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J/MNRAS/447/1996    Ophiuchus molecular cloud CO observations     (White+, 2015)

The James Clerk Maxwell telescope Legacy Survey of the Gould Belt: a molecular line study of the Ophiuchus molecular cloud. White G.J., Drabek-Maunder E., Rosolowsky E., Ward-Thompson D., Davis C.J., Gregson J., Hatchell J., Etxaluze M., Stickler S., Buckle J., Johnstone D., Friesen R., Sadavoy S., Natt K.V., Currie M., Richer J.S., Pattle K., Spaans M., Di Francesco J., Hogerheijde M.R. <Mon. Not. R. Astron. Soc., 447, 1996-2020 (2015)> =2015MNRAS.447.1996W (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds ; Carbon monoxide ; Morphology Keywords: molecular data - stars: formation - ISM: jets and outflows - ISM: kinematics and dynamics - submillimetre: general Abstract: CO, 13CO, and C18O J=3-2 observations are presented of the Ophiuchus molecular cloud. The 13CO and C18O emission is dominated by the Oph A clump, and the Oph B1, B2, C, E, F, and J regions. The optically thin(ner) C18O line is used as a column density tracer, from which the gravitational binding energy is estimated to be 4.5x1039J (2282Mkm2/s2). The turbulent kinetic energy is 6.3x1038J (320Mkm2/s2), or seven times less than this, and therefore the Oph cloud as a whole is gravitationally bound. 30 protostars were searched for high-velocity gas, with 8 showing outflows, and 20 more having evidence of high-velocity gas along their lines of sight. The total outflow kinetic energy is 1.3x1038J (67Mkm2/s2), corresponding to 21 percent of the cloud's turbulent kinetic energy. Although turbulent injection by outflows is significant, but does not appear to be the dominant source of turbulence in the cloud. 105 dense molecular clumplets were identified, which had radii ∼0.01-0.05pc, virial masses ∼0.1-12M, luminosities ∼, and excitation temperatures ∼10-50K. These are consistent with the standard Giant Molecular Cloud (GMC) based size-linewidth relationships, showing that the scaling laws extend down to size scales of hundredths of a parsec, and to subsolar-mass condensations. There is however no compelling evidence that the majority of clumplets are undergoing free-fall collapse, nor that they are pressure confined. Description: The HARP (Heterodyne Array Receiver Programme) receiver contains an array of 16 heterodyne detectors, arranged in a 4x4 footprint on the sky. HARP was used to make maps in the CO, 13CO, and C18O J=3-2 lines, where it has a beamsize of 14 arcsec at 345GHz (corresponding to a linear size of 0.008pc at the Ophiuchus cloud). The molecular line observations were made up of 3.2h of CO data taken in 2008 February and March and 16.6h of 13CO and C18O observations taken during 2008 March, July, and August. The maps were observed using the standard on-the-fly mapping mode, and referenced against an off-source reference position at RA(J2000)=16:38:00.6, Dec(J2000)=-25:36:42.0, which had been verified to show no line emission from examination of 60s position-switched 'stare' observation in CO. The CO data were taken with the AutoCorrelation Spectrometer and Imaging System (ACSIS) using its 250 MHz dual subband mode that provided 4096 channels, each with a velocity resolution ∼0.05km/s per channel. The 13CO/C18O data were taken simultaneously with each other, with each subband having a central rest frequency of 330.587 or 329.330GHz, respectively, providing a velocity resolution ∼0.055km/s. All of the isotopologue maps were then further convolved to a resolution of 0.1km/s. To support the JCMT observations, a deep United Kingdom Infrared Telescope (UKIRT) image of the Oph region was obtained using a near-IR K-band filter, and a matching narrow-band H2 image. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table5.dat 70 105 The clumplet catalogue
See also: J/A+A/430/549 : C18O/C17O near rho Oph (Wouterloot+, 2005) J/A+A/472/519 : N2H+(1-0) maps of Ophiuchus main cloud (Andre+, 2007) J/A+A/510/A98 : 12C18O(3-2) map of rho Oph A (Liseau+, 2010) J/A+A/587/A118 : N2H+, N2D+ & C17O spectra in Ophiuchus (Punanova+, 2016) Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Sequential number 5- 6 I2 h RAh Clump centre right ascension (J2000) 8- 9 I2 min RAm Clump centre right ascension (J2000) 11- 14 F4.1 s RAs Clump centre right ascension (J2000) 16 A1 --- DE- Clump centre declination sign (J2000) 17- 18 I2 deg DEd Clump centre declination (J2000) 20- 21 I2 arcmin DEm Clump centre declination (J2000) 23- 26 F4.1 arcsec DEs Clump centre declination (J2000) 28- 32 F5.1 arcsec Maj Major axis of the clump deconvolved from the beam 34- 37 F4.1 arcsec Min Minor axis of the clump deconvolved from the beam 39- 41 I3 deg PA [] Position angle (measured east of north) 43- 46 F4.2 pc Rad Deconvolved radius of the clump as defined by Rosolowsky et al. (2006PASP..118..590R) 48- 51 F4.2 km/s Vlsr Centre LSR velocity of the clump as determined from the C18O data 53- 56 F4.2 km/s sigma Centre velocity dispersion of the clump as determined from the C18O data 58- 62 F5.2 Msun MassVir Viral mass 64- 70 F7.5 Lum Luminosity estimated from the CO observations
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 26-May-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

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