Herschel observations of water vapour in Markarian 231
文献类型：期刊论文
| 作者 | Gonzalez-Alfonso, E.1; Fischer, J.2; Isaak, K.3; Rykala, A.3; Savini, G.4; Spaans, M.5; van der Werf, P.6; Meijerink, R.6; Israel, F. P.6; Loenen, A. F.6 |
| 刊名 | ASTRONOMY & ASTROPHYSICS
 |
| 出版日期 | 2010-07-01 |
| 卷号 | 518页码:L43 |
| 关键词 | ISM: molecules galaxies: ISM galaxies: individual: Mrk 231 line: formation infrared: ISM submillimeter: galaxies |
| ISSN号 | 0004-6361 |
| 英文摘要 | The Ultra luminous infrared galaxy (ULIRG) Mrk 231 reveals up to seven rotational lines of water (H(2)O) in emission, including a very high-lying (Eupper = 640 K) line detected at a 4 sigma level, within the Herschel/SPIRE wavelength range (190 < lambda(mu m) < 640), whereas PACS observations show one H(2)O line at 78 mu m in absorption, as found for other H(2)O lines previously detected by ISO. The absorption/emission dichotomy is caused by the pumping of the rotational levels by far-infrared radiation emitted by dust, and subsequent relaxation through lines at longer wavelengths, which allows us to estimate both the column density of H(2)O and the general characteristics of the underlying far-infrared continuum source. Radiative transfer models including excitation through both absorption of far-infrared radiation emitted by dust and collisions are used to calculate the equilibrium level populations of H(2)O and the corresponding line fluxes. The highest-lying H(2)O lines detected in emission, with levels at 300-640 K above the ground state, indicate that the source of far-infrared radiation responsible for the pumping is compact (radius = 110-180 pc) and warm (T(dust) = 85-95 K), accounting for at least 45% of the bolometric luminosity. The high column density, N(H(2)O) similar to 5 x 10(17) cm(-2), found in this nuclear component, is most probably the consequence of shocks/cosmic rays, an XDR chemistry, and/or an "undepleted chemistry" where grain mantles are evaporated. A more extended region, presumably the inner region of the 1-kpc disk observed in other molecular species, could contribute to the flux observed in low-lying H(2)O lines through dense hot cores, and/or shocks. The H(2)O 78 mu m line observed with PACS shows hints of a blue-shifted wing seen in absorption, possibly indicating the occurrence of H(2)O in the prominent outflow detected in OH (Fischer et al. 2010, A&A, 518, L41). Additional PACS/HIFI observations of H(2)O lines are required to constrain the kinematics of the nuclear component, as well as the distribution of H(2)O relative to the warm dust. |
| WOS标题词 | Science & Technology ; Physical Sciences |
| 学科主题 | Astronomy & Astrophysics |
| 类目[WOS] | Astronomy & Astrophysics |
| 研究领域[WOS] | Astronomy & Astrophysics |
| 关键词[WOS] | ULTRALUMINOUS INFRARED GALAXIES ; EXCITATION ; NUCLEI ; H2O |
| 收录类别 | SCI |
| 语种 | 英语 |
| WOS记录号 | WOS:000281527200044 |
| 公开日期 | 2011-11-23 |
| 源URL | [http://159.226.72.40/handle/332002/1123]  |
| 专题 | 紫金山天文台_星系中的恒星形成研究团组 |
| 作者单位 | 1.Univ Alcala de Henares, Dept Fis, Madrid 28871, Spain 2.USN, Res Lab, Remote Sensing Div, Washington, DC 20375 USA 3.ESTEC SRE SA, Res & Sci Support Dept, ESA Astrophys Missions Div, NL-2201 AZ Noordwijk, Netherlands 4.UCL, Dept Phys & Astron, London WC1E 6BT, England 5.Univ Groningen, Kapteyn Astron Inst, NL-9700 AV Groningen, Netherlands 6.Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands 7.Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA 8.Univ Crete, Dept Phys, Iraklion 71003, Greece 9.Chalmers, Onsala Space Observ, S-43992 Onsala, Sweden 10.MPIfR, D-53121 Bonn, Germany |
| 推荐引用方式 GB/T 7714 | Gonzalez-Alfonso, E.,Fischer, J.,Isaak, K.,et al. Herschel observations of water vapour in Markarian 231[J]. ASTRONOMY & ASTROPHYSICS,2010,518:L43. |
| APA | Gonzalez-Alfonso, E..,Fischer, J..,Isaak, K..,Rykala, A..,Savini, G..,...&Gao, Y..(2010).Herschel observations of water vapour in Markarian 231.ASTRONOMY & ASTROPHYSICS,518,L43. |
| MLA | Gonzalez-Alfonso, E.,et al."Herschel observations of water vapour in Markarian 231".ASTRONOMY & ASTROPHYSICS 518(2010):L43. |
入库方式： OAI收割
来源：紫金山天文台
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