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天文和天体物理学研究
天文和天体物理学研究

汪景琇 景益鹏

月刊

1674-4527

wenyy@bao.ac.cn

010-64853746

100717

北京朝阳区大屯路甲20号国家天文台 RAA编辑部

天文和天体物理学研究/Journal Research in Astronomy and AstrophysicsCSCD北大核心CSTPCDSCI
查看更多>>本刊1981年创刊至2000年已出版20卷。创刊时为中文期刊，2001年改为《中国天文和天体物理学报》（英文版）。主要刊登天文学和天体物理学领域的原创性研究论文。主要栏目和报道范围：“研究快报”用来报道天文观测的新结果及新理论；“特约综述”聘请国际知名天文学家就某些热点问题进行专题评述。“研究论文”具有原创性。2009年更名为《天文和天体物理学研究》（英文版），由双月刊变为月刊。
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    New HⅠ Observations Toward the NGC 5055 Galaxy Group with FAST

    Xiao-Lan LiuMing ZhuJin-Long XuPeng Jiang...
    249-256页
    查看更多>>摘要：We report a new high-sensitivity HⅠ mapping observation of the NGC 5055 galaxy group over an area of(1.°5)×(0°75)with the Five-hundred-meter Aperture Spherical radio Telescope(FAST).Our observation reveals that the warped HⅠ disk of NGC 5055 is more extended than what was previously observed by WSRT,out to(23'.9)(61.7 kpc).The total HⅠ mass of NGC 5055 is determined to be～1.1 × 1010M⊙.We identified three HⅠclouds with HⅠ masses of the order of～107M⊙ at the southeastern edge of the HⅠ disk,as well as a candidate high-velocity cloud with an HⅠ mass of(1.2±0.5)× 106M⊙to the north of NGC 5055.The HⅠ content of UGCA 337 is robustly detected for the first time by the FAST observations.It has a narrow HⅠ linewidth of W50=17.4±3.8 km s-1 with a total HⅠ mass of(3.5±0.3)× 106 M⊙.Comparing the gas content and g-r color of UGCA 337 with typical low-mass dwarf galaxies,UGCA 337 appears relatively gas-poor despite its blue color.This suggests that UGCA 337 may have undergone gas stripping in the past.We also analyzed the possible origin of the diffuse HⅠ clouds located at the outskirts of NGC 5055,and speculate that they might be the remnant features of a merger event in the past.
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    Identifying Three New AGNs among Fermi Unidentified Gigaelectronvolt Sources

    Shun-Hao JiZhong-Xiang WangQiang-Meng HuangRuo-Heng Yang...
    257-267页
    查看更多>>摘要：We report our identification of three gigaelectronvolt γ-ray sources,4FGL J0502.6+0036,4FGL J1055.9+6507,and 4FGL J1708.2+5519,as Active Galactic Nuclei(AGNs).They are listed in the latest Fermi-Large Area Telescope source catalog as unidentified ones.We find that the sources all showed γ-ray flux variations in recent years.Using different survey catalogs,we are able to find a radio source within the error circle of each source's position.Further analysis of optical sources in the fields allows us to determine the optical counterparts,which showed similar variation patterns to those seen in γ-rays.The optical counterparts have reported redshifts of 0.6,1.5,and 2.3,respectively,estimated from photometric measurements.In addition,we also obtain an X-ray spectrum of 4FGL J0502.6+0036 and a flux upper limit on the X-ray emission of 4FGL J1055.9+6507 by analyzing the archival data.The broadband spectral energy distributions of the three sources from radio to γ-rays are constructed.Comparing mainly the γ-ray properties of the three sources with those of different sub-classes of AGNs,we tentatively identify them as blazars.Followup optical spectroscopy is highly warranted for obtaining their spectral features and thus verifying the identification.
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    Calculating the Excitation Temperature for H2CO Absorption Lines in Molecular Clouds

    Jia BuJarken EsimbekJianjun ZhouToktarkhan Komesh...
    268-271页
    查看更多>>摘要：The excitation temperature Tex for molecular emission and absorption lines is an essential parameter for interpreting the molecular environment.This temperature can be obtained by observing multiple molecular transitions or hyperfine structures of a single transition,but it remains unknown for a single transition without hyperfine structure lines.Earlier H2CO absorption experiments for a single transition without hyperfine structures adopted a constant value of Tex,which is not correct for molecular regions with active star formation and H Ⅱregions.For H2CO,two equations with two unknowns may be used to determine the excitation temperature Tex and the optical depth τ,if other parameters can be determined from measurements.Published observational data of the 4.83 GHz(λ=6 cm)H2CO(110-111)absorption line for three star formation regions,W40,M17 and DR17,have been used to verify this method.The distributions of Tex in these sources are in good agreement with the contours of the H110α emission of the H Ⅱ regions in M17 and DR17 and with the H2CO(1 10-1 11)absorption in W40.The distributions of Tex in the three sources indicate that there can be significant variation in the excitation temperature across star formation and H n regions and that the use of a fixed(low)value results in misinterpretation.
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