Access to Astronomical Catalogues

← Click to display the menu
J/A+A/603/A10       ALMA view of G351.77-0.54                   (Beuther+, 2017)

Fragmentation and disk formation in high-mass star formation: The ALMA view of G351.77-0.54 at 0.06'' resolution. Beuther H., Walsh A.J., Johnston K.G., Henning T., Kuiper R., Longmore S.N., Walmsley S.M. <Astron. Astrophys. 603, A10 (2017)> =2017A&A...603A..10B (SIMBAD/NED BibCode)
ADC_Keywords: H II regions ; Interferometry Keywords: stars: formation - stars: massive - stars: individual: G351.77-0.54 - stars: winds, outflows - instrumentation: interferometers Abstract: The fragmentation of high-mass gas clumps and the formation of the accompanying accretion disks lie at the heart of high-mass star formation research. We resolve the small-scale structure around the high-mass hot core G351.77-0.54 to investigate its disk and fragmentation properties. Using the Atacama Large Millimeter Array at 690GHz with baselines exceeding 1.5km, we study the dense gas, dust, and outflow emission at an unprecedented spatial resolution of 0.06" (130AU at 2.2kpc). Within the inner few 1000AU, G351.77 is fragmenting into at least four cores (brightness temperatures between 58 and 201K). The central structure around the main submm source #1 with a diameter of ∼0.5" does not show additional fragmentation. While the CO(6-5) line wing emission shows an outflow lobe in the northwestern direction emanating from source #1, the dense gas tracer CH3CN shows a velocity gradient perpendicular to the outflow that is indicative of rotational motions. Absorption profile measurements against the submm source #2 indicate infall rates on the order of 10-4 to 10-3M/yr, which can be considered as an upper limit of the mean accretion rates. The position-velocity diagrams are consistent with a central rotating disk-like structure embedded in an infalling envelope, but they may also be influenced by the outflow. Using the CH3CN(37k-36k) k-ladder with excitation temperatures up to 1300K, we derive a gas temperature map for source #1 exhibiting temperatures often in excess of 1000K. Brightness temperatures of the submm continuum barely exceed 200K. This discrepancy between gas temperatures and submm dust brightness temperatures (in the optically thick limit) indicates that the dust may trace the disk mid-plane, whereas the gas could trace a hotter gaseous disk surface layer. We conduct a pixel-by-pixel Toomre gravitational stability analysis of the central rotating structure. The derived high Q values throughout the structure confirm that this central region appears stable against gravitational instability. Resolving for the first time a high-mass hot core at 0.06 resolution at submm wavelengths in the dense gas and dust emission allowed us to trace the fragmenting core and the gravitationally stable inner rotating disk-like structure. A temperature analysis reveals hot gas and comparably colder dust that may be attributed to different disk locations traced by dust emission and gas lines. The kinematics of the central structure #1 reveal contributions from a rotating disk, an infalling envelope, and potentially an outflow as well, whereas the spectral profile toward source #2 can be attributed to infall. Description: The target region G351.77-0.54 was observed with ALMA in cycle 2 in the 690GHz band with 42 antennas in the array. One noisy antenna and very short baselines have been flagged because of outlying amplitudes. This results in a baseline length coverage from 40m to almost ∼1.6km. The total duration of that one execution of one scheduling block was 1h40min with an on-target time of 35min. Because of the large number of antennas, even in such a short time, ALMA achieves an excellent uv-plane coverage. This results in an almost circular beam and allows us to recover spatial scales between approximately 0.06" and 2.7". The phase center of the observations was RA (J2000.0) 17:26:42.568 and Dec (J2000.0) -36:09:17.6. Objects: ------------------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------------------- 17 26 42.8 -36 09 17 G351.77-0.54 = IRAS 17233-360 ------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 162 26 List of fits files fits/* 0 26 Individual fits files
See also: Byte-by-byte Description of file: list.dat 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- 23 I4 --- Nx Number of pixels along X-axis 25- 28 I4 --- Ny Number of pixels along Y-axis 30- 52 A23 "date" Obs.date Observation date (YYYY-MM-DDThh:mm:ss.sss) 54- 58 F5.2 --- offsetX ? Offset in X 60- 63 F4.2 --- offsetY ? Offset in Y 65- 68 F4.2 --- doffset ? Offset resolution 70- 72 I3 km/s bVel ? Lower value of velocity interval or velocity 74- 77 F4.1 km/s BVel ? Upper value of velocity interval 79- 81 F3.1 km/s dVel ? Velocity resolution 83- 87 I5 Kibyte size Size of FITS file 89-111 A23 --- FileName Name of FITS file, in subdirectory fits 113-162 A50 --- Title Title of the FITS file
Acknowledgements: Henrik Beuther, beuther(at)mpia.de
(End) Patricia Vannier [CDS] 04-Apr-2017
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

catalogue service

© UDS/CNRS

Contact