adsabs/AstroCLIMB huggingface dataset:
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Sky map of the number of visits across all filters of the 10 yr LSST survey cadence based on the one snap v4.0 simulation (SCOC 2024). The main WFD survey making up ∼80% of the total survey time will receive ∼800 visits per pointing. There are additional “Mini” surveys highlighted that make up ∼3%–10% of the survey time. These cover differing areas of the sky, including the NES, the South Celestial Pole (SCP), and the Dusty Plane. Additionally highlighted are DDFs, regions within the WFD that will receive deeper coverage and more frequent temporal sampling and use a total of ∼6.5% of the survey time. For complete details of the survey strategy, see SCOC (2024).
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Orbital space 2D histograms for the three dynamical classifications of the input Centaur models used in this work, namely the G08 sample in the left column, the S19 sample in the middle column, and the Hybrid sample in the right column. The top row shows histograms of Centaur eccentricity as a function of semimajor axis, whereas the bottom row shows histograms of Centaur inclination as a function of perihelion distance.
Paper: Predictions of the LSST Solar System Yield: Discovery Rates and Characterizations of Centaurs
Authors: Joseph Murtagh, Megan E. Schwamb, Stephanie R. Merritt, Pedro H. Bernardinelli, Jacob A. Kurlander, Samuel Cornwall, Mario Jurić, Grigori Fedorets, Matthew J. Holman, Siegfried Eggl, David Nesvorný, Kathryn Volk, R. Lynne Jones, Peter Yoachim, Joachim Moeyens, Jeremy Kubica, Drew Oldag, Maxine West, Colin Orion Chandler
Figure caption: Cumulative histogram of the model absolute magnitude H distribution of objects with H less than a given absolute magnitude Hr for the G08 sample. The inset represents a zoom-in of the bright end of the same distribution where H <  11.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Examples of injected partial transits that pass our S/N = 7 detection threshold, spanning the range of Rp and r that we explore. Each plot falls within one of our r and Rp bins, with binned r increasing from left to right and binned Rp increasing from bottom to top. The bin edges are denoted in bold along the top and right. r-band data are shown in blue, while z-band data are shown in red.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Examples of injected transits that pass our S/N = 7 detection threshold, spanning the range of Rp and P that we explore. Each plot falls within one of our P and Rp bins, with binned P increasing from left to right and binned Rp increasing from bottom to top. The bin edges are denoted in bold along the top and right. r-band data are shown in blue, while z-band data are shown in red.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Examples of injected full transits that pass our S/N = 7 detection threshold, spanning the range of Rp and r that we explore. Each plot falls within one of our r and Rp bins, with binned r increasing from left to right and binned Rp increasing from bottom to top. The bin edges are denoted in bold along the top and right. r-band data are shown in blue, while z-band data are shown in red.
Paper: The Multiband Imaging Survey for High-alpha PlanetS (MISHAPS). I. Preliminary Constraints on the Occurrence Rate of Hot Jupiters in 47 Tucanae
Authors: Alison L. Crisp, Jonas Klüter, Marz L. Newman, Matthew T. Penny, Thomas G. Beatty, L. Ilsedore Cleeves, Karen A. Collins, Jennifer A. Johnson, Marshall C. Johnson, Michael B. Lund, Clara E. Martínez-Vázquez, Melissa K. Ness, Joseph E. Rodriguez, Robert Siverd, Daniel J. Stevens, Steven Villanueva, Carl Ziegler
Figure caption: Two-dimensional occurrence rate upper limits, estimated in bins of Rp and P. The labels on each bin give the occurrence rate in percent.
Paper: Sorcha: Optimized Solar System Ephemeris Generation
Authors: Matthew J. Holman, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Drew Oldag, Maxine West, Kevin J. Napier, Stephanie R. Merritt, Grigori Fedorets, Samuel Cornwall, Jacob A. Kurlander, Siegfried Eggl, Jeremy Kubica, Kathleen Kiker, Joseph Murtagh, Shantanu P. Naidu, Colin Orion Chandler
Figure caption: Cartoon schematic of ephemeris generation within Sorcha. Each color represents a different moving object on a different orbit. Slower moving objects will cover fewer Hierarchical Equal Area Iso Latitude pixelation (HEALPix) tiles. The green circle represents an area slightly bigger than LSSTCam’s footprint. For the given observation time, any orbits with a HEALPix tile within the circle are integrated to calculate their exact positions at the time of the observation. Those orbits that land within the circle are then identified, and the resulting ephemerides associated with those objects and the observation are saved and passed on to later stages of the simulator that calculate the apparent magnitude and estimate the likelihood of discovery.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Mass–radius diagram made using mr-plotter (A. Castro-González et al. 2023) of sub-Neptunes with measured masses as well as theoretical models from L. Zeng et al. (2019). Only planets with 5σ mass and radius measurements are shown for clarity. HD 35843 c lies in the overlapping region between rocky planets with an H2 atmosphere and water worlds.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Left: eccentricity measurements of transiting sub-Neptune systems vs. orbital period. Empty markers denote upper limits on eccentricity. HD 35843 c has the highest eccentricity of the six sub-Neptunes. Right: HD 35843 and the five other sub-Neptune systems with a nontransiting inner planet. HD 35843 has the hottest host star and fewest number of planets of the six systems.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Left: mass fractions for the core, mantle, water, and gas layers calculated using ExoMDN. Right: radius fractions for the same layers.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: HD 35843 c TTVs for the TESS, LCOGT, and NGTS observations.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Corner plots of modeled parameters obtained from allesfitter.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Corner plots of derived parameters obtained from allesfitter.
Paper: HD 35843: A Sun-like Star Hosting a Long-period Sub-Neptune and Inner Super-Earth
Authors: Katharine Hesse, Ismael Mireles, François Bouchy, Diana Dragomir, Solène Ulmer-Moll, Nora L. Eisner, Keivan G. Stassun, Samuel N. Quinn, Hugh P. Osborn, Sergio G. Sousa, Cristilyn N. Watkins, Karen A. Collins, Edward M. Bryant, Jonathan M. Irwin, Coel Hellier, Marshall C. Johnson, Carl Ziegler, Steve B. Howell, David R. Anderson, Daniel Bayliss, Allyson Bieryla, César Briceño, R. Paul Butler, David Charbonneau, Ryan Cloutier, Jeffrey Crane, Jason Dittmann, Jason D. Eastman, Sebastián A. Freigeiro, Benjamin J. Fulton, Samuel Gill, Maximilian Günther, Haedam Im, Jon M. Jenkins, Michelle Kunimoto, Baptiste Lavie, Monika Lendl, Michael B. Lund, Andrew W. Mann, Belinda Nicholson, David Osip, Martin Paegert, Nuno C. Santos, Richard P. Schwarz, Sara Seager, Stephen Shectman, Johanna Teske, Joseph D. Twicken, Stéphane Udry, Vincent Van Eylen, José Vinés, Sharon X. Wang, Peter J. Wheatley, Joshua N. Winn, Edward E. Zuidema
Figure caption: Corner plot of the modeled parameters obtained from an allesfitter joint fit including the PFS RVs.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: Average power vs. pulse period for 140 million pulses detected by SETI@home at times the telescope beam was moving within 5% of the sidereal rate. The magenta points mark the 5th percentile, which provides an estimate of sensitivity to pulses of that period. The blue line is a fit to those points, as described in Section 5.3.4.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: Waterfall plots showing the SETI@home analysis of a GBT observation of Voyager 1. The upper panel shows the results with the default cutoff of 30 total detections. The lower panel shows detections when the analysis is allowed to run to completion.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: The upper panel shows the number of computers actively participating in SETI@home. The lower panel shows the rate of computing done by these machines in petaFPOP s–1 (1 petaFPOP = 1015 floating-point operations).
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: Comparison of the sensitivity of SETI@home (black) relative to ∼0.8 Hz resolution spectrometers using post-threshold Doppler correction (magenta), pre-threshold incoherent Doppler correction (blue) over the frequency drift range ±100 Hz s−1.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: Comparison of the sensitivity to signals of nonzero bandwidth of SETI@home (black) vs. the 0.8 Hz resolution spectrometer SERENDIP VI (red), which also used the ALFA receiver at Arecibo.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: Simplified pseudo code describing the client data analysis. Its input is 1 Mi samples of time-domain data.
Paper: SETI@home: Data Acquisition and Front-end Processing 
Authors: E. J. Korpela, D. P. Anderson, J. Cobb, M. Lebofsky, W. Liu, D. Werthimer
Figure caption: The SETI@home data acquisition and analysis pipeline.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Gaia-EDR3 CMDs for the NGC 1605a (left panel) and NGC 1605b member lists (right panel). The color bar denotes the binary probability for the cluster member candidates. The bulk of probable binary stars in both CMDs are located in the region corresponding to the NGC 1605a upper MS.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: In the top left panel is shown the result of applying the PCA elbow method, which found six clusters in the NGC 1605 area. The within-cluster sum-of-squares metric measures the sum of the squared distances between each star and its assigned cluster center as a function of the number of clusters. The other panels show the t-SNE 2D projection (perplexity = 50) of the stars in the NGC 1605b member list clustered using the k-means (top right), fuzzy (bottom left), and GMM (bottom right) methods.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Gaia-EDR3 PM distribution, for NGC 1605b, highlighted by the KNN smoothing algorithm for K = 12 (top panels) and K = 5 neighbors (bottom panels). The black circles are the stars in the cluster member list.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Top panel: MST for the NGC 1605b member list implemented by a combination of KNN and HDBSCAN. Bottom panel: a zoom-in of the PM diagram built by using the KNN smoothing algorithm.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Heat maps of the spatial distribution for stars in the NGC 1605b member list, built by using the KNN smoothing algorithm on K = 28 (top panels) and K = 5 (bottom panels) nearest neighbors. The right panels display the schematic distribution of the cluster probable member stars as black circles overlaid on the heat maps.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Parallax vs. G magnitude for the NGC 1605b member list. The heat maps are built by the KNN smoothing algorithm.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: RDP for NGC 1605b and NGC 1605a. Blue region: 1σ King fit uncertainty.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Parallax and PM errors vs. G magnitude for stars in the NGC 1605b member list.
Paper: Multiple Machine Learning as a Powerful Tool for Star Cluster Analysis
Authors: Denilso Camargo
Figure caption: Gaia CMDs for the NGC 1605b member list color coded by the HDBSCAN and GMM membership probabilities.
Paper: Exploring the Wolf Approach to Constraining NIR Extinction Laws in the Corona Australis Molecular Cloud
Authors: Botao Jiang, 博韬 江, Jun Li, 军 李, Xi Chen, 曦 陈
Figure caption: Density plots of photometric data of the CrA molecular cloud in the J, H, and KS bands from the VISIONS. The dashed lines in all the panels indicate the completeness limiting magnitudes of 20.3 mag, 19.8 mag, and 18.6 mag in the J, H, and KS bands, respectively.
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: Left: Distance vs. absolute Ks-band magnitude of the HARMONI IMBH (red; this work), MASSIVE (green; C.-P. Ma et al. 2014), ATLAS3D (blue; M. Cappellari et al. 2011), and MMBH (black; N23) surveys. There is an overlapping region between the HARMONI IMBH sample and the ATLAS3D survey (i.e., ≈1.8 MK mag or 1010 < M⋆ < 5 × 1010M⊙). The plotted distance is the angular size distance D = DA. Right: The mass–size diagram of the 2MRS sources (gray dots) shows a wide range of stellar mass: 107 < M⋆ < 6 × 1012M⊙. The inclined red-dashed lines indicate constant σ⋆ of 10, 20, 30, 40, 50, and 70 km s−1. The ATLAS3D, MASSIVE, MMBH, and HARMONI IMBH samples occupy different regions of the diagram. The thick-solid red curve defines the zone of exclusion described by Equation (4) of M. Cappellari et al. (2013a) in the previously explored stellar-mass range of 5 × 109 ≤ M⋆ ≲ 1012 M⊙. The thick dashed–dotted blue line shows the relation ﹩({R}_{e}/\mathrm{kpc})=8\times {[{M}_{\star }/(1{0}^{10}\ {M}_{\odot })]}^{0.24}﹩, which provides a convenient approximation for the lower 99% contour for the distribution of early-type galaxies (M. Cappellari et al. 2013a).
Paper: Simulating Intermediate Black Hole Mass Measurements for a Sample of Galaxies with Nuclear Star Clusters Using ELT/HARMONI High Spatial Resolution Integral-field Stellar Kinematics
Authors: Dieu D. Nguyen, Michele Cappellari, Hai N. Ngo, Tinh Q. T. Le, Tuan N. Le, Khue N. H. Ho, An K. Nguyen, Phong T. On, Huy G. Tong, Niranjan Thatte, Miguel Pereira-Santaella
Figure caption: The 40 available observations out of the total number of 44 dwarf galaxies from our HARMONI IMBH sample, as captured in HST, SDSS, DSS, and 2MASS images. To emphasize their NSCs at the core, the galaxy brightness has been adjusted. Each galaxy’s name and galaxy types are also shown. Two red circles define the region around the galaxy’s center, spanning from 12″ to 60″, where we search for a faint natural guide star (NGS) essential for laser tomography adaptive optics performance. The white crosses pinpoint the available NGS locations, specifying their apparent AB magnitudes measured in the H band. Here, dE = dwarf Elliptical, S0 = lenticular, S = Spiral, Irr = Irregular.