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1.
Doing a homogenious and fast survey requires an intelligent model for the observing-strategy. This contribution shows a model simulating the parameters for the survey of the southern hemisphere. Input parameters are weather statistics and requirements of the photometry and of the technical equipment. It does not include priorities for special zones of the sky or deeper observations, even if the program is already able to consider such parameters. 相似文献
2.
Kimeswenger 《Monthly notices of the Royal Astronomical Society》1998,294(2):312-314
In 1977, Weinberger published a list of 12 new extended possible planetary nebulae (PNe). Whereas, because of their characteristic morphology and/or the presence of a blue central star, almost all of them could easily be suspected to be genuine planetary nebulae, one object (No. 12) captivated because of its unusually bright central star. This find prompted Kaler & Feibelman to question the PN nature of this object (We 1–12) on the basis of IUE spectra. A definite conclusion could, however, not be drawn by them; thus, until now, the real nature of We 1–12 remained unsolved. For the first time, a spectral investigation of both the central star and the nebula is presented in this paper. It definitely shows that this intriguing object is an (isolated) H ii region and its central star, as previously assumed, is an early B star which serves as the ionizing source. We 1–12, a part of which is coincident with a weak IRAS point source, is at a distance of 2–2.6 kpc and is reddened by E ( B − V )=0.6–0.8 mag. 相似文献
3.
Nebulae around low mass Wolf-Rayet [WC] stars often show a strong midand near infrared (MN-IR) emission which cannot be explained with asingle grain size and an equilibrium temperature model. Weinvestigated the effect of the grain size, radiation density, andtemperature fluctuations of small dust grains on the spectral energydistribution (SED) in the infrared.A model of ISOCAM and IRAS measurements of V605 Aql (Kimeswenger et al., 1998) has beencomputed using a gas-dust combination model including transiently heatedparticles. Our calculations show that the central knot in V605 Aql(Abell 58) is too compact or just on the lower boundary that temperature fluctuations really have to be considered in model calculations forthe infrared SED. 相似文献
4.
5.
S. Kimeswenger F. Kerber & R. Weinberger 《Monthly notices of the Royal Astronomical Society》1998,296(3):614-618
We present ISO observations of A58 and A78. Both objects are suspected to have undergone late He flashes ('born-again' nebulae). With ISOCAM we have been able to obtain data of much higher spatial resolution over the wavelength range 4.5–18 μm than has been possible in the past. In order to extract full information from our data we have developed a method to eliminate residual variations in the dark field. The results for A58 and A78 are compared with literature data and with A30 – the most prominent 'born-again' planetary nebula (PN). 相似文献
6.
At the end of the workshop the contributors bounced some ideas aroundand shared their thoughts about maximizing the advancement thata study of Sakurai's Object can provide. In particular it was resolvedto set up a web site http://astro.uibk.ac.at/sakurai, witha finding chart and a record of data obtained, and to maintain theoriginal workshop web site at http://www.astro.keele.ac.uk/sakurai. Observers and theoreticians are urged to consult,and to contribute to, this resource. 相似文献
7.
A. Bacher S. Kimeswenger P. Teutsch 《Monthly notices of the Royal Astronomical Society》2005,362(2):542-548
Online Digitized Sky Survey (DSS) material is often used to obtain information on newly discovered variable stars for older epochs (e.g. Nova progenitors, flare stars, etc.). We present here the results of an investigation of photometry on online DSS material in small fields calibrated by CCD sequences. We compared different source extraction mechanisms and found that even down near to the sensitivity limit, despite the H-compression used for the online material, photometry with an accuracy better than 0.1 mag rms is possible on DSS-II. Our investigation shows that the accuracy depends strongly on the source extraction method. The SuperCOSMOS scans, although retrieved with a higher spatial resolution, do not give us better results. The methods and parameters presented here allow the user to obtain good plate photometry in small fields down to the Schmidt plate survey limits with a few bright CCD calibrators, which may be calibrated with amateur-size telescopes. Especially for the events mentioned above, new field photometry for calibration purposes mostly exists, but the progenitors were not measured photometrically before. Also, the follow-up whether stellar concentrations are newly detected clusters or similar work may be done without using mid-size telescopes. The calibration presented here is a 'local' one for small fields. We show that the method presented here gives higher accuracies than 'global' calibrations of surveys (e.g. Guide Star Catalogue-II (GSC-II), SuperCOSMOS and the US Naval Observatory Astrometry Catalog B). 相似文献
8.
S. Kimeswenger 《Astrophysics and Space Science》2002,279(1-2):79-89
The central star V4334 Sgr (Sakurai's Object) of the planetary nebula PN G010.4+04.4 underwent in 1995–1996 the rare event of a very late helium flash. It represents only one out of two such events during the era of modern astronomy (the other event was V605 Aql = Nova Aql 1919). All the other prominent objects of that type originate from events occurring several thousands of years ago (e.g. A30, A78). Thus it is of special interest for stellar evolution theory to model the detailed observations obtained during the last four years. Those models depend essentially on basic stellar parameters like effective temperature, surface gravity and stellar radius. Most of them depend strongly on the assumed distance to the object. Some models may give some constraints on this parameter, but most of them depend on the assumption as input parameter. Hence to determine a reliable distance is of considerable significance. This should be obtained through models that give us lower and upper boundaries, or through means which are independent of models. The detailed review, by using every kind of determination available up to now, leads to a Galactic foreground extinction of E
B–V =0m75 ±0.05 and a distance of D = 2.0-0.6
+1.0 kpc. 相似文献
9.
N. Epchtein B. De Batz E. Copet P. Fouqué F. Lacombe T. Le Bertre G. Mamon D. Rouan D. Tiphène W. B. Burton E. Deul H. Habing J. Borsenberger M. Dennefeld A. Omont J. C. Renault B. Rocca Volmerange S. Kimeswenger I. Appenzeller R. Bender T. Forveille F. Garzon J. Hron P. Persi M. Ferrari-Toniolo I. Vauglin 《Astrophysics and Space Science》1994,217(1-2):3-9
The DENIS project is the first attempt to carry out a complete digitized survey of the southern sky in the range 1–2.5µm. The main objectives of the programme and the main specifications of the camera and of the data processing stream are briefly outlined 相似文献
10.
E. Copet B. De Batz N. Epchtein P. Fouqué F. Lacombe T. Le Bertre D. Rouan D. Tiphène J. Borsenberger S. Kimeswenger 《Astrophysics and Space Science》1994,217(1-2):25-26
We briefly report on the first astronomical results obtained with the DENIS camera at the ESO 1 meter telescope. 相似文献