adsabs/AstroCLIMB huggingface dataset:
Paper: Survival of Terrestrial N2–O2 Atmospheres in Violent XUV Environments through Efficient Atomic Line Radiative Cooling
Authors: Akifumi Nakayama, Masahiro Ikoma, Naoki Terada
Figure caption: Contributions of individual energy deposition/removal rates as functions of XUV irradiation level. Each heating/cooling rate is integrated over the entire atmosphere. The red line represents the absorption in the XUV, the blue one shows the molecular cooling, the green one shows the molecular absorption, the purple one shows the atomic line cooling, the yellow one shows the radiative recombination, and the black one shows the hydrodynamic cooling. Note that the contribution of chemical reactions is not shown, because chemical reactions only change the chemical potentials and do not bring about deposition nor loss of energy from the atmosphere.
Paper: Survival of Terrestrial N2–O2 Atmospheres in Violent XUV Environments through Efficient Atomic Line Radiative Cooling
Authors: Akifumi Nakayama, Masahiro Ikoma, Naoki Terada
Figure caption: Temperature profiles for different XUV irradiation levels up to 1000 times that of the present-day Earth’s, F XUV,⊕.
Paper: Survival of Terrestrial N2–O2 Atmospheres in Violent XUV Environments through Efficient Atomic Line Radiative Cooling
Authors: Akifumi Nakayama, Masahiro Ikoma, Naoki Terada
Figure caption: Temperature profiles for solar irradiation at different ages.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Two-sector (m = 1) power from 27 day (top), 28.5 day (middle), and 30 day (bottom) structures (blue) compared with their total m = 1 power (red). This figure shows that 27 day power originates in all four sunspot cycles, but the 28.5 day and 30 day power come mainly from the stronger sunspot cycles 21 and 22.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Power spectrum of daily WSO mean-field measurements during 1975–2021, showing three main sectorial peaks at ω ≈ 0.231, 0.460, and 0.702 rad day−1 (corresponding to a rotation period of 27.2 days and its second and third harmonics). The plot has been smoothed in a moving average of 12 resolution elements, each of size Δω = 2π/N = 3.70 × 10−4 rad day−1.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Segments of the power spectrum in Figure 4, showing the fine structure of the m = 1 (left), m = 2 (middle), and m = 3 (right) components for the full time interval 1975–2021.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Power in the two-sector (top), four-sector (middle), and six-sector (bottom) patterns of the mean field. Referring to Table 1, we expect this power to originate mainly in the ﹩{Y}_{1}^{1}﹩, ﹩{Y}_{2}^{2}﹩, and ﹩{Y}_{3}^{3}﹩ components of the field.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Result of inverting the Fourier transform of the mean field back to the temporal domain using all three frequency windows (0.20–0.25), (0.42–0.50), and (0.65–0.73) rad day−1 (corresponding to the m = 1, m = 2, and m = 3 sectorial modes, respectively), and then displaying the 27 day moving standard deviation of this inverted transform.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Rms deviation of the WSO mean field from its 27 day average value (red), compared with the monthly averaged sunspot number from the Royal Observatory of Belgium (SILSO) divided by 2000 (blue) during cycles 21–24. This comparison shows the tendency of the mean field to occur in episodic bursts, often when the sunspot cycle begins its decline.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Power spectra of the mean field, showing the m = 1 fine structures at 0.21, 0.22 and 0.23 rad day−1 as the starting time, t, of the Fourier transform is increased. The 30 day and 28.5 day sidebands are successively reduced as t shifts from 1989 to 1991 and then to 1996. The 27 day peak is reduced when t shifts to 2005, leaving a small contribution from 2015 to 2016.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Power spectra of WSO mean-field measurements from time, t, to the end of the data set on 2021 November 16, showing the emergence of the ∼30 day (0.208 rad day−1) peak as t decreases from 1990 February 22 to 1989 January 9.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Mean-field measurements during the first year of observations at WSO, showing the end of a 27 day recurrence pattern, that was associated with the gradual demise of a long-lived coronal hole.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: The [O III]/Hβ vs. [N II]/Hα diagnostic diagram (Baldwin et al. 1981) for all 388 AGN candidates found in this work. The [N II]/Hα AGNs and composites are shown as teal triangles and orange circles, respectively, while the He II/Hβ AGNs are shown as brown squares and [Fe X]-selected AGNs as black pluses. The [Ne V]-AGNs are added as unfilled back diamonds. Eleven of the He II-selected AGNs, 2 of the [Fe X]-selected AGNs, and all 3 of the [Ne V]-selected AGNs overlap with the [N II]/Hα AGNs/composites.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: Simulated emission-line ratios in the He II/Hβ and [O III]/Hβ vs. [N II]/Hα diagrams from various combinations of AGN + SF line fluxes demonstrating that it is possible to have He II-selected AGNs that fall in the SF region of the [N II]/Hα diagram. We show the results using three AGNs: NGC 4395 (first two columns), a He II-selected AGN from this work (CATAID 1787285; middle two columns), and a mock low-metallicity AGN (last two columns). The SF line fluxes are scaled by the ratio of the [O III]λ5007 line for each AGN to each SF galaxy by “SF contribution factors” of 0.5 (first row), 1 (second row), and 2 (third row) before the addition. See Section 4.2 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: The [O III]/Hβ vs. [N II]/Hα narrow-line diagnostic diagram (left panel) for galaxies with stellar masses M ⋆ ≤ 1010 M ⊙ in the GAMA survey using the classification scheme summarized in Kewley et al. (2006). We show the 71 AGN and 238 composite galaxies as teal triangles and orange circles, respectively, and those consistent with star-forming galaxies as sky blue points. The middle and right panels show the AGN and composite objects in the [O III]/Hβ vs. [S II]/Hα and [O I]/Hα diagrams. Only AGN candidates with reliable [S II] and/or [O I] detection are plotted in the middle and right panels. Characteristic error bars are located in the lower right region of each panel. See Section 4.1 for details.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: An example of a redshift-corrected spectrum (top panel) for a broad-line AGN in our sample with chunks showing various emission lines (bottom panels). This galaxy has CATAID 852508 and is among the [N II]/Hα-selected AGN candidates that also has broad Hα emission. In the top panel, we show the observed spectrum in black and the best-fit continuum + absorption line model in blue. In the bottom panels, we plot chunks of the emission-line spectra in black, the best-fitting total model (Gaussian emission-line model + local linear continuum model) in red, and the individual Gaussian components in gold. The Gaussian broad Hα and Hβ components are plotted in dotted dark blue.
Paper: Hundreds of Low-mass Active Galaxies in the Galaxy And Mass Assembly (GAMA) Survey
Authors: Sheyda Salehirad, Amy E. Reines, Mallory Molina
Figure caption: The He II/Hβ vs. [N II]/Hα diagnostic diagram. We apply the criterion log(He II/Hβ) > −1 (see Section 4.2) to separate star-forming galaxies from galaxies with AGN activity, which is shown as the black dotted line. Of the 44 galaxies with detectable He II emission in our parent sample, 36 fall above this line, which we show as brown squares, while the SF galaxies are shown as steel blue circles, 12 of the galaxies in this sample are also AGNs/composites in the [N II]/Hα diagnostic, which we indicate with unfilled circles, while one AGN is observed with [Fe X] emission and two AGNs are also observed with [Ne V] emission, which are plotted as a plus and unfilled black diamonds, respectively. The characteristic error bars are added in the lower right of this diagram.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: Comparison between the β radial profile inferred from the TNG50 simulation using different selection criteria and various isolated data points from different observations. From left to right, we present the β profile with ﹩\tilde{r}\geqslant 1﹩, ﹩\tilde{r}\geqslant 1,\tilde{Z}\geqslant 5﹩ and ﹩\tilde{r}\geqslant 1,\tilde{Z}\geqslant 5,﹩ [Fe/H] ≤ −1.3. In each panel, we also present the data points from Sirko et al. 2004, Bond et al. 2010, Deason et al. 2012, Sohn et al. 2018, Watkins et al. 2019, Lancaster et al. 2019, and Cunningham et al. 2019. It is seen that adding the metallicity cut with [Fe/H] ≤ −1.3 somewhat reduces the diversity of models, as it substantially removes the young stars. On the contrary, the model diversity is maximal for ﹩\tilde{r}\geqslant 1﹩, in which the diversity is comparable to the error bars from changing the observations. This demonstrates that including/altering the stellar types may significantly affect the β, causing different observations to have different results.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: Comparison of the β radial profile from the TNG50 simulation with three extended observational data points. The top panels present the data from Kafle et al. (2012), the middle panels show the results from King et al. (2015), and the bottom panels present the results from Bird et al. (2019). In each row, we present the TNG50 results using different selection criteria. It is seen that there is a good overall agreement between the TNG50 results and these extended observations. The model diversity is somewhat comparable to the error bars in Kafle et al. (2012), while it is smaller than the ones from King et al. (2015). Finally, while the first two panels show a prominent dip in the β radial profile, the third one does not show any particular dips. Since proper motion has not been considered in the first two cases, the third one may be more reliable.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The β energy profile vs. the β radial profile for different halos in our galaxy sample. For each energy shell, we infer the median distance of stars and compute the β r for that location. In inferring the β E, we use a spatial cut of 1 kpc ≤ r ≤ 100 kpc.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The β radial profile for stars located at r ≥ 1 kpc (top panels) and with r ≥ 1 kpc and Z ≥ 5 kpc (bottom panels). In each row, from left to right, we consider stars with [Fe/H] ≤ −1.3, −1.3 ≤ [Fe/H] ≤ 0, and [Fe/H] ≤ 0.0. While in the left panels, we present the β itself to facilitate the comparison, in the middle and right panels, we compute δ β subtracting the β from the left panel with [Fe/H] ≤ −1.3. It is clearly seen that expanding over the range of metallicity, on average, diminishes the β.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The β profile for different eccentric orbits. From left to right, we present the entire population of stars and stars with e ≤ 0.3, 0.3 ≤ e ≤ 0.7, and e ≥ 0.7. It is noted that low-eccentricity stars have lower β than the parent population, as such stars are on nearly circular orbits. On the other hand, stars with higher eccentricities are more on radial orbits than tangential, producing higher β values.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The β profile for stars of different orbital types. From left to right, we study the β radial profile for all, retrograde, radial, and prograde orbits. It is generally seen that stars on radial orbits have slightly higher β than the retrograde and prograde orbits. On the contrary, stars on retrograde and prograde orbits show similar trends in the β radial profile.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The 1D distribution of the eccentricity of stars in our galaxy sample. Quite interestingly, most galaxies have an eccentricity peak between 0.2 and 0.4. In very few cases, there is a second peak at higher eccentricities of about 1.0 coming from those stars located at larger distances.
Paper: On the Robustness of the Velocity Anisotropy Parameter in Probing the Stellar Kinematics in Milky Way–Like Galaxies: Takeaway from TNG50 Simulation
Authors: Razieh Emami, Lars Hernquist, Mark Vogelsberger, Xuejian Shen, Joshua S. Speagle, 佳士 沈, Jorge Moreno, Charles Alcock, Shy Genel, John C. Forbes, Federico Marinacci, Paul Torrey
Figure caption: The 2D distribution plot of the radii vs. the eccentricity for a subsample of four galaxies from our galaxy sample. The Spearman correlation demonstrates that the eccentricity is uncorrelated with the radii.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: The intrinsic vs. “observed” radius distributions of exoplanets, when employing a mixture model of Ed10  2  and Ed10  4  simulations to mimic Kepler planet occurrence per Section 2.2.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: The density vs. semimajor axis distributions of detected planets for both models of atmosphere erosion. The more pronounced clustering of planets sculpted by giant impacts makes it possible to distinguish which model is the dominant one.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: The distribution of observed simulated system monotonicity as defined in Gilbert & Fabrycky (2020). Systems close to 1 are more ordered in radius from smallest to largest; systems close to −1 are ordered from largest to smallest. Giant impacts and photoevaporation largely follow the same trend of increasing size ordering, but systems sculpted by giant impacts are ordered to a lesser degree.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: Period–radius distributions for full simulated planet population, color-coded by the difference in bulk density between giant impacts and photoevaporation.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: The intrinsic radii distributions of Ed10  2  (associated with dynamically cooler outcomes) and Ed10  4  (associated with dynamically hotter outcomes) simulations.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: The probability that an observed planet retains an atmosphere under both models of atmosphere loss. Planets in STIPS are highly likely to retain their atmospheres when sculpted by giant impacts.
Paper: Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets
Authors: Quadry Chance, Sarah Ballard, Keivan Stassun
Figure caption: A comparison between planet radii distributions in scenarios where photoevaporation is dominant (far left), where giant impacts are dominant (far right), or where both kinds of atmosphere loss occur in equal proportion (center).
Paper: Migration Traps as the Root Cause of the Kepler Dichotomy
Authors: Brianna Zawadzki, Daniel Carrera, Eric B. Ford
Figure caption: Frequency of single (1t) and multitransiting (2t, 3t, etc.) systems for models A and B, as well as four thought experiments. The low-mass runs (model B) produce planets with larger periods, wider separations, higher mutual inclinations, and smaller planet radii. The thought experiments progressively alter each of these variables. In B 1 we scale down planet periods so that the innermost period matches model A. In B 2 we also scale down the separations to make the number of planets within 200 days match model A. In B 3 we also lower the inclinations to match model A, and in A 1 we lower planet masses in half, similar to model B. Since A 1 and B 3 look similar, these four variables explain most of the difference between the high-mass and low-mass systems. The error bars show the 25th and 75th percentiles of the distribution resulting from 10,000 bootstrap resamples.
Paper: Migration Traps as the Root Cause of the Kepler Dichotomy
Authors: Brianna Zawadzki, Daniel Carrera, Eric B. Ford
Figure caption: For each planet in a system with at least three planets within 200 days we plot the planet’s inclination i relative to the invariant plane, and ascending node ΔΩ after rotating the system so that the mean ascending node is zero. Rotating the system like this makes nodal alignment easier to identify, as aligned nodes appear as an overdensity of dots around ΔΩ = 0°. Runs where the probability of detecting at least three transiting planets is greater than the probability of detecting two transiting planets (top) show nodal alignment, while the other runs (bottom) do not.
Paper: Migration Traps as the Root Cause of the Kepler Dichotomy
Authors: Brianna Zawadzki, Daniel Carrera, Eric B. Ford
Figure caption: The occurrence of 1t systems as a function of stellar noise (obtained by the 4.5 hr CDPP) for a sample of Kepler planet candidates with radii of 1–3 R ⊕ and periods <200 days around G dwarf stars. Error bars are shown assuming a binomial distribution. The noisiest stars tend to have larger fractions of 1t systems, effectively increasing the magnitude of the Kepler dichotomy. We have verified that this trend is robust to the choice of planet radii included, especially for the noisiest 20% of stars.
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Four reconstructions of TSI are reported, obtained with different methods for comparison purposes only. Our TSI reconstruction is shown as a continuous red line; the red bold line is the TSI smoothed over a period of 22 yr with a 2σ uncertainty shown as the orange stripe. The NRL-TSI data Climate Data Record (green line) is from Coddington et al. (2019). TSI values from Wu et al. (2018) are in magenta. CHRONOS, MC17 TSI values from Egorova et al. (2018) are in blue. The names refer to the grand minima that occurred in the analyzed period, i.e., Spörer, Maunder, Dalton, and Gleissberg.
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Annual values of the fractional solar disk coverage by plage as a function of time. This composite is derived by merging the values from a reconstructed time series using Equation (5) (red solid line) and observed data (green solid line). The light red region indicates the uncertainty range in the reconstructed time series, while the light green region shows the 5σ confidence interval of the mean annual value.
Paper: The Sun’s Mean Line-of-sight Field
Authors: Neil R. Sheeley
Figure caption: Daily measurements of the Sun’s mean line-of-sight field obtained at WSO from 1975 May 16 to 2021 November 16. The blurred cloud of points shows peaks of strength ≳1G in each cycle, and valleys of strength ≲0.2G near sunspot minimum.
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Comparison between the TSI PMOD composite (in gray) and the reconstructed TSI time series for solar cycles 22 (green) and 23 (red). The TSI reconstruction was computed independently for cycles 22 and 23 (see text).
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Dependence of the parameter Ts  k  on the k-cycle averaged solar modulation potential 〈Φ〉 k . Individual solar cycle numbers are indicated in the plot, while the error bars are 1σ standard error of the mean. This relationship is well described by the linear model (solid line) given by Equation (5). The Pearson’s correlation coefficient is −0.77, at a confidence level greater than 95%.
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Empirical mode decomposition of the standardized potential ﹩\hat{{\rm{\Phi }}}﹩. The IMFs and the residual are shown. IMF1 and IMF2 capture the shortest periods, i.e., periods of approximately 11 yr and 22 yr, respectively. The residual shows the monotonic trend of the signal. The ordinates have the same scale, so the IMFs can be easily compared.
Paper: Total Solar Irradiance during the Last Five Centuries
Authors: Valentina Penza, Francesco Berrilli, Luca Bertello, Matteo Cantoresi, Serena Criscuoli, Piermarco Giobbi
Figure caption: Annual values of the standardized fractional solar disk coverage by sunspots ﹩{\hat{\alpha }}_{s}﹩ (dotted black line) and standardized potential ﹩\hat{{\rm{\Phi }}}﹩ (continuous red line). The sunspot signal has been reconstructed until 1873, while more recent values are recorded (Mandal et al. 2020).