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36 GHz methanol lines from nearby galaxies: maser or quasi-thermal emission?

文献类型：期刊论文

作者Humire, P.12; Henkel, C.10,11,12; Gong, Y.12; Leurini, S.9,12; Mauersberger, R.12; Levshakov, S. A.6,7,8; Winkel, B.12; Tarchi, A.9; Castangia, P.9; Malawi, A.11
刊名ASTRONOMY & ASTROPHYSICS
出版日期2020-01-17
卷号633页码:A106
关键词masers galaxies: spiral galaxies: individual: IC 342 galaxies: individual: Maffei 2 galaxies: ISM radio lines: galaxies
ISSN号0004-6361
DOI10.1051/0004-6361/201936330
产权排序3
英文摘要Methanol (CH3OH) is one of the most abundant interstellar molecules, offering a vast number of transitions to be studied, including many maser lines. However, while the strongest Galactic CH3OH lines, the so-called class II masers, show no indications for the presence of superluminous counterparts in external galaxies, the less luminous Galactic class I sources appear to be different. Here we report class I 36 GHz (lambda approximate to 0.8 cm) CH3OH 4(-1) -> 3(0) E line emission from the nearby galaxies Maffei 2 (D approximate to 6 Mpc) and IC 342 (D approximate to 3.5 Mpc), measured with the 100 m telescope at Effelsberg at three different epochs within a time span of about five weeks. The 36 GHz methanol line of Maffei 2 is the second most luminous among the sources detected with certainty outside the Local Group of galaxies. This is not matched by the moderate infrared luminosity of Maffei 2. Higher-resolution data are required to check whether this is related to its prominent bar and associated shocks. Upper limits for M 82, NGC 4388, NGC 5728 and Arp 220 are also presented. The previously reported detection of 36 GHz maser emission in Arp 220 is not confirmed. Nondetections are reported from the related class I 44 GHz (lambda approximate to 0.7 cm) methanol transition towards Maffei 2 and IC 342, indicating that this line is not stronger than its 36 GHz counterpart. In contrast to the previously detected 36 GHz CH3OH emission in NGC 253 and NGC 4945, our 36 GHz profiles towards Maffei 2 and IC 342 are similar to those of previously detected nonmasing lines from other molecular species. However, by analogy to our Galactic center region, it may well be possible that the 36 GHz methanol lines in Maffei 2 and IC 342 are composed of a large number of faint and narrow maser features that remain spatially unresolved. In view of this, a search for a weak broad 36 GHz line component would also be desirable in NGC 253 and NGC 4945.
WOS关键词STAR-FORMATION ; MOLECULAR CLOUDS ; ORION-KL ; NGC 253 ; SEARCH ; OH ; DISCOVERY ; ABUNDANCE ; DENSITY ; REGIONS
资助项目Menten ; RSF[19-12-00157]
WOS研究方向Astronomy & Astrophysics
语种英语
WOS记录号WOS:000508200600002
出版者EDP SCIENCES S A
资助机构Menten ; RSF
源URL[http://ir.xao.ac.cn/handle/45760611-7/3321]  
专题恒星形成与演化研究团组
新疆天文台_射电天文研究室
通讯作者Henkel, C.
作者单位1.Chinese Acad Sci, Key Lab Radio Astron, Urumqi 830011, Peoples R China
2.Chinese Acad Sci, Shanghai Astron Observ, Shanghai 200030, Peoples R China
3.GuangZhou Univ, Ctr Astrophys, Guangzhou 510006, Peoples R China
4.CSIRO, Australia Telescope Natl Facil, POB 76, Epping, NSW 1710, Australia
5.Univ Tasmania, Sch Nat Sci, Hobart, Tas 7001, Australia
6.Petersburg Nucl Phys Inst, Gatchina 188300, Russia
7.Electrotech Univ LETI, St Petersburg 197376, Russia
8.Ioffe Phys Tech Inst, St Petersburg 194021, Russia
9.INAF Osserv Astron Cagliari, Via Sci 5, I-09047 Selargius, CA, Italy
10.Chinese Acad Sci, Xinjiang Astron Observ, Urumqi 830011, Saudi Arabia
推荐引用方式
GB/T 7714		 Humire, P.,Henkel, C.,Gong, Y.,et al. 36 GHz methanol lines from nearby galaxies: maser or quasi-thermal emission?[J]. ASTRONOMY & ASTROPHYSICS,2020,633:A106.
APA Humire, P..,Henkel, C..,Gong, Y..,Leurini, S..,Mauersberger, R..,...&Tang, X..(2020).36 GHz methanol lines from nearby galaxies: maser or quasi-thermal emission?.ASTRONOMY & ASTROPHYSICS,633,A106.
MLA Humire, P.,et al."36 GHz methanol lines from nearby galaxies: maser or quasi-thermal emission?".ASTRONOMY & ASTROPHYSICS 633(2020):A106.

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来源：新疆天文台

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