J/A+A/582/A18 HI data cubes of 4 edge-on spiral galaxies (Allaert+, 2015) ================================================================================ HERschel Observations of Edge-on Spirals (HEROES). II. Tilted-ring modelling of the atomic gas disks. Allaert F., Gentile G., Baes M., De Geyter G., Hughes T.M., Lewis F., Bianchi S., De Looze I., Fritz J., Holwerda B.W., Verstappen J., Viaene S. =2015A&A...582A..18A (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Galaxies, nearby ; Galaxies, radio ; Galaxies, rotation ; H I data ; Interferometry ; Interstellar medium Keywords: galaxies: ISM - galaxies: structure - galaxies: kinematics and dynamics - galaxies: interactions Abstract: Edge-on galaxies can offer important insight into galaxy evolution because they are the only systems where the distribution of the different components can be studied both radially and vertically. The HEROES project was designed to investigate the interplay between the gas, dust, stars, and dark matter (DM) in a sample of 7 massive edge-on spiral galaxies. In this second HEROES paper, we present an analysis of the atomic gas content of 6 out of 7 galaxies in our sample. The remaining galaxy was recently analysed according to the same strategy. The primary aim of this work is to constrain the surface density distribution, the rotation curve, and the geometry of the gas disks in a homogeneous way. In addition we identify peculiar features and signs of recent interactions. We have constructed detailed tilted-ring models of the atomic gas disks based on new GMRT 21-cm observations of NGC 973 and UGC 4277 and re-reduced archival HI data of NGC 5907, NGC 5529 IC 2531, and NGC 4217. Potential degeneracies between different models were resolved by requiring good agreement with the data in various representations of the data cubes. From our modelling we find that all but one galaxy are warped along the major axis. In addition, we identify warps along the line of sight in three galaxies. A flaring gas layer is required to reproduce the data for only one galaxy, but (moderate) flares cannot be ruled out for the other galaxies either. A coplanar ring-like structure is detected outside the main disk of NGC 4217, which we suggest could be the remnant of a recent minor merger event. We also find evidence of a radial inflow of 15 +/-5km/s in the disk of NGC 5529, which might be related to the ongoing interaction with two nearby companions. For NGC 5907 the extended, asymmetric, and strongly warped outer regions of the HI disk also suggest a recent interaction. In contrast, the inner disks of these three galaxies (NGC 4217, NGC 5529, and NGC 5907) show regular behaviour and seem largely unaffected by the interactions. Our models further support earlier claims of prominent spiral arms in the disks of IC 2531 and NGC 5529. Finally, we detect a dwarf companion galaxy at a projected distance of 36 kpc from the centre of NGC 973. Description: The reduced and Cleaned HI data cubes of the HEROES galaxies NGC 973, UGC 4277, NGC 5529 and NGC 5907 are presented as FITS files. The equatorial coordinates and the beam FWHM, velocity resolution and rms noise of the data cubes are given in a separate table. NGC 973 and UGC 4277 were observed by the authors with the GMRT. The total time on source was 5.7 and 6.2 hours, respectively. For NGC 5529, the data were obtained by Kregel et al. (2004MNRAS.352..768K) using the Maxi-Short configuration of the WSRT, with a total time on source of 11.9 hours. Finally, NGC 5907 was observed by Shang et al. (1998ApJ...504L..23S) with the VLA in Modified C configuration. The total time on source was 4.7 hours. The raw interferometric data can be obtained from the online data archives of the telescopes in question. For IC 2531 and NGC 4217, the reduced data were made available to us by S. Peters (Peters et al., 2013arXiv1303.2463P) and M. Verheijen (Verheijen & Sancisi, 2001A&A...370..765V), respectively. We refer the user to the original papers for further questions or requests about the data. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file cubes.dat 126 4 Properties of the presented data cubes cubes/* . 4 FITS HI data cubes of four HEROES galaxies -------------------------------------------------------------------------------- Byte-by-byte Description of file: cubes.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 8 A8 --- Name Galaxy name 10- 11 I2 h RAh Right ascension (J2000.0) (NED) 13- 14 I2 min RAm Right ascension (J2000.0) (NED) 16- 20 F5.2 s RAs Right ascension (J2000.0) (NED) 22 A1 --- DE- Declination sign (J2000.0) 23- 24 I2 deg DEd Declination (J2000.0) (NED) 26- 27 I2 arcmin DEm Declination (J2000.0) (NED) 29- 32 F4.1 arcsec DEs Declination (J2000.0) (NED) 34- 37 F4.1 arcsec Bmaj Beam major axis FWHM 39- 42 F4.1 arcsec Bmin Beam minor axis FWHM 44- 47 F4.1 km/s dHVel Velocity resolution 49- 51 F3.1 mJy rms rms noise level (mJy/beam) (1) 53- 56 F4.2 arcsec/pix Scale Scale of the image 58- 60 I3 --- Nx Number of pixel along X-axis 62- 64 I3 --- Ny Number of pixel along Y-axis 66- 68 I3 --- Nz Number of slices 70- 90 A21 --- Date Observation date (YYYY-MM-DDThh:mm:ss.s) 92- 99 F8.3 km/s bHVel Lower value of heliocentric velocity 101-108 F8.3 km/s BHVel Upper value of heliocentric velocity 110-114 I5 Kibyte size Size of the fits file 116-126 A11 --- FileName Name of the fits file in subdirectory cubes -------------------------------------------------------------------------------- Note (1): Conversion to SI units: 1 mJy/beam = (1e-29)/(1.133*bmaj*bmin) W/(m^2^*Hz*arcsec^2^) with bmaj, bmin in arcsec -------------------------------------------------------------------------------- Acknowledgements: Flor Allaert, Flor.Allaert(at)UGent.be Refeences: Verstappen et al., Paper I 2013A&A...556A..54V ================================================================================ (End) Flor Allaert [Universiteit Gent], Patricia Vannier [CDS] 08-Sep-2015