Letter to the Editor: The collisional broadening of carbon radio recombination lines     

N.I. Rovenskaya 《Astrophysics and Space Science》2004,293(3):355-362

The density matrix equations of highly excited carbon are analytically solved as functions of line number and temperature. Allowing for the series of the impact approximation theory and quadrupole interaction potential, the line widths are found with the theoretical error less than 0.06 in the range of temperatures T _e = 25 − 100 K. To determine the medium temperature and density by using the experimental values of line widths, the Doppler, radiational and impact broadening are calculated for the lines with the principal quantum numbers n > 300. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

The 21-cm forest     

Steven R. Furlanetto 《Monthly notices of the Royal Astronomical Society》2006,370(4):1867-1875

We examine the prospects for studying the pre-reionization intergalactic medium (IGM) through the so-called 21-cm forest in spectra of bright high-redshift radio sources. We first compute the evolution of the mean optical depth τ for models that include X-ray heating of the IGM gas, Wouthuysen–Field coupling, and reionization. Under most circumstances, the spin temperature T _S grows large well before reionization begins in earnest; this occurs so long as the X-ray luminosity of high-redshift starbursts (per unit star formation rate) is comparable to that in nearby galaxies. As a result,  τ≲ 10⁻³  throughout most of reionization, and background sources must sit well beyond the reionization surface in order to experience absorption that is measurable by square-kilometre class telescopes. H  ii regions produce relatively large 'transmission gaps' and may therefore still be observable during the early stages of reionization. Absorption from sheets and filaments in the cosmic web fades once T _S becomes large and should be rare during reionization. Minihaloes can produce strong (albeit narrow) absorption features. Measuring their abundance would yield useful limits on the strength of feedback processes in the IGM as well as their effect on reionization.  相似文献   

Extreme vacuum ultraviolet solar spectra obtained during the SPIRIT experiment aboard CORONAS-F: A catalog of lines in the range 280–330 Å     

I. A. Zhitnik  S. V. Kuzin  A. M. Urnov  I. L. Beigman  S. A. Bozhenkov  I. Yu. Tolstikhina 《Astronomy Letters》2005,31(1):37-56

We present a catalog of 100 lines in the wavelength range 280–330 Å detected by the RES-C spectroheliograph in solar active regions and flares during the SPIRIT experiment aboard the CORONAS-F orbital station. We identified 54 lines. The line intensities recorded during the X3.4 (GOES) solar flare of December 28, 2001, are given. The data reduction procedure is discussed.  相似文献   

The relationship between class I and class II methanol masers     

S. P. Ellingsen 《Monthly notices of the Royal Astronomical Society》2005,359(4):1498-1516

The Australia Telescope National Facility Mopra millimetre telescope has been used to search for 95.1-GHz class I methanol masers towards 62 6.6-GHz class II methanol masers. A total of 26 95.1-GHz masers were detected, 18 of these being new discoveries. Combining the results of this search with observations reported in the literature, a near complete sample of 66 6.6-GHz class II methanol masers has been searched in the 95.1-GHz transition, with detections towards 38 per cent (25 detections; not all of the sources studied in this paper qualify for the complete sample, and some of the sources in the sample were not observed in the present observations).
There is no evidence of an anticorrelation between either the velocity range, or peak flux density of the class I and II transitions, contrary to suggestions from previous studies. The majority of class I methanol maser sources have a velocity range that partly overlaps with the class II maser transitions. The presence of a class I methanol maser associated with a class II maser source is not correlated with the presence (or absence) of main-line OH or water masers. Investigations of the properties of the infrared emission associated with the maser sources shows no significant difference between those class II methanol masers with an associated class I maser and those without. This may be consistent with the hypothesis that the objects responsible for driving class I methanol masers are generally not those that produce main-line OH, water or class II methanol masers.  相似文献   

红外暗云G79.2+0.38的性质     

吴凌翔  杨戟 《天文学报》2005,46(2):136-144

对MSX红外暗云G79.2+0.38的11'×7'的区域范围进行了12CO(1-0)、13CO(1-0)和C18O(1-0)谱线的同时观测.观测到的两个C18O(1-0)谱线所界定的云核峰值分布分别对应MSX A波段的两块高消光区域.该区域的氢分子柱密度N(H2)-(5-12)×1022 cm-2,平均密度n-(3±1)×104cm-3.两块分子云核的13CO的线尺度分别是1.7和1.2 pc,而C18O的线尺度分别是1.2和0.6 pc,它们包含的质量为2×102-2×103M(?).分子云核的视向平均密度结构可用幂函数(?)(p)-p-0.34±0.02表征. 13CO和C18O的丰度和典型的光学暗云相比低了4至11倍,但是目前还没有证据表明13CO和C18O的相对丰度比X13/18随柱密度有显著变化.  相似文献   

A molecular face-on view of the Galactic Centre region   总被引：1，自引：0，他引：1  

Tsuyoshi Sawada  Tetsuo Hasegawa  Toshihiro Handa  R. J. Cohen 《Monthly notices of the Royal Astronomical Society》2004,349(4):1167-1178

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The electron temperature and density in interstellar medium by using carbon radio recombination line observations     

N.I. Rovenskaya 《Astrophysics and Space Science》2004,291(2):113-122

The intensities of carbon radio recombination lines (RRL’s) are definedallowing for the effect of dielectronic-like recombination. The rate ofdielectronic-like recombination is calculated as functions of line number,electron density and temperature accurate to 0.05. Following from the balanceequation solutions for populations, the RRL intensities are analytically foundby the method of successive approximations to an accuracy of 0.15. Theobservations of carbon RRL’s are analyzed toward Cassiopeia A. The averageelectron temperature, density, expanded CII region lengths and inaccuraciesare found with the experimental values of RRL widths and intensities.  相似文献   

Dust obscuration studies along quasar sight-lines using simulated galaxies     

D. K. Churches  A. H. Nelson  M. G. Edmunds 《Monthly notices of the Royal Astronomical Society》2004,347(4):1234-1240

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Visibility of old supernova remnants in H i 21-cm emission line     

Bon-Chul Koo  Ji-hyun Kang 《Monthly notices of the Royal Astronomical Society》2004,349(3):983-993

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Erratum: The spectrum of BAL QSO 03 + 308: intrinsic variability and line-locking stability     

E.Y. Vilkoviskij  M.J. Irwin 《Monthly notices of the Royal Astronomical Society》2001,326(1):416-416

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