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J/A+A/613/A11       SDC13 NH3(1,1) and NH3(2,2) datacubes  (Williams+, 2018)

Gravity drives the evolution of infrared dark hubs: JVLA observations of SDC13. Williams G.M., Peretto N., Avison A., Duarte-Cabral A., Fuller G.A. <Astron. Astrophys. 613, A11 (2018)> =2018A&A...613A..11W (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Interferometry ; Molecular clouds Keywords: stars: formation - stars: massive - ISM: clouds - ISM: kinematics and dynamics - ISM: structure Abstract: Converging networks of interstellar filaments, that is hubs, have been recently linked to the formation of stellar clusters and massive stars. Understanding the relationship between the evolution of these systems and the formation of cores and stars inside them is at the heart of current star formation research. The goal is to study the kinematic and density structure of the SDC13 prototypical hub at high angular resolution to determine what drives its evolution and fragmentation. We have mapped SDC13, a ∼1000M infrared dark hub, in NH3(1,1) and NH3(2,2) emission lines, with both the Jansky Very Large Array and Green Bank Telescope. The high angular resolution achieved in the combined dataset allowed us to probe scales down to 0.07pc. After fitting the ammonia lines, we computed the integrated intensities, centroid velocities and line widths, along with gas temperatures and H2 column densities. The mass-per-unit-lengths of all four hub filaments are thermally super- critical, consistent with the presence of tens of gravitationally bound cores identified along them. These cores exhibit a regular separation of ∼0.37±0.16pc suggesting gravitational instabilities running along these super-critical filaments are responsible for their fragmentation. The observed local increase of the dense gas velocity dispersion towards starless cores is believed to be a consequence of such fragmentation process. Using energy conservation arguments, we estimate that the gravitational to kinetic energy conversion efficiency in the SDC13 cores is ∼35%. We see velocity gradient peaks towards ∼63% of cores as expected during the early stages of filament fragmentation. Another clear observational signature is the presence of the most massive cores at the filaments' junction, where the velocity dispersion is largest. We interpret this as the result of the hub morphology generating the largest acceleration gradients near the hub centre. We propose a scenario for the evolution of the SDC13 hub in which filaments first form as post-shock structures in a supersonic turbulent flow. As a result of the turbulent energy dissipation in the shock, the dense gas within the filaments is initially mostly subsonic. Then gravity takes over and starts shaping the evolution of the hub, both fragmenting filaments and pulling the gas towards the centre of the gravitational well. By doing so, gravitational energy is converted into kinetic energy in both local (cores) and global (hub centre) potential well minima. Furthermore, the generation of larger gravitational acceleration gradients at the filament junctions promotes the formation of more massive cores. Description: The FITS files of the JVLA+GBT combined data cubes in NH3(1,1) and NH3(2,2) molecular line emission, towards the SDC13 infrared dark cloud. The combined spectral resolution is 0.049km/s. The rest frequencies of the NH3(1,1) and NH3(2,2) lines are 23.694GHz and 23.723GHz. The brightness intensity unit is Jy per beam. The data was combined in CASA feather. Right ascension and declination coordinates are in the J2000 epoch. The central cloud coordinate is 18:14:30.0, -17:32:50.0, with a systemic cloud velocity of 37km/s. Objects: ----------------------------------------------------------------------- RA (2000) DE Designation(s) ----------------------------------------------------------------------- 18 14 30.0 -17 32 50 SDC13 = [PFA2014] SDC13 ----------------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 175 2 List of fits datacubes fits/* 0 2 Individual datacubes
See also: J/A+A/561/A83 : SDC13 infrared dark clouds spectra (Peretto+, 2014) Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 22 I3 --- Nx Number of pixels along X-axis 24- 26 I3 --- Ny Number of pixels along Y-axis 28- 30 I3 --- Nz Number of slices 32- 52 A21 --- Obs.Date Observation date 54- 60 F7.1 m/s bVRAD Lower value of VRAD interval 62- 68 F7.1 m/s BVRAD Upper value of VRAD interval 70- 76 F7.4 m/s dVRAD VRAD resolution 78- 83 I6 Kibyte size Size of FITS file 85- 96 A12 --- FileName Name of FITS file, in subdirectory fits 98-175 A78 --- Title Title of the FITS file
Acknowledgements: Gwenllian Williams, williamsgm8(at)>
(End) Gwenllian Williams [Cardiff Univ., UK], Patricia Vannier [CDS] 26-Jan-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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