adsabs/AstroCLIMB huggingface dataset:
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Left panel: recovered RM vs. injected RM for 5000 simulated compact components before applying the median filter. The red dashed line is the one-to-one line. The extreme outliers are components that are fainter than the local foreground diffuse emission. The inset is a close-up of ϕ ± 20 rad m−2. Right panel: same as the left panel but after applying the median filter. There is an 80% reduction in the most extreme outliers and an overall increase in the accuracy of the recovered RMs of all components.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Total intensity images of the three observations analyzed in this paper. The yellow circles indicate the formed beam footprint, and the green rectangles outline our defined region of uniform sensitivity within which all analysis is performed. Top row: Pilot I EL observation (left) and Pilot I EM observation (right). Bottom row: GL Pilot II observation.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Left: the peak polarized intensity map of the EL observation before applying the median filter. The ripple-like bright patches are presumed to be artifacts of solar interference during observing. Right: the peak polarized intensity map of the EL observation after the application of the median filter with a 120″  box. The median filter is able to completely remove the ripple-like artifacts from the data.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Peak polarized intensity maps from the diffuse cubes (top) and component cubes (bottom) of the GL observation after applying a 120″ median filter. Faint residual diffuse emission can be seen in the component map, particularly on the right half of the image, where the diffuse emission or the polarization angle varies on smaller scales. The unfiltered peak polarized intensity map of the GL observation is shown in Figure 2.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Peak polarized intensity map of the GL observation highlighting extensive diffuse emission present along the line of sight. The green box outlines the region of uniform sensitivity, as per Figure 1.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Scatter in RM as a function of S/Npol for four Faraday depth search limits.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Example Stokes Iqu spectra, polarization angles, and Faraday spectra for a variety of components from our four observations. (a) Median-filtered EL Faraday simple component J221024-505540. Top left: Stokes I spectrum (black) and model fit from 1D RM synthesis with RM-Tools (red dashed). Top center: Stokes q (blue), u (red), and polarized fraction (black) spectra. Top right: polarization angle ﹩\psi ﹩ as a function of ﹩{\lambda }^{2}﹩. Bottom: clean Faraday spectrum (black) with clean peaks (green) and 8﹩\sigma ﹩ GES clean threshold (red dashed). (b) As for 18(a), but in the EM, convolved to the resolution of EL and EC (21 arcsec). (c) As for 18(a), but for the EC data. (d) Unfiltered GL observation component J154230-545826. Plots are as described in Figure 18(a). This is an example of where foreground diffuse emission is brighter in polarized intensity than a faint background component. We confirm that this is in fact a situation of diffuse emission dominating the background component by visual inspection of the diffuse and component maps from the median filter process. The clean peak at ﹩\phi ﹩ = +31.7 rad m−2 is due to foreground diffuse emission, while the clean peak at clean peak at ﹩\phi ﹩ = −32.3 rad m−2 is the background component RM. The clean peak associated with the diffuse emission is brighter in polarized intensity than the peak associated with the background component, so 1D RM synthesis returns the diffuse emission ﹩\phi ﹩ as the component RM. (e) As for 18(d), but after median filtering. The application of the median filter reduces the intensity of the diffuse emission peak at ﹩\phi ﹩ = +31.7 rad m−2 to below the 8﹩\sigma ﹩ GES clean threshold, leaving the component clean peak at ﹩\phi ﹩ = −32.3 rad m−2 as the brightest detectable peak, as desired. (f) Unfiltered EL Faraday complex component J220307-494052. Plots are as described in Figure 18(a). The dominant clean peak is at ﹩\phi ﹩ = 9.7 ﹩\pm ﹩ 1.0 rad m−2. (g) As for 18(f) but after median filtering. We see the expected reduction in polarized intensity due to the application of the median filter in the Stokes ﹩qu﹩ spectra and Faraday spectrum as compared with 18(f). The dominant clean peak is at ﹩\phi ﹩ = 9.4 ﹩\pm ﹩ 0.9 rad m−2, which is consistent with 18(f).﹩\psi ﹩
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: RM grids of the median-filtered EC (left) and GL (right) observations plotted over the Hutschenreuter et al. (2022) all-sky Faraday depth map in each region. The diamond-shaped markers are the components used to construct the Hutschenreuter et al. (2022) Faraday depth map in each region and are included for reference only. The dashed yellow line in the GL observation lies along b = 0° in the Galactic plane.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: Top: SF for the EC observation. Bottom: SF for the GL observation. In both panels, the best-fit power-law model is shown by the green dashed line, and previous SF measurements are included in dotted–dashed lines for comparison. The Stil et al. (2011) SF in the top panel is for the south Galactic pole.
Paper: Prototype Faraday Rotation Measure Catalogs from the Polarisation Sky Survey of the Universe’s Magnetism (POSSUM) Pilot Observations
Authors: S. Vanderwoude, J. L. West, B. M. Gaensler, L. Rudnick, C. L. Van Eck, A. J. M. Thomson, H. Andernach, C. S. Anderson, E. Carretti, G. H. Heald, J. P. Leahy, N. M. McClure-Griffiths, S. P. O'Sullivan, M. Tahani, A. G. Willis
Figure caption: RM grids of the EL, EM, EC, and GL observations with no median filter applied. The markers indicate the presence of a polarized component at that location in the observation. Positive RMs are red and negative RMs are blue, while the depth of the color indicates the magnitude of the RM. Circle and star markers denote Faraday simple and complex components, respectively. Crosses indicate Faraday simple components where the RM is consistent with 0 within the uncertainty.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: SDSS 3585856: panels (a) and (b) show the raw data and folded LC, respectively. Magenta points are data from SDSS and blue points are from ZTF. Panels (c), (d), and (e) are the steps of prewhitening the LC shown as the Fourier spectra. (c) shows the raw spectrum around the main frequency f 1, (d) shows the position of the Blazhko peaks f 1 ± f  m  in the residual spectrum after we prewhitened with the main frequency and its harmonics, and (e) is the noise after prewhitening the LC with all the previous frequencies.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: SDSS 747380: panels (a) and (b) show the raw data and folded LC, respectively. Magenta points are data from SDSS, and blue ones are from ZTF. Panels (c), (d), and (e) are the steps of prewhitening. (c) shows the spectrum around the main pulsation frequency f 1, (d) shows left-hand side Blazhko peak f 1 − f m after we prewhitened the LC with f 1 and its significant harmonics, and (e) is the noise at the end of the prewhitening process.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: SDSS 2863787: panels (a) and (b) are similar to that of the Figure 3. (c) shows the Fourier spectrum around f1, (d) shows the first pair of the Blazhko side peaks after we prewhitened the LC with f 1 and its significant harmonics, (e) shows the second pair after we prewhitened the LC with the first Blazhko pair, and (f) shows the noise at the end of the prewhitening process.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: Histogram of the Blazhko period P B. Black and gray colors represent BRRc stars with single and multiple P B, respectively.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: Ratio of P to P B plotted against ﹩\mathrm{log}({P}_{{\rm{B}}})﹩. The green and red points represent BRRc stars with single and multiple P B, respectively, and the silver points are Netzel et al. (2023) data. The black curve shows the fitting.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: Plot of the main pulsation period P to the Blazhko period P B in log-log scale. Green and red points show the BRRc stars with single and multiple Blazhko effect, respectively.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: BRRc star SDSS ID 3585856: Fourier analysis of individual LCs from SDSS (left panels) and ZTF (right panels). In the left panels, (a) shows f 1 detected from SDSS LC, and (b) shows no Blazhko peaks but just the background noise. Similarly in the right panels, (c) shows f 1 detected from ZTF LC, and (d) shows no Blazhko peaks but just the background noise.
Paper: Study of the Blazhko Type RRc stars in the Stripe 82 Region Using SDSS and ZTF
Authors: Vaidehi Varma, József M. Benkő, Chow-Choong Ngeow
Figure caption: SDSS 1482164: the meaning of panels (a)–(e) are the same as in Figure 4, panel (f) shows the result of one more prewhitening step due to the third Blazhko modulation. Panel (g) shows the noise at the end of the prewhitening.
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: Left: the mock galaxy population (gray contours) and the inferred galaxy population (blue contours) using our method. We calculate the average SFR within the past 0.1 Gyr (logSFR0.1Gyr) and the mass-weighted age (t age,MW) using the inferred SPS parameters. The lighter blue histograms show the individual normalizing flows, and the dark blue histogram is the result after averaging 10 flows. The inferred galaxy population agrees with the truth very accurately. Right: the mock photometric data in the SDSS ugriz bands (gray contours) are practically indistinguishable from the photometry of the inferred galaxy population using POPSED (blue contours).
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: Performance of the galaxy spectrum emulator. The left panel shows the fractional error of the emulated rest-frame spectrum L  λ  at 1000–12000  Å. The shaded regions correspond to the 68th (1σ) and 95th (2σ) percentiles of the fractional error distribution. The right panel shows the emulation error of the broadband photometry X  k  in the SDSS ugriz bands for galaxies at z = 0. Here we use the SDSS ugriz filters as a demonstration and take the transmission curves from Doi et al. (2010), assuming an airmass of 1.3. The emulator achieves a high accuracy of <1% for λ > 4000 Å, but suffers at the very blue end. However, the emulated photometry is accurate to <0.02 mag, which is negligible for analyzing nearby galaxies in large photometric surveys.
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: Left: the inferred galaxy population from GAMA photometric data (red contours) and the distribution of spectroscopic redshift and stellar mass from the GAMA catalog (gray contours). The inferred redshift and stellar mass distributions agree well with the spectroscopic results. Right: the GAMA photometric data (gray contours) and the synthetic photometry of the inferred galaxy population (red contours). Despite the small difference in the u − g color, the two photometric distributions agree with each other quite well.
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: A schematic diagram of POPSED (details in Section 2). The galaxy population distribution p( θ ∣{ X   i }) is approximated by a normalizing flow q   ϕ  ( θ ). We sample from the normalizing flow and forward model the synthetic photometry ﹩\{{\hat{{\boldsymbol{X}}}}_{j}^{{\boldsymbol{\phi }}}\}﹩ using the galaxy SED emulator ﹩F({{\boldsymbol{\theta }}}_{j}^{\phi })﹩. Then we compare the distributions of the observed photometry and the synthetic photometry by calculating the Wasserstein distance ﹩{{ \mathcal W }}_{2}(\{{\hat{{\boldsymbol{X}}}}_{j}^{\phi }\},\{{{\boldsymbol{X}}}_{i}\})﹩, which is used as a loss to train the normalizing flow until the synthetic photometry from the normalizing flow agrees with the observed photometry.
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: Similar to the left panel in Figure 3, but showing the distributions of the inferred galaxy population (red) in the full parameter space. For comparison, the gray contours show the joint distribution of the spectroscopic redshift and the stellar mass from the GAMA catalog.
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: The distribution of the inferred galaxy population at z < 0.1 on the M ⋆–SFR plane. The SFMS and the quiescent population are clearly shown. The inferred galaxy population agrees well with the SFMSs from Renzini & Peng (2015), McGaugh et al. (2017), and Sánchez et al. (2019).
Paper: PopSED: Population-level Inference for Galaxy Properties from Broadband Photometry with Neural Density Estimation
Authors: Jiaxuan Li, 嘉轩 李, Peter Melchior, ChangHoon Hahn, Song Huang, 崧 黄
Figure caption: Similar to the left panel in Figure 2, but showing the distributions of the mock galaxy population (gray) and the inferred galaxy population (blue) in the full parameter space.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Corner plots for O3 at 0.64 μm at S/N = 20 to portray the lack of continuum and its impact on O3 abundance retrieval. We also show a corner plot for S/N = 200 with all parameters set to exact grid points to portray the interpolation error in A  s . The 68% credible region is shown as pink shading in the 1D marginalized posterior distributions along the diagonal of the corner plot, and the true values are represented by black lines in the diagonals of the corner plot, and black stars within the 2D plots. It is clear that the error in A  S  is due to a combination of parameter degeneracy and interpolation error in the grid-derived forward models.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Results of the fiducial case study for O2, but showing only a narrow range of S/N values. The y-axis shows the abundance values for each molecule in log scale, with the true value shown with the black dashed line (in this case, a modern-Earth-like O2 value of 0.21 VMR). Each dot represents a bandpass center, with the pink line portraying the median retrieved values of O2 abundance for that bandpass, and the gray-shaded region representing the upper and lower limits for the 68% credible region. Increased retrieval certainty can be seen where the gray regions narrow. Each point is colored to indicate varying detection strength. Unconstrained regions (lnB < 2.5) are shown in light pink dots, weak detections (2.5 ≤ lnB < 5) are shown in dark pink diamonds, and strong detections (lnB > 5) are shown in purple squares. We present the range at which detectability materially changes for O2.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Results of the fiducial case study for O3 focused on a specific narrow S/N range. We show the S/N range at which detectability materially changes for O3. All facets of the plot remain the same as in Figure 2. We notice that for S/N = 20, 3 bandpasses achieve a strong detection but none of these bandpasses correctly constrain the abundance of O3 within the 68% credible region. We present further investigation on this in Figure 4.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). II. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for O2 and O3 
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael D. Himes, Michael Dane Moore, Nicholas Susemiehl, Jaime Crouse, Shawn Domagal-Goldman, Giada Arney, Vincent Kofman, Amber V. Young
Figure caption: Reflection spectra of a modern-Earth atmospheric composition but with varied O3 and O2 abundances. We feature a high O3 abundance (3 × 10−6), a 50% PAL O2 abundance (2.1 × 10−2), and a modern Earth (7 × 10−7 O3, and 2.1 × 10−1 O2), respectively. All spectra are binned at R = 140.
Paper: Galaxy Morphological Classification of the Legacy Surveys with Deformable Convolutional Neural Networks
Authors: Shoulin Wei, 守林 卫, Wei Lu, 伟 陆, Wei Dai, 伟 戴, Bo Liang, 波 梁, Longfei Hao, 龙飞 郝, Zhijian Zhang, 志坚 张, Xiaoli Zhang, 晓丽 张
Figure caption: Examples from the data set. First six rows are classes of Round, In-between, Cigar-shaped, Edge-on, Spiral, and Irregular, respectively. The last row shows stamps with imaging errors sampled from Legacy Surveys.
Paper: Revisiting ϵ Eridani with NEID: Identifying New Activity-sensitive Lines in a Young K Dwarf Star
Authors: Sarah Jiang, Arpita Roy, Samuel Halverson, Chad F. Bender, Carlos Selgas, O. Justin Otor, Suvrath Mahadevan, Guđmundur Stefánsson, Ryan C. Terrien, Christian Schwab
Figure caption: Example of how we fit each line (blue) with a standard Gaussian function (red) and extract all line parameters. The centroid, depth, and FWHM of the line are measured from the Gaussian fit. The range over which we calculate integrated flux in this example line is denoted in green. Note that the exact wavelength bounds of this region vary slightly from line to line since our integrated flux window is uniform in velocity, not wavelength, though on average the integrated flux window captures a similarly wide region of each line around the line core as shown in this figure.
Paper: Polarization Criterion in Targeted SETI Observation
Authors: Jian-Kang Li, Yu Chen, Bo-Lun Huang, Zhen-Zhao Tao, Xiao-Hang Luan, Xiao-Hui Sun, Tong-Jie Zhang, 同杰 张, Vishal Gajjar
Figure caption: Left: the changes of parallactic angle, altitude, and azimuth of Kepler-438 during the ∼4 hr observation in local time 2021.06.29 of FAST. Right top: the variation of ﹩Q^{\prime} ﹩ and ﹩U^{\prime} ﹩ of the synthetic ETI signal during the ∼4 hr observation of Kepler-438. Right bottom: The variation of ﹩Q^{\prime} ﹩ and ﹩U^{\prime} ﹩ of the synthetic RFI during the ∼4 hr observation of Kepler-438.
Paper: Polarization Criterion in Targeted SETI Observation
Authors: Jian-Kang Li, Yu Chen, Bo-Lun Huang, Zhen-Zhao Tao, Xiao-Hang Luan, Xiao-Hui Sun, Tong-Jie Zhang, 同杰 张, Vishal Gajjar
Figure caption: The change of parallactic angle with hour angel for observation targets at different decl. and telescopes at different latitudes, respectively. The black horizontal dashed line represents the case that Δq = 45°.