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: Comparison of selected 2D output variables for the DALI fiducial model (left column) and the same DALI model with no inner dust disk within 30 au (right column), as described in Section 5.2.1. First row: dust temperature; second row: gas temperature; third row CO gas abundance; fourth row: UV flux in ISM units. Bottom row: Comparison of the gas temperature at the τ = 1 surface for the 12CO, 13CO, and C18O lines; the blue shaded region indicates the CO freeze-out temperature range. The τ = 1 surface for the 12CO, 13CO, and C18O is overlaid as solid, dashed, and dotted lines, respectively.
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: Same as Figure 21, but for the comparison of different values of δ dust2 within 5 au, as described in Section 5.2.2. First row: dust temperature; second row: UV flux in ISM units.
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: Midplane (z = 0) temperature (top panel) and abundance of various volatile species locked into ices (bottom panel) in the fiducial DM Tau model within 10 au. X/H+H2 denotes the ratio of the number densities of ice X and the total gas density. Note: the gas and dust temperature at the midplane are essentially identical in this region of the disk.
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: Same as Figure 9, but for the effects of changing the global PAH abundance with respect to the ISM in the DALI model described in Section 5.2.6.
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: Same as Figure 9, but for the effects of changing the stellar accretion rate in the DALI model described in Section 5.2.5.
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: Same as Figure 9, but for the effects of changing the disk scale height angle at the critical radius h  c  in the DALI model described in Section 5.2.4.
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: Comparison of the gas surface density for the input DALI models with varying enhancements in the inner disk with the gas surface density estimated from accretion rate with different alpha values.
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: Observed (left column), fiducial DALI model (center column), and residual (right column) deprojected images for the 1.3 mm dust continuum (first row) and 12CO, 13CO, and C18O moment 0 maps (second to fourth rows). The beam for each image is shown in the bottom left of each panel as a white ellipse.
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: The same fiducial DALI model as Figure 6, but showing the full model grid from from 0 to 500 au.
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: Left panels: from the uppermost to the bottom, the individual surface brightness profiles for all the MaNDala galaxies, in the g, r, and z bands, respectively. On top of them, an average profile is shown, calculated in radial bins of 0.4 R  e . The dashed lines represent the mean depth limit values for the galaxies in the sample for each band, while 1σ of those values are shown by the shaded areas around them. Right panels: on the top are shown the same surface brightness profiles for all the MaNDala galaxies in the r band, as in the right panel, with their depth limits shown as dashed lines, but color-coded in terms of morphology (blue for late types and red for early types). In the bottom panels, the g − r profiles for each MaNDala galaxy are shown, with the same color code as in the top panels. On top of both panels, the median profiles for early- and late-type galaxies are plotted in magenta and dark blue, respectively, with error bars representing the 16th and 84th percentiles. The surface brightness and color profiles shown in this figure are cut according the individual depth limit for each galaxy.
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: Example of the radial profiles derived from the photometric analysis for the MaNGA-8145-3702 galaxy. Top panel, from left to right: ellipticity (ϵ) measured in the r band, surface brightness profiles for the z, r, and g bands (in yellow, red, and black, respectively) and the cumulative flux in the r band, along with three estimates of the R  e , from an interpolation of this curve, from the same interpolation but deconvolving with the PSF, and from the Sérsic fit in the r band. Bottom panels, from left to right: P.A. measured in the r band, the g − z and g − r color profiles (in blue and magenta, respectively), and Sérsic fits to the surface brightness profiles for the three bands, displayed in the same color code as the top middle panel.
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: filled green bars show the histogram of the two morphological types for the 121 MaNDala galaxies with central/satellite information available in the GEMA Catalog. Empty bars show the histograms for the same morphological types, but only for central and satellite galaxies, in solid and dashed lines, respectively. Lower panel: filled green bars show the histogram of the two morphological types for the 135 MaNDala galaxies with information from Geha et al. (2012) on the distance, D host, to the nearest luminous galaxy. Solid and dashed line bars show the histograms for field (D  host  > 1 Mpc, relatively isolated) galaxies and those in more dense environments (D  host  ≤ 1 Mpc).
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: histogram representing the luminosity distance distribution of the 136 galaxies that comprise the current version of the MaNDala sample. Lower panel: relation between the redshift and M * for the galaxies in our sample, along with the distribution of M *. Redshifts and M * are retrieved from the NSA Catalog.
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: Comparisons of the principal results from our Sérsic fit against those previously presented in the NSA Catalog. From the top to the bottom panels, we show the following comparisons: Sérsic index and effective radius in the r band, and apparent magnitudes in the g, r, and z bands. The red line shows the one-to-one relation. In all panels, the Pearson correlation coefficient is shown.
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: Mosaic displaying the images derived from the photometric analysis for the galaxy MaNGA-8145-3702. Upper panels: r-band DESI image (left) and g − z 2D color map (right). Lower panels: g-band DESI image with a Gaussian filter (left) and RGB DESI image. The hexagon in the RGB image represents the MaNGA field of view.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Top panel: Histograms of Hubble types for the galaxies in the Yu & Ho (2020) sample with z < 0.03. Red histogram: all galaxies. Hatched black histogram: unbarred galaxies. Cyan histogram: galaxies with measured pitch angles. Dotted blue histogram: galaxies with log M* ≥ 10. Bottom panel: Concentration vs. Hubble Type. Individual galaxies are plotted as red dots. The blue filled diamonds give the median value for each Hubble type. The blue error bars represent the range from the first quartile to the third quartile.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of redshifts for each set of galaxies. Top panel: field galaxies. Second panel: galaxies in massive clusters. Third panel: galaxies in moderate clusters. Bottom panel: Galaxies in groups. Red histograms: all galaxies. Hatched black histograms: unbarred galaxies. Dotted blue lines: galaxies with stellar mass ≥1010 M ☉. Histograms in cyan: galaxies with pitch angle measurements.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of the number of Yu & Ho (2020) z < 0.03 galaxies as a function of pitch angle, for galaxies identified by Galaxy Zoo as having arms that are “tightly wound” (top panel), “medium wound” (second panel), and “loosely wound” (third panel). The black histograms in the top three panels are based on vote fractions uncorrected for classification bias, and include only “securely identified” spirals with at least 20 Galaxy Zoo classifications, and only include galaxies for which at least half of the participants agreed on the winding class. The blue dotted histograms include only galaxies flagged by Hart et al. (2016) as having a bias-corrected vote fraction greater than 80%. The bottom panel gives the distribution of ϕ for galaxies not considered “secure spirals” in Galaxy Zoo. The black filled diamonds and blue open triangles give the median ϕ value for the black and blue histograms, respectively, with the error bars marking the range from the first quartile to the third quartile. The red circle with error bars illustrates the median measurement uncertainty on ϕ.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The sSFR from the GSWLC-2 vs. the sSFR from the NSA FUV fluxes combined with AllWISE 22 μm fluxes using the prescription from Hao et al. (2011). Field galaxies are displayed in the top panel, and galaxies in massive clusters in the bottom panel. In both plots, the blue dashed line is the one-to-one line, the green line is the best-fit for the field galaxies, and the red line is the best-fit for the cluster galaxies. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plots, along with the Spearman (ρ) and Pearson (r) correlation coefficients. 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: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: SFRs from FUV+22 μm vs. stellar mass from the NSA, for field galaxies (top panel) and galaxies in massive clusters (bottom panel). In both plots, the black dotted line is the star-forming main sequence as defined by Saintonge et al. (2016), while the upper and lower blue lines, respectively, are the Trussler et al. (2020) dividing lines between the blue cloud and green valley, and between the green valley and red sequence galaxies. The galaxies are color coded into the blue cloud, green valley, and red sequence galaxies according to their color, based on the alternative classification scheme of Boselli et al. (2014), which relies upon location in the NUV—i vs. M* plane.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Histograms of the number of Yu & Ho (2020) z < 0.03 galaxies as a function of concentration. In the black histograms in the top four panels, only galaxies with p disk > 0.5 and at least 20 Galaxy Zoo classifications are included, and only galaxies for which at least half of the participants agreed on the bulge class. The blue dotted histograms include galaxies with bias-corrected vote fractions greater than 80% as tabulated by Hart et al. (2016). The bottom histogram gives the distribution of concentrations for galaxies with vote fractions of ≤0.5 for “features/disk.” Only galaxies with at least 20 classifications in Galaxy Zoo are included in these plots.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: GSWLC-2 SFR vs. stellar mass, for field galaxies (top panel) and galaxies in massive clusters (bottom panel). In both plots, the black dotted line is the star-forming main sequence as defined by Saintonge et al. (2016), while the upper and lower blue lines, respectively, are the Trussler et al. (2020) dividing lines between the blue cloud and green valley, and between the green valley and red sequence galaxies. The galaxies are color coded into the blue cloud, green valley, and red sequence galaxies according to their color, based on the alternative classification scheme of Boselli et al. (2014), which relies upon location in the NUV—i vs. M* plane.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: A comparison of the Galaxy Zoo bulge prominence parameter B avg (Masters et al. 2019; Lingard et al. 2021) and concentration, where B avg = 0.2 × p just noticeable + 0.8 × p obvious bulge + 1.0 × p dominant bulge. Here, p just noticeable, p obvious bulge, and p dominant bulge are the Galaxy Zoo vote fractions for a “just noticeable” bulge, an “obvious bulge,” and a “dominant bulge,” respectively. Only galaxies with at least 20 classifications in Galaxy Zoo are included. The slope (m), y-intercept (b), and rms are provided, along with the Spearman (ρ) and Pearson (r) correlation coefficients.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: Diagram illustrating the relationships between the various parameters discussed in this paper. We define correlations as relations with either the Pearson or Spearman correlation coefficient larger than 0.3, and an anticorrelation as one with either coefficient less than −0.3, limiting the sample to field galaxies with 10 ≤ log M* < 11.
Paper: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The log of the spiral arm strength vs. log sSFR for field galaxies (top panel) and galaxies in massive clusters (bottom panel). The sSFRs in these plots come from NSA FUV fluxes combined with AllWISE 22 μm fluxes, using the SFR prescription from Hao et al. (2011). In both plots, the green and red lines are the best fits for the field and cluster galaxies, respectively, with 10 ≤ log M* < 11. The slope (m), y-intercept (b), and rms of the best-fit lines are printed on the corresponding plot, along with the Spearman (ρ) and Pearson (r) correlation coefficients. 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: The Effect of Environment on Galaxy Spiral Arms, Bars, Concentration, and Quenching
Authors: Beverly J. Smith, Mark L. Giroux, Curtis Struck
Figure caption: The Galaxy Zoo “winding score” w avg = 0.5 × p medium + 1.0 × p tight, plotted against the pitch angle from Yu & Ho (2020). Here, p medium is the vote fraction for “medium wound,” and p tight is the vote fraction for “tightly wound”; a larger w avg means more tightly wound arms. The Spearman (ρ) and Pearson (r) correlation coefficients are provided. Only galaxies with at least 20 Galaxy Zoo classifications are included in this plot.
Paper: Zwicky Transient Facility and Globular Clusters: Calibration of the gr-band Absolute Magnitudes for the Yellow Post-asymptotic-giant-branch Stars
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Daniel Reiley, Russ R. Laher, Josiah Purdum, Ben Rusholme
Figure caption: Extinction-corrected CMD for M79 PAGB (magenta triangles), the three Type II Cepheids (blue squares), and other Type II Cepheids compiled in (Ngeow et al. 2022; cyan circles). The crosses marked the discarded yellow PAGB star, M19 ZNG4. The solid lines represent the mean absolute magnitudes as given in Equation (1), while the dashed lines are the fitted linear regressions given in Equation (2), extrapolated to redder colors. The dotted lines are the theoretical PAGB evolution track adopted from Moehler et al. (2019), with a metallicity of −2.3 dex and a zero-age horizontal-branch mass of 0.55 M ⊙, converted to the observed planes using the PARSEC Bolometric Correction online tool. Note that the track is used for illustration purpose and not for fitting the data. Error bars on the majority of the data points are smaller than the size of the symbols.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Comparison of 2MASS J0619-2903’s mid-IR variability compared to sources of comparable magnitude (±0.25 mag) and within 1°. Top: Reduced χ 2 values for each day-long visit compared to a model of constant flux. (Each object has ≈1 dozen visits.) The histogram shows that 2MASS J0619-2903’s variations are undistinguished, i.e., no significant evidence for variability. Bottom: Reduced χ 2 values for each object compared to a model where the weighted averages at each visit are consistent with constant flux. 2MASS J0619-2903 has the third and fourth highest ﹩{\tilde{\chi }}^{2}﹩ values, suggesting possible mid-IR variability. (For all plots, note that the number of exposures and/or visits is not the same for every object, so these histograms cannot be directly compared to a specific χ 2 distribution.)
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: NEOWISE mid-IR light curve of 2MASS J0619-2903 from 2014 March to 2020 September using single-exposure photometry, with the weighted average at each visit plotted as a large circle with short, wide-hatted error bars. The tall, small-hatted error bars show the rms photometric scatter at each visit. The intra-visit scatter on day-long timescales is consistent with constant flux given the measurement uncertainties, while the inter-visit scatter on 6 month timescales suggests possible ≈0.1 mag variability (Section 3.2.2).
Paper: Zwicky Transient Facility and Globular Clusters: Calibration of the gr-band Absolute Magnitudes for the Yellow Post-asymptotic-giant-branch Stars
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Daniel Reiley, Russ R. Laher, Josiah Purdum, Ben Rusholme
Figure caption: Similar to Figure 2, but with additional four yellow PAGB stars in the southern globular clusters (open circles, see text for details). Note that the dispersions of the photometric transformations as given in Tonry et al. (2012) dominate the errors on the (g − r) colors for these four southern yellow PAGB stars. V1 in ω Centauri (ω Cen) is a Type II Cepheid.
Paper: On the Unusual Variability of 2MASS J06195260–2903592: A Long-lived Disk around a Young Ultracool Dwarf
Authors: Michael C. Liu, Eugene A. Magnier, Zhoujian Zhang, Eric Gaidos, Trent J. Dupuy, Pengyu Liu, Beth A. Biller, Johanna M. Vos, Katelyn N. Allers, Jason T. Hinkle, Benjamin J. Shappee, Sage N. L. Constantinou, Mitchell T. Dennis, Kenji S. Emerson
Figure caption: Comparison of the AllWISE mid-IR photometry for 2MASS J0619-2903 with disk-bearing M dwarfs in the Upper Sco region (≈11 Myr) from Luhman & Mamajek (2012). The colors represent different evolutionary states of the circumstellar disks. The colors show that 2MASS J0619-2903 possesses either a full or evolved disk, which is unexpected given its ≈30 Myr age.
Paper: Zwicky Transient Facility and Globular Clusters: Calibration of the gr-band Absolute Magnitudes for the Yellow Post-asymptotic-giant-branch Stars
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Daniel Reiley, Russ R. Laher, Josiah Purdum, Ben Rusholme
Figure caption: ZTF gr-band light curves for M79 PAGB (top panel) and M19 ZNG4 (bottom panel), after excluding the data points with non-zero flags and infobits. The remaining numbers of data points are listed as N.