adsabs/AstroCLIMB huggingface dataset:
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: Cloudy models are able to reproduce extreme emission line ratios of O3, O2, and O32 (y-axis) given varied contributions of emission from low- and high-ne gas (x-axis). The circles show O3, the diamonds are O2, and the triangles describe O32. The colors show different metallicities ranging from 0.05 Z⊙ and 0.40 Z⊙ given in the color bar on the right.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: Final coadded rest-UV spectrum for Leo P. We combined the high-resolution G130M and G160M gratings from O. G. Telford et al. (2023) and the G140L grating from HST-GO-17102 to obtain wavelength coverage of all key emission lines used in this study. The pink dashed lines highlight the locations of these key emission lines in the rest-UV spectrum of Leo P.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Relationship between the microscopic filling factor of pebbles, ϕp (common x-axis), and (from top to bottom): a/rp, v0, Pc,p, and rbounce. The solid, dashed, and dotted lines represent Tagg = 1.5 Pa, 100 Pa, and Pcomp, respectively. The blue and orange lines represent ice and silicate pebbles, respectively.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Left: relationship between the collision velocity v0 and a/rp for ice pebbles. The dashed and solid lines represent the pebble radius and our model (Equations (6) and (13)), respectively. The circles and crosses are simulation results with Np = 8507–8693 and 67803–68692, respectively. The initial volume filling factors are ϕs = 0.1, 0.2, 0.3, and 0.4 from light to dark colors. The error is estimated with the Monte Carlo method as described in Appendix B. Right: relationship between the collision velocity v0 and a/rp for silicate pebbles.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Left: relative number of connections between monomers against the number of time steps for ice pebbles. The solid, dashed, and dotted lines represent v0 = 2000, 600, and 200 cm s−1. The initial volume filling factors are ϕs = 0.1, 0.2, 0.3, and 0.4 from light to dark colors. Right: relative number of connections between monomers against the number of time steps for silicate pebbles. The solid, dashed, and dotted lines represent v0 = 200, 60, and 20 cm s−1.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Left: values of σ2 against the constant C, calculated using Equation (C1). The minimum value is σ2 = 1.6 when C2 = 7.1. Right: relationship between the collision velocity v0 and a/rp for ice pebbles and model 2. The solid lines represent model 2 (Equations (A3) and (A4)). The other lines, markers, and colors are the same as in Figure 3.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Projected y-z plane coordinates of monomers (blue) and contact points (orange) of two colliding pebbles along the x-axis. Each pebble has Np = 8555 monomers, with an initial volume filling factor of ϕs = 0.1. The two circles represent the pebble radius (blue, from Equation (18)) and the contact surface radius (orange, from Equation (16)).
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Left: relationship between a/rp and ﹩{N}_{{\rm{con}}}{({r}_{{\rm{p}}}/{r}_{0})}^{-2}﹩ for ice pebbles. The solid lines represent our model (Equations (6) and (20)). The other lines, markers, and colors are the same as in Figure 3. Right: relationship between a/rp and ﹩{N}_{{\rm{con}}}{({r}_{{\rm{p}}}/{r}_{0})}^{-2}﹩ for silicate pebbles.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Schematic of the cylindrical region near the contact surface. It contains pairs of monomers that are in contact and contribute to contact points, as well as monomers that do not contribute to pebble contact.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Schematic of the formation process of 67P. A pebble cloud gravitationally collapses into a planetesimal. Inside the collapsing cloud, pebbles sequentially bounce, lose their kinetic energy in inelastic collisions, and finally stick.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Values of σ2 against the constant C, calculated using Equation (C1). The minimum value is σ2 = 0.62 when C = 1.5.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The ratio of observed to absorption-corrected 8–24 keV flux (Sobs/Sint) as a function of absorption. The flux ratios are shown for the CLUMPY (purple) and baseline (pink) models at z = 0.0 (solid lines), 0.5 (dashed lines), and 1.0 (dotted lines). The black points denote the ratios used in Equation (4) for each log(NH) bin (see Table 4).
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Top: relationship between the collision velocity v0 and a/rp for ice pebbles. The solid lines and colors are the same as in Figure 3. The dotted lines show the power law of ﹩(a/{r}_{{\rm{p}}})\propto {v}_{0}^{1/2}﹩ under the assumption that a ≪ rp. The circles represent ﹩{v}_{0}=\sqrt{4\pi {E}_{{\rm{roll}}}/(3{m}_{0})}{\phi }_{{\rm{s}}}﹩. Bottom: relative error to our model (Equations (6) and (13)).
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The effective number N and fraction ﹩{f}_{{N}_{{\rm{H}}}}﹩ of AGN observed in each log(NH) bin within 1σ for the baseline (pink; hatched) and CLUMPY (purple; dotted) models, as derived by integrating the summed PDF shown in Figure 13 (Appendix B).
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: A schematic demonstrating the spectral components (unabsorbed (purple; dashed) and absorbed (purple; dotted) primary power law, scattered power law (red; dotted–dashed), and galactic emission (gold; solid)) of the baseline model described in Section 3.2. This model is shown for a typical C-Thin AGN with NH = 1023 cm−2. The total spectrum is shown in bolded black. The background is shaded to demonstrate the energy range of XMM-Newton (gray) and NuSTAR (purple).
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: A comparison of the best-fit column densities (NH) for the baseline and CLUMPY models. The shaded regions mark the C-Thin (purple) and CT (gray) regimes. Sources without redshift measurements are shown as red squares.
Paper: Modeling the Contact Surfaces Formed by Pebble Collisions: Application to Formation of Comet 67P/Churyumov–Gerasimenko
Authors: Misako Tatsuuma, Satoshi Okuzumi, Akimasa Kataoka, Hidekazu Tanaka
Figure caption: Values of ﹩{\sigma }_{{\rm{con}}}^{2}﹩ against the constant Ccon, calculated using Equation (C2). The minimum value is ﹩{\sigma }_{{\rm{con}}}^{2}=1.2﹩ when Ccon = 0.72.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The redshifts (left) and observed 3–24 keV X-ray luminosities (right) for sources with detected multiwavelength counterparts. Shown are quasars (dotted; pink), galaxies (hashed; purple), and unclassified (solid; gray) objects.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: A histogram of the net spectral counts in NuSTAR (pink; dotted) and XMM-Newton (purple; hashed) for the sources in our sample.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The median 8–24 keV logN–logS models (black lines) and 3σ confidence intervals (hatched regions) are shown in each log(NH) bin over 1000 iterations of the sample, as described in Section 4.2. The nominal data (binned using the median NH from the posterior) are plotted in solid pink with Poisson error bars (shaded region). logN–logS relations from population synthesis models (Y. Ueda et al. 2014; J. Buchner et al. 2015; T. T. Ananna et al. 2019) are shown for comparison.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The NH distribution (top) and NH fraction (bottom) of the sample down to an observed (left) and absorption-corrected (right) 8–24 keV flux of 6.0 × 10−14 erg s cm−2. The distribution has been calculated over 1000 realizations, all plotted in black, and the median and 3σ errors of the distribution are plotted in pink. The predicted observed ﹩{f}_{{N}_{{\rm{H}}}}﹩ for our sample is shown for three population synthesis models (Y. Ueda et al. 2014; J. Buchner et al. 2015; T. T. Ananna et al. 2019) in the bottom-left figure.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The posterior distributions for NH found by BXA using both baseline (pink) and CLUMPY (purple) models. The vertical dashed line in each panel indicates the CT threshold, and the CT portions of each posterior are shaded. The error bar under the posterior distributions indicates the frequentist results for that source found using the standard XSPEC routines. Red labels indicate that XMM-Newton spectra did not exist for that source. Objects excluded from the analysis are shaded in gray.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The added PDFs of the sample for the baseline (left) and CLUMPY (right) models, giving the observed NH distribution. The sum under the curve in the C-Thin (purple; solid) and CT (gray; hatched) regimes gives the effective C-Thin and CT sample size.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: fCT as a function of observed 8–24 keV flux (solid pink), with the shaded region denoting 3σ error bars for this work. For comparison, predictions from population synthesis models (z < 3; Y. Ueda et al. 2014; J. Aird et al. 2015; J. Buchner et al. 2015; T. T. Ananna et al. 2019) and fCT measurements from the NuSTAR COSMOS (F. Civano et al. 2015, black star) and UDS (A. Masini et al. 2018, black dot) surveys are shown.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The unabsorbed 2–10 keV luminosity distribution of sources with redshift measurements. The sample is split into low (z < 1; pink, hatched) and high (z > 1; purple, dotted) redshift bins. The shaded region gives 1σ confidence intervals.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: The observed column density distribution of the sample for low (z < 1; pink, hashed) and high (z > 1; purple, dotted) redshifts.
Paper: The NH Distribution of Hard X-Ray Selected Active Galactic Nuclei in the NEP Field
Authors: Samantha Creech, Francesca Civano, Daniel R. Wik, Ross Silver, Xiurui Zhao, Rafael Ortiz, Tonima Ananna, Norman A. Grogin, Rolf Jansen, Anton M. Koekemoer, Christopher N.A. Willmer, Rogier A. Windhorst
Figure caption: Best-fit CLUMPY (purple) and baseline (pink) EEMODEL for each source compared to the delta-chi error (Δ).
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: In the top panels, PARSEC isochronal ages plotted against the lithium depletion (left) and dynamical (right) ages, with a 1:1 line of equivalence for reference. In the lithium depletion panel, we plot solutions that use the analytical eagles modules in black and the ML solutions in blue. Some lithium depletion ages provide only upper limits, which are plotted accordingly. We mark SCYA-79 with lighter shades, as its isochronal ages are made uncertain by a weak separation from the field. Both the lithium and dynamical results show broad agreement with the PARSEC isochronal results. The lithium depletion ages often exceed the PARSEC isochronal ages; however, they agree closely for some populations, especially populations with the most complete coverage of their lithium sequences like AqE and CMaN. Nearly all dynamical ages are consistent with the PARSEC isochronal age solutions within uncertainties. In the bottom panel, we show all age solutions for each association, including the three isochrone models, dynamical ages, and lithium depletion ages from the analytical and ML EAGLES modules. There we show that most methods often agree, although the BHAC15 models frequently disagree with nonisochronal methods.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: Fits to the background contamination for all 15 associations included in this paper, which provide false-positive rates, or the rate at which field stars are incorrectly assigned to the association. For populations where a Gaussian fit was used to fit the background, the fit is shown in dark blue, while the RV histogram of all stars is shown in light blue. The shaded region is masked, as that is the RV range occupied by the association. For populations with features that make a fit difficult, we take the mean and standard deviation of a set of probable nonmembers, which are indicated by the red bins. A curve representing the field model in these cases is shown in dark red. In TOR1, we show Pfp results separately for the two components discussed in Section 3.2.1.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: EAGLES lithium depletion fits for each of the 16 associations covered in this work, including both the original and ML EAGLES modules. For each association and EAGLES module, we show two panels; the left one shows the best fit to the lithium sequence, and the right panel shows the combined posterior for all stars included in the fit. For populations with substructure, we color the Li measurements by their subgroup, following the color scheme in Figure 5. Fits that use the EAGLES ML module are labeled in the top right of the age posterior plot, and these are shown in purple and pink rather than the blue and red color scheme for the analytical results.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: CMDs for all 15 associations, adjusted for distance and reddening. Orange diamonds mark probable members with Pfin > 0.5, purple squares indicate stars with Pfin < 0.5, and black triangles mark stars that lack Pfin because they fail one or more of the quality cuts required for a PAge<50 Myr result. The black curve indicates a typical field sequence, represented by a PARSEC 1 Gyr isochrone. In the panel for CasE, we include a cut to avoid contamination from an elevated field sequence in red, which avoids older populations that share its parameter space. In the TOR1 panel, we use different markers for probable members of the two components discussed in Section 3.2.1, as noted in the legend.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: Substructure in young associations where we detect it, shown in l and b galactic sky coordinates and ΔvT,l and ΔvT,b transverse velocity anomalies. We only show stars with Pfin > 0.5. The two components in TOR1 also differ by ∼10 km s−1 in radial velocity, indicating that they are dynamically distinct populations. We rename TOR1-1 to TOR1A, and TOR1-0 to TOR1B.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: Li-6708 Å equivalent width against color for all 15 associations covered by this paper. Stars marked as lithium members are shown with green star icons, while stars that are marked as lithium nonmembers are marked with orange diamonds. Black circles indicate stars with inconclusive lithium membership, while red triangles indicate the stars without a conclusive Li assessment that are rejected due to their lack of Hα emission in Figure 2. Stars with open markers are velocity nonmembers.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: Dynamical ages for all associations and subpopulations where a solution is possible. The black lines represent the median branch length over time for each Monte Carlo sample used in age calculation, and the thickest black line represents the median branch length curve of all members included in sampling. The thick vertical red line and shading represent the best-fit dynamical age solution after debiasing and its 1σ confidence range, while the thinner purple vertical line provides the age solution before debiasing. The population and age solution are annotated.
Paper: SPYGLASS. VII-A. The Demographics and Ages of Small Nearby Young Associations
Authors: Ronan Kerr, Facundo Peŕez Paolino, Jonathan C. Tan, Joshua S. Speagle, 佳士 沈, Adam L. Kraus, José G. Fernández-Trincado, Keivan G. Stassun, Julio Chanamé
Figure caption: Hα equivalent width against color for all 15 associations covered by this paper. Stars rejected as members by Hα are marked as red triangles, and all other stars are marked with black dots.