adsabs/AstroCLIMB huggingface dataset:
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: The evolution of the fraction of the stellar population that is detected in the F158 band as a function of distance for ﹩{t}_{\exp }={10}^{3}\,﹩ s (solid lines) and ﹩{t}_{\exp }={10}^{4}\,﹩ s (dashed lines) exposures with Roman and how this varies with the stellar population parameters (τ in top panels and [Fe/H] in bottom panels). For each panel we also indicate the main-sequence turnoff (MSTO), horizontal branch (HB), and tip of the red giant branch (TRGB) according to the point at which they fall below the 5σ point-source detection apparent magnitude. These each correspond to noticeable drops in ﹩{f}_{\det }﹩. Some main takeaways that are apparent in this figure are as follows: (i) as a population ages, it dims, and even at fixed surface brightness, we detect a smaller fraction of the populations; (ii) the TRGB can be seen out to 35 Mpc for 104 s exposures and populations of interest to halo studies; and (iii) metallicity mainly has an effect on the observability of the RGB, not other parts of the population.
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: The evolution of the total number density of stars, both detected and undetected, with distance. The panels correspond to two different Roman bands, which are indicated in the lower right corner of each panel. We pick three assumed surface brightnesses, spanning from values typical of the outer disks of galaxies, where crowding can begin to dominate (﹩24\,\mathrm{mag}/{\mathrm{arcsec}}^{2}﹩), to the predicted values for faint streams in galaxy halos (﹩32\,\mathrm{mag}\,{\mathrm{arcsec}}^{-2};﹩ see Figure 6). The number density is most strongly dependent on the surface brightness of the population, which is indicated by numbers on the right-hand side of each panel in units of AB magnitudes per square arcsecond. The number density is also dependent on the metallicity of the population being considered (which is indicated by the curve colors) and the age of the population; the solid lines indicate an 11 Gyr old population, while the dotted–dashed lines indicate a 4 Gyr old population. We emphasize the bluest (F062) and reddest (F184) bands to show the extreme ends of this evolution. Generally, n tot ∝ d 2 and increases with age as a population dims (since ﹩{n}_{\mathrm{tot}}\propto {\left\langle {L}_{B}\right\rangle }^{-1}﹩).
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: The evolution of the number density of detected stars with exposure time, ﹩{t}_{\exp }﹩, for a theoretical observation of a population with a surface brightness ﹩{\rm{\Sigma }}=32\,\mathrm{mag}\,{\mathrm{arcesec}}^{-2}﹩, an age of τ = 11.2 Gyr, and a metallicity of [Fe/H] = −2, at a distance of d = 10 Mpc. Note that, realistically, the same population would not have the same surface brightness in each band. We plot each curve up until the crowding limit is reached for the individual bands, indicated by the circular points. We can see that, for such a low surface brightness, this crowding limit is only reached after a very long integration in most bands. Figures such as this can be very helpful when deciding how to effectively use exposure time. For example, we can see a drastic increase in ﹩{n}_{\det }﹩ for the F062 band between 200 and 1000 s, with not nearly as much return on invested exposure time afterward.
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: The evolution of the number density of detected stars with distance for 103 s (solid lines) and 104 s (dashed lines) exposures using the Padova isochrones. We stop plotting the curves once ﹩{f}_{\det }\lt \,{10}^{-6}﹩. As in Figure 3, the panels correspond to different Roman bands, which are indicated in the lower right corner of each panel. The number density is most strongly dependent on the surface brightness of the population, which is indicated by numbers one the left side of each panel in units of AB magnitudes per square arcsecond. The density is also dependent on the metallicity of the population being considered (which is indicated by the curve colors), and slightly on the age of the population, though we only show a τ = 11 Gyr old population here. There are two interesting summary points: (i) The number of detected stars per unit sky area is roughly constant once the HB is no longer detectable as n tot ∝  d 2 and ﹩{f}_{\det }\propto \,{d}^{-2}﹩, and (ii) the redder bands, such as F184 here, are extremely helpful in detecting parts of the RGB out to very great distances.
Paper: Walter: A Tool for Predicting Resolved Stellar Population Observations with Applications to the Roman Space Telescope
Authors: Lachlan Lancaster, Sarah Pearson, Benjamin F. Williams, Kathryn V. Johnston, Tjitske K. Starkenburg, Erin Kado-Fong, Anil C. Seth, Eric F. Bell
Figure caption: The conversion factors between surface brightness in the F158 band and several other bands, indicated by color, as a function of metallicity of the population being observed. We show the conversion factors at an age of τ = 2.8 and 11.2  Gyr as dashed and solid lines, respectively. These conversion factors can be strong functions of metallicity but are relatively independent of age, especially for the redder bands.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Binned spectra of V367 Cyg at three orbital phases in the wavelength interval 6330–6525 Å. The spectra have been normalized to the continuum, and the results have been shifted vertically for display purposes. The main absorption components of the Si II and Fe II lines originate in the circumsystem shell, and it is shown in Section 5 that there are transient absorption features in the shell lines that originate in the spectrum of the donor star. The emission features in the shoulders of the shell lines change with phase in a manner that is not consistent with a shell origin and are strongest at phase 0.5, when the accreting star is eclipsed. [O I] 6364 is a broad, low-amplitude emission feature, with a shape that varies with orbital phase. The wavelength interval used for the cross-correlation velocity measurements in Section 4 is indicated at the top of the figure.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Same as Figure 1, but covering the wavelength interval 6600–6850 Å. The shell lines at these wavelengths are weaker than those in Figure 1 but have similar transient features. He I 6678 is located in a region that is dominated by shell absorption lines.
Paper: Coaxing the Eclipsing Binary V367 Cygni out of Its Shell
Authors: T. J. Davidge
Figure caption: Same as Figure 1, but covering the wavelength interval 6525–6600 Å. The dominant feature is Hα, and the strengths of the emission and absorption components change with orbital phase. These components are most pronounced near primary minimum (spectrum not shown here) and secondary minimum.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Evolution of the resonance angles φ  b  (top panel), φ  c  (middle panel), and Δϖ (bottom panel) for 1000 yr with a step of 0.1 yr. The system exhibits both libration and circulation, with libration happening around 0° for φ  b  and 180° for φ  c . The system goes through circulation, as indicated by φ  c  and Δϖ, near orbit alignment.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Polar plot of apsidal trajectory of the HD 45364 system for 10,000 yr with each point in the plot being 1 yr apart. Two apsidal modes (libration and circulation) are present, and the system’s dynamics appears to be swinging in between the two.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Simulation result for a test particle with an Earth-mass planet injected at 1000 different locations evenly spaced between the boundaries of OHZ. Particle survival rates were calculated as the percentage of the total integration time that the particle survived and remained stable within the system. Only at separations where the particle achieved 100% survival rate do we consider the location dynamically viable for the presence of an additional Earth-mass terrestrial planet. Such locations are only possible near the outer edge of the HZ.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: RV completeness contour of the HD 45364 data set from the injection–recovery test. Two black dots are the known two planets in the system. Blue and red dots are the injected fictitious planet that was recovered and the one not recovered, respectively. The black line represents the 50% detection probability of the contour. Detection probability was color coded according to the color bar on the right.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Best-fit Keplerian model to the RV data from pre- and post-upgraded HARPS (HARPS1 and HARPS2, respectively), and HIRES spectrographs. Best-fit model is in blue with data color coded according to instruments. Upper panels show the total RV model and the residual after the subtraction of the best-fit model from the data. Lower panels show the phase-folded fit for each of the two planets.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Eccentricity variations for planets (b) (upper panel) and (c) (lower panel) for 1000 yr. The variation goes through a similar ∼250 yr quasi-periodic cycle as those observed for the resonance angles in Figure 8.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: RV difference between the best-fit Keplerian and dynamical models in this work with the same data from Figures 2 and 3. In the upper panel, Keplerian model is in gold, and dynamical model is in blue. ΔRV between the two models is shown in purple in the bottom panel.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: Best-fit dynamical model to the same RV data shown in Figure 2. Best-fit model is in black.
Paper: New Dynamical State and Habitability of the HD 45364 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Paul A. Dalba, Andrew W. Howard, Howard T. Isaacson
Figure caption: ln ﹩{ \mathcal L }﹩ for models with different inclination cases, where 0° and 90° represent face-on and edge-on orbits, respectively. Inclination step size is 5°. The system becomes unstable for inclination angles smaller than 9°, and angles up to 40° are disfavored by BIC.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Galactocentric velocity as a function of the Galactocentric distance. Filled markers have f ≤ 0.2 while hollow markers have f > 0.2. Orange markers represent stars with velocities > 450 km s−1. Blue markers correspond to stars that exceed the escape velocity of the MWPotential2014 potential (unbound candidates). Red, gray, and green lines are the Galactic escape velocity curves from the Irrgang13I, McMillan17, and MWPotential2014 potentials, respectively.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Spatial distribution of HiVel stars in the left-handed Galactocentric coordinates. Left, distribution in the X–Y plane. Right, distribution in the X–Z plane. Dashed horizontal lines indicate the transition between the thick disk and the halo. The Sun is located at (X, Y, Z) = (8.12, 0.00, 0.02) kpc. Markers and colors are the same as in Figure 1.
Paper: High-velocity Stars in SDSS/APOGEE DR17
Authors: F. Quispe-Huaynasi, F. Roig, D. J. McDonald, V. Loaiza-Tacuri, S. R. Majewski, F. C. Wanderley, K. Cunha, C. B. Pereira, S. Hasselquist, S. Daflon
Figure caption: Toomre diagram of the HiVel sample. Markers and colors are the same as in Figure 1. The gray region represents stars with kinematic behavior typical of the disk. The dashed vertical line separates stars with retrograde and prograde motion.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: Composite W3-band image of Phaethon in 17.6 s integration (2 × 8.8 s) taken by WISE on UT 2010 January 7. The frame size is 200″ × 200″. No coma or tail is visible on the object having an FWHM of 7.″8. Heliocentric distance, WISE-centric distance, and phase angle are R h = 2.32 au, Δ = 2.08 au, and α = 25.°1, respectively. The cardinal directions (north, N, and east, E), the direction of the negative heliocentric velocity vector (−V), and the antisolar direction (−•) are marked. A 40″ scale bar corresponding to 60,000 km at the Δ distance to Phaethon is shown.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: WISE W3-band image of 1999 YC on UT 2010 January 10 showing a point source with FWHM ∼ 7.″1 in 35.2 s integration (4 × 8.8 s), centered in the frame of 200″ × 200″. R h = 1.62 au, Δ = 1.22 au, and α = 37.°3. N and E exhibit the cardinal directions. − V shows the direction of the negative heliocentric velocity vector, and − • shows the antisolar direction, respectively. A 40″ scale bar corresponding to 35,000 km at the Δ distance to 1999 YC is shown.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: Averaged surface brightness cuts perpendicular to the projected orbital plane of Phaethon. The red and blue lines show a random cut measured in the W3 and W4 bands at the expected trail location (−V), respectively. The W3-band profile was obtained at distance 50″ (≈75,000 km) from Phaethon while, in the W4 band, the profile was extracted at distance 72″ (≈110,000 km). The green region shows the expected location and approximate width of the in-plane dust trail. Surface brightness expressed in digital units (1 count per pixel) corresponds to 20.0 mag arcsec−2 at W3 and 16.6 mag arcsec−2 at W4.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: NEOWISE observation of 2005 UD on UT 2018 September 22 (MJD 58383.2977). Points show the measured flux densities at W1 (3.4 μm) and W2 (4.6 μm). The model descriptions are the same as in Figure 1.
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: Same as Figure 1 but for 1999 YC observed on UT 2010 January 10 (MJD 55213.6428).
Paper: WISE/NEOWISE Multiepoch Imaging of the Potentially Geminid-related Asteroids: (3200) Phaethon, 2005 UD, and 1999 YC
Authors: Toshihiro Kasuga, Joseph R. Masiero
Figure caption: Same as Figure 6 but for 1999 YC. The W3-band profile is at a distance 160″ (≈140,000 km) from 1999 YC, and the W4-band profile is at a distance 215″ (≈190,000 km).
Paper: Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems
Authors: Kai Li, Xiang Gao, Xin-Yi Liu, Xing Gao, Ling-Zhi Li, Xu Chen, Guo-You Sun
Figure caption: The comparison between the synthetic and observed light curves of the ten targets. The lower panels show the O − C residuals.
Paper: Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems
Authors: Kai Li, Xiang Gao, Xin-Yi Liu, Xing Gao, Ling-Zhi Li, Xu Chen, Guo-You Sun
Figure caption: The comparison between the synthetic and observed TESS light curves. The lower panels show the O − C residuals.
Paper: Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems
Authors: Kai Li, Xiang Gao, Xin-Yi Liu, Xing Gao, Ling-Zhi Li, Xu Chen, Guo-You Sun
Figure caption: The relationship between the mean residual and mass ratio q for the ten targets.
Paper: Extremely Low Mass Ratio Contact Binaries. I. The First Photometric and Spectroscopic Investigations of Ten Systems
Authors: Kai Li, Xiang Gao, Xin-Yi Liu, Xing Gao, Ling-Zhi Li, Xu Chen, Guo-You Sun
Figure caption: The O − C diagrams of the ten binaries.
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Histogram (solid black line) of the mean flare temperature, ﹩{\bar{T}}_{\mathrm{flare}}﹩, for all 209 flares in intervals of 983 K, which is close to the median of flare temperature uncertainty. The pdf’s obtained with the kernel density estimation (Silverman 1986; using a Gaussian kernel) with and without taking into account flare temperature uncertainty are shown as blue and red lines, respectively. The histogram shown with a dashed black line is for mean flare temperatures obtained using wavelength limits estimated assuming a smaller uncertainty in the stellar classification used (i.e., half a spectral type and one luminosity class). It is slightly displaced horizontally for a better visualization. Its pdf estimate, without taking into account the uncertainty, is shown by the dashed red line. The green solid and dashed lines show the pdf (without taking into account flare temperature uncertainty) obtained by increasing the input ED by 50% and 100%, respectively. The pdf’s plotted here were normalized to be compared with the histograms; they were multiplied by the number of flares (209) and the size of the histogram bin (983 K).
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Top: Gaia flare energy as a function of spectral type, going from late- to early-type stars, in intervals of half a spectral class. The spectral type at the center of each interval is indicated at the bottom of the plot. The flare energies are in ascending order inside each interval. The different colors represent the different luminosity classes, as in Figure 6, where classes I to V are in red, orange, blue, cyan, and, green respectively. Bottom: weighted average of the flare energy as a function of the average spectral subclass corresponding to the flares within each interval of half a spectral class shown in the top panel. The averages for a given luminosity class, when there are four or more flares, are shown in different colors (as in the top panel). The averages including all luminosity classes are shown in black. The vertical error bars correspond to the standard deviation of the flare energy weighted average, and the horizontal error bars correspond to the standard deviation of the average of the spectral subclass. The absence of a horizontal bar means that only one spectral type was used in the energy averaged.
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Observed GAIA G magnitude as a function of CoRoT White channel magnitude for all analyzed stars. The three open black circles are more than 1″ from the nearest star in the GAIA EDR3 catalog. One of the three has m CoRoT = −13.9 mag and is not easily visible in the figure. The two open blue circles are more than 4σ away from the fitted straight line and were also removed from the fitting. The small red horizontal lines link the CoRoT magnitudes of stars that have been observed twice.
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Gaia flare energy E  G,f  vs. flare duration d  r+d . The black lines correspond to ﹩{E}_{G,f}=c^{\prime} {d}_{r+d}^{3}{B}^{5}﹩ for different B values (see text). The different colors stand for different intervals of stellar rotation in the top panel and for different intervals of flare temperature in the bottom panel. Eclipsing binaries are shown by stars and T Tauri stars by triangles.
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Absolute magnitude of the flare peak as a function of absolute stellar magnitude. Red circles correspond to flares in stars with an unreliable match to a star in the Gaia EDR3 catalog (i.e., open circles in Figure 10) and were not used in the fitting (solid line). The vertical line shows the solar absolute magnitude estimated for the G band, M  G,⊙ = 4.68 mag (Andrae et al. 2018).
Paper: Blackbody Temperature of 200+ Stellar Flares Observed with the CoRoT Satellite
Authors: M. Cristina Rabello Soares, Marcia C. de Freitas, Bernardo P. L. Ferreira
Figure caption: Flare temperature ﹩{\bar{T}}_{\mathrm{flare}}(k)﹩ (as in the top panel of Figure 6) vs. stellar rotation period. The horizontal error bars correspond to the uncertainty in the estimated rotation period, which is very small in most cases. Two flares with temperatures larger than 30,000 K have uncertainties around 10,000 K, and their error bars are not shown for a better visualization. Stars identified as T Tauri are shown in red, and eclipsing binaries in blue, and their flare temperatures are connected by a dotted line of the same color. CoRoT 223983509 is shown in green, as it has been classified as T Tauri and eclipsing binary. In the case of binaries, the period shown is their orbital period.