adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of the Extended γ-Ray Emission from the New Supernova Remnant G321.3–3.9 with Fermi-LAT
Authors: Xiaolei Guo, Xi Liu
Figure caption: 4.°0 × 4.°0 TS map for photons above 1 GeV smoothed with a Gaussian kernel of σ = 0.°04. The red crosses show the background and/or foreground sources in the 4FGL-DR4 catalog and the green crosses mark the three 4FGL-DR4 point sources in the region of G321.3–3.9. The white solid circle shows the extension of R68 for the 2D Gaussian template, and the magenta ellipse shows the radio size of G321.3–3.9 (S. Mantovanini et al. 2024). The cyan contours describe the elliptical-shaped radio shell of the SNR G321.3–3.9 by Parkes–MIT–NRAO radio survey at 4.85 GHz (M. R. Griffith & A. E. Wright 1993), and the green contours show the X-ray image in the eROSITA all-sky surveys from 0.2 to 1.0 keV (S. Mantovanini et al. 2024). The inset of the panels in the white square shows the simulated LAT PSF in the same energy range, adopting the same smoothing.
Paper: An Independent Measure of the Kinematic Dipole from SDSS
Authors: Prabhakar Tiwari, Dominik J. Schwarz, Gong-Bo Zhao, Ruth Durrer, Martin Kunz, Hamsa Padmanabhan
Figure caption: The footprints of BOSS and eBOSS tracers in galactic coordinates, along with the location of the CMB dipole (shown as a red star), are illustrated. The panel displaying eCMASS galaxies represents the CMASS galaxies from eBOSS. The final panel shows all the tracers, with only 1% of the sources displayed for visibility.
Paper: Detection of the Extended γ-Ray Emission from the New Supernova Remnant G321.3–3.9 with Fermi-LAT
Authors: Xiaolei Guo, Xi Liu
Figure caption: The γ-ray SED of G321.3–3.9 in the energy range of 100 MeV–1 TeV. The red error bars demonstrate the statistical errors. The sums of the statistical and systematic errors calculated by σ = ﹩\sqrt{{\sigma }_{\mathrm{stat}}^{2}+{\sigma }_{\mathrm{syst}}^{2}}﹩ are marked by the blue error bars. The flux data with 95% upper limits are shown as the arrows, and the gray histogram indicates the TS value for each energy bin. The best-fit log-parabola spectral model in 100 MeV–1 TeV is shown as the green solid line, together with its 1σ statistic error shown as the green dashed lines.
Paper: An Independent Measure of the Kinematic Dipole from SDSS
Authors: Prabhakar Tiwari, Dominik J. Schwarz, Gong-Bo Zhao, Ruth Durrer, Martin Kunz, Hamsa Padmanabhan
Figure caption: The dipole recovery using 1000 EZmocks for LRG tracers. The top panel shows the histogram of the recovered velocity magnitude, and the bottom panel displays the recovered angular position relative to the input (red-filled square) direction. The large blue dot indicates the mean angular position from mocks. The 1σ, 2σ, and 3σ contours indicate measurement errors.
Paper: An Independent Measure of the Kinematic Dipole from SDSS
Authors: Prabhakar Tiwari, Dominik J. Schwarz, Gong-Bo Zhao, Ruth Durrer, Martin Kunz, Hamsa Padmanabhan
Figure caption: The dipole recovery using 1000 random mocks, which includes a clustering dipole of D = 0.86 × 10−2 in the direction (l, b) = (217°, +20°). Other details are the same as in Figure 3.
Paper: Time Variation of the Solar Tachocline
Authors: Sarbani Basu, Wesley Antônio Machado Andrade de Aguiar, Sylvain G. Korzennik
Figure caption: Estimates of r  d  and ΔΩ for different sets of GONG splittings obtained with 10 × 72 days long time series.
Paper: An Independent Measure of the Kinematic Dipole from SDSS
Authors: Prabhakar Tiwari, Dominik J. Schwarz, Gong-Bo Zhao, Ruth Durrer, Martin Kunz, Hamsa Padmanabhan
Figure caption: The redshift distribution of BOSS and eBOSS tracers used in this work.
Paper: Detection of the Extended γ-Ray Emission from the New Supernova Remnant G321.3–3.9 with Fermi-LAT
Authors: Xiaolei Guo, Xi Liu
Figure caption: The multiwavelength SED of the SNR G321.3–3.9. The top panels are for the leptonic models with different values of gas density, and the bottom panels are for the hadronic models. The radio data shown as the magenta dots are from S. Mantovanini et al. (2024). The green solid line shows the synchrotron component. The blue, red, and green dotted lines represent the ICS component of the different seed photons, shown in the legend. The bremsstrahlung component is shown as the magenta dashed line. The black solid curve represents the sum of the different radiation components for the γ-ray emission. In the bottom panels, the red solid and dashed lines indicate the hadronic models with E  p,cut = 3 PeV and E  p,cut = 1 TeV, and the contributions from ICS components are too low to show in the bottom right panel.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: This MIRI image is a combination of four filters: F770W is in blue, F1000W is in cyan, F1500W is in yellow, and F2100W is in red. This image was made by ESA/NASA/CSA/STScI. The central source within H72.97-69.39 is emitting strongly at the longest (i.e., reddest) wavelengths, an indication that it is still embedded, and therefore is still in the process of forming. The blue and cyan colors represent wispy filament-like structures of possible PAH emission.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: The F700W – F1000W vs. F1000W CMD. There are 133 sources that have F770W – F1000W > 0.1; of these 133 sources, 58 have only two photometric points and we are unable to constrain their SEDs, while for the remaining 72 sources, we fit all available photometric points for each sources with model YSO SEDs from T. P. Robitaille (2017). We find three of the 72 red sources do not have well-fit models to the observed data (reduced χ 2 > 10), which we show with green triangles.
Paper: Detection of the Extended γ-Ray Emission from the New Supernova Remnant G321.3–3.9 with Fermi-LAT
Authors: Xiaolei Guo, Xi Liu
Figure caption: Typical γ-ray SEDs of various γ-ray luminous SNRs (M. Ackermann et al. 2013; H.E.S.S. Collaboration et al. 2018a, 2018b). The energy fluxes of the SNR G321.3–3.9 are scaled upward by 40 times for spectral shape comparison with other γ-ray SNRs.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: Six YSO candidates fit with T. P. Robitaille (2017) SED models. These are sources with at least three photometric points and within the color cut F770W – F1000W > 0.5. The black circles are the observed photometry, the black line is the best-fit model to the observations, and the gray lines are all models with Δχ 2 < 3 compared to the best-fit model.
Paper: Detection of the Extended γ-Ray Emission from the New Supernova Remnant G321.3–3.9 with Fermi-LAT
Authors: Xiaolei Guo, Xi Liu
Figure caption: The velocity-integrated CO emission intensity with the unit of K km s−1 around the SNR G321.3–3.9 (T. M. Dame et al. 2001). The 68% containment radius of the extended γ-ray emission is marked by the white solid circle. The cyan contours show the radio image of G321.3–3.9 at 4.85 GHz, as shown in the left panel of Figure 1.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: We plot the five YSOs and 97 YSO candidates separated by evolutionary stage on the MIRI F1000W wavelength image. Left: 55 Stage I YSO candidates. Center: 19 Stage II YSO candidates. Right: 28 Stage III YSO candidates. We overlay a green circle with radius 59″ (14.8 pc) within which 70% of the YSO mass is contained.
Paper: Embedded Young Stellar Objects near H72.97-69.39: A Forming Super Star Cluster in N79
Authors: Omnarayani Nayak, Conor Nally, Alec S. Hirschauer, Olivia C. Jones, Jeroen Jaspers, Laura Lenkić, Margaret Meixner, Nolan Habel, Megan Reiter, Laurie Chu, Patrick J. Kavanagh, Massimo Robberto, B. A. Sargent
Figure caption: Top left: effective temperature histogram of the five spectroscopically confirmed YSOs and 97 YSO candidates in this work. Top right: luminosity histogram of the YSO candidates. Bottom left: stellar radius histogram of the YSO candidates. Bottom right: mass histogram of the YSO candidates.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Overview of the time-domain correlation method. (a) Intensity signals extracted from the DT plots, with r 1 (red) and r 2 (blue) representing the radial distances. (b) Detrended intensity signals for r 1 (red) and r 2 (blue) used in the TDC method. (c) Determination of the peak in the cross-correlation coefficient: the solid black line represents the TDC without interpolation, while the red dashed line indicates the refined peak after interpolation. (d) Velocity measurements obtained using the TDC method: the blue line shows the velocity without interpolation, and the red dashed line represents the corrected velocity after interpolation.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Fine-scale structures associated with the velocity distribution. Top: an L7 snapshot with several features of interest annotated. The velocity distribution overlaid indicates that some anomalies in the velocity profile align with the highlighted features. Bottom: the same image processed using the Sobel operator (refer to C. DeForest et al. 2018 for more details) to emphasize brightness gradients (edges). The velocity plot uncovers the fine-scale structures in the highlighted image, matching the minor irregularities observed in the solar velocity profile. Background image adapted from C. DeForest et al. (2018). Note: this figure has the polar angle plotted as specified by C. DeForest et al. (2018), which is measured clockwise from the west limb. In all other sections of this paper, we adopt the convention of measuring the polar angle counterclockwise from the north pole.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Measured velocity distribution around the Sun at different position angles. The observed velocity anomalies between position angles may indicate the presence of CMEs in the STEREO data, as mentioned by C. DeForest et al. (2018), due to the setup of the velocity measurement method. The superimposition of the velocity plot on the coronagraph image emphasizes the slow CME at the velocity kink.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Analysis of velocity measurement errors. (a) Probability distribution histograms for the velocity discrepancy using two approaches, the ST in blue and the TDC in red. The ST shows a broader distribution, indicating more variability in velocity discrepancy, with mean, standard deviation, and median calculations included. (b) Semi-log graph showing log p vs. velocity discrepancy. The TDC shows increased occurrence of larger discrepancies, while the ST demonstrates greater stability under varying conditions.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Simulated profile and its analysis. (a) Speed profile analysis of solar parameters. Black dashes show the speed profile measured from COR2 data using the TDC and used to create SynCOM images with solar parameters; blue: speed profile of the ST; red: TDC speed profile. (b) Illustration of the difference between simulated and measured speeds. Red: the speed difference for the TDC; blue: the speed difference for the ST.
Paper: SynCOM: An Empirical Model for High-resolution Simulations of Transient Solar Wind Flows
Authors: Valmir P. Moraes Filho, Vadim M. Uritsky, Barbara J. Thompson, Sarah E. Gibson, Craig E. DeForest
Figure caption: Distance–time plot showing two intensity signals at different altitudes.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Initial t E–π E plane, populated with the results from the parallax PSPL fit to all Spitzer events (gray points). Colored crosses and circles mark all the events that were also observed by the Gaia mission and published either through GSA (blue) or in Ł. Wyrzykowski et al. (2023; green). Red diamonds mark those events that were selected for detailed analysis, as they host potentially massive lenses. For a given value of relative lens–source proper motion, one can draw a line of constant lens mass. Assuming a typical value of μ rel = 4 mas yr−1, all the events lying below the gray line would be caused by lenses heavier than 1.4 M ⊙, while those below the black line are caused by lenses heavier than 2.5 M ⊙. To visualize the impact of proper motion, we also plot the dashed–dotted line for μ rel = 2 mas yr−1 and M  L  = 2.5 M ⊙. We note that there are two groups of events with faulty fits: one with high values of t E (∼500 days), and the other with π E (∼2); see Section 2.4 for details.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Same as Figure 3, but for the remaining five events. For the case of OGLE-2018-BLG-0483 the Spitzer data allowed only for estimation of the upper limit on the flux, which excludes part of the π EN−π EE space (marked with red hatched area in panels (m) and (n)). The magenta contours in panels (k) and (l) represent ground-based-only fits with fixed blending parameter g = 0.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Posterior distributions for lens mass and distance, under the assumption of the Kroupa mass function (slope α = −2.35)—see text for the details. The orange, yellow, cyan, light-blue, and dark-blue contours mark 1σ, 2σ, 3σ, 4σ, and 5σ confidence levels, respectively. Note that we show the distributions for all the possible solutions (both u 0+ and u 0− models for each event), even though some of them can be rejected based on the light-curve analysis. We list the results for preferred solutions in Table 4.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: CMDs for all the massive lens candidate events, constructed from the indicated catalog of stars (mostly OGLE, in all events but OGLE-2015-BLG-0211) in a ﹩2{\rm{^{\prime} }}\times 2{\rm{^{\prime} }}﹩ box around the magnified object. The large red circles mark positions of the source stars, while the cyan circle marks the color and brightness of the baseline (i.e., including blend). They overlap whenever the blending is low, which is the case for almost all events in the subsample, excluding OGLE-2016-BLG-0689.
Paper: Analysis of the Full Spitzer Microlensing Sample. I. Dark Remnant Candidates and Gaia Predictions
Authors: Krzysztof A. Rybicki, Yossi Shvartzvald, Jennifer C. Yee, Sebastiano Calchi Novati, Eran O. Ofek, Ian A. Bond, Charles Beichman, Geoff Bryden, Sean Carey, Calen Henderson, Wei Zhu, Michael M. Fausnaugh, Benjamin Wibking, Andrzej Udalski, Radek Poleski, Przemek Mróz, Michał K. Szymański, Igor Soszyński, Paweł Pietrukowicz, Szymon Kozłowski, Jan Skowron, Krzysztof Ulaczyk, Patryk Iwanek, Marcin Wrona, Yoon-Hyun Ryu, Michael D. Albrow, Sun-Ju Chung, Andrew Gould, Cheongho Han, Kyu-Ha Hwang, Youn Kil Jung, In-Gu Shin, Hongjing Yang, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Hyoun-Woo Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge, Fumio Abe, Richard Barry, David P. Bennett, Aparna Bhattacharya, Akihiko Fukui, Ryusei Hamada, Shunya Hamada, Naoto Hamasaki, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Naoki Koshimoto, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Tutumi Nagai, Kansuke Nunota, Greg Olmschenk, Clement Ranc, Nicholas J. Rattenbury, Yuki K. Satoh, Takahiro Sumi, Daisuke Suzuki, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Łukasz Wyrzykowski, Kornel Howil, Katarzyna Kruszyńska
Figure caption: Light curves of all the events from our Spitzer–Gaia subsample, with all the data sets used during the modeling. Solid lines represent the best fit of the PSPL+parallax model, showing Earth/Gaia (black line) and Spitzer (red line) perspectives. The ground-based data from all the surveys are plotted together (blue circles). All models and data points are displayed with respect to I OGLE baseline brightness. For the case of OGLE-2018-BLG-0483 we only derive limits on the Spitzer flux, which are represented by downward-pointing triangles. The inset in the bottom left panel shows residuals of the region with a small deviation that might have been caused by a low-mass companion to the lens (see details in the text).