adsabs/AstroCLIMB huggingface dataset:
Paper: The Detectability of Rocky Planet Surface and Atmosphere Composition with the JWST: The Case of LHS 3844b
Authors: Emily A. Whittaker, Matej Malik, Jegug Ih, Eliza M.-R. Kempton, Megan Mansfield, Jacob L. Bean, Edwin S. Kite, Daniel D. B. Koll, Timothy W. Cronin, Renyu Hu
Figure caption: Nongray albedo vs. wavelength for each of the six tested surfaces as well as the gray control case with a constant 0.1 albedo (dashed). The nongray albedo extends over the wavelength range from 0.3 to 25 μm and thus captures the physically correct amount of reflected stellar light as well as thermal emissivity. The albedo data are from Hu et al. (2012).
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Examples of light curves from the OGLE-III survey. Eight different variability classes are shown in each row. In column 1 the original phase-folded light curves are shown; column 2 shows the resampled light curves, column 3 shows the phase-shifted light curve, and column 4 depicts the undersampling to t len = 300 observations.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The median Sérsic half-light radius (top panel) and index (bottom panel) of galaxies behind a fixed redshift, as a function of that redshift.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: Schematic illustration of the process used to calculate the fraction ﹩{{ \mathcal F }}_{9}﹩ of each galaxy’s flux that falls within a 3 × 3 pixel aperture on the focal plane.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The fraction ﹩{{ \mathcal F }}_{9}﹩ of a galaxy’s flux that falls within a 3 × 3 pixel aperture, as a function of cluster redshift for median Sersíc morphology.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The ratio of resolvable to detectable sources in the Mandelbaum et al. (2012) catalog as a function of redshift for each of SUPERBIT’s bands.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The number of sources with z > 0.3 that SUPERBIT can expect to detect if it was to observe the EL-COSMOS zone5 as a function of exposure time. The results are presented in all three relevant environments for each one of the bands presented in Figure 1.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: Median tangential shear profiles over 30 simulated observations of a 4.1 × 1014 Msol galaxy cluster at z = 0.45. Error bars represent the standard deviation of the mean tangential shear in a radial bin. The red line is the theoretical NFW shear input to all simulations. The variance is more than three times larger in S than B or L.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The ratio of the metric value for the B and S bands in the stratospheric environment as a function number of 300 s exposures with varying brightness cuts applied on the catalog. This figure demonstrates that the bias introduced into our result due to the increasing uncertainty in source redshift is negligible.
Paper: Weak Lensing in the Blue: A Counter-intuitive Strategy for Stratospheric Observations
Authors: Mohamed M. Shaaban, Ajay S. Gill, Jacqueline McCleary, Richard J. Massey, Steven J. Benton, Anthony M. Brown, Christopher J. Damaren, Tim Eifler, Aurelien A. Fraisse, Spencer Everett, Mathew N. Galloway, Michael Henderson, Bradley Holder, Eric M. Huff, Mathilde Jauzac, William C. Jones, David Lagattuta, Jason S.-Y. Leung, Lun Li, Thuy Vy T. Luu, Johanna M. Nagy, C. Barth Netterfield, Susan F. Redmond, Jason D. Rhodes, Andrew Robertson, Jürgen Schmoll, Ellen Sirks, Suresh Sivanandam
Figure caption: The value of the performance metric for each SUPERBIT band as a function of time, in all three relevant observing environments.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Neural network architecture of a conditional variational autoencoder. The left-hand side of the diagram represents the encoder (blue boxes), while the right-hand side represents the decoder (green boxes). Red boxes show the latent space. Each side, encoder and decoder, uses a sequential architecture (TCN or RNN) and a fully connected dense layer to map the outputs. Yellow boxes represent input data, such as light curves (LC), variability labels (l), and the corresponding physical parameters (η).
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Distributions of Gaia color (G BP − G RP, upper row) and absolute g-band magnitudes (M G, lower row) color-coded by variability classes. The left two panels show the confirmed cross-matches (sources with only one match within PM radius and with matching variability class), while the right panels show the sources validated by CMD comparisons (last group in Table 4).
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Joint distributions of physical parameters—period P, effective temperature T eff, and absolute g-band magnitude M  g —used during training of the generative model (see Section 4.2) color-coded by variability class.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Displays of reconstructed phase-folded light curves obtained at the decoder level by the best-performing model trained only with time series (cVAE). Three examples per variability class are shown. Gray markers denote the observed photometric OGLE-III I-band light curve, while in blue are the decoder reconstructions.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Generated light curves of RR Lyrae stars as effective temperature T eff increases (column direction). The three rows show the results from the three regression models: linear, random forest, and multilayer perceptron. The RF regressor, second row, shows a better representation along the temperature series for RR Lyrae variables, which agrees with its comparative RMSE performance.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Joint distributions of all μ (encoded features) values for the four dimensions of the latent space obtained by the best-performing model trained only with time-series data (cVAE). Color coding corresponds to the eight variability types.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Reconstructed light curves obtained at the decoder level by the best-performing network (cVAE-P) exploiting physical parameters as auxiliary inputs. Displays of three objects per variability class are shown. Gray markers denote the observed photometric OGLE-III I-band light curve, and in blue are the decoder reconstructions.
Paper: Deep Generative Modeling of Periodic Variable Stars Using Physical Parameters
Authors: Jorge Martínez-Palomera, Joshua S. Bloom, Ellianna S. Abrahams
Figure caption: Validation loss during training epochs for VAE models without physical parameters and GRU (blue) and TCN (yellow) architectures, while the red line shows a model with TCN layers that include physical parameters during training.
Paper: The 3D Galactocentric Velocities of Kepler Stars: Marginalizing Over Missing Radial Velocities
Authors: Ruth Angus, Adrian M. Price-Whelan, Joel C. Zinn, Megan Bedell, Yuxi (Lucy) Lu, Daniel Foreman-Mackey
Figure caption: Residual velocity distributions calculated by marginalizing over missing RV measurements (green) or by assuming the RV can be set to zero (purple) for 5000 stars in our sample. Each distribution shows the residuals between the inferred/calculated velocities, and the velocities calculated using full 6D information: parallaxes, positions, proper motions, and RVs. The vertical lines show the medians of each distribution. This figure demonstrates that calculating stellar velocities using proper motions and distances alone will significantly bias the results. Marginalizing over missing RV measurements ensures the resulting velocities will be unbiased.
Paper: The 3D Galactocentric Velocities of Kepler Stars: Marginalizing Over Missing Radial Velocities
Authors: Ruth Angus, Adrian M. Price-Whelan, Joel C. Zinn, Megan Bedell, Yuxi (Lucy) Lu, Daniel Foreman-Mackey
Figure caption: Velocities calculated with full 6D information compared with velocities inferred without RVs, for 5000 Kepler targets with RV measurements.
Paper: Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?
Authors: Howard E. Bond, Jessica Mink, Alison Doane, Sarah Lavallee
Figure caption: Color rendition of the field surrounding the site of V1148 Sgr, created using the PanSTARRS-1 Image Access tool. Frame is 55″ high, and has north at the top, east on the left. Red, green, and blue correspond to the y, i, and g filters, respectively. A small red cross marks the astrometric position of V1148 Sgr. The immediately adjacent star to the southwest, with i magnitude 19.18, is a candidate remnant, as discussed in the text.
Paper: Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?
Authors: Howard E. Bond, Jessica Mink, Alison Doane, Sarah Lavallee
Figure caption: Image cutouts from digital scans of four plates from the Harvard College Observatory’s Astronomical Photographic Glass Plate Collection, centered on the site of the transient V1148 Sgr. Each frame is 350″ high; north at the top, east on the left. Outskirts of the globular cluster NGC 6553 are visible at the northeast corners of the frames. First panel: 1935 June 4. V1148 Sgr is not detected to a g magnitude of ∼17.3. Second panel: 1943 August 24. The nova is near maximum brightness, at magnitude 9.55. Third panel: 1944 August 20. V1148 Sgr (between the two ink marks, and encircled in red) is detected at 16.7 mag. Fourth panel: postoutburst plate, taken on 1949 June 8. V1148 Sgr is fainter than g ≃ 18.3 mag.
Paper: Nova Sagittarii 1943 (V1148 Sgr): A Luminous Red Nova?
Authors: Howard E. Bond, Jessica Mink, Alison Doane, Sarah Lavallee
Figure caption: Images of the site of V1148 Sgr at the optical r band (from PanSTARRS-1) and at five near- and mid-infrared wavelengths (from the Spitzer Space Telesceope). Frames are centered on the position of the transient, have the same 55″ height as in Figure 2, and have north at the top, east on the left. No near- or mid-infrared counterpart of the nova is detected.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Instrumental (cyan filled triangles) and calibrated (black filled circles) magnitude differences between a reference UVIS2 (amps C and D) F606W image collected in 2009 for the Galactic globular cluster ω Cen and the subsequent 161 images. The instrumental magnitude differences were not corrected for time-sensitivity changes, while the calibrated magnitude differences were corrected by using the time-dependent inverse sensitivity values provided in the image header as the PHTFLAM2 keyword.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: The F814W, F275W − F814W (left), F814W, F438W − F814W (middle), and F814W, F555W − F814W (right) CMDs of the LMC globular cluster NGC 1978. A set of BaSTI isochrones with different ages and the same metallicity is overplotted. The assumed distance modulus and reddening are labeled in each panel.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Scan mode F814W UVIS2 (amp C) uncorrected (cyan filled triangles) and corrected (black filled circles) observed over synthetic count rate ratios for the standard star GD 153 (top) and GRW 70 (bottom) as a function of date. The scan observation count rates were corrected for sensitivity changes by using the time-dependent inverse sensitivity values provided in the image header as the PHTFLAM2 keyword.
Paper: New Photometric Calibration of the Wide Field Camera 3 Detectors
Authors: Annalisa Calamida, Varun Bajaj, Jennifer Mack, Mariarosa Marinelli, Jennifer Medina, Aidan Pidgeon, Vera Kozhurina-Platais, Clare Shanahan, Debopam Som
Figure caption: Staring mode F814W UVIS2 (amp C) uncorrected (cyan filled triangles) and corrected (black filled circles) observed over synthetic count rate ratios for the standard star GD 153 (top) and GRW 70 (bottom) as a function of date. The observed count rates were corrected for sensitivity changes by using the time-dependent inverse sensitivity values provided in the image header as the PHTFLAM2 keyword.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: A visualization of the posterior probability distribution for GJ 1132's starspot properties, including data used in the fit (left panels, with 20 random sample curves) and parameter samples (right panels, with 1000 random samples). Curves and points are colored from red to blue by T spot/T unspot, with paler colors closer to 1. Dashed lines highlight useful reference values in each parameter distribution. A fitted offset was applied to the LDSS3C depths, as explained in the text. The code used to generate this plot is available online (</>).
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: The 0.7–4.5 μm transmission spectrum of GJ 1132b, combining all available archival data sets with as-published transit depths. The same atmospheric models from Figure 12 are included for comparison. Goodness-of-fit values for each model were calculated using the LDSS3C spectrum, TESS, MEarth, and Spitzer photometry, and the WFC3 depths from this work. The noisy z-band flux point (Southworth et al. 2017) was cropped out to ease model visualization on the y-axis. From the ﹩{\chi }_{r}^{2}﹩ calculated with as-published depths, it appears that no planetary atmosphere model explains all transit depths; however, this is largely driven by the disagreement in the optical LDSS3C spectroscopic depths.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: MEarth out-of-transit light curve of GJ 1132, in the MEarth photometric bandpass (roughly 715–1000 nm), corrected for time-variable precipitable water vapor in Earth’s atmosphere. Nightly bins are shown with a color intensity inversely proportional to the nightly variance, for two MEarth telescopes (tel13 in blue, tel16 in orange). The epochs of the five WFC3 visits are marked with vertical lines.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: Definition of the variables used for modeling the impact of stellar surface inhomogeneities on the inferred transmission spectrum. In this framework, “spots” can represent patches that are either cooler or hotter than the surrounding stellar photosphere.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: Similar to Figure 14, but including the best-fit flat line offset of 205.7 ppm added to the Diamond-Lowe et al. (2018) spectroscopic transit depths for visualization. Best-fit statistics noted above the plot are calculated by applying the best-fit offset to the Diamond-Lowe et al. (2018) points for their respective models. The addition of archival data strongly supports a featureless transmission spectrum from 0.7 to 4.5 μm for GJ 1132b.
Paper: The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination
Authors: Jessica E. Libby-Roberts, Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M.-R. Kempton, Benjamin V. Rackham, David Charbonneau, Jean-Michel Désert, Jason A. Dittmann, Ryan Hofmann, Caroline V. Morley, Elisabeth R. Newton
Figure caption: Similar to Figure 15, including the best-fit 1× solar metallicity model offset of 15.9 ppm added to the Diamond-Lowe et al. (2018) spectroscopic transit depths for visualization.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: The LMC with the Molecular Ridge, 30 Dor, N159, and N113 highlighted in blue. The gray scale is PACS 250 μm from the HERITAGE survey (Meixner et al. 2013), and the red contours are 12CO (1–0) from the NANTEN survey (Fukui et al. 2008) showing the extent of all the CO-bright molecular gas in the LMC. Levels are 1.6, 5, and 12 K km s−1.
Paper: Structural and Dynamical Analysis of the Quiescent Molecular Ridge in the Large Magellanic Cloud
Authors: Molly K. Finn, Remy Indebetouw, Kelsey E. Johnson, Allison H. Costa, C.-H. Rosie Chen, Akiko Kawamura, Toshikazu Onishi, Jürgen Ott, Marta Sewiło, Kazuki Tokuda, Tony Wong, Sarolta Zahorecz
Figure caption: Left: integrated intensity map of the Molecular Ridge in 13CO (1–0). Contours show 1, 5, and 9 K km s−1. Right: integrated intensity map of the Molecular Ridge in CS (2–1), with the same contour lines from 13CO (1–0) overplotted. In both images, the beam is shown in the lower left corner.