adsabs/AstroCLIMB huggingface dataset:
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Comparison between BPT plots with different selection cuts applied. (a) All EDGE samples plotted where each of the four emission-line fluxes exceeds its 1σ uncertainty. (b) Points from (a) where each line’s flux exceeds 3σ. (c) Points from (a) where the BPT probability estimate exceeds 0.9. Gray contours indicate the density of points. Demarcation lines defined by Kewley et al. (2001), Kauffmann et al. (2003), and Cid Fernandes et al. (2010) are shown as dashed, dotted, and solid curves respectively.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Integrated CO intensity (moment-0) maps of NGC 4047, obtained with (a) no masking; (b) a dilated mask expanding from a 3.5σ threshold over 2 consecutive channels out to a 2σ threshold; and (c) a smoothed mask where the cube is convolved to 14″ FWHM before a dilated mask is generated. Each panel is approximately 147″ square. The colormap range is shown at the bottom of each panel.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: (a) Location of EDGE-CALIFA sample in a plot of SFR vs. M *. The dashed magenta line shows the approximate locus of the star-forming main sequence from Cano-Díaz et al. (2016). CO nondetections are indicated by red squares. Small gray dots are used to represent the full CALIFA DR3 sample. (b) Vertical offset from the star-forming main sequence as a function of molecular to stellar mass ratio. The two quantities are correlated, underscoring the importance of gas content for continued star formation. CO nondetections (2σ upper limits) are indicated by horizontal arrows.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: The construction of the hexagonal grid. L is the side length of the hexagon and can be set by the user. Blue and green vectors form the basis used to construct the grid. Hexagons are first created along the diagonal, following the blue vector ﹩\hat{P}﹩. Then, for each hexagon along ﹩\hat{P}﹩, additional hexagons are created following the green vertical vector ﹩\hat{Q}﹩.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The eigenspectra corresponding to the first through the fifth PCs constructed from the Doppler-corrected ALMA spectral map of NGC 253. The upper five rows present the eigenspectra obtained by NRPCA, and the lower five rows show that obtained by A-SPCA.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Responsible features to characterize PCs from A-SPCA for the ALMA map of NGC 253. Stars represent the features responsible for PC1, and triangles are for PC2.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The two-dimensional structure to map PC1 and PC2 obtained by A-SPCA. The left panel shows the map of PC1, and the right panel describes the map of PC2.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The eigenspectra corresponding to the first through the fifth PCs constructed from the Doppler-corrected ALMA spectral map of NGC 253. The upper five rows present the eigenspectra obtained by A-SPCA with 0.25, and the lower five rows show that obtained by A-SPCA with 0.75.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The scatter plot between PCs and observed physical properties. Left: the correlation between PC1 and the integrated intensity over the whole frequency range I [Jy beam−1] on the ALMA map of NGC 253. Right: the correlation between PC2 and the peculiar velocity on the ALMA map.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The two-dimensional structures of the distribution of PC1 and PC2 of the NGC 253 obtained by A-SPCA, after correcting the effect of the Doppler shifts of the systemic Bottom: same as the top panel, but with PC1 and PC3. Note that the PC2 in this figure is different from that in Figure 8.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Normalized eigenvalues (contributions) obtained from the analysis of the ALMA spectroscopic map of NGC 253 by NRPCA, after correcting the effect of the Doppler shifts of the systemic rotation.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Same as Figure 14, but for PC1 and PC3.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Same as Figure 14, but for PC2 and PC3.
Paper: Inferring the Redshift of More than 150 GRBs with a Machine-learning Ensemble Model
Authors: Maria Giovanna Dainotti, Elias Taira, Eric Wang, Elias Lehman, Aditya Narendra, Agnieszka Pollo, Grzegorz M. Madejski, Vahe Petrosian, Malgorzata Bogdan, Apratim Dey, Shubham Bhardwaj
Figure caption: Scatter plot between z obs and z pred. Predictions from SuperLearner after 100 10fCV without using M-estimation outlier removal.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Comparison of SQL and edge_pydb databases, following the analysis of Dey et al. (2019). The “standardized slope” on the horizontal axis is the coefficient of each quantity considered in the multilinear fit for ﹩\mathrm{log}{{\rm{\Sigma }}}_{\mathrm{SFR}}﹩, scaled by the standard deviation of the same quantity in order to reflect its contribution to the fit. In both analyses, Σ* and Σmol are the dominant contributors to the SFR. The blue open triangle for O/H shows the edge_pydb result if the N2 estimator used in the SQL database were to be used.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Same panels and data as in Figure 8, but limited to pixels classified as star-forming [below the Kauffmann et al. 2003 BPT curve and with EW(Hα) > 6 Å]. Upper limits are shown as pink triangles for the vertical axis and blue triangles for the horizontal axis. Overlaid are best-fit power-law relations based on ordinary least-squares (magenta dotted line) and LEO-Py, which takes into account nondetections (green solid line with vertical scatter indicated by shading).
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Cumulative star formation history, binned in radial rings from 0 to 3 R  e , for NGC 3687 (upper left, also shown in Figure 4) and NGC 5614 (lower left). The intersection of each curve with the dashed line indicates the median age at each radius. A relatively young age for the outskirts of NGC 3687 is inferred, whereas the inner regions appear younger in NGC 5614. These general trends are corroborated by the radial profiles of specific SFR (ΣSFR/Σ*) shown in the right panels.
Paper: The EDGE-CALIFA Survey: An Extragalactic Database for Galaxy Evolution Studies
Authors: Tony Wong, Yixian Cao, Yufeng Luo, Alberto D. Bolatto, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Leo Blitz, Dario Colombo, Helmut Dannerbauer, Alex Green, Veselina Kalinova, Ferzem Khan, Andrew Kim, Eduardo A. D. Lacerda, Adam K. Leroy, Rebecca C. Levy, Xincheng Lin, Yuanze Luo, Erik W. Rosolowsky, Mónica Rubio, Peter Teuben, Dyas Utomo, Vicente Villanueva, Stuart N. Vogel, Xinyu Wang
Figure caption: Spearman partial correlation coefficients calculated based on the LEO-Py fits. The coefficients indicate that the relation between ΣSFR and Σmol is the tightest among the three correlation pairs.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Comparison of the zero-points for each of the two methods based on stars common to both the XPSP and SCR methods' samples for all 12 bands, as a function of star number (denoted as N) in each image. The bands are marked in each panel. The green points show the difference of the zero-points, and their median values and standard deviations are estimated using Gaussian fitting with a running width of 15 stars and a running step of 1 star, and are indicated by the gray and red curves, respectively. The median value of the standard deviations, for N ranging from 60 to 70, is labeled in each panel. The dashed black lines represent the zero-residual line. The distribution of zero-point differences is not symmetric about zero at intermediate and/or large N, and is primarily due to the limited common fields covered by both LAMOST (a northern-sky survey) and S-PLUS (a southern-sky survey). But the decreasing trend of scatter along N is clearly seen in all bands.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Histograms of the residuals in the zero-points between the XPSP magnitudes, along with the S-PLUS magnitudes. The results shown are for the main survey with PStotal photometry (light red), the MCs with PStotal photometry (dark red), the main survey with PSF photometry (purple), the MCs with PSF photometry (blue), and the disk region with PSF photometry (light blue). The bands are labeled in the top-left corner of each panel. Gaussian fitting results are plotted with the same colors, using solid and dashed curves for PStotal photometry and PSF photometry, respectively. The sigma values are labeled on the left side of each panel with the same colors.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: The WD loci G − uJAVA vs. G BP − G RP before (left panel) and after (right) recalibration in the uJAVA band. The red and black points represent the R.A. < 90° and decl. < −40° region and the R.A. > 180° and decl. > −30° region, respectively. The red dashed curve and the black curve correspond to the quadratic polynomial fitting results for the red and black dots, respectively.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Magnitude offsets between the XPSP-predicted magnitudes and the S-PLUS magnitudes, as a function of G BP − G RP color, for all 12 bands. The colors represent the density of points, and the bands are indicated in each panel. Zero residuals and two color cuts are denoted by black and green dashed lines, respectively. Color bars are plotted in the lower-right corner of each panel.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: An example showing the spatial distribution over the CCD of the difference between the XPSP method and the S-PLUS magnitudes. From left to right, the results are shown for the gSDSS, J0515, and J0861 bands. From top to bottom, three different observations are shown with tile_id of HYDRA−0161, HYDRA−0152, and HYDRA−0145. A color bar is shown on the right.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Spatial variations of the difference between the XPSP zero-points and the S-PLUS zero-points in each image of the main survey, using PStotal photometry from S-PLUS. The bands are marked in each panel in red, and the color bar indicating the differences is shown on the right.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Correlation plots between the zero-point offsets. The correlation coefficients are shown when they have values greater than 0.7. The colors in each panel indicate the number density of stars, and the dashed black lines represent the one-to-one line.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Same as Figure 10, but for the results after recalibration.
Paper: S-PLUS: Photometric Recalibration with the Stellar Color Regression Method and an Improved Gaia XP Synthetic Photometry Method
Authors: Kai Xiao, Yang Huang, Haibo Yuan, Timothy C. Beers, Bowen Huang, Shuai Xu, Lin Yang, Felipe Almeida-Fernandes, Hélio D. Perottoni, Guilherme Limberg, William Schoenell, Tiago Ribeiro, Antonio Kanaan, Natanael Gomes de Oliveira
Figure caption: Comparison of the zero-points for each of the two methods based on stars common to both the XPSP and SCR methods' samples for all 12 bands. The dashed black lines represent the one-to-one line.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The eigenspectra corresponding to the first through the fifth PCs constructed from the original ALMA spectral map of NGC 253. Upper five rows: eigenspectra obtained by NRPCA. Lower five rows: same as upper rows, but obtained by A-SPCA. Only the controlling features have nonzero values.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Normalized eigenvalues (contributions) obtained from the analysis of the ALMA spectroscopic map of NGC 253 by NRPCA.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: A schematic description of high-dimensional PCA. Even if we have significant important features because of the existence of a huge noise sphere, they are completely embedded in the observed data. High-dimensional PCA can subtract the noise sphere and enable the extraction of the desired features.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Velocity map of NGC 253 estimated from HCN(4–3) (top), HNC(4–3) (middle), and CS(7–6) (bottom). The systemic velocity of 243 km s−1 is subtracted.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The bright regions of NGC 253 map cut out by the mask. Left: the mask region map. White regions have significant intensity signals. Center: the cutout region with significantly bright emission. Right: the bird’s view of the signal.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: Schematic description of the relation between a sample covariance matrix ﹩\tilde{S}﹩ and its dual matrix ﹩{\tilde{S}}_{{\rm{D}}}﹩. The top panel describes the sample covariance matrix, and the bottom panel describes the dual matrix, respectively.
Paper: High-dimensional Statistical Analysis and Its Application to an ALMA Map of NGC 253
Authors: Tsutomu T. Takeuchi, Kazuyoshi Yata, Kento Egashira, Makoto Aoshima, Aki Ishii, Suchetha Cooray, Kouichiro Nakanishi, Kotaro Kohno, Kai T. Kono
Figure caption: The distribution of PC1 and PC2 of the ALMA map of NGC 253 by A-SPCA.
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: PC scores of the first to sixth principal components (i.e., ﹩{\{{z}_{{ij}}\}}_{1\leqslant i\leqslant n}﹩ for j = 1–6). GMC positions listed in Table 1 are shown with black crosses. The origin is at the phase center of the observation, α = 00h47m33.ˢ26, ﹩\delta =-25^\circ 17^{\prime} 17\buildrel{\prime\prime}\over{.} 7﹩ (ICRS).
Paper: The ALCHEMI Atlas: Principal Component Analysis Reveals Starburst Evolution in NGC 253
Authors: Nanase Harada, David S. Meier, Sergio Martín, Sebastien Muller, Kazushi Sakamoto, Toshiki Saito, Mark D. Gorski, Christian Henkel, Kunihiko Tanaka, Jeffrey G. Mangum, Susanne Aalto, Rebeca Aladro, Mathilde Bouvier, Laura Colzi, Kimberly L. Emig, Rubén Herrero-Illana, Ko-Yun Huang, Kotaro Kohno, Sabine König, Kouichiro Nakanishi, Yuri Nishimura, Shuro Takano, Víctor M. Rivilla, Serena Viti, Yoshimasa Watanabe, Paul P. van der Werf, Yuki Yoshimura
Figure caption: Top: a scree plot for our PCA. Bottom: the same as the top figure, but for a narrower range of the y-axis.
Paper: Identifying Flare-indicative Photospheric Magnetic Field Parameters from Multivariate Time-series Data of Solar Active Regions
Authors: Khaznah Alshammari, Shah Muhammad Hamdi, Soukaina Filali Boubrahimi
Figure caption: MINIROCKET is used as the downstream classifier. Shown is the test TSS score when the selected number of features is used compared to when all features are used.