adsabs/AstroCLIMB huggingface dataset:
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: FWHM (top left), aperture flux (top right), PA (bottom left), and eccentricity (bottom right) results for MS V1, K  V1, and RL V1 as a function of simulated central wavelength.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Same as Figure B2, but for D AGN, D  V3, and D  V4.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Same as Figure B2, but for MS V2, K  V2, and RL V2.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: High to low S/N MS V6 images, where the S/N for each image is given in the title. Each image is displayed log scaled, scaled to the corresponding D  V6 image peak (Figure B10), and shows the central 150 × 150 MIRIM pixels. The input model variation (V 6) number is given as an inset in each image.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: MS V6 and D  V6 aperture signal measurements for AStotal (left) and ASsmall (right) as a function of S/N.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: FS detection comparisons between MS V5 (right) and D  V5 (left). Each image is log scaled and shows the central 60 × 60 MIRIM pixels. For both images the centroid locations of the nucleus and FS are marked with a “+” and the FS detected with a 3σ certainty is highlighted with a black aperture.
Paper: Deconvolution of JWST/MIRI Images: Applications to an Active Galactic Nucleus Model and GATOS Observations of NGC 5728
Authors: M. T. Leist, C. Packham, D. J. V. Rosario, D. A. Hope, A. Alonso-Herrero, E. K. S. Hicks, S. Hönig, L. Zhang, R. Davies, T. Díaz-Santos, O. González-Martín, E. Bellocchi, P. G. Boorman, F. Combes, I. García-Bernete, S. García-Burillo, B. García-Lorenzo, H. Haidar, K. Ichikawa, M. Imanishi, S. M. Jefferies, Á. Labiano, N. A. Levenson, R. Nikutta, M. Pereira-Santaella, C. Ramos Almeida, C. Ricci, D. Rigopoulou, W. Schaefer, M. Stalevski, M. J. Ward, L. Fuller, T. Izumi, D. Rouan, T. Shimizu
Figure caption: Same as Figure B9, but for the D  V6 images.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Steps and accuracy of the close-loop positioning. Left: Steps needed to reach the points within the required accuracy before, after, and after calibration using the pulse-reduction strategy. Right: Corresponding accuracy of positioning after at most four steps.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Simulation results of errors caused by pulse reduction. Left and middle: errors caused by the pulse reduction of alpha and beta arms, respectively. Right: errors caused by pulse reduction.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Comparison of the positioning precision before and after calibration.
Paper: The Calibration of theta-phi Fiber Positioners Based on the Differential Evolution Algorithm
Authors: Feifan Zhang, Ye Huang, Baolong Chen, Longfeng Yu, Yu Wang, Zengxiang Zhou, Jianping Wang
Figure caption: Workflow of the proposed calibration algorithm.
Paper: Orbit of the Patroclus–Menoetius Binary System and Predictions for the 2024/2025 Mutual Events Season
Authors: Marina Brozović, Robert A. Jacobson, Ryan S. Park, Pascal Descamps, Jérôme Berthier, Noemí Pinilla-Alonso, Marcel Popescu, Javier Licandro
Figure caption: Model fits to the mutual events lightcurves from 2012 June to November.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: A comparison of the SED of the prototype blazar source BL Lacertae obtained with Firmamento and other online SED tools. Firmamento data is shown as filled red points, SSDC SED builder as open light-blue circles, NED as magenta open squares, and Vizier as orange open diamonds. The SED in the inset, adapted from Giommi et al. (1995), illustrates the amount of multifrequency data available from public sites in the mid 1990s.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: Example of a possible identification of a blazar counterpart in the error ellipse of a still-unidentified gamma-ray source. Top left: the user selects a source from the list of unidentified Fermi 4FGLDR3 detections. Top right: the 4FGLDR3 localization error ellipse of the chosen source with a possible blazar counterpart appearing as an orange symbol. Lower left: the SED of the blazar candidate. Lower right: the error regions of cataloged radio and X-ray sources (red and blue circles) matching the position of the candidate blazar are superposed to the image from an optical survey chosen in the Firmamento Aladin interface.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: Top left: the error circle of the source eFEDS J085920.5+004711 including the blazar 5BZB J0859+0047. On the lower left is shown the very small error circle overlaid to the Sloan Digital Sky Survey optical image of this part of the sky. Right: the SED of the Blazar 5BZB J0859+0047 = eFEDS J085920.5+004711 generated with Firmamento. The red points are from the eRosita eFEDS survey.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: The name or the position of an astronomical source, or of a localization error to be processed by Firmamento can be provided by specifying a source name or a set of R.A., decl. coordinates, or selecting one entry from a list uploaded by the user (top), or by choosing an entry from one of the lists provided, e.g., the table of eROSITA detections from the eFEDS survey matching flat-spectrum radio sources, as in the lower part of the figure.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: The SED of the well-known source named BL Lacertae, the archetype of the class of blazars. The right side shows part of the corresponding data file, which can be downloaded by clicking next to the chosen format.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: The correlation between the average 3.4–4.6μ spectral slope and ν peak in the subsample of blazars frequently observed by Swift whose IR emission can be attributed to the jet.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: The 90% localization uncertainty of the IceCube neutrino track IceCube200107A and the SED of the possible electromagnetic counterpart 3HSP J095507.1+355100. See text for details.
Paper: Firmamento: A Multimessenger Astronomy Tool for Citizen and Professional Scientists
Authors: Dhurba Tripathi, Paolo Giommi, Adriano Di Giovanni, Rawdha R. Almansoori, Nouf Al Hamly, Francesco Arneodo, Andrea V. Macciò, Goffredo Puccetti, Ulisses Barres de Almeida, Carlos Brandt, Simonetta Di Pippo, Michele Doro, Davit Israyelyan, A. M. T. Pollock, Narek Sahakyan
Figure caption: A schematic view of Firmamento’s architecture.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: CPVs found in the TESS 2 minute data. Phased TESS light curves over 1 month are shown for 50 CPVs in the high-quality sample. Gray are raw 2 minute data; black bins to 300 points per cycle. Objects are ordered such that sources with the most TESS data available are on top (see Section 3.1). Zero phase is chosen to correspond to minimum light. Each panel is labeled by the TIC identifier, the TESS sector number, the period in hours, and the three-bit binarity flag from Table 1, which denotes Gaia DR3 radial_velocity_error outliers (bit 1), Gaia DR3 ruwe outliers (bit 2), and stars with secondary TESS periods (bit 3).
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Properties of CPVs identified by our search. CPVs are mostly pre-main-sequence M dwarfs, younger than ≈150 Myr, with rotation periods faster than ≈1 day. The 50 bona fide CPVs in Table 1 are the dark blue dots; 13 ambiguous CPV candidates are light blue dots. Unresolved binaries (red rings) are objects for which the Gaia DR3 radial velocity scatter exceeded 20 km s−1, or if Gaia RUWEDR3>2 and multiple photometric signals were present in the TESS light curve. The top panels show the 65,760 target stars with 2 minute cadence TESS data as the shaded gray background; darker regions correspond to a larger relative number of searched stars. The lower left panel compares the rotation–color distribution of CPVs against the rotation periods of K and M dwarfs in the Pleiades from Rebull et al. (2016). The lower middle panel plots the derived corotation radii ﹩{R}_{{\rm{c}}}={({GM}/{{\rm{\Omega }}}^{2})}^{1/3}﹩ in units of stellar radii against the measured CPV periods, in units of hours. Ages in the final panel are known from cluster membership.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Completeness of the TESS 2 minute data for late-K and early M dwarfs near the Sun, from Sectors 1–55. The orange dotted curve shows the number of stars in successive radial shells, each with a width of 10 pc. To be part of our selection function, these stars must meet the following conditions: they must be red dwarf stars (G BP − G RP > 1.5; M  G  > 4) amenable for TESS observations (T < 16). The blue solid curve shows the fraction of such stars with at least one sector of TESS 2 minute cadence data acquired between Sectors 1–55.
Paper: Transient Corotating Clumps around Adolescent Low-mass Stars from Four Years of TESS
Authors: Luke G. Bouma, Rahul Jayaraman, Saul Rappaport, Luisa M. Rebull, Lynne A. Hillenbrand, Joshua N. Winn, Alexandre David-Uraz, Gáspár Á. Bakos
Figure caption: Complex periodic variables (CPVs). Top: Phase-folded TESS light curves for three CPVs. Each panel shows the average of the data accumulated over 1 month, relative to the mean stellar brightness. Gray circles are raw 2 minute data; black circles are binned to 300 points per cycle. The period in hours is printed in the bottom right corner. Left to right, the objects are LP 12-502 (TIC 402980664; Sector 19), TIC 94088626 (Sector 10), and TIC 425933644 (Sector 28). Bottom: Cartoon configurations for magnetically entrained corotating material. The dust clump scenario (left) and gas prominence scenario (right) propose different opacity sources, and different occultation geometries.
Paper: Detecting Biosignatures in Nearby Rocky Exoplanets Using High-contrast Imaging and Medium-resolution Spectroscopy with the Extremely Large Telescope
Authors: Huihao Zhang, Ji Wang, 吉 王, Michael K. Plummer
Figure caption: The albedos of H2O, CO2, CH4, and O2 in the atmosphere of modern Earth. The interval where the albedo of a gas exceeds 0.15 is considered as the feature wavelength for that gas. The black dashed line is the criterion for albedo of 0.15. The wavelengths where two or more gases have overlapping features will not be considered as feature wavelengths. The wavelengths of the intervals with albedos higher than 0.15 are described in Table 3.
Paper: Detecting Biosignatures in Nearby Rocky Exoplanets Using High-contrast Imaging and Medium-resolution Spectroscopy with the Extremely Large Telescope
Authors: Huihao Zhang, Ji Wang, 吉 王, Michael K. Plummer
Figure caption: TRAPPIST-1 e photon flux detected on Earth, assuming TRAPPIST-1 e has a biosignature-free and modern Earth atmosphere. The difference between the two curves is caused by biosignature gases. The greater the differences, the stronger the impact of gases on the observed spectrum, resulting in a higher S/N of gases. We assumed a spectral resolution of 1000.
Paper: Detecting Biosignatures in Nearby Rocky Exoplanets Using High-contrast Imaging and Medium-resolution Spectroscopy with the Extremely Large Telescope
Authors: Huihao Zhang, Ji Wang, 吉 王, Michael K. Plummer
Figure caption: Top: flux of TRAPPIST-1 from SIMBAD vs. flux of TRAPPIST-1 from BT-Settl. Bottom: the residual between SIMBAD and BT-Settl in percent. For comparison, we choose data from the R, i, Z, J, H, K, and W 1 bands in SIMBAD.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Color temperature map, annotated with all compact objects and extended features. Previously known features are marked in green, and newly reported ones are marked in cyan.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: The inner half-parsec region of the Galactic center as observed in the L′ band (3.8 μm) of the NIRC2 imager at the Keck Observatory. The coordinate offsets in this figure, and in all other figures in this paper, are relative to the position of Sgr A* (Reid & Brunthaler 2004), which is marked with a cyan plus sign. The cyan circle encloses the domain of the known G objects (Ciurlo et al. 2020).
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: The inner parsec region of the Galactic center as observed with the PAH1 band (8.6 μm) of the VISIR imager at the VLT. The position of Sgr A* is marked with a cyan plus sign. Extended features such as the northern arm curling in along the left-hand side of the image dominate this band.
Paper: High-resolution, Mid-infrared Color Temperature Mapping of the Central 10″ of the Galaxy
Authors: Cuc K. Dinh, Anna Ciurlo, Mark R. Morris, Rainer Schödel, Andrea Ghez, Tuan Do
Figure caption: Optical depth map at L′ (3.8 μm), with contours at τ = 0.007, 0.014, and 0.028. The little variation in temperature yields what is essentially an inverted map; low-temperature features such as the northern arm translate into a higher optical depth analog.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Distribution of our initial sample (blue points) and results of this work (red star points) in Galactic coordinates.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: CMDs of some examples in our sample in the LISC catalog. Blue points denote the observed CMDs.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Comparison of CMDs the observed and the best-fitting based on Powerful CMD for some clusters with r  n  < 0.02.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: CMDs and parallax distributions of some examples in this work. Black points denote the CMDs resulted from the pyUPMASK method, and blue points denote the CMDs selected within the 1σ (blue dotted line) from the mean value following Gaussian distribution of parallax (red dotted line).
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Similar to Figure 8, but for some clusters with r  n  ≥ 0.02.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Comparison between the G vs. (G BP − G RP) and the V vs. (V − I) in CMDs for some clusters. The 1D plots show distributions of the color, magnitude and residual. The 2D density contours are the confidence containing 1σ(68%) and 2σ(95%) of the color and magnitude distribution space.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Observed CMDs (blue points) and best-fitting theoretical isochrones (red points) are presented for some examples based on Padova database. l and b are the Galactic longitude and Galactic latitude respectively.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Comparison of the CMDs between in LISC and this work.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Comparison between a good matched sample (top panels) and a mismatched one (bottom panels).
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: CMDs (a), distributions of parallaxes (b), coordinates (c), and proper motions (d) for five potential binary clusters of this work.
Paper: Revisit of 77 Clusters Candidates with Multiple Main Sequences using Gaia DR3
Authors: Jing Chen, Zhongmu Li, Su Zhang, Wenchang Zhao, You Wu
Figure caption: Correlation coefficient between cluster parameters. The darker the color of the rectangle, the larger the correlation coefficient, and the shadow area of the circle are similar.