adsabs/AstroCLIMB huggingface dataset:
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory and field) together with the predictions and residuals for the models of KMT-2018-BLG-0247 specified in Table 4. The double-horned profile centered at t anom = 8305.70 is caused by the source crossing the main body of a resonant caustic due to a ﹩\mathrm{log}q\sim -2.2﹩ super-Jovian mass-ratio planet. It is subject to a close–wide degeneracy (see insets) due to the lack of data on the caustic exit.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the models of OGLE-2018-BLG-1119 specified in Table 7. The short bump at t anom = 8310.7 is caused by the source crossing a ridge extending from the planetary caustic (or planetary wing of the resonant caustic) due to a ﹩\mathrm{log}q\sim -2.75﹩ Jovian mass-ratio planet. It is subject to an inner–outer degeneracy. See insets. The 1L2S model is disfavored by Δχ 2 = 14.0 and, in addition, is very heavily disfavored by kinematic arguments. Hence, it is excluded.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the models of KMT-2018-BLG-2602 specified in Table 6. The short bump at t anom = 8243.8 is caused by the source crossing a ridge extending from the planetary caustic (or planetary wing of the resonant caustic) due to a ﹩\mathrm{log}q\sim -2.8﹩ Jovian mass-ratio planet. It is nominally subject to an inner–outer degeneracy (see insets), but we adopt the outer solution because it is favored by Δχ 2 = 10.3. The 1L2S model is disfavored by Δχ 2 = 30.7 and, in addition, is very heavily disfavored by kinematic arguments. Hence, it is excluded.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the prediction and residuals for the model of KMT-2018-BLG-0030 specified in Table 2. The short bump at t anom = 8248.0 is caused by the source crossing a ridge extending from the planetary caustic due to a ﹩\mathrm{log}q=-2.5﹩ super-Jovian mass-ratio planet. See inset.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the models of KMT-2018-BLG-1714 specified in Table 10. The short bump at t anom = 8318.10 has 4 possible explanations: 2 from an inner–outer degeneracy (top insets), 1 from an off-axis cusp approach (lower right inset) [together with ﹩-2.4\lesssim \mathrm{log}q\lesssim -1.8﹩], or 1L2S model. The last has Δχ 2 = 0.9, and there are no other arguments against it. Therefore, this event should not be cataloged as planetary.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the models of OGLE-2018-BLG-0298 specified in Table 5. The short bump at t anom = 8190.6 is caused by the source crossing a ridge in or extending from the major-image side of the caustic structure due to a ﹩\mathrm{log}q\sim -3.7﹩ sub-Saturn mass-ratio planet. It is subject to a close–wide degeneracy. See insets. The 1L2S model is disfavored by Δχ 2 = 33.7 and, in addition, is heavily disfavored by kinematic arguments. Hence, it is excluded.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory) together with the predictions and residuals for the models of KMT-2018-BLG-1497 specified in Table 9. The short bump at t anom = 8233.9 has 4 possible explanations: 2 from an inner–outer degeneracy (right insets), 1 from an off-axis cusp approach (left inset) [together with ﹩-3.7\lesssim \mathrm{log}q\lesssim -1.8﹩], or 1L2S model. The last has Δχ 2 = 2.1, and there are no other arguments against it. Therefore, this event should not be cataloged as planetary.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Data (color-coded by observatory and field) together with the predictions and residuals for the models of KMT-2018-BLG-0087 specified in Table 3. The short dip at t anom = 8281.73 is caused by the source crossing the trough that runs along the minor-image axis due to a ﹩\mathrm{log}q\sim -2.6﹩ super-Jovian mass-ratio planet. It is subject to the inner–outer degeneracy. See insets.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Color–magnitude diagrams for 6 of the events analyzed in this paper, each identified by an abbreviation, e.g., KB180030 for KMT-2018-BLG-0030. The centroid of the red clump and the lens position are always shown in red and blue, respectively. Where relevant, the blended light is shown in green. In one case (KB180173), we show the baseline object in magenta. When there are multiple solutions, we show only the source and blend for the lowest-χ 2 solution.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Astrometric offsets Δ θ  of nearest Gaia entry relative to KMT coordinates for 32 events (33 planets) likely to form the 2018 statistical sample. There are 18 excellent matches (yellow circle), four other real matches in the main panel, and 10 spurious matches to unrelated stars (inset, crosses). Filled circles have full PPM Gaia solutions, while open circles only have Gaia positions. Events for which the baseline object is dominated by a star other than the source are shown as star symbols. Events are color-coded by source magnitude (see legend).
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Six-dimensional scatter plot of 33 planets. (1) Abscissa: log mass ratio. (2) Ordinate: source magnitude of unperturbed event at time of anomaly. (3) Primary (red, blue) vs. nonprimary (orange, cyan) colors; prime vs. subprime fields. (4) Reddish (red, orange) vs. bluish (blue, cyan) colors; AnomalyFinder vs. by-eye discoveries. (5) Filled vs. open symbols: caustic-crossing vs. non-caustic-crossing anomalies. (6) Shape: major-image (triangles), minor-image (circles), and central-caustic (squares) perturbations. The two most important patterns are: (A) a threshold of detections at ﹩{I}_{S}-2.5\mathrm{log}[A({u}_{\mathrm{anom}})]=18.75﹩, and (B) the dearth of by-eye discoveries of non-caustic-crossing anomalies (bluish open symbols) for ﹩\mathrm{log}q\lt -3﹩.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Same as Figure 12, except that this figure shows the remaining 3 unambiguously planetary events.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Histograms of the host mass (left) and lens distance (right) for 3 of the 6 unambiguously planetary events, as derived from the Bayesian analysis. Disk (blue) and bulge (red) distributions are shown separately, with their total shown in black.
Paper: Systematic KMTNet Planetary Anomaly Search. VI. Complete Sample of 2018 Sub-prime-field Planets
Authors: Youn Kil Jung, Weicheng Zang, Cheongho Han, Andrew Gould, Andrzej Udalski, Michael D. Albrow, Sun-Ju Chung, Kyu-Ha Hwang, Yoon-Hyun Ryu, In-Gu Shin, Yossi Shvartzvald, Hongjing Yang, Jennifer C. Yee, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Przemek Mróz, Michał K. Szymański, Jan Skowron, Radek Poleski, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Krzysztof Ulaczyk, Krzysztof A. Rybicki, Patryk Iwanek, Marcin Wrona
Figure caption: Same as Figure 10, but for the remaining 3 events (normal-sized panels). The undersized panel shows the determination of I cl from an [(I − K), I] CMD. See Section 4.4.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Anomalous Cepheids Supplemented with Large Magellanic Cloud Sample
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Reed Riddle
Figure caption: Comparison of the ACep in Crater II (filled magenta pentagons) with the calibrating ACep (the symbols are the same as in Figure 2) in the gi-band PL and PW relations. Data for ACep in Crater II have been extinction corrected and vertically shifted by a distance modulus of μ = 20.45 mag. The filled pentagon with a black cross is V108. The black solid lines are the PL and PW relations derived in Section 3, while the red dotted lines are the B-band PL relations (for both fundamental mode and first-overtone ACep) adopted from Pritzl et al. (2002).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Anomalous Cepheids Supplemented with Large Magellanic Cloud Sample
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Reed Riddle
Figure caption: The PL (left panels) and PW (right panels) relations for ACep. Filled circles and open triangles are for the fundamental mode (ACF) and first-overtone (AC1) ACep, while the darker and lighter color symbols represent the GC and LMC ACep, respectively. Solid lines are the fitted PL and PW relations to fundamental mode ACep, as given in Equations (1)–(6).
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Anomalous Cepheids Supplemented with Large Magellanic Cloud Sample
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Reed Riddle
Figure caption: ZTF light curves for the two ACep in GC. The numbers of data points in the gri-band light curves are 410, 630, and 180 for NGC5466 V19, and 1433, 1402, and 432 for M92 V7. The black crosses are rejected outliers based on a two-step process as described in the text (see also Ngeow et al. 2022b). The black curves are the fitted low-order Fourier expansion to the remaining data points on the light curves.
Paper: Zwicky Transient Facility and Globular Clusters: The Period–Luminosity and Period–Wesenheit Relations for Anomalous Cepheids Supplemented with Large Magellanic Cloud Sample
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Matthew J. Graham, Steven L. Groom, Frank J. Masci, Reed Riddle
Figure caption: Slopes (upper panel) and ZPs (lower panel) of the fundamental mode ACep PL relations as a function of wavelengths (λ). For PL ZPs, we rescaled the ZP of the published LMC- and SMC-based PL relations with the latest and most precise distance moduli of LMC (Pietrzyński et al. 2019, 18.477 mag) and SMC (Graczyk et al. 2020, 18.977 mag). Errors on the PL ZP, in the order of ∼0.02 to ∼0.05 mag, are smaller than the size of the symbols. Effective wavelengths for each filters were adopted from the Spanish Virtual Observatory Filter Profile Service (Rodrigo et al. 2012; Rodrigo & Solano 2020).
Paper: The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Authors: Kim-Vy H. Tran, Anishya Harshan, Karl Glazebrook, Keerthi Vasan G. C., Tucker Jones, Colin Jacobs, Glenn G. Kacprzak, Tania M. Barone, Thomas E. Collett, Anshu Gupta, Astrid Henderson, Lisa J. Kewley, Sebastian Lopez, Themiya Nanayakkara, Ryan L. Sanders, Sarah M. Sweet
Figure caption: Imaging taken by DECam (26″ × 26″) from DES and DECaLS for the gravitational lenses with spectroscopy from our ongoing follow-up campaign combined with published redshifts from the literature (see Section 2.2). Each system has a spectroscopic redshift (Q  z  = 1, 2, or 3) for either the foreground deflector, background source, or both; the lenses are ordered by increasing deflector redshift with the lens candidates that have only source redshifts at the bottom. Considering only redshifts with Q  z  ≥ 2, we present 53 confirmed lenses with both z defl and z src, and 15 lenses with either z defl or z src (see Table 3 for the AGEL redshift tally). Many systems have Einstein radii larger than the SDSS fiber (3″ diameter) and several are likely in clusters/groups.
Paper: The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Authors: Kim-Vy H. Tran, Anishya Harshan, Karl Glazebrook, Keerthi Vasan G. C., Tucker Jones, Colin Jacobs, Glenn G. Kacprzak, Tania M. Barone, Thomas E. Collett, Anshu Gupta, Astrid Henderson, Lisa J. Kewley, Sebastian Lopez, Themiya Nanayakkara, Ryan L. Sanders, Sarah M. Sweet
Figure caption: The slit positions of our spectroscopic observations overlaid on the DECam imaging (26″ × 26″) where the observed lens candidates are in the same order as in Figure 1 (north up, east to the left). The bottom row of seven systems are confirmed either to not be a lens or to have Q  z  ≤ 1 (Table 2). We select spectroscopic targets from the CNN-selected catalogs described in Section 2.1, where systems with spectroscopic redshifts from the literature are prioritized (see Section 2.2). Considering only spectroscopic redshifts with Q  z  ≥ 2, the AGEL redshift tally (Table 3) includes 53 confirmed lenses with both z defl and z src, and 15 lenses with either z defl or z src (Table 2).
Paper: The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Authors: Kim-Vy H. Tran, Anishya Harshan, Karl Glazebrook, Keerthi Vasan G. C., Tucker Jones, Colin Jacobs, Glenn G. Kacprzak, Tania M. Barone, Thomas E. Collett, Anshu Gupta, Astrid Henderson, Lisa J. Kewley, Sebastian Lopez, Themiya Nanayakkara, Ryan L. Sanders, Sarah M. Sweet
Figure caption: Distribution of our spectroscopic redshifts measured from follow-up with Keck and the VLT; here we show only our measured z spec and exclude the literature redshifts. The deflectors (orange) and sources (blue) have higher average redshifts (solid arrows) relative to SLACS, BELLS, and CASSOWARY (dashed arrows, see Table 4; Bolton et al. 2008; Brownstein et al. 2012; Stark et al. 2013). The SL2S survey based on CFHT imaging (Sonnenfeld et al. 2013) has a higher average source redshift than AGEL, but the spectroscopic ranges for both the deflectors and sources are marginally lower (see Table 4). By combining our spectroscopic redshifts with literature redshifts, we secure redshifts for both z defl and z src for 53 gravitational lenses, and either z defl or z src for 15 lenses.
Paper: The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Authors: Kim-Vy H. Tran, Anishya Harshan, Karl Glazebrook, Keerthi Vasan G. C., Tucker Jones, Colin Jacobs, Glenn G. Kacprzak, Tania M. Barone, Thomas E. Collett, Anshu Gupta, Astrid Henderson, Lisa J. Kewley, Sebastian Lopez, Themiya Nanayakkara, Ryan L. Sanders, Sarah M. Sweet
Figure caption: By combining optical and near-infrared spectroscopy, we confirm candidate lenses by measuring redshifts for the foreground deflectors and/or background sources. Here are six examples of confirmed gravitational lenses with spectroscopic redshifts for the deflectors (left) and higher-redshift sources (middle); all have redshift quality flag of Q  z  = 3. The high signal-to-noise ratio (black/red) spectra show strong absorption features for the deflector and emission lines for the source. The RGB images (26″ × 26″; right) are generated from multiband optical imaging from DECam.
Paper: The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Authors: Kim-Vy H. Tran, Anishya Harshan, Karl Glazebrook, Keerthi Vasan G. C., Tucker Jones, Colin Jacobs, Glenn G. Kacprzak, Tania M. Barone, Thomas E. Collett, Anshu Gupta, Astrid Henderson, Lisa J. Kewley, Sebastian Lopez, Themiya Nanayakkara, Ryan L. Sanders, Sarah M. Sweet
Figure caption: We compare the total r magnitudes reported in DESI DR9 for AGEL, SLACS, BELLS, and CASSOWARY to the spectroscopic redshifts for deflectors (circles) and sources (triangles). The DESI DR9 photometry is deeper and of higher resolution than SDSS and is thus able to deblend systems reported in earlier surveys. The lenses from the earlier surveys (open symbols) tend to be brighter than those in AGEL; only BELLS reaches comparable depths. The combination of deeper imaging with higher angular resolution and optical–NIR spectroscopy results in AGEL deflectors (orange filled circles) and sources (blue filled triangles) that reach higher redshifts.