adsabs/AstroCLIMB huggingface dataset:
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: Schematic of a 2+1+1 quadruple, showing how star B would slow down binary A relative to star C on the sky. Both the center of mass of the A binary and star C would, for a small fraction of the orbit of the AB binary, be moving in approximately the same direction, and with comparable speed.
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: TESS light curves of TIC 114936199 for sector 14 (top panel), sector 40 (middle panel), and sector 53 (bottom panel), constructed using eleanor (Feinstein et al. 2019).
Paper: TIC 114936199: A Quadruple Star System with a 12 Day Outer-orbit Eclipse
Authors: Brian P. Powell, Saul A. Rappaport, Tamás Borkovits, Veselin B. Kostov, Guillermo Torres, Rahul Jayaraman, David W. Latham, Hana Kučáková, Zoltán Garai, Theodor Pribulla, Andrew Vanderburg, Ethan Kruse, Thomas Barclay, Greg Olmschenk, Martti H. K. Kristiansen, Robert Gagliano, Thomas L. Jacobs, Daryll M. LaCourse, Mark Omohundro, Hans M. Schwengeler, Ivan A. Terentev, Allan R. Schmitt
Figure caption: TESS light curve of TIC 114936199 from BJD 2458698 to 2458707, with labeled eclipses.
Paper: Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution
Authors: Jin-Ping Zhu, Yuan-Pei Yang, Bing Zhang, He Gao, Yun-Wei Yu
Figure caption: Rest-frame light curves of X-ray (top left panel), optical (top right panel), and radio (bottom panel) afterglows. The gray points denote the afterglow data points of cosmological sGRB afterglows collected from Fong et al. (2015) and Rastinejad et al. (2021). The gray region corresponds to the 3σ simulated region fitting the gray data points. The orange, cyan, and magenta points and lines denote the observed afterglow data of GRB170817A and the corresponding light-curve fitting, respectively. The predicted on-axis X-ray, optical, and radio afterglow light curves for GRB170817A are marked as red, green, and purple lines, respectively. The blue points in the middle panel show the observed kilonova data of AT2017gfo (Villar et al. 2017). Afterglow data were obtained from Troja et al. (2017), Troja et al. (2018), Troja et al. (2020), Piro et al. (2019), Hallinan et al. (2017), Lamb et al. (2019a), Lyman et al. (2018), Resmi et al. (2018), Margutti et al. (2018), and Mooley et al. (2018).
Paper: Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution
Authors: Jin-Ping Zhu, Yuan-Pei Yang, Bing Zhang, He Gao, Yun-Wei Yu
Figure caption: Kilonova and afterglow light curves along the polar axis (i.e., ﹩\sin {\theta }_{{\rm{v}}}=0﹩). The shaded regions from light to dark represent 1σ, 2σ, and 3σ simulated regions for cosmological afterglow. The solid and dashed colored lines show the light curves of GW170817-like kilonova and afterglow, respectively. Different panels correspond to different bands, including the griJ bands. The bottom subpanels of each panel show the brightness ratio of afterglow and kilonova emissions. The dashed colored lines are the brightness ratio of the GW170817-like afterglow and kilonova along the line of sight. The dashed gray lines show where the brightness of afterglow emission is equal to that of the kilonova emission.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Edge-on projection images, effective optical depth, and surface brightness profiles of the CCC, X99, and T04 model galaxies. Top three image panels: edge-on projection images of the CCC, X99, and T04 models. Middle plot panel: effective optical depth profiles along the galactic plane of the three models. Bottom panel: surface brightness profiles along the galactic plane of the three models.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Extinction and attenuation curves of the CCC model and the Calzetti law represented by ﹩\tfrac{A(\lambda )}{{A}_{V}}﹩. Top panel: extinction curve (Equation (9)) used in the CCC model (red curve) and the Calzetti attenuation curve (blue curve). Bottom panel: attenuation curves derived from the CCC model for the edge-on case (dashed, θ = 90°, R  V  = 7.0), face-on case (dotted, θ = 0°, R  V  = 3.7), and median case (solid, θ = 60°, R  V  = 4.1); the blue curve shows the Calzetti attenuation curve for comparison.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Consistence of the model-predicted optical depth of clumpy regions between the Gaussian approximation and numerical calculation of binomial distributions for different parameter sets, which are color coded by ﹩1-{\hat{\tau }}_{\mathrm{cl}}/{\hat{\tau }}_{\mathrm{Bio}}﹩ in each panel. Panel (a): ﹩{\bar{\tau }}_{\mathrm{cl}}=0.67﹩, p ranges from 0 to 0.01 and n ranges from 100 to 100,000; panel (b): p = 10−4, n ranges from 10 to 100,000 and ﹩{\bar{\tau }}_{\mathrm{cl}}﹩ ranges from 0 to 1; panel (c): n = 10,000, p ranges from 0 to 0.01 and ﹩{\bar{\tau }}_{\mathrm{cl}}﹩ ranges from 0 to 1.
Paper: Kilonova and Optical Afterglow from Binary Neutron Star Mergers. I. Luminosity Function and Color Evolution
Authors: Jin-Ping Zhu, Yuan-Pei Yang, Bing Zhang, He Gao, Yun-Wei Yu
Figure caption: Multiwavelength observed kilonova data (colored points) of AT2017gfo and our fitting model (colored lines). Kilonova data were collected from Andreoni et al. (2017), Arcavi et al. (2017), Coulter et al. (2017), Cowperthwaite et al. (2017), Díaz et al. (2017), Drout et al. (2017), Evans et al. (2017), Hu et al. (2017), Valenti et al. (2017), Pozanenko et al. (2018), Shappee et al. (2017), Smartt et al. (2017), Tanvir et al. (2017), Troja et al. (2017), Utsumi et al. (2017), and Villar et al. (2017).
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Cartoon of clumpy dust distribution(left) and continuous dust distribution(right) for the same amount of dust in the same volume V = S ∗ l.
Paper: The Chocolate Chip Cookie Model: Dust Geometry of Milky Way–like Disk Galaxies
Authors: Jiafeng Lu, 家风 卢, Shiyin Shen, 世银 沈, Fang-Ting Yuan, 方婷 袁, Zhengyi Shao, 正义 邵, Jinliang Hou, 金良 侯, Xianzhong Zheng, 宪忠 郑
Figure caption: Inclination dependence of the average metallicity (left panel) and stellar age (right panel) obtained from SPS fitting of our MW-like galaxy sample.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Optical spectra of SN 1991T obtained at −8 days, −3 days, and +14 days with respect to the time of maximum light in the B-band. Spectra of SN 1999aa, SN 1999ee, and SN 2011fe at similar phases are plotted for comparison. The spectra for SN 1991T are taken from Phillips et al. (1992), those of SN 1999aa from Blondin et al. (2012), those of SN 1999ee from Hamuy et al. (2002), and those of SN 2011fe from Pereira et al. (2013). Each spectrum was corrected for Galactic reddening using the the Schlafly & Finkbeiner (2011) recalibration of the Schlegel et al. (1998) infrared dust maps. In addition, based on SNooPy (Burns et al. 2011) fits to the photometry using the color vs. decline rate calibration of Burns et al. (2014), corrections for host galaxy reddenings of E(B − V)host = 0.15 and 0.31 mag were applied to the spectra of SN 1991T and SN 1999ee, respectively, while E(B − V)host was assumed to be zero for both SN 1999aa and SN 2011fe.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: (E1) Two columns shows the Hα ribbon images taken from SOT/BFI and the bottom QSL evolution during E1, respectively. (E2) The same as E1 but during the second eruption. The green and yellow region of QSL are the open field of the negative and positive fields, respectively. The red and blue region denotes the closed field of the positive and negative fields, respectively. The upper limit of the Q factor in red and blue region is log10 Q                    ﹩{}_{\max }=5﹩. The QSL evolution in the second column of E1 and E2 are shown at the top panel in the animation of Figure 5
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Evolution of pEW(Si II λ6355) for 91T-like SNe identified in the CSP-II sample. The trajectories of SN 1991T and SN 1999aa in this diagram are plotted for reference.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Velocity field at bottom boundary in our simulation.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Same as Figure A2, except for the 91T-like SNe 2013bz, 2014dl, OGLE-2014-SN-107, and ASASSN-14kd.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption:  SNooPy fits to the 91T-like SNe LSQ12gdj, SN2013U, CSS130303:105206-133424, and SN 2014eg derived using the intrinsic color analysis described by Burns et al. (2018). Magnitudes plotted on the y-axis for each filter are as observed. The x-axis gives the time in days in the observer frame after the epoch of B maximum.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Time series of X-ray images of two X-class flares taken from Hinode/XRT.
Paper: MHD Simulation of Homologous Eruptions from Solar Active Region 10930 Caused by Sunspot Rotation
Authors: Xinyi Wang, Chaowei Jiang, Xueshang Feng, Aiying Duan, Xinkai Bian
Figure caption: Time series of Stokes V images of Hinode/SOT from December 10 to December 15. Black and white represent the negative and positive polarities, respectively.
Paper: The Absolute Magnitudes of 1991T-like Supernovae 
Authors: M. M. Phillips, C. Ashall, Christopher R. Burns, Carlos Contreras, L. Galbany, P. Hoeflich, E. Y. Hsiao, Nidia Morrell, Peter Nugent, Syed A. Uddin, E. Baron, Wendy L. Freedman, Chelsea E. Harris, Kevin Krisciunas, S. Kumar, J. Lu, S. E. Persson, Anthony L. Piro, Abigail Polin, Shahbandeh M., Maximilian Stritzinger, Nicholas B. Suntzeff
Figure caption: Same as Figure A2, except for the 91T-like SNe OGLE-2014-SN-141 and SN 2014eg.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: Left: annotated, mosaic, background-subtracted, and exposure-corrected Suzaku image of the A98 system in the 0.5–7.0 keV band. The image is binned to emphasize the diffuse features in the system, and smoothed with a 20.″8 Gaussian. The sectors are the regions used for the temperature and entropy profiles for A98N. The yellow circle denotes r 200 for A98N derived from the T 500–r 500 relation found by Vikhlinin et al. (2009), assuming r 200 ∼ 1.7 r 500 (e.g., AMI Consortium et al. 2012). The dashed green circles are regions used to constrain the sky background. The excluded regions are point sources, and are excluded from further analysis. The potential background cluster is denoted by the white circular region (see Section 4.2). The cyan dashed circle regions mark the point sources that are modeled simultaneously with the outermost sector to the west of A98N. The box region to the north is used to estimate the large-scale properties described in Section 4.2. Right: the Suzaku image is smoothed with a 10.″4 circular Gaussian. The box regions are used for the intercluster filament thermodynamic profiles presented in Section 4.2.2. The dashed cyan boxes are used to derive the temperatures, electron densities, and entropy profiles for A98N and A98S presented in Figure 11. The dashed yellow circle denotes the XMM-Newton field of view. The cyan dashed regions and exclusion regions are the same as in the left panel.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: Left: XMM-Newton MOS2 total counts image of A98N and A98S smoothed with a 15″ Gaussian kernel. The point sources modeled with the XMM-Newton data in this work are highlighted with dashed cyan regions. The local background region used for the point-source fits is represented by the green circle. Right: 0.3–7.0 keV blank-sky, background-subtracted, exposure-corrected, mosaic image of the Chandra observations (see Table 2). The image is smoothed with a 10″ Gaussian.
Paper: Suzaku Observations of the Cluster Outskirts and Intercluster Filament in the Triple Merger Cluster A98
Authors: Gabriella E. Alvarez, Scott W. Randall, Yuanyuan Su, Arnab Sarkar, Stephen Walker, Nicholas P. Lee, Craig L. Sarazin, Elizabeth Blanton
Figure caption: The deprojected temperature profile of A98N for the sectors to the north and west shown in Figure 1. The pink points are for the sectors to the west of A98N and the green points are for the sectors to the north of A98N. The blue line is the “universal” temperature profile presented by Ghirardini et al. (2019).
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Completeness results based on an analysis of synthetic clusters. The top panels present results as a function of F475W magnitude, the bottom panels as a function of mass. The leftmost panels present results for individual synthetic clusters: detections in black, non-detections in red. The left-middle panels show a binned version of the same results, where the shading denotes the fraction of clusters detected in each bin. The middle-right panels show the completeness model fit, and the rightmost panels showing the data–model residuals. The vertical gray dashed lines in each panel highlight the age bins whose data are presented in Figure 11. The blue dotted–dashed line in each panel represents the fitted exponential 50% completeness model fit to the full synthetic data.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: A comparison of LGCS classifications for objects in the San Roman et al. (2010) and Sarajedini & Mancone (2007) catalogs that fall within the PHATTER footprint. Top: left and center panels show f cluster,W distributions for the San Roman et al. (2010) catalog, where object classes include “confirmed star cluster” (class 3), “highly probable star cluster” (class 2), “candidate star cluster” (class 1), “unknown” (class 0), and “background galaxy” (class −1). The dashed line represents the f cluster,W threshold we use for cluster catalog inclusion. The right panel shows the San Roman et al. (2010) classes for objects located in the PHATTER footprint that did not match to a LGCS identification. Bottom: same as top, but for matched (left and center) and unmatched (right) objects from the Sarajedini & Mancone (2007) catalog and its different sets of object classes.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: An example cluster: PHATTER 22. Top: two 12″ × 12″ F475W+F814W color images, where the pink circles represent user cluster identifications, and the green circle represents the final cluster aperture (R ap of 2.″04) derived from the median radius of the individual user apertures. Middle: the PHATTER 22 SED (blue) created from six-band integrated photometry. The results of SLUG SED fitting for PHATTER 22 are printed in the lower right (50th percentile value with the 16th–84th percentile confidence interval), and gray lines show the 100 best-fit SLUG models. Bottom: the PHATTER 22 cluster CMD, where stellar photometry for sources within the cluster aperture (blue) are accompanied by surrounding photometry of field stars (red). CMD fitting results from Wainer et al. (2022) are listed in the lower right, and a stellar isochrone (black) depicting the cluster’s best-fit properties is overplotted.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Spatially matched Spitzer 24 μm (top) and HST F475W−F814W (bottom) color cutouts for three Corbelli et al. (2017) and Sharma et al. (2011) objects that represent three scenarios for the objects: an object which shows evidence of being a young embedded star-forming region (left; Corbelli YSCC 225), an object where there is sufficient background visible to rule out an embedded cluster (middle; Corbelli YSCC 215), and a rare object which we classify as a star cluster in the PHATTER catalog (right; Corbelli YSCC 297, PHATTER 529).
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Shown here are the F475W magnitude distributions of PHATTER clusters (black) and previously identified literature objects (blue). Shown in black are 1166 PHATTER clusters with F475W detections. In blue are 391 literature objects included in the PHATTER cluster catalog with F475W detections. Literature objects not represented above: 13 objects lacking F475W detections and 178 objects with low f cluster,W  omitted from the PHATTER cluster catalog.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Logistic function fits to catalog completeness as a function of F475W magnitude (top) and mass (bottom) for synthetic clusters with ages ﹩7.3\lt \mathrm{log}(\mathrm{Age}/\mathrm{yr})\lt 7.77﹩. Dashed lines represent the Agresti–Coull binomial proportion confidence interval for each bin.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: Top: color–color diagram of 729 PHATTER clusters with three-band photometric detections. Bottom: comparison of the color–color distributions for PHATTER clusters in M33 and PHAT clusters in M31 (J15), which shows that the PHATTER clusters are significantly bluer, denoting younger cluster age.
Paper: The Panchromatic Hubble Andromeda Treasury: Triangulum Extended Region (PHATTER). IV. Star Cluster Catalog
Authors: L. Clifton Johnson, Tobin M. Wainer, Estephani E. TorresVillanueva, Anil C. Seth, Benjamin F. Williams, Meredith J. Durbin, Julianne J. Dalcanton, Daniel R. Weisz, Eric F. Bell, Puragra Guhathakurta, Evan Skillman, Adam Smercina
Figure caption: A comparison between the SLUG integrated light fits and CMD-based fits for 763 clusters in M31. The panels show the distribution of results relative to the one-to-one relation (dashed red line) for cluster mass (left), age (middle), and A  V  (right).