The Virgo High-Resolution CO Survey: III. NGC 4254

Abstract

Abstract We present high-angular-resolution (${1\rlap {.}{}^{\mathrm {\prime \prime }}5}$-${5{}^{\mathrm {\prime \prime }}}$) interferometer observations of the ${{12\atop} \mathrm{CO}}$ ($J=1 \hbox{--} 0$) line emission in the central region of the SA(s)c galaxy NGC 4254 (M 99). The observations were obtained using the Nobeyama Millimeter-wave Array (NMA) during the course of a long-term CO-line survey of Virgo spirals. We present the spectra, channel maps, integrated intensity distributions, velocity fields, position–velocity diagrams, and compare the data with various optical images. The rotation velocity is already finite at the nucleus, or at least it rises steeply to $80 \,\mathrm{km} \,\mathrm{s}^{-1}$ within the central $1^{\prime\prime}$, indicating the existence of a massive core of $10^8 \,{{{M}_{\odot}}}$ within $1^{\prime\prime}$ (80 pc) radius. The CO intensity maps show that the inner disk has well-developed multiple spiral arms, winding out from a bar-shaped elongated molecular complex. In addition to the bisymmetric spiral arms, an asymmetric tightly wound arm with high molecular gas density is found to wind out from the molecular bar. The molecular spiral arms, particularly the tightly wound arm, well traces optical dark lanes, and are associated with $\mathrm{H}\alpha$ arms having many H ii regions. The inner asymmetric spiral structures can be explained by ram-pressure distortion of inter-arm low density regions of the inner disk by the intra-cluster gas wind, and is indeed reproduced by a hydrodynamical simulation.