adsabs/AstroCLIMB huggingface dataset:
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: G23.207−00.377: (a) The continuum emission detected using JVLA at the C band (colors) and K band (white contours). The contours correspond to 3σ, 7σ, 9σ, and 12σ (where σ is listed in Table 1). The synthesized beam sizes are presented at the bottom left corner; the transparent ellipse with black outline and the white ellipse correspond to C- and K-band data, respectively. (b) The continuum emission overlaid with methanol and water maser spots detected using JVLA. Their sizes are proportional to the logarithm of Sp of methanol and water peak fluxes, respectively. The colors of spots correspond to the LSR velocities as presented on wedges. (c) The spectra and the distributions of the maser transitions presented in this article and from A. Bartkiewicz et al. (2009, 2011). The (0, 0) point corresponds to the brightest methanol maser spot (Table 3). The vertical light gray lines in the spectra represent the systemic velocities of sources as in M. Szymczak et al. (2007). The sizes of the symbols are proportional to the logarithm of the peak flux density of a spot. The gray arrows in the left and right panels point out the variable (over 14 yr) methanol maser features. The thin and thick crosses correspond to the peaks of C- and K-band radio continua with their positional uncertainties, respectively. The gray ellipse traces the best flux-weighted fit as in A. Bartkiewicz et al. (2024).
Paper: Earth Analogs in Reflected Light: Insights from Early Spectral Characterization in Unconstrained Orbits
Authors: Arnaud Salvador, Tyler D. Robinson
Figure caption: Reflected-light spectrum of the fiducial case (black curve; see Figure 2 and Table 1) and corresponding signal-to-noise ratio (S/N; colored y-axes) as a function of wavelength for each color-coded spectral coverage (Table 2). The left, oblique, and right ticks of each colored y-axis correspond to ﹩{\rm{S}}/{{\rm{N}}}_{{\lambda }_{0}}=10﹩, 15, and 20, respectively, where λ0 (indicated by vertical lines) is the lower bound of each spectral coverage at which the specified ﹩{\rm{S}}/{{\rm{N}}}_{{\lambda }_{0}}﹩ is defined; see text to extract the S/N at any wavelength of interest.
Paper: Earth Analogs in Reflected Light: Insights from Early Spectral Characterization in Unconstrained Orbits
Authors: Arnaud Salvador, Tyler D. Robinson
Figure caption: Corner plot showing the marginal univariate (along the diagonal) and joint bivariate (off-diagonal) posterior distributions of all 17 retrieved parameters from observations conducted in the visible bandpass at S/N = 10. The retrieved values (loosely dashed) and their ±1σ (68%) credible intervals (loosely dotted) are indicated by vertical lines on the 1D marginal distributions (i.e., the 16th, 50th, and 84th percentiles). The contours of the 2D posterior distributions correspond to the 1σ, 2σ, and 3σ levels, which encompass 68%, 95%, and 99.7% of the observed values, respectively. Note that these levels correspond to 39.3%, 86.5%, and 98.9% of the volume in 2D distributions, and to 68%, 95%, and 99.7% in 1D distributions. The vertical and horizontal dashed lines indicate the Earth-based input values.
Paper: Earth Analogs in Reflected Light: Insights from Early Spectral Characterization in Unconstrained Orbits
Authors: Arnaud Salvador, Tyler D. Robinson
Figure caption: Corner plot showing the marginal univariate (along the diagonal) and joint bivariate (off-diagonal) posterior distributions of all 17 retrieved parameters from observations conducted in the NIR bandpass at S/N = 20. The retrieved values (loosely dashed) and their ±1σ (68%) credible intervals (loosely dotted) are indicated by vertical lines on the 1D marginal distributions (i.e., the 16th, 50th, and 84th percentiles). The contours of the 2D posterior distributions correspond to the 1σ, 2σ, and 3σ levels, which encompass 68%, 95%, and 99.7% of the observed values, respectively. Note that these levels correspond to 39.3%, 86.5%, and 98.9% of the volume in 2D distributions, and to 68%, 95%, and 99.7% in 1D distributions. The vertical and horizontal dashed lines indicate the Earth-based input values.
Paper: Earth Analogs in Reflected Light: Insights from Early Spectral Characterization in Unconstrained Orbits
Authors: Arnaud Salvador, Tyler D. Robinson
Figure caption: Posterior distributions of the orbital distance (top) and planetary phase angle (bottom) obtained from observations in different color-coded spectral coverages at signal-to-noise ratios (S/Ns) of 10 (left side of the split-violins, without contour lines), 15 (right side, with dashed contours), and 20 (right side, with solid contours). The horizontal dashed lines spanning each violin row indicate Earth-like input values, while the dashed lines within the violins show the 25th, 50th, and 75th percentiles of the data (the first quartile, median, and third quartile, respectively). The density has been normalized across all kernel density plots so that each has the same area.
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Similar to Figure 1 but for G23.389+00.185. (a) The contours of the K-band emission correspond to 3σ, 7σ, 11σ, 16σ, and 20σ. (c) The red and orange crosses trace the NIR and MIR emissions from (J. M. De Buizer et al. 2012), respectively. The crosses trace the likely spurious spots (see Section 4.1).
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Similar to Figure 1 but for G23.657−00.127: (a) The contours of the K-band emission correspond to 1σ and 3σ. (c) The red and orange crosses trace the NIR and MIR emissions from J. M. De Buizer et al. (2012), respectively. The crosses trace the likely spurious spots (see Section 4.1).
Paper: Detections of Compact Radio Continuum toward Methanol Maser Rings Using the VLA
Authors: Anna Bartkiewicz, Olga Bayandina, Alberto Sanna, Marian Szymczak, Luca Moscadelli, Agnieszka Kobak, Huib Jan van Langevelde, Ashwin Varma
Figure caption: Similar to Figure 1 but for G28.817+00.365: (a) The contours of the K-band emission correspond to 3σ, 10σ, 40σ, and 80σ.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Top: Swift-XRT light curve, with the quiescent level (red dashed line) and ±3σ bounds (dotted lines) estimated via one iteration of the 2σ-clipping method. Bottom: NuSTAR light curve with selected flare intervals shaded in gray. The red-shaded regions indicate intervals overlapping with the EP observations. Quiescent level and ±3σ band are overlaid using the same sigma-clipping procedure, with seven iterations. Bin size = 3600 s.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Count rates from Swift, NuSTAR, and EP observations of AU Mic. The main panel shows background-subtracted Swift (0.3–10 keV), NuSTAR FPM-A/B average (3–20 keV), and EP-FXT-A/B average (0.5–10 keV) count rates, all binned at 3600 s. The 0–0.15 cps range is expanded in the inset, which displays the NuSTAR data in greater detail. Error bars denote 1σ uncertainties.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Correlation between HXR (NuSTAR, 3–20 keV) and SXR (corrected EP, 0.3–3 keV) luminosities. The data are binned with a fixed bin size of 240 s to minimize statistical noise from NuSTAR’s relatively low count rates. NuSTAR time bins with zero count rates were excluded to avoid suppression of correlation strength. Additionally, a small number of bins exhibiting anomalously high or low luminosities, often due to edge effects or dominated by upper limits with large uncertainties, were excluded from the regression fits. These excluded points typically had extremely weak or absent hard X-ray signals. The blue line shows the best-fit LSR, while the red line represents the ODR, which accounts for errors in both axes. The purple line represents the median of the Bayesian linear regression posterior, obtained via Markov Chain Monte Carlo sampling, with the shaded region showing the 90% posterior confidence interval. Corresponding fit parameters are listed in Table 4. The SXR–HXR luminosity scaling we derive spans only 1 order of magnitude in luminosity; expanding the dynamic range is required in order to generalize the slope.
Paper: The ALMA-QUARKS Survey: Evidence of a Candidate High-mass Prestellar Core Aside a Bright-rimmed Cloud IRAS 18290-0924
Authors: Dongting Yang, Hong-Li Liu, Sheng-li Qin, Tie Liu, Anandmayee Tej, Siju Zhang, Xunchuan Liu, Fengwei Xu, Guido Garay, Lei Zhu, Patricio Sanhueza, Xiaofeng Mai, Wenyu Jiao, Paul F. Goldsmith, Sami Dib, Pablo García, Di Li, Jinhua He, A. Y. Yang, Prasanta Gorai, Suinan Zhang, Yankun Zhang, Jianjun Zhou, Mika Juvela, James O. Chibueze, Chang Won Lee, Jihye Hwang, Leonardo Bronfman, Xindi Tang, Archana Soam, Tapas Baug, Yichen Zhang, Swagat Ranjan Das, L. K. Dewangan, L. Viktor Tóth
Figure caption: Three-color image of Spitzer 8 μm (red), 4.5 μm (green), and 3.6 μm (blue) of the region associated with I18290. The black contours represent the 1.28 GHz MeerKAT emission. The white and green dashed circles show the field of view of the ATOMS and QUARKS survey, respectively. ATOMS 3 mm dust continuum emission is shown as the cyan contours, with levels starting at 3σ3 mm (∼0.1 mJy beam−1) and increasing as [6, 12, 24, 48] × σ3 mm. The purple cross symbol shows the location of Core 2 (S. Zhang et al. 2023). The synthesized beam size of the ATOMS survey and the 0.5 pc scale bar are shown in the lower left corner and upper right corner, respectively.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Full-band total luminosity and HXR energy fraction (bin size = 3600 s). Top: Total luminosity Ltot = LHXR + LSXR + LEUV obtained using ODR scaling relations. Error bars show 1σ uncertainties. Shaded gray bands mark flare intervals. Bottom: Time evolution of the HXR energy fraction EHXR/Etot, where energies are per-bin integrals E = L Δt with Δt = 3600 s. Results use the same ODR relations; error bars denote 1σ uncertainties in EHXR/Etot. The fraction stays at the few-percent level in quiescence and modestly increases during flares, indicating only limited changes in the spectral energy partitioning across HXR, SXR, and EUV.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Flare 2 spectral comparison. Absorbed thermal model tbabs+apec (left) versus absorbed thermal+nonthermal model tbabs∗(apec+power-law) (right). In both panels, the observed spectrum (points) is shown together with the best-fit model (solid line) and the background level (star symbols). Adding the power law reveals a modest high-energy tail relative to a purely thermal fit. After outlier rejection, all data channels above 20 keV lie below the background, indicating that emission beyond this energy is background-dominated. Black points denote FPM-A; red points denote FPM-B.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: NuSTAR hard X-ray light curves and hardness evolution. Top: energy-flux light curves in 3–6 keV (LEHXR, blue circles) and 6–20 keV (HEHXR, red squares) obtained by converting FPM-A/B count rates using spectral-fit ECFs and averaging the two modules; points show 1σ uncertainties. Gray shaded bands mark the identified flare intervals. Bottom: time-resolved fraction of HEHXR relative to the LEHXR; the red dashed line denotes equal contributions from low and high bands. The HEHXR fraction decreases during flares, indicating that the flare-associated enhancement is concentrated in the lower-energy 3–6 keV range. Bin size is 3600 s.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: NuSTAR hard-band light curves and time-resolved plasma diagnostics (bottom). The lower panel shows the best-fit temperature T (left axis) and emission measure EM (right axis) with asymmetric error bars. Note that the bin sizes for T and EM differ: for the first flare, we use 1200 s bins; for the second flare, we use per-orbit bins, except for the early rise, which uses 1800 s. Shaded regions indicate flare intervals; time is in hours since the reference epoch on the x-axis.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Joint spectral fitting results. Black points: FPM-A data. Red points: FPM-B data. Green points: FXT-A data. Blue points: FXT-B data. The top panel shows the observed spectra and the best-fit folded model, while the bottom panel displays the residuals in units of σ.
Paper: Hard X-Ray Emission in AU Mic Flares: A Minor Contributor to Planetary Atmospheric Escape
Authors: Yifan Hu, Murray Brightman, Fabio Favata, Haiwu Pan, Brian Grefenstette, Fiona A. Harrison, Daniel Stern, Weimin Yuan, Yuk L. Yung, Xiurui Zhao
Figure caption: Top: NuSTAR spectrum of Flare 1 with the best-fit absorbed apec model overlaid. Bottom: NuSTAR spectrum of Flare 2 with the best-fit absorbed apec model overlaid. Black points denote FPM-A data, and red points denote FPM-B data.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Four diagrams describing a simplified geometric picture of the shell. The top left and top right panels show a three-dimensional schematic of the “biconcave disk” shape viewed from two different angles and with a solid and transparent wireframe surface, respectively. The front side has been opened to show the inside of the shape as well as model how M16 may be broken open; observations suggest it is either broken or very thin toward the front and back. Pink frames numbered 1–3 outline the crosscuts, which are diagrammed in the lower left (1) and lower right (2) panels of this figure and in the top panel of Figure 16 (3). The top right panel shows the shell viewed approximately face-on from the observer’s perspective and includes a semitransparent rectangular overlay representing the Northern Cloud, which obstructs the left lobe of the cavity, and a circle representing N19, both of which appear in the #2 crosscut. The bottom left panel shows crosscut #1 marked in the top right panel, along the plane of the sky. Gas phases and the exciting cluster, NGC 6611, are labeled. The bottom right panel shows crosscut #2, marked in the top two panels, which includes the Northern Cloud and N19. It is not determined whether N19 has an intact background shell, so that side is represented by a hashed surface. We do not detect a foreground or background molecular gas shell, so these are excluded from the diagram. The scale bar indicates that the physical separation between NGC 6611 and the Northern Cloud/N19 is unknown, although we estimate it in Section 5.2 to be ≲102 pc.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The top panel shows an observer’s line-of-sight crosscut through the M16 shell and cavity, marked as #3 in the three-dimensional diagrams in Figure 15. The front and back of the shell are depicted as broken open. The black horizontal arrow through the top of the shell shows an observer’s line of sight, and numbered black-dashed circles mark where the line of sight crosses neutral PDRs, which would radiate [C II] line emission. The bottom panels show a cartoon spectrum on the left and observed [C II] spectra on the right. The line-of-sight PDR crossings circled in the top panel would contribute the colored dashed-line spectrum components, numbered accordingly, in the cartoon spectrum. The solid black cartoon spectrum is the sum of the four component spectra, representing what would be observed. This is described in more detail in Section 5.1. The observed spectrum labeled “Western cavity circle” is from the circular region shown in Figure 10 toward the shell fragments. We include a spectrum toward the blueshifted clump, a shell fragment with a clear IR counterpart (Section 4.4, Figure 11). The average [C II] spectrum from the entire field is shown in dashed–dotted gray to emphasize the natal cloud component near VLSR = 25–26 km s−1. The observed spectra are consistent with our model.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The top two panels show [C II] (black) and [13C II] (red) spectra averaged within the two circles in Figure 17; the left circle’s spectra are on the left here. The step plots show spectra binned to 1 km s−1 channels. The [13C II] spectra are scaled up by the factor α/sF, described in the text, and shifted by −11.2 km s−1 to account for the [13C II] rest frequency. The horizontal line shows the 1σ level for [C II] scaled up by α/sF and adjusted for the number of averaged spectra. Note that the lower-velocity side of the [13C II] line overlaps with the relatively bright high-velocity line wing of the [C II] line. The bottom panels show the [C II]/ [13C II] ratio (gray bars) and the [C II] optical depth and associated uncertainty (blue points). We exclude channels where [13C II] is below 1σ or where [C II] TMB exceeds the adjusted [13C II] TMB. This figure is based on those by C. Guevara et al. (2020).
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Ratio of the shell kinetic energy to the cluster’s mechanical energy (mechanical luminosity × age) plotted against the age of the cavity for a few H II regions including M16 and N19 from this work. Lines represent idealized evolutionary tracks following a burst, and subsequent decoupling of gas motion from mechanical input, at the age given in the legend. The diagram and evolution within it are discussed further in the text of Section 9.1.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Equivalent shell density plotted against shell expansion velocity for a few H II regions including M16 and N19 from this work. The mass of the shell is translated to an “equivalent” density ﹩\frac{{Q}_{0}}{{\beta }_{B}}\frac{\mu {m}_{{\rm{H}}}}{{M}_{{\rm{shell}}}}﹩ where the recombination rate coefficient βB = 2.3 × 10−13 cm3 s−1 (A. G. G. M. Tielens 2010). We use PDR shell masses for N19 and M16, neglecting any molecular gas. The equivalent density and expansion velocity are related through the initial density of the medium. Contours show several initial, prebubble densities (per cubic centimeters; L. Spitzer 1978). Regions that fall to the left of all contours have expanded too rapidly to be purely thermally driven and must have been wind blown. Note that expansion velocity decreases to the right, so that over time a shell would advance to the right-hand side along a contour.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: The CO line model grid solutions for N19. Gray points in the central panels mark individual pixel solutions and their χ2 = 1 contours, which we use as error ellipses. Each pixel’s error bars are calculated from the error ellipse. The curves show the median (solid) and mean (dashed) line measurements. The shaded regions around the curves show the 16th to 84th percentile ranges for the measurements. Histograms along each axis show the pixel solution distributions for each parameter. Their medians (circle) and means (X) are marked in pink along with the 16th to 84th percentile range, which is used as uncertainty. The median solutions and uncertainties are overlaid onto the central grid in pink.
Paper: SOFIA FEEDBACK Survey: The Eagle Nebula in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G.G.M. Tielens, Jelle S. Kaastra, Leisa K. Townsley, Patrick S. Broos, Maitraiyee Tiwari, Lars Bonne, Ümit Kavak, Mark G. Wolfire, Nicola Schneider, Robert Simon, Rolf Güsten, Jürgen Stutzki, Marc Mertens, Oliver Ricken, Friedrich Wyrowski, Lee G. Mundy
Figure caption: Integrated [C II] (color image) and [13C II] (contours) intensities between VLSR = 26–31 km s−1 toward IRAS 18156–1343 (orange diamond) along the Bright Northern Ridge. Circles show the two regions in which spectra are averaged for Figure 18. Each circle is 4 [C II] beams across. The emission from within the left circle is ∼1 km s−1 higher velocity than that from the right circle. The brightest [C II] emission locations are slightly offset from the [13C II] emission locations.