VizieR Online Data Catalog: LEGO II. 3mm molecular line study (Barnes+, 2020)
Abstract
table2.dat contains information on the selected observed molecular lines, ordered by increasing rest frequency. Section 2.1.2 of the paper describes how the lines recorded in this table were selected, and how the line characteristics recorded here were obtained. Columns 1 to 10 show the name of each molecule, the transition information, the frequency of the transition (Lovas, 2004JPCRD..33..177L), the upper energy level of the transition, the Einstein spontaneous decay coefficient, the collisional deexcitation rate coefficients at a kinetic temperature of 20K, and the critical and effective densities for emission. Transitions that are not available within the LAMDA database have the corresponding information blanked. Additional information on the molecular line database used within this work can be found in Table A1 of the paper.
table3b1.dat contains observational properties across the mapped region (i.e. that covered with both vertical and horizontal on-the-fly scans). The columns show the molecule name, the average cube rms (in a 1kms-1 channel), mean uncertainty of the integrated intensity, the minimum values of all pixels within the map, and the minimum, mean, and 5, 16, 50, 84, and 95 percentile ranges for the intensities at positions above a 3-sigma uncertainty threshold. Also given is the area percentage, within the mapped region that has an integrated intensity above five times the uncertainty. The information given is for maps that have been smoothed to an angular resolution of 60arcsec, and have a spectral resolution of 0.6km/s. table4.dat contains properties determined from the cumulative distributions of the emission from each molecular line. Tabulated is the molecule, and its characteristic column density, which is defined as the column density that contains half the total line intensity. The uncertainties show the range of characteristic densities after adding a synthetic noise of 1 sigma (see shaded region on Figure 9 in the paper). We provide the results of the analysis across the whole mapped region (i.e. using the cumulative distributions shown in Section 4.1), and when limited to W49A (i.e. using the cumulative distributions shown in Section 5.2). Also shown for W49A is the characteristic density (see Section 5.2). tableA1.dat contains details on the emission lines covered by the LEGO survey, and processed by our pipeline. Section 2.1.2 explains how lines examined in this study were selected. Each of the selected lines was given a LEGO reference code in the reduction pipeline, which are presented in the first column of the Table. The rest frequency recorded in this table refers to the specific full transition (Lovas, 2004JPCRD..33..177L). These transitions are sometimes part of larger groups, as explained in Sec. 2.1.2 (see the final column of this Table). In those cases, the minimum and maximum frequencies of the lines considered to form a group. tablee1a.dat contains calculated conversion factors for the various molecular line transitions. The values shown in this half of the Table have been calculated using the column density and mass of Av>8mag gas divided by the mean integrated intensity and total luminosity of the given line across the region. tablee1b.dat contains calculated conversion factors for the various molecular line transitions. The values shown in this half of the Table have been calculated using both the column density and mass, and integrated intensity and luminosity above the Av>8mag threshold. tablee2.dat contains calculated conversion factors for the various molecular line transitions. The values in this table have been calculated without imposing any extinction threshold on the gas column density and gas mass, and the integrated intensity and luminosity of the given line. (7 data files).- Publication:
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VizieR Online Data Catalog
- Pub Date:
- September 2020
- Bibcode:
- 2020yCat..74971972B
- Keywords:
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- Star Forming Region;
- Molecular data;
- Interstellar medium