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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>
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>
CaFe interstellar clouds<sup>★</sup>
Bondar, A.,Kozak, M.,Gnaciń,ski, P.,Galazutdinov, G. A.,Beletsky, Y.,Krełowski, J. Blackwell Publishing Ltd 2007 MONTHLY NOTICES- ROYAL ASTRONOMICAL SOCIETY Vol.378 No.3
<P>ABSTRACT</P><P>A new kind of interstellar cloud is proposed. These are rare (just a few examples among ∼300 lines of sight) objects with the Ca <SMALL>I</SMALL> 4227-Å, Fe <SMALL>I</SMALL> 3720-Å and 3860-Å lines stronger than those of K <SMALL>I</SMALL> (near 7699 Å) and Na <SMALL>I</SMALL> (near 3302 Å). We propose the name ‘CaFe’ for these clouds. Apparently they occupy different volumes from the well-known interstellar H <SMALL>I</SMALL> clouds where the K <SMALL>I</SMALL> and ultraviolet Na <SMALL>I</SMALL> lines are dominant features. In the CaFe clouds we have not found either detectable molecular features (CH, CN) or diffuse interstellar bands which, as commonly believed, are carried by some complex, organic molecules. We have found the CaFe clouds only along sightlines toward hot, luminous (and thus distant) objects with high rates of mass loss. In principle, the observed gas-phase interstellar abundances reflect the combined effects of the nucleosynthetic history of the material, the depletion of heavy elements into dust grains and the ionization state of these elements which may depend on irradiation by neighbouring stars.</P>