adsabs/AstroCLIMB huggingface dataset:
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 angle-averaged Lorentz factor of the jet (defined by σ > 1) for the same simulations, as a function of radius.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The location of the sample selection on the Gaia color–magnitude diagram. In all panels, scatter points and the overlaid two-dimensional histogram show the stellar density of the Gaia 200 pc background sources. (a) The red solid lines show the color-cut range that we defined, using the lower edge of the MS as an upper limit and the upper edge of the WD cooling sequence as a bottom limit, and using a color-cut G BP − G RP < 1.0 as a right color limit. The blue dashed lines show a color-cut and absolute magnitude selection scheme for searching hot subdwarfs using Gaia data proposed by Geier et al. (2019). The green dashed lines show the color–magnitude diagram selection scheme for searching ELM-WD candidates based on Gaia DR2 data by Pelisoli & Vos (2019). (b) The red scatter points show all samples under the initial query conditions. (c) The red scatter points show the variable samples after using the Gaia variability metric select condition. (d) The red scatter points show the final binary samples after examining ZTF light-curve data.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Empirical Gaia variability metric as a function of G-band magnitude for all initial samples, with the exponential fit proposed by Guidry et al. (2021) for Gaia EDR3 delineated in green. The 1.5% most variable samples are marked in red, and 15 ultracompact binaries reported by Burdge et al. (2020a) are marked as blue stars.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The VARINDEX and G-band magnitude of the 12,480 candidates after Gaia variability cut. The green dashed line shows that 1.5% of most variable samples have VARINDEX > 0.00. The gray dashed line shows El-Badry et al. (2021b) used VARIANDEX > 0.02 to cut the samples in search of evolved CVs. The 1.5% most variable samples are marked in red, and 15 ultracompact binaries reported by Burdge et al. (2020a) are marked as blue stars.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The corner plot for the main parameters of different types of light-curve shapes of binaries within our binary sample. In panels (a), (c), (f), and (j), we show the one-dimensional histogram over Gaia BP-RP color, the Gaia G-band apparent magnitude, the distance, and the orbital period, respectively. The other panels ((b), (d), (e), (g), (h), and (i)) show the correlation distribution between the two parameters for different types of binaries.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Characteristic GW strain of the sources described in this work (shown as colored diamonds), compared with the samples of candidate VBs from Huang et al. (2020; shown as gray squares) and Burdge et al. (2020a, 2020b), Kilic et al. (2021), and Chandra et al. (2021; shown as gray thin diamonds), overplotted with LISA sensitivity curve (solid black line) and TianQin sensitivity curve (solid red line).
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Sky distribution in equatorial coordinates of the variable sample (gray dots) and the binary sample (colored dots). The black circles show the potential GW source candidates.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Examples of the variability types of light-curve shapes caused by the binary eclipse effect in our binary sample. All panels show the frequency spectra of the BLS and CE corresponding to the above (Figure 5) variability types of the ELL-type binary and reflection binary.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Examples of the variability types of light-curve shapes caused by the binary eclipse effect in our binary sample. All panels show the frequency spectra of the BLS and CE corresponding to the above (Figure 5) variability types of the HW Vir binary and EA-type binary.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Examples of the variability types of light-curve shapes caused by the binary eclipse effect in our binary sample. All panels show the frequency spectra of the BLS and CE corresponding to the above (Figure 5) variability types of the EB-type binary and EW-type binary.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Phase-folded ZTF light curves of the potential GW candidates with an orbital period of less than 100 minutes, at GW amplitude and TianQin/LISA S/Ns for these candidates as described in Section 6.4.
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: POLISH2 QE curves for the blue-sensitive Hamamatsu H10721-210 SEL (dotted curves) and the red-sensitive H7422P-40 SEL PMTs (solid curves). These are convolved with Bessel UBVR bandpasses and are also shown with clear, unfiltered bandpasses. The R bandpasses are illustrative, as POLISH2 has not obtained R-band measurements to date.
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: POLISH2 optical layout.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Histogram of the corrected antenna temperature for all voxels in COHRS, displayed on a logarithmic scale. The bin width is 0.1 K. The red curve shows a Gaussian fit to the distribution described by ﹩1.14\,\times {10}^{9}\,\exp \left(-\tfrac{1}{2}{({T}_{{\rm{A}}}^{* }-0.032)}^{2}/{0.49}^{2}\right)﹩. The inset shows the same distribution on a linear scale.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Histogram of the noise for all pixels in COHRS, displayed on a logarithmic scale. The bin width is 0.02 K. A dotted vertical line indicates the mean value of noise levels across the survey. The inset shows the same data on a linear scale.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Examples of the variability types of light-curve shapes caused by the binary eclipse effect in our binary sample. (a) HW Vir-type binary, in which a low-mass MS star (M dwarf) orbits a core helium-burning sdO/sdB primary nearly edge-on (El-Badry et al. 2021b). (b) EA-type eclipsing binary, the unique shape of light curves is that between eclipses the light remains almost constant or varies insignificantly, and the light curves showing two minima per cycle or secondary minima may be absent. (c) EB-type eclipsing binary, showing two minima per cycle, and secondary minimum depth usually being considerably smaller than that of the primary minimum. (d) EW-type eclipsing binary, consisting of ellipsoidal components almost in contact, and the depths of the primary and secondary minima of the light curves are almost equal or differ insignificantly. (e) ELL-type binary, the light-curve shape has the characteristics of quasi-sinusoidal variability produced by tidal deformation and shows two different minima in one orbit. (f) Reflection binary, in which an M dwarf orbits a hot white dwarf and is heated on one side (El-Badry et al. 2021b).
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The location of the binary samples on the Gaia H-R diagram. The blue dashed lines show our selection scheme for searching CWDBs based on Gaia EDR3 data. The red dashed lines show the selection rule proposed by Geier et al. (2019) based on Gaia DR2 data to search the population of hot subdwarfs. The black dashed lines show the selection scheme proposed by Pelisoli & Vos (2019) based on Gaia DR2 data to search ELM-WD candidates. The solid red line is the cooling model offset by −0.75 mag for the 0.21M ⊙ and 0.69M ⊙ white dwarf. We use the publicly available WD_models package provided by Cheng et al. (2020). The black scatter points show the Gaia 200 pc background sources. The five differently colored scatter points show the different types of light-curve shapes in the final binary samples searched using ZTF data, and the black circles show the binaries in the binary sample whose periods are less than 100 minutes, which are potential GW source candidates.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The pie chart of the percentage of binaries with the different types of light-curve shapes in our binary sample.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The light curves of ZTF J161133.96+630831.67. The top panel shows the raw ZTF g-band (dark cyan), r-band (dark red), and i-band (black) light curves, and raw CSS (dark orange) photometric data. The middle panels show the phased ZTF light curves for the g band, r band, and i band, and the phased CSS light curve, respectively. The bottom panel shows the phase-folded light curves of ZTF J1611+6308 at phase ϕ ∼ 0.975–1.025 in the eclipse duration. The blue dashed lines show the duration of the conjunction of the eclipse, and the black dashed lines show the entire duration of the eclipse from ingress to egress. Archival ZTF (g, r, and i band) and CSS light curves of the system are folded at a period of 49.708 minutes.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The light curves of ZTF J181311.10+425150.51. The top panel shows the raw ZTF g-band (dark cyan), r-band (dark red), and i-band (black) light curves, and raw CSS (dark orange) light curves. The middle and the bottom panels show the phased ZTF (g band, r band, and i band), and phased CSS light curves for ZTF J1813+4251, respectively. Archival ZTF (g, r, and i), and CSS light curves of the system are folded at a period of 51.161 minutes.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The light curves of ZTF J011242.48+582757.60. The top panel shows the raw ZTF g-band (dark cyan) and r-band (dark red) light curves. The middle and bottom panels show the phase-folded light curves for ZTF J0112+5827 in the g and r bands, which show a clear difference between the two bands. The r band exhibits two obvious spikes in one phase; between two spikes there is a transit phase.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The light curves of ZTF J235115.32+630528.23. The top panel shows the raw ZTF g (dark cyan), r (dark red), and i (black) light curves. The middle and bottom panels show the ZTF g-band and r-band folded light curves, respectively. Archival ZTF g-band and r-band light curves of the system are folded at a period of 42.985 minutes.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: Examples of the variability types of light-curve shapes caused by the binary eclipse effect in our binary sample. Panels (a)–(f) show the frequency spectra of the LS periodogram corresponding to the variability types of the phase-folded ZTF light curve listed in Figure 5.
Paper: A Systematic Search for Short-period Close White Dwarf Binary Candidates Based on Gaia EDR3 Catalog and Zwicky Transient Facility Data
Authors: Liangliang Ren, 亮亮 任, Chengyuan Li, 程远 李, Bo Ma, 波 马, Sihao Cheng, 思浩 程, Shun-Jia Huang, 顺佳 黄, Baitian Tang, 柏添 汤, Yi-ming Hu, 一鸣 胡
Figure caption: The pie chart of the percentage of binaries for particular variability classes in our variable sample.
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: Simultaneous linear and circular polarimetry of the daytime sky above the Lick 3 m measured with POLISH2 while the Cassegrain rotator was continuously rotated. Top: Linear polarization (Stokes q and u) varies sinusoidally as a function of the polarization orientation ﹩{\rm{\Theta }}={\mathtt{atan}}{\mathtt{2}}({\mathtt{u}},{\mathtt{q}})﹩. Middle: Circular polarization (Stokes v) varies sinusoidally as a function of Θ, which must be due to instrumental crosstalk (blue points) as intrinsic circular polarization is invariant under rotation. Utilization of the POLISH2 Mueller matrix (yellow curve, Equation (16)) yields the corrected circular polarization (red points). Note the factor of ∼100 scale difference between the top and middle panels. Bottom: The residual circular polarization has a standard deviation of 0.02%.
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: Gemini North POLISH2 B-band measurements of the exoplanet hosts HD 189733 and WASP-12, the nearly unpolarized HR 8585, and the strongly polarized HD 204827. WASP-12 was observed on 2016 November 12–14 UT, while the others were observed on 2018 August 2–7 UT. Data are aggregated over all nights of each run and fit by Equations 20(a) and (b). Left: The intrinsic stellar polarizations q * (top) and u * (middle) are included, which manifest as constant offsets with respect to parallactic angle. Right: Stellar polarization is removed to isolate telescope polarization. The intrinsic and telescope-induced circular polarization are conflated (bottom). Note the change in scale in the bottom panel.
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: FFT of raw Lick 3 m POLISH2 observations of incandescent flat-field lamp light reflected by the inside of the closed dome. The frequencies of significant FFT peaks are labeled. The presence of incident Stokes Q is exposed by the power at 100 and 200 kHz (dashed, red lines), while all other harmonics at and above 10 kHz indicate Stokes U. The peaks below 1 kHz are due to intrinsic flicker of the lamp and dimmer circuit due to the United States power grid.
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: POLISH2 lab measurements of light injected through two sequential, linear polarizers as the upstream polarizer rotates continuously. For an opening angle of 90°, the two polarizers are crossed. Two ideal polarizers would show constant Stokes q, u, and v = 0 as the opening angle varies, so observed discontinuities in the Stokes parameters require crosstalk intrinsic to the polarizers. The right panels zoom in on the discontinuity observed when the polarizers are perfectly crossed, and the vertical scale is maintained between the left and right panels.
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: POLISH2 Mueller matrix elements indicating crosstalk measured during continuous rotation of the Lick 3 m Cassegrain rotator under the daytime sky. Unwanted instrumental conversion of Stokes u to v, indicated by m 43, is plotted against Stokes q to v conversion m 42. A linear fit to the data indicates a striking, wavelength-dependent trend (dashed line).
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: Simultaneous measurement of the linear (Stokes q and u) and circular polarization (Stokes v) obtained in the lab with POLISH2 by injecting light through a rotating linear polarizer (LP) and a quarter-wave Fresnel rhomb in series. This polarization modulation is measured in real time during the ∼1.5 minutes long polarizer rotation. Data points are binned every 0.9 s, and the solid curves represent fits to Equations 11(a)–(c).
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: Top: Laboratory Fresnel rhomb orientation calculated from the relative amplitude of Stokes q and u measurements via Equation (13). The best-fit line, Θ = (−5.°726 ± 0.°050) × Θmicrometer + (5.°783 ± 0.°028), is shown in red. Bottom: The residuals to the linear fit are shown, and the standard deviation of the residuals is only 0.°035.
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: Gemini North POLISH2 B-band measurements of the exoplanet host WASP-12 on three successive nights, which highlights the repeatability of self-calibration of telescope polarization.