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J.H. Telting G. Avila L. Buchhave S. Frandsen D. Gandolfi B. Lindberg H.C. Stempels the NOT staff S. Prins 《Astronomische Nachrichten》2014,335(1):41-45
FIES is a cross‐dispersed high‐resolution echelle spectrograph at the 2.56 m Nordic Optical Telescope (NOT), and was optimised for throughput and stability in 2006. The major 2006 upgrade involved the relocation of FIES to a stable environment and development of a fiber bundle that offers 3 different resolution modes, and made FIES an attractive tool for the user community of the NOT. Radial‐velocity stability is achieved through double‐chamber active temperature control. A dedicated data reduction tool, FIEStool, was developed. As a result of these upgrades, FIES is now one of the work‐horse instruments at the NOT. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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R. Oreiro J. H. Telting R. H. Østensen M. Briquet C. Aerts U. Heber M. Vučković 《Astrophysics and Space Science》2010,329(1-2):211-216
We have produced simulated time series of high resolution spectroscopy for sdBs. We present the first results of testing classical mode identification techniques. Here, in particular, we analyse the behaviour of individual spectral lines and discuss the results and applicability of the moment method. 相似文献
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R. H. Østensen J. H. Telting R. Oreiro U. Heber E. De Beck M. Reed 《Astrophysics and Space Science》2010,329(1-2):167-174
We obtained 1955 high-resolution spectra of the high-amplitude pulsating subdwarf B star V338 Ser with the FIES spectrograph at the 2.5 m Nordic Optical Telescope covering 4 full nights in May–June 2009. Here we present the first results from phase-folding the data on the main pulsation mode, as revealed by simultaneous B-band photometry obtained with the Mercator 1.25 m and Baker 0.4 m telescopes. We compare the results with a sample line-profile model produced with LTE atmospheres and bruce+kylie. 相似文献
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Historically, any newly discovered object needed to be “confirmed” with optical observations. Catalogs were published, such as the PKS (Parkes Catalog), with stamp-sized photographs that allowed us to “see” what was just found. This is still somewhat true, although far less than in the past. We are probably reaching an information overload with more efficient instruments, larger detectors, multiple wavelength coverage and an increasing number of ground and space-based facilities. At the same time, information technology is catching up and is allowing us to use the data regardless of where they reside. An increasing need of multi-wavelength observations to understand the underlying physics of the observed phenomena and the challenge to mine petabyte databases is leading to a federation of archives and cooperation among computer scientists and astronomers. These are the seeds of a virtual observatory, a cyberspace entity where the data are ready to be found and analyzed. In the United States, the National Science Foundation (NSF) and the National Aeronautics and Space Administration (NASA) are funding initiatives that will lead to the creation of this entity. This paper describes these projects. 相似文献
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C. Aerts P. De Cat G. Handler U. Heiter L. A. Balona J. Krzesinski P. Mathias H. Lehmann I. Ilyin J. De Ridder S. Dreizler A. Bruch I. Traulsen A. Hoffmann D. James E. Romero-Colmenero T. Maas M. A. T. Groenewegen J. H. Telting K. Uytterhoeven C. Koen P. L. Cottrell J. Bentley D. J. Wright J. Cuypers 《Monthly notices of the Royal Astronomical Society》2004,347(2):463-470
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M. Hernandez W. P. S. Meikle A. Aparicio C. R. Benn M. R. Burleigh A. C. Chrysostomou A. J. L. Fernandes T. R. Geballe P. L. Hammersley J. Iglesias-Paramo D. J. James P. A. James S. N. Kemp T. A. Lister D. Martinez-Delgado A. Oscoz D. L. Pollacco M. Rozas S. J. Smartt P. Sorensen R. A. Swaters J. H. Telting W. D. Vacca N. A. Walton M. R. Zapatero-Osorio 《Monthly notices of the Royal Astronomical Society》2000,319(1):223-234
We present first-season infrared (IR) and optical photometry and spectroscopy of the Type Ia Supernova 1998bu in M96. We also report optical polarimetry of this event. SN 1998bu is one of the closest type Ia supernovae of modern times, and the distance of its host galaxy is well determined. We find that SN 1998bu is both photometrically and spectroscopically normal. However, the extinction to this event is unusually high, with We find that SN 1998bu peaked at an intrinsic Adopting a distance modulus of 30.25 (Tanvir et al.) and using Phillips et al.'s relations for the Hubble constant, we obtain Combination of our IR photometry with those of Jha et al. provides one of the most complete early-phase IR light curves for a SN Ia published so far. In particular, SN 1998bu is the first normal SN Ia for which good pre- t B max IR coverage has been obtained. It reveals that the J , H and K light curves peak about 5 days earlier than the flux in the B -band curve. 相似文献
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M. Desmet M. Briquet † A. Thoul ‡ W. Zima P. De Cat G. Handler I. Ilyin E. Kambe J. Krzesinski H. Lehmann S. Masuda P. Mathias D. E. Mkrtichian J. Telting K. Uytterhoeven S. L. S. Yang C. Aerts 《Monthly notices of the Royal Astronomical Society》2009,396(3):1460-1472
We present the results of a spectroscopic multisite campaign for the β Cephei star 12 (DD) Lacertae. Our study is based on more than thousand high-resolution high S/N spectra gathered with eight different telescopes in a time span of 11 months. In addition, we make use of numerous archival spectroscopic measurements. We confirm 10 independent frequencies recently discovered from photometry, as well as harmonics and combination frequencies. In particular, the slowly pulsating B-stars (SPB)-like g -mode with frequency 0.3428 d−1 reported before is detected in our spectroscopy. We identify the four main modes as (ℓ1 , m 1 ) = (1, 1), (ℓ2 , m 2 ) = (0, 0), (ℓ3 , m 3 ) = (1, 0) and (ℓ4 , m 4 ) = (2, 1) for f 1 = 5.178 964 d−1 , f 2 = 5.334 224 d−1 , f 3 = 5.066 316 d−1 and f 4 = 5.490 133 d−1 , respectively. Our seismic modelling shows that f 2 is likely the radial first overtone and that the core overshooting parameter αov is lower than 0.4 local pressure scale heights. 相似文献
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J. Telting R. Østensen R. Oreiro U. Heber M. Vučković S. Randall A. Baran 《Astrophysics and Space Science》2010,328(1-2):163-166
In this work, a standard solar model is computed with new reaction rates that take into account the exact astrophysical S-factor, S e for the 3He(3He,2p)4He, 3He(α,γ)7Be and 7Be(p,γ)8B reactions. The exact S-factor which is valid for all energies is an improved version of the S-factor in the lower-energy approximation (Yusof and Kassim in Astrophys. Space Sci., 2009b). The effects of these new nuclear reaction rates on the solar neutrino fluxes are then discussed by comparing this model to a solar model computed with the standard NACRE reaction rates (Angulo et al. in Nucl. Phys. A. 656:3, 1999). The new reaction rates are found to decrease the neutrinos flux for 7Be and 8B by about 6% and 16%, respectively. A solar model is also computed with the reaction rates of the LUNA collaboration for 14N(p,γ)15O (Formicola et al. in Phys. Lett. B 591:61, 2004). In this case, a clear decrease of the fluxes for 13N and 15O is observed to be in good agreement with previous results (see e.g. Bahcall et al. in Astrophys. J. 621:L88, 2005). 相似文献