ner_tags: O O O O O O O O O O O B-Wavelength I-Wavelength O B-Wavelength 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 B-CelestialObject I-CelestialObject O O O O O O O O O B-CelestialObject I-CelestialObject B-CelestialObject I-CelestialObject 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 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 B-Wavelength I-Wavelength O O O B-Wavelength I-Wavelength 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-Citation I-Citation I-Citation 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 B-Wavelength I-Wavelength O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula B-Citation I-Citation I-Citation O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula 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 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 B-Citation I-Citation I-Citation I-Citation O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula 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 O O O B-Telescope O O O B-CelestialObject I-CelestialObject O O O O O O O B-Wavelength B-Wavelength B-Wavelength O O B-Wavelength I-Wavelength O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength O O O O B-Wavelength I-Wavelength O O O O O O O O O B-Wavelength I-Wavelength O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O O B-Database I-Database I-Database B-Database O O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula O O O O B-Citation I-Citation I-Citation I-Citation O O O B-Tag O O O O O O O O O O O O O O B-CelestialObject I-CelestialObject O O O O O B-Telescope O O O O O O O O O O O O B-Wavelength I-Wavelength I-Wavelength I-Wavelength 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-Software I-Software I-Software I-Software O B-Software 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
tokens: it with the stellar mass derived using the optical colors. The H α and NUV emission were used to derive the SFR in the disk. We then discuss the importance of NGC 4701 for understanding the morphological classification of late-type dwarf galaxies and accretion-driven star formation in extended H i disks. Throughout the paper we will assume the distance of NGC 4701 to be 17.1 Mpc. 2. The Bulgeless Spiral Galaxy NGC 4701 NGC 4701 was studied as part of a follow-up H i study of bulgeless disk galaxies (Das et al. 2012 ). It is a nearby spiral galaxy that has often been classified as a blue dwarf galaxy (Vanzi et al. 2009 ) on account of its bright, star-forming disk and small size. It has a small, stellar disk of diameter 8.3 kpc in the K band but in the B band the disk appears far more extended and has a diameter of 13.7 kpc (Table 1 and Figure 1 ). The inner disk has a very compact bright nucleus that is due to nuclear star clusters (Georgiev Böker 2014 ); such clusters have been observed in many bulgeless galaxies (Walcher et al. 2005 ). The nucleus has a bright, slightly off-center hard X-ray source (Lemons et al. 2015 ) that may be due to an active galactic nucleus (AGN; Desroches Ho 2009 ). The disk is very rich in H i gas and has a flux of S ν = 58.2 Jy km s −1 (Popping Braun 2011 ), which corresponds to a mass of M (H i ) = 4 × 10 9 M ⊙ . The H i spectral line width indicates that the disk is possibly extended. The molecular hydrogen gas has a double-horned structure about the nucleus (Vanzi et al. 2009 ) and has a flux of 2.90 K km s −1 (Böker et al. 2003 ) or 13.92 Jy km s −1 . At a distance of 17.10 Mpc (Tully et al. 2009 ), this corresponds to a molecular gas mass of M (H 2 ) = 4.48 × 10 7 M ⊙ . The molecular gas appears to be centrally concentrated, with a total width of ∼150 to 170 km s −1 and a rotation velocity ∼100 km s −1 (Popping Braun 2011 ). Figure 1. HCT optical images of NGC 4701. Clockwise from the top left are the B-, V-, I -, and R- band images. The dashed ellipse in white is the R 25 radius of the galaxy in the B band and is 108′′. The V -band emission extends out to 1/2 R 25 and the B -band extends to 2/3 R 25 approximately. Table 1 Parameters of NGC 4701 Notes. The parameters are from the NASA Extragalactic Database (NED). a The inclination was calculated from the galaxy major and minor axis ratios in the optical band i.e., inc = Cos −1 (179/216). b Tully Fisher distance (Tully et al. 2009 ). 3. H <sc>i</sc> Observations and Data Analysis 3.1. Observations and Moment Maps The H i observations of NGC 4701 were carried out with the GMRT during 2009 November. The baseband bandwidth used was 8 MHz for the H i 21 cm line observations, giving a velocity resolution of 13.6 km s −1 . Further details on the observations are given in Table 2 . To reduce the data the Astronomical Image Processing System ( AIPS ) software package was used. The flux densities are on the scale of mJy (Baars et al. 1977 ), with flux density