adsabs/AstroCLIMB huggingface dataset:
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: (a) Source images obtained at an average energy of 4.6 keV. (b) The on-axis PSF of the telescope is modeled as the sum of a Gaussian core and a King function, along with a power-law component that dominates the outer regions of the field of view.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: Spurious-modulation measurements at MSFC compared with data taken at INAF-IAPS on a flat field illumination of 3.57 mm radius.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: The test facility crystal box.
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: (a) IXPE MMA in test facility. (b) Focal plane test detectors including a CCD camera, a fast silicon drift detector (SDD) and the flight-spare IXPE detector unit (circled).
Paper: The Telescope Calibration of the Imaging X-Ray Polarimetry Explorer
Authors: Brian D. Ramsey, Jeffery K. Kolodziejczak, Wayne H. Baumgartner, Nicholas E. Thomas, Stephen D. Bongiorno, Philip Kaaret, Stephen L. O'Dell, Allyn Tennant, Martin C. Weisskopf, Sergio Fabiani, Fabio Muleri, Paolo Soffitta, Enrico Costa, Alessandro Di Marco, Riccardo Ferrazzoli, Fabio La Monaca, John Rankin, Ajay Ratheesh, Alessio Trois, Luca Baldini, Ronaldo Bellazzini, Alessandro Brez, Luca Latronico, Leonardo Lucchesi, Alberto Manfreda, Massimo Minuti, Leonardo Orsini, Michele Pinchera, Carmelo Sgrò, Gloria Spandre
Figure caption: The summary of the modulation factor calibration at MSFC and at INAF-IAPS (3.57 mm dither) showing good agreement.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Residual phases in radian of secondary calibrators and estimated phase corrections for the target (V1859 Ori). Phases are in radians. Left panels: baseline BR-PT. Right panels: baseline HN-PT. Top panels: original sequences. Middle panels: flagged sequences for sMV. Bottom panels: flagged sequences for cMV. Semitransparent calibrator scans are flagged and not used for sMV or cMV. Target scans within time ranges with pink background are not used in imaging.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Images of V1859 Ori in BZ087B1 calibrated with different techniques. cMV⋆ and sMV⋆ denote cMV and sMV with flagged sequence respectively. Image size is 128 × 128 with a cell size of 0.5 mas. Contour levels are [−0.05, 0.05, 0.3, 0.55, 0.8] × peak flux density, in which the −0.05 level is shown in dashed line. The restored beam is shown at the bottom-left corner of each panel.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Schematic of a ternary tree with a depth n = 3. Red (dashed line) subtrees are pruned. Losses of leaf nodes calculated from Equation (2) are listed below, and the green branch is chosen as the “best,” so “±0” (at depth n = 1) is selected as the phase-wrap solution for this step.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Original observing sequence and the flagged sequences. Gray cells are flagged to simulate a 1/3 sampling rate of secondary calibrators. Time length in seconds of each scan is shown in each cell.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Flowchart of the recursive function used for creating the ternary tree of phase-wrap solutions (preorder traversal). “Overlimit” means the pruning threshold is reached, while “max depth” means the leaf node has been reached.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Flowchart of the recursive function used for traversing the ternary tree of phase-wrap solutions (post-order traversal). “max depth” means the leaf node has been reached.
Paper: Serial MultiView: An Efficient Approach to Mitigating Atmospheric Spatial-structure Errors for Very-long-baseline-interferometry Astrometry
Authors: Jingdong Zhang, Bo Zhang, Shuangjing Xu, Maria J. Rioja, Richard Dodson, Xiaofeng Mai, Oleg Titov
Figure caption: Images of V1859 Ori in BZ087B2 calibrated with different techniques. All notations are kept the same as Figure 8.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: The orbits of the HD 22879 (a), HD 144579 (b), HD 188510 (c), and HD 201891 (d) around the Galactic center. The red-ringed yellow circles in the panels indicate the current positions of the stars, and the red arrows show their direction of motion.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Corner plot illustrating the two-dimensional joint and one-dimensional marginalized posterior distributions for the properties of four stars. The contours in the two-dimensional joint posterior distributions represent the confidence levels of 68%, 90%, and 95%. In the one-dimensional posterior distributions, the vertical lines indicate the median and the 16th and 84th percentile confidence intervals. The ﹩{M}_{{\rm{G}}}\times {({G}_{{\rm{BP}}}-{G}_{{\rm{RP}}})}_{0}﹩ CMDs of the stars (red stars) are shown on the right side of the corner plots. The black solid lines are the PARSEC isochrones derived from the median values of the posterior distributions, and black dashed lines indicate the calculated age errors of the stars.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: The positions of the stars on the Toomre diagram. The stars were color-coded according to their space-velocity errors. The color scale in the upper panel shows the errors in total space velocity. The red curves in the figure represent velocity values of 50 km s−1, whereas the dashed line in the gray region corresponds to a velocity of SLSR = −230 km s−1 (L. Necib & T. Lin 2022).
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: The standard deviation of the Ti, Cr, and Fe abundances from the suite of Ti I, Ti II, Cr I, Cr II, Fe I, and Fe II lines as a function of ξ.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Best-fitting SED model for HD 22879 (a), HD 144579 (b), HD 188510 (c), and HD 201891 (d). The black curve represents the best-fitting model, whereas the cyan pluses and circles denote the retrieved photometric measurements. The blue diamonds correspond to synthetic photometry.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Corner plot illustrating the posterior distributions for four stars, with confidence contours at 68%, 90%, and 95%. One-dimensional distributions indicate the median and 16th/84th percentile intervals. The positions of the stars in the Kiel diagram are shown on the right-hand side of the panels. Definitions are as provided in the previous Figure 5.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Posterior distributions from the best-fit SED model for HD 22879 (a), HD 144579 (b), HD 188510 (c), and HD 201891 (d) are shown. Red points indicate mean posteriors, and red vertical lines represent 16, 50, and 84 percentiles, respectively.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Small regions of the spectra for HD 188510, HD 201891, HD 22879, and HD 144579. For convenience, the spectra were shifted vertically. A selection of neutral and ionized lines used in the analysis are indicated by a vertical dashed line.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Comparison of stellar atmospheric parameters derived from Gaia catalog data and three different methods with literature values. The red star symbols represent Gaia results, pink triangles indicate photometric and astrometric analysis, green circles correspond to literature values, blue circles denote SED analysis results, and yellow plus signs show parameters determined via spectroscopic analysis.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Ö. Önal Taş et al. (2018) showing the Galactic center, bulge, CR, OLR (W. Dehnen 2000), and the Sun’s position (R0 = 8 kpc). It also illustrates the metallicity variation within the two ﹩{Z}_{{\rm{\max }}}﹩ ranges (﹩0\lt {Z}_{{\rm{\max }}}\,{\rm{(kpc)}}\,\leqslant \,﹩ 0.5, and ﹩0.5\lt {Z}_{{\rm{\max }}}\,{\rm{(kpc)}}\,\leqslant \,﹩ 1) based on the MW and MWBS models represented by different colors. The blue star symbol represents the three stars studied in this study.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Element abundance patterns ([X/Fe]) for four stars (blue) and GCs (red). Each panel compares the chemical abundances of a star with those of a GC, showing variations across different elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, and Cr). Error bars represent the measurement uncertainties. The lower section of each panel illustrates the abundance differences (Δ[X/Fe]) between the star and the GC.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: The Galactic orbits on the Galactic X–Y and X–Z planes have been calculated for the GC of which the four stars studied are members with the highest probability. The blue line indicates the orbits of the stars, while the gray lines represent the orbits of the GCs.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: Likelihood of stars encountering various GCs, based on spatial and velocity parameters. The matrix displays three key probability values: spatial probability (P(θ)), velocity probability (P(ν)), and combined probability (P(origin∣θ, ν)) for each cluster. Colors in the matrix reflect the probability values, as indicated by the scale.
Paper: Tracing the Galactic Origins of Selected Four G-type Stars in the Solar Neighborhood
Authors: Deniz Cennet Çınar, Selçuk Bilir, Timur Şahin, Olcay Plevne
Figure caption: The chemical and kinematic classification of Galactic populations for the stars examined in this study, compared to 714 FGK stars from T. Bensby et al. (2014). The red circle denotes a halo star, the green circle indicates a TD star, the blue circle represents a thin-disk star, and the yellow triangle corresponds to the four stars analyzed in this study.
Paper: MEGA Mass Assembly with JWST: The MIRI EGS Galaxy and Active Galactic Nucleus Survey
Authors: Bren E. Backhaus, Allison Kirkpatrick, Guang Yang, Gregory Troiani, Kurt Hamblin, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Erini Lambrides, Casey Papovich, Kaila Ronayne
Figure caption: MEGA MIRI imaging (red), with CEERS MIRI imaging (blue), and CEERS NIRCam imaging (gray).
Paper: MEGA Mass Assembly with JWST: The MIRI EGS Galaxy and Active Galactic Nucleus Survey
Authors: Bren E. Backhaus, Allison Kirkpatrick, Guang Yang, Gregory Troiani, Kurt Hamblin, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Erini Lambrides, Casey Papovich, Kaila Ronayne
Figure caption: Final mosaic before any background subtraction (left), after one iteration of super background subtraction (middle), and after three iterations of super background subtraction (right) for the F770W filter (top) and F2100W filter (bottom). With further iterations of super background subtraction, the row and column striping improves and produces a more uniform background.
Paper: MEGA Mass Assembly with JWST: The MIRI EGS Galaxy and Active Galactic Nucleus Survey
Authors: Bren E. Backhaus, Allison Kirkpatrick, Guang Yang, Gregory Troiani, Kurt Hamblin, Jeyhan S. Kartaltepe, Dale D. Kocevski, Anton M. Koekemoer, Erini Lambrides, Casey Papovich, Kaila Ronayne
Figure caption: Red-blue-green image of MEGA pointings using all four of the MEGA filters. The zoomed-in areas show HST F606W, NIRCam F444W, MIRI F770W, and MIRI F2100W.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: The MZR (left panel) and FMR (right panel) of the BGS sample across different redshift bins. Each colored line represents the fitted MZR or FMR for a specific redshift range. The colors transition from yellow and red to green as redshift increases. The legend provides detailed information about the specific redshift bins represented by each line.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: MZR for the ELG sample, with solid black contours representing the regions that enclose 68% and 95% of the data distribution. The purple line shows the ELG fitted MZR. Comparative trends are provided for reference: the yellow line represents the relation from N. Oi et al. (2017) at z ≈ 0.88, and the green line represents the relation from K. Yabe et al. (2014) at z ≈ 1.4 with the dashed line representing the extrapolated parts. Uncovered data points, which lie outside the 95% contour, are plotted as gray dots. The typical uncertainty is depicted by the error bar located in the lower-right corner.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: The MZR for the BGS sample, with solid black contours representing the regions that enclose 68% and 95% of the data distribution. The red dashed line shows the BGS fitted MZR. Comparative trends from J. Nadolny et al. (2020) are provided for reference: the purple line corresponds to the z ≈ 0.1 SDSS sample, the blue line to the z ≈ 0.31 SDSS sample, and the yellow line to the z ≈ 0.32 GAMA sample. Uncovered data points, which lie outside the 95% contour, are plotted as gray dots. The typical uncertainty is illustrated by the error bar located in the lower-right corner.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: The left panel shows the MZR for ELGs in red and BGS in green. The right panel presents the FMR using ﹩{\mu }_{0.32}=\mathrm{log}{M}_{\star }-0.32\mathrm{log}\mathrm{SFR}﹩. Contours represent galaxy distributions, and dashed lines indicate the fitted trends.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: These panels show three classic BPT diagrams, based on the emission-line ratios [N II]/Hα, [S II]/Hα, and [O II]/Hβ. Light-blue points represent star-forming galaxies, and red points indicate galaxies hosting AGNs. The solid lines are the empirical classification boundaries proposed by G. Kauffmann et al. (2003), L. J. Kewley et al. (2001), and F. Lamareille (2010), with modifications done by H. Zou et al. (2024), respectively, in (a), (b), and (c).
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: Histograms of logarithmic SFR (log(SFR)) distribution (top) and sSFR distribution (bottom) for BGS and ELG samples.
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: Contour plot showing the distribution of log(sSFR) versus μ0.32 for BGS (blue) and ELG (orange) samples
Paper: Exploring the Mass–Metallicity Relationships with the DESI BGS and ELG Samples
Authors: Yunxiao Jia, Hu Zou, Ali Luo, Wen Hou, Shuguo Ma, Jipeng Sui
Figure caption: Histograms of stellar mass distribution (top) and stellar mass error distribution (bottom) for BGS and ELG samples.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Keck K-band data from August 5 (top panels) and August 6 (bottom panels), showing a zoom of the target, the one-star residual where the source is subtracted, and the two-star residual where both the source and lens are subtracted. In the one-star residual frame the source and lens positions are indicated in red and cyan, respectively.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Bayesian probability distributions of the planetary system, including host mass and distance, separation, and planetary companion mass. Orange represents πE,N > πE,E − 0.33 values, and green respresents πE,N < πE,E − 0.33 values. The central 68.3% of the distributions are shaded in darker hues (of either orange or green) and the remaining central 95.4% of the distributions are shaded in lighter hues. The vertical black line marks the median of the probability distribution of the respective parameters for the large and small πE values.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: Corner plot from the MCMC probability distribution showing the parameters due to the microlensing parallax, orbital motion, xallarap, and magnification of the secondary source.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: From left to right: the first panel shows the stacked image of the 2018 HST I-band data, and the second shows a zoom of the target with the constrained lens and source positions indicated in cyan and red, respectively. The third and fourth panels show the one- and two-star fits to the target, respectively. The faint lens star cannot be directly identified in these images, however, since we know the lens-source separation from the Keck analysis, we can measure the lens and source magnitudes with a fit that constrains their separation to be the same as measured from the Keck data.
Paper: MOA-2010-BLG-328: Keck and HST Expose the Limits of Occams Razor in Microlensing
Authors: Aikaterini Vandorou, David P. Bennett, Jean-Philippe Beaulieu, Aparna Bhattacharya, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Naoki Koshimoto, Clément Ranc, Natalia E. Rektsini, Sean K. Terry
Figure caption: CMD of OGLE III stars within 120″ of the MB10328 microlensing event, in gray. In orange is the color–magnitude diagram of the HST field from the 2018 epoch transformed to the same extinction and Galactic bar distance. The red clump giant centroid is indicated with a red dot. The purple marker is the primary source (S1), and the blue markers show the secondary source (S2) color and magntitude. The green markers represent the lens. The diamond markers indicate the values for the small πE distribution, while the circles indicate values for the large πE. For S1, the difference and the error bars are too small to be seen on the figure.