adsabs/AstroCLIMB huggingface dataset:
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Lick 3 m POLISH2 UBV and clear bandpass measurements of telescope polarization from 2011 to 2021. Telescope polarization is typically p ∼ 100 ppm (0.01%) with an orientation of Θ ∼ 30°.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: The association rate of the WGOs in each group with five kinds of masers (methanol Class I/II, H2O, OH, and SiO; upper panel). N associated is the number of the WGOs associated with the maser. N total is the total number of WGOs in each group. The red, blue, and green bars represent Groups 1, 2, and 3 respectively. The lower panel is the association rate of WGOs with the cumulative number of masers (≥N fig6). N associated in this panel is the number of WGOs associated with at least N fig6 masers. The inset in panel (b) shows the change of association rate between each group of WGOs and the cumulative number of masers.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Distribution of WGOs, EGOs, and Hi-GAL sources in the Galactic plane. Green circles represent WGOs; red and blue circles represent EGOs identified by Cyganowski et al. (2008) and Chen et al. (2013) respectively. The gray points show the Hi-GAL compact sources (Elia et al. 2021). The coverage of GLIMPSE I and II surveys are shaded in red and blue, respectively.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Panel (a) is the number distribution of WGOs as a function of Galactic longitude in 5° bins. The locations of giant molecular clouds are indicated by red arrows. Panel (b) shows the number distribution of WGOs as a function of Galactic latitude in 0.°1 bins and fitted with a Gaussian curve. The red vertical line denotes the peak position of the Gaussian curve.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Accretion rate versus protostellar mass. Red circles, blue squares, and cyan crosses represent WGOs in groups 1, 2, and 3, respectively. The WGOs listed in Tables 2 and 3 are located in the deep blue and light yellow areas, respectively. The green dotted line marks the mass equal to 1 M ⊙, and almost all MYSO candidates are above this line.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Flow chart describing the identification procedure of WGOs.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: An example of SED fitting. Photometric data from WISE and Hi-GAL were fitted using the YSO models of Robitaille (2017). Black and gray lines represent the best fit and good fit that satisfy ﹩{\chi }^{2}\mbox{--}{\chi }_{\mathrm{best}}^{2}\lt 3{N}_{\mathrm{data}}﹩, where N data is the number of data points. The P(D∣M) score of this fitting is 4.564.
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: The distribution of WGOs in the Galactocentric system. The axes are Galactocentric distances. We mark the WGOs of three different groups with green, yellow, and black crosses, respectively. The background image is a sketch of the galaxy produced by Robert Hurt (artist's concept, R. Hurt: NASA/JPL-Caltech/SSC). The position of the Sun is shown by the red circle above the Galactic midplane. The two solid white lines enclose the inner Galactic plane (∣l∣ < 60°).
Paper: WISE Green Objects (WGOs): The Massive Star Candidates in the Whole Galactic Plane (∣b∣ < 2°)
Authors: Chang Zhang, Guo-Yin Zhang, Jin-Zeng Li, Jing-Hua Yuan
Figure caption: Morphology of the exemplary WGOs. Panels (a), (b), and (c) represent groups 1, 2, and 3. Panels (a1), (b1), and (c1) are trichromatic maps of emission at 3.4, 4.6, and 12 μm, rendered in blue, green, and red. Panels (a2), (b2), and (c2) are W2/W1 ratio maps. Panels (a3), (b3), and (c3) show 22 μm images. The black cross marks the center of each WGO.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Top left: SiO(1−0) integrated intensity in 18553 shown in color and black contours. The black contours represent the [−3, 3, 3.5, 4.5, 5.5]  × σ SiO levels, with σ SiO = 18  mJy beam−1 km s−1. The white contours show the 7 mm continuum emission and represent the [−3, 3, 5, 7, 9, 9.3]  × σ 7 mm levels, with σ 7 mm = 91.2 μJy beam−1. The white cross marks the position of the radio continuum source, and the white ellipse in the bottom left represents the synthesized beam sizes. Top right: CS(1−0) integrated intensity shown in color and black contours. The latter represent −25%, 25%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 676 and 107 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and are the same as in the left panel. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam size, respectively. In both top panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow direction. Bottom: spectra of the SiO (×5) and CS J = 1–0 line emission shown in blue and red, respectively. The former was obtained integrating over both SiO knots, while the latter represents the entire emission surrounding C 1 and enclosed in the 35% contour level. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Top left: SiO(1−0) integrated intensity in 18345 shown in color and black contours. The latter represent the [−3, 3, 3.5, 4, 4.7]  × σ SiO levels, with σ SiO = 20.8  mJy beam−1 km s−1. The white contours are the same as in Figure A1 left and show the 7 mm continuum emission. The white cross marks the position of the radio continuum source. The filled, white ellipse in the bottom left represents the SiO and 7 mm continuum synthesized beam size. Top right:  CS(1−0) integrated intensity in 18345 shown in color and black contours. The black contours represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 490 and 108 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and are the same as in Figure A1 (left), while the outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam size, respectively. In both top panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow directions. Bottom: spectra of the SiO (×5) and CS J = 1–0 emission in 18345 shown in blue and red, respectively. The spectra were obtained integrating over the entire emission that appears to be connected to C 1. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left: SiO(1−0) integrated intensity in 18517 shown in color and black contours. The latter represent the [−3, 3, 3.5, 4, 4.5] × σ SiO levels, with σ SiO = 18.1  mJy beam−1 km s−1. The white cross shows the position of the radio continuum source, and the white ellipse in the bottom left represents the synthesized beam size. The white contours show the 7 mm continuum emission and are the same as in the left panel of Figure A5. Right: CS(1−0) integrated intensity in 18517 shown in color and black contours. The black contours represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 600 and 147 mJy beam−1 km s−1, respectively. The white contours are the same as in the left panel, while the outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam sizes, respectively. In both panels the field of view is the same, and the green lines were drawn to guide the reader on the possible flow directions.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as the left panel of Figure A1, but for 19012. The red square and × mark the positions of the 22 GHz water maser and 25 GHz methanol emission from Beuther et al. (2002b) and Sanchez-Tovar et al. (2022), respectively. Note the different color scales and contour levels used in each panel.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left:  CS(1−0) integrated intensity in 18440 is shown in color and black contours. The latter represent −35%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 255 and 92 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and are the same as in Figure A3 (left). The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam size, respectively. Right: spectrum of the CS(1−0) line emission in 18440, obtained integrating over the entire emission enclosed by the 35% contour level from the left panel. The vertical dotted line marks the systemic velocity.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1, but for 18440. The red circle shows the position of the 6.7 GHz methanol maser from Beuther et al. (2002b).
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1, but for 18517. The red cross and diamonds in the left panel mark the positions of the 25 and 44 GHz methanol emission from Sanchez-Tovar et al. (2022) and Rodríguez-Garza et al. (2017).
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1 but for 18553. The red square, diamond, and × mark the positions of the 22 GHz water maser, 44 GH methanol maser, and 25 GHz methanol emission from Beuther et al. (2002b), Rodríguez-Garza et al. (2017), and Sanchez-Tovar et al. (2022), respectively.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left: spectra of the SiO (×5) and CS emission in 18517 shown in blue and red, respectively. The spectra were obtained integrating over the entire emission that appears to be connected to C 1. The vertical dotted line marks the systemic velocity. Right: Spitzer IRAC color composite, showing the 3.6 (blue), 4.5 (green), and 8.0 μm (red) emission. The blue and magenta contour levels show the 7 mm continuum emission and SiO integrated intensity, respectively, and are the same as in the left panel of Figure A6. The black × marks the position of the radio continuum source.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Left: CS(1−0) integrated intensity map shown in color and black contours. The latter represent −25%, 35%, 55%, 75%, and 95% of the peak CS(1−0) emission, with the peak emission and rms of the map being 291 and 113 mJy beam−1 km s−1, respectively. The white contours show the 7 mm continuum emission and represent [−2.5, 2.5, 3, 4, 4.5, 5, 5.5]  × σ 7 mm, with σ 7 mm = 98.2 μJy beam−1. The outlined and filled white ellipses in the bottom left represent the CS and 7 mm continuum synthesized beam size, respectively. Right: spectrum of the CS(1−0) line emission in 20343, obtained integrating over the entire emission enclosed by the 35% contour level from the left panel. The vertical dotted line marks the systemic velocity.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: The prior on the SFR implied by taking uniform priors over the double-power-law SFH parameters ﹩({\mathrm{log}}_{10}\alpha ,{\mathrm{log}}_{10}\beta ,\tau )﹩ over the ranges specified in Table 2 is shown in blue, while the target prior (specified by the SFS measurement of Leja et al. 2022) is shown in orange. The SFR prior obtained by recalibrating the baseline prior with a normalizing flow (as described in Section 3.2.3) is shown by the black dotted line, giving excellent agreement with the target SFS prior.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Magnitude uncertainties vs. magnitudes for the GAMA data (left panels) vs. the trained MDN model for the error distribution conditioned on flux (right panels). Note that the magnitudes in both the left and right panels are MAP magnitudes, from an initial fit of the SPS model to the GAMA galaxies, as described in Section 3.4.
Paper: Searching for Molecular Jets from High-mass Protostars
Authors: Tatiana M. Rodríguez, Peter Hofner, Isaac Edelman, Esteban D. Araya, Viviana Rosero
Figure caption: Same as Figure A1 but for 20343. Note the different color scale and contour levels used in the continuum images.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: SFS prior on the SFR (in units of M ⊙yr−1) conditioned on mass and redshift, based on the measurement from Leja et al. (2022; see Appendix B for details). The vertical lines represent the mass-complete limit for the three-dimensional HST data on which the Leja et al. (2022) fit was performed; we extrapolate the SFS below the mass limit, as shown in the images.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: FMR priors on gas-phase metallicity conditioned on mass and specific SFR (in units of Gyr−1). The solid lines represent the mean, and the bands show the FWHMs of the assumed student-t distribution.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Left: the redshift-evolving mass function from Leja et al. (2020). Right: the implied redshift distribution for the background galaxy population (without selection) at M = 1010 M ⊙.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Prior on the diffuse dust attenuation conditioned on SFR. The solid line shows the mean and the bands show the 1σ and 2σ contours.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Magnitude errors vs. magnitudes for the VVDS data (left panels) vs. the trained MDN model for the error distribution conditioned on flux (right panels). Note that the magnitudes in both the left and right panels are MAP magnitudes, from an initial fit of the SPS model to the VVDS galaxies, as described in Section 3.4.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: The bias on the mean redshifts of the model redshift distributions vs. the data for GAMA, Δz = 〈z model〉 − 〈z data〉. The distributions are obtained by bootstrapping samples from the model n(z), taking a kernel density estimate of the bootstrapped sample means, then centering the kernel density estimate on the difference between the sample mean of the spec-zs and the mean of the model n(z).
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: The bias on the mean redshifts of the model redshift distributions vs. the data for VVDS, Δz = 〈z model〉 − 〈z data〉. The distributions are obtained by bootstrapping samples from the model n(z), taking a kernel density estimate of the bootstrapped sample means, then centering the kernel density estimate on the difference between the sample mean of the spec-zs and the mean of the model n(z).
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Samples from the prior on the SFR implied by taking uniform priors over the double-power-law SFH parameters ﹩({\mathrm{log}}_{10}\alpha ,{\mathrm{log}}_{10}\beta ,\tau )﹩, over the ranges specified in Table 2, are shown as the blue histograms, while the learned normalizing flow model for the implied distribution (as a function of redshift) is shown in orange.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Tomographic redshift distributions obtained by the forward model (blue) compared to histograms of the GAMA spectroscopic redshifts (orange). The model predictions are in excellent agreement with the distributions of the spectroscopic redshifts.
Paper: Forward Modeling of Galaxy Populations for Cosmological Redshift Distribution Inference
Authors: Justin Alsing, Hiranya Peiris, Daniel Mortlock, Joel Leja, Boris Leistedt
Figure caption: Tomographic redshift distributions obtained by the forward model (blue) compared to histograms of the VVDS spectroscopic redshifts (orange). The widths of the histogram bars indicate the ﹩\pm \sqrt{N}﹩ Poisson noise. The model predictions are in excellent agreement with the distributions of the spectroscopic redshifts.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Same as Figure 5 but for R3 (top) and R4 (bottom). Both have an adiabatic index ﹩\hat{\gamma }=5/3﹩ and differ by r max and the value of β 0.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Left: logical Cartesian grid in MKS coordinates (t, q 1, q 2, q 3) used for the numerical computation. Right: corresponding grid in spherical KS coordinates. For the clarity of the figure, the resolution is reduced to ﹩{N}_{r}={N}_{{q}^{1}}=128﹩ and ﹩{N}_{\theta }={N}_{{q}^{2}}=32﹩, and only a few cells of q 1 are shown. The red line represents the outer horizon ﹩{r}_{H}^{+}﹩. The q 3 (so also the ϕ) component is outside of the plane and not shown. Here ﹩{\bar{q}}^{1}=\mathrm{log}(1+\sqrt{1+{a}^{2}})﹩. Finally the blue square shows the correspondence between both grids. In this figure and the others, ﹩x=r\sin (\theta )﹩ and ﹩z=r\cos (\theta )﹩.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Accretion diagnostics at the horizon. Top left: Accretion rate ﹩\dot{M}﹩, given by Equation (43). Top right: MAD parameter, given by Equation (44). Bottom left: Angular momentum through the horizon, given by Equation (45). Bottom right: Energy flux, given by Equation (46). The horizontal lines represent the time average for time between 5000M and 104M, whose value is given in the legend of each plot and with its 2σ variation in Table 2. Runs with different resolutions only, that is to say, R1–R2 and R5–R6, are shown in the same subfigure. We note that the vertical scaling of each subfigure varies.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Time and azimuthal averages of the density (left), β (middle), and σ (right) for R1 (top) and R2 (bottom). The black thick line in the middle and right plots shows β = 1 and σ = 1. The red line in the right plots represents z = x 1.6, which describes the surface σ = 1 in force-free models.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Same as Figure 5 but for R5 (top) and R6 (bottom). Both runs assume the initial disk configuration expected for an adiabatic index ﹩\hat{\gamma }=5/3﹩, yet evolve using ﹩\hat{\gamma }=4/3﹩. They do not reach a steady state at the end of the simulation time.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Left: Time-averaged mass accretion rate as a function of radius r for different time intervals. Right: Time-averaged angular momentum flux as a function of radius. The pink region corresponds to the 2σ variance during the last time interval, 8000M < t < 104M. From this figure, it is clear that at the end of our run, a quasi-steady state up to radius r = 10M has been reached for R1, R2, R3, R7, and R8 and is only marginally achieved for the remaining runs.
Paper: cuHARM: A New GPU-accelerated GRMHD Code and Its Application to ADAF Disks
Authors: D. Bégué, A. Pe'er, G.-Q. Zhang, B.-B. Zhang, B. Pevzner
Figure caption: Correlation between the initial torus mass M and the quasi-steady-state mass accretion rate. The slope of the fit is 0.84.
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Left: Absolute value of B-band circular polarization ∣v∣ vs. degree of linear polarization p obtained with POLISH2 at Gemini North (open stars), the Lick 3 m (filled circles), and the Lick 1 m (open circles). Stars with circular polarization detected with at least 3σ confidence are plotted in large, colored stars or circles and labeled in the legend. The dashed lines indicate circular polarization scaling with the degree of linear polarization with 1:1 and 1:100 ratios. Right: Same as the left panel but for the clear POLISH2 bandpass.