J/MNRAS/426/1972 H2O Southern Galactic Plane Survey, HOPS. II (Purcell+, 2012)
The H2O Southern Galactic Plane Survey: NH3(1,1) and (2,2) catalogues.
Purcell C.R., Longmore S.N., Walsh A.J., Whiting M.T., Breen S.L.,
Britton T., Brooks K.J., Burton M.G., Cunningham M.R., Green J.A.,
Harvey-Smith L., Hindson L., Hoare M.G., Indermuehle B., Jones P.A., Lo N.,
Lowe V., Phillips C.J., Thompson M.A., Urquhart J.S., Voronkov M.A.,
White G.L.
<Mon. Not. R. Astron. Soc., 426, 1972-1991 (2012)>
=2012MNRAS.426.1972P 2012MNRAS.426.1972P
ADC_Keywords: Galactic plane; Masers; Radio lines
Keywords: surveys - stars: early-type - stars: formation - ISM: evolution -
Galaxy: structure - radio lines: ISM
Abstract:
The H2O Southern Galactic Plane Survey (HOPS) has mapped a 100°
strip of the Galactic plane (-70°>l>30°, |b|<0.5°) using
the 22m Mopra antenna at 12mm wavelengths. Observations were conducted
in on-the-fly mode using the Mopra spectrometer (MOPS), targeting
water masers, thermal molecular emission and radio-recombination
lines. Foremost among the thermal lines are the 23GHz transitions of
NH3 J,K=(1,1) and (2,2), which trace the densest parts of molecular
clouds (n>104cm-3). In this paper, we present the NH3(1,1) and
(2,2) data, which have a resolution of 2arcmin and cover a velocity
range of ±200km/s.
Description:
The HOPS observations and survey design are described in Walsh et al.
(2008PASA...25..105W 2008PASA...25..105W) and in Paper I (Walsh et al., 2011, Cat.
J/MNRAS/416/1764).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 146 687 Properties of the NH3(1,1) clouds identified in HOPS
table2.dat 146 324 Properties of the NH3(2,2) clouds identified in HOPS
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See also:
J/A+AS/98/589 : IRAS Sources behind the Solar circle (Wouterloot+ 1993)
J/A+A/366/481 : ATCA/VLA OH 1612 MHz survey. III. (Sevenster+, 2001)
J/A+A/418/103 : 86GHz SiO maser survey in the Inner Galaxy (Messineo+, 2004)
J/ApJ/656/255 : Arecibo methanol maser Galactic Plane Survey (Pandian+ 2007)
J/ApJ/669/435 : Arecibo Methanol Maser Galactic Plane Survey II
(Pandian+ 2007)
J/PASJ/59/559 : SiO maser search off the Galactic plane (Deguchi+, 2007)
J/PASJ/62/525 : SiO maser survey off the Galactic Plane (Deguchi+, 2010)
J/MNRAS/416/1764 : H2O Southern Galactic Plane Survey (HOPS) (Walsh+, 2011)
Byte-by-byte Description of file: table[12].dat
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Bytes Format Units Label Explanations
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1- 20 A20 --- Cloud Cloud Name (GLLL.lll+B+bbb+VVV.v) (1)
22- 28 F7.3 deg GLON Brightness weighted Galactic longitude (2)
30- 35 F6.3 deg GLAT Brightness weighted Galactic latitude (2)
37- 42 F6.1 km/s Vlsr Brightness weighted LSR velocity (2)
44- 50 F7.3 deg GLONp Bightest voxel in the cloud Galactic longitude
52- 57 F6.3 deg GLATp Bightest voxel in the cloud Galactic latitude
59- 64 F6.1 km/s Vlsrp Bightest voxel in the cloud LSR velocity
66- 71 F6.1 km/s Vmin Velocity range over which DUCHAMP detects
emission within that clump (4)
73- 78 F6.1 km/s Vmax Velocity range over which DUCHAMP detects
emission within that clump (4)
80- 84 F5.1 arcmin rc Angular radius of a circular source subtending
an equivalent solid angle on the sky
86- 89 F4.1 arcmin rw Brightness-weighted radius measured from the
integrated intensity map
91- 97 F7.2 arcmin+2 Omega Solid angle subtended by the cloud Ω
99-103 I5 --- N2 Number of spatial pixels in the cloud
105-111 I7 --- N3 Number of emitting voxels in the cloud
113-121 F9.2 K.km/s Int Total integrated intensity, ∫TmbdV
(transitions at 23.69448GHz for NH3(1,1)
and 23.7226336GHz for NH3(1,1))
123-128 F6.2 K.km/s e_Int rms uncertainty on Int
130-133 F4.2 K Tpeak Peak brightness temperature
135-138 F4.2 K Trms Local RMS noise temperature
140-142 A3 --- fl1 [XZY ] Flags noting if the cloud touches a
survey boundary in b (=X), l (=Y) or v (=Z)
144-146 A3 --- fl2 [EAM ] flags about multiplicity (3)
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Note (1): Cloud name constructed from the centroid position of the cloud
in Galactic longitude, latitude and velocity.
Note (2): measured from a masked and smoothed version of the original cube.
Note (3): Flags as follows:
M = if multiple velocity components were detected, i.e., if the velocity range
is greater than the expected velocity width of a single NH3 spectrum.
Here we assume a full-width half-maximum for each line-group of 3km/s,
which is typical of gas forming massive stars. The expected velocity
range of an NH3 (1,1) spectrum from an isolated cloud is then 44.6km/s.
E = clouds which exhibit significantly different peak and brightness-weighted
velocities (>5km/s) are likely to contain multiple sub-clouds overlapping
in position.
A = a small number of clouds detected in the NH3 (1,1) and (2,2) bandpass are
in fact broad line-wings of NH3 (2,2) encroaching on the (1,1) bandpass
and are flagged as artifacts.
Note (4): DUCHAMP is a software to automatiquely detect emission in 3-D
data, see http://www.atnf.csiro.au/people/Matthew.Whiting/Duchamp/
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History:
From electronic version of the journal
References:
Walsh et al., Paper I 2011MNRAS.416.1764W 2011MNRAS.416.1764W, Cat. J/MNRAS/416/1764
(End) Patricia Vannier [CDS] 15-Apr-2013