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J/A+A/526/A151      Hi-Gal sources distance determination      (Russeil+, 2011)

Giving physical significance to the Hi-GAL data: determining the distance of cold dusty cores in the Milky Way. Russeil D., Pestalozzi M., Mottram J.C., Bontemps S., Anderson L.D., Zavagno A., Beltran M.T., Bally J., Brand J., Brunt C., Cesaroni R., Joncas G., Marshall D., Martin P., Massi F., Molinari S., Moore T., Noriega-Crespo A., Olmi L., Thompson M.A., Wienen M., Wyrowski F. <Astron. Astrophys., 526, A151 (2011)> =2011A&A...526A.151R
ADC_Keywords: Galactic plane ; H II regions ; Stars, distances ; Spectroscopy Keywords: Galaxy: structure - Galaxy: general - infrared: general - infrared: ISM - HII regions - ISM: clouds Abstract: Hi-GAL, an open time key-project of the Herschel satellite, was awarded 343 hours observing time to carry out a 5-band photometric imaging survey at 70, 160, 250, 350, and 500um of a |b|≤1° wide strip of the Milky Way Galactic plane in the longitude range -70°≤l≤70°. Two 2°x2° fields centred at l=30° and l=59° have been observed with the SPIRE and PACS photometric cameras in parallel mode during the Herschel science demonstration phase (SDP). From the images, compact sources are extracted for which the distance must be established in order to determine their physical properties. The aim of this paper is to present the distance determination strategy for the Hi-GAL compact sources. We illustrate this strategy for the two fields at l=30° and l=59°. Description: We obtain velocities along the line of sight to Hi-GAL sources, where possible, using CO data observed with the SEQUOIA receiver on the FCRAO 14m telescope. In the l=30 ° region we use the 13CO J=1-0 data from the BU-FCRAO Galactic Ring Survey (GRS, Jackson et al., 2006ApJS..163..145J) while in the l=59° region we use 13CO and C18O J=1-0 observations obtained as part of the Exeter-FCRAO CO Galactic Plane Survey (Brunt et al., in prep.). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tableb1.dat 170 208 Star-forming complexes in the l=30° field tableb2.dat 170 20 Star-forming complexes in the l=59° field
See also: J/ApJ/582/756 : Velocities of HII regions (Kolpak+, 2003) J/ApJS/154/553 : Inner galaxy massive star formation regions (Sewilo+, 2004) J/ApJ/653/1325 : Galactic distribution of infrared dark clouds (Simon+, 2006) J/A+A/486/191 : Distances towards 6.7GHz methanol masers (Pandian+, 2008) J/ApJ/680/349 : Galactic distribution of IRDCs (Jackson+, 2008) J/ApJS/181/255 : CO in Galactic HII regions (Anderson+, 2009) J/ApJ/690/706 : Distances of Galactic HII regions (Anderson+, 2009) Byte-by-byte Description of file: tableb[12].dat
Bytes Format Units Label Explanations
1- 2 I2 --- Cplx Complex number 4- 6 F3.1 kpc Dist1 ?=- Near distance 7 A1 --- --- [/] 8- 11 F4.1 kpc Dist2 ?=- Far distance 12 A1 --- --- [/] 13- 15 F3.1 kpc Dist3 ?=- Tangent distance 17- 21 A5 --- n_Dist Adopted distance (Near, Far or Tang.) (1) 22- 25 F4.2 kpc Dist ? Stellar (or maser parallax) distance 26- 31 A6 --- HII Optical name of associated HII region 33- 56 A24 --- Source Source name or galactic position name (2) 57- 60 F4.1 km/s VHa ? Hα (LSR) velocity 61 A1 --- --- Separation code (3) 62- 65 F4.1 km/s VHa2 ? Hα (LSR) velocity 66 A1 --- --- [(] 67- 70 F4.1 km/s VHa3 ? Hα (LSR) velocity 71 A1 --- --- [)] 73- 77 F5.1 km/s Vrad ? Radio recombination-line (LSR) velocity 78 A1 --- --- Separation code (3) 79- 83 F5.1 km/s Vrad2 ? Radio recombination-line (LSR) velocity 84 A1 --- --- Separation code (3) 85- 89 F5.1 km/s Vrad3 ? Radio recombination-line (LSR) velocity 90 A1 --- --- Separation code (3) 91- 94 F4.1 km/s Vrad4 ? Radio recombination-line (LSR) velocity 95 A1 --- --- Separation code (3) 96- 99 F4.1 km/s Vrad5 ? Radio recombination-line (LSR) velocity 101-105 F5.1 km/s Vmol ? Molecular line velocity (CO and/or CS) 106 A1 --- --- Separation code (3) 107-111 F5.1 km/s Vmol2 ? Molecular line velocity (CO and/or CS) 112 A1 --- --- Separation code (3) 113-117 F5.1 km/s Vmol3 ? Molecular line velocity (CO and/or CS) 118 A1 --- --- Separation code (3) 119-123 F5.1 km/s Vmol4 ? Molecular line velocity (CO and/or CS) 125-127 I3 km/s Vabs ? H2CO or OH absorption line (LSR) velocity 128 A1 --- --- Separation code (3) 129-131 I3 km/s Vabs2 ? H2CO or OH absorption line (LSR) velocity 132 A1 --- --- Separation code (3) 133-135 I3 km/s Vabs3 ? H2CO or OH absorption line (LSR) velocity 136 A1 --- --- Separation code (3) 137-139 I3 km/s Vabs4 ? H2CO or OH absorption line (LSR) velocity 140 A1 --- --- Separation code (3) 141-143 I3 km/s Vabs5 ? H2CO or OH absorption line (LSR) velocity 144 A1 --- --- Separation code (3) 145-147 I3 km/s Vabs6 ? H2CO or OH absorption line (LSR) velocity 148 A1 --- --- Separation code (3) 149-151 I3 km/s Vabs7 ? H2CO or OH absorption line (LSR) velocity 152 A1 --- --- Separation code (3) 153-154 I2 km/s Vabs8 ? H2CO or OH absorption line (LSR) velocity 155 A1 --- --- Separation code (3) 156-157 I2 km/s Vabs9 ? H2CO or OH absorption line (LSR) velocity 159-162 A4 --- NF Near/far/tangent solution (4) 163-165 A3 --- r_NF NF references (5) 166 A1 --- --- [,;] 167 A1 --- NF2 Near/far/tangent solution (4) 168-170 A3 --- r_NF2 NF2 references (5)
Note (1): if not indicated, the stellar distance (Dist) is adopted Note (2): "Wat", "SW", "A" correspond to radio sources listed mainly in Watson et al. (2003ApJ...587..714W), Sewilo (2004, Cat. J/ApJS/154/553) and Anderson et al. (2009, Cat. J/ApJS/181/255), respectively. The molecular information is from Dame et al. (1986ApJ...305..892D) for "GMC", from Roman-Duval et al. (2009ApJ...699.1153R) for "GRSMC" clouds, from Solomon et al. (1987ApJ...319..730S) for "Sol" clouds, from Jacq et al. (1988A&A...195...93J) for "Bx" clouds and from Simon et al. (2006, Cat. J/ApJ/653/1325) and Jackson et al. (2008, Cat. J/ApJ/680/349) for "IRDC". For "GMC" and "Bx" clouds the radius and velocity FWHM of the cloud is given in brackets. Note that the typical radius and velocity FWHM of "GRSMC" clouds are 0.35±0.12 degrees and 3.57±1.21km/s. These values are lower than the typical values for GMC. Note (3): When different values are found in the literature, they are given separated by a semicolon. If several velocities (along the line of sight) are measured they are separated by a backslash. Note (4): Near/far/tangent solution mainly from HI emission/absorption or HI self-absorption methods and references. N means near, F means far, T means tangent. When two solutions are proposed in brackets the first comes from the HI emission/absorption method, the second from the HI self-absorption method (Anderson & Bania, 2009, Cat. J/ApJ/690/706). For sources where the two methods disagree, the favoured one by Anderson & Bania (2009, Cat. J/ApJ/690/706) is marked with an asterisk. Note (5): References as follows: a = Watson et al. (2003ApJ...587..714W) b = Solomon et al. (1987ApJ...319..730S) c = Sewilo et al. (2004, Cat. J/ApJS/154/553) d = Pandian et al. (2008, Cat. J/A+A/486/191) e = Kolpack et al. (2003, cat. J/ApJ/582/756) f = Anderson et al. (2009, Cat. J/ApJS/181/255) g = Anderson & Bania (2009, Cat. J/ApJ/690/706) h = Roman-Duval et al. (2009ApJ...699.1153R) i = Kuchar & Bania (1994ApJ...436..117K)
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 31-May-2011
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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