adsabs/AstroCLIMB huggingface dataset:
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Panel (a) shows an image of a single star in the F154W filter. (b) Mean stack of six stars in the N242W filter. (c), (d) Isophotal radial intensity profiles in F154W and N242W filters. The green and red lines show the individual Moffat and exponential functions, while the solid line represents the total fit to observed data points. The vertical dashed blue line indicates the radius of 80% EE on either panel. (e) The normalized COG for the F154W and N242W filters obtained using circular apertures.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Upper panels: histograms of mean background in F154W and N242W. Bottom panels: standard deviation in the F154W, and N242W filters. The dashed lines represent the mean values provided in Table 1. The sample background pixel histograms of a randomly selected subpatch from each deep and shallow part of N242W and F154W with full integration time (﹩{t}_{\exp }﹩) are shown as inset plots in the top left corners of upper panels; their distribution clearly suggests their Poisson nature.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: (Top left): the recovery fraction of injected simulated sources as a function of input magnitude (aperture radius = 1.″2) for the N242W image region. The deep and shallow image recovery fractions are marked in red and blue, respectively. The 90% and 50% completeness limits for the deep N42W image region are marked as dotted and dashed lines, respectively. (Top right): the offset of measured magnitude from the input magnitude (aperture radius = 1.″2) of injected simulated sources as a function of the same N242W input magnitude. (Bottom): same as the top panel but for the F154W image regions (aperture radius = 1.″6).
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: The differential number count (number/deg2/0.5 mag) of all objects (minus the stars) detected by SExtractor in the AUDFs field using the detection parameters in Table 4 (left: F154W, right: N242W). The inset plots denote the Kron magnitude distribution of identified stars in the catalog. The source magnitudes are measured within apertures of radius 0.″7 (green), 1.″2 (blue), 1.″6 (golden), and the Kron radius (red). The 3σ detection limits are marked by the golden dashed line (F154W) and blue dashed line (N242W). Also indicated by the black dashed lines are the 50% completeness limits.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: The background map for the F154W (left) and N242W (right) filters. The randomly placed black boxes are of size ﹩4{\rm{^{\prime} }}\times 4{\rm{^{\prime} }};﹩ numbers within represent their percentage deviation from the mean background. Each subpatch (which resembles a pseudopixel in the map) has the sizes of 60″ × 60″ and 30.″8 × 30.″8 for the F154W and N242W images, respectively.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Combined exposure maps: in the overlapping region, the exposure time is the highest. On either panel, the contour is drawn at 60 ks (∼43 orbits on average). At the edge of the FOV, the exposure time drops drastically. Outside the overlapping region and within 1′ from the edge of the FOV; local exposure time is greater than 30 ks in either case. The footprint of the UDF mosaic is shown for reference only.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Magnitude vs. SNR plot for the F154W (upper panel) and N242W (lower panel) objects in the UVIT catalogs showing the effect of exposure time in deep and shallow regions of the image. The effect is prominent for relatively brighter sources.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Hot- and cold-mode detections in the N242W image. Kron ellipses (green, cold; red, hot) denote some of the detected sources.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: All sampled background pixels from deep and shallow regions of N242W and F154W with full integration time, plotted with the Poisson distribution having λ = ﹩\widetilde{B}\times {\widetilde{t}}_{{\rm{e}}x{\rm{p}}}﹩ from Table 1.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the distribution of optical depth (left), effective temperature (center), and luminosity (right) for AGBs and RSGs in the MCs. All sources with sflag ≠ 1 or −1 are included. The gray filled line represents optically thin AGBs, the blue line represents O-rich AGBs, the red line represents C-rich AGBs, the green line represents x-AGBs, the black dashed–dotted line represents all RSGs (regardless of chemical type), and the gray line represents all AGBs and RSGs.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Luminosity–MLR diagram of RSGs in the SMC. In the left panel, the luminosity is derived by integrating the observed SED (L obs), while the right panel depicts the luminosity obtained by integrating the best-fit model SED (﹩{L}_{\mathrm{mod}}﹩). Excluded stars (sflag ≠ 0 and τ 9.7/11.3 ≤ 0.001) are marked in gray, while retained stars are marked in black. The red curves represent our fitted relations. The bottom row shows the comparisons between our luminosity–MLR relations and those from previous studies (D. Reimers 1975; C. de Jager et al. 1988; J. T. van Loon et al. 2005; T. Wang et al. 2021; E. R. Beasor et al. 2023; M. Yang et al. 2023). Various curves represent the relations derived from our work and previous studies.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Two examples of refitting after adding MIPS and Herschel data. Only a few sources show reasonable fitting after the addition of data (left panel, with both MIPS and Herschel data added), while the majority of the refitted results are unreliable (right panel, with only MIPS data added). The solid black line and text represent the original best-fit model and result, while the red line and red text represent the best-fit model obtained from the refitting. The gray lines depict the top 50 models with the minimum χ 2 values calculated during the refitting.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the distribution of optical depth (left), effective temperature (center), and luminosity (right) for RSGs in the MCs. All RSGs with sflag ≠ 1 or −1 are included. The gray line represents Op-thin RSGs, the blue line represents O-rich RSGs, and the red line represents C-rich RSGs.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Examples of high-DPR stars in our sample. The red line represents the IRS spectral data.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: An example of SED fitting with a mixed dust component model. The best-fitting model (black line, C-rich) and mixed dust model (green dashed line) are nearly indistinguishable.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the DPR (﹩\dot{{M}_{{\rm{d}}}}﹩) distribution of AGBs in the MCs. Different colors represent different types.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Histograms of the DPR (﹩\dot{{M}_{{\rm{d}}}}﹩) distribution for RSGs in the MCs. Different colors represent different types.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Two typical examples of SED fitting for x-AGBs, with x-O on the left and x-C on the right.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Differential number of positive (red) and negative (blue) sources as a function of peak S/N, summed over the 33 ALCS fields. Based on the excess of the positive to the negative sources, a total of ﹩{177}_{-14}^{+12}﹩ sources are expected to be real down to S/N = 4.0 in the natural map (black solid line). The purity p exceeds 0.99 at S/N = 5.0 and 4.5 in the natural and tapered maps, respectively (black dashed line). We identify 141 sources at p > 0.99, referred to as the blind catalog.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Footprints of ALMA Band 6 (left), HST/F160W (middle), and IRAC/ch1 (right) in one of the ALCS fields. The dashed and solid cyan lines show the relative sensitivity response to the deepest 30% and 50% of the mosaic, respectively. The white lines denote the μ = 200 magnification curve at z = 2, estimated from our fiducial lens model of this cluster. The labeled solid and dashed green circles represent the ALMA continuum catalog sources with S/Nnat ≥ 5 and = 4–5, respectively.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Comparison between our various photometric methods described in Section 3.3 for S/N ≥ 5 sources. The red dots are our measurements, and the dashed line is the one-to-one relation. From left to right, we show the comparison between the 2.″0 radius aperture flux (S ap) and the peak flux in the natural-weighted map (S nat), the peak flux in the uv-tapered map (S tap), and the 2D fit flux with IMFIT (S imf).
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Difference of the magnification factor at random positions among different lens models. We evaluate the difference with Δμ/μ and Δμ = ∣μ − μ other∣, where μ and μ other are the magnification factors with our fiducial and other lens models, respectively. The different color plots indicate different lens models for z = 2, where there are 8, 3, and 4 publicly available lens models in A2744 (HFF, left), M1115 (CLASH, middle), and R0032 (RELICS, right), respectively, including our fiducial lens model constructed with GLAFIC (Oguri 2010). The black squares denote the median of Δμ/μ in each μ bin.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Comparison of the effective survey area among seven different lens models publicly available in AS1063. The red line is drawn from a median magnification map created from these lens models. We find that the median magnification map underestimates the effective survey, especially at 0.01 mJy, which corresponds to the area with μ ≳ 10. This is because the highly magnified regions are smeared out by sampling the median values due to slight differences in the critical curve positions among different lens models.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Same as Figure 1, but for the remaining 32 lensing clusters and the sky positions of the ALCS sources. ALMA Band 6, HST/F160W, and IRAC/ch1 maps are presented from left to right. The green solid and dashed circles show the ALCS sources in the primary and secondary samples, respectively. The white lines denote the magnification curve of μ = 200 at z = 2 with our fiducial lens model. The solid and dashed cyan lines indicate the PB sensitivity at 50% and 30%, respectively.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Comparison of the effective survey area among the HFF, CLASH, and RELICS clusters based on our fiducial lens model at z = 2.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: 10″ × 10″ image cutouts—ALMA 1.2 mm (natural-weighted), ALMA 1.2 mm (uv-tapered, HST/F814W, HST/F160W, and IRAC/ch1 from left to right—for 141 ALCS sources in the blind catalog. The contours indicate the intensity at 3σ, 4σ, and 5σ levels.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: A heatmap showing a 2D UMAP projection of the 1536-dimensional embedding space of that shows the different areas of the astro-ph literature corpus. The heatmap color denotes the density of papers in different parts of the corpus, with the auto-tagging keywords at various locations shown to illustrate the way the embeddings group the different topics by semantic similarity. Similar to a world map, the axes here do not hold a particular meaning. Regions close to each other hold a semantic similarity, while distant regions do not.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: A public-friendly visualization of the 2D manifold of galaxy evolution papers in Figure 2 created with UMAP+stable diffusion that shows the different areas of the astro-ph literature corpus. Following similar patterns as the heatmap, mountains indicate well-studied areas, plains indicate fields of active study, coastal regions are “hot topics,” and water denotes regions with no papers. Similar to a world map, the axes here do not hold a particular meaning. Regions close to each other have semantic similarity, while distant regions do not.