adsabs/AstroCLIMB huggingface dataset:
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Surface density structure of the gas and dust model in DALI used to simulate the DM Tau transition disk. The dashed lines show the truncated power-law profile for the gas and dust with no depletion.
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Spectral energy distribution for DM Tau; red circles are photometric measurements, black dots are Spitzer IRS spectra. Top panel: overall SED. Bottom panel: zoom in on the near-to-mid infrared portion.
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: A set of DEM models and diagnostic plots. For all of the plots, red lines and symbols represent the DEM models, while black lines and symbols represent the HST/COS data presented in this paper. Panel (A) shows the DEM models of the COS FUV emission lines of AU Mic in quiescence. The average DEM model is shown in the thick line, with individually measured DEM values. The thin lines represent 50 random draws from the models fit with emcee. Panel (B) shows the integrated flux in bins of 10Å from the DEM output (red) spectra compared to the HST/COS data (black). The Lyα line is masked in these bins. The unbinned spectrum is plotted as the pink line with shaded 1σ errors. In panel (C), we show a comparison of line fluxes from XMM-Newton observations of AU Mic to the DEM modeled spectra. In panel (D), we show a comparison of line fluxes from EUVE observations (Del Zanna et al. 2002) of AU Mic to the DEM modeled spectra. These data are for Fe IX–Fe XXIV. Panel (E) shows a comparison of line fluxes from the presented HST/COS observations to line fluxes. The solid lines in panels (C), (D), and (E) represent a one-to-one relationship in the flux. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/dem_figure.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: A panchromatic spectrum for AU Mic in its quiescent state. The spectra comprise archival observations of AU Mic with XMM-Newton (10–39 Å), FUSE (900–1181 Å), HST/COS (this work; 1064–1372 Å), IUE (2000–3347 Å), and HARPS-N (3789–6912 Å). To fill in gaps in data coverage, we utilize a DEM synthetic spectrum (40–900 Å), a linear interpolation (1372–2000 Å and 3334–3782 Å), and a PHOENIX synthetic generated stellar atmospheric model (6912–2 × 105 Å). For Lyα (1211–1220 Å), we use the reconstructed profile from Flagg et al. (2022). We present Spitzer 24 and 70 μm color-corrected detections of AU Mic (white points) for completeness (Plavchan et al. 2009). We do not correct the PHOENIX spectrum for the infrared excess from the debris disk. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/panchromatic_spectrum.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Flux-calibrated light curves from two HST/COS visits to AU Mic across the entire wavelength coverage (1064–1361 Å). Time of peak flare events are marked with vertical orange lines. Highlighted yellow regions are excised for the creation of a clean out-of-flare template spectrum. A total of 13 flares were identified, with one double-peaked flare identified in the third orbit of Visit 1 (Flare B) and five flares present in the last orbit of Visit 2 (Flares H-L). We present the parameters for each flare in Table 1.
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Top: a comparison of time offsets for the primary (circles) and secondary (triangles) flare peaks with respect to the peak in the “white light” for the complex Flare B as a function of formation temperature. We plot the zero-point as a horizontal dashed line and note the time offset of the secondary peak in the “white light” as a dotted black line. We set the zero-points for the primary and secondary peaks as t  p  = 12531 s and t  s  = 12651 s, with respect to the visit start time (MJD = 59362.148). We do not see the secondary peak in N V and Fe XXI. Bottom: a comparison of the measured energies for each flare from the spectroscopic light curves (E SLC) compared to the measured white-light energy (E WLC). All flares have the strongest measured energy in C III (﹩{{\rm{log}}}_{10}({T}_{\mathrm{form}}[﹩ K ]) = 4.8). Flare B has the highest E SLC/E WLC in C III, likely due to the increased prominence of the second flare at this wavelength (see Figure 2).
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: The continuum of the mean spectrum for the quiescent state (gray points) and Flares B, D, J, K, and M (black points per each subpanel). The continuum was visually identified by inspecting regions of the spectrum lacking emission features. For the purposes of this calculation, the spectrum is subdivided into 1Å bins. We fit an additional thermal bremsstrahlung profile (colored lines) to the continuum of the flare data, as there is an obvious rise at λ ≤ 1100 Å. The resulting best-fit temperature for the thermal bremsstrahlung profile is presented in each subpanel. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/blackbody_fits.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: A comparison of line profiles in quiescence compared to Flares B, D, J, K, and M (left to right). The best-fit quiescent line profile is plotted in orange; the best-fit in-flare line profile is plotted in black, with the data plotted in color. All line profiles were fit with a multi-Gaussian model, where the exact number of Gaussians in each model is presented in Table 2. We find that for Flares B, J, K, and M, each ion exhibits a bulk flux increase. Flare D poses the only exception to this, where there is little change in the profiles of C II, N V, and Fe XXI. In Si III, Flares B, J, K, and M all show a bulk increase in the blue side of the line center. In N V doublet, Flares B, J, K, and M all exhibit additional flux in the peak and red wing of both the blue and red components. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/line_analysis.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: Comparison of line flux during Flare B (see Figure 1) and in quiescence (F Q ) for all lines identified in the AU Mic spectrum. Points are colored by line flux in quiescence. The values and error bars are presented in Table A1. There is an overall increase in flux for all identified lines during Flare B as compared to the quiescent state. The blue and yellow lines represent no change and a doubling of flux values. (https://github.com/afeinstein20/cos_flares/blob/paper-version/notebooks/big_table.ipynb)
Paper: AU Microscopii in the Far-UV: Observations in Quiescence, during Flares, and Implications for AU Mic b and c
Authors: Adina D. Feinstein, Kevin France, Allison Youngblood, Girish M. Duvvuri, D. J. Teal, P. Wilson Cauley, Darryl Z. Seligman, Eric Gaidos, Eliza M.-R. Kempton, Jacob L. Bean, Hannah Diamond-Lowe, Elisabeth Newton, Sivan Ginzburg, Peter Plavchan, Peter Gao, Hilke Schlichting
Figure caption: A comparison of flares seen in emission lines that originate from different formation temperatures (provided in Table 2), moving from coolest to hottest emission line from left to right. The best-fit model for each flare is over-plotted as a solid line. The first and second rows are light curves for Flares B and D. The third row shows light curves for Flares J, K, and M (teal, green, and yellow). We were unable to properly model Flares D, J, K, and M in Fe XXI due to a lack of obvious flare shape.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption:  Upper panel: Global SFR vs. M * for the MaNDala (circles) and whole MaNGA (isodensity contours) samples. The SFRs were calculated from the H α line integrated within the FoV of each galaxy using the Chabrier IMF (see text). The stellar masses are from the NSA catalog. No correction for volume completeness was applied. Lower panel: Same as in the upper panel but for the specific SFR. The shaded area is the 1σ region describing the SF main sequence inferred from several observational data at z ∼ 0.1 by Rodríguez-Puebla et al. (2020a).
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Relationship between the look-back times at which 50% and 80% of the stellar masses of the MaNDala galaxies were formed. The colors of the symbols represent the mass-weighted ages, Agemw. The half-mass look-back time correlates well with Agemw. Circles, squares, and triangles correspond to SFg, T, and P galaxies. The diagonal thin dashed lines indicate differences between the 50% and 80% look-back times of 2, 4, 6, and 8 Gyr.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Bar strength plotted against the FUV+WISE/NSA-derived sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The data points are color coded based on concentration (red: C ≥ 4.5; yellow: 4.0 ≤ C < 4.5; green: 3.5 ≤ C < 4.0; blue: C < 3.5).
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Normal probability plots of normalized coordinate differences UBSC(J2016) − EDR3 χ  α* (left) and χ  δ  (right). The diagonal straight line represents the scaling CDF of the fitted normal distribution for the bin_flag = 0 sample.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Probability plots of normalized parallax differences UBSC − EDR3 ﹩({\varpi }_{h}-{\varpi }_{g})/\sqrt{{\sigma }_{{\varpi }_{h}}^{2}+{\sigma }_{{\varpi }_{g}}^{2}}﹩. The diagonal straight line represents the scaling CDF of the fitted                       ﹩{ \mathcal N }(0.304,1.339)﹩ distribution for the bin_flag = 0 sample.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Formal errors of proper motion R.A. components vs. Hp magnitude. Source 2 (URSOL) solutions are marked with black circles, sources 1 and 3 (UBSOL and mixed UBSOL+URSOL) with brown circles.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Histograms of χ 2 proper motion vector differences UBSC(J2016) − EDR3.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Probability plots of normalized proper motion vector differences UBSC(J2016) − EDR3 ﹩{\chi }_{{\boldsymbol{\mu }}}^{2}﹩. The diagonal straight line represents the scaling CDF of the expected χ 2(2) distribution for each sample.
Paper: USNO Bright Star Catalog, Version 1
Authors: Norbert Zacharias, Valeri V. Makarov, Charles T. Finch, Hugh C. Harris, Jeffrey A. Munn, John P. Subasavage
Figure caption: Probability plots of normalized position vector differences UBSC(J2016) − EDR3 χ 2. The diagonal straight line represents the scaling CDF of the expected χ 2(2) distribution for each sample.
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 WFC3 transmission spectrum of GJ 1132b, averaged over the five visits of WFC3, plotted against cloud-free atmospheric models of varying metallicities for comparison. For each model, we provided the ﹩{\chi }_{r}^{2}﹩ and the p-value evidence against the model. We translated the p-value to the number of σ (nσ) confidence that we can reject this model. The spectrum is most consistent with a flat line, indicating a high mean molecular weight atmosphere or no atmosphere. We could easily detect an atmosphere with a metallicity less than 300× solar by volume (or mean molecular weights less than 8.9 amu).
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 comparison between the average transit depths in Swain et al. (2021) (blue/triangle points), in Mugnai et al. (2021) (orange/square points), and in this work (black/circle points). All utilize the same HST/WFC3 data, though Swain et al. (2021) determine very different transit depths, most notably at shorter wavelengths. Transit depths derived in this work and in Mugnai et al. (2021) are statistically the same, with similar uncertainties as well.
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: Same as Figure 12, except with 100% molecular composition atmospheric models for comparison. We are unable to rule out any of these atmospheric models, as their higher mean molecular weights produce transit depth variations smaller than the precision of the data points.
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: Searching for TTVs in the mid-transit times of GJ 1132b yielded scatter around a flat line. Points are color-coded by telescope, and the HST uncertainties are inflated 10.7× such that the ﹩{\chi }_{r}^{2}﹩ of those five points is equal to unity.
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: TESS folded light curve of GJ 1132b’s transit. Top panel includes the detrended light curve points (gray), binned points for clarity (blue), and the best-fit model in light blue. Bottom panel shows the residuals from this fit.
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 comparison of the transit depths from each visit in their respective wavelength bins. The weighted-mean transit depths between the five visits are included in black. All bins demonstrated <2σ spread, except for wavelengths 1.25 and 1.40 μm. Removing the outlying visits in these bins had no appreciable effect on the final spectrum.
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 TESS Sectors 9 and 36 light curve of GJ 1132, folded assuming the best-fit period (8.922 ± 0.009 days) from our TESS analysis of GJ 1132c, with the best-fit maximum-likelihood model plotted in light blue as a straight line. We find no significant evidence that GJ 1132c transits.
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 comparison between the WFC3 transit depths (black points) and the spectroscopic (dark blue) and broadband (light blue) transit depths from Diamond-Lowe et al. (2018). While the spectroscopic depths appear smaller than the WFC3 values, the broadband depth is statistically the same.
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 transit depth comparison between the RECTE (teal/square) and divide-white (purple/circle) methods for each wavelength bin. Overall, transit depths vary less than 2σ for each bin (except for the second bin) with an average discrepancy of less than 1σ.
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: Map of the Molecular Ridge colored by each structure’s α vir parameter. For this map we used structures found with quickclump to minimize structure overlap. Where there is overlap along the line of sight, we show the average α vir. The small blue circles indicate YSOs from infrared surveys (Whitney et al. 2008; Gruendl & Chu 2009; Seale et al. 2014), and the large green circles indicate H II regions and their sizes from Henize (1956). The black lines show the boundaries used to split the Ridge into four different regions to analyze, and the dashed lines show the observation footprint.
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: Distribution of surface densities in the Ridge and 30 Dor. The Ridge has significantly lower surface densities than 30 Dor, which results in structures in the Ridge having higher α vir values despite their lower kinetic energies. Also shown is the A  V  > 8 mag threshold for massive-star formation from Lada et al. (2010), converted to Σgas > 490 M ⊙ pc−2. This indicates that the Ridge is likely not forming massive stars because it lacks dense gas.