adsabs/AstroCLIMB huggingface dataset:
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: NIRCam galaxy counts in the JWIDF and the El Gordo noncluster module (orange and brown filled circles, respectively). Each row of three panels shows one wavelength as indicated in the panels. (a) (Left panels): differential galaxy counts in 0.5 mag bins. Open diamonds show a combination of previous ground-based, HST, and Spitzer/WISE counts (Driver et al. 2016a; Koushan et al. 2021) with different surveys shown in different colors as indicated in the legends. The green lines represent the hierarchical-model predictions for the 0.9–4.5 μm galaxy counts of Yung et al. (2022). When broadband filters in different instruments are similar but not identical, small corrections for effective wavelength differences may be needed (Robotham et al. 2020; Koushan et al. 2021, see Appendix B.2 here). (b) (Middle panels): energy counts after dividing the left panels by a 0.40 dex mag−1 slope. Units used are described in Section 4 and Koushan et al. (2021). Triangles without error bars indicate bins having only a single object. The brightest bins of the PEARLS counts at 18 ≲ AB ≲ 20 mag show cosmic variance (Sections 2 and 4.5), but do not weigh into the IGL fits, which at these flux levels are dominated by the faint end of the brighter surveys. PEARLS counts beyond the respective 80% completeness limits (as derived in Table 1 from a best-fit power-law extrapolation) are plotted as lightly shaded points, and are not included in the spline extrapolations to estimate the total IGL. (c) (Right panels): integral of the middle panels normalized to 100% of the IGL energy received.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: Object detection, classification, and counts in the El Gordo noncluster module in the F090W, F115W, F150W, and F200W filters. (a) (Left): SourceExtractor AB-magnitude error bars vs. MAG_AUTO AB-mag resulting from the adopted SourceExtractor-parameters (Section 3.1). Horizontal dashed lines show the adopted 5σ point-source detection limits (Table 1). (b) (Middle): star–galaxy classification diagram based on SourceExtractor MAG_AUTO AB-magnitudes vs. image FWHM. Left solid vertical lines indicate the NIRCam diffraction limit for each image with its current sampling. Blue points represent galaxies. The box to the right of the vertical line identifies objects classified as stars (red points). Objects with FWHM < FWHM(PSF) have been flagged and removed from this plot as spurious detections or border imperfections. The green dashed lines indicate for each image the effective point-source (horizontal) and SB (slanted) detection limits. (c) (Right): resulting star counts (red) and galaxy counts (blue). The vertical dashed line is the limit to which stellar objects are defined.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: Same as Figure 6 for the object detection, classification, and counts for all detectors covering the JWIDF in the F150W, F200W, F356W, and F444W filters. (Please magnify these figures to see all data points.)
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: PEARLS NIRCam image of the IRAC Dark Field (JWIDF) Epoch-1 at the north Ecliptic pole. Filter F150W is rendered as blue, F200W as green, and F356W+F444W as red using a log scaling (e.g., Lupton et al. 2004; Coe 2015). This 2040 × 3644 pixel section covers 61.″2 × 109.″3, and image orientation is shown by the labeled arrows. Areas with remaining wisps and snowball imprints were masked before making object catalogs and counts. (Please magnify all PDF images to see details.)
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: Summary of the area and depth covered by JWST Cycle 1 surveys                      . Colors and line types identify seven GO and GTO surveys as shown in the legend, and the order in the legend matches the maximum survey area as shown along the left ordinate. The thick black line shows the total area–depth of all public Cycle 1 surveys, and the thick gray line shows the same including surveys with proprietary data. The thick green line indicates PEARLS, which combines a smaller area of significant depth with a much larger area of 16 shallower fields to significantly average over CV (Sections 2 and 4.5), and include seven lensing clusters.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: PEARLS NIRCam image of the VV 191 system. Filter F150W is rendered as blue, F200W as green, and F356W+F444W as red. The elliptical galaxy VV 191a on the left backlights the spiral VV 191b on the right. Separation between the nuclei is 20.″4, and the image orientation is shown by the labeled arrows. The orange arclet south of VV 191a is gravitationally lensed by the bright elliptical (for details, see Keel et al. 2022). Note the background objects of similar angular size but different color. This 1500 × 1500 pixel section covers 45.″0 × 45.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: PEARLS NIRCam image of the El Gordo module 3′ away from the cluster. Filters F090W+F1115W are rendered as blue, F150W+F200W+F277W as green, and F356W+F410M+F444W as red. This El Gordo 4466 × 4424 pixel section covers 134.″0 × 132.″7, and image orientation is shown by the labeled arrows. Areas with remaining detector border effects and bright-star diffraction spikes (e.g., the blue spike from a bright star just outside the lower-left FOV) were masked before making object catalogs and counts.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: NIRCam image of the z = 4.1 TNJ1338 protocluster. Filters F150W+F182M are rendered as blue, F210M+F300M as green, and F335M+F360M as red. This 1850 × 1850 pixel section covers 55.″5 × 55.″5, and the image orientation is shown by the labeled arrows. The radio galaxy is the irregular orange object in the center.
Paper: JWST PEARLS. Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
Authors: Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Jake Summers, Scott Tompkins, Christopher J. Conselice, Simon P. Driver, Haojing Yan, Dan Coe, Brenda Frye, Norman Grogin, Anton Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Nor Pirzkal, Aaron Robotham, Russell E. Ryan, Christopher N. A. Willmer, Timothy Carleton, Jose M. Diego, William C. Keel, Paolo Porto, Caleb Redshaw, Sydney Scheller, Stephen M. Wilkins, S. P. Willner, Adi Zitrin, Nathan J. Adams, Duncan Austin, Richard G. Arendt, John F. Beacom, Rachana A. Bhatawdekar, Larry D. Bradley, Tom Broadhurst, Cheng Cheng, Francesca Civano, Liang Dai, Hervé Dole, Jordan C. J. D'Silva, Kenneth J. Duncan, Giovanni G. Fazio, Giovanni Ferrami, Leonardo Ferreira, Steven L. Finkelstein, Lukas J. Furtak, Hansung B. Gim, Alex Griffiths, Heidi B. Hammel, Kevin C. Harrington, Nimish P. Hathi, Benne W. Holwerda, Rachel Honor, Jia-Sheng Huang, Minhee Hyun, Myungshin Im, Bhavin A. Joshi, Patrick S. Kamieneski, Patrick Kelly, Rebecca L. Larson, Juno Li, Jeremy Lim, Zhiyuan Ma, Peter Maksym, Giorgio Manzoni, Ashish Kumar Meena, Stefanie N. Milam, Mario Nonino, Massimo Pascale, Andreea Petric, Justin D. R. Pierel, Maria del Carmen Polletta, Huub J. A. Röttgering, Michael J. Rutkowski, Ian Smail, Amber N. Straughn, Louis-Gregory Strolger, Andi Swirbul, James A. A. Trussler, Lifan Wang, Brian Welch, J. Stuart B. Wyithe, Min Yun, Erik Zackrisson, Jiashuo Zhang, Xiurui Zhao
Figure caption: Same as Figure 6 for the object detection, classification, and counts in the El Gordo noncluster module in the F277W, F356W, F410M, and F444W filters. (Please magnify these PDF plots to see all data points.)
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: Variability functions for the scale time function (plots (a.0) and (b.0)) and bias time function (plots (a.1) and (b.1)) computed from the temporal modulations learned by the P-TimeModAttn model after the pretraining process as a function of time in the range ﹩[0,100]\left[\mathrm{days}\right]﹩. A high variability can be observed before the SN-peak time (dotted line). Each model iteration (total of N runs) is represented with a black curve. The red curves are computed as the median curve using all of the N runs model iterations. The SN-peak time is computed as the median empirical maximum brightness time from the original data set ﹩{{ \mathcal D }}_{}﹩. The gray region starts at the empirical median SN last observation time computed from the data set ﹩{{ \mathcal D }}_{}﹩. Green borders (plots (a.0) and (a.1)) correspond to the band g. Red borders (plots (b.0) and (b.1)) correspond to the band r.
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: Attention-based statistics for the P-TimeModAttn model after pretraining. In the top row (plots (a.0) and (b.0) corresponding to the g and r band, respectively), the joint distribution is shown for both local SN features: the SN local slope and the SN peak distance. In the bottom row (plots (a.1) and (b.1)), the conditional joint distribution is shown using a threshold for normalized attention scores of ﹩{\bar{s}}_{\mathrm{th}}=.75﹩. This allows highlighting the regions with higher attention scores. Visual guides, for zero SN local slope and zero SN peak distance, are shown as black lines. Green borders (plots (a.0) and (a.1)) correspond to the band g. Red borders (plots (b.0) and (b.1)) correspond to the band r.
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: b-AUCROC metric curve vs. moving threshold day for the attention-based models, BRF baselines, and RNN baselines in the weak data-augmentation level (for the sake of better visualization, the mean ﹩\pm \tfrac{1}{2}﹩ std curve is shown from five-fold cross-validation). The moving threshold-day curve average (mtdCA) is shown for the TimeModAttn model and RNN baselines. Note that the horizontal axis (evolution of the threshold day) is related with the observation time since the first observation. (a) Models with serial encoder. (b) Models with parallel encoder.
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: Proposed temporal modulation ﹩{\tilde{{\boldsymbol{x}}}}_{i,j}﹩, where ﹩{\breve{x}}_{i,k}({t}_{i,j})﹩ is the kth component of the vector time function ﹩{\breve{{\boldsymbol{x}}}}_{i}({t}_{i,j})﹩, which represents the vector ﹩{\breve{{\boldsymbol{x}}}}_{i,j}﹩ associated with the time value t  i,j . The scale γ  k (t) and bias β  k (t) functions, represented with solid lines, can be evaluated at any arbitrary continuous-time value, giving a nonredundant and continuous-time modulation range ﹩[0,{T}_{\max }]﹩. Dashed lines represent empirical unobserved time functions, which are associated with the model input.
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: Confusion matrices for the SNe classification task using 100 day multiband light curves (mean ± std from five-fold cross-validation). The corresponding b-Recall and b-F 1 score metrics are given on the top of each matrix. (a) BRF baseline trained with real data. (b) BRF baseline trained with synthetic data. (c) S-TimeModAttn model. (d) P-TimeModAttn model.
Paper: Deep Attention-based Supernovae Classification of Multiband Light Curves
Authors: Óscar Pimentel, Pablo A. Estévez, Francisco Förster
Figure caption: ROC curves for the SNe classification task using 100 day light curves, where TPR and FPR stand for the true-positive rate and false-positive rate, respectively (the 50th percentile curve and 30th to 70th percentiles are shown from five-fold cross-validation). In both plots, the BRF ROC curves are shown as dashed lines (both: trained with real data and trained with synthetic data). (a) S-TimeModAttn. (b) P-TimeModAttn model.