adsabs/AstroCLIMB huggingface dataset:
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Plot of the lowest S/N values at which a strong detection is achieved for notable H2O feature bandpasses, as a function of H2O abundance. The VMR values are on the x-axis, with S/N on the y-axis. The 0.9, 0.83, 0.85, and 0.74 μm bandpasses are shown in light pink stars, pink dots, dark pink diamonds, and purple dots, respectively. We also mark the rough H2O abundance ranges for several epochs through Earth’s history, including a Neoproterozoic slushball period (in dark pink), a mid-Cretaceous greenhouse warm period (pink), and the measured range for modern Earth values (light pink). We note that, for display purposes, we have left off the lowest abundance values for the Neoproterozoic slushball and modern epochs from the plot range.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Results of the analysis for the fiducial abundance for H2O, but for a narrower S/N range. All facets of the plot remain the same as in Figure 3. Detectability at wavelengths below 0.84 μm occurs for S/N> 11.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Summary of the bandpasses where H2O and O2 are detectable for our fiducial modern Earth scenario, based on results as shown in Figures 3 and 4. The shortest bandpass centers at which one can achieve a strong or weak detection for H2O, or a strong detection for O2, are shown in dark purple squares, pink dots, and light purple triangles, respectively. S/N is on the y-axis, and the bandpass centers are on the x-axis. We also show the ranges out to the longest wavelengths at which the same detections are achieved as shaded regions. We note that a strong detection of both H2O and O2 can be achieved with bandpasses at or below 0.83 μm and S/N≥ 10.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Default spectrum used for simulations, plotted with the high-probability values as drawn from the corner plots and posterior values of P 0 and H2O. The top panel shows a zoomed-in view of the longer wavelength ranges, and the bottom panel is identical but zooms in to the shorter wavelengths. Each portrays the three bandpasses that are most centered with the features of interest. The presence of O2 in the short-wavelength region helps to break the degeneracies between multiple parameters.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Heatmap plots illustrating detection strength as a function of S/N and varying H2O abundance. S/N is on the y-axis, H2O abundance is on the x-axis, and the colorbar shows the range of log-Bayes factor (lnB) from 0 to 5 to describe detection strength. ﹩\mathrm{ln}B\lt 2.5﹩ are unconstrained, ﹩2.5\leqslant \mathrm{ln}B\lt 5﹩ are weak, and ﹩\mathrm{ln}B\gt 5﹩ are strong, as in prior figures.
Paper: Bayesian Analysis for Remote Biosignature Identification on exoEarths (BARBIE). I. Using Grid-based Nested Sampling in Coronagraphy Observation Simulations for H2O
Authors: Natasha Latouf, Avi M. Mandell, Geronimo L. Villanueva, Michael Dane Moore, Nicholas Susemiehl, Vincent Kofman, Michael D. Himes
Figure caption: Comparison of spectra with varying H2O abundance. Shown are the lowest and highest abundance in our simulations (3 × 10−4 VMR and 3×10−2 VMR) as well as the modern Earth value (3 × 10−3 VMR). All spectra are binned at R = 140. At the highest abundances, H2O spectral features begin to overlap.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: SparsePak IFU (WIYN 3.5 m) map of UGC 4305, with Hα line measurements from PAN and FXCOR. Left: Hα flux on a logarithmic scale in units of 10−16 erg s−1 cm−1; center: Hα recessional velocities; right: map of Hα velocity dispersion (σ Hα ). Each filled circle corresponds to a fiber’s size and position on the sky. See Figure 4 for where the Sparsepak fibers fall compared to UGC 4305's H I and optical distributions.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: Top: TESS light curve of FU Tau A (Sectors 43 and 44), which has been presented in Bowler et al. (2023) and is reproduced here. Lower left: the two flares identified in the TESS data. Lower right: periodograms for the TESS and Lulin observations. When excluding the data on December 9, the Lulin curve peaks at 112.3 hr, much closer to the rotation period of 94.3 hr derived from the TESS data (see 164.4 hr in Figure 3), though also close to the duration of our monitoring.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: Relative photometry between FU Tau A and 2MASS J04241447+2506106 between UT 2021 December 4–9. Top: Hα light curve of FU Tau A and the corresponding Lomb–Scargle periodogram which peaks at 164.4 hr. Bottom: zoomed-in light curve of each night.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: Relative photometry between FU Tau B and 2MASS J04241447+2506106 between UT 2021 December 4–9. To increase the S/Ns, we merged the data into 30 minute bins except for the fourth night, in which we merged into 1 hr bins. For reference, the variability for the binned reference star is about 0.3%.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: UGC 4305. Left: two-color image from HST observations with ACS where the F814W image is mapped to red and the F555W image is mapped to blue. Center: the VLA H I dispersion map with isovelocity contours at a step size of 3 km s−1. Right: the WIYN 3.5 m SparsePak IFU σ Hα  map. In the right panel, each filled circle represents a fiber’s size and position on the sky. Overlaid in red are the outlines of regions used for the analysis.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: Example CMD and SFH for two 400 × 400 pc regions in UGC 4305 from ACS data. The main sequence (blue), blue helium-burning stars (HeB; green), and red HeB (red) sequences are traced. The SFHs have ≤15 Myr time resolution in the t < 70 Myr time bins with Δlog(t) = 0.15 time steps and cover the 560 Myr baseline necessary for our science goals. The green shading represents the random uncertainties. To determine the timescales of stellar feedback, each region’s CMD-derived SFH is compared with its H I and Hα turbulence measures.
Paper: Timescale of Stellar Feedback-driven Turbulence in the ISM: A Deep Dive into UGC 4305
Authors: Laura Congreve Hunter, Liese van Zee, Kristen B. W. McQuinn, Roger E. Cohen, Madison Markham, Andrew E. Dolphin
Figure caption: The VLA-derived H I moment maps of UGC 4305. Left: H I zeroth moment map (column density) in units of 1021 H atoms cm−2; center: H I first moment map (velocity field) with isovelocity contours spaced every 10 km s−1; right: H I second moment map (velocity dispersion) with isovelocity contours at 3 km s−1 spacing. In the bottom left of the first panel is the beam size (10.″73 × 10.″40) of the H I data cube used.
Paper: Monitoring Hα Emission from the Wide-orbit Brown-dwarf Companion FU Tau B
Authors: Ya-Lin Wu, Yu-Chi Cheng, Li-Ching Huang, Brendan P. Bowler, Laird M. Close, Wei-Ling Tseng, Ning Chen, Da-Wei Chen
Figure caption: Daily Hα variation of FU Tau B. The data points are listed in Table 4.
Paper: Imaging the Milky Way with Millihertz Gravitational Waves
Authors: Kaitlyn Szekerczes, Scott Noble, Cecilia Chirenti, James Ira Thorpe
Figure caption: Simulated LISA (left) and AMIGO (right) images for a 10° × 10° region around the Galactic center. The size of the median CDL, ﹩\bar{\mathrm{CDL}}﹩, over all sources is represented by a red circle in each image.
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Top: the HIRES RV measurement of TOI-2018 (black symbols) and the best-fit RV model (red). The best-fit model only includes the contribution from TOI-2018 b (cyan), a RV drift (orange), and a GP model for stellar activity (blue). TOI-2018.02 (green dotted line) was not detected. Bottom: the RV measurements phase-folded at the orbital period of TOI-2018 b after removing the contribution from the other effects in the top panel.
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The chromospheric activity of TOI-2018 (orange star) in comparison with other stars in the California Planet Search sample (Isaacson & Fischer 2010). Both S  HK  and log﹩{R}_{\mathrm{HK}}^{{\prime} }﹩ are close to the fiftieth percentile of stars with similar B–V color. Unfortunately, the star is too cool to apply previously calibrated age–activity relations (e.g., Mamajek & Hillenbrand 2008).
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The detrended TESS light curve of TOI-2018. The color symbols indicate the transits of TOI-2018 b (magenta) and TOI-2018.02 (cyan).
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The phase-folded and binned transit light curves of TOI-2018 b (left) and TOI-2018.02 (right). The best-fit linear ephemeris model is shown in red. We note that TOI-2018.02 is below the typical S/N threshold (5.8 vs. 7.1) to be counted as a planet candidate.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: Comparison of the abundance patterns of the eight stars to that of the superficially normal star ν Cap (HR 7773).
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: TOI-2018 is α-element enhanced and [α/Fe]-depleted, which is suggestive of a thick-disk star. However, the kinematics (UVW) of TOI-2018 only gives a 3.1% chance of being a thick-disk star. The thick-disk membership of the system needs further confirmation. The gray points are [α/Fe] and [Fe/H] for the TESS Input Catalog (Stassun et al. 2019) as presented in Carrillo et al. (2020).
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: Companion sensitivity for the near-infrared AO imaging. The black points represent the 5σ limits and are separated in steps of 1 FWHM; the purple represents the azimuthal dispersion (1σ) of the contrast determinations (see the text). The inset image is of the primary target showing no additional close-in companions.
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The SED of TOI-2018. The red symbols are the various reported photometric measurements of the system (see the text). The horizontal error bars indicate the effective widths of the passbands. The black curve is the best-fit Kurucz atmosphere model (Kurucz 1979), while the blue symbols are the integrated model flux within each passband. No obvious infrared excess is detected.
Paper: Directly Deriving Parameters from SDSS Photometric Images
Authors: Fan Wu, Yude Bu, Mengmeng Zhang, Zhenping Yi, Meng Liu, Xiaoming Kong
Figure caption: Regression results for three stellar atmospheric parameters. In order to more intuitively demonstrate the overall trend, we employ the kernel density estimation (KDE) method to fit the probability density of the result data and use it as the color gradient in the graph. Here, “Bias” refers to the residuals between the sample labels and the model predictions, while “Density” is the probability density fitted to the Bias using the KDE method (the same setting below). The results are (a) effective temperature (T eff), (b) surface gravity (log g), (c) metallicity ([Fe/H]). The figure shows that the T eff and [Fe/H] estimates are good, with σ(T eff) = 172.37 K, σ([Fe/H]) = 0.23 dex. But for ﹩\mathrm{log}g﹩, an anomaly exists. A series of horizontal scatter points is observed near where the label equals 4 dex, and ﹩\sigma (\mathrm{log}g)=0.49﹩ dex.
Paper: Directly Deriving Parameters from SDSS Photometric Images
Authors: Fan Wu, Yude Bu, Mengmeng Zhang, Zhenping Yi, Meng Liu, Xiaoming Kong
Figure caption: Feed-forward process of our model. Our approximate Bayesian framework consists of a deep model for extracting image features and a probabilistic model for producing outputs and uncertainties. In the deep model, we adopted the backbone of ConViT (bottom left), a version of ViT in that some of the MHSA layers are replaced with gated positional self-attention layers (GPSA; middle and right in orange frame). We use 10 GPSA layers followed by 2 vanilla MHSA layers. FFN: feed-forward network (two linear layers separated by a GeLU activation); W qry: query weights; W key: key weights; v pos: attention center and span embeddings (learned); r  qk : relative position encodings; λ: gating parameter; σ: sigmoid function. E(Y) and D(Y) are the sample mean and sample variance, respectively, of the random variable Y. In the probabilistic model, we adopted BNNs (bottom right) to accept the regression token from the backbone. We provide a theoretical analysis that MLP can approximately erode uncertainties (ϵ) from the backbone.
Paper: Directly Deriving Parameters from SDSS Photometric Images
Authors: Fan Wu, Yude Bu, Mengmeng Zhang, Zhenping Yi, Meng Liu, Xiaoming Kong
Figure caption: Distribution of APOGEE stars in the ﹩{T}_{\mathrm{eff}}\mbox{--}\mathrm{log}g﹩ plane. The colorbar utilizes the same color gradient as the scatter plot to represent point density, computed using the KDE method and normalized to a range from 0 to 1. We can clearly see that for different temperatures, there are two distinct ﹩\mathrm{log}g﹩ values, mainly located in the regions above and below 4 dex. Moreover, the strong correlation between T eff and photometry implies that there might be a similar relationship between images and ﹩\mathrm{log}g﹩.
Paper: Directly Deriving Parameters from SDSS Photometric Images
Authors: Fan Wu, Yude Bu, Mengmeng Zhang, Zhenping Yi, Meng Liu, Xiaoming Kong
Figure caption: Results after introducing a classification stage. (a) The regression results for the stars with ﹩\mathrm{log}g﹩ less than 4 dex. (b) The regression results for the stars with ﹩\mathrm{log}g﹩ greater than 4 dex. (c) The final combined results. The figure shows that dividing the stars by ﹩\mathrm{log}g﹩ can effectively eliminate the anomaly in the region with ﹩\mathrm{log}g﹩ greater than 4 dex, resulting in a lower ﹩\sigma (\mathrm{log}g)=0.41﹩ dex.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Fraction of asteroid rotation period matches between TESS and LCDB (U = 3) as a function of the observation and Lomb–Scargle normalized power cutoff. An object falls within a bin if it has at least the number of observations and Lomb–Scargle power as shown on the vertical and horizontal axes, respectively. (Top) Exact matches. (Bottom) Exact and aliased matches. The black outlined cells show the cases where there are more than 200 data points and the normalized Lomb–Scargle power is greater than 0.2, as discussed in the text.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Comparison of the derived periods from this work with the literature periods stored in the LCDB for those objects with greater than 200 detections within TESS.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Generalized Lomb–Scargle periodogram obtained from period analysis for 135886.