure cosmological distances 4,5,6, the nature of. near-ultraviolet (near-UV) spectra from the HubbleSpaceTelescopeand ground-based optical spectra and light curves.

SNjn was discovered by the Palomar Transient Factory (PTF) 15d before maximum light, allowing us to secure a time series of four near-UV spectra at epochs from − to +d relative to B-band maximum.

The photospheric near-UVCited by: Ultraviolet and Visible Spectra. When electromagnetic radiation in the ultraviolet (UV) or visible region of the spectrum is absorbed by a molecule, π or non‐bonding (n) electrons are promoted into antibonding orbitals.

Removing #book# from your Reading List will. The ultraviolet-visible reference spectra presented here were obtained by the use of double-beam spectrophotometers with sample solutions prepared as specified in the individual mono-graphs.

The horizontal axis indicates the wavelength (nm) and the vertical axis indicates the. UV-VIS spectroscopy plays an important role in analytical chemistry and has widespread application in chemistry, physics and life sciences.

The author has created a detailed and comprehensive reference work on all important aspects of UV-VIS spectroscopy, including investigations on chemical kinetics and chemical equilibria. Photometric determinations, multicomponent and multiwavelength.

EarlySpectra of Supernovae E. Baron,1,2,3 Peter E. Nugent,2 David Branch,1 and Peter the agreement of synthetic spectra with observations across a broad class of astrophysical objects is a very good consistency check.

We have Early spectra of supernovae are important to. The temporal evolution of the optical spectra of various types of supernovae (SNe) is illustrated, in part to aid observers classifying supernova candidates. Type II SNe are defined by the presence of hydrogen, and they exhibit a very wide variety of photometric and spectroscopic properties.

Optical Spectra of Supernovae David Branch 1, E. Baron, ery2 1 University of Oklahoma, Norman, OKUSA 2 New Mexico Institute of Mining and Technology, Socorro, NMUSA Abstract. Supernova flux and polarization spectra bring vital information on the geometry, physical conditions, and composition structure of the ejected matter.

We present optical spectra, obtained with the Keck 10 m telescope, of two high-redshift Type Ia supernovae (SNe Ia) discovered by the High-z Supernova Search Team: SN. Spectroscopic Atlas for Amateur Astronomers 5 Table Page Topic Objects Wavelength domain Gra-ting 23 59 Metallicity: Vega vs.

Sirius Vega α Lyr Sirius A α CMa – L 30 62 Development of spectral features within the F-class Adhafera ζ Leo Procyon α CMi – L 31 64 Effects of the luminosity on spectra. These supernovae would then “contaminate” the galaxy spectra. In Graur & Maoz (), we developed a computer code that allowed us to identify such contaminated spectra and tweeze out the supernovae from the data.

In Graur et al. (), we used this code to detect 91 Type Ia and 16 Type II .The classification of supernovae in types was introduced by Rudolph Minkowski (Minkowski ) on the grounds of their spectra: Type I supernovae show no hydrogen lines in their spectra, whereas these lines are present in those of Type II.

Later these types were subdivided, again based on their spectra; for a summary see e.g. Turatto (The Atlas of Stellar Spectra and the accompanying outline have been prepared from the viewpoint of the practical stellar astronomer. Problems connected with the astrophysical interpretation of the spectral sequence are not touched on; as a consequence, emphasis is placed on “ordinary” stars.