adsabs/AstroCLIMB huggingface dataset:
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: K-band spectra of the L3–T8 planetary mass objects with masses between 7 and 10 MJup. In red is the spectrum of target 473 of our sample (1–3 Myr old). In orange is the JWST/NIRSpec spectrum of the L6 spectral type planet 2M1207b (∼10 Myr old). In purple, we show the VLT/X-shooter spectrum of the L8 free-floating brown dwarf PSO 318–22 (∼23 Myr). In blue, we show the VLT/X-shooter spectrum of GU Psc b (T3.0, ∼100 Myr), and in dark blue, we show the JWST/NIRSpec spectrum of Ross 458 c (T8.0, ∼200 Myr).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: H-band spectra of the L3–T8 planetary mass objects with masses between 7 and 10 MJup. In red is the spectrum of target 473 of our sample (1–3 Myr old). In orange is the JWST/NIRSpec spectrum of the L6 spectral type planet 2M1207b (∼10 Myr old). In purple, we show the VLT/X-shooter spectrum of the L8 free-floating brown dwarf PSO 318–22 (∼23 Myr). In blue, we show the VLT/X-shooter spectrum of GU Psc b (T3.0, ∼100 Myr), and in dark blue, we show the JWST/NIRSpec spectrum of Ross 458 c (T8.0, ∼200 Myr).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: JHK MOSFIRE spectra of all the high-mass brown dwarfs in our sample with masses between 41 and 76 MJup. The data set used to generate this figure is available in machine-readable format from the online journal.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: NIR emission lines for the six accreting objects. Five show accretion from Pa-β, while one (Obj 473) shows accretion in Bra-γ (gray spectrum).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Mass accretion rate vs. mass for the six ONC accretors (gold diamonds). The four objects with masses below the deuterium burning limit have accretion rates calculated using planetary Lacc–Lline scaling relations (gold stars). The black circles indicate the stars, brown dwarfs, and planetary mass companions (PMCs; filled circles) from CASPAR (S. K. Betti et al. 2023). The black line is the ﹩\dot{M}\propto {M}^{2.02}﹩ relation for all objects in CASPAR, while the gold lines are the ﹩\dot{M}-M﹩ relationships for stars (dashed–dotted line) and brown dwarfs (dashed line) at 1 Myr from CASPAR (Equations (10)–(11) from S. K. Betti et al. 2023).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: JHK MOSFIRE spectra of all the high-mass brown dwarfs in our sample with masses between 7 and 13 MJup. The data set used to generate this figure is available in machine-readable format from the online journal (see Figure 20).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: J-band MOSFIRE spectra of the objects showing spurious emission features, before being removed (left-hand-side plot) and after (right-hand-side plot), and the skylines expected to overlap, to show that some of those might be introduced by incomplete skyline removal during the data reduction process.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: JHK MOSFIRE spectra of all the high-mass brown dwarfs in our sample with masses between 14 and 40 MJup. The data set used to generate this figure is available in machine-readable format from the online journal (see Figure 20).
Paper: Prestellar Cores in Turbulent Clouds: Observational Perspectives on Structure, Kinematics, and Lifetime
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Density and velocity structures of a representative core at tcrit. (a) The measured volume density profile (black) and the semianalytic solutions for the BE sphere (purple) and the TES (cyan) with matching ρc, rs, and p. The circles mark the critical radius for each model. The inset shows the column density map made by projecting the (0.3 pc)3 cubic region around this core along the z-axis. (b) The radial velocity dispersion profile (black) and the best-fit power-law relation ﹩{\left\langle \delta {v}_{r}^{2}\right\rangle }_{\rho }^{1/2}={c}_{s}{(r/0.062\,{\rm{pc}})}^{0.69}﹩ (cyan). (c) The column density profile with projection along x- (dashed), y- (dotted), and z-axis (dashed–dotted), and their average (black line with markers). The cyan and purple lines are the projected column density profiles for the TES and the BE sphere, respectively (see text). The inset shows a similar column density map to that in panel (a), but projecting along the entire Lbox = 7.6 pc along the z-axis; this is more analogous to observed maps. The size of the box and the color scale are the same as in the inset of panel (a). (d) The projected radial profiles of the line-of-sight velocity dispersion (Equation (24)), for ﹩{n}_{{\rm{\min }}}=2\times 1{0}^{3}\,{{\rm{cm}}}^{-3}﹩ (blue) and 2 × 104 cm−3 (red). Different line styles correspond to different projection directions, as in panel (c). The profiles are truncated at the smallest radius where the Nd contour drops by a factor of 10 relative to its central value.
Paper: Prestellar Cores in Turbulent Clouds: Observational Perspectives on Structure, Kinematics, and Lifetime
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: (a) Ensemble of column density profiles of cores, normalized to each core’s central column density and color coded by τevol. (b) The true central volume density vs. its observational proxy ﹩{n}_{{\rm{H}},c}^{{\rm{obs}}}\equiv {N}_{{\rm{H}},c}/{R}_{{\rm{FWHM}}}﹩, also color coded by τevol; the dotted diagonal line indicates identical values. Note that the radius at which NH/NH,c = 0.5 in panel (a) defines RFWHM/2 (see Equation (28)).
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: Best matches of our targets with templates from the literature.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: K-band MOSFIRE spectra of the objects showing spurious emission features, before being removed (left-hand-side plot) and after (right-hand-side plot), and the skylines expected to overlap, to show that some of those might be introduced by incomplete skyline removal during the data reduction process.
Paper: A Near-infrared Spectral Library of Very Young Brown Dwarfs and Planetary Mass Objects in the Orion Nebula Cluster
Authors: Elena Manjavacas, Mario Gennaro, Sarah Betti, Laurent Pueyo, William O. Balmer, Massimo Robberto
Figure caption: H-band MOSFIRE spectra of the objects showing spurious emission features, before being removed (left-hand-side plot) and after (right-hand-side plot), and the skylines expected to overlap, to show that some of those might be introduced by incomplete skyline removal during the data reduction process.
Paper: Prestellar Cores in Turbulent Clouds: Observational Perspectives on Structure, Kinematics, and Lifetime
Authors: Sanghyuk Moon, Eve C. Ostriker
Figure caption: Similar to Figure 1, but at earlier evolutionary stage of τevol = −0.5 when the runaway collapse has not yet begun.
Paper: Extreme Geomagnetic Storm on the Early Earth Induced by Corotating Interaction Regions from the Young Sun
Authors: Dibyendu Sur, Vladimir S. Airapetian
Figure caption: Correlation of dynamic pressure and local noon magnetopause standoff distance.
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: The MFCI model results of the fore-event. Panel definitions are the same as Figure 2. Red curves show the ICME magnetic field estimation from the MFCI model, the pink curve shows the result without ICME arrival estimation error, and the blue curves show the MC fitting results calculated from in situ magnetic field data of STEREO-A. Black vertical lines show the beginning and end time of the observed ICME.
Paper: Extreme Geomagnetic Storm on the Early Earth Induced by Corotating Interaction Regions from the Young Sun
Authors: Dibyendu Sur, Vladimir S. Airapetian
Figure caption: Temporal variations of (a) stellar wind speed (Vx), (b) proton density, (c) By, and (d) Bz component of stellar magnetic field.
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: Interplanetary magnetic field (IMF) and solar wind data of the fore-event at VEX. The variables are displayed in VSO coordinates. From top to bottom, the panels display total IMF, the latitudinal and longitudinal angle, and the x, y, z components of IMF. Black vertical lines refer to the beginning and ending of the ICME, and thick curves show the MC fitting results.
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: The sketch of the original observer O trajectory through the MFR, along with the target observer T position. S refers to the Sun, and line AB refers to the MFR axis since. ﹩{{\boldsymbol{D}}}_{{\rm{obs}}}﹩ and ﹩{{\boldsymbol{D}}}_{{\rm{tar}}}﹩ refer to the normal vector to plane SAB (the “Sun-axis plane”) from the original or the target observer, and ﹩{{\boldsymbol{e}}}_{{\rm{axis}}}﹩ refers to the unit vector along the MFR axis.
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: Sketch of the flux rope axis at both observers. The format is the same as Figure 6. Panel (a) shows the projection in the x–y plane, and panel (b) in the y–z plane. A longitudinal separation of ﹩-4\mathop{.}\limits^{\unicode{x000b0}}2﹩ lies between the spacecraft.
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: The GCS fitting results of the fore-event. Coronagraphic images from STEREO-B, SOHO, and STEREO-A are displayed from left to right, and blue curves are the modeled CME shells. The fitting program used is developed by J. L. Forstner (2024).
Paper: Inferring the Magnetic Field Configuration of an ICME From the In Situ Observations at Different Points
Authors: Dongwei Mao, Chenglong Shen, Yutian Chi, Junyan Liu, Mengjiao Xu, Zhihui Zhong, Zhiyong Zhang, Can Wang, Yuming Wang
Figure caption: The position of observers at the initial time of the CME, generated with the website solar-Mach (J. Gieseler et al. 2023). The black arrow shows the CME direction.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Upper row (left panel): VLBI intensity map from the 3C 454.3 observation at 43 GHZ on 2016 December 23, convolved with a beam of 0.14 × 0.33 mas2 and a PA of −10∘. Middle panel: model of the observed flux distribution generated by the algorithm. Right panel: residual image. The gray contours correspond to contour levels of 0.20%, 0.40%, 0.79%, 1.60%, 3.17%, 6.40%, 12.68%, 25.36%, 50.72%, and 99.00% of the peak total intensity. Bottom row: similar to the above. Left panel: VLBI intensity map from the 3C 454.3 observation at 15 GHz on 2016 August 9, convolved with a beam of 0.44 × 1.00 mas2 and PA = −3﹩\mathop{.}\limits^{\unicode{x000b0}}﹩75. Middle panel: model of the observed flux distribution delivered by the algorithm. Right panel: residual image. The gray contours correspond to contour levels of 0.02%, 0.05%, 0.10%, 0.21%, 0.41%, 0.83%, 1.66%, 3.32%, 6.63%, 13.27%, and 36.73% of the peak total intensity. The first contour level at both observations is at the detection limit.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Examples of different detection limits calculated for the VLBI intensity map of the blazar source 3C 279 under the BEAM-ME monitoring program. Top row: observed map (left) taken at 43 GHz on 2015 August 1, convolved with a beam of 0.15 × 0.36 mas2 and a PA of −10∘, background map (middle), and rms map (right) returned by the detection limit function. The gray contours correspond to contour levels of 0.2%, 0.4%, 0.7%, 1.4%, 2.9%, 5.8%, 11.5%, 23.0%, 46.0%, and 92.1% of the peak total intensity. Bottom row: masked pixels from the observed map with the detection limit calculated to be 6 (left), 9 (middle), and 12 (right) times the median rms. Pixels with values greater than the detection limit are masked with a value of 1, while pixels with values lower than the detection limit are set to 0.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Schematic of the AAP-Imfit routine. This flowchart is applied to each map to be modeled, retrieving the astrometry and photometry of each Gaussian fitted. The algorithm consists of four main steps: First, all the parameters required by the code are extracted from the header of the FITS/IMAP file. Next, a detection limit is calculated, which separates real source emission from the background level. The final step involves removing Gaussian components that do not accurately represent the flux distribution. Finally, the map, model, and residuals are plotted for visualization, accompanied by a summary of the component properties and a general overview of all the fitted maps. Inputs and outputs are denoted in green and purple, respectively. Sections that use CASA tasks are denoted in yellow.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Left panel: VLBI intensity map from the 3C 279 observation at 43 GHz on 2015 September 22, convolved with a beam of 0.15 × 0.36 mas2 and a PA of −10∘. Middle panel: model of the observed flux distribution generated by the algorithm. Right panel: residual image. The gray contours correspond to contour levels of 0.37%, 0.75%, 1.50%, 3.00%, 6.00%, 12.00%, 24.00%, 47.93%, and 95.90% of the peak total intensity. The first contour level is at the detection limit.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Comparison between rms values for the source 3C 279 using the observations from the BEAM-ME survey. (a) Upper: rate between the model and map rms, close values to one are expected if the model accurately retrieves the original flux distribution. Bottom: percentage differences between both rates. (b) Upper: model rms, similar values between samples are expected if the routine retrieves similar models to the control sample. Bottom: percentage differences between both model rms values with respect to the observed map rms. (c) Upper: rate between the residual and map rms, values close to zero are expected if the residual does not show source information and only background info. Bottom: percentage differences between both rates. (d) Upper: residual rms, similar values between samples are expected if the routine retrieves a similar residual to the control sample. Bottom: percentage differences between both residual rms values with respect to the map rms. Green dashed lines represent the linear one-to-one relation. The red dashed line denotes zero difference.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Similar to Figure 5, but for the BEAM-ME observations of 3C 454.3.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Similar to Figure 5, but for the MOJAVE observations of 3C 454.3.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Example of a model delivered by the routine where a manual improvement could be performed. Left panel: VLBI intensity map from the 3C 279 observation at 43 GHz on 2017 February 4, convolved with a beam of 0.15 × 0.36 mas2 and a PA of −10∘. Middle panel: model of the observed flux distribution generated by the algorithm. Right panel: Residual image. The gray contours correspond to contour levels of 0.37%, 0.75%, 1.50%, 3.00%, 6.00%, 12.00%, 24.00%, 47.93%, and 95.90% of the peak total intensity. The first contour level is at the detection limit.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Upper panel: VLBI intensity map from the 3C 454.3 observation at 43 GHZ on 2020 October 3, convolved with a beam of 0.14 × 0.33 mas2 and a PA of −10∘. Middle panel: corresponding retrieved model from E. Palafox et al. (2025) Bottom panel: corresponding model of the observed flux distribution generated by the routine. The first contour level is at the detection limit.
Paper: Automated Modeling with AAP-Imfit: Astrometry and Photometry via CASA
Authors: Alfredo Amador-Portes, Eva Palafox, Víctor M. Patiño-Álvarez, Vahram Chavushyan, Andrei P. Lobanov, Sergio A. Dzib
Figure caption: Upper panel: VLBI intensity map from the 3C 454.3 observation at 15 GHz on 2011 September 12, convolved with a beam of 0.53 × 1.03 mas2 and a PA of 0﹩\mathop{.}\limits^{\unicode{x000b0}}﹩53. Middle panel: corresponding retrieved model from E. Palafox et al. (2025). Bottom panel: corresponding model of the observed flux distribution generated by the routine. The first contour level is at the detection limit.
Paper: ML-driven Strong Lens Discoveries: Down to θE﹩\,\sim \,0\mathop{.}\limits^{\unicode{x02033}}03﹩ and Mhalo < 1011M⊙
Authors: Ethan Silver, R. Wang, Xiaosheng Huang, Adam S. Bolton, Christopher J. Storfer, S. Banka
Figure caption: Examples of different types of systems for the purposes of counting (here we show simulated lensing systems from those generated in Section 3.1). The letters in the upper-left corners correspond to the criteria under which the system would be counted to contribute to the lens-able area, explained in Section 2.1.2. Image 3 shows crosshairs pointing at the lens. Note that image 1 is not a double source: it has one source that has a complex source structure from the VELA simulations.
Paper: ML-driven Strong Lens Discoveries: Down to θE﹩\,\sim \,0\mathop{.}\limits^{\unicode{x02033}}03﹩ and Mhalo < 1011M⊙
Authors: Ethan Silver, R. Wang, Xiaosheng Huang, Adam S. Bolton, Christopher J. Storfer, S. Banka
Figure caption: Distribution of σv given by T. E. Collett (2015) and CosmoDC2 using H. J. Zahid et al. (2018) on 1 deg2 of sky (CosmoDC2 provides halo mass, which is converted to stellar velocity dispersion σv using Equation (2)).
Paper: ML-driven Strong Lens Discoveries: Down to θE﹩\,\sim \,0\mathop{.}\limits^{\unicode{x02033}}03﹩ and Mhalo < 1011M⊙
Authors: Ethan Silver, R. Wang, Xiaosheng Huang, Adam S. Bolton, Christopher J. Storfer, S. Banka
Figure caption: Random cutouts from the C. C. Williams et al. (2018) catalog around sources with flux >5σ
Paper: ML-driven Strong Lens Discoveries: Down to θE﹩\,\sim \,0\mathop{.}\limits^{\unicode{x02033}}03﹩ and Mhalo < 1011M⊙
Authors: Ethan Silver, R. Wang, Xiaosheng Huang, Adam S. Bolton, Christopher J. Storfer, S. Banka
Figure caption: Pixel-level precision vs. recall curve for various ResNet thresholds chosen at Step 2 of the ResNet and U-Net pipeline, for the Einstein radius range of ﹩0\mathop{.}\limits^{^{\prime\prime} }02\lt {\theta }_{{\rm{E}}}\lt 0\mathop{.}\limits^{^{\prime\prime} }15﹩ and all halo mass values. Colored shapes represent U-Net probability thresholds that are multiples of 0.1 (leftmost is 0.9), corresponding to the curve of the same color. Across all U-Net probability thresholds, the combination of the ResNet and U-Net (ResNet threshold = 0.5 or 0.96) is a strict improvement over the U-Net alone (ResNet threshold = 0) in pixel-level precision. From Section 3.2.2.4, a high classification threshold of 0.96 for the ResNet provides a precision of 1.0 (no false positives) on the testing set with no overlapping galaxies. Evaluating the U-Net at a detection threshold of 0.5 on this set yields a pixel-level precision of 99.0% (sixth blue square from the right). To reach a pixel-level precision of 1.0 (no false positives) for this set, the U-Net requires a detection threshold of 0.72 (blue X-mark), which achieves a recall of 15.3% (306 lenses). Note that the rightmost orange circle represents a U-Net probability threshold of 0.0. At this threshold, the pixel with the maximum probability is the U-Net’s predicted location of the lens, regardless of what that probability is, and the pixel with the maximum probability can be arbitrarily small.