Ring structure and warp of NGC 5907: Interaction with dwarf galaxies

Zhaohui Shang, Zhongyuan Zheng, Elias Brinks, Jiansheng Chen, David Burstein, S. U. Hongjun, Yong I.K. Byun, Licai Deng, Zugan Deng, Xiaohui Fan, Zhaoji Jiang, L. I. Yong, Weipeng Lin, Feng Ma, Wei Hsin Sun, Beverley Wills, Rogier A. Windhorst, W. U. Hong, Xiaoyang Xia, X. U. WenSuijian Xue, Haojing Yan, X. U. Zhou, Jin Zhu, Zhenlong Zou

Research output: Contribution to journalArticlepeer-review

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Abstract

The edge-on, nearby spiral galaxy NGC 5907 has long been used as the prototype of a "noninteracting" warped galaxy. We report here the discovery of two interactions with companion dwarf galaxies that substantially change this picture. First, a faint ring structure is discovered around this galaxy that is likely due to the tidal disruption of a companion dwarf spheroidal galaxy. The ring is elliptical in shape with the center of NGC 5907 close to one of the ring's foci. This suggests that the ring material is in orbit around NGC 5907. No gaseous component to the ring has been detected either with deep Hα images or in Very Large Array H i 21 cm line maps. The visible material in the ring has an integrated luminosity ≤108 L, and its brightest part has a color R - I ∼ 0.9. All of these properties are consistent with the ring being a tidally disrupted dwarf spheroidal galaxy. Second, we find that NGC 5907 has a dwarf companion galaxy, PGC 54419, which is projected to be only 36.9 kpc from the center of NGC 5907, close in radial velocity (ΔV = 45 km s-1) to the giant spiral galaxy. This dwarf is seen at the tip of the H I warp and in the direction of the warp. Hence, NGC 5907 can no longer be considered noninteracting but is obviously interacting with its dwarf companions much as the Milky Way interacts with its dwarf galaxies. These results, coupled with the finding by others that dwarf galaxies tend to be found around giant galaxies, suggest that tidal interaction with companions, even if containing a mere 1% of the mass of the parent galaxy, might be sufficient to excite the warps found in the disks of many large spiral galaxies.

Original languageEnglish
Pages (from-to)L23-L26
JournalAstrophysical Journal
Volume504
Issue number1 PART II
DOIs
Publication statusPublished - 1998

Bibliographical note

Funding Information:
We thank McDonald Observatory for supporting part of the observations and data reductions, David Spergel for a helpful conversation, the VLA personnel for efficient service, and the anonymous referee for helpful comments. This research is supported in part by the Chinese National Natural Science Foundation (CNNSF) and by the US National Science Foundation (NSF grant INT-93-01805).

Funding Information:
1Partially based on observations taken with the Very Large Array of the National Radio Astronomy Observatory is a facility of the National Science Foundation operated by a cooperative agreement with Associated Universities, Inc. 2 Beijing Astronomical Observatory, Chinese Academy of Sciences, Beijing 100080, China. 3Department of Astronomy, University of Texas at Austin, Austin, TX 78712; shang@astro.as.utexas.edu. 4Beijing Astrophysics Center, Beijing, 100871, China. 5 Departamento de Astronomía, Universidad de Guanajuato, Apartado Postal 144, Guanajuato, Gto. 36000, Mexico. 6Department of Physics and Astronomy, Box 871504, Arizona State University, Tempe, AZ 85287-1504. 7Institute of Astronomy, National Central University, Chung-Li, Taiwan. 8Graduate School, Chinese Academy of Sciences, Beijing 100080, China. 9Princeton University Observatory, Princeton, New Jersey, 08544. 10Department of Physics, Tianjin Normal University, China.

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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