J/A+A/542/A101 LABOCA 870um mapping of 4 Galactic plane fields (Miettinen, 2012) ================================================================================ LABOCA 870 {mu}m dust continuum mapping of selected infrared-dark cloud regions in the Galactic plane. Miettinen O. =2012A&A...542A.101M ================================================================================ ADC_Keywords: Galactic plane ; Millimetric/submm sources ; Morphology Keywords: stars: formation - ISM: clouds - submillimeter: ISM Abstract: Imaging surveys of dust emission at (sub)millimetre wavelengths provide a powerful tool for studying molecular clouds and the early stages of star formation. Through submm dust continuum mapping, we attempt to search for genuine infrared-dark clouds (IRDCs) and precursors to massive stars and stellar clusters in the Galactic plane, and to determine their basic physical properties. We have mapped four selected fields of about 0.5degx0.5deg that contain Spitzer 8-um dark regions with LABOCA at 870um. Selected positions in the fields were observed in C^17^O(2-1) to obtain kinematic information. The obtained LABOCA maps are used in conjunction with the Spitzer IR images. Description: Our LABOCA observations took place on 19 May 2011, during the UTC time ranges of 03:17-06:20 and 07:54-10:50. Fields are G1.87-0.14, G2.11+0.00, G11.36+0.80 and G13.22-0.06. File Summary: -------------------------------------------------------------------------------- FileName Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file table3.dat 380 91 Characteristics of the clumps identified from the LABOCA maps notes.dat 79 31 Notes -------------------------------------------------------------------------------- See also: J/ApJ/680/349 : Galactic distribution of IRDCs (Jackson+, 2008) J/ApJ/639/227 : MSX IRDC candidate catalog (Simon+, 2006) Byte-by-byte Description of file: table3.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 11 A11 --- Field Field 13- 23 A11 --- Source Clump (SMM NN(A,B)) designation, within the field 25 A1 --- n_Source [bh] Note on Source (1) 27- 28 I2 h RAh Right ascension (J2000) 30- 31 I2 min RAm Right ascension (J2000) 33- 36 F4.1 s RAs Right ascension (J2000) 38 A1 --- DE- Declination sign (J2000) 39- 40 I2 deg DEd Declination (J2000) 42- 43 I2 arcmin DEm Declination (J2000) 45- 46 I2 arcsec DEs Declination (J2000) 48- 51 F4.2 Jy I870 Peak surface brightnesses at 870um (in Jy/beam) 53- 56 F4.2 Jy e_I870 rms uncertainty on I870 58- 62 F5.2 Jy S870 Integrated flux density at 870um 64- 67 F4.2 Jy e_S870 rms uncertainty on S870 69- 72 F4.1 arcsec Reff Clump effective radius (in arcsec) 74- 77 F4.2 pc Reffl Clump effective radius (in pc) 79- 82 F4.2 pc e_Reffl rms uncertainty on Reff 84- 88 I5 Msun Mass Mass 90- 93 I4 Msun e_Mass rms uncertainty on Mass 95- 98 F4.1 10+22mm-2 N(H2) H_2_ column density 100-102 F3.1 10+22mm-2 e_N(H2) rms uncertainty on N(H2) 104-106 F3.1 10+4mm-3 n(H2) H_2_ density number 108-110 F3.1 10+4mm-3 e_n(H2) rms uncertainty on n(H2) 112-114 A3 --- M8 Morphological code at 8um (2) 115 A1 --- n_M8 [cdefg] Note on M8 (3) 116 A1 --- --- [/] 117 A1 --- M24 Morphological code at 24um (2) 119-380 A262 --- Assos Association (4) -------------------------------------------------------------------------------- Note (1): Note on sources as follows: b = The clump is associated with the marked C^17^O(2-1)-observation target position. h = The clump can be resolved by eye into two "subclumps", but they are dealt with as a one source by clumpfind. Note (2): Morphological codes as follows: e = extended d = dark p = point source g = group i = diffuse w = weak pfg = point source, likely a foreground star Note (3): Notes on 8um as follows: c = The 8um point source is associated with SSTGLMC G001.8134-00.1136, which has the [3.6]-[4.5], [4.5]-[5.8], and [4.5]-[8.0] colours of 0.098, 0.245, and 0.031, respectively, and is likely to be a foreground star. d = The 8um point source corresponds to SSTGLMC G001.9301-00.1234 with the colours [3.6]-[4.5]=0.081, [4.5]-[5.8]=0.158, and [4.5]-[8.0]=0.167, and is likely a foreground star. e = The 8um point source corresponds to SSTGLMC G001.9716-00.1375 with the colours [3.6]-[4.5]=-0.033, [4.5]-[5.8]=0.294, and [4.5]-[8.0]=0.141, and is likely a foreground star. f = The 8um point source is associated with SSTGLMC G002.0927-00.0039, which has the [3.6]-[4.5], [4.5]-[5.8], and [4.5]-[8.0] colours of 0.802, 0.775, and 0.290, respectively, and is likely to be a foreground star. g = The 8um point source corresponds to SSTGLMC G002.2440+00.0447. Its [3.6]-[4.5], [4.5]-[5.8], and [4.5]-[8.0] colours are, respectively, 0.523, 0.436, and 0.838, and it is likely a foreground star. Note (4): Remarks on the associated sources. Offset from the 870-um peak position is indicated in parenthesis (#"). Reference, indicated in parenthesis (#) are detailled in notes.dat file. -------------------------------------------------------------------------------- Byte-by-byte Description of file: notes.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 1- 2 I2 --- Note Note number 4- 79 A76 --- Text Text of the note -------------------------------------------------------------------------------- History: From electronic version of the journal ================================================================================ (End) Patricia Vannier [CDS] 16-Sep-2012