adsabs/AstroCLIMB huggingface dataset:
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Ratios of the power spectra of different polarization modes. From left to right, the three panels show the power spectrum ratio for P  Q /P  I , P  U /P  I , and P  Q /P  U . The black and red lines represent before and after the imposition of scattering. The blue error bars are the thermal noise associated with telescopes. We used PV and APEX, which have intermediate sensitivities among all EHT telescopes, to generate the error bars. The gray error bands are the sampling noise associated with the intrinsic spatial variability of the intrinsic source, which we averaged down assuming 25 independent observations. The green band represents the size of Earth-bound baselines at 230 GHz.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Mean intrinsic (black) and observed (red) ratios of the power spectra associated with polarization modes defined by the Stokes vectors  S  1 and  S  2 at 86 (left), 230 (middle), and 345 (right) GHz. The sampling noise and thermal errors associated with N = 25 observations and based on ngEHT telescope sensitivities are indicated by the gray band and blue error bars, respectively. The green band represents the size of Earth-bound baselines at 86, 230, and 345 GHz, from left to right.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Power spectra for the total intensity and two linear polarization modes. From left to right, the three panels are for total intensity, first linear polarization, and second linear polarization. The black and red lines are the intrinsic and scattered power spectra, respectively. The blue dotted lines are the diffractively scattered power spectra. The green dashed line in the left panel is the power spectrum of the Gaussian delta ring with a radius of 25 μas, which is the same envelope for the simple source model.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Relative orientations of  S  0,  S  1, and  S  2 are shown on the Poincaré sphere. Here  S  1 is orthogonal to  S  0 and restricted to lie on the Q–U plane, and  S  2 is orthogonal to both  S  0 and  S  1. See the text for explicit definitions.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Power spectrum ratio between the total intensity and the first polarization mode (left), the total intensity and the second polarization mode (middle), and the two polarization modes (right) for the simple source structure defined in Section 3. The black line shows the intrinsic power spectrum ratio, while the red line is the power spectrum ratio observed after scattering. The green band represents the size of Earth-bound baselines at 230 GHz.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Intrinsic (black) and observed (red) P  S2/p  S1 along rays at different orientations relative to the u-axis. From left to right: 0° (u-axis), 45°, and 90° (v-axis). The sampling noise and thermal errors associated with N = 25 observations are indicated by the gray band and blue error bars, respectively.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Arbitrary snapshot drawn from the GRMHD simulation used. The figure includes the Stokes I, Q, U, and V components (left) and their corresponding scattered versions (right). Bottom row: the constructed polarization modes  S  1 and  S  2 are shown, both intrinsic and scattered.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Power spectra for Stokes I (left), Stokes Q (middle), and the optimal  S  1 (right) before (black) and after (red) application of the scattering screen. The dotted blue line represents the diffractively scattered power spectrum.
Paper: Probing Accretion Turbulence in the Galactic Center with EHT Polarimetry
Authors: Chunchong Ni, Avery E. Broderick, Roman Gold
Figure caption: Same arbitrary snapshot drawn from the GRMHD simulation used in Figure 5. The figure includes the constructed polarization modes  S  1 and  S  2, both intrinsic and scattered.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Visualization of the morphology and change in core-mass fraction for all collision types. Gray represents the mantle of a body, and purple its core. When two bodies collide with angle θ and impact velocity v imp, there are nine different collision types assigned by the code (following Stewart & Leinhardt 2012 and Leinhardt & Stewart 2012), but four main outcomes. Merger (top); a grazing collision with no real effect on the mass or CMF of the bodies (top right); a grazing impact that significantly strips one body, changing CMF and producing debris (right); an impact that leaves only one body intact and some debris (bottom right); a destructive impact that leaves only debris (bottom left).
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Observed rocky planets below 10 M ⊕ with good mass and radius measurements taken from the NASA Exoplanet Archive (NASA Exoplanet Science Institute 2022), plotted over lines of constant CMF. The top line is a planet with no core (CMF = 0), the middle two lines are Earth’s (CMF = 0.326 (Stacey 2005)) and Mercury’s (CMF ∼ 0.69 (Hauck et al. 2013)) values, respectively, and the bottom line is a planet made of only core (CMF = 1). The blue shaded area is the region that planets should occupy if they follow stellar compositional ratios, taken from Scora et al. (2020). The planets span the range of possible CMFs and have a maximum CMF close to Mercury’s.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Eccentricities of the planets formed (purple) compared to the eccentricities of super-Earths with well-constrained values from the NASA Exoplanet Archive (teal; NASA Exoplanet Science Institute 2022). The distribution of planets across each axis is shown in the histograms. The size of the dots corresponds to the mass of the embryos. The embryos begin with high eccentricities, but the dynamical friction caused by the debris from collisions brings the eccentricities of most of the final planets down to values comparable to observed exoplanet systems.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: The frequency of each type of collision (black outline), compared to the average mass of debris that the type of collision creates (teal). Super-catastrophic collisions are the most common and create the most debris. The second-most common type of collision is the hit’n'spray. Erosive collisions create a significant amount of debris and can modify the CMF of the remnant, but make up only 8% of the collisions that occur.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Impact angle and impact to escape velocity ratio of all the collisions in the simulated runs. The size of the points corresponds to the total colliding mass of the collision. The collisions in the simulations cover the entire parameter space of collision velocities and angles. Early on in the formation process, when embryos are small, there are large numbers of super-catastrophic collisions. The distribution of collisions for larger embryos later on in the formation process sticks to lower velocities and other, less destructive collision types.
Paper: Rocky Histories: The Effect of High Excitations on the Formation of Rocky Planets
Authors: Jennifer Scora, Diana Valencia, Alessandro Morbidelli, Seth Jacobson
Figure caption: Initial embryo distributions for the cases with (left) surface density slope α = 1.5, e avg = 0.1, and incavg = 0.2, and (right) surface density slope α = 2.5, e avg = 0.5, and incavg = 0.5.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Comparison of the inferred rotation rates as a function of the stellar mass coordinate (green points from asteroseismology, rose point from spectroscopy) to one theoretical model of the radial rotation profile (Fuller et al. 2019). We note that the model is included to provide guidance on what a plausible internal rotation profile might look like, but that any such model includes assumptions (internal magnetic field, initial surface velocity, etc.) that have not been tuned for this star specifically. Radiative shells are marked in blue and convective shells are marked in pink; vertical dashed lines mark the location of the hydrogen burning shell. The seismic points are qualitatively consistent with the model predictions, but the spectroscopic surface velocity is deeply inconsistent.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Illustration of the periods and (minimum) secondary masses compatible with the radial velocity trend derived from Gaia DR3 radial velocities. The blue line indicates the minimum secondary mass derived from the radial velocity trend for each period, while the blue shaded region indicates the 1σ confidence region. The red line denotes the primary mass, and the red shaded region shows the limit on the secondary mass based on the fact that the star is an SB1 only. The purple shaded overlap region indicates the combinations of period and secondary mass compatible with both constraints. Based on the nominal value for the radial velocity trend, periods roughly between 5 and 12 yr and companion masses between 0.3 and 1.0 M ⊙ are compatible with all constraints.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Abundance vs. metallicity for the remaining elements from APOGEE in KIC 9267654 (green circle) and the comparison stars from APOKASC (smaller black circles). In each panel, the element is identified in the upper left corner, with light odd-Z elements labeled in red, alpha elements labeled in green, iron peak elements labeled in magenta, and neutron capture elements labeled in purple. The abundance pattern of KIC 9267654 is consistent with the comparison sample in all elements except for Al, where it is depleted, and Cu, where it is enhanced. The blue cross in the lower left corner of each panel shows the median uncertainty for the comparison stars. As in Figures 6 and 7, the uncertainty in [M/H] is expanded by a factor of 5 for visibility.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Top panels: abundance vs. metallicity for the light elements C, N, and O in KIC 9267654 (green circle) and the comparison stars from APOKASC (smaller black circles). Bottom: the carbon-to-nitrogen ratio correlates well with stellar mass in the sample. The comparison of KIC 9267654 to the trend suggests it could not have gained more than a few hundredths of a solar mass since its first dredge-up. The blue cross in the lower left corner of each panel shows the median uncertainty for the comparison stars. As in Figure 6, the uncertainty in [M/H] is expanded by a factor of 5 for visibility.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Top: metallicity vs. α-enhancement for KIC 9267654 (green circle) and the comparison stars from APOKASC (smaller black circles). Bottom: mass vs. age for KIC 9267654 and the comparison stars from APOKASC. The blue cross in the lower left corner of each panel shows the median uncertainty for the comparison stars. The reported APOGEE uncertainties in the fundamental stellar properties [M/H] and [α/M] are expanded by a factor of 5 for visibility.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Top: the power spectrum density (PSD) of KIC 9267654 (black) in logarithmic scale. The red line represents the sum of the fitted background components. Magenta dotted lines are the two convective contributions. The white noise is the blue dashed line. Bottom: zoom of the above PSD in linear scale around ﹩{\nu }_{\max }﹩ (in light gray), and a smoothed version by an 11 point boxcar function in dark gray. Both PSDs are plotted in S/N after dividing the PSD by the background model (red continuous line on the top plot). The magenta line is the fitted model containing modes with degrees ℓ = 0, 2, and 3. Mixed dipolar modes were not fitted.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: The minimum-mass companion required to produce an ingestion-derived lithium enrichment signature with a 5σ statistical significance along the evolutionary track of KIC 9267654. At its current evolutionary phase, depicted as the red star, the ingestion of a 33 M  Jup brown dwarf companion is required to produce a statistically significant lithium enrichment signature. The locations of the main-sequence turnoff (gray cross) and luminosity bump (salmon diamond) are also illustrated.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Marginalized posterior probability distribution obtained from the apollinaire MCMC sampling, for the mean rotational splitting ν  s  (top) and the inclination angle i (bottom right). The bottom left panel shows the marginalized posterior probability on the couple ν  s –i and allows visualizing the covariance of the two parameters.
Paper: Spinning up the Surface: Evidence for Planetary Engulfment or Unexpected Angular Momentum Transport?
Authors: Jamie Tayar, Facundo D. Moyano, Melinda Soares-Furtado, Ana Escorza, Meridith Joyce, Sarah L. Martell, Rafael A. García, Sylvain N. Breton, Stéphane Mathis, Savita Mathur, Vincent Delsanti, Sven Kiefer, Sabine Reffert, Dominic M. Bowman, Timothy Van Reeth, Shreeya Shetye, Charlotte Gehan, Samuel K. Grunblatt
Figure caption: Top: χ-squared minimization of the fit to ﹩v\sin i﹩ in the HERMES spectrum gives a value of ﹩{5.96}_{-0.97}^{+0.91}﹩ km s−1, with points indicating combinations of temperature, metallicity, gravity, and ﹩v\sin i﹩ that were tested, and lower values of χ-squared indicating better fits. Middle: comparison to the magnesium triplet region suggests stellar parameters that are well fit and consistent with the published APOGEE results. Bottom: we also note that the lithium 6707 feature is not detected in this spectrum, indicating that the lithium abundance is subsolar.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Families of rotation curves generated for log(M 200/M ⊙) = 108–1011.2, in increments of 0.1 dex (gray lines) and 0.5 dex (colored lines; see legend for details) based on a steeply rising Einasto density profile (left) and a more slowly rising cored Einasto density profile (right). Overplotted on both panels as a filled black circle are the V cor and R max values for one galaxy, AGC 731921. M bary, M H I , and M * measurements are listed at the top below the galaxy name. The values of log(M 200/M ⊙) and V max (in units of kilometers per second) based on the best-fitting rotation curves are listed at the bottom of each panel. The core radius r  c  (in units of kiloparsecs), for the cored Einasto profile is shown at the bottom of the right panel. Similar figures for all other galaxies are presented in Appendix B. For uniformity, we plot rotation curves for the same range in halo mass, but note that not all curves are appropriate for a given galaxy (i.e., in the current figure, M 200 − 108 M ⊙ is not appropriate given that M bary ∼  108 M ⊙, resulting in a rotation curve that crosses the others at small radii).
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: The BTFR with our empirical measurements of baryonic mass and H I rotational velocities. Inclination corrected rotational velocities (V rot) are shown with open green circles; asymmetric drift corrected velocities (V cor) are shown with solid blue circles. Galaxies with rotational velocities that are reaching the flat part of the rotation curve (i.e., where the velocity fields in the PV diagrams plateau) are plotted with uncertainties. All other velocities are measured on the rising part of the rotation curves and are lower limits for the maximum rotational velocities (V max) in the galaxies. V max measured for higher-mass galaxies with well-resolved rotation curves are plotted as black circles (Lelli et al. 2019). The best-fitting line to those points is shown as a solid line, with the 1σ dispersion shaded in gray; an extrapolation of the line to lower masses is shown as a dashed line.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Ratio of M bary(<R max) to M dyn<R max) as a function of the radius at which the velocity measurements were made (R max). While it is only a rough surrogate for determining whether the galaxies are dark matter dominated at R max, the comparison provides a useful check for our analysis mapping the measured kinematics of galaxies to theoretical rotation curves in Section 5.3. Points are color-coded by the fraction of baryonic mass within R max; the horizontal line marks where the baryonic mass is 50% of the dynamical mass at R max.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Example PV diagrams for a galaxy with a velocity field that plateaus (left; DDO154) and one that is still rising (right; AGC731921). H I contours are plotted at 3, 6, and, for DDO154, 9 × the rms value. The location of the best-fitting V PV and D PV values and their uncertainties are shown in white. An atlas of PV diagrams for the rest of the sample is presented in Appendix A.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Rotational velocities (V rot; open green circles) and asymmetric drift corrected velocities (V cor, filled blue circles) compared with the maximum physical radius of the H I (R max) for the SHIELD, VLA-ANGST, and LITTLE THINGS galaxies. The asymmetric drift corrections have the largest relative impact on galaxies with the slowest measured rotational velocities and little impact on galaxies with V rot ≳ 30 km s−1.
Paper: The Turndown of the Baryonic Tully–Fisher Relation and Changing Baryon Fraction at Low Galaxy Masses
Authors: Kristen. B. W. McQuinn, Elizabeth A. K. Adams, John M. Cannon, Jackson Fuson, Evan D. Skillman, Alyson Brooks, Katherine L. Rhode, Martha P. Haynes, John L. Inoue, Joshua Marine, John. J. Salzer, Anjana K. Talluri
Figure caption: Comparison of M 200 for our galaxy sample estimated from fits to the Einasto and cored Einasto rotation curves. The steeply rising nature of the Einasto profile places the lowest-mass galaxies in halos that are up to ∼2 orders of magnitude less massive than fits to the cored Einasto profiles. The solid black lines represent perfect agreement between the two sets of values.