adsabs/AstroCLIMB huggingface dataset:
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: One-dimensional and two-dimensional marginalized distributions with 1σ and 2σ contours of H 0, Ωb h 2, Ωc h 2, τ, A s, n s, and ∑m  ν  constrained from Planck-2015 CMB temperature and polarization power spectra and Pantheon SN-Ia. Three Gaussian components are used here for the MDN method.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: One-dimensional and two-dimensional marginalized distributions with 1σ and 2σ contours of w, Ωm, and μ  c  constrained from Pantheon SN-Ia, with no systematic uncertainty. Three Gaussian components are used here for the MDN method.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: The general structure of a multibranch MDN with Gaussian components. The inputs are multiple data sets {D 1, D 2, D 3, ..., D  n } from different experiments, and the outputs are the parameters of the mixture model. The yellow part shows the combination of the outputs of these branches.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: The general structure of an MDN with Gaussian components. The input is the observational data, and the outputs are the parameters of the mixture model. Each node here is a neuron.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: Two-dimensional marginalized distributions with 1σ and 2σ contours of w and Ωm constrained from Pantheon SN-Ia when considering the systematic uncertainties.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: The same as Figure 7, but nine Gaussian components are used here.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: The same as Figure 5, but including systematic uncertainties.
Paper: Likelihood-free Inference with the Mixture Density Network
Authors: Guo-Jian Wang, Cheng Cheng, Yin-Zhe Ma, Jun-Qing Xia
Figure caption: Losses of the training set and validation set. There are 3000 samples in the training set, and 500 samples in the validation set.
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: The CO distribution (contours) of 16 group galaxies is overlaid on the Digitized Sky Survey 2 (DSS2, https://archive.stsci.edu/dss/index.html) blue images. The contour levels from outer to inner, indicating the molecular gas surface density, are shown at the bottom of each panel. The surface density of the molecular gas is calculated by adopting α CO = 4.35 M ⊙ pc−2 (K km s−1)−1 (Strong & Mattox 1996; Bolatto et al. 2013). In this calculation, we did not apply an inclination correction. Galaxies in the I1459G are shown in the first two rows (their names in blue), and galaxies in the N4636G are shown in the second three rows (their names in black). The green cross indicates the stellar disk center, which is obtained from Spitzer 3.6 μm data (Salo et al. 2015). The bar in the bottom-left corner represents the physical scale of 2 kpc. The synthesized beam is shown in the bottom-right corner.
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: Distribution of sample galaxies in the I1459G (left) and the N4636G (right). Our targets are indicated by open circles (red: detection of CO, black: nondetection of CO). Open diamonds display some of the samples, which display asymmetric H I and/or CO distributions. Green large cross in each panel is the BGG. Small crosses (gray: late-type, yellow: early-type) represent galaxies taken from the Hyperleda database, which are also within 1.5 × R 200 (dashed circles, I1459G: 0.55 Mpc, N4636G: 0.70 Mpc) and ±3 × σ group (I1459G: 223 km s−1, N4636G: 284 km s−1) and brighter than the absolute magnitude of −15.5 (the faintest galaxy among small crosses in the I1459G) in the B-band. The bar in the bottom-left corner represents the physical scale of 0.25 Mpc.
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: Distribution of sample galaxies on the projected phase-space diagram (left: I1459G, right: N4636G). Symbols are the same as in Figure 1. The x-axis is a projected distance from the group center (r/R 200, normalized by R 200). The y-axis is a line-of-sight velocity with respect to the systemic velocity of the group (ΔV/σ group, normalized by the group velocity dispersion). The dashed (solid) line indicates the averaged (the maximum) escape velocity as a function of the projected distance from the group center (r/R 200).
Paper: ALMA/ACA CO Survey of the IC 1459 and NGC 4636 Groups: Environmental Effects on the Molecular Gas of Group Galaxies
Authors: Bumhyun Lee, Jing Wang, Aeree Chung, Luis C. Ho, Ran Wang, Tomonari Michiyama, Juan Molina, Yongjung Kim, Li Shao, Virginia Kilborn, Shun Wang, Xuchen Lin, Dawoon E. Kim, Barbara Catinella, Luca Cortese, Nathan Deg, Helga Denes, Ahmed Elagali, Bi-Qing For, Dane Kleiner, Bärbel S. Koribalski, Karen Lee-Waddell, Jonghwan Rhee, Kristine Spekkens, Tobias Westmeier, O. Ivy Wong, Frank Bigiel, Albert Bosma, Benne W. Holwerda, Jan M. van der Hulst, Sambit Roychowdhury, Lourdes Verdes-Montenegro, Martin A. Zwaan
Figure caption: The histograms show the stellar mass distributions of CO-detected (green) and non-CO-detected (black solid line) group samples. Left panel: all sample galaxies, middle panel: the I1459G, right panel: the N4636G. The stellar mass range of galaxies with CO detections is ∼109–1010 M ⊙.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Lyα luminosity density ρ Lyα . The red star shows the value inferred from our quasar–Lyα emission measurement, assuming that the detected Lyα emission is due to star-forming galaxies with a typical luminosity-weighted bias of b  α  = 3. As a comparison, we also show the values with previous IM measurements (Croft et al. 2016, 2018; Chiang et al. 2019) and those from integrating the Lyα LFs of LAEs (Ouchi et al. 2008, 2010; Drake et al. 2017a; Sobral et al. 2018; de La Vieuville et al. 2019; Hu et al. 2019) and scaling Hα luminosities with an escape fraction of 5% (Sobral et al. 2013; Wold et al. 2017).
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: The probability distribution of parameters 〈μ  α 〉, β  α , and SB0 as a result of the joint fit to the modified multipoles and SB profile of the quasar–Lyα emission cross-correlation, with an assumption that star-forming galaxies dominate the large-scale Lyα emission and thus b  α  = 3. The parameter 〈μ  α 〉−21 is 〈μ  α 〉 in units of ﹩{10}^{-21}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathring{\rm A} }^{-1}\,{\mathrm{arcsec}}^{-2}﹩, and SB−20 is SB0 in units of ﹩{10}^{-20}\,\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{arcsec}}^{-2}﹩. The dashed lines in the histograms denote the 16th, 50th, and 84th percentiles of the marginalized distributions.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Same as Figure 8 but the Lyα luminosity density ρ Lyα  is converted to SFRD ρ SFR under the assumption that Lyα emission is purely caused by star formation. Given the effect of dust extinction and the Lyα escape fraction, these Lyα-converted ρ SFR values should be considered as lower limits of the intrinsic star formation. The orange-shaded region represents the parameterized model for the evolving SFRD in Robertson et al. (2015), based on IR and UV observations.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: The average residual SB 〈μ(z)〉, obtained by averaging all the individual residual spectra in the observed frame after subtraction of the best-fit galaxy model spectra from the LRG spectra. The gray regions, centered at 3934 Å and 3969 Å spanning 30 Å and at 4358 Å spanning 40 Å, are masked for zero-redshift Ca H and K lines and the strong mercury G line from streetlamps.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: The measured (left panel), best-fit (middle panel), and residual (right panel) quasar–Lyα emission cross-correlation as a function of r ∥ and r ⊥. The model fit is only to large-scale signals by using the modified multipoles (Equation (13)). The best-fit pattern shown here is reconstructed from the corresponding multipoles (Equation (16)) with the best-fit parameters. The residual is obtained by subtracting the best-fit model from the measurement, with elongated distortion along the r ∥ direction on small scales, and small-scale anisotropy not included in our model. All the three images are smoothed using a 2D Gaussian kernel with a standard deviation of 4 h −1 cMpc.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Modified monopole, quadrupole, and hexadecapole of the quasar–Lyα emission cross-correlation (see Equation (13)) and their fitting results based on the galaxy-dominated model (see Section 3.4.1). The points represent our measurements with jackknife error bars. The solid curves denote the modeled modified multipoles with parameters randomly drawn from their posterior probability distributions, among which the thickest ones correspond to the best fits. The modified multipoles remove any information within r < r ⊥,cut, i.e., the gray-shaded regions, to avoid small-scale contamination.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: The quasar–Lyα emission cross-correlation as a function of r ⊥ and r ∥. To reduce noise in the image, the data is smoothed with a 2D Gaussian kernel with a standard deviation of 4 h −1 cMpc. Potential light contamination is removed by a pixel veto. For display, the pattern is mirrored along r ⊥ = 0.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Projected Lyα SB profile (red points) around quasars obtained from our cross-correlation measurement. For comparison, the power-law fit (Equation (9)) from the IM result in Croft et al. (2018) is shown as a black dashed line. The SB profiles from observations of Lyα emission around quasars on smaller scales are shown as a green-shaded region (representing the range of 25th and 75th percentiles in Cai et al. 2019) and purple points (Borisova et al. 2016), with green and purple dashed lines denoting the power-law fit and extrapolation (Equation (8)). In the bottom panel, the measured SB is shown in linear scale.
Paper: Probing the Diffuse Lyα Emission on Cosmological Scales: Lyα Emission Intensity Mapping Using the Complete SDSS-IV eBOSS
Authors: Xiaojing Lin, Zheng Zheng, Zheng Cai
Figure caption: Lyα SB profile. The data points are from integrating the measured quasar–Lyα emission cross-correlation function along the line of sight, and the solid curve is the best-fit SB profile for the galaxy-dominated model depicted in Section 3.4.1. The dashed lines denote the best-fit one-halo and two-halo terms, and the shaded region represents the ±1σ range. In the bottom panel, a linear scale is used on the y-axis.
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Color–magnitude diagram of bulges. From top to bottom, the symbols are color coded according to the bulge-to-total ratio B/T, Sérsic index n, and residual average effective surface brightness Δ〈μ  e 〉. The left panels show the original data, and the right panels are the LOESS-smoothed versions. The symbols surrounded by large open squares are ultradense bulges (Section 4.2.3). The stars in the left panels mark three outliers (NGC 4947, NGC 5188, and NGC 7689), which are discussed in the main text. The black dashed line in the bottom panel is the demarcation between classical and pseudo bulges classified using the Kormendy relation, obtained, for illustration purposes only, by fitting the data with Δ〈μ  e 〉 ≈ 0 (yellowish symbols).
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: The Kormendy relation of ellipticals and bulges (labeled E and B, respectively), shown in the traditional flux-based units in the R band (left) and stellar-mass units (right). The dashed and dotted lines represent the best-fit relation and its 3σ boundary of ellipticals (filled black squares). The filled circles in the left panel are bulges color coded based on their B − R color. In the right panel, the filled blue circles and open red circles are pseudobulges (labeled PB) and classical bulges (labeled CB), respectively, classified using the flux-based Kormendy relation; the filled magenta circles are ultradense bulges (labeled UDB; Section 4.2.3); the smaller greenish/blueish squares are high-z ETGs color coded according to their redshift and LOESS-smoothed. Representative error bars are given in the lower-left corner.
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Color–magnitude diagram of bulges. The symbols are color coded according to (top) ﹩{\rm{\Delta }}\mathrm{log}\langle {{\rm{\Sigma }}}_{e}\rangle ﹩ and (bottom) ﹩{\rm{\Delta }}\mathrm{log}{{\rm{\Sigma }}}_{1}﹩. The left panels show the original data, and the right panels are the LOESS-smoothed versions. The black dashed lines in the right panels are the demarcation between classical and pseudo bulges classified using (top) the mass-based Kormendy relation and (bottom) the M ⋆–Σ1 relation (Section 4.3), obtained, for illustration purposes only, by fitting the data with ﹩{\rm{\Delta }}\mathrm{log}\langle {{\rm{\Sigma }}}_{e}\rangle \approx 0﹩ and ﹩{\rm{\Delta }}\mathrm{log}{{\rm{\Sigma }}}_{1}\approx 0﹩, respectively (yellowish symbols).
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Comparison of structural parameters of classical (reddish) and pseudo (blueish) bulges classified using the original (dotted–dashed histograms; Gao et al. 2020) and the new (solid histograms) mass-based Kormendy relation. From left to right, top to bottom, the panels display distributions of R-band bulge-to-total flux ratio, bulge-to-total mass ratio, average effective surface brightness (〈μ  e 〉), Sérsic index (n), apparent ellipticity (ϵ), and effective radius (r  e ) of the bulge.
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Correlation between Σ1 and M ⋆ of CGS ellipticals and disk galaxies. Black filled squares are ellipticals; filled circles are disk galaxies. The hosts of classical bulges are in red, and the hosts of pseudobulges, as selected by Equation (3), are in blue; the hosts of ultradense classical bulges defined by Equation (4) are in magenta. The contours show the distribution of all galaxies. The red sequence is readily recognizable but the blue cloud is sparsely sampled. The black dashed line is the structural valley from Luo et al. (2020).
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Correlation between ﹩{\rm{\Delta }}\mathrm{log}{{\rm{\Sigma }}}_{1}﹩ and bulge Δ〈μ  e 〉 (left) and bulge ﹩{\rm{\Delta }}\mathrm{log}\langle {{\rm{\Sigma }}}_{e}\rangle ﹩ (right) for disk galaxies. The Pearson correlation coefficient (r) and Spearman’s rank correlation coefficient (ρ) are given in the lower-right corner. Consistency is defined as the fraction of bulges in the first and third quadrants.
Paper: The Carnegie-Irvine Galaxy Survey. X. Bulges in Stellar Mass–based Scaling Relations
Authors: Hua Gao, 桦 高, Luis C. Ho, Zhao-Yu Li
Figure caption: Atlas of the galaxies that host ultradense bulges. Their stellar masses and Hubble types from HyperLeda (Paturel et al. 2003) are labeled in the lower-left and upper-right corner of each panel, respectively.
Paper: Thermodynamics of the Inner Heliosheath
Authors: G. Livadiotis, D. J. McComas, H. O. Funsten, N. A. Schwadron, J. R. Szalay, E. Zirnstein
Figure caption: (a) Temperatures of the 8 pixels surrounding the (central) pixel located at (long = 13, lat = 9) for year 2016, presented with respect to the projected angle α (with α = 360° simply repeating α = 0°). This is reflecting a typical case of what is observed in the sky maps of GDF. (b) Similar to (a), but plotted in polar coordinates. (c) Fraction of all GDF sky-map pixels of year 2016 with p-values above some confidence level (the two dots indicate the commonly used levels of 0.05 and 0.01, corresponding to fractions ∼52% and ∼75%). (d) Estimated error of the (logarithm of) temperature, plotted on a log-log scale for all of the sky-map pixels of the year 2016, with respect to the p-value. The red points indicate the average value of ﹩\delta \mathrm{log}T﹩ within binned p-values with bin width Δ(p-value) = 0.1; the blue line shows the trend of these points, that is, ﹩\mathrm{log}(\delta \mathrm{log}T)﹩ ≈ −0.859 ± 0.013—(0.0173 ± 0.0067)·log(p-value).
Paper: Thermodynamics of the Inner Heliosheath
Authors: G. Livadiotis, D. J. McComas, H. O. Funsten, N. A. Schwadron, J. R. Szalay, E. Zirnstein
Figure caption: Each sky-map pixel is surrounded by eight closest neighboring pixels (here the examined central pixel is colored brown). Each combination of the central pixel with one neighboring pixel is used to estimate a pair of temperature and density values, (T, n). Then, we perform a statistical analysis for averaging the derived set of eight values of (T, n). The procedure is repeated for each sky-map pixel.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: (a) Noncoronagraphic image acquired by locating the model star A on the bright fringe of the CP-VNC, (θ  x , θ  y ) ≈ (−3.8 λ A/D, 3.8 λ A/D). (b)–(d) Coronagraphic images for three positions of the model star (θ  x , θ  y ) = (0, 0) and (0, ±100 λ A/D).
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: Experimental results of wave front control at identical separation from both stars: (top) before and (bottom) after wave front control. Red dashed circles in the top row indicate the target dark-hole region. The center of the target region is 100 λ 0/D away from both stars, and the diameter of the region is set to 40 λ 0/D.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: Radial average contrast profiles as a function of angular separation from model star A. The center of the dark hole was 100 λ 0/D away from both stars as shown in Figure 8. Dashed and solid lines show the profiles before and after wave front control, respectively. Blue lines are profiles of the model binary star, while red and orange lines show the contribution of only model star A or B, respectively.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: Numerical simulation of fourth-order CP-VNC for observing a trinary-star system. The left panel shows an on-sky transmission map of the fourth-order CP-VNC (assuming bandwidth of 20%). The right two panels show the numerical simulation of the observed images (assuming monochromatic light) without and with the fourth-order CP-VNC.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: Radial average contrast profiles as a function of angular separation from model star A. The dark hole was generated close to model star A as shown in Figure 6. Dashed and solid lines show the profiles before and after wave front control, respectively. Blue lines are profiles of the model binary star, while red and orange lines show the contribution of only model star A or B, respectively.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: (Top, middle) Radial average profiles of the contrasts when the model star is located on the positive and negative sides of θ  y , respectively. (Bottom) Contrast gains as a function of the star position θ  y  within three regions, 0–3, 3–20, and 20–100 λ A/D.
Paper: Binary-star Wave Front Control Based on a Common-path Visible Nulling Coronagraph
Authors: Kenta Yoneta, Naoshi Murakami, Ryuta Koike, Jun Nishikawa
Figure caption: (Left) Optical setup of a CP-VNC with an SLM inserted for wave front control. Arrows in the optical devices indicate the transmission axes of the polarizers (P1 and P2) and the polarization axis for operating the SLM in phase-modulation mode. Arrows in light beams indicate the direction of linear polarization. (Right) On-sky transmission map of the CP-VNC assuming polychromatic light of 20% bandwidth.