adsabs/AstroCLIMB huggingface dataset:
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 distribution of χ 2 values found using Equation (3) when comparing the sCMDs to the observed data. The empirical χ 2 distribution is shown in red, and the χ 2 values found when fitting the M92 data to the MC isochrones are shown as a function of age (scale shown on the right vertical axis). The 1100 isochrones which are within 3σ of the mean of the empirical distribution are shown as blue dots. The remaining isochrones have χ 2 > 4100 and are shown as gray dots. Note that the x-axis is on a logarithmic scale.
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 empirical χ 2 distribution is shown in red, while the χ 2 values determined from fitting the MC isochrones to M92 are shown in blue (as a function of age). Only the 1100 isochrones which are within 3σ of the mean of the empirical distribution are shown in this figure. The x-axis is in linear scale.
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 best-fit age corresponding to each combination of distance modulus and reddening. The annotation on each block represents the estimated age (Gyr) from each combination. The color represents the occurrence of each combination as a percentage of the total 1100 best-fit isochrones. 78 out of the 1100 best-fit isochrones choose distance modulus =14.71 and reddening = 0.0 with an estimated age of 13.78 Gyr.
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 distribution of mixing length as an input parameter (see Table 1). The solar-calibrated mixing length used as the median set of MC parameters is 1.75.
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 weighted distribution of ages corresponding to best-fit isochrones (blue histogram). The orange curve represents the best-fit Gaussian model, ﹩{ \mathcal N }(13.80,0.75)﹩. The 95% confidence interval of the estimated age is ﹩\left(12.4,15.4\right)﹩ Gyr.
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 example of the result of the adaptive Voronoi binning method (Cappellari & Copin 2003). The CMD is divided into 800 different subsets. Blue dots are the 180,000 data points used to generate the Voronoi tessellation. The red curve is the isochrones used to simulate the CMD.
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 function of the χ 2 values which are higher than the mean of the empirical χ 2 distribution while being within 3σ of the mean of the empirical distribution.
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 distribution of the weight p for 20,000 sets of MC isochrones.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: The aCXB gradient model incorporated in nuskybgd for FPMA (left) and FPMB (right). The red squares represent the locations of each detector including some padding inside the entire 360 × 360 pixel focal plane defined by DET1 coordinates (left column of Figure 4). Each image ranges in pixel value from ∼440 mm2 (dark blue) to ∼370,000 mm2 (yellow). These areas scale with the solid angle visible to each pixel and correspond to the area projected onto the optics bench plane.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Mollweide projection in Galactic coordinates displaying the qualifying observations and overall total exposure time for the Blank Sky list (top) and the Full Sky list (bottom). The toroidal shapes of the points reflect the summed area of the sky visible to both telescopes A and B by stray light.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Left panels: light curves binned in 100 s intervals, shown with the best model fit (solid blue line). Right panels: histograms showing the distribution of residual bin values around the best-fit line, fitted by a Gaussian curve. The 3.5σ filtering thresholds are shown as green lines on either side of the distribution; red bins indicate those time intervals removed from the GTI file. The top and bottom panels show ObsID 50002019004 (FPMA) and ObsID 60001068002 (FPMB), respectively.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Left and middle columns: stacked science data in the 3–12 keV energy band with the Full Set ObsID list for FPMA (top) and FPMB (bottom) for a total exposure time of ∼18.53 Ms and ∼18.46 Ms respectively. The left images show raw stacked counts, and the middle images are exposure-corrected versions with the maximum exposure time normalized to 1. Right column: stacked exposure maps for all observations used with this source list.
Paper: The Absolute Age of M92
Authors: Jiaqi (Martin) Ying, Brian Chaboyer, Emily M. Boudreaux, Catherine Slaughter, Michael Boylan-Kolchin, Daniel Weisz
Figure caption: Contributions to the error of the age of M92 from each Monte Carlo parameter with distance modulus and reddening. The covariance and parameters that contribute less than 0.05% (i.e., less than 1% of the total error budget) are combined as “others”. All the errors are converted to the percentage of the age of M92. The black dotted line represents the combined age error of 5.43%.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Combined images from telescopes A and B in the energy band of 3–30 keV displaying examples of exclusion regions based on the source-detection program described in Section 3.1. Left to right, top to bottom displays the smallest to largest sources found that qualified for this study with an observation ID and radii given, in pixels, 60101101002 at 47.85 pixels, 60001134002 at 56.65 pixels, as 90201019002 at 108.35 pixels and 60102051006 at 155.65 pixels, 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: Distribution (bottom panels) of the four parameters with >1% (or ≳140 Myr) contribution to the age error from Figure 13 and their correlation with the measured age (top panels). Orange histograms represent the input distribution corresponding to Table 1 and blue histograms show the distribution of corresponding MC parameters from the 1100 best-fit 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: The distribution of mixing length from the 1100 sets of best-fit isochrones for all three models of atmosphere used.
Paper: Measuring the Cosmic X-Ray Background in 3–20 KeV with Stray Light from NuSTAR
Authors: Steven Rossland, Daniel R. Wik, Brian Grefenstette, Nico Cappelluti, Francesca Civano, Fabio Gastaldello, Roberto Gilli, Fiona Harrison, Ann Hornschemeier, Ryan Hickox, Roman Krivonos, Kristin Madsen, Silvano Molendi, Andrew Ptak, Daniel Stern, Andreas Zoglauer
Figure caption: Same as Figure 14 but including the less reliable CXB Measurement measurements up to 40 keV, also placing no a priori constraints on the detector components a 0 through a 3 while including all detectors for both telescopes. Below 10 keV, the CXB Measurement measurements still follow the HEAO 1 measurements closely, while above 10 keV both telescopes display more deviation from the expected CXB shape.
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: Top panel: TESS light curve and our best-fit detrending and transit model for planet b, with illustrations of the possible transit ephemerides of the planet candidate. The orange solid line corresponds to the detrending model using GP, while the transit fitting results are marked in red. The short vertical lines near the bottom illustrate the most probable transit ephemerides of the candidate based on the MAP grid search from RadVel (see Section 4.2.1). Each probable set of ephemerides is marked with two sets of vertical lines: the top set of magenta to cyan colors correspond to an increasing period value as labeled on the right, while the bottom set of yellow to red corresponds to an increasing MAP value. Bottom panel: residuals of the photometric fit. In this panel only the transit events of planet b are marked with small red vertical lines. Note that the time axis is not continuous as there is a 683 day gap with no TESS measurements.
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: The ASAS V-band photometry (top) and its GLS periodogram. The three dashed lines from top to bottom in the lower panel correspond to 1%, 5%, and 10% significance threshold levels, respectively. The maximum signal appears at around 1 day, which is likely an alias due to the observing cadence. No significant signal was identified for the stellar rotation.
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: An example of the two-planet Keplerian orbital model. The period P  c  and RV semiamplitude K  c  are fixed at 34.05 days and 4.1 m s−1, respectively, which is the solution with the highest MAP value among our MAP grid search (see Section 4.2.1). RVs from different instruments are marked with different colors following previous plots: red—PFS, purple and magenta—NRES (indices of 1 and 2 represent the facilities at the South African Astronomical Observatory and Cerro Tololo Inter-American Observatory, respectively), and yellow—CHIRON.
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: The best SED fit for TOI-784. Red symbols represent the observed photometric measurements, where the horizontal bars represent the effective width of the bandpass. Blue symbols are the model fluxes from the best-fit Kurucz atmosphere model (black solid line; Kurucz 1979; Castelli & Kurucz 2003).
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: Zorro high-resolution speckle image contrast limits in both 562 and 832 nm bandpasses. The inserts show the reconstructed images in both bandpasses, highlighting that TOI-784 is a single star to the contrast levels achieved (1.3–77.5 au).
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:  O − C diagram of the TTV analysis, showing the timing of the transit midpoint for each epoch. In total there were 36 transits in our TTV analysis using juliet. We found no apparent TTV signals.
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: SOAR high-resolution speckle image contrast limits in the Cousins I bandpass. The inserts show the speckle auto-correlation function. SOAR did not detect a nearby companion to TOI-784.
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: Phase-folded TESS light curve (light blue) and the best-fit transit model (red line with yellow 1σ band) for planet b, with the residuals plotted in the lower panel. The big circular points show the binned photometry with 40 data points in each bin.
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: The one-planet RV fit with a GP model using RadVel and celerite. The magenta points are the used PFS RVs. The best-fit model is shown by the thin blue line. (b) The RV residuals after subtracting the best-fit GP and Keplerian models. (c) The phase-folded RV plot of TOI-784 b after subtracting the GP model component. Red circles are the same velocities binned in 0.08 units of orbital phase.
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: The joint fit of the TESS light curve and RVs of planet b using pre-2022 PFS RVs with the two best-fit linear trends subtracted. The transit fit is in the left panel, and the RV fit is on the right, with the best-fit model in red solid lines. The white dots circled by blue rings are binned TESS photometric data points with a 40 bin size.
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 the derived parameters in the one-planet RV fit using RadVel.
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 two-planet fit using Juliet. See Section 4.2.2 for more details.
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 P  V /E(B − V) upper limit per IPS-GI field (gray dotted–dashed lines). The red solid line and pink area are the weighted polarization efficiency upper limit and confidence interval in field C16. The light-green dotted–dashed lines are slopes affected by potential outliers in polarization efficiency (see the figure set for more details). The blue and orange solid lines are, respectively, Planck's and Serkowski's limits.
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: Left: polarization efficiency histogram of high-quality IPS-GI data. The cumulative percentage function is shown by the red curve. Dashed lines are the 0.25 (Q 1) and 0.75 (Q 3) quantiles, while the dotted–dashed line shows the 0.5 (Q 2) quantile or median value. Right: polarization degree as a function of the reddening. Upper limits of Serkowski and Planck are represented by the dotted–dashed lines in orange and blue, respectively. The red dotted line is the nonweighted 99th percentile, and the red solid line, with the underlying shaded region, is the weighted calculation with the 68% confidence interval.
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 reddening difference of G19 (left), M06 (middle), and PC16 (right) with Anders22 shown as a function of Anders22's reddening (top row) and distance (bottom row). Only the diffuse fields, i.e., C2, C16, C36, and C37, are used in the PC16 comparison (right; see Table 1 and the explanation in Section 3.2). Red solid lines represent the median value of the difference, and the pink shaded area is the ∼1σ confidence interval delimited by the 16th and 84th percentiles.