adsabs/AstroCLIMB huggingface dataset:
Paper: A Transiting Super-Earth in the Radius Valley and an Outer Planet Candidate Around HD 307842
Authors: Xinyan Hua, Sharon Xuesong Wang, Johanna K. Teske, Tianjun Gan, Avi Shporer, George Zhou, Keivan G. Stassun, Markus Rabus, Steve B. Howell, Carl Ziegler, Jack J. Lissauer, Joshua N. Winn, Jon M. Jenkins, Eric B. Ting, Karen A. Collins, Andrew W. Mann, Wei Zhu, Su Wang, R. Paul Butler, Jeffrey D. Crane, Stephen A. Shectman, Luke G. Bouma, César Briceño, Diana Dragomir, William Fong, Nicholas Law, Jennifer V. Medina, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Chris Stockdale, Roland Vanderspek, Joel Villaseñor
Figure caption: Corner plot of all fitted parameters in the one-planet RV fit using RadVel.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Intermediate Galactic latitude LOSs (C2, C16, and C37) on top of the Lallement et al. (2022) and Vergely et al. (2022) dust map, at 25 pc resolution, of the nearby Galaxy (d < 2 kpc). The blue color bar is the V-band extinction density in log space. The red color bar is the distance of the stars in parsecs. Top: edge-on views of the Galaxy centered at different (l, b) coordinates depending on the sight line. Bottom: face-on view of the Galaxy centered at the Sun at (0, 0) pc. The Galactic center, (l, b) = (0, 0), is at (8200, 0) pc, toward the right, in all maps.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top: sky plot showing the IPS-GI fields location colored by the weighted P  V /E(B − V) upper limits. The turquoise circles are unreliable upper limits due to potential outliers. The background image is the optical emission of the Galaxy adapted from ESA/Gaia/DPAC. Bottom: weighted P  V /E(B − V) upper limits with Galactic longitude (left), and absolute Galactic latitude (right). Error bars show the 68% confidence interval of the weighted 99th percentile (Section 4.2).
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Differential optical extinction profile (25 pc resolution) from Vergely et al. (2022) and Lallement et al. (2022; top row), reddening (middle row), and polarization intensity (bottom row), as a function of distance in fields C2 (left), C16 (middle), and C37 (right). The red solid line is the median value. The pink shaded area is the 16th–84th confidence interval. The vertical orange dotted–dashed line is the approximated distance at which the sight line leaves the Galactic thin disk, assuming a scale height of 300 pc.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Top: polarization vectors in field C16 colored by the polarization efficiency. Bottom: polarization angle (in the Galactic frame) of the same field. The dispersion is corrected in quadrature by the measured error average as in Pereyra & Magalhães (2007).
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Similar to Figure 4 but using G19 (left), M06 (middle), and PC16 (right) reddening to calculate the upper limits on each IPS-GI field (gray dashed lines). The red dashed lines show the upper limit of field C2. Light-green dashed lines are unreliable upper envelopes due to potential outliers or unreliable reddening measurements. For PC16, only the intermediate-latitude fields are plotted; see Section 3.2.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Weighted polarization efficiency upper envelope (top) and weighted median polarization efficiency (bottom) as a function of the dispersion of the polarization angle corrected by the average of the measured errors as in Pereyra & Magalhães (2007). Bad Gaussian fits of the polarization angle distribution are indicated with red “X” markers.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Polarization efficiency upper limits with Galactic longitude. The red and blue curves are the toy models for different pitch angles, p.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Systematic difference between the weighted polarization efficiency upper envelopes calculated with G19 (dark-blue circles), M06 (orange triangles), and PC16 (red squares) reddening, and those calculated with Anders22 reddening.
Paper: Interstellar Polarization Survey. III. Relation between Optical Polarization and Reddening in the General Interstellar Medium
Authors: Y. Angarita, M. J. F. Versteeg, M. Haverkorn, C. V. Rodrigues, A. M. Magalhães, R. Santos-Lima, Koji S. Kawabata
Figure caption: Similar to the systematic reddening differences of Figure 1 but only for field C2. The histogram shows the distribution of the difference and the values under the 3σ  limit (the gray-shaded area).
Paper: Erratum: “Kepler and the Behemoth: Three Mini-Neptunes in a 40 Million Year Old Association” (2022, AJ, 164, 215)
Authors: L. G. Bouma, R. Kerr, J. L. Curtis, H. Isaacson, L. A. Hillenbrand, A. W. Howard, A. L. Kraus, A. Bieryla, D. W. Latham, E. A. Petigura, D. Huber
Figure caption: Age-diagnostic diagrams from the stellar groups near Kepler-1643, KOI-7368, and KOI-7913. Top row: color–absolute magnitude diagram of candidate Cep-Her members, plotted over candidate members of the δ Lyr cluster (≈38 Myr; Bouma et al. 2022) and the Gaia EDR3 Catalog of Nearby Stars (gray background). The left and right columns shows stars in RSG-5 and CH-2, respectively. The range of colors is truncated to emphasize the pre-main-sequence; approximate spectral types are shown on the upper axes. Stars that fall far below the cluster sequences are field interlopers. Bottom row: TESS and ZTF-derived stellar rotation periods, with the Pleiades (≈112 Myr) and Praesepe (≈650 Myr) shown for reference (Rebull et al. 2016; Douglas et al. 2017). The detection efficiency for reliable rotation periods falls off beyond ﹩{({G}_{\mathrm{BP}}-{G}_{\mathrm{RP}})}_{0}\gtrsim 2.6﹩.
Paper: Inner Planetary System Gap Complexity is a Predictor of Outer Giant Planets
Authors: Matthias Y. He, Lauren M. Weiss
Figure caption: The root mean square (rms) of the RV residuals (top) and the number of RV observations (bottom) vs. the gap complexity for the KGPS targets with at least three planets. The points are plotted using a similar convention as in Figure 3, where the gap complexity only includes the inner small planets (except for the red triangles, which also include the OG planets). The gap complexity is uncorrelated with the RV rms or the number of RV observations.
Paper: TOI-3785 b: A Low-density Neptune Orbiting an M2-dwarf Star
Authors: Luke C. Powers, Jessica Libby-Roberts, Andrea S. J. Lin, Caleb I. Cañas, Shubham Kanodia, Suvrath Mahadevan, Joe P. Ninan, Guđmundur Stefánsson, Arvind F. Gupta, Sinclaire Jones, Henry A. Kobulnicky, Andrew Monson, Brock A. Parker, Tera N. Swaby, Chad F. Bender, William D. Cochran, Leslie Hebb, Andrew J. Metcalf, Paul Robertson, Christian Schwab, John Wisniewski, Jason T. Wright
Figure caption: The TSM of known exoplanets with both a measured (>3σ) mass and radii >4 R ⊕ as a function of equilibrium temperature. Planets orbiting M dwarfs are labeled according to Table 6 and are noted with colors varying by their respective planetary radii, while planets orbiting FGK-dwarf stars are plotted as gray points. TOI-3785 b (navy blue circle) possesses one of the highest TSMs for any planet cooler than 600 K, making it a promising target for future transmission spectroscopy observations.
Paper: Satellite Optical Brightness
Authors: Forrest Fankhauser, J. Anthony Tyson, Jacob Askari
Figure caption: Comparison of satellite brightness models. We use Pearson correlation to measure model trend. Histograms of the residuals are also shown. For our calculations using BRDFs measured in the lab, we find a Pearson correlation of R = 0.69. This model systematically underpredicts brightness, because it only accounts for the two primary satellite surfaces and ignores smaller components on the satellite. For our empirical model, we find R = 0.68. Because this model has free parameters, it does not underpredict brightness. Both of these models are a respectable improvement over the optimal diffuse sphere model, which has a correlation of R = 0.47. We note that this model has systematic error, as the residual distribution is not Gaussian-like. This demonstrates that, if either lab-measured BRDFs or sufficient satellite brightness observations are available, our techniques are a better choice than the diffuse sphere model.
Paper: Satellite Optical Brightness
Authors: Forrest Fankhauser, J. Anthony Tyson, Jacob Askari
Figure caption: The diffuse sphere model shows little variation in brightness. Satellites in the western sky are shadowed by Earth (1). The controlling factors of brightness are satellite range and the illuminated fraction of the sphere. Satellite brightness falls off with satellite range (2). Modeling satellite brightness as a function of just these two variables is overly simplistic.
Paper: Satellite Optical Brightness
Authors: Forrest Fankhauser, J. Anthony Tyson, Jacob Askari
Figure caption: With BRDFs best fit to observed data, our model captures both forward scatter from the chassis (7) and backscatter from the solar array (8) to some degree. This model could be improved by using more Starlink v1.5 observations over a wider variety of solar angles and less noisy observations.
Paper: Satellite Optical Brightness
Authors: Forrest Fankhauser, J. Anthony Tyson, Jacob Askari
Figure caption: In our model, two distinct brightness peaks are clearly visible. The first is visible earlier in the morning and is caused by light forward-scattered from the chassis nadir. This specular peak is visible just above the eastern horizon (3). The second brightness peak is caused by light backscattering from the solar array. It is most prominent in the western sky near dawn (5). There is also a transition where both peaks are visible (4).
Paper: Satellite Optical Brightness
Authors: Forrest Fankhauser, J. Anthony Tyson, Jacob Askari
Figure caption: Earthshine from vegetation adds an additional component of brightness, low in the eastern sky (6). This effect becomes more and more pronounced as the Sun rises.
Paper: Magnetic Field Measurements of Low-mass Stars from High-resolution Near-infrared IGRINS Spectra
Authors: Eunkyu Han, Ricardo López-Valdivia, Gregory N. Mace, Daniel T. Jaffe
Figure caption: Comparison between the measured magnetic field strengths from this work and literature values. The left panel shows the magnetic field measurements from the Zeeman intensification method vs. those from the literature, while the right panel shows the measurements from the Zeeman broadening method. The solid black lines mark the 1-to-1 relations and dashed and dotted lines mark 1 and 2 kG offsets.
Paper: Magnetic Field Measurements of Low-mass Stars from High-resolution Near-infrared IGRINS Spectra
Authors: Eunkyu Han, Ricardo López-Valdivia, Gregory N. Mace, Daniel T. Jaffe
Figure caption: Comparison between the measured magnetic field strengths derived from IGRINS with those derived from iSHELL and CARMENES data. Solid black lines mark the 1-to-1 relations and dashed and dotted lines mark 1 and 2 kG offsets. Different colors represent the S/N of each IGRINS (left and middle panels) and iSHELL (right panel) spectrum from the present study.
Paper: Magnetic Field Measurements of Low-mass Stars from High-resolution Near-infrared IGRINS Spectra
Authors: Eunkyu Han, Ricardo López-Valdivia, Gregory N. Mace, Daniel T. Jaffe
Figure caption: Comparison between the measured magnetic field strengths from IGRINS H- and K-band spectra. The left panel shows the measurements using the Zeeman intensification method and the right panel shows the measurements using the Zeeman broadening method. In both panels, solid black lines mark the 1-to-1 relations, and dashed and dotted lines mark 1 and 2 kG offsets. Different colored circles represent T eff for the individual stars.
Paper: Magnetic Field Measurements of Low-mass Stars from High-resolution Near-infrared IGRINS Spectra
Authors: Eunkyu Han, Ricardo López-Valdivia, Gregory N. Mace, Daniel T. Jaffe
Figure caption: Comparison between the magnetic field strengths measured by the Zeeman broadening and Zeeman intensification methods. The solid black line represents the best-fit relation between the two measurements with the 1σ uncertainty regime in gray, and the dashed line marks the 1-to-1 relation.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: The rotation–effective temperature sequence of α Per (79 Myr) compared against other benchmark clusters. Possible photometric, astrometric, and visual binaries have been removed (see Section 6.1). This selection against binaries significantly decreases the number of stars on the fast sequence. The 670 Myr sequence comprises stars from Praesepe (Rampalli et al. 2021), the 300 Myr sequence of NGC 3532 (Fritzewski et al. 2021) and Group X (Messina et al. 2022), and the 120 Myr sequence of Blanco 1 (Gillen et al. 2020), the Pleiades (Rebull et al. 2016), and Pisces-Eridani (Curtis et al. 2019b). A solar-metallicity, 0.75M ⊙ star arrives on the ZAMS at ≈80 Myr with T eff ≈ 4700 K.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption:  α Per’s position in XY space. Galactic rotation is in the ﹩+\hat{Y}﹩ direction, and the galactic center is in the ﹩+\hat{X}﹩ direction. Each study’s selection of α Per members are plotted in the panels around the outside, while the center panel shows all samples combined. Gray points represent cluster members for which rotation periods were expected to be detectable, while black points represent stars that are rotationally consistent with α Per membership.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: Absolute magnitude as a function of color for K and M-dwarfs in α Per, IC 2602, the Pleiades, and the field (gray). The Pleiades is elevated off of the main sequence, indicating that it is still on the pre-main sequence, while α Per and IC 2602 are elevated above the Pleiades, indicating that both clusters are younger than the Pleiades.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: Positions, velocities, and color–absolute magnitude diagram (CAMD) for α Per. The Sun is spatially located at the origin and is represented by the ⊙ symbol. The gray points represent candidate α Per members from the literature while the black points represent stars that comprise our sample of benchmark rotators. See Section 6.1 for details on how the sample of benchmark rotators was created.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: An image of α Per taken from DSS. The image is ∼4° across, which corresponds to ∼24 pc at the distance of the cluster’s core. The image is oriented so equatorial north is up and east is left. Reported α Per members in the literature span ∼100° on the sky, far beyond the extent of this image.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: Rotation sequences of the Pleiades and α Per plotted with the 100 Myr gyrochrone from Spada & Lanzafame (2020), a sixth-order polynomial fit to the Pleiades slow sequence, and our model fit to α Per’s slow sequence. The model is extended to 4500 K even though α Per’s slow sequence breaks down at temperatures lower than 5000 K.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption:  α Per’s position in YZ space. Galactic rotation is in the ﹩+\hat{Y}﹩ direction. Points are the same as in Figure 6.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption:  α Per’s position in XZ space. The galactic center is in the ﹩+\hat{X}﹩ direction. Points are the same as in Figure 6.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: The rotation–effective temperature sequence for α Per with different choices of selection function. Upper left: α Per members selected using the brightness, internal consistency, periodogram strength, S/N, and external criteria described in Section 4 (flag_quality_period). Upper right: α Per members selected using the same criteria as the upper-left panel but that pass our manual check (manual_check = g). Lower left: Same as upper-left panel except with binaries removed according to the criteria described in Section 6 (flag_benchmark_period). Lower right: α Per members that compose our sample of stars used to calibrate gyrochronology as described in Section 6.1 (in_gyro_sample). This sample has the same binarity requirements as in the lower-left panel, but only consists of stars that pass our manual vetting, have no subpeaks in a periodogram within 70% the height of the main peak, and that lie within ∼30 pc and ∼3 km s−1 of α Per’s core.
Paper: Stellar Rotation and Structure of the α Persei Complex: When Does Gyrochronology Start to Work?
Authors: Andrew W. Boyle, Luke G. Bouma
Figure caption: The mass needed to create a gravitational potential that overcomes the Milky Way’s potential at α Per’s position as a function of distance from the mass.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: S/N spatial detection maps for our pathfinder survey with Keck/OSIRIS, obtained after combining all of the data for each target at this midsurvey stage. The plate scale is 0.02“ per spaxel.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Depth of search for the 20 stars observed in this Keck/OSIRIS survey. The contours denote the number of stars to which the survey is complete for planets and brown dwarfs as a function of separation (in au) and mass (in Jupiter masses). Our survey probes a similar parameter space as extreme adaptive optics surveys of stars in young moving groups (Nielsen et al. 2019), despite our target stars being about three times further away.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Detection limits for all of the 23 targets of the survey as a function of angular separation from the star. The sensitivity is shown in terms of the planet-to-star flux ratio (Kn5 filter) in the upper panel and in terms of the companion mass in the lower panel. The flux to mass conversion was done using a BT-Settl evolutionary grid (Allard 2013) assuming an age of 2 Myr. The detection threshold was chosen to 8 × σ  p  accounting for the non-Gaussianity of the S/N residuals. This threshold matches an equivalent false-positive rate of a 5 × σ threshold, assuming a Gaussian distribution.
Paper: Detecting Exoplanets Closer to Stars with Moderate Spectral Resolution Integral-field Spectroscopy
Authors: Shubh Agrawal, Jean-Baptiste Ruffio, Quinn M. Konopacky, Bruce Macintosh, Dimitri Mawet, Eric L. Nielsen, Kielan K. W. Hoch, Michael C. Liu, Travis S. Barman, William Thompson, Alexandra Z. Greenbaum, Christian Marois, Jenny Patience
Figure caption: Sensitivity of Keck/OSIRIS at Kn5 (solid/dash) compared with K-band sensitivities of other direct-imaging surveys (dot/dashed–dotted). LkCa 15 (purple) and ROXs 43B (red) illustrate the median sensitivity of the survey, while the best performance was achieved for AB Aurigae (green) and Em* SR 3 (blue).
Paper: The Absolute Age of M92
Authors: Jiaqi (Martin) Ying, Brian Chaboyer, Emily M. Boudreaux, Catherine Slaughter, Michael Boylan-Kolchin, Daniel Weisz
Figure caption: An illustration of the 20,000 13 Gyr MC isochrones (gray) generated for this project. The red curve is the interpolated isochrone which is selected by taking the median F606W-F814W value of all isochrones at a given F606W value. The corresponding 68% confidence intervals and 95% confidence intervals are shown in blue and green curves, respectively.
Paper: The Absolute Age of M92
Authors: Jiaqi (Martin) Ying, Brian Chaboyer, Emily M. Boudreaux, Catherine Slaughter, Michael Boylan-Kolchin, Daniel Weisz
Figure caption: The cumulative distribution of the minimum χ 2 values for all MC isochrones.
Paper: The Absolute Age of M92
Authors: Jiaqi (Martin) Ying, Brian Chaboyer, Emily M. Boudreaux, Catherine Slaughter, Michael Boylan-Kolchin, Daniel Weisz
Figure caption: Top left (a): an example of a “high probability fit” for M92. The χ 2 value is within 1σ of the mean of the empirical distribution. Blue dots are parts of the sCMD and red dots are observed data for M92. Top Right (b): an example of “low probability fit” for M92. The χ 2 value is almost 3σ greater than the mean of the empirical distribution. Blue dots are parts of the sCMD and red dots are observed data for M92. Bottom left (c): an example of “high probability fit” for M92. The size of the blue dots indicates the χ 2 value for the Voronoi bin they located at. Bottom Right (d): an example of “low probability fit” for M92. The size of the blue dots indicates the χ 2 value for the Voronoi bin they located at.