eDIG-CHANGES. II. Project Design and Initial Results on NGC 3556

Author:

Li 李 Jiang-Tao 江涛ORCID,Lu 芦 Li-Yuan 李源ORCID,Qu 屈 Zhijie 稚杰ORCID,Benjamin Robert A.ORCID,Bregman Joel N.ORCID,Dettmar Ralf-JürgenORCID,English JayanneORCID,Fang 方 Taotao 陶陶ORCID,Irwin Judith A.ORCID,Jiang 姜 Yan 燕,Li 李 Hui 辉ORCID,Liu 刘 Guilin 桂琳ORCID,Martini PaulORCID,Rand Richard J.ORCID,Stein Yelena,Strong Andrew W.ORCID,Vargas Carlos J.ORCID,Wang Q. DanielORCID,Wang 王 Jing 菁ORCID,Wiegert TheresaORCID,Xu 许 Jianghui 蒋辉,Yang 杨 Yang 阳ORCID

Abstract

Abstract The extraplanar diffuse ionized gas (eDIG) represents ionized gases traced by optical/UV lines beyond the stellar extent of galaxies. We herein introduce a novel multislit narrow-band spectroscopy method to conduct spatially resolved spectroscopy of the eDIG around a sample of nearby edge-on disk galaxies (eDIG-CHANGES). In this paper, we introduce the project design and major scientific goals, as well as a pilot study of NGC 3556 (M108). The eDIG is detected to a vertical extent of a few kiloparsecs above the disk, comparable to the X-ray and radio images. We do not see significant vertical variation of the [N ii]/Hα line ratio. A rough examination of the pressure balance between different circumgalactic medium phases indicates the magnetic field is in a rough pressure balance with the X-ray emitting hot gas and may play an important role in the global motion of both the eDIG and the hot gas in the lower halo. At the location of an Hubble Space Telescope/Cosmic Origins Spectrograph observed UV bright background active galactic nucleus ∼29 kpc from the center of NGC 3556, the magnetic pressure is much lower than that of the hot gas and the ionized gas traced by UV absorption lines, although the extrapolation of the pressure profiles may cause some biases in this comparison. By comparing the position–velocity diagrams of the optical and CO lines, we also find the dynamics of the two gas phases are consistent with each other, with no evidence of a global inflow/outflow and a maximum rotation velocity of ∼150 km s−1.

Funder

National Natural Science Foundation of China

National Key R&D Program of China

science research grant from the China Manned Space Project

Deutsche Forschungsgemeinschaft

MCIU/AEI

Publisher

American Astronomical Society

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