The Nuclear Source of the Galactic Wind in NGC 253

Abstract

We present Br$\gamma$ emission line kinematics of the nuclear region of NGC 253, recently known to host a strong galactic wind that limits the global star formation of the galaxy. We obtained high-resolution long-slit spectroscopic data with PHOENIX at Gemini-South, positioning the slit on the nucleus Infrared Core (IRC), close to the nuclear disk major axis. The spatial resolution was 0.35"($\sim$6 pc) and the slit length 14"($\sim$240 pc). The spectral resolution was $\sim$74000, unprecedented high for galactic nuclei observations at $\sim$2.1$\mu$m. The line profiles appear highly complex, with blue asymmetry up to 3.5'' away of the IRC, and red asymmetries further away to NE. Several Gaussian components are necessary to fit the profile, nevertheless a narrow and a wide ones predominate. The IRC presents kinematic widths above 700 kms${}^{-1}$ (FWZI), and broad component FWHM$\sim$400 kms${}^{-1}$, the highest detected in a nearby galaxy. At the IRC, the blue-shifted broad component displays a 90 km s${}^{-1}$ bump in radial velocity distribution, a feature we previously detected in molecular gas kinematics. The narrow component velocity dispersion ($\sim$32 kms${}^{-1}$) is within the expected for normal galaxies and LIRGs. Intermediate components (FWHM$\sim$150 kms${}^{-1}$, red-shifted to NE, blue-shifted to SW) appear at some positions, as well as weaker blue (-215 kms${}^{-1}$) and red line wings (+300 kms${}^{-1}$). The IRC depicts a large broad vs. narrow line flux-ratio (F(B)/F(N)$\sim$1.35), and the broad component seems only comparable with those observed at very high star-forming rate galaxies. The results indicate that the IRC would be the main source of the galactic winds originated in the central region of NGC 253.

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Cited by in corpus (2)

• Unveiling Kinematic Structure in the Starburst Heart of NGC 253
• Physical Conditions of the Ionized Superwind in NGC 253 with VLT/MUSE