*************************************************************************** Credit: ------- When making use of the data inside this archive, please cite: Pety et al., 2017, A&A doi:10.1051/0004-6361/201629862 *************************************************************************** Archive URL: ------------ The original version of this archive is available at https://www.iram.fr/~pety/ORION-B/data/orionb-2017-pety.tar.xz *************************************************************************** Contents: --------- This archive contains the data used in Pety et al. (2017). I) These data are mostly derived from observations with the IRAM-30m telescope in the context of the ORION-B project, cf., https://www.iram.fr/~pety/ORION-B/ 1) Two different flavors of the line integrated intensity map are used for each of the 18 studied lines: A) On one hand, we use the line intensity integrated over the full line profiles when we aim to study the gas properties along the full line of sight. This happens, for instance, when we compute the CO-traced mass, and the correlations between the column density of material along the full line of sight and the line integrated intensity. The used velocity range is here [-5.25; +20.25 km/s]. The corresponding data files contains the "-area-" string in their FITS file names. B) On the other hand, lines are detected over different velocity ranges. Using the same velocity range for all lines, [-2; +18 km/s] for example, results in noisy integrated intensities for tracers that have the narrowest lines. In contrast, adapting the velocity range to each line could bias the results. We thus adopted a compromise for sections where we can restrict our investigations to the bulk of the gas: we computed the line integrated intensity over the velocity range where the core of the line can be found for each species and transition over the measured FoV. This velocity range is exactly [+8.75; +12.25 km/s], i.e., 0.25 km/s more than quoted in Pety et al. (2017) because of the width of each channel. The corresponding data files contains the "-900-1200-" string in their FITS file names. In both case, the associated map of the rms noise level is distributed in FITS file postfixed with the "-noise" string. The next table lists the FITS file names and a few characteristics of the data, i.e., the line name and rest frequency, the data unit, and the angular resolution of the data. ! File name => Line name Freq. [MHz] Array unit Beam [arcsec] 12co10-area.fits => 12CO10 115271.20200 K (Tmb).km/s 31.0 12co10-area-noise.fits => 12CO10 115271.20200 K (Tmb).km/s 31.0 12co10-900-1200.fits => 12CO10 115271.20200 K (Tmb).km/s 31.0 12co10-900-1200-noise.fits => 12CO10 115271.20200 K (Tmb).km/s 31.0 13co10-area.fits => 13CO10 110201.35430 K (Tmb).km/s 31.0 13co10-area-noise.fits => 13CO10 110201.35430 K (Tmb).km/s 31.0 13co10-900-1200.fits => 13CO10 110201.35430 K (Tmb).km/s 31.0 13co10-900-1200-noise.fits => 13CO10 110201.35430 K (Tmb).km/s 31.0 c18o10-area.fits => C18O10 109782.17300 K (Tmb).km/s 31.0 c18o10-area-noise.fits => C18O10 109782.17300 K (Tmb).km/s 31.0 c18o10-900-1200.fits => C18O10 109782.17300 K (Tmb).km/s 31.0 c18o10-900-1200-noise.fits => C18O10 109782.17300 K (Tmb).km/s 31.0 c17o10-area.fits => C17O10 112358.98200 K (Tmb).km/s 31.0 c17o10-area-noise.fits => C17O10 112358.98200 K (Tmb).km/s 31.0 c17o10-900-1200.fits => C17O10 112358.98200 K (Tmb).km/s 31.0 c17o10-900-1200-noise.fits => C17O10 112358.98200 K (Tmb).km/s 31.0 n2hp10-area.fits => N2H+10 93173.76400 K (Tmb).km/s 31.0 n2hp10-area-noise.fits => N2H+10 93173.76400 K (Tmb).km/s 31.0 n2hp10-900-1200.fits => N2H+10 93173.76400 K (Tmb).km/s 31.0 n2hp10-900-1200-noise.fits => N2H+10 93173.76400 K (Tmb).km/s 31.0 ch3oh-area.fits => CH3OH 96741.37500 K (Tmb).km/s 31.0 ch3oh-area-noise.fits => CH3OH 96741.37500 K (Tmb).km/s 31.0 ch3oh-900-1200.fits => CH3OH 96741.37500 K (Tmb).km/s 31.0 ch3oh-900-1200-noise.fits => CH3OH 96741.37500 K (Tmb).km/s 31.0 hcop10-area.fits => HCO+10 89188.52500 K (Tmb).km/s 31.0 hcop10-area-noise.fits => HCO+10 89188.52500 K (Tmb).km/s 31.0 hcop10-900-1200.fits => HCO+10 89188.52500 K (Tmb).km/s 31.0 hcop10-900-1200-noise.fits => HCO+10 89188.52500 K (Tmb).km/s 31.0 hcn10-area.fits => HCN10 88631.84750 K (Tmb).km/s 31.0 hcn10-area-noise.fits => HCN10 88631.84750 K (Tmb).km/s 31.0 hcn10-900-1200.fits => HCN10 88631.84750 K (Tmb).km/s 31.0 hcn10-900-1200-noise.fits => HCN10 88631.84750 K (Tmb).km/s 31.0 hnc10-area.fits => HNC10 90663.56800 K (Tmb).km/s 31.0 hnc10-area-noise.fits => HNC10 90663.56800 K (Tmb).km/s 31.0 hnc10-900-1200.fits => HNC10 90663.56800 K (Tmb).km/s 31.0 hnc10-900-1200-noise.fits => HNC10 90663.56800 K (Tmb).km/s 31.0 h13cop10-area.fits => H13CO+10 86754.28840 K (Tmb).km/s 31.0 h13cop10-area-noise.fits => H13CO+10 86754.28840 K (Tmb).km/s 31.0 h13cop10-900-1200.fits => H13CO+10 86754.28840 K (Tmb).km/s 31.0 h13cop10-900-1200-noise.fits => H13CO+10 86754.28840 K (Tmb).km/s 31.0 h13cn10-area.fits => H13CN10 86340.18400 K (Tmb).km/s 31.0 h13cn10-area-noise.fits => H13CN10 86340.18400 K (Tmb).km/s 31.0 h13cn10-900-1200.fits => H13CN10 86340.18400 K (Tmb).km/s 31.0 h13cn10-900-1200-noise.fits => H13CN10 86340.18400 K (Tmb).km/s 31.0 hn13c10-area.fits => HN13C10 87090.82520 K (Tmb).km/s 31.0 hn13c10-area-noise.fits => HN13C10 87090.82520 K (Tmb).km/s 31.0 hn13c10-900-1200.fits => HN13C10 87090.82520 K (Tmb).km/s 31.0 hn13c10-900-1200-noise.fits => HN13C10 87090.82520 K (Tmb).km/s 31.0 12cn10-area.fits => 12CN10 113490.97020 K (Tmb).km/s 31.0 12cn10-area-noise.fits => 12CN10 113490.97020 K (Tmb).km/s 31.0 12cn10-900-1200.fits => 12CN10 113490.97020 K (Tmb).km/s 31.0 12cn10-900-1200-noise.fits => 12CN10 113490.97020 K (Tmb).km/s 31.0 12cs21-area.fits => 12CS21 97980.95330 K (Tmb).km/s 31.0 12cs21-area-noise.fits => 12CS21 97980.95330 K (Tmb).km/s 31.0 12cs21-900-1200.fits => 12CS21 97980.95330 K (Tmb).km/s 31.0 12cs21-900-1200-noise.fits => 12CS21 97980.95330 K (Tmb).km/s 31.0 32so-area.fits => 32SO 99299.87000 K (Tmb).km/s 31.0 32so-area-noise.fits => 32SO 99299.87000 K (Tmb).km/s 31.0 32so-900-1200.fits => 32SO 99299.87000 K (Tmb).km/s 31.0 32so-900-1200-noise.fits => 32SO 99299.87000 K (Tmb).km/s 31.0 cch-area.fits => CCH 87316.89800 K (Tmb).km/s 31.0 cch-area-noise.fits => CCH 87316.89800 K (Tmb).km/s 31.0 cch-900-1200.fits => CCH 87316.89800 K (Tmb).km/s 31.0 cch-900-1200-noise.fits => CCH 87316.89800 K (Tmb).km/s 31.0 c3h2-area.fits => C3H2 85338.89300 K (Tmb).km/s 31.0 c3h2-area-noise.fits => C3H2 85338.89300 K (Tmb).km/s 31.0 c3h2-900-1200.fits => C3H2 85338.89300 K (Tmb).km/s 31.0 c3h2-900-1200-noise.fits => C3H2 85338.89300 K (Tmb).km/s 31.0 sio21-area.fits => SIO21 86846.96000 K (Tmb).km/s 31.0 sio21-area-noise.fits => SIO21 86846.96000 K (Tmb).km/s 31.0 sio21-900-1200.fits => SIO21 86846.96000 K (Tmb).km/s 31.0 sio21-900-1200-noise.fits => SIO21 86846.96000 K (Tmb).km/s 31.0 All details, included the exact species names and line quantum numbers are available in Pety et al. (2017). Note that the quantum numbers quoted in the Table ??? of this paper for the 32SO line refers to a SO line at another frequency than the studied one. The right quantum numbers associated with 99299.87000 MHz are ????. 2) The spectra stacked over different subsets of the observed field of view are also available in ASCII files formatted as follows: - Column 1: Channel number. - Column 2: Rest frequency at channel center. - Column 3: LSR velocity at channel center. - Column 3: Flux in Jansky or main beam temperature in Kelvin depending on the flavor. Two flavors of each spectra is delivered: A) First the spectra are SUMMED over all pixels belonging to a given mask. This gives the line flux associated with the mask. The associated file names contain the "-flux-" string. B) Second the spectra are AVERAGED over all pixels belonging to a given mask. This flavors delivers the mean spectrum associated with the mask. Assuming that there is no radiative transfer issue, it thus allow one to estimate the typical line integrated profiles when varying the percentage of the field of view that sample different physical regimes (e.g., diffuse, translucent, filamentary, and dense core gas). This could be used to quantify the amount of each kind of gas in unresolved extra-galactic observations. The spectra are stacked over either the visual extinction mask (file names containing the "-av-" string) or the dust temperature mask (file names containing the "-tdust-" string). The range of visual extinction or dust temperatures used to define the mask are quoted as the last two values in the file name. For example, the next table lists all the file names and their associated properties for the 12CO10 line. 12co10-stacked-spectrum-flux.dat => 12CO10 flux over the full field of view 12co10-stacked-spectrum-flux-av-1-2.dat => 12CO10 flux inside regions where 1 < Av <= 2 magn 12co10-stacked-spectrum-flux-av-2-6.dat => 12CO10 flux inside regions where 2 < Av <= 6 magn 12co10-stacked-spectrum-flux-av-6-15.dat => 12CO10 flux inside regions where 6 < Av <= 15 magn 12co10-stacked-spectrum-flux-av-15-225.dat => 12CO10 flux inside regions where 15 < Av <= 225 magn 12co10-stacked-spectrum-flux-tdust-16-19.5.dat => 12CO10 flux inside regions where 16.0 < Td <= 19.5 K 12co10-stacked-spectrum-flux-tdust-19.5-23.5.dat => 12CO10 flux inside regions where 19.5 < Td <= 23.5 K 12co10-stacked-spectrum-flux-tdust-23.5-32.dat => 12CO10 flux inside regions where 23.5 < Td <= 32.0 K 12co10-stacked-spectrum-flux-tdust-32-100.dat => 12CO10 flux inside regions where 32.0 < Td <= 100.0 K 12co10-stacked-spectrum-mean-av-1-2.dat => 12CO10 typical spectra over the full field of view 12co10-stacked-spectrum-mean-av-15-225.dat => 12CO10 typical spectra where 1 < Av <= 2 magn 12co10-stacked-spectrum-mean-av-2-6.dat => 12CO10 typical spectra where 2 < Av <= 6 magn 12co10-stacked-spectrum-mean-av-6-15.dat => 12CO10 typical spectra where 6 < Av <= 15 magn 12co10-stacked-spectrum-mean.dat => 12CO10 typical spectra where 15 < Av <= 225 magn 12co10-stacked-spectrum-mean-tdust-16-19.5.dat => 12CO10 typical spectra where 16.0 < Td <= 19.5 K 12co10-stacked-spectrum-mean-tdust-19.5-23.5.dat => 12CO10 typical spectra where 19.5 < Td <= 23.5 K 12co10-stacked-spectrum-mean-tdust-23.5-32.dat => 12CO10 typical spectra where 23.5 < Td <= 32.0 K 12co10-stacked-spectrum-mean-tdust-32-100.dat => 12CO10 typical spectra where 32.0 < Td <= 100.0 K II) The data also contain the results of the Lombardi et al. (2011) SED fit of the Herschel Gould Belt survey observations of the Orion B Giant Molecular Cloud (Andre et al. 2010). The next table lists the associated FITS file names and their contents. Av-values.fits => Spatial distribution of the dust visual extinction Av-masks.fits => Spatial distribution of the four masks of dust visual extinction Td-values.fits => Spatial distribution of the dust temperature Td-masks.fits => Spatial distribution of the four masks of dust temperature III) All the images are gridded in a custom set of coordinates, with the projection center set on the PDR of the Horsehead Nebula (RA-Dec coordinates provided in the header), and with an axis position angle of 14 degrees with respect to the North-South orientation [1]. The FITS file headers are WCS compliant, and our custom set of coordinates should be understood by any standard FITS reader. *************************************************************************** References: ----------- [4] Schneider et al., 2013, ApJ, doi:10.1088/2041-8205/766/2/L17 [3] Orkisz et al., 2017, A&A, doi:10.1051/0004-6361/201629220 [2] Gratier et al., 2017, A&A, doi:10.1051/0004-6361/201629847 [1] Pety et al. 2017, A&A doi:10.1051/0004-6361/201629862 ***************************************************************************