skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: The Peculiar Filamentary H i Structure of NGC 6145

Abstract

In this paper, we report the peculiar H i morphology of the cluster spiral galaxy NGC 6145, which has a 150 kpc H i filament on one side that is nearly parallel to its major axis. This filament is made up of several H i clouds and the diffuse H i gas between them, with no optical counterparts. We compare its H i distribution with other one-sided H i distributions in the literature and find that the overall H i distribution is very different from the typical tidal and ram-pressure stripped H i shape, and that its morphology is inconsistent with that of a pure accretion event. Only ∼30% of the total H i gas is anchored on the stellar disk, while most of the H i gas forms the filament in the west. At a projected distance of 122 kpc, we find a massive elliptical companion (NGC 6146) with extended radio emission whose axis points to an H i gap in NGC 6145. The velocity of the H i filament shows an overall line-of-sight motion of 80–180 km s{sup −1} with respect to NGC 6145. Using the long-slit spectra of NGC 6145 along its major stellar axis, we findmore » that some outer regions show enhanced star formation, while in contrast, almost no star formation activities are found in its center (<2 kpc). Pure accretion, tidal, or ram-pressure stripping are not likely to produce the observed H i filament. An alternative explanation is the jet stripping from NGC 6146, although direct evidence for a jet-cold gas interaction has not been found.« less

Authors:
; ;  [1];  [2]; ; ; ;  [3]
  1. CAS Key Laboratory for Research in Galaxies and Cosmology, Department of Astronomy, University of Science and Technology of China, Hefei, Anhui 230026 (China)
  2. Australia Telescope National Facility, CSIRO Astronomy and Space Science, P.O. Box 76, Epping, NSW 1710 (Australia)
  3. Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Astronomical Society, 80 Nandan Road, Shanghai 200030 (China)
Publication Date:
OSTI Identifier:
22663345
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (Online); Journal Volume: 154; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ATOMS; CLOUDS; COMPARATIVE EVALUATIONS; COSMIC RADIO SOURCES; DISTANCE; FILAMENTS; GALAXIES; GALAXY CLUSTERS; JETS; MORPHOLOGY; SHAPE; STAR CLUSTERS; STARS; STRIPPING; VELOCITY

Citation Formats

Wang, Enci, Kong, Xu, Mou, Guobin, Wang, Jing, Guo, Fulai, Lin, Lin, Li, Cheng, and Xiao, Ting, E-mail: ecwang16@ustc.edu.cn, E-mail: xkong@ustc.edu.cn. The Peculiar Filamentary H i Structure of NGC 6145. United States: N. p., 2017. Web. doi:10.3847/1538-3881/AA7DDE.
Wang, Enci, Kong, Xu, Mou, Guobin, Wang, Jing, Guo, Fulai, Lin, Lin, Li, Cheng, & Xiao, Ting, E-mail: ecwang16@ustc.edu.cn, E-mail: xkong@ustc.edu.cn. The Peculiar Filamentary H i Structure of NGC 6145. United States. doi:10.3847/1538-3881/AA7DDE.
Wang, Enci, Kong, Xu, Mou, Guobin, Wang, Jing, Guo, Fulai, Lin, Lin, Li, Cheng, and Xiao, Ting, E-mail: ecwang16@ustc.edu.cn, E-mail: xkong@ustc.edu.cn. Tue . "The Peculiar Filamentary H i Structure of NGC 6145". United States. doi:10.3847/1538-3881/AA7DDE.
@article{osti_22663345,
title = {The Peculiar Filamentary H i Structure of NGC 6145},
author = {Wang, Enci and Kong, Xu and Mou, Guobin and Wang, Jing and Guo, Fulai and Lin, Lin and Li, Cheng and Xiao, Ting, E-mail: ecwang16@ustc.edu.cn, E-mail: xkong@ustc.edu.cn},
abstractNote = {In this paper, we report the peculiar H i morphology of the cluster spiral galaxy NGC 6145, which has a 150 kpc H i filament on one side that is nearly parallel to its major axis. This filament is made up of several H i clouds and the diffuse H i gas between them, with no optical counterparts. We compare its H i distribution with other one-sided H i distributions in the literature and find that the overall H i distribution is very different from the typical tidal and ram-pressure stripped H i shape, and that its morphology is inconsistent with that of a pure accretion event. Only ∼30% of the total H i gas is anchored on the stellar disk, while most of the H i gas forms the filament in the west. At a projected distance of 122 kpc, we find a massive elliptical companion (NGC 6146) with extended radio emission whose axis points to an H i gap in NGC 6145. The velocity of the H i filament shows an overall line-of-sight motion of 80–180 km s{sup −1} with respect to NGC 6145. Using the long-slit spectra of NGC 6145 along its major stellar axis, we find that some outer regions show enhanced star formation, while in contrast, almost no star formation activities are found in its center (<2 kpc). Pure accretion, tidal, or ram-pressure stripping are not likely to produce the observed H i filament. An alternative explanation is the jet stripping from NGC 6146, although direct evidence for a jet-cold gas interaction has not been found.},
doi = {10.3847/1538-3881/AA7DDE},
journal = {Astronomical Journal (Online)},
number = 2,
volume = 154,
place = {United States},
year = {Tue Aug 01 00:00:00 EDT 2017},
month = {Tue Aug 01 00:00:00 EDT 2017}
}