J/ApJS/161/361 Millimeter continuum survey for protoclusters (Klein+, 2005)
A millimeter continuum survey for massive protoclusters in the outer Galaxy.
Klein R., Posselt B., Schreyer K., Forbrich J., Henning T.
<Astrophys. J. Suppl. Ser., 161, 361-393 (2005)>
=2005ApJS..161..361K 2005ApJS..161..361K
ADC_Keywords: Millimetric/submm sources ; Infrared sources
Keywords: stars: formation - submillimeter - surveys
Abstract:
Our search for the earliest stages of massive star formation turned up
12 massive pre-protocluster candidates plus a few protoclusters. For
this search, we selected 47 FIR-bright IRAS sources in the outer
Galaxy. We mapped regions of several square arcminutes around the IRAS
source in the millimeter continuum in order to find massive cold cloud
cores possibly being in a very early stage of massive star formation.
Masses and densities are derived for the 128 molecular cloud cores
found in the obtained maps.
Description:
The millimeter continuum maps were collected at three observatories:
the Heinrich Hertz Submillimeter Telescope (SMT, Mount Graham,
Arizona), the Institut de Radioastronomie Millimetrique (IRAM) 30m
telescope (Pico Veleta, Spain), and the James Clerk Maxwell Telescope
(JCMT, Mauna Kea, Hawaii).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 70 47 Source list
table4.dat 52 7 The observing runs
table56.dat 92 137 Source components
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See also:
J/A+AS/115/81 : A CS(2-1) survey of UC HII regions (Bronfman+, 1996)
J/A+AS/143/269 : 6.7GHz methanol maser emission survey (Szymczak+, 2000)
J/A+A/368/845 : Arcetri Catalog of H2O maser sources. Update.
(Valdettaro+, 2001)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS name
12- 15 F4.2 kpc Dist Distance
16 A1 --- f_Dist [a] Indicates a photometric distance
17- 25 A9 [solLum] Lum Luminosity (1)
27- 30 F4.1 K Tdust Dust temperature (1)
32- 68 A37 --- ONames Other designations
70 I1 --- Ref Reference (2)
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Note (1): From Schreyer et al. (1996A&A...306..267S 1996A&A...306..267S)
Note (2): Reference number, defined as follows:
1 = Henning et al. (1992A&AS...93..525H 1992A&AS...93..525H)
2 = Bronfman et al. (1996, Cat. J/A+AS/115/81)
3 = Schreyer (1997, Ph.D. thesis, Univ. Jena)
4 = Mueller et al. (2002ApJS..143..469M 2002ApJS..143..469M)
5 = Szymczak et al. (2000, Cat. J/A+AS/143/269)
6 = Valdettaro et al. (2001, Cat. J/A+A/368/845)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1 I1 --- Run Observing run number
3- 6 A4 --- Tel Telescope
8- 21 A14 --- Inst Instrument
23- 25 I3 GHz Freq Frequency
27- 28 I2 GHz DFreq Frequency width
30- 41 A12 --- ObsDate Date of observation
43- 46 F4.1 arcsec FWHM Full width at half maximum
48- 52 F5.1 mJy rms Noise rms (in units of mJy/beam)
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Byte-by-byte Description of file: table56.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- IRAS IRAS name
11- 12 A2 --- m_IRAS [/1-9] Merged IRAS name
14 I1 --- Run Observing run number
16- 18 I3 GHz Freq Frequency
20- 21 A2 --- Comp Source component
23- 27 F5.2 Jy Fint ? Mean integrated flux density at Freq
29- 33 F5.2 Jy e_Fint ? Error in Fint
35- 39 I5 arcsec2 Aint ? Mean integration area
41- 45 F5.2 Jy Fpeak ? Peak flux density at Freq (in units of
Jy/θbeam)
47- 49 I3 mJy sigma σ level of the map (in units of
mJy/θbeam)
51- 54 F4.2 pc theta ? Component extension θsource derived
from Aint (beam-deconvolved angular diameter
of the source)
55 A1 --- f_theta [a] Flag on theta (1)
57- 60 I4 solMass Mgas ? Gas mass
62- 65 F4.1 10+22cm-2 NH ? Column density N(H)
67- 71 F5.1 10+4cm-3 nH ? Number density n(H)
73- 74 I2 h RAh ? Hour of Right Ascension (B1950) (2)
76- 77 I2 min RAm ? Minute of Right Ascension (B1950) (2)
79- 82 F4.1 s RAs ? Second of Right Ascension (B1950) (2)
84 A1 --- DE- Sign of the Declination (B1950) (2)
85- 86 I2 deg DEd ? Degree of Declination (B1950) (2)
88- 89 I2 arcmin DEm ? Arcminute of Declination (B1950) (2)
91- 92 I2 arcsec DEs ? Arcsecond of Declination (B1950) (2)
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Note (1): A "a" indicates that the beam area is larger than the source extent,
and it is used for further calculations.
Note (2): Peak position
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History:
From electronic version of the journal
(End) Marianne Brouty [CDS] 20-Sep-2006