adsabs/AstroCLIMB huggingface dataset:
Paper: A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO
Authors: Mandana Amiri, Daniel Amouyal, Bridget C. Andersen, Shion Andrew, Kevin Bandura, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Alyssa Cassity, Shami Chatterjee, Alice P. Curtin, Matt Dobbs, Fengqiu Adam Dong, Yuxin Dong, 雨欣 董, Gwendolyn M. Eadie, Tarraneh Eftekhari, Wen-fai Fong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Hans Hopkins, Adaeze L. Ibik, Ronniy C. Joseph, Jane Kaczmarek, Lordrick Kahinga, Victoria Kaspi, Kholoud Khairy, Charles D. Kilpatrick, Adam E. Lanman, Mattias Lazda, Calvin Leung, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Nikola Milutinovic, Kenzie Nimmo, Gavin Noble, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Emily Petroff, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mubdi Rahman, Andre Renard, Mawson W. Sammons, Ketan R. Sand, Paul Scholz, Vishwangi Shah, Kaitlyn Shin, Seth R. Siegel, Sunil Simha, Kendrick Smith, Ingrid Stairs, Keith Vanderlinde, Haochen Wang, Dallas Wulf, Tarik J. Zegmott
Figure caption: Publicly available images for the 21 host galaxies in our gold sample (those with P(O∣x) > 0.9) as well as FRB 20230311A (see text), taken from the DECaLS or Pan-STARRS archive. The hosts of FRB 20231202A and 20230730A are difficult to detect in imaging due to Galactic extinction; the latter was spectroscopically confirmed (see Table 2). The images of other fields (FRB 20230222B, 20231123A, and 20231223C) lacked one or more color channels in publicly available images, resulting in their tinted appearance.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: Coverage and depth from various published (blue) and ongoing or planned (red) TNO surveys. The proposed project (Rubin-NHDDF) would reach deeper into the KBO population, opening a new component of this phase space.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: Example of detection of a real moving object made via the shift-and-stack technique from W. C. Fraser et al. (2024a). Top: three individual frames acquired with the Hyper Suprime-Cam on the Subaru Telescope. Red circles mark the object’s positions, barely visible above the noise floor. Bottom: shift-stacks of difference imagery from the same regions as presented above. The stacks were made at rates of motion of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩0, 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5, and 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩0  hr−1 (left to right). The true rate of motion of the object is 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩9 hr−1.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: The opaque circle indicates the NHDDF relative to the Galactic plane (image from 2MASS M. F. Skrutskie et al. 2006) displayed using the Aladin Sky Atlas (F. Bonnarel et al. 2000). The coordinate grid is latitude by longitude in ecliptic degrees.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: H magnitude distribution for KBOs discoverable at the New Horizons search location as a function of survey depth. The input model is the OSSOS++ model and does not include the putative distant population; see text for details. The corresponding size of these objects, assuming an albedo of pV = 0.10, is shown along the top axis. The y-axis is the number of objects discovered at each H magnitude/size based on survey magnitude depth, denoted by the color shown in the inset key.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: The probability density (p) vs. discovery distance from the New Horizons spacecraft for Rubin discoveries with projected LORRI magnitudes of V < 20.5 and currently beyond 70 au. Approximately 40% of objects discovered beyond 70 au will come within 1 au of the spacecraft.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: A sample of image-series stacks followed by subtraction of a sky template of stable sources, and then identification of moving objects within those differenced images.
Paper: An Extremely Deep Rubin Survey to Explore the Extended Kuiper Belt and Identify Objects Observable by New Horizons
Authors: J. J. Kavelaars, Marc W. Buie, Wesley C. Fraser, Lowell Peltier, Susan D. Benecchi, Simon B. Porter, Anne J. Verbiscer, David W. Gerdes, Kevin J. Napier, Joseph Murtagh, Takashi Ito, Kelsi N. Singer, S. Alan Stern, Tsuyoshi Terai, Fumi Yoshida, Michele T. Bannister, Pedro H. Bernardinelli, Gary M. Bernstein, Colin Orion Chandler, Brett Gladman, Lynne Jones, Jean-Marc Petit, Megan E. Schwamb, Pontus C. Brandt, Joel W. Parker
Figure caption: New Horizons search field with the Rubin footprint (pink circle). This plot shows the current sky locations of model objects (black points and sky-density contours) that pass within 1 au of New Horizons between 2027 and 2040 and have r < 28.5 in 2026 July. The model is based on the OSSOS++ sample (J.-M. Petit et al. 2023a) and is a 20× oversampling of the expected total population of the Kuiper Belt.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: The extent of our Quaia-VLASS sample along the G (optical) and t (radio) bands. Radio-loud and radio-quiet sources are separated by the black line. We defined three bins in the G band, which we later analyze separately in the rest of the paper when looking for brightness-dependent trends in radio-loudness. The dashed line shows the t = 16.6 sensitivity limit, as inferred from the rms noise limit stated in M. Lacy et al. (2022), which agrees reasonably well with the lack of sources in the figure at t > 16.6. The Quaia catalog has a limit at G = 20.5 as imposed by K. Storey-Fisher et al. (2024). The region within which there is sensitivity in G and sources would be radio-loud, but lies beyond the sensitivity limit in t, is labeled “indeterminate region.”
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: The G − t magnitude difference, i.e., our proxy for radio-loudness, and its median in various bins. All error bars are equal to ﹩{\rm{median}}(G-t)/\sqrt{{n}_{{\rm{c}}}}﹩, with nc being the number of crossmatched QSOs in this bin and median(G − t) being the median within the same bin. Top: we bin our catalog on the Quaia selection function (completeness) values, and also illustrate the role of the Galactic extinction correction. Bottom: we bin our sample on redshift, and also on G magnitudes (see colors), and identify weak trends at the lowest redshifts (z < 0.5).
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: The RLF Nloud/Nquaia of QSOs in different bins as a function of G (black curve), the number of Quaia quasars within these bins (blue histogram) and the number of radio-loud crossmatches (orange histogram). The background color coding along G is equivalent to the color coding in Figure 4. The black curve shows that even though it is expected to underestimate the RLF at G > 18.5, due to the effect of the indeterminate region (see Figure 4), such a trend of a sudden drop in the curve is not observed. The errors are calculated via the binomial standard error ﹩\sqrt{f(1-f)/{n}_{{\rm{b}}}}﹩, where f is the RLF in a bin and nb is the total number of QSOs in the bin.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: The distribution of the radio-loudness measure G − t for all Quaia sources and the Quaia-VLASS crossmatches. The vertical black line is the delineation between radio-quiet (G − t ≤ 2.5) and radio-loud (G − t > 2.5) sources. The blue arrow indicates that the shape of the blue distribution would shift to the left, if for these sources, real measurements for t, instead of estimates, were present.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: On the left, the distribution of the 1.1 million Quaia sources that fall within the joint coverage with the VLASS survey (δ > −40°). The dust obscuration in the Milky Way disk results in the detection of fewer QSOs in the optical. On the right, the distribution of the 1.9 million VLASS2 QL sources after applying quality flags (see Table 1). Unlike for optical QSOs, the radio coverage is virtually unaffected by the Galactic disk.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: Left: the number of crossmatched sources as a function of a search radius parameter in arcseconds. We performed a robustness test using randomly perturbed sky coordinates, and found that a search radius of 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 results in a low level of contamination (<0.1%) from false matches (right). We thus choose this threshold for our crossmatched Quaia-VLASS sample.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: The distribution of angular separation values when crossmatching the Quaia and VLASS samples, up to the 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 search radius threshold that we applied. The inset shows the closest matches below Δθ = 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩2.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: Normalized histograms of the radio-loud and radio-quiet populations as a function of Gabs. On the left, we show the full sample of crossmatches, while on the right, a G < 18.5 cut is applied. The error bars in the figure are Poisson errors equal to ﹩{n}_{{\rm{norm}}}/\sqrt{{n}_{0}}﹩with nnorm being the displayed normalized counts within the bin and n0 the nonnormalized counts in the same bin.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: RLF of Quaia sources color-coded as a function of the absolute magnitude Gabs and the redshift z. We observed significant noise due to the small number of statistics at the bright-end pixels, leading to strong fluctuations in the RLF. The inset shows the spread of ΔGabs being comparatively small to the grid width of Gabs in the large figure.
Paper: Radio-loudness Statistics of Quasars from Quaia-VLASS
Authors: Nestor Arsenov, Sándor Frey, András Kovács, Lyuba Slavcheva-Mihova
Figure caption: Quasar RLF in different parts of the sky. We find significant fluctuations near the Milky Way, i.e., where the Quaia catalog is knowingly less complete (although on average, there are no clear biases near the Galactic plane either, see the top panel of Figure 7). In the cleanest areas of the sky, we do not identify any relevant anisotropies in the RLF.
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 plot for Sector 300 of the distribution of radiative transfer solutions for NCO, derived from the three iso-CO species as a function of the observed ICO in each voxel (i.e., each pixel and velocity channel) of (l, b, V) space at the native ThrUMMS angular resolution of 72″. Similar plots for the other Sectors are shown in Appendix B. The  >106 data points here (black dots) are plotted in the N/I vs. I plane, effectively an X vs. I plot once a gas-phase R12 = [H2]/[12CO] abundance ratio is chosen. The magenta label and dotted line are then illustrative of where the standard X factor would lie for the given R12. Thin yellow contours outline the distribution where the density of points is high, at levels of 10% to 80% of the peak density, in intervals of 10%. Underlying the plot is a grid of radiative transfer solutions, with solid curves at constant τ and dotted curves at constant Tex, as labeled. The dotted red curve joins up the mean X value in each of 30 equally spaced bins of data in logI, while the dotted green curves join the  ±1σ levels around the red means in each bin. The cyan curves show the 1σ and 2σ limits in the data: the vertical limits to the left are from the 12CO noise limits; the curved limits dropping to the right come from the 13CO noise limits. The red and green curves are shown as solid, where a linear regression to the mean ±σ values gives the results labeled in red, generally where the points have an S/N   >   2–3. Because the fit is made in X vs. I space, one must add 1 to the labeled slope to obtain the corresponding value for p in the conversion law, N ∝ Ip. In this case, p = 1.91 ± 0.03. The intercept logN0 applies at logI = 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: Sample 15° × 2° area (one-quarter) of ThrUMMS DR6; the full mosaics are given in Appendix A. Top. Pseudocolor image of integrated intensity (0th moment) in the three iso-CO J = 1 → 0 lines, as labeled. Note the wide variations in line ratios across the Galactic plane, evident from the varying colors in this image. The data maximum, saturated color, median uncertainty, and black levels in this image are respectively at 1137, 265, 1.91, –5 K km s−1 (12CO); 229, 70, 0.75, –2.4 K km s−1 (13CO); and 33, 9.6, 0.37, 0.0 K km s−1 (C18O). Bottom. Same area as top panel, but with color-coded physical parameter solutions (as labeled) from the analysis in Section 3, which makes manifest the radiative transfer implied in the iso-CO line ratios. The data maximum, saturated color, median uncertainty, and black levels in this image are respectively at 3.16, 0.85, 0.054, –0.03 K (mean Tex), 257, 44, 1.43, and –0.4 × 1024 mol cm−2 (NCO), and 5.53, 3.67, 0.0093, –0.11 (mean ﹩{\tau }_{{}^{12}{{\rm{CO}}}}﹩). Note that the Tex and τ scales are artificially low, since the averaging has been done over channels with no solution (taken as 0), putting the intensity in each on a relative scale only.
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: Iso-CO line intensity ratio–ratio diagram across all ThrUMMS DR6 data. Each point is one (l, b, V) data voxel where all three iso-CO lines are above the color-coded S/N ratio, from among 360,000 voxels with S/N  >  0. Contours of pixel density, at 67%, 78%, and 89% of the peak density, are also shown for each of the top three S/N levels, to highlight their near concentricality around ratios I13/I12 = 0.6 ± 0.2 and I18/I13 = 0.35 ± 0.10. Also shown is the grid of radiative transfer solutions from Section 3 for any ratio–ratio point. If we use a different value for R13 than that shown here (say, 40), it changes the underlying grid (and the solutions for all the data points) very little, compressing only the three leftmost contours of τ18 in the top left corner of the diagram slightly to the right, far from any 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: Summary of conversion law analysis, where the index p in Equation (5) equals 1+the slope as measured in Figure 3, and its brethren described in Appendix B. (Left) All measured slopes from the per voxel analysis (panels of Figures B1–B4) labeled by Sector. (Right) All measured slopes from fits to the velocity-integrated data (panels of Figures B5–B8).
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 (2nd moments) across all 3 × 106 (l, b) pixels. Overlaid are yellow contours of pixel density at 2%, 6%, 10%, ..., 98% of the peak, showing that the data distribution in this space is not random, but rather, appears constrained to two separate, distinct domains. The majority of pixels lie close to the dotted black line (along the x-axis); these pixels have σV(NCO) ≪ σV(12CO). Nearly all other pixels lie close to the dotted blue line of equality, and so obey σV(NCO) ≈ σV(12CO).
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 (in this case, integrated NCO) into an (l, d) map using our favored BGT distance scale (Table C1). The mirroring red tangent-point curve runs from (360°, 8.24 kpc) to (300°, 4.12 kpc) in the BGT 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: More samples of the physical parameter composites (as labeled, similar to the lower panel of Figure 1), illustrating the overall gradient in NCO across the 4Q. The color scales here are identical in each panel and the same as those in Figure A2.
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: Color-composite images of the physical parameter solutions in (l, b) mosaics (red = mean Tex, green = integrated NCO, blue = mean ﹩{\tau }_{{}^{12}{{\rm{CO}}}}﹩) from the analysis in Section 3. This makes manifest the radiative transfer effects implied in the iso-CO line ratios of Figure A1. The data maximum, saturated color, median error, and black levels in these images are respectively at 3.16, 0.85, 0.054, –0.03 K (mean Tex); 257, 44, 1.43, and –0.4 × 1024 molec m−2 (NCO); and 5.53, 3.67, 0.0093, –0.11 (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: Color-composite images of the integrated intensity (0th moment in V) (l, b) mosaics in the three iso-CO lines, as labeled. Each of the three mosaics is available digitally as part of DR6. The data maximum, saturated color, median error, and black levels in this image are respectively at 1137, 265, 1.91, –5 K km s−1 (12CO); 229, 70, 0.75, –2.4 K km s−1 (13CO); and 33, 9.6, 0.37, 0.0 K km s−1 (C18O).
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 1st moment in V, the column-weighted mean VLSR. The displayed velocity scale is the same as in Figure A3 for ease of comparison. The spatial coverage of the NCO data is, of course, less than that of the 12CO data, since solving the radiative transfer equations requires a reasonable S/N for both 12CO and 13CO data.