adsabs/AstroCLIMB huggingface dataset:
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Correction of defects in the raw images. Top panels: effect of the subtraction to remove the 1/f noise in both vertical and horizontal directions. Left: original calibrated image; center: dilated mask to remove objects and bad pixels from the estimate of the median row/column level; right: image after noise removal. Middle panels: effect of the method adopted to remove the “snowballs” from the images. Left: original image; center: data quality image as produced by the first two stages of the STScI pipeline. Snowballs are identified as large clusters of pixels typically flagged with value 4. Right: mask obtained by the procedure described in the text. This example is drawn from one image in the F115W filter. Bottom panels: an illustration of the presence of scattered light due to a “wing-tilt’’ event during observation which caused the offset/doubling of sources in three detectors of the F090W and F115W data, and results of the tentative masking and removal procedure. This example deliberately shows the worst-case scenario, i.e., a portion of the b4 chip in the F090W filter. The effect is much milder or absent in other modules and at wavelengths longer than F150W. Left: mosaic of all F090W images without any masking/removal. Center: individual frames with scattered light patterns. They are more evident in the two longer exposure (upper panels). Right: mosaic of all F090W images after masking of pixels affected by scattered light following the method described in the text.
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Top panel: detection completeness as a function of the F444W magnitude, estimated by injecting artificial sources in empty regions of the mosaic and detecting with SEXTRACTOR. The colored lines correspond to disks with half-light radii going from 1″ (leftmost cyan line) to 0.″1 (rightmost blue line); the black line is for point sources. Horizontal thin lines mark the 50%, 75%, and 90% completeness levels. Bottom panel: number counts (sources per arcmin2) of the detected sources, as a function of their measured total magnitude (computed using colors in 2 FWHMs, see Section 4), in all bands. We included all the detections, without attempting to isolate stars or spurious detections, which anyway are a small fraction of the total. The dashed vertical blue line marks the 50% completeness limit in detection. For comparison, we also show the SPITZER IRAC 4.5 μm counts on the same region, obtained by running SEXTRACTOR on the Hubble Frontier Fields images by Lotz et al. (2017).
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Signal-to-noise ratio in apertures of radius 0.″1, as a function of the total magnitude, in the seven bands. Red dots: all real detected sources; blue open circles: averages of the artificial point sources injected in the images to estimate depths (see text for details); black star: expected S/N for point sources at mag = 28.5 (based on the JWST Exposure Time Calculator estimates)(https://jwst.etc.stsci.edu/).
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Top panel: full view of the F444W mosaics. Module b is shown on the left, module a on the right. Middle panels: the small region in the green box of the FoV (25″ × 48″) in the seven observed bands (left to right, F090W, F115W, F150W, F200W, F277W, F356W, and F444W); the color cut is the same in all bands. A three-color composite image of the field is available for download (see Section 6) . Bottom panels: histograms of the 5σ limiting magnitude for all pixels in each mosaic, computed using the rescaled rms maps as described in Section 2. Note the double peak in F444W, caused by the slightly different depth of the two modules.
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Comparison between SEXTRACTOR FLUX_AUTO (green) and A-PHOT (red) estimated Kron flux on a simulated F444W image; the plots show the relative error with respect to the input (simulated) flux as a function of the input magnitude, and demonstrate that the A-PHOT estimate yields an overall lower median bias.
Paper: Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Authors: Emiliano Merlin, Andrea Bonchi, Diego Paris, Davide Belfiori, Adriano Fontana, Marco Castellano, Mario Nonino, Gianluca Polenta, Paola Santini, Lilan Yang, Karl Glazebrook, Tommaso Treu, Guido Roberts-Borsani, Michele Trenti, Simon Birrer, Gabriel Brammer, Claudio Grillo, Antonello Calabrò, Danilo Marchesini, Charlotte Mason, Amata Mercurio, Takahiro Morishita, Victoria Strait, Kristan Boyett, Nicha Leethochawalit, Themiya Nanayakkara, Benedetta Vulcani, Marusa Bradac, Xin Wang
Figure caption: Comparison between NIRCam total magnitudes and catalogs obtained running SEXTRACTOR on archival data, at four wavelengths sampled by similar filters by the JWST and the corresponding instrument (with a color correction applied on the basis of theoretical SEDs). The red lines are the medians of the distributions. The overall consistency is good and the typical average offsets are below 0.1–0.2 mag.
Paper: The X-Ray Polarization View of Mrk 421 in an Average Flux State as Observed by the Imaging X-Ray Polarimetry Explorer
Authors: Laura Di Gesu, Immacolata Donnarumma, Fabrizio Tavecchio, Iván Agudo, Thibault Barnounin, Nicolò Cibrario, Niccolò Di Lalla, Alessandro Di Marco, Juan Escudero, Manel Errando, Svetlana G. Jorstad, Dawoon E. Kim, Pouya M. Kouch, Ioannis Liodakis, Elina Lindfors, Grzegorz Madejski, Herman L. Marshall, Alan P. Marscher, Riccardo Middei, Fabio Muleri, Ioannis Myserlis, Michela Negro, Nicola Omodei, Luigi Pacciani, Alessandro Paggi, Matteo Perri, Simonetta Puccetti, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicolas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Multiwavelength polarization degree (top panel) and angle (low panel) of Mrk 421 as a function of energy. The red circles represent detections, while the arrows indicate upper or lower limits. The instruments that provided each measurement are labeled on top. The dashed line represents theoretical estimations assuming the formalism of Hughes & Miller (1991) for a turbulent jet. In the second panel, the horizontal shaded area indicates the time-averaged jet position angle and its uncertainty, measured with the Very Long Baseline Array at 43 GHz (Weaver et al. 2022).
Paper: The X-Ray Polarization View of Mrk 421 in an Average Flux State as Observed by the Imaging X-Ray Polarimetry Explorer
Authors: Laura Di Gesu, Immacolata Donnarumma, Fabrizio Tavecchio, Iván Agudo, Thibault Barnounin, Nicolò Cibrario, Niccolò Di Lalla, Alessandro Di Marco, Juan Escudero, Manel Errando, Svetlana G. Jorstad, Dawoon E. Kim, Pouya M. Kouch, Ioannis Liodakis, Elina Lindfors, Grzegorz Madejski, Herman L. Marshall, Alan P. Marscher, Riccardo Middei, Fabio Muleri, Ioannis Myserlis, Michela Negro, Nicola Omodei, Luigi Pacciani, Alessandro Paggi, Matteo Perri, Simonetta Puccetti, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicolas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: From the top to the bottom: Light curves of the optical, IR, and millimeter flux densities; light curve of Swift-XRT hardness ratio; light curve of the soft (S-band: 0.3–2.0 keV) and hard (H-band: 2.0–10.0 keV) Swift-XRT fluxes; and light curve of the IXPE count rates. In the first panel, the legend displays the symbols for the different instruments and wavelengths. Multiple data points from the same instrument are connected by a line to guide the eye. In the third panel, soft and hard fluxes are coded as red circles and black asterisks. The dashed vertical lines indicate the beginning and the end of the IXPE observation.
Paper: The X-Ray Polarization View of Mrk 421 in an Average Flux State as Observed by the Imaging X-Ray Polarimetry Explorer
Authors: Laura Di Gesu, Immacolata Donnarumma, Fabrizio Tavecchio, Iván Agudo, Thibault Barnounin, Nicolò Cibrario, Niccolò Di Lalla, Alessandro Di Marco, Juan Escudero, Manel Errando, Svetlana G. Jorstad, Dawoon E. Kim, Pouya M. Kouch, Ioannis Liodakis, Elina Lindfors, Grzegorz Madejski, Herman L. Marshall, Alan P. Marscher, Riccardo Middei, Fabio Muleri, Ioannis Myserlis, Michela Negro, Nicola Omodei, Luigi Pacciani, Alessandro Paggi, Matteo Perri, Simonetta Puccetti, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Riccardo Ferrazzoli, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Vladimir Karas, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Francesco Massaro, Giorgio Matt, Ikuyuki Mitsuishi, Tsunefumi Mizuno, C.-Y. Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Maura Pilia, Andrea Possenti, Juri Poutanen, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Paolo Soffitta, Gloria Spandre, Toru Tamagawa, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicolas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Martin C. Weisskopf, Kinwah Wu, Fei Xie, Silvia Zane
Figure caption: Polar plot of the Πx–ψ x plane. We show the confidence contours of X-ray polarization derived with ixpeobssim (black), a spectropolarimetric fit of the IXPE data (red), and a spectropolarimetric fit of the IXPE, XMM EPIC-pn, and NuSTAR data (blue). For each case, the contours at the 68.3%, 95.4%, 99.7%, and 99.994% confidence levels are shown.
Paper: Observation and Modeling of the Solar Wind Turbulence Evolution in the Sub-Mercury Inner Heliosphere
Authors: Daniele Telloni, Laxman Adhikari, Gary P. Zank, Lina Z. Hadid, Beatriz Sánchez-Cano, Luca Sorriso-Valvo, Lingling Zhao, Olga Panasenco, Chen Shi, Marco Velli, Roberto Susino, Daniel Verscharen, Anna Milillo, Tommaso Alberti, Yasuhito Narita, Andrea Verdini, Catia Grimani, Roberto Bruno, Raffaella D'Amicis, Denise Perrone, Raffaele Marino, Francesco Carbone, Francesco Califano, Francesco Malara, Julia E. Stawarz, Ronan Laker, Alessandro Liberatore, Stuart D. Bale, Justin C. Kasper, Daniel Heyner, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Anthony W. Case, Kelly E. Korreck, Davin Larson, Roberto Livi, Michael L. Stevens, Phyllis Whittlesey, Hans-Ulrich Auster, Ingo Richter
Figure caption: (a) Locations of PSP (blue) and BC (red) projected onto the solar wind source region (circles) and source surface (crosses) during the selected time intervals. Both spacecraft sample plasma from the same open magnetic field region with negative polarity (azure), below the neutral line (thick black curve). (b)–(c) Trajectories of PSP (red) and BC (blue) in the XZ and XY planes of the heliocentric inertial (HCI) coordinate system from 2022 February 19 to 28. Mercury’s orbit (green) is also displayed for reference. Color-coded dots refer to the time of the PSP–BC lineup (marked by a dotted line); the corresponding PSP, BC, and Mercury distances from the Sun are reported in panel (c).
Paper: Observation and Modeling of the Solar Wind Turbulence Evolution in the Sub-Mercury Inner Heliosphere
Authors: Daniele Telloni, Laxman Adhikari, Gary P. Zank, Lina Z. Hadid, Beatriz Sánchez-Cano, Luca Sorriso-Valvo, Lingling Zhao, Olga Panasenco, Chen Shi, Marco Velli, Roberto Susino, Daniel Verscharen, Anna Milillo, Tommaso Alberti, Yasuhito Narita, Andrea Verdini, Catia Grimani, Roberto Bruno, Raffaella D'Amicis, Denise Perrone, Raffaele Marino, Francesco Carbone, Francesco Califano, Francesco Malara, Julia E. Stawarz, Ronan Laker, Alessandro Liberatore, Stuart D. Bale, Justin C. Kasper, Daniel Heyner, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Anthony W. Case, Kelly E. Korreck, Davin Larson, Roberto Livi, Michael L. Stevens, Phyllis Whittlesey, Hans-Ulrich Auster, Ingo Richter
Figure caption: Magnetic spectral density δ  B  2 (a), magnetic compressibility C (b), and flatness ﹩{ \mathcal F }﹩ (c) at PSP (red) and BC (blue). Power-law fits to δ  B  2 and ﹩{ \mathcal F }﹩ are superposed in the inertial range, and the spectral indexes α and β are given.
Paper: Observation and Modeling of the Solar Wind Turbulence Evolution in the Sub-Mercury Inner Heliosphere
Authors: Daniele Telloni, Laxman Adhikari, Gary P. Zank, Lina Z. Hadid, Beatriz Sánchez-Cano, Luca Sorriso-Valvo, Lingling Zhao, Olga Panasenco, Chen Shi, Marco Velli, Roberto Susino, Daniel Verscharen, Anna Milillo, Tommaso Alberti, Yasuhito Narita, Andrea Verdini, Catia Grimani, Roberto Bruno, Raffaella D'Amicis, Denise Perrone, Raffaele Marino, Francesco Carbone, Francesco Califano, Francesco Malara, Julia E. Stawarz, Ronan Laker, Alessandro Liberatore, Stuart D. Bale, Justin C. Kasper, Daniel Heyner, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Anthony W. Case, Kelly E. Korreck, Davin Larson, Roberto Livi, Michael L. Stevens, Phyllis Whittlesey, Hans-Ulrich Auster, Ingo Richter
Figure caption: Magnetic field RTN components and magnitude (top) and inclination θ RB of  B  with respect to the radial direction (bottom) as measured by PSP (left) and BC (right) at 0.11 and 0.33 au from the Sun. The dashed vertical lines mark the intervals corresponding to the same plasma parcel sampled by PSP and BC during their radial alignment.
Paper: Observation and Modeling of the Solar Wind Turbulence Evolution in the Sub-Mercury Inner Heliosphere
Authors: Daniele Telloni, Laxman Adhikari, Gary P. Zank, Lina Z. Hadid, Beatriz Sánchez-Cano, Luca Sorriso-Valvo, Lingling Zhao, Olga Panasenco, Chen Shi, Marco Velli, Roberto Susino, Daniel Verscharen, Anna Milillo, Tommaso Alberti, Yasuhito Narita, Andrea Verdini, Catia Grimani, Roberto Bruno, Raffaella D'Amicis, Denise Perrone, Raffaele Marino, Francesco Carbone, Francesco Califano, Francesco Malara, Julia E. Stawarz, Ronan Laker, Alessandro Liberatore, Stuart D. Bale, Justin C. Kasper, Daniel Heyner, Thierry Dudok de Wit, Keith Goetz, Peter R. Harvey, Robert J. MacDowall, David M. Malaspina, Marc Pulupa, Anthony W. Case, Kelly E. Korreck, Davin Larson, Roberto Livi, Michael L. Stevens, Phyllis Whittlesey, Hans-Ulrich Auster, Ingo Richter
Figure caption: Comparison between the theoretical and observed fluctuating magnetic energy (a), correlation length of the magnetic field fluctuations (b), and turbulent magnetic energy cascade rate (c) as a function of radial distance. Thick (thin) curves denote the 2D (slab) turbulence component. Red (blue) dots refer to PSP (BC) measurements. The dotted line in panel (a) marks the r −3 scaling predicted by the WKB assumption. The red filled and open dots in panel (c) refer to the ﹩{\epsilon }_{{E}_{b}}﹩ estimate from Equation (1) and the Yaglom law, respectively.
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: The critical curve at z = 1.45 from the SMACS 0723 lens model is overlaid as a color composite image generated from the six existing JWST NIRCam filters depicting the central 1.5′ by 1′ of the cluster. The model incorporates strong-lensing constraints from the 19 image families identified in total, 14 of which are discovered by this work using the JWST data). The two “+” symbols mark the positions of the two dark matter halos used in this model, and the four magenta rings mark the galaxies whose weight is left free in the model. Image 2.2 is rare for containing ≥ 10 bright knots located at large projected galactocentric radii (inset).
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: Close-up view of system 5 with the z = 1.43 critical curve marked in the dashed line on this F090W+F150W+F200W composite color image. Two compact sources in the inset, knots A and B, have a separation of ∼0.″16, and have sizes that are consistent with the width of the PSF. The knots bracket the critical curve that must pass in between them at an angular separation of ∼ 0.″08. We estimate high magnification factors as a result of this close proximity to the critical curve of ∣μ∣ ∼ 750 for each source. A red knot is also detected at a position slightly offset from knot A, Tr, which may be a microlensed transient. We refer to Section 4 for more information regarding this potential microlensed transient.
Paper: Unscrambling the Lensed Galaxies in JWST Images behind SMACS 0723
Authors: Massimo Pascale, Brenda L. Frye, Jose Diego, Lukas J. Furtak, Adi Zitrin, Tom Broadhurst, Christopher J. Conselice, Liang Dai, Leonardo Ferreira, Nathan J. Adams, Patrick Kamieneski, Nicholas Foo, Patrick Kelly, Wenlei Chen, Jeremy Lim, Ashish K. Meena, Stephen M. Wilkins, Rachana Bhatawdekar, Rogier A. Windhorst
Figure caption: The image pair A and B of system 5 across all six available JWST filters. In each filter we center on the positions of A and B with rings of radius 0.16″, which is roughly equal to their angular separation. The F090W, F150W, F200W filters exhibit two separate knots consistent with the marked positions of A and B. F200W, however, also shows the bright source Tr that is slightly offset from the position of knot A. Only a single peak is detected in each of the LW filters, which is also slightly offset from the position of knot A. The insets depict the F200W and F444W images with the diffuse arc background subtracted off and the position of knot B indicated by a “+” sign. Since knot A and knot B are counter images of one another and must appear together, the Tr object seen in F200W and the LW filters is instead understood to be a candidate microlensing event.