http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
A search for interstellar naphthalene and anthracene cations
Galazutdinov, G.,Lee, Byeong‐,Cheol,Song, In‐,Ok,Kazmierczak, M.,Krełowski, J. Blackwell Publishing Ltd 2011 Monthly notices of the Royal Astronomical Society Vol.412 No.2
<P><B>ABSTRACT</B></P><P>The evidence for naphthalene and anthracene cations reported by Iglesias‐Groth and co‐authors in 2008 and 2010 respectively in the spectra of a rather cool object, (A3V) Cernis 52, was carefully examined with the aid of high‐resolving‐power (30 000 ≲<I>R</I>≲ 90 000) spectra. No possible bands of these molecules were found in high signal‐to‐noise ratio spectra of HD 147889, HD 204827, HD 207538 and HD 281259 – these objects represent both weaker and stronger interstellar molecular features and diffuse bands than Cernis 52. The idea that possible naphthalene and anthracene feature detection has a connection to the anomalous microwave emission reported in the direction of Cernis 52 has been examined using high‐quality spectra of HD 278942 and HD 281159 observed in the same area as Cernis 52. Despite the high microwave flux density in the direction of HD 281159 (∼four times higher at 60 μm than in the direction to Cernis 52), no expected features were detected. Accordingly, we consider these PAH discoveries as premature. Using the spectrum of HD 281159 we estimate the column density of interstellar naphthalene and anthracene normalized to <I>E</I>(<I>B</I>−<I>V</I>) = 1.0 as less than 2.16 × 10<SUP>12</SUP> and 1.4 × 10<SUP>12</SUP> respectively.</P>
A SURVEY OF INTERSTELLAR LINES: RADIAL VELOCITY PROFILES AND EQUIVALENT WIDTHS
GALAZUTDINOV GAZINUR The Korean Astronomical Society 2005 Journal of The Korean Astronomical Society Vol.38 No.2
An atlas of high resolution (${\lambda}/{\Delta}{\lambda}$=45,000) profiles of interstellar atomic lines of K I (7665, 7699 ${\AA}$), Na I (D 1, D2), Ca II (H, K), Ca I (4227 ${\AA}$), molecular structures of CH, CH+, CN and the major diffuse interstellar bands at 5780 and 5797 ${\AA}$ based on ${\~}$300 echelle spectra of ${\~}$200 OB stars is presented. Relationships between the reddenings, distances and equivalent widths of NaI, CaII, KI, CH, CH+, CN and diffuse bands are discussed. The equivalent width of K I (7699 ${\AA}$) as well as of CH4300 ${\AA}$ / correlate very tightly with E(B- V) in contrast to the features of neutral sodium, ionized calcium and the molecular ion CH+. The equivalent widths of the Hand K lines of Call grow with distance at a rate ${\~}$250m${\AA}$ per 1 kpc. A similar relation for NaI is much less tight. The strengths of neutral potassium lines, molecular features and diffuse interstellar bands do not correlate practically with distance. These facts suggest that ionized calcium fills the interstellar space quite homogeneously while the other carriers mentioned above, especially K I, CH and these of diffuse bands occupy more and more compact volumes, also filled with dust grains. Apparently the carriers of narrow diffuse bands are spatially correlated with simple molecules and dust grains - all abundant in the so-called 'zeta' type clouds. The same environment seems to be hostile to the carriers of broad diffuse interstellar bands (DIEs) (like 5780 or 6284) and -to a certain extent - also to CaII, NaI and CH+.
Blueshifted diffuse interstellar bands in the spectrum of HD 34078
Galazutdinov, G. A.,Manicò,, G.,Krełowski, J. Blackwell Science Ltd 2006 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.366 No.3
<P>ABSTRACT</P><P>In this paper, we report the very first observation of diffuse interstellar bands (DIBs) that, in the spectrum of HD 34078 (AE Aur), are blueshifted with respect to the normal position that they have in other objects, where the rest-wavelength velocity frame is determined using very sharp interstellar atomic lines or molecular features. Only reasonably narrow DIBs seemingly show this effect, which is absent in broader ones. The result is confirmed independently using three different spectrographs attached to two different telescopes.</P>
ON THE HOMOGENEITY OF THE EXTINCTION LAW IN OUR GALAXY
Bondar, A.,Galazutdinov, G.,Patriarchi, P.,Krelowski, J. The Korean Astronomical Society 2006 Journal of The Korean Astronomical Society Vol.39 No.3
We analyze the extinction law towards several B1V stars-members of our Galaxy, searching for possible discrepancies from the galactic average extinction curve. Our photometric data allow to build extinction curves in a very broad range: from extreme UV till infrared. Two-colour diagrams, based on the collected photometric data from the ANS UV satellite, published UBV measurements and on the infrared 2MASS data of the selected stars, are constructed. Slopes of the fitted straight lines are used to build the average extinction curve and to search for discrepant objects. The selected stars have also been observed spectroscopically from the Terskol and ESO Observatories; these spectra allow to check their Sp/L's. The spectra of only about 30% of the initially selected objects resemble closely that of HD144470, considered as the standard of B1 V type. Other spectra either show some emission features or belong clearly to another spectral types. They are not used to build the extinction curve. Two-colour diagrams, constructed for the selected B1 V stars, showing no emission stellar features, prove that the interstellar extinction law is homogeneous in the Galaxy. Both the shape of the curve and the total-to-selective extinction ratio do not differ from the galactic average and the canonical value(3.1) respectively. The circumstellar emissions usually cause some discrepancies from the average interstellar extinction law; the discrepancies observed in the extraterrestrial ultraviolet, usually follow some misclassifications.