adsabs/AstroCLIMB huggingface dataset:
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: Same as Figure 8 but now showing the numerical orbital simulation of 2021 PH27 out to 100,000 yr. The orbit of 2021 PH27 is dynamically unstable over a few million years with numerous close encounters with Venus. The coupling of the eccentricity and inclination over time suggests 2021 PH27 is experiencing a resonant interaction with the planets.
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: The moving object detection efficiency for the survey for a typical field with 1.″4 seeing. The typical field limiting magnitude was around 21.3 mag in the r band. Table 1 and Figure 5 shows the limiting magnitude of each field of the DECam twilight survey.
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: The orbit of the newly discovered Atira asteroid 2021 PH27, which has the smallest semimajor axis of any known asteroid. Though it orbits the Sun faster than Venus as its semimajor axis is less than that of Venus, 2021 PH27 has an aphelion exterior to Venus. It also has a perihelion interior to Mercury’s orbit, causing 2021 PH27 to experience the largest general relativistic effects from the Sun’s gravity of any object known in the solar system.
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: The twilight survey fields taken with DECam showing their elongation position from the Sun and inclination from the ecliptic. The maximum elongation from the Sun to Mercury and Venus are shown by vertical dotted and dashed lines, respectively.
Paper: A Deep and Wide Twilight Survey for Asteroids Interior to Earth and Venus
Authors: Scott S. Sheppard, David J. Tholen, Petr Pokorný, Marco Micheli, Ian Dell'Antonio, Shenming Fu, Chadwick A. Trujillo, Rachael Beaton, Scott Carlsten, Alex Drlica-Wagner, Clara Martínez-Vázquez, Sidney Mau, Toni Santana-Ros, Luidhy Santana-Silva, Cristóbal Sifón, Sunil Simha, Audrey Thirouin, David Trilling, A. Katherina Vivas, Alfredo Zenteno
Figure caption: The limiting magnitude of each twilight field vs. its elongation distance from the Sun. Most of the fields had a limiting magnitude above 21 mag in the r band, with the best fields reaching nearly 22nd mag.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We plot the mutual inclinations between the inner and outer orbits of our systems. Without RV information on the long-period outer binary orbit, most of our systems have two possible measurements for mutual inclination. We show both possibilities, split between the lower-inclination and higher-inclination options in the plot. The degeneracy does not exist for HD 173093 (green cross). The prevalence of misaligned orbits is somewhat surprising, as Tokovinin (2017) found that triples with an outer binary semimajor axis <50 au are generally aligned within 20° (depicted in the prograde and retrograde case with gray dashed lines). Only three of our systems potentially fall within <20° of the outer orbit orientation, hinting that higher-mass triples have more misalignments.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Plot of the PS1/Gaia EDR3 residuals of reference objects as a function of PS1 i-band magnitude for uncorrected (blue), iteration 0 (orange), and iteration 8 (red) cases, in Stripes 2, 16, and 30. (The orange line is hidden behind the red line for Stripe 16.) The solid lines are for all reference objects in the stripe, while the dotted lines are for the very point-like reference objects having a point-source score greater than 0.99 (Tachibana & Miller 2018).
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Mean g − i color of PS1/Gaia reference stars as a function of R.A. and decl. The lower decl. limit of the PS1 survey is δ = −30°. Over most of the sky the color is relatively uniform, but dust absorption in the plane of the Galaxy leads to extremely red mean colors. Note also the blue halo slightly off the plane, which is the population of younger stars near the plane peeking out above the edge of the dust. The blue spots at higher latitudes are globular clusters. These color differences lead to the need for an iterative solution to the DCR correction. The object density is much higher in regions of unusual color, so the effect of color variations on the convergence is large despite the small sky area covered by the plane.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Distribution of hour angles for PS1 observations. The distributions are shown for each of the five PS1 filters (grizy), as well as the combined distribution for all filters. The observations are sufficiently close to the meridian to produce DCR effects that are strongly concentrated along decl. except near the zenith (where the air mass of the observations is always moderate, leading to small DCR effects). The observations that are off the meridian are approximately symmetrical about the y-axis, leading to small biases (<1 mas) due to DCR in the R.A. direction. See the discussion for additional description of the figure.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Plot of the distributions of Gaia EDR3 minus PS1 residuals δRA (purple), δdecl. for iteration 8 (red) and for iteration 0 (orange) in Stripes 2, 16, and 30. The bin size is 0.1 mas. R.A. residuals do not change across iterations. The R.A. and decl. distributions are much more similar after the DCR correction.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Plot of the normalized number distribution of Gaia EDR3/PS1 positional residuals of reference objects after the median neighbor shift correction algorithm using Gaia DR2 (black), using Gaia EDR3 (blue; iteration 0), and with additional DCR corrections (red; iteration 8) for all stripes. The bin size is 0.1 mas. The number distributions are normalized such that their integrals are unity.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Distribution of predicted R.A. and decl. components of DCR for PS1 observations of extremely blue stars. The combined hour-angle distribution (bottom right panel of Figure 8) was used, along with the largest amplitude correction that was measured for any color stars in our sample. The DCR effects in R.A. are typically small even in this worst-case example; the effects on the mean positions are significantly smaller because most PS1 objects use many measurements to determine the means, reducing the DCR bias by a factor ﹩\sqrt{N}﹩ for N observations (typically N = 10–60).
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Convergence of the iterative DCR correction. The left column plots the Gaia EDR3 minus PS1 decl. residuals δdecl. vs. PS1 g − i color in Stripes 2, 16, and 30 for iteration 0 (blue), iteration 1 (green), iteration 2 (orange), and iteration 8 (red). Notice that the scale is smaller for Stripe 16 in the left column. The right column is a more detailed view of δdecl. for iteration 8.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Plot of the number distribution of Gaia EDR3/PS1 positional residuals of reference objects in Stripe 30 with colors 0 < g − i < 1 for iteration 0 (blue) and iteration 8 (red). The bin size is 0.1 mas.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Plot of the number distribution of reference objects on a log scale as a function of PS1 g − i color in three decl. stripes. The bin size is 0.03 mag.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Mean positional bias in PS1 catalog positions compared with Gaia as a function of sky position for blue stars (left column) and red stars (right column). The top row shows the decl. offset before the DCR correction (iteration 0), and the middle row shows the decl. offset after the DCR correction (iteration 8). The bottom row shows the offset in R.A., which is not changed by the DCR correction. The same scale is used for all panels. The faintly seen difference between higher and lower decl. regions in the R.A. plot is due to uncorrected DCR effects. However, the very small amplitude (<1 mas), combined with the complex nature of an algorithm to correct it, led us not to attempt a DCR correction for the R.A.
Paper: Improvements to Pan-STARRS1 Astrometry. II. Corrections for Differential Chromatic Refraction
Authors: Richard L. White, Stephen H. Lubow, Bernie Shiao
Figure caption: Mean positional bias in PS1 catalog positions after DCR correction for (a) blue stars and (b) red stars. The remaining bias in the coordinates is less than 1 mas, even for these very red and blue objects.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Observing conditions for each target. The time is measured from the start of each observation. The seeing is the average optical seeing at zenith throughout each exposure, as reported by the Paranal Differential Image Motion Monitor (DIMM).
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: High-resolution model spectra of MASCARA-1 b with contributions from CO and H2O shown individually. The wavelength coverage of the CRIRES+ K band (setting K2166) used for the observation of MASCARA-1 b is shown in red at the bottom. The right panel shows the pressure–temperature profile used to generate the spectra.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Detection of combined CO and H2O in emission in the atmosphere of MASCARA-1 b. The top panel shows the CCF as a function of orbital phase and planet radial velocity. The white dotted lines indicate the planet radial velocity using the K  p -V sys corresponding to the peak in the CCF map below. The bottom panel shows the S/N detection map, resulting in a significance of S/N = 13.8. White dashed lines show the K  p -V sys at the signal maximum. The atmospheric model used for the cross correlation has combined contributions from CO and H2O along with a thermal inversion as discussed in Section 5.3.
Paper: A First Look at CRIRES+: Performance Assessment and Exoplanet Spectroscopy
Authors: Måns Holmberg, Nikku Madhusudhan
Figure caption: Cross-correlation maps for CO and H2O individually in the atmosphere of MASCARA-1 b, using CRIRES+ spectra from the ExoRES pipeline. The peak significance of the detections is measured to be S/N = 12.9 and S/N = 5.3 for CO and H2O, respectively. The white dotted lines indicate K  p  = 197 km s−1 and V sys = 10 km s−1, the signal maximum of the combined model.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-201 (UVB X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-503 (UVB X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-439 (UVB X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-463 (UVB X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-503 (VIS X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-505 (UVB X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-439 (VIS X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-463 (VIS X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-201 (VIS X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: Chemical Abundances of Young Massive Clusters in NGC 1313 
Authors: Svea Hernandez, Autumn Winch, Søren Larsen, Bethan L. James, Logan Jones
Figure caption: Example synthesis fits for NGC 1313-505 (VIS X-shooter coverage). In black we show the best-fitting model spectra. These models use the final abundances obtained as part of this work.
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: Detection limits for various debris disk surveys of Solar-type stars in the Pleiades, in terms of fractional luminosity (L dust/L star). The colored curves show the typical limits from the Spitzer 24 μm surveys of the Pleiades sample targeted for ALMA (green; Sierchio et al. 2010), the Spitzer 70 μm observations of a subsample of 20 systems (red; Stauffer et al. 2005), and IRAM 30 m 1.2 mm observations of 5 of those systems (blue; Roccatagliata et al. 2009). The purple line shows the ALMA detection limit, which improves on the millimeter sensitivity by about an order of magnitude (for more than an order of magnitude more systems).
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: The hatched histograms show population synthesis models predictions for the detection frequency of debris disks in the Pleiades Solar-type star sample (left) by ALMA at 1.3 mm at the achieved sensitivity, and (right) by Spitzer at 24 μm, following the detection criterion of Sierchio et al. (2010). The gray shaded regions in each panel indicate the observed number (with associated uncertainties).
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: Top: belt masses plotted against blackbody temperature for an example population of simulated debris disks at four representative ages. The leftmost panel shows the initial masses, and subsequent panels show the belt masses after collisional evolution at 20 Myr, 115 Myr, and 4.6 Gyr. By 20 Myr, the warmest belts are already significantly depleted, while the coldest belts experience negligible mass depletion. Bottom: the fractional luminosities plotted against disk blackbody temperature for the same example population.
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: ALMA 1.3 mm continuum images for Pleiades fields where significant( > 5σ) emission sources were detected that are not associated with the target stars located at the field center. Table 4 lists the locations and flux densities of these sources. The beam sizes are indicated in the lower left corner of each panel.
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: ALMA 1.3 mm images of the Pleiades FGK star sample, with typical at the origin of its panel. The synthesized beam is indicated by the ellipse in the lower left corner. No circumstellar dust emission is detected from any of the target stars.
Paper: An ALMA 1.3 millimeter Search for Debris Disks around Solar-type Stars in the Pleiades
Authors: Devin Sullivan, David J. Wilner, Luca Matrà, Mark C. Wyatt, Sean M. Andrews, Meredith A. MacGregor, Brenda Matthews
Figure caption: ALMA 1.3 mm images of the Pleiades FGK star sample (continued).
Paper: A Taxonomy for the Configurations of Quadruply Lensed Quasars
Authors: Paul L. Schechter
Figure caption: Classification scheme for the configurations of quadruply lensed quasars. The white lines show the results of fitting theoretical models of perfect kites and superkites to the image positions. The models for the top row were constrained to be circular. The red circles (top row) and ellipses (bottom row) show the loci of image positions allowed by each model. The models are described in Appendix A. The systems in the top row are J2344−30, J0259−16, and HS 0810 + 25. On the bottom row are J1134−21, J1606−23, and J2033−47.
Paper: A Taxonomy for the Configurations of Quadruply Lensed Quasars
Authors: Paul L. Schechter
Figure caption: HST exposures of a dozen arbitrarily selected quadruply lensed quasars. The reader is invited to classify them using the precepts of Section 1. The lensing galaxy is always visible at the center of the field. The faint background galaxies in panels A and H should be disregarded. Likewise ignore the two faint starlike images in panel I and a faint charged particle detection in panel D. The four brightest images are those of the quadruply lensed quasar. In panels D, E, and G, the galaxy that hosts the quasar can be seen forming something of a ring.
Paper: A Taxonomy for the Configurations of Quadruply Lensed Quasars
Authors: Paul L. Schechter
Figure caption: For each of the systems in our test sample, orange circles have been drawn through the three closest images. The fourth image in systems D and E, both unkites, lie very close to the circle. By contrast, in system H, also an unkite, the fourth image lies very far from the circle. By coincidence, a charged particle detection lies on the circle of system D.
Paper: A Taxonomy for the Configurations of Quadruply Lensed Quasars
Authors: Paul L. Schechter
Figure caption: An HST image of the lensed quasar system PS J0147+46 with a circle drawn through the three closest images, as described in Section 4.2. The fourth image lies well inside the circle, demonstrating the strong noncircularity of the system. In their Figure 1(a), Luhtaru et al. (2021) show an ellipse passing through all four quasar images.
Paper: System Architecture and Planetary Obliquity: Implications for Long-term Habitability
Authors: Pam Vervoort, Jonathan Horner, Stephen R. Kane, Sandra Kirtland Turner, James B. Gilmore
Figure caption: Testing the obliquity model. (a) Fast Fourier power spectrum of the La93 astronomical solution. (b) Fast Fourier power spectrum of the simulation in this study most comparable to the solar system configuration. (c) Obliquity model output for initial obliquity values of 23°, 30°, 40°, 50°, and 60° for the modern solar system configuration. (d) The maximum variation in the obliquity (in degrees) of an Earth-like planet under different planetary architectures, i.e., Figure 7(a) in low-resolution (40×40 simulations across the full parameter space). (e) Same as Figure A1(d) but the input signals are shifted in time by 100 yr to demonstrate the sensitivity to the initial conditions. (f) Difference in the maximum obliquity variation between A1(e) and A1(d).