ner_tags: O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula O O B-CelestialObject I-CelestialObject B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-TextGarbage O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model I-Model I-Model O O O O O O O O O B-Wavelength O B-Wavelength O O O O B-CelestialObject I-CelestialObject O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation B-CelestialObject I-CelestialObject O O O O O O O O O O B-Formula I-Formula I-Formula O O O O O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Telescope O O B-CelestialObject I-CelestialObject O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Model I-Model I-Model O O O O O O O O O O O O
tokens: starbursts that have inclination-corrected central brightness ( = 22.6 mag arcsec −2 for a kinematic inclination = 452) comparable to VCC 848 (Lelli et al. 2014 ). Because the rotation velocity gradient slope is proportional to the square root of local matter density for a solid-body rotation curve, we can infer that the merging event of VCC 848 has not built up an exceptionally compact core. 4.3. Dynamical and Baryonic Mass Profiles We use the rotation curve of the approaching half to determine the cumulative dynamical mass profiles (=/G), which are shown in Figure 5 . We also overplot mass profiles of the baryonic components, including stars and atomic and molecular gas, in Figure 5 . All of the profiles are extracted using the same geometric parameters as determined from the 2 dbat kinematic fitting. The stellar mass is estimated by using the ( g − i )–mass-to-light relation calibrated for Local Group dwarf galaxies (Zhang et al. 2017 ). Details about the procedure of stellar mass estimation are given in Paper I . We adopt a logarithmic stellar mass uncertainty of 0.2 dex, which is applicable to color-based mass estimation for low-dust-extinction cases (Zhang et al. 2017 ). The atomic gas mass is equal to the H i gas mass multiplied by a factor of 1.36 to account for helium. The molecular gas mass is indirectly inferred from the SFR estimated with H α luminosities (Catalan-Torrecilla et al. 2015 , Equation (10)) by adopting a constant molecular gas consumption timescale of (5.25 ± 2.5) × 10 −10 yr −1 found for nearby disk galaxies at (sub)kiloparsec scales (Bigiel et al. 2008 ; Leroy et al. 2008 ). 18 18 Another method of estimating the molecular gas mass is based on a metallicity-dependent gas-to-dust ratio (G/D). According to the G/D−metallicity relation from Rémy-Ruyer et al. ( 2014 ), VCC 848 is expected to have a of 3.00 ± 0.37 for (O/H) = 8.03 (Table 1 ). In addition, Grossi et al. ( 2015 ) determined a total dust mass of 10 5.01 M ⊙ (the value has been adjusted to reflect our adopted distance) within the central ∼30′′ of VCC 848. Therefore, the total gas mass (atomic plus molecular) within the central 30′′ is estimated to be , and hence the most likely molecular gas mass is ∼10 7.5 M ⊙ , found by subtracting the atomic gas contribution (Figure 5 ). This molecular gas mass is in reasonable agreement with that (10 7.6 M ⊙ ) inferred from the SFR-based method shown in Figure 5 . We choose to use the SFR-based method in this paper. This is because, besides their low spatial resolution, the Herschel images of VCC 848 generally have signal-to-noise ratios that are too low (except for the brightest star-forming sites) to allow for constructing a robust radial profile of dust mass densities. Figure 5. Accumulated radial profiles of the dynamical mass as well as the stellar, atomic, and molecular gas masses within the central 30′′. The same geometric parameters derived from the 2 dbat fitting of the H i velocity field (Figure 3 ) are used to