中国科学院紫金山天文台机构知识库
Advanced  
PMO OpenIR  > 星系中的恒星形成研究团组  > 期刊论文
题名: Herschel Spectroscopy of the Taffy Galaxies (UGC 12914/12915=VV 254): Enhanced [C II] Emission in the Collisionally Formed Bridge
作者: Peterson, B. W.; Appleton, P. N.; Bitsakis, T.; Guillard, P.; Alatalo, K.; Boulanger, F.; Cluver, M.; Duc, P. -A.; Falgarone, E.; Gallagher, S.; Gao, Y.; Helou, G.; Jarrett, T. H.; Joshi, B.; Lisenfeld, U.; Lu, N.; Ogle, P.; des Forets, G. Pineau; van der Werf, P.; Xu, C. K.
刊名: ASTROPHYSICAL JOURNAL
出版日期: 2018
卷号: 855, 期号:2, 页码:141
英文摘要: Using the PACS and SPIRE spectrometers on board Herschel, we obtained observations of the Taffy galaxies (UGC 12914/12915) and bridge. The Taffy system is believed to be the result of a face-on collision between two gas-rich galaxies, in which the stellar disks passed through each other, but the gas was dispersed into a massive H I and molecular bridge between them. Emission is detected and mapped in both galaxies and the bridge in the [C II] 157.7 mu m and [O I]63.2 mu m fine-structure lines. Additionally, SPIRE FTS spectroscopy detects the [C I] P-3(2) -> P-3(1)(809.3 GHz) and [C I] P-3(1) -> P-3(0)(492.2 GHz) neutral carbon lines, and weakly detects high-J CO transitions in the bridge. These results indicate that the bridge is composed of a warm multi-phase medium consistent with shock and turbulent heating. Despite low star formation rates in the bridge, the [C II] emission appears to be enhanced, reaching [C II]/FIR ratios of 3.3% in parts of the bridge. Both the [C II] and [O I] lines show broad intrinsic multi-component profiles, similar to those seen in previous CO (1-0) and H I observations. The [C II] emission shares similar line profiles with both the double-peaked H I profiles and shares a high-velocity component with single-peaked CO profiles in the bridge, suggesting that the [C II] emission originates in both the neutral and molecular phases. We show that it is feasible that a combination of turbulently heated H-2 and high column-density H I, resulting from the galaxy collision, is responsible for the enhanced [C II] emission.
语种: 英语
WOS记录号: WOS:000427697100010
Citation statistics:
内容类型: 期刊论文
URI标识: http://libir.pmo.ac.cn/handle/332002/18069
Appears in Collections:星系中的恒星形成研究团组_期刊论文

Files in This Item:
File Name/ File Size Content Type Version Access License
2018110.pdf(2508KB)期刊论文作者接受稿限制开放View 联系获取全文
Service
Recommend this item
Sava as my favorate item
Show this item's statistics
Export Endnote File
Google Scholar
Similar articles in Google Scholar
[Peterson, B. W.]'s Articles
[Appleton, P. N.]'s Articles
[Bitsakis, T.]'s Articles
CSDL cross search
Similar articles in CSDL Cross Search
[Peterson, B. W.]‘s Articles
[Appleton, P. N.]‘s Articles
[Bitsakis, T.]‘s Articles
Related Copyright Policies
Null
Social Bookmarking
Add to CiteULike Add to Connotea Add to Del.icio.us Add to Digg Add to Reddit
文件名: 2018110.pdf
格式: Adobe PDF
所有评论 (0)
暂无评论
 
评注功能仅针对注册用户开放,请您登录
您对该条目有什么异议,请填写以下表单,管理员会尽快联系您。
内 容:
Email:  *
单位:
验证码:   刷新
您在IR的使用过程中有什么好的想法或者建议可以反馈给我们。
标 题:
 *
内 容:
Email:  *
验证码:   刷新

Items in IR are protected by copyright, with all rights reserved, unless otherwise indicated.

 

 

Valid XHTML 1.0!
Copyright © 2007-2018  中国科学院紫金山天文台 - Feedback
Powered by CSpace