The Nuclear Source of the Galactic Wind in NGC 253. (arXiv:1908.06538v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gunthardt_G/0/1/0/all/0/1">G. I. Günthardt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Diaz_R/0/1/0/all/0/1">R. J. Díaz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aguero_M/0/1/0/all/0/1">M. P. Agüero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gimeno_G/0/1/0/all/0/1">G. Gimeno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dottori_H/0/1/0/all/0/1">H. Dottori</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Camperi_J/0/1/0/all/0/1">J. A. Camperi</a>
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$1.35), and the broad component seems
only comparable with those observed at very high star-forming rate galaxies.
The results indicate that the IRC would be the main source of the galactic
winds originated in the central region of NGC 253.
We present Br$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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