adsabs/AstroCLIMB huggingface dataset:
Paper: Around the Spindle Galaxy: The Dark Halo Mass of NGC 3115
Authors: I. D. Karachentsev, L. N. Makarova, G. S. Anand, R. B. Tully
Figure caption: Color-composed images of four new probable companions of NGC 3521 taken from DECaLS survey. The size of the images is 2′. North is up and east is left.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Histograms of the number of ZTF observations for our sample of RR Lyrae in the globular clusters. The mean and median numbers of observations are also given in the upper right corner of each panel.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the PL relations from Bhardwaj et al. (2021; black dashed lines) and this work (i.e., Table 4; red solid lines), evaluated at [Fe/H] = −2.27 dex for M15 (see Table 2). The orange open circles and magenta open triangles are for RR0 and RR1 in our sample, respectively, with mean magnitudes transformed to the SDSS system. Filled light green circles and triangles represent the RR Lyrae taken from Bhardwaj et al. (2021). Consistent extinction of A  g  = 0.379 and A  i  = 0.209 (Bhardwaj et al. 2021) in the SDSS system was applied to all data points. Our PL relations were shifted vertically using the distance of M15 as listed in Table 2. The bottom two panels are for the combined sample of RR0 and RR1 after fundamentalizing the pulsation periods of RR1.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the i-band PLZ relations given in Cáceres & Catelan (2008; dashed lines) and our derived relations presented in Table 4 (red solid lines), evaluated at [Fe/H] = −2.4 (left panel) and −0.4 (right panel) dex. For the theoretical PLZ relations, we also included the corresponding PLZ relations at three different adopted values of [α/Fe] (see text for details). Note that the data points and our i-band PLZ relations have been transformed to the SDSS photometric system following the procedures described in Section 4.1. The top and bottom panels are for the RR0 only and RR0 and RR1 (after fundamentalizing the pulsation periods) combined samples, respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: The PL relations (left panels, after correction for extinction) and PW relations for all of the RR Lyrae listed in Table 3 by adopting the distance of the globular clusters as listed in Table 2. The color bar represents the metallicity of the host globular clusters. Circles and triangles are for the RR Lyrae with pulsation types of RR0 and RR1, respectively. Error bars are omitted for clarity.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the PL relations from Vivas et al. (2017; black dashed lines) and this work (i.e., Table 4; red solid lines) evaluated at [Fe/H] = −1.12 dex for M5 (see Table 2). The orange circles and cyan triangles are for RR0 and RR1 in our sample, respectively. Data points with black circles or triangles represent the RR Lyrae in M5.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Metallicity-dependent PWZ relations for our sample of RR Lyrae. The solid and dashed lines (both red and black) represent the PWZ relations evaluated at [Fe/H] = −2.4 and −0.4 dex, respectively. The orange circles and cyan triangles are for RR0 and RR1, respectively. The PWZ relations for the combined sample of RR0 and RR1 (after fundamentalizing the periods) are similar; hence, they are not included in this figure.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Examples of the light curves for RR Lyrae with three (top panels), two (middle panels), and one (bottom panels) ACR flag. The black crosses are rejected data points during the first pass of the two-iteration template light-curve fitting procedure, and the black curves are the best-fit template light curves after the second pass of the procedure (see Section 2.4 for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Examples of the randomly selected light curves for RR Lyrae without any flags. The black crosses are rejected data points during the first pass of the two-iteration template light-curve fitting procedure, and the black curves are the best-fit template light curves after the second pass of the procedure (see Section 2.4 for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the PLZ relations for RR0 from Sesar et al. (2017; black) and this work (i.e., Table 4; red) evaluated at two metallicities, [Fe/H] = −2.4 and −0.4 dex, as solid and dashed lines, respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Histograms of [Fe/H] distribution for the full sample of 1209 RR Lyrae and the remaining sample of 755 RR Lyrae. The [Fe/H] values for the RR Lyrae are based on their host globular clusters (see Table 2).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the g-band PLZ relations given in Marconi et al. (2006; dashed lines) and our derived relations presented in Table 4 (red solid lines), evaluated at [Fe/H] = −2.4 (top panel) and −0.4 (bottom panel) dex, with a fixed [α/Fe]= +0.2 dex. For the semitheoretical PLZ relations (see text for details), we also included the corresponding PLZ relations at three different adopted values of the mass M, covering the expected mass range for RR Lyrae. Note that the data points and our g-band PLZ relations have been transformed to the SDSS photometric system following the procedures described in Section 4.1. Circles and triangles represent RR0 and RR1, respectively.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Comparison of the PCZ relations given in Cáceres & Catelan (2008; dashed lines) and our derived relations presented in Table 4 (red solid lines), evaluated at [Fe/H] = −2.4 (left panels) and −0.4 (right panels) dex, for the (g − r) and (r − i) colors in the top and bottom panels, respectively. For the theoretical PLZ relations, we adopted a value of [α/Fe] = +0.2 dex (see text for details). Note that the data points and our PCZ relations have been transformed to the SDSS photometric system following the procedures described in Section 4.1. In each panel, the top and bottom subpanels are for RR0 only and the RR0 and RR1 (after fundamentalizing the pulsation periods) combined samples, respectively.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Combined residuals for Nereid from various data sources in Table 6. The top panel shows 61 ﹩{\rm{\Delta }}\alpha \cos \delta ﹩ residuals in red (Nereid relative to Neptune), 1941 α residuals in blue, and 171 ﹩{\rm{\Delta }}\alpha \cos \delta ﹩ residuals in gray (Nereid relative to Triton). The bottom panel shows 62 Δδ residuals in red (Nereid relative to Neptune), 1941 δ residuals in blue, and 1941 Δδ residuals in gray (Nereid relative to Triton).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Extinction-corrected color–color relations for RR0 (left panel) and RR1 (right panel) in our sample, where the mean magnitudes have been transformed to the SDSS system using the transformations provided in Tonry et al. (2012). The typical error bars of the colors are shown in the lower left corners. Both the solid and dashed lines represent the theoretical color–color relations taken from Marconi et al. (2006) at a given metallicity (see text for more details).
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Corner plot based on the emcee sampling on the posterior distributions for μ 0 and [Fe/H]. The sampling was run with 128 walkers for 10,000 steps. The vertical dashed lines represent the 16th, 50th, and 84th percentiles of the distributions. The blue lines mark the results obtained from the OLS regression.
Paper: Zwicky Transient Facility and Globular Clusters: The RR Lyrae gri-band Period–Luminosity–Metallicity and Period–Wesenheit–Metallicity Relations
Authors: Chow-Choong Ngeow, Anupam Bhardwaj, Richard Dekany, Dmitry A. Duev, Matthew J. Graham, Steven L. Groom, Ashish A. Mahabal, Frank J. Masci, Michael S. Medford, Reed Riddle
Figure caption: Extinction-corrected PC relations (top three panels) and extinction-free PQ relation (bottom panel) for our sample of RR Lyrae. The solid and dashed lines (in both red and black) represent the PCZ and PQZ relations evaluated at [Fe/H] = −2.4 and −0.4 dex, respectively. The relations for the combined sample of RR0 and RR1 (after fundamentalizing the periods) are similar; hence, they are not included in this figure.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Osculating eccentricities for the satellites of Neptune for 30,000 yr.
Paper: Orbits of the Irregular Satellites of Uranus and Neptune
Authors: Marina Brozović, Robert A. Jacobson
Figure caption: Osculating eccentricities for the satellites of Uranus for 30,000 yr.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Examples of light curves for regular Miras in the LMC (subfigures on the left) and SMC (subfigures on the right). The middle panel presents the I-band light curve taken from the OGLE-III in each subfigure. The top and bottom panels show the determined magnitudes at maximum and minimum light, respectively, for each pulsation cycle (whenever available). The top two subfigures are examples of light curves with minimal light magnitudes that do not exhibit any periodicity. The middle two subfigures are the light curves in which the magnitude at minimum light can be fitted with a periodic sinusoidal function (shown as dashed curves) with periods P min of around 1000 days. The bottom two subfigures are similar to the subfigures in the middle, except P min was found to be much longer than 3000 days.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Example of the decision trees for one randomly selected Mira in our sample. An example of the leaves in the decision trees is enlarged and shown on the bottom left based on the output from the Scikit-learn package. Regular and nonregular Miras are indicated by the orange and blue boxes, respectively. The decision tree works as follows. First, the algorithm collects the features in an initial root node (the top cyan box) from all training data set. Then, the RF algorithm divides the decision tree into two leaves based on the features of the input training data, and each leaf is further divided into two leaves until the groups in the leaves are all identical. An example is illustrated in the bottom left with enlarged boxes (or leaves). The white box represents a leaf with two samples. If one of them has Q31 smaller than 0.65 (based on the training set), then it is classified as a regular Mira in the orange box, else it is classified as a nonregular Mira in the blue box.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: The ROC curve applied the RF algorithm to our training set. The area under the ROC curve (AUC) represents the performance of the RF algorithm; a value of 1 means perfect performance. The dashed line indicates AUC=0.5, implying random guessing. In our case, we achieved an AUC of 0.94.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Correlations of the standard deviations σ for the maximum, mean, and minimum magnitudes. The left panels are for σ mean vs. ﹩{\sigma }_{\max }﹩, and the right panels show σ mean vs. ﹩{\sigma }_{\min }﹩, separated for the C-rich (top panels) and O-rich (bottom panels) regular Miras. The dashed lines indicate a 1:1 correlation.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: The confusion matrix for the RF classification is based on the test data selected as part of the training data.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Rank of the importance of the light-curve features.
Paper: Difference of Photometric Properties between Regular and Nonregular Miras in the Magellanic Clouds
Authors: Jia-Yu Ou, Chow-Choong Ngeow
Figure caption: Examples of a regular and a nonregular Miras light curve are shown in the left and right panels, respectively.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. V. Chemical Abundances of CTIO/Hydra Clusters Using The Cannon
Authors: Amy E. Ray, Peter M. Frinchaboy, John Donor, S. D. Chojnowski, Matthew Melendez
Figure caption: A comparison of the average [Fe/H] values in common open clusters from this survey and from the literature compilation in Table 6. Magenta clusters are from Santos et al. (2009), blue clusters are from Netopil et al. (2016), and orange clusters are from Reddy et al. (2013, 2015).
Paper: The Open Cluster Chemical Abundances and Mapping Survey. V. Chemical Abundances of CTIO/Hydra Clusters Using The Cannon
Authors: Amy E. Ray, Peter M. Frinchaboy, John Donor, S. D. Chojnowski, Matthew Melendez
Figure caption: Spatial Galactic distribution of open clusters in this survey color coded with ages and R GC distance from Cantat-Gaudin et al. (2020). Also shown are the locations of the OCCAM-IV DR16-based cluster from Donor et al. (2020) also updated with ages and R GC distance from Cantat-Gaudin et al. (2020; red crosses).
Paper: The Open Cluster Chemical Abundances and Mapping Survey. V. Chemical Abundances of CTIO/Hydra Clusters Using The Cannon
Authors: Amy E. Ray, Peter M. Frinchaboy, John Donor, S. D. Chojnowski, Matthew Melendez
Figure caption: A comparison of effective temperature (Teff) and surface gravity (log g) values obtained by The Cannon and values obtained using APOGEE DR16 data. Most of the values fall within the scatter, which is illustrated by the gray shaded areas.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. V. Chemical Abundances of CTIO/Hydra Clusters Using The Cannon
Authors: Amy E. Ray, Peter M. Frinchaboy, John Donor, S. D. Chojnowski, Matthew Melendez
Figure caption: A comparison of [Fe/H], [Mg/Fe], [Si/Fe], [Al/Fe], and [O/Fe] values obtained by The Cannon and values obtained using APOGEE DR16 data. The shaded areas represent the acceptable scatter as in Figure 2.
Paper: Revisiting WASP-47 with ESPRESSO and TESS
Authors: Edward M. Bryant, Daniel Bayliss
Figure caption: Orbital configuration of the inner three planets in the WASP-47 system. The three lines show the orbits of the planets: WASP-47 b (green), WASP-47 d (blue), and WASP-47 e (orange). The position of the WASP-47 star is depicted by the black cross. The filled circles give the positions of the planets at T = 2549449.35 BJD, which is the time of the first transit of WASP-47 b observed by the Transiting Exoplanet Survey Satellite, assuming observer viewing from the bottom of the plot and orbits in the anticlockwise direction. The relative sizes of the filled circles are proportional to the the relative radii of the planets.
Paper: Plaskett 1.8 m Observations of Starlink Satellites
Authors: Aaron C. Boley, Ewan Wright, Samantha Lawler, Paul Hickson, Dave Balam
Figure caption: Similar to Figure 2, but including a diffuse sphere model for the apparent magnitude (red, downward pointing triangle) and a heuristic power-law STO (phase) model (blue, upward pointing triangle). The right panel shows the difference between the observed magnitudes and the predictions from the heuristic phase model.
Paper: Plaskett 1.8 m Observations of Starlink Satellites
Authors: Aaron C. Boley, Ewan Wright, Samantha Lawler, Paul Hickson, Dave Balam
Figure caption: Select observational properties for the observed satellites, emphasizing Starlinks (square) Starlink-Vs (circle). A slight dimming of the satellites is seen with increasing STO. A sudden change in brightness occurs around 43° for both Starlink and Starlink-V. This feature is not understood. The brightest satellites are seen at a range near 650 km due to the combination of distance and favorable STO. The satellites with the smallest possible range (550 km), due to the orbital altitude, occur near an STO of about 70°. Higher STOs were not observed due to restrictions on telescope azimuth for slew considerations.
Paper: A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
Authors: Sam Christian, Andrew Vanderburg, Juliette Becker, Daniel A. Yahalomi, Logan Pearce, George Zhou, Karen A. Collins, Adam L. Kraus, Keivan G. Stassun, Zoe de Beurs, George R. Ricker, Roland K. Vanderspek, David W. Latham, Joshua N. Winn, S. Seager, Jon M. Jenkins, Lyu Abe, Karim Agabi, Pedro J. Amado, David Baker, Khalid Barkaoui, Zouhair Benkhaldoun, Paul Benni, John Berberian, Perry Berlind, Allyson Bieryla, Emma Esparza-Borges, Michael Bowen, Peyton Brown, Lars A. Buchhave, Christopher J. Burke, Marco Buttu, Charles Cadieux, Douglas A. Caldwell, David Charbonneau, Nikita Chazov, Sudhish Chimaladinne, Kevin I. Collins, Deven Combs, Dennis M. Conti, Nicolas Crouzet, Jerome P. de Leon, Shila Deljookorani, Brendan Diamond, René Doyon, Diana Dragomir, Georgina Dransfield, Zahra Essack, Phil Evans, Akihiko Fukui, Tianjun Gan, Gilbert A. Esquerdo, Michaël Gillon, Eric Girardin, Pere Guerra, Tristan Guillot, Eleanor Kate K. Habich, Andreea Henriksen, Nora Hoch, Keisuke I Isogai, Emmanuël Jehin, Eric L. N. Jensen, Marshall C. Johnson, John H. Livingston, John F. Kielkopf, Kingsley Kim, Kiyoe Kawauchi, Vadim Krushinsky, Veronica Kunzle, Didier Laloum, Dominic Leger, Pablo Lewin, Franco Mallia, Bob Massey, Mayuko Mori, Kim K. McLeod, Djamel Mékarnia, Ismael Mireles, Nikolay Mishevskiy, Motohide Tamura, Felipe Murgas, Norio Narita, Ramon Naves, Peter Nelson, Hugh P. Osborn, Enric Palle, Hannu Parviainen, Peter Plavchan, Francisco J. Pozuelos, Markus Rabus, Howard M. Relles, Cristina Rodríguez López, Samuel N. Quinn, Francois-Xavier Schmider, Joshua E. Schlieder, Richard P. Schwarz, Avi Shporer, Laurie Sibbald, Gregor Srdoc, Caitlin Stibbards, Hannah Stickler, Olga Suarez, Chris Stockdale, Thiam-Guan Tan, Yuka Terada, Amaury Triaud, Rene Tronsgaard, William C. Waalkes, Gavin Wang, Noriharu Watanabe, Marie-Sainte Wenceslas, Geof Wingham, Justin Wittrock, Carl Ziegler
Figure caption: The disk precession timescale as simulated for the sample of binary-star systems with exoplanets. The horizontal dashed line indicates the typical 2.5 Myr half-lifetime of protoplanetary disks (Mamajek 2009). The well-aligned sample of binaries with semimajor axes shorter than about 700 au typically have disk precession timescales short enough that this mechanism could explain the alignment.