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Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: (l, b) mosaic of 12CO 1st moment in V, the intensity-weighted mean VLSR. The displayed velocity scale (from –190 to +96  km s−1) reflects all reliable 12CO emission, i.e., ignoring data from artifacts such as “weather stripes.”
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: (l, b) mosaic of 12CO 2nd moment in V, the intensity-weighted velocity dispersion σV. The displayed velocity scale (0–59  km s−1) reflects nearly all reliable 12CO emission, i.e., ignoring data from artifacts such as “weather stripes,” and saturating only a few small areas (e.g., near the Galactic center) with σV up to 166.5  km s−1.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Mean height vs. distance for each pixel in 355﹩\mathop{.}\limits^{^\circ }﹩3   >   l   >   348﹩\mathop{.}\limits^{^\circ }﹩0 from the (l, d) map of 12CO. The dots for each pixel are color coded by their S/N in the moment-0 map, as labeled, where the noise σrms ≈ 7 K arcmin (the limiting S/N  >  0 for the yellow dots is actually more like S/N  >  4 given the thresholding inherent in the SAMed data). Also overlaid is a rough visual fit of a sinusoid to the maximal 12CO ridgeline. This has a wavelength of 4 kpc and an amplitude of 50 pc, offset by z = +10 pc. The sloping lines indicate ThrUMMS’ latitude limits of  ± 1°, with a vertical exaggeration of about 20:1.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Sample deprojection of (l, V) data (mean height of NCO) into an (x, y) map on the BGT distance scale. The mirroring red tangent-point curve appears as a circle in this diagram.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Sample disambiguated ﹩\bar{z}﹩ map from NCO data using the ζ+ function as described in Appendix C.4.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Location of the Far Ara Clouds in (l, V) space, demarked by colored polygons (FA1 = red, FA2 = orange, FA3 = blue) overlaid on the mean latitude ﹩\bar{b}﹩ map for NCO, as in Figure A10.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Two 60° × 181  km s−1 ThrUMMS DR6 RGB-composite mosaics of (top) line intensity and (bottom) physical property, integrated or averaged across b (0th or –1st moment) as appropriate: i.e., lV diagrams. These are from the same data cubes as portrayed in Figures A1 and A2, except restricted to a smaller VLSR range in order to focus on the spiral arm emission. Line ratio and physical property variations persist in these projections as well. The data maximum and saturated color levels in these images are respectively at (top) 780.8 and 623.7 K arcmin (12CO), 233.4 and 153.7 K arcmin (13CO); and 37.49 and 15.85 K arcmin (C18O); (bottom) 7.095 and 3.751 K (mean Tex), 21.6 and 9.38 × 1026 molec m−2 arcmin (NCO), and 21.07 and 16.79 (mean ﹩{\tau }_{{}^{12}{{\rm{CO}}}}﹩).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: In Sector 342, as an example, an illustration of the origin of the velocity dispersion distributions can be seen in Figure A7. Using RGB color composites similar to Figures A1, A2, the panels show from top to bottom (with appropriate labels): the iso-CO composite masked to areas with σV(NCO)   > σthr = 2  km s−1; the same composite masked to areas with σV(NCO) ≤ σthr; the (Tex,N, τ) composite masked to areas with σV(NCO)   >  σthr; and the same (Tex,N, τ) composite masked to areas with σV(NCO) ≤ σthr. For a given composite, the three color channels are scaled to the same brightness and contrast levels in each mask, in order to normalize comparisons. A similar relationship between σV(NCO) and the brightness distributions of each quantity exists in all the other Sectors as well.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Two 60° × 200  km s−1 ThrUMMS DR6 mosaics of (top) 12CO-weighted and (bottom) NCO-weighted mean latitude: i.e., 1st-moment lV diagrams integrated across b. These are from the same data cubes as portrayed in Figure A9.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Comparison of NCO-weighted (labeled “ZM”) and 12CO-weighted velocity dispersions, i.e., the 2nd moment, across all (l, b) Sector data. Panel (a) is a copy of Figure 5. Panels (b) and (c) show histograms of pixel incidence for each dispersion separately, labeled with statistics of their distributions. Panel (d) shows, overlaid for both dispersions with red = NCO and black = 12CO, cumulative histograms of pixel incidence.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: (l, b) mosaic of NCO 2nd moment in V, the column-weighted velocity dispersion σV. The displayed velocity scale is the same as in Figure A3 for ease of comparison, and saturating only a few very small areas (e.g., near the Galactic center) with σV up to 86.7  km s−1. The spatial coverage of the NCO data is less than that of the 12CO data, as in Figure A4.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure 3, but for Sectors 300, 306, and 312 (left, middle, right columns respectively). The top panel in each column is at ThrUMMS’ native resolution of 72″. The second and subsequent rows show the analysis results for the cubes progressively convolved to a resolution of 126″, 252″, 504″, and 1008″, the last being the same resolution as that of the CfA survey (T. Dame et al. 2001).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Two 60° × 200  km s−1 ThrUMMS DR6 mosaics of (top) 12CO-weighted and (bottom) NCO-weighted latitude dispersion: i.e., 2nd moment lV diagrams integrated across b. These are from the same data cubes as portrayed in Figure A9.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B1, but for Sectors 318, 324, and 330 (left, middle, right columns, respectively). For S324–S354, the gas-phase [H2]/[12CO] abundance level was drawn at 3 × 104.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B2, but for Sectors 336, 342, and 348 (left, middle, right columns, respectively).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Two 60° × 210  km s−1 ThrUMMS DR6 mosaics of latitude-integrated (top) 12CO emission and (bottom) NCO: i.e., standard 0th-moment lV diagrams. [For computational convenience, the NCO scale is labeled as the equivalent mass surface density Σ = fNCO, where f = 1.88 × 10−24 M⊙ pc−2/(molec m−2), although we already know that this underestimates the gas-phase 12CO to H2 conversion (P. J. Barnes et al. 2018).] The 12CO and NCO moments are from the same data cubes as portrayed in Figure A9, but are here overlaid by curves at a series of fixed heliocentric distances. These start at –0.3 kpc (light gray; see text for an explanation), then run from 0 kpc (dark gray, very close to the VLSR = 0  km s−1 grid line) in steps of 1 kpc (red, green, ...) to 8 kpc (red again). They reflect the IAU-standard definition of LSR with the original conversions to (u0, v0, w0), but using the M. J. Reid et al. (2019) values for R0, Θ0, and their URC (line 1 of Table C1).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Direct overlay of all conversion law fits from CHaMP maps on the same scale (from P. J. Barnes et al. 2018), shown as representative power laws in log–log space, and labeled by Region or BYF catalog designator from P. J. Barnes et al. (2011). Because of the velocity integration, the  I fits are naturally located to the right of the V fits in the X = N/I vs. I diagram. The lower limits on the I scale among the V plots are set by the average noise levels in the respective data, while the upper-I limits come from the brightest pixels; the lower I limits among the I plots are typically where the data runs out, rather than where they become noise affected. The error bars in X for both groups are from the fit uncertainties in N0 at the lower-I end, and from uncertainties in the slope (= p–1) at the upper-I end. The axis scales are chosen to be square, so that slopes of 1 make a 45° angle to the axes.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: NCO/ICO ratio vs. ICO as in Figure B1, i.e., arranged in columns by Sector and in rows by resolution, but where each quantity is integrated over all velocity channels, regardless of whether NCO is defined in all the channels where ICO is detected. We do not include a (τ, Tex) grid here, since the velocity integration blurs the grid due to the variable number of channels used for each point.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Direct overlay of all conversion law fits from ThrUMMS Sectors (Figures B1–B4 and B5–B8), but presented similarly to Figure B9. The scale is set for the results from the finest-resolution data (dotted line labeled 72″). For the convolved data, each group (labeled 126″, ..., 1008″) is successively offset one order of magnitude lower for clarity of display, but they should be understood to lie on the same scale. The noise limits at the lower-I end for each group at 72″ are higher than for the CHaMP data (Figure B9), but in the case of the V fits, these limits go to lower levels with each successive convolution. The I-fit lower limits do not decrease because these are more affected by the lack of data, rather than just noise.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B1, but for Sector 354. The panels are at the same five progressive resolutions as in the previous three figures.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B5, but for Sector 354. The panels are at the same five progressive resolutions as in the previous three figures.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C1, except that the heliocentric curves were obtained using the full BeSSeL solution from M. J. Reid et al. (2019; line 2 of Table C1).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B5, but for Sectors 318, 324, and 330 (left, middle, right columns, respectively).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar plots to Figure B5, but for Sectors 336, 342, and 348 (left, middle, right columns, respectively).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C3, except that the heliocentric curves are now from a hybrid BeSSeL+Gaia-Cepheids solution as described in the text, plus optimized fits to the local clouds near l ≈ 300°–306°and 340°–353° (line 5 of Table C1).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C6 but deprojected onto the BGT distance scale (Figure C5 contours) as an (l, d) map. The mirroring red tangent-point curve runs from (360°, 8.24 kpc) to (300°, 4.12 kpc) in the BGT model. (Top) 12CO data. (Bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: (Top) 12CO (l, V) data as in Figures A9 and C1–C5, but deprojected onto the IAU distance scale (Figure C1 contours) as an (l, d) map. This includes both the near and far kinematic distance solutions, which are mirrored along a sinusoidal curve (in red) from (360°, 8.15 kpc) to (300°, 4.075 kpc), at the tangent-point distance for each l. (Bottom) Same as the top panel but with the NCO (l, V) data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C2, except that the heliocentric curves are now from a modified BeSSeL solution, optimized to fit the 0 kpc curve (dark gray) to the local clouds near l ≈ 300°–306°and 340°–353° (line 3 of Table C1).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Cartesian deprojection, based on the IAU model for Galactic rotation (Figure C1 contours), of the 12CO (l, V) data into Galactic (x, y) space, where the +x-direction points from the Sun up to the Galactic center (GC) and the +y-direction from the Sun left toward l = 90°. The Sun is at coordinates (0,0), the GC at (8.15,0), and the red circle denotes the locus of tangent-point distances in this model.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C7 (i.e., using the BGT model) but for the 1st latitude moment (mean latitude ﹩\bar{b}﹩) in the 12CO (top) and NCO (bottom) data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C3, except that the heliocentric curves are now from a hybrid BeSSeL+VERA solution as described in the text, plus optimized fits to the local clouds near l ≈ 300°–306°and 340°–353° (line 7 of Table C1).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C8 but using the BGT rotation model (Figure C5 contours), where the Galactic center is at coordinates (8.24,0).
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C10 but for the NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Same as Figure C8 but for the NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C13 (latitude dispersion σb) but where the angular dispersion has been rescaled to a physical size via the distance (y-axis), as in Figure C15. This gives a height dispersion which becomes progressively wider as d increases, up to ∼230 pc at far kinematic distances, even while it remains small (≲30 pc) where d ≲ 3 kpc. (Top) 12CO and (bottom) NCO data.
Paper: The Three-mm Ultimate Mopra Milky Way Survey. III. Data Release 6, An Atlas of Physical Conditions, Global Mass Conversion Laws, and 3D Physical Architecture of the Molecular Interstellar Medium in the Fourth Quadrant
Authors: Peter J. Barnes, Dylan G. H. Barnes, Audra K. Hernández, Sebastian Lopez, Erik Muller
Figure caption: Similar (l, d) maps to Figure C7 (latitude-integrated 12CO emission and NCO (l, d) diagrams) but where the integrals have been masked via the ζ+ function. This gives a first-order near/far deprojection of molecular clouds across the 4Q, based on the known thickness of the Galaxy’s molecular layer, a few tens of parsecs, at both near (below the tangent mirror curve) and far (above the curve) distances. (Top) 12CO and (bottom) NCO data.