adsabs/AstroCLIMB huggingface dataset:
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison between the S4G IRAC 3.6 photometry (Sheth et al. 2010) with the SPARC pipeline. There were 51 galaxies in common, the correspondence is good with a 7%–10% shift between SPARC and S4G fluxes with either isophotal apertures or asymptotic magnitudes. The residuals are shown in the bottom panels with a normalized histogram for each panel to the far right. We attribute the difference to varying photometric techniques (see text).
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison between the Neill et al. (2014) WISE photometry and SPARC WISE. Both SPARC and Neill et al. use similar photometric pipelines, particularly with respect to the use of drizzled WISE images. The residuals are shown in the bottom panels with a normalized histogram for each panel to the far right. The correspondence is excellent with a slight deviate at low luminosities. The comparison with asymptotic 3.6 mag recovers this missing flux.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison with the W1 and IRAC 3.6 photometry of Cluver et al. (2014) and Bell et al. (2023). The residuals are shown in the bottom panels with a normalized histogram for each panel to the far right. Both these studies use the procedures developed in Jarrett et al. (2013) and there is an excellent correspondence over five orders of magnitude.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: CDFs of the extinction-corrected Hα emission intensity distributions for our real SN sample, for all the map pixels, and for our populations of model SNe. In the top panel, we compare the models to our whole real SN sample. In the bottom panel, we maintain the same comparison, but instead sort our SNe by type. The whole real SN sample (32 SNe) is drawn with a solid black line, the map pixels are drawn with a long-dashed, dark-purple line. The Hα model SNe are drawn with a dotted purple line, the stellar disk model SNe with a dashed pink line, and the random local models are drawn with orange dotted–dashed and yellow dotted for 1 kpc and 500 pc local boxes respectively. Behind each model line, we use transparent shading to represent the 16th–84th percentile values from 1000 random pulls, each the size of our observed SN sample, from each model distribution. The shaded percentiles are drawn on the lower plot as well but we remove the lines for readability. In the lower plot we sort our real SN by type, plotting the SNe Ia with a dashed dark blue line, the SNe II with a dotted–dashed blue line, the SESNe (SNe Ib/c) with a closely dashed teal line, and the unclassified SNe with a dotted–dotted–dashed light green line. Note the increasing association with higher intensity Hα emission as progenitor mass increases.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Recent SNe (green symbols) that occurred within the footprint of the PHANGS–MUSE survey (Emsellem et al. 2022) plotted over PHANGS–MUSE images of extinction-corrected Hα intensity on the same logarithmic stretch, shown in the color bar. Black dots are where foreground stars have been removed from the image. Each SN in each galaxy is given a unique marker shape, with details of each galaxy given in Table A1 and each SN given in Table A2. The Appendix presents “zoom in” images around each SN and comparison to higher-resolution HST Hα mapping. Continued in Figure 2.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption:  A  V  values estimated by Belfiore et al. (2022, 2023) based on the Balmer decrement at each SN site. Lavender bars mark the distribution of A  V  for SNe that are coincident with H II regions. Salmon bars show extinction for SNe not coincident with the H II region and are shifted to the right by one bar width. The KDE of the H II and non-H II populations are drawn in lavender and salmon lines respectively. The KDE for all pixels across all galaxies in our sample is shown by a blue line and the mean for all pixels and all H II regions (with or without SNe) are shown by vertical dashed lines. The average extinction value for all pixels in all maps is A  V  ≈ 0.4 mag, while the average value for all pixels associated with H II regions is A  V  ≈ 1.1 mag.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: PHANGS–MUSE Hα emission cutouts (500 × 500 pc) centered on the locations of the SNe in our sample. Each galaxy is plotted at its native resolution, listed in the top right corner. Lime contours enclose H II regions identified by Groves et al. (2023). SNe are marked with white circles. In the legend, SNe are labeled with their type classification. Each panel is oriented with the top of the figure as north; east is left.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Normalized cumulative rank (NCR) plot of the association of SNe with Hα emission at native, 150 pc, and 1 kpc resolutions. Results for the PHANGS–MUSE native resolution (44–109 pc) are plotted with a solid purple line, 150 pc resolution results are plotted with a dashed magenta line, and 1 kpc resolution results are plotted with a dashed–dotted salmon line.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Example 500 pc × 500 pc zoom in for SN1995V (Type II) in NGC 1087. The left panel shows Hα intensity from the PHANGS–MUSE maps. The right panel shows Hα emission from the same region at a higher than ≈0.″1 resolution from new narrowband HST mapping (Chandar, A. Barnes et al. 2024, in preparation) In both panels, the hatched green regions indicate the footprint of the Groves et al. (2023) nebular region catalog.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: CDF of SNe over time from a simple stellar population modeled with STARBURST99. The CDF of the SNe is plotted with a solid black line, the normalized SN rate is plotted with a dotted red line, the CDF of Hα emission is plotted with a dotted–dashed green line, and the normalized Hα brightness with a dashed blue line. In purple, we shade the SN CDF to indicate when it reaches the level of excess CCSNe (20%) that we find coincident with H II regions. We also mark the delay time (7.11 Myr, 24.9M ⊙) that accounts for that excess with a dashed purple vertical line.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Estimated metallicity values at each SN site based on Groves et al. (2023). The small circles plot estimates of metallicity based on radial gradients. The large, transparent circles show estimates for the specific H II region coincident with the SN. Both estimates use the Scal system. We separate the sample by SN type.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison with the SED study of Brown et al. (2014), Clark et al. (2018), and WISE photometry from Vaddi et al. (2016). The residuals are shown in the bottom panels with a normalized histogram for each panel to the far right. The correspondence is good, but the dispersion is higher than previous comparisons. For the Brown et al. (2014; black symbols) and Clark et al. (2018; green symbols) studies, this reflects varying aperture sizes that appear to reproduce a Kron magnitude (90% the total luminosity shown by the dashed line). The Vaddi et al. (2016) also has a larger dispersion, but with the largest overlap to the SPARC sample in terms of galaxy numbers. The dashed line is the 90% flux comparison. The dispersion from this offset is 0.06 mag, which probably reflects the true uncertainty in galaxy photometry regardless of error bars quotes by each study.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The left panel displays a comparison of aperture colors between SPARC and Brown et al. (2014). The relationship is one-to-one in relative values, and the dispersion is within the observational errors (a mean error bar is shown). However, there is a 0.17 mag shift from the Brown et al. W1-3.6 colors compared to SPARC. We attribute this to differences in the zero point of the AB system used by Brown et al. and varying aperture sizes between their WISE and Spitzer measurements. The right panel displays a histogram of SPARC W1-3.6 colors. We note that a majority are redward of the mean elliptical color (red dashed line; Schombert 2016), in agreement with the expectation that star-forming disks will have redder colors than passive, old stellar population galaxies.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The near-IR and optical color–magnitude relation for the SPARC sample. The upper panel displays the SDSS g vs. WISE W1 color where HSB and LSB are marked as red and blue respectively. Seyferts or LINER galaxies are colored magenta. The CMR for ellipticals are indicated by the red dotted line (Schombert 2018). The difference between the passive ellipticals and spirals/dwarfs of the SPARC sample is evident in the steeper, bluer colors due to recent star formation. The dispersion in the elliptical CMR is very small at 0.1 mag whereas the large scatter in the SPARC galaxies represents a wide range in star formation histories as well as slower chemical enrichment. The lower panel displays the CMR for the near-IR color W1-3.6 where star formation effects are negligible. Aside from the Seyfert outliers, the range in W1-3.6 color is small and constant over the luminosity range of the SPARC sample.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The range in optical and IR color with respect to Hubble type for the SPARC sample. The trend in g-W1 matches the known trends outlined in Schombert & McGaugh (2021). The slight trend for redder W1-3.6 color with later Hubble type is not statistically significant and demonstrates why IR fluxes are significantly better for stellar mass determinations than optical flux due to their independence from star formation history as related to galaxy type.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The optical g-3.6 color compared to the IR W1-3.6 color for 87 galaxies in the SPARC sample with both WISE and SDSS imaging. While there is a wide dispersion in optical color, the range in W1-3.6 color is quite small (when Seyferts are excluded). The distinction between LSB and HSB galaxies in W1-3.6 probably reflects a metallicity effect (see Figure 10).
Paper: Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists
Authors: Lauren A. Sgro, Paul A. Dalba, Thomas M. Esposito, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Mario Billiani, Margaret Loose, Nicola Meneghelli, Darren Rivett, Fadi Saibi, Sophie Saibi, Bryan Martin, Georgios Lekkas, Daniel Zaharevitz, Robert T. Zellem, Ivan A. Terentev, Robert Gagliano, Thomas Lee Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler
Figure caption: Confirmed planets with 10 < P < 200 days and 0.1 ≤ a ≤ 0.5 au from the NEA that have available mass measurements. Giant planets with M  P  ≥ 0.25 M J are plotted such that colors denote the mass of the planet, while planets below this mass cutoff are plotted in gray. The yellow star indicates TIC 393818343 b at 4.34 ± 0.15  M J.
Paper: Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists
Authors: Lauren A. Sgro, Paul A. Dalba, Thomas M. Esposito, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Mario Billiani, Margaret Loose, Nicola Meneghelli, Darren Rivett, Fadi Saibi, Sophie Saibi, Bryan Martin, Georgios Lekkas, Daniel Zaharevitz, Robert T. Zellem, Ivan A. Terentev, Robert Gagliano, Thomas Lee Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler
Figure caption: APF-Levy RVs of TIC 393818343. Panel (a) is the time series. Panel (c) is phase-folded on the best-fit ephemeris. Panel (b) shows that an additional long-term RV trend may be present although from this data set alone it is statistically consistent with no trend.
Paper: Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists
Authors: Lauren A. Sgro, Paul A. Dalba, Thomas M. Esposito, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Mario Billiani, Margaret Loose, Nicola Meneghelli, Darren Rivett, Fadi Saibi, Sophie Saibi, Bryan Martin, Georgios Lekkas, Daniel Zaharevitz, Robert T. Zellem, Ivan A. Terentev, Robert Gagliano, Thomas Lee Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler
Figure caption: Light curve of observations taken by Unistellar Network observers during the second photometric confirmation campaign (Epoch 19, described in Section 3.3). Note that observer Margaret L.'s data were affected by fog near the expected mid-transit time.
Paper: Confirmation and Characterization of the Eccentric, Warm Jupiter TIC 393818343 b with a Network of Citizen Scientists
Authors: Lauren A. Sgro, Paul A. Dalba, Thomas M. Esposito, Franck Marchis, Diana Dragomir, Steven Villanueva, Benjamin Fulton, Mario Billiani, Margaret Loose, Nicola Meneghelli, Darren Rivett, Fadi Saibi, Sophie Saibi, Bryan Martin, Georgios Lekkas, Daniel Zaharevitz, Robert T. Zellem, Ivan A. Terentev, Robert Gagliano, Thomas Lee Jacobs, Martti H. Kristiansen, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler
Figure caption: Individual transit observations of TIC 393818343 b and the best-fit model from EXOFASTv2 shown in red. The names of observers and relevant epochs are listed in Table 1.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: Left: MCELS Hα image of the SGS LMC 4, which is delineated by the red dashed ellipse. The position of NGC 2021 is marked on the image. Right: a close-up of the NGC 2021 region. The dashed red circle is centered on NGC 2021, and the red square marks the 15′ × 15′ field of view of Figure 2.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: CTIO 4 m MOSAIC [S II] image of the NGC 2021 region with massive stars marked. NGC 2021 is located at the center of the image. The black solid circle shows the NGC 2021 region with a radius of 0.′5. The dashed circles show the LH79-NW region, the NGC 2021 surrounding region, and the LH78 region, all with radii of 1.′5.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: The B vs. (U − B) color–magnitude diagram of stars in the 15′×15′ region centered on NGC 2021. The stellar evolutionary tracks and isochrones reddened by an extinction of A  V  = 0.48 are overplotted in the left and right panels, respectively.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: CTIO 4 m MOSAIC [S II] image of the NGC 2021 region. The [S II] image is used because both stars and nebulosity can be seen in the same image. The boundaries of the OB associations LH78 and LH79 are marked in red according to Lucke (1972).
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: In this 4 m MOSAIC R-band image, we present the stellar population in NGC 2021 and its surroundings. The stars with masses of 3–5 M ⊙ (magenta), 5–10 M ⊙ (yellow), 10–15 M ⊙ (lime green), and >15 M ⊙ (cyan) are marked on the image. The two concentric black dashed circles centered on NGC 2021 are at radii of 0.′5 and 1.′5, respectively.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: Same as Figure 3, but for the annulus of radii 0.′5–1.′5 centered on NGC 2021.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: Same as Figure 3, but for the region of 0.′5 radius centered on NGC 2021.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: Same as Figure 3, but for the LH78 region of 1.′5 radius.
Paper: Stellar Population near NGC 2021: Procession of Star Formation in the South Rim of Supergiant Shell LMC 4
Authors: Po-Sheng Ou, 柏昇 歐, Rui-Ching Chao, 瑞青 趙, You-Hua Chu, 有花 朱, Chin-Yi Hsu, 晉翊 許, Chuan-Jui Li, 傳睿 李
Figure caption: Same as Figure 3, but for the LH79-NW region of 1.′5 radius.
Paper: Gaia22dkvLb: A Microlensing Planet Potentially Accessible to Radial-velocity Characterization
Authors: Zexuan Wu, Subo Dong, Tuan Yi, Zhuokai Liu, Kareem El-Badry, Andrew Gould, L. Wyrzykowski, K. A. Rybicki, Etienne Bachelet, Grant W. Christie, L. de Almeida, L. A. G. Monard, J. McCormick, Tim Natusch, P. Zieliński, Huiling Chen, Yang Huang, Chang Liu, A. Mérand, Przemek Mróz, Jinyi Shangguan, Andrzej Udalski, J. Woillez, Huawei Zhang, Franz-Josef Hambsch, P. J. Mikołajczyk, M. Gromadzki, M. Ratajczak, Katarzyna Kruszyńska, N. Ihanec, Uliana Pylypenko, M. Sitek, K. Howil, Staszek Zola, Olga Michniewicz, Michal Zejmo, Fraser Lewis, Mateusz Bronikowski, Stephen Potter, Jan Andrzejewski, Jaroslav Merc, Rachel Street, Akihiko Fukui, R. Figuera Jaimes, V. Bozza, P. Rota, A. Cassan, M. Dominik, Y. Tsapras, M. Hundertmark, J. Wambsganss, K. Bąkowska, A. Słowikowska
Figure caption: Gaia22dkv’s light curve and the best-fit planetary microlensing model (black solid line) considering microlens parallax and orbital motion effects. Data points observed by various sites are shown as open circles in different colors, respectively. The magnitudes are transformed into the ﹩i^{\prime} ﹩ band using the magnifications from the best-fit model. The inset panel presents the zoomed-in view of the region in the neighborhood of the planetary anomaly. The gray line represents the best-fit binary-source (1L2S) model, which fails to match the anomaly.