adsabs/AstroCLIMB huggingface dataset:
Paper: Scaling K2. VII. Evidence For a High Occurrence Rate of Hot Sub-Neptunes at Intermediate Ages
Authors: Jessie L. Christiansen, Jon K. Zink, Kevin K. Hardegree-Ullman, Rachel B. Fernandes, Philip F. Hopkins, Luisa M. Rebull, Kiersten M. Boley, Galen J. Bergsten, Sakhee Bhure
Figure caption: As for Figure 4, but for the significantly smaller Hyades GKM sample.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: A comparison between models with different ﹩{l}_{\max }﹩ and N using different model selection criteria. For clarity we have left off N = 1 and ﹩{l}_{\max }=1﹩ fits as they are all rejected with very high confidence. Note that higher ﹩{\mathrm{elpd}}_{\mathrm{LOO},{ \mathcal M }}﹩ and lower BIC are desired; this is reflected in the color bars, where yellow indicates better performance. Top: ﹩{\mathrm{elpd}}_{\mathrm{LOO},{ \mathcal M }}﹩ for each combination of ﹩{l}_{\max }﹩ and N relative to the lowest score in the grid. There is a clear jump in model preference when adding the fifth component, after which model improvement decreases. Bottom: BIC scores relative to the lowest score in the grid. The local minima at L2N5 and L5N5 are the two fits presented in Coulombe et al. (2023) that are equally probable when considering the BIC alone.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: Two example sets of eigencurves and eigenmaps for ﹩{l}_{\max }=2﹩ (left) and ﹩{l}_{\max }=5﹩ (right) for the JWST NIRISS/SOSS observation in Coulombe et al. (2023). We show the top eight highest-variance eigencurves ranked from top to bottom by decreasing variance. The flux units on the eigencurves and eigenmaps are arbitrary, as they are scaled by the fitted parameters when modeling data.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: Comparison between models with N and N − 1 model components with constant ﹩{l}_{\max }﹩, normalized by standard error. A model is favored over the previous model if the addition of the new parameter increases elpd N  and increases by more than 1 SE are significant (i.e., the y-axis is >1, above the dotted line). Generally, the addition of the second, third, and fifth eigencurves are easily justified. However, the fourth eigencurve often results in a decrease in the predictive performance of the model.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: Posterior distribution of parameter c 5, the weight of the fifth eigencurve E 5, in models with and without the fourth eigencurve E 4 for ﹩{l}_{\max }=5﹩. The best-fit value of c 5 (vertical lines) changes depending on whether E 4 is in the model. While E 4 does not significantly improve the fit on its own, its presence allows for further flexibility in the value of c 5 within the positive-flux constraint, which does make a significant improvement to the fit.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: The total ﹩{\mathrm{elpd}}_{\mathrm{LOO},{ \mathcal M }}﹩ over each region for one to eight eigencurves (one to three for ﹩{l}_{\max }=1﹩ as there are only three first-degree harmonics). Increases from left to right indicate that adding a given component to the model improves the model’s out-of-sample predictive power in that region and vice versa. Because adding eigencurves to the model does not affect the model during total eclipse (planet flux is zero), the change in model predictive power in that region is negligible and thus, is not shown here.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: A comparison of models with model complexity increasing from top to bottom. The left column shows the entire data set, the middle column shows the eclipse ingress, and the right column shows the eclipse egress. Δelpd i  is the difference in out-of-sample predictive power of the model with larger N and the model with smaller N. That is, positive values show where the additional parameters provides increased predictive performance, and vice versa. For visibility, the color bars are on different scales.
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: A comparison of elpd i  between the two competing map models for WASP-18b, L5N5, and L2N5. The differences between the models are most significant in ingress (left) and egress (right). The insets show the flux map models (see Figure 2) in the same colors as their corresponding light-curve models. The L5N5 model is primarily preferred by data in the first half of ingress (red data points), while the L2N5 model is primarily preferred by data in the second half of egress (blue data points).
Paper: Bringing 2D Eclipse Mapping out of the Shadows with Leave-one-out Cross Validation
Authors: Ryan C. Challener, Luis Welbanks, Peter McGill
Figure caption: The two competing brightness map models of WASP-18b: L2N5 (top) and L5N5 (bottom). The L2N5 model has a peaked hot spot with a latitudinal offset, and the L5N5 model has a broader hot spot close to the equator. The longitudes have been restricted to those visible during the observation. Note that the uncertainties in the maps at longitudes on the nightside and high latitudes are significant as these regions contribute minimal flux to the observed light curve.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Isochrones overlaid with the 5σ constraints from the Keck-NIRC2 survey. The horizontal lines represent our imaging survey's 5σ sensitivity at 1 and 4 au of separation. (a) We use the BHAC15/DUSTY/COND models (Chabrier et al. 2000; Baraffe et al. 2003, 2015) to rule out all tight stellar and brown dwarf companions (>13 M Jup) outside of 0.25 au (0.″1). (b) From 1 to 4.18 au of separation, we apply the Linder et al. (2019) low-mass planetary cooling models to place upper mass limits on planetary companions. We rule out planets with masses >1.5 M Jup to 5σ if Wolf 359 is younger than 500 Myr in this region.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Final reduced image of the Wolf 359 system from the Keck-NIRC2 HCI survey. Our final reduced image of the Wolf 359 system was created using the high-pass-filtered 3 night combined image cube. The corresponding S/N map is shown in panel (b). The red circle shown in panel (a) corresponds to the predicted semimajor axis of the Wolf 359 b candidate. The stellar PSF was subtracted using full-frame PCA with VIP. No companion-like point sources were detected to more than 2σ above the background using VIP's built-in detection function.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Keck-NIRC2 HCI survey completeness. (a) The NIRC2 combined-nights 5σ contrast was converted to mass space using the Linder+2019 and Ames-COND isochrone models. (b)–(d) The NIRC2 survey completeness maps for ages of 100 Myr, 500 Myr, and 1 Gyr were estimated using the Exo-DMC python package from the mass-space combined-nights 5σ contrast curves. Our imaging survey has 10% coverage to companions with a semimajor axis of 0.2–10 au and reaches 95% coverage for companions with a semimajor axis between 1 and 3 au. The black star represents the Wolf 359 b semimajor axis and minimum mass as predicted by Tuomi et al. (2019).
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Kinematic age dating. Wolf 359's kinematic age was measured using the methods outlined in Kiman et al. (2019). The results of the Monte Carlo simulation shown here find the kinematic age to be 1.53 ± 0.3 Gyr. We adopt this kinematic age as our age upper bound for Wolf 359.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: CMD comparison with young moving groups. We plot the CMD for Wolf 359 with empirical sequences from young associations of ages 10, 24, 112, 562, and 750 Myr (Gagné et al. 2021) and the Gaia 100 pc sample of M dwarfs. The red star represents the position of Wolf 359. The color–magnitude position of Wolf 359 is not in agreement with the youngest moving groups of 10–112 Myr. We find that Wolf 359 is in better agreement with the Coma Berenices (562 Myr) and Hyades (750 Myr) moving groups and the field sample. We conclude that Wolf 359 has converged onto the main sequence and that its age is older than 112 Myr.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Isochrone age dating. We used the MIST isochrone models with the Gaia eDR3 photometry in G and BP to estimate an age for Wolf 359. The blue line represents the MIST isochrone track for a star of 0.11 M ⊙ with a metallicity of [Fe/H] = +0.25 dex. Wolf 359 is represented by the red star, which lies closest to the isochrone point with an age of 393 Myr (between 373 and 414 Myr). We estimate an age of 400 Myr from isochrone dating.
Paper: A Wolf 359 in Sheep's Clothing: Hunting for Substellar Companions in the Fifth-closest System Using Combined High-contrast Imaging and Radial Velocity Analysis
Authors: Rachel Bowens-Rubin, Joseph M. Akana Murphy, Philip M. Hinz, Mary Anne Limbach, Andreas Seifahrt, Rocio Kiman, Maïssa Salama, Sagnick Mukherjee, Madison Brady, Aarynn L. Carter, Rebecca Jensen-Clem, Maaike A. M. van Kooten, Howard Isaacson, Molly Kosiarek, Jacob L. Bean, David Kasper, Rafael Luque, Gudmundur Stefánsson, Julian Stürmer
Figure caption: Contrast curves from the Keck-NIRC2 imaging survey. The contrast curves were created using the full-frame PCA algorithm in VIP with the images that were not high-pass filtered. The solid black line represents the 5σ sensitivity achieved with the combined-nights cube.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Residuals of our HST–2MASS filter transformations with respect to the J − K  S  color for our fitting sample (773 spectra of 648 unique stars). Color maps show relevant stellar parameters where available, including effective temperature T eff, metallicity [Fe/H], surface gravity log(g), and reddening E(B − V). Reddenings are as described in Section 2.2.2; all other parameters are adopted as is from the literature sources.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Synthetic 2MASS CMD (left) and filter transformation residuals (center, right) with several subtypes of evolved stars used as primary distance indicators highlighted by color. These include C- and O-rich TP-AGB variables in blue and orange respectively; first-ascent RGB stars in green; RR Lyrae variables in red; and classical Cepheids in pink. Repeat observations of the same stars are connected with solid lines.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: As Figure 10 with respect to the J − H color on the x-axis.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: As Figure 10, but showing the residuals for stars excluded from our fitting sample (424 spectra of 643 unique stars). Note the changes in both the x- and y-axis ranges relative to Figures 10 and 11.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Pair plots of E(B − V) measurements for stars common to the different extinction catalogs. Stars with high-quality measurements in both E(B − V) maps per pair are shown by blue points, and stars with data quality flags in one or both maps are shown in light gray. Summary data for individual tables are given in Table 7, and the MADs of pairwise differences in Table 8.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: As Figure 12, with J − H color on the x-axis. Again, note the differences in the x- and y-axis ranges between this and previous figures.
Paper: Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry
Authors: M. J. Durbin, R. L. Beaton, A. J. Monson, B. Swidler, J. J. Dalcanton
Figure caption: Comparisons to previously published transformations for F125W – J (Riess 2011; upper panel) and F160W – H (lower panel; Riess 2011 in blue; Dalcanton et al. 2012 in orange). Results of this work are shown in gray.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: (Left) JWST color composite prepared by Joseph DePasquale (STScI), Anton M. Koekemoer (STScI), Alyssa Pagan (STScI). Colors are as follows: Purple: F090W, Blue: F187N, Cyan: F200W, Yellow: F335M, Orange: F444W, and Red: F470N. The image was obtained from https://webbtelescope.org/contents/media/images/2022/052/01GF423GBQSK6ANC89NTFJW8VM. (Center) Three-color composite using JWST filters F090W (blue), F187N (green), and F335M (red). The stretches are nonlinear and limits have been adjusted. The 3.3μm band, in red, includes a polycyclic aromatic hydrocarbon (PAH) feature and therefore indicates far-UV illumination. Section 2.4 includes a more detailed summary of the significance of these filters. (Right) Schematic diagram of the Pillars on the sky at the same angular scale as the two images to the left. Features are marked with labels that will be used throughout the paper. P1a refers to the northern half of Pillar 1, including the Cap and Eastern and Western Threads. P1b refers to the southern half and includes the Eastern and Western Horns and part of the Shared Base. The dashed line to the south marks a boundary that is kinematically discontinuous with the Ridge despite its apparent continuity in the visible and IR images; this is discussed in Section 3.6. The three images are nearly R.A.-decl. aligned; “up” in the image is 2.°3 east of north. The scale bar in the top-left corner shows ﹩1^{\prime} \approx 0.5﹩ pc at 1740pc line of sight.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Integrated [C II] (black) and CS (white) line intensities between V LSR = 19 and 27 km s−1 overlaid on the F335M image. [C II] integrated intensities are marked at the [25, 50, 75, 100, 125, 150, 175, 200, 225] K km s−1 levels, and CS at [0.8, 3.2, 5.6, 8, 10.4, 12.8, 15.2, 17.6, 20, 22.4, 24.8] K km s−1. The dotted white line marks the 50% gain contour for the CS observations; see the caption of Figure 2 for more detail. The [C II] beam is shown in gray in the lower-right corner, and the CS beam superimposed in white. Note the spatial offsets between the two lines toward the Cap and the Threads, among other locations. The large-scale [C II] emission indicated by the lowest two contours is the V LSR ∼ 25  km s−1 background discussed in detail in Appendix B.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Integrated intensity and photometry centered on the Pillars. Contoured observations are marked with (c). The beam for each observation is shown in the lower-right corner; the beam for the contoured observation, if present, is shown to the left of the color-scale observation’s beam. All observations are shown at the same angular scale. [C II] and [O I] are integrated between V LSR = 18 and 27 km s−1, as they tend to have longer blue wings, and molecular lines not otherwise specified are integrated between V LSR = 19 and 27 km s−1. N2H+ and HCN are integrated between V LSR = 12.6 and 32 km s−1 with respect to the rest frequencies given in Table 1 in order to include several satellite lines for each species (see Section 2). Contours are [0.5, 3.0] K km s−1 for C18O(J = 1-0); [4, 24, 44] K km s−1 for 13CO(J = 3-2); and [9, 18, 27, 45] ×105 MJy sr−1 for the 160 μm image (the last contour spacing is intentionally uneven to increase visibility toward P1a). The contour colors are chosen to increase contrast with the image and have no further significance. The dashed white contour on the interferometric molecular line observations marks 50% gain from the primary beam mosaic pattern; outside this contour the sensitivity falls off (noise increases). Note the BIMA CO(J = 1-0) maps are smaller than the CARMA maps of the other species and so cover the southeast Ridge with very low sensitivity. Nonetheless it is weakly detected.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: (Left) Color composite using [C II] line integrated intensities between V LSR = 19–21.5 km s−1 (blue), 22–23.5 km s−1 (green), and 24–27.5 km s−1 (red). The color stretches are linear and start at 0 but have different upper limits. (Right) NOAO optical composite prepared by T.A. Rector (NRAO/AUI/NSF and NOIRLab/NSF/AURA) and B.A. Wolpa (NOIRLab/NSF/AURA) using observations from the WIYN 0.9 m telescope at the Kitt Peak National Observatory. The image was obtained from https://noirlab.edu/public/images/noao-04086 and coordinate metadata applied using Astrometry.net a  (Lang et al. 2010). The colors show the O III line at 499~nm (blue), the Hα line at 656~nm (green), and the S II line at 672~nm (red).  a  https://astrometry.net
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Same layout as in Figure 8, but with PV diagrams along different paths. The first path runs across the Cap and shows its peak velocity gradient. The second path crosses the two Threads and shows the differences in [C II] and CO velocity structure. The third path crosses the head of P2 and shows the spatial and kinematic offset of the [C II] peak with respect to CO as well as the velocity gradient across the head in both lines. Velocities are V LSR.
Paper: SOFIA FEEDBACK Survey: The Pillars of Creation in [C II] and Molecular Lines
Authors: Ramsey L. Karim, Marc W. Pound, Alexander G. G. M. Tielens, Maitraiyee Tiwari, Lars Bonne, Mark G. Wolfire, Nicola Schneider, Ümit Kavak, Lee G. Mundy, Robert Simon, Rolf Güsten, Jürgen Stutzki, Friedrich Wyrowski, Netty Honingh
Figure caption: Position–velocity (PV) diagram along each pillar using the [C II] and 12CO(J = 1-0) line observations. The left panel shows the F335N image with the three paths overlaid. The paths are numbered and the labels are placed at the beginning of the path. The next three panels show, from left to right, the PV diagrams of P1, P2, and P3 along the numbered paths. In each PV diagram, the grayscale image is the CO PV diagram at the native CO spatial resolution, while the contours show both CO and [C II] at the [C II] resolution. Contour labels are main beam temperatures T MB in degrees kelvin. Emission at V LSR ≳ 27  km s−1 is from background features not directly related to the Pillars. Velocities are V LSR.