adsabs/AstroCLIMB huggingface dataset:
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: Δχ 2 map of the binary-lens point-source grid-search results on the ﹩\left(\mathrm{log}s,\mathrm{log}q\right)﹩ and ﹩\left(\alpha ,\mathrm{log}q\right)﹩ planes. The upper and lower panels show u 0+ and u 0− grid searches, respectively. The solutions with Δχ 2 < 50, 200, 450, 800, 1250, and >1250 compared with the best fits (﹩{\chi }_{\min }^{2}\approx 868﹩ for u 0+ and ﹩{\chi }_{\min }^{2}\approx 690﹩ for u 0−) are color coded with red, yellow, green, blue, gray, and light gray, respectively.
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: Two degenerate microlens parallax solutions from PSPL analysis of the light curve with the region in the neighborhood of the planet anomaly removed. The upper and the lower panels display the u 0+ and u 0− grid-search results, respectively. The solutions with Δχ 2 < 1, 4, 9, 16, 25, and >25 of the best fit are color coded with red, yellow, green, blue, cyan, and gray. The insets display zoomed-in views.
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: Physical constraints on M L − D L for the best-fit solution. The contours are 1σ constraints by jointly fitting lens fluxes using isochrones, microlens parallax π E, and Gaia parallax π base. The dotted, solid, and dashed-dotted contours are constrained by isochrones at [Fe/H] = −0.2, 0 and 0.2, respectively. The red and blue lines show the isochrones for constraining fluxes in the ﹩i^{\prime} ﹩ and ﹩r^{\prime} ﹩ bands, respectively. We display isochrones with stellar ages at 3.6 Gyr and 6 Gyr, which are the 1σ lower and upper limit of the posterior, respectively. The results are consistent with those from circular orbital motion using P ⊥ (blue). The green shaded region shows the 3σ exclusion region using the upper limit on θ E by fitting the finite-source effects, and it is also consistent with the lens’ physical constraints.
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: Spectral BF for the blue (left), green (middle), and red (right) regions of Gaia22dkv’s MIKE spectrum. We identify two distinct peaks on the BFs, which correspond to the source (larger RV) and the lens (smaller RV) respectively. In each panel, the dots are the computed BF values to which we fit a function (solid color curve) using the sum of two Gaussians (gray curves). The RVs values (i.e., the centers of the Gaussians) are marked with dashed lines. Note that the BFs include the contributions from the instrumental spectral resolution ﹩{\sigma }_{\mathrm{instr}}\sim 5\,\mathrm{km}\,{{\rm{s}}}^{-1}﹩, and thus the stellar line widths are smaller than the Gaussians.
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: (For u 0+ cases) The source trajectories and light curves in the neighborhood of the planet anomaly for several u 0+ solutions. Left: The upper and middle panels show the caustics and source trajectories for solutions UPS−3.8, UPS−3.3 (the global best-fit solution), and LFS−2.6, respectively. The trajectories with arrows indicating the direction of motion are plotted with respect to the binary-lens axis. The insets of each subpanel on the left display the caustics (blue) and source position (red) at t 0,kep−1 day, t 0,kep and t 0,kep + 1 day with increasing opacities. The radii of the red circles indicate the best-fit source sizes (upper limits) for the FS (PS) solutions. Right: The light curves and best-fit models of the four solutions (UPS−3.8: dotted line, UPS−3.3: solid lines, LFS−2.6: dashed lines) are shown in the upper panel. The residuals are displayed in the lower panel.
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: The upper panel displays the predicted radial velocity curves based on the orbital parameters of the best fit. The black lines represent the MCMC sample with Δχ 2 < 1. The lower panel displays the RV semi-amplitude K and circular orbital period P circ for all solutions. Each solution is shown as the color coded filled dots with error bars in red, yellow, green, and blue, representing Δχ 2 < 1, 4, 9, 16 compared with best fit, respectively. One year period is indicated as a dashed line. The best-fit solution UPS −3.3(u 0+) is marked out with a black arrow.
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: Results of the xallarap fits by fixing β and λ at period P = 1 yr and setting u 0 > 0. The colors marked as red, yellow, green, blue, and gray represent solutions with Δχ 2 < 1, 4, 9, 16, and 25 of the best fit. The ecliptic coordinates of Gaia22dkv, which represents the Earth parameter, are indicated by the black circles, with the lower and upper circles corresponding to the u 0 > 0 and u 0 < 0 cases due to perfect symmetry, respectively.
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: Upper: spectrum from SALT/HRS (blue) and best-fit synthetic spectrum (red). Lower: zoomed region including Ca II (top) and Mg I (bottom).
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: The black crosses connected by solid lines show the χ 2 distributions for best-fit xallarap solutions at fixed binary-source orbital periods P. The red open circle at P = 1 yr shows the χ 2 for the best-fit microlens parallax solution.
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: (For u 0− cases) The source trajectories and light curves for three u 0− solutions. Left: source trajectories and caustics for the LPS−3.0 (upper), UPS−2.6 (middle), and UFS−2.6 (lower) solutions. Right: light curves in the neighborhood of the planet anomaly and best-fit models (upper) and corresponding residuals (lower) for the LPS−3.0 (dotted lines), UPS−2.6 (dotted-dashed lines), and UFS−2.6 (dashed lines) solutions.
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:                       ﹩r^{\prime} -i^{\prime} ﹩ vs. ﹩i^{\prime} ﹩ CMD using stars in the LCOGT template images (﹩26\buildrel{\,\prime}\over{.} 6\times 26\buildrel{\,\prime}\over{.} 6﹩), calibrated with the ATLAS All-Sky Stellar Reference Catalog (Refcat2; Tonry et al. 2018) to the Pan-STARRS1 photometric system (Tonry et al. 2012). The blue and green filled circles represent the source and the blend (i.e., the unlensed light within the PSF), respectively. Our primary interpretation assumes that the blend is the lens.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Left: H I distribution around Clouds 1 (top) and 2 (bottom) from Canadian Galactic Plane Survey data (Taylor et al. 2003; Cloud 1: v LSR = −104.5–99.6 km s−1, Cloud 2: v LSR = −103.7–96.3 km s−1). The gray squares indicate the locations of Clouds 1 and 2. Right: zoomed-in images (top: Cloud 1, bottom: Cloud 2) of the gray squares in the left panels. The magenta contours in the top panel show the integrated 12CO(1–0) map of Digel Cloud 1 from our NRO 45 m data (V LSR = −105.4–98.9 km s−1; Izumi et al. 2014; Izumi et al. 2017). Contour levels are 3σ, 5σ, 7σ, 9σ, and 11σ, where 1σ = 0.92 K km s−1. The magenta contours in the bottom panel show the integrated 12CO(1–0) map of Digel Cloud 2 from our NRO 45 m data (V LSR = −106.1–99.1 km s−1; Izumi et al. 2017), with contour levels at 3σ, 5σ, 7σ, 9σ, and 11σ, where 1σ = 1.35 K km s−1. Contour widths increase with contour levels. The white and cyan rectangles in both panels represent the FoV of the MIRI and NIRCam observations, respectively. The red star in the bottom-right panel marks the location of MR 1 (R.A.: 02h49m22.35, decl.: +58d26m44.6s; Kobayashi & Tokunaga 2000). The green rectangles in both panels are the FoV of the previous Subaru observations. The green dotted polygon in the bottom panel is the FoV of the previous observation with the University of Hawaii telescope. The white filled circle in both panels shows the spatial resolution of the NRO 45 m telescope (∼17″).
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: Host properties of microlensing planets. We use the parameters of the default models (modeldef = 1) in the microlensing planet catalog of the NASA Exoplanet Archive for all discoveries in the bulge field (black dots). The host properties of Kojima-1Lb (blue star) are from Zang et al. (2020), and those of Gaia22dkvLb are based on the globally best-fit UPS−3.3(u 0+) in this work. Panel (A): host mass (M L) vs. distance (D L). Panel (B): host brightness in the V band (m  V ) vs. distance (D L). For the systems in the bulge field, we make crude V-band brightness estimates by assuming the lens star is a main-sequence star with stellar mass M L at D L. We use the isochrone at a stellar age of 5 Gyr from the Dartmouth Stellar Evolution Database (Dotter et al. 2008) to estimate the stellar luminosities. Then we apply the extinction corrections using the near-infrared extinction maps by Gonzalez et al. (2012) and convert it to A  V  with the relationship in Cardelli et al. (1989). Panel (C): Galactic longitude (l) vs. latitude (b) distribution.
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: Semimajor axis (normalized to snow line) vs. planet mass distribution of microlensing planets (black dots: bulge field, red star: Gaia22dkvLb, blue star: Kojima-1-Lb). We scale the projected separation by a factor of ﹩\sqrt{3/2}﹩ (the averaged value assuming random orbital orientation) to estimate the semimajor axis. The parameters are from the same sources as in Figure 16.
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: Simulated Gaia astrometric data and fitted models of the microlens relative to those of the baseline object (i.e., subtracting the baseline coordinates and the effects of its trigonometric parallax and proper motion). The black dots and red lines display the simulated Gaia observations and AL error bars. The error bars in the AC direction are 2 orders of magnitude larger than those in the AL and are not shown. The black solid line represents the best-fit u 0+ model. The blue line shows the best-fit u 0−, which has Δχ 2 ≈ 115 higher than u 0+.
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: Galactic kinematics of the lens (green dot with error bar) and the source (blue dot with error bar) based on the best-fit solution. Upper: Galactocentric distance R and height z with respect to the Galactic plane positions (the red dot represents the Sun at z ⊙ = 25 pc; Jurić et al. 2008). Lower: Toomre diagram. Dashed curves indicate constant peculiar velocities = 50, 100, 150, and 200 km s−1.
Paper: Overview Results of JWST Observations of Star-forming Clusters in the Extreme Outer Galaxy
Authors: Natsuko Izumi, Michael E. Ressler, Ryan M. Lau, Patrick M. Koch, Masao Saito, Naoto Kobayashi, Chikako Yasui
Figure caption: Larger surroundings of our targets: Digel Clouds 1 and 2 in galactic coordinates. The background is the WISE w1, w2, and w4 filters pseudocolor image. This image was made by Astronomers Proposal Tool Aladin Viewer (Bonnarel et al. 2000; Boch & Fernique 2014).