J/MNRAS/363/405 SIMBA observations of cold cores (Hill+, 2005)
Millimetre continuum observations of southern massive star formation regions.
I. SIMBA observations of cold cores.
Hill T., Burton M.G., Minier V., Thompson M.A., Walsh A.J.,
Hunt-Cunningham M., Garay G.
<Mon. Not. R. Astron. Soc., 363, 405-451 (2005)>
=2005MNRAS.363..405H 2005MNRAS.363..405H
ADC_Keywords: H II regions ; Masers ; Radio sources ; Millimetric/submm sources
Keywords: masers - stars: formation - stars: fundamental parameters -
H II regions - radio continuum: ISM
Abstract:
We report the results of a 1.2-mm continuum emission survey toward 131
star-forming complexes suspected of undergoing massive star formation.
These regions have previously been identified as harbouring a methanol
maser and/or a radio continuum source [ultracompact (UC) HII region],
the presence of which is in most instances indicative of massive star
formation. The 1.2-mm emission was mapped using the SIMBA instrument
on the 15-m Swedish ESO Submillimetre Telescope (SEST). Emission is
detected toward all of the methanol maser and UC HII regions
targeted, as well as towards 20 others lying within the fields mapped,
implying that these objects are associated with cold, deeply embedded
objects. Interestingly, there are also 20 methanol maser sites and
nine UC HII regions within the fields mapped which are devoid of
millimetre continuum emission.
In addition to the maser and UC HII regions detected, we have also
identified 253 other sources within the SIMBA maps. All of these (253)
are new sources, detected solely from their millimetre continuum
emission.
In total, 404 sources are detected, representing four classes of
sources which are distinguished by the presence of the different
combination of associated tracers.
Description:
The observations were undertaken on the Swedish ESO Submillimetre
Telescope (SEST), using the SEST IMaging Bolometer Array (SIMBA)
during three separate observing periods between 2001 October and 2002
October.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table5.dat 112 404 Parameters for the 404 1.2-mm continuum sources
found in the survey
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See also:
V/114 : MSX6C Infrared Point Source Catalog (Egan+ 2003)
J/A+A/417/615 : Maser and outflows in UC HII region (Codella+, 2004)
J/ApJS/155/123 : JHKs photometry of ultracompact HII regions (Alvarez+, 2004)
J/A+A/336/339 : VLA observations of ultracompact HII regions (Molinari+ 1998)
J/A+AS/133/29 : Molecular line survey towards UC HII (Hatchell+ 1998)
J/A+AS/115/81 : A CS(2-1) survey of UC HII regions (Bronfman+, 1996)
J/ApJS/91/659 : Ultracompact HII regions radio images (Kurtz+ 1994)
Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 2 I2 h RAh Right ascension (J2000)
4- 5 I2 min RAm Right ascension (J2000)
7- 10 F4.1 s RAs Right ascension (J2000)
12 A1 --- DE- Declination sign (J2000)
13- 14 I2 deg DEd Declination (J2000)
16- 17 I2 arcmin DEm Declination (J2000)
19- 20 I2 arcsec DEs Declination (J2000)
22- 36 A15 --- [HBM2005] Source name (1)
37- 38 A2 ---- n_[HBM2005] [*+ct ] Note on [HBM2005] (2)
40- 43 A4 --- Tracer Tracer type (3)
45- 59 A15 --- mmmap Millimetre map in which the source was
identified (for the 'mm-only' sources only)
61- 64 F4.1 Jy Fi1.2mm ?=- 1.2mm integrated flux
65 A1 --- n_Fi1.2mm [abdg] Note on Fi1.2mm (4)
67- 70 F4.1 Jy Fp1.2mm ?=- 1.2mm peak flux (in Jy/beam)
72- 74 I3 arcsec FWHM ?=- FWHM
75 A1 ---- n_FWHM [+] Note on FWHM (5)
76- 79 F4.1 kpc Dist ? Distance or near distance if
ambiguity exists
80 A1 --- --- [/]
81- 84 F4.1 kpc Dist2 ? Far distance if ambiguity exists
85- 87 A3 --- f_Dist [Ind ] Ind for sources for which a distance
is indeterminate
88 A1 --- r_Dist Reference for distance (6)
90- 96 E7.2 solMass Mass ? Mass or lower mass if ambiguity exists
97 A1 --- --- [/]
98-104 E7.2 solMass Mass2 ? Upper Mass if ambiguity exists
106-108 A3 --- MSC [DC? N] Lack of an 8um MSX correlation
code (7)
110-112 A3 --- f_Mass [Ind ] "Ind" for sources for which
a distance is indeterminate
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Note (1): Source names given to two (or fewer) decimal places in galactic
longitude and latitude are consistent with those reported by Walsh
et al. (1997, Cat. J/MNRAS/291/261, 1998, Cat. J/MNRAS/301/640,
2003, Cat. J/A+A/410/597 and 2004, Cat. J/A+A/417/115); Thompson
et al. (in preparation) and Minier et al. (2001A&A...369..278M 2001A&A...369..278M,
2005A&A...429..945M 2005A&A...429..945M) from which they were targeted. Source names given
to three decimal places denote those source identified in this survey,
with the extended Galactic names intended to distinguish closely
associated sources.
Note (2): Sources which have been targeted in the millimetre and submillimetre
studies from:
c = Beuther et al. (2002ApJ...566..945B 2002ApJ...566..945B)
+ = Williams et al. (2004, Cat. J/A+A/417/115)
* = Faundez et al. (2004, cat. J/A+A/426/97)
t = faint millimetre sources, which produce masses uncharacteristic
of massive star formation regions if located at the near distance.
Note (3): Tracer types as follows:
m = maser source
mm = mm-only source
mr = maser radio continuum source
r = radio continuum source
IRAS = NM-IRAS source
Note (4): Notes as follows:
a = sources that have more than one millimetre peak encompassed, for
which it was not possible to clearly distinguish the individual
cores. The flux quoted here is for all the sources.
b = sources located too close to the edge of the map, for their
fluxes to be calculated. In the majority of cases it is not
possible to determine the peak of the millimetre emission either.
g = sources situated quite close to the edge of the map, with some
uncertainty in source size. The fluxes quoted here are a lower limit.
d = the two NM-IRAS positions where no millimetre emission is
detected at the reported IRAS coordinates.
Note (5): Sources denoted with a "+" indicate those for which a radius could
not be determined using the gaia program.
Note (6): Only those sources that were targeted have the distance reference
indicated. The 'mm-only' sources have distances adopted from the
nearby tracer and accordingly their distance reference is the same
as the nearby tracer.
e = Kurtz et al. (1994, Cat. J/ApJS/91/659)
k = Pestalozzi et al. (2005, Cat. J/A+A/432/737)
i = Walsh et al. (1997, Cat. J/MNRAS/291/261)
m = Norris et al. (1993ApJ...412..222N 1993ApJ...412..222N)
n = Wood & Churchwell (1989ApJS...69..831W 1989ApJS...69..831W)
r = Palagi et al. (1993, Cat. J/A+AS/101/153) as quoted in
Thompson et al. (in preparation);
s = Minier et al. (2005A&A...429..945M 2005A&A...429..945M)
v = Thompson et al. (in preparation);
x = Walsh et al. (2003, Cat. J/A+A/410/597)
Note (7): Indicates the lack of mid-IR MSX association ('N') or an association
with a mid-IR dark cloud ('DC'). A 'DC?' in this column indicates
that there is no mid-IR emission; however, it is not clear whether
the lack of emission is due to absorption (i.e. a dark cloud) or
simply an absence of emission. Note that an absence in this column
does not indicate that an MSX source is present.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 24-Apr-2006