adsabs/AstroCLIMB huggingface dataset:
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Weighted average number of catastrophic impacts N  c  (colored lines) a single target of radius R experiences with an impactor of radius r ≤ R for a range of different collision cases in Table 3. Each panel refers to a target body belonging to a particular TNO population. The dashed horizontal line corresponds to N  c  = 1. (Author note—In calculating the curves for all cases, the catastrophic disruption threshold of Benz & Asphaug (1999) was used. Using the disruption threshold formalism of Leinhardt & Stewart (2012) does not change the results, as they produce similar disruption threshold curves for a given material and impact speed; see previous figures.) For all cases, a uniform impact speed of v = 3 km s−1 and target bulk density of ρ = 500 kg m−3 were assumed.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Average radius r of the largest impactor that can collide with a target of radius R over a range of collision cases. All curves (colored solid lines) are weighted by the relative population estimate of each TNO impactor population. The radius of the largest impactor, by definition, is r ≤ R. The different panels denote targets belonging to different TNO populations. The dashed lines indicate the minimum radius r of an impactor required to catastrophically disrupt a target body of radius R based on the analysis of Benz & Asphaug (1999) and Leinhardt & Stewart (2012) for two different impact speeds of v = 0.5 and 3 km s−1. All four theoretical curves have been calculated for icy bodies with an assumed bulk density of ρ = 500 kg m−3.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Nominal case (current mass of the Kuiper Belt) for the radius r of the largest impactor belonging to a particular TNO population expected to impact a particular target of radius R (different subplots) over 4 Gyr. All of our modeled curves (colored solid lines) are estimated for a uniform impact speed of v = 3.0 km s−1. The gray and cyan dashed lines indicate the radius r of the impactor required to collisionally disrupt a target of radius R, derived from Benz & Asphaug (1999), for collisions with impact speeds of v = 0.5 and 3.0 km s−1, respectively. Similarly, the yellow and blue dashed lines correspond to the radius r of an impactor required to fragment a target of radius R according to Leinhardt & Stewart (2012) for two different impact speeds. All experimental curves are derived for icy bodies with an assumed bulk density of ρ = 500 kg m−3.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Specific impact energy Q  s  of collision between a target of radius R and the weighted average largest impactor of radius r ≤ R it can collide with for a range of different cases in Table 3. All cases are calculated for a uniform impact speed of v = 3  km s−1. The different panels denote targets belonging to different TNO populations, with different colors indicating different cases. The dashed lines denote the disruption energy threshold ﹩{Q}_{D}^{\star }﹩ for a target of radius R based on the analysis of Benz & Asphaug (1999) and Leinhardt & Stewart (2012) for two different collision speeds, v = 0.5 and 3  km s−1. All four theoretical curves are derived for ice, with an assumed bulk density of ρ = 500  kg m−3.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Same as Figure 6.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Schematic of the cumulative H  r  (r-band absolute magnitude distribution) of the excited (left) and cold classical (right) TNOs (Kavelaars et al. 2021; Petit et al. 2021). The colored labels denote the logarithmic slopes α. The horizontal lines show the range of TNOs detected by surveys and inferred from crater mapping of the Pluto–Charon system and Arrokoth by the New Horizons mission science team (Singer et al. 2019; Spencer et al. 2020).
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Same as Figure 2.
Paper: OSSOS. XXVI. On the Lack of Catastrophic Collisions in the Present Kuiper Belt
Authors: Abedin Y. Abedin, J. J. Kavelaars, Jean-Marc Petit, Brett Gladman, Michele Bannister, Mike Alexandersen, Ying-Tung Chen, Stephen Gwyn, Kathryn Volk
Figure caption: Same as Figure 4.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: STIS visit 1&3, WFC3, and Spitzer data (Case 1) fitted by the best-fit model (black line) that includes an active star together with the contributions from CIA, active trace gases, clouds, and hazes. Stellar activity induces wavelength variations at the base of the model, which is why the gray cloud and Mie cloud contributions are not flat at the bottom.
Paper: The Transmission Spectrum of WASP-17 b From the Optical to the Near-infrared Wavelengths: Combining STIS, WFC3, and IRAC Data Sets
Authors: Arianna Saba, Angelos Tsiaras, Mario Morvan, Alexandra Thompson, Quentin Changeat, Billy Edwards, Andrew Jolly, Ingo Waldmann, Giovanna Tinetti
Figure caption: STIS visit 2&3, WFC3, and Spitzer data (Case 2) fitted by the best-fit model (black line) that includes a homogeneous star together with the contributions from CIA, active trace gases, clouds, and hazes.
Paper: The COS CGM Compendium. IV. Effects of Varying Ionization Backgrounds on Metallicity Determinations in the z < 1 Circumgalactic Medium
Authors: Justus L. Gibson, Nicolas Lehner, Benjamin D. Oppenheimer, J. Christopher Howk, Kathy L. Cooksey, Andrew J. Fox
Figure caption: Various EUVBs used in the literature at z = 0.5 showing the large differences between different models. The colored lines show the KS19 EUVBs that we adopt here, with each color corresponding to a different α EUVB value (see legend). KS19 consider α EUVB = −1.8 to be their fiducial background. The other two backgrounds shown are HM05 (dashed black line) and HM12 (solid black line). The dashed vertical colored lines show the ionization potentials of the various ions included in our model with the addition of O VI, and the horizontal colored bars show the energy ranges probed. The CCC data used here measure metal species with ionization energies between 6 and 60 eV, although no absorber has positive detections of all ion species. Generally, the KS19 backgrounds are harder than either of the HM backgrounds.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper plot shows the predictions of surface temperatures of DYNAMITE predicted planets in the e Eridani system for Hypothesis H[a]. The lower plot shows the predictions of surface temperature of DYNAMITE predicted planet in the e Eridani system for Hypothesis H[d]. Eccentricities for all planets in the system were set to zero for calculating these temperatures, but utilizing the expected low eccentricity values typical of these multiplanet systems does not significantly affect the temperature.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: This plot shows a side-by-side comparison of the DYNAMITE planet prediction and the new module of DYNAMITE that allows statistical prediction of surface temperatures of planets and candidates for Hypotheses H[a] and H[d]. Eccentricities for all planets were set to zero for calculating these temperatures, but utilizing the expected low eccentricity values typical of these multiplanet systems does not significantly affect the temperature.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: Relationship between Bond albedos and calculated radiative equilibrium temperatures for planets, satellites, and asteroids in the solar system. For the adopted Gaussian albedo prior (μ = 0.3, σ = 0.1), roughly 69% and 99.8% of the drawn albedo values fall below A  B  = 0.35 and A  B  = 0.63 respectively. Thus our adopted albedo prior is consistent with known solar system and exoplanet constraints.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates g and f. The lower left plot shows DYNAMITE analysis without planet candidate f while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates g and f. The lower left plot shows DYNAMITE analysis without planet candidate g while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: Hypotheses and analysis predictions for the planetary system e Eridani .
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates g and c. The lower left plot shows DYNAMITE analysis without planet candidate g while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: The upper left plot shows the DYNAMITE analysis without planet candidates g, c, and f. The upper right plot shows DYNAMITE analysis without planet candidates g and c. The lower left plot shows DYNAMITE analysis without planet candidate c while the lower right plot shows the DYNAMITE analysis with all the planets and planet candidates.
Paper: An Integrative Analysis of the Rich Planetary System of the Nearby Star e Eridani: Ideal Targets for Exoplanet Imaging and Biosignature Searches
Authors: Ritvik Basant, Jeremy Dietrich, Dániel Apai
Figure caption: Likelihood of surface temperatures for planets b, d, and e in the system e Eridani .
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Fractional spotted area of stars from O’Neal et al. (1998, 2001, 2004), Morris et al. (2017, 2019), and Howard et al. (1984) vs. their Rossby number. The points are colored by their rotational period in days. Rossby numbers were calculated using their convective turnover time in days derived from their (B − V) color as done in Mittag et al. (2018). Stars that have their fractional area derived from spectroscopic methods are shown with squares, with the other photometric methods denoted by circles. KOI-340 is denoted with a dark-blue star symbol around 0.4 in Rossby number. The Sun is the blue point around 0.65 in Rossby number with no clear error bar, and HAT-P-11 is shown as both a light-blue circle and square around 0.3 in Rossby number, as it has both photometric and spectroscopic fractional spotted area measurements (Morris et al. 2017, 2019).
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Fractional spotted area plotted vs. midpoint time of primary transits in BKJD. KOI-340 is shown using green symbols, with the Sun’s total fractional spotted area coverage given as a solid red bar (Howard et al. 1984) and HAT-P-11's range of fractional spotted areas given as two black dashed lines (Morris et al. 2017). The green upward-pointing triangles denote the minimum fractional spotted area for that transit found using the in-transit spots, and the green points are positioned at the total fractional spotted area found using the full out-of-transit light curve modeled using the minimum number of additional spots as described in Section 4.6.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Total spotted area for Transit 21's full out-of-transit light curve plotted vs. total number of spots needed to fit the data. The in-transit spots are fixed at 1, so in total seven additional spots were needed until the fractional spotted area started to level out. The minimum number of spots needed to fit the data was 3, so we added more spots on top of those four until the spotted area starts to level out, meaning that we are approaching the minimum total spotted area for the entire star.
Paper: Modeling Stellar Surface Features on a Subgiant Star with an M-dwarf Companion
Authors: Maria C. Schutte, Leslie Hebb, Simon Lowry, John Wisniewski, Suzanne L. Hawley, Suvrath Mahadevan, Brett M. Morris, Paul Robertson, Graeme Rohn, Gudmundur Stefansson
Figure caption: Full light curve encompassing one full rotation period (12.96 days) for the simplest primary transit model (Transit 21). The original Kepler data are shown in blue, with the STSP model shown in red. Three spots were needed (at minimum) to model the full light curve in addition to the one fixed in-transit spot.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Luminosity function and fraction with substructures, disks, and clumps of our Fornax dwarf ETG sample. In red, the histogram of all Fornax dwarf ETGs (“dEs”) in the FDSDC as a function of their total r-band absolute magnitude (left y-axis). Similarly, in blue, the histogram of our galaxy sample that has either disk or clump substructures (top panel; “Disky+Clumpy”), disk substructures (middle panel; “Disky”), and clump substructures (bottom panel; “Clumpy”). The black lines correspond to the ratio of both histograms, and thus represent the relative fraction of each subpopulation (right y-axis). The histogram bins are calculated at the position of each galaxy, where each bin includes all the galaxies that lie within a range of ±0.5 mag. The histograms were created following the same technique and binning used in Figure 12 of Lisker et al. (2006b), such that the distribution of our Fornax sample can be directly compared to their Virgo sample (see upcoming Section 6.1). The luminosity functions are complete, and are plotted out to the faintest galaxy in our sample.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Color–magnitude diagram and projected spatial distribution of the FDSDC dwarf galaxies and the dwarf ETGs in our sample. Left panel: g − r color measured within one effective radius vs. r-band total absolute magnitude of the galaxies. Right panel: projected spatial distribution of the galaxies in the ICRS. In both panels, all the FDSDC galaxies are plotted as gray points, while the galaxies that belong to our sample are highlighted as red and blue points, depending on their classification into the disky or clumpy categories, respectively. In the right panel, the central galaxy of the Fornax cluster (NGC 1399) is marked with a “+” sign, while the central galaxy of the Fornax A subgroup (NGC 1316) is marked with a “×” sign. The dotted circle indicates the virial radius of the Fornax cluster (R vir = 0.7 Mpc; Drinkwater et al. 2001) centered on NGC 1399, which is equivalent to a radius of 2.0 deg assuming a Fornax cluster distance of 20.0 ± 1.4 Mpc (Blakeslee et al. 2009).
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Substructure component vs. diffuse component g − r colors of our Fornax dwarf ETG sample. Top panel: the galaxies classified as disky are shown as red points, while galaxies classified as clumpy are shown as blue points. Middle panel: the galaxies are color coded based on their total r-band absolute magnitude, with lighter colors corresponding to brighter galaxies. Bottom panel: the galaxies with CO, H I, and Hα detections are highlighted by red, blue, and green squares, respectively. In all panels, the measurements are performed within one and two effective radii of the galaxies, shown as filled and empty markers, respectively. The error bars are given by the 16th and 84th percentiles of the distributions. The one-to-one relation is shown as a gray line.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption:  g − r color of the diffuse and substructure components of our Fornax dwarf ETG sample as a function of the total r-band absolute magnitude of the galaxies. Left panel: g − r color of the diffuse component vs. total r-band absolute magnitude. Right panel: g − r color of the substructure component vs. total r-band absolute magnitude. Galaxies classified as disky are shown as red points, while galaxies classified as clumpy are shown as blue points. The measurements are performed within one and two effective radii of the galaxies, shown as filled and empty circles, respectively. The error bars are given by the 16th and 84th percentiles of the distributions.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Residual light fractions in the g band vs. the r band of our Fornax dwarf ETG sample. Left panel: residual light fractions measured within one effective radius. Right panel: residual light fractions measured within two effective radii. Galaxies classified as disky are shown as red points, while galaxies classified as clumpy are shown as blue points. The error bars are given by the 16th and 84th percentiles of the distributions. The one-to-one relation is shown as a gray line.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Galaxy residual images in the r band of our Fornax dwarf ETG sample. The parameter setup used to obtain these particular residual images corresponds to a smoothing kernel size equal to 5 times the Gaussian standard deviation of the PSF, and a sampling step size with a growth rate of 20% between successive isophotes. Each image is labeled with the name of the corresponding dwarf galaxy, and has its own gray-scale bar in units of erg cm−2 s−1 Hz−1. The red letter indicates the classification of the galaxy as either disky (“D”) or clumpy (“C”). The image scale is shown as a green line, and corresponds to 15″ (1.5 kpc). North is up, east is to the left.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption:                         Surface brightness and g − r color profiles of the diffuse component (red points) and substructure component (blue points) of the Fornax dwarf galaxy F02D000. Left panel: surface brightness profiles in the g and r bands. The bright-red and bright-blue points correspond to the r-band profile, while the faint-red and faint-blue points correspond to the g-band profile. Right panel: g − r color profiles. The measurements are performed in elliptical annuli of constant width that match the geometry of the isophotes of the diffuse component of the galaxy out to two effective radii. The central region is excluded due to the effects of the PSF, and disregard an amount equal to 1.5 times the PSF FWHM. The gray-shaded area indicates the extension of the PSF FWHM. For figures of the complete sample, see Figure 12 in the Appendix.
Paper: Brought to Light. III. Colors of Disk and Clump Substructures in Dwarf Early-type Galaxies of the Fornax Cluster
Authors: Josefina Michea, Anna Pasquali, Rory Smith, Paula Calderón-Castillo, Eva K. Grebel, Reynier F. Peletier
Figure caption: Residual light fractions of our Fornax dwarf ETG sample as a function of their total absolute magnitude. Left panel: g-band residual light fraction vs. total g-band absolute magnitude. Right panel: r-band residual light fraction vs. total r-band absolute magnitude. Galaxies classified as disky are shown as red points, while galaxies classified as clumpy are shown as blue points. The measurements are performed within one and two effective radii of the galaxies, shown as filled and empty circles, respectively. The error bars are given by the 16th and 84th percentiles of the distributions.