adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Log(temperature)-log(temperature) plot of F090W–F150W vs. F250M–F430M for all objects (red: type 1 objects; blue: type 2 objects; and yellow: type 3 objects). The gray line shows where temperatures for both colors are the same to indicate how well the objects are represented by a blackbody. If our objects are embedded clusters, the infrared colors are affected by extinction and infrared excess of young stars and less sensitive to effective temperature, which may explain the larger F250M–F430M uncertainties at higher temperatures.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Top: mass of type 1 objects vs. the mass of the CO core that the object is associated with. Bottom: histogram of object radii in pc for each of the three objects types.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Top: GALEX FUV image of WLM showing FUV-bright star-forming region (pink box). Bottom: close-up of the FUV-bright star-forming region in Spitzer 8 μm showing that type 1 objects (red circles) are typically associated with 8 μm sources while most type 2 objects (blue circles) do not overlap 8 μm sources. The CO cores within the type 1 objects are also included (orange circles).
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of each type 2 object (in FUV and away from CO; blue circles). The orientation of the image is such that north is up and east is to the left. The object number corresponding to the number in the extended version of Table 2 provided in the online materials is given in the upper right of the image.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of each type 1 object (in FUV and near CO, red circles) and the CO cores (orange circles) within them. The orientation of the image is such that north is up and east is to the left. The object number corresponding to the number in Table 2 is given in the upper right of the image.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Mass histograms near star formation: type 1 (red with circle hatches) and a comparison of all type 2 objects (dark blue; 2a) to only type 2 objects in the ALMA FOV where CO was observered (light blue; 2b). Mass is in units of M ⊙.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of each type 3 object (away from FUV and away from CO; yellow circles). The orientation of the image is such that north is up and east is to the left. The object number corresponding to the number in the extended version of Table 2 provided in the online materials is given in the upper right of the image.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of select obvious background galaxies (magenta circles). The orientation of the image is such that North is up and East is to the left. The object number corresponding to the number in the extended version of Table 2 provided in the online materials is given in the upper right of the image.
Paper: Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope
Authors: Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang
Figure caption: Schematic of different collision detection situations. (a; top) the first situation; (b; middle) the second situation; (c; down) the third situation.
Paper: Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope
Authors: Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang
Figure caption: Schematic of a theta-phi positioner: O represents the center of the RFP, L 1 represents the rotational center of the eccentric arm, L 2 represents the fiber end, l  θ  is the length of the central arm, and l  φ  is length of the eccentric arm.
Paper: Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope
Authors: Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang
Figure caption: Schematic of selected WR with nearest target but large theta rotation angle, and its six neighbors.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: In each plot on the left, correlated noises simulated using a GP with an SHO kernel are added (blue line) to an original light curve containing a transit of depth Δ = 0.8%, duration D = 0.1 day, and white noise with a standard deviation of 0.15% (top left). The hyperparameters of the kernel are fixed to Q = 10 and σ = 0.8%, with the pulsation ω increasing from top to bottom. The resulting stellar variability signals are then reconstructed using (in purple) Tukey’s bi-weight filter with an optimal window size of 3 × D (see Hippke et al. 2019), and (in red) a GP with the same kernel used to simulate the data. In each case the variability is reconstructed, subtracted, and the transit S/N computed using Equation (2).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Transit S/N computed for 10,000 differential light curves with varying morphological characteristics. All light curves span 2.8 days with an exposure time of 2 minutes and contain the same transit signal of duration D = 1 hr, depth of 0.5%, and white noise with a standard deviation of 0.1%. Light curves at the top and right side of the central plot are shown with their corresponding τ and δ values, which again correspond to the relative timescale of stellar variability against the transit duration, and the relative amplitude of stellar variability against the transit depth. The two central plots show the transit S/N after detrending the light curves with one of two methods. On the left, light curves are detrended using Tukey’s bi-weight filter with an optimal window size of 3 × D (see Hippke et al. 2019), while on the right, light curves are detrended using a GP with the same kernel used to simulate the data.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Principle and output of the linear search. The simulated data set (top) corresponds to the one shown and described in Figure 1. First, a set of durations and depths { T  i , D  j  } i,j  is generated. For each pair of indices (i,j), the likelihood ﹩\mathrm{ln}p({\boldsymbol{f}}| {T}_{i},{D}_{j},{{\rm{\Delta }}}_{i,j})﹩ is computed using the parameters from Equation (6) and the expression of Equation (5). This process yields the grid of log-likelihoods ﹩\mathrm{ln}{ \mathcal L }﹩ (bottom plot), as well as the {Δ i,j , σ  i,j } i,j  transit depths and errors inferred linearly using Equation (6).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Rate of true positives for the 4000 simulated light curves. The color scale represents the fraction of true positives, white if all injected transits are recovered in a given portion of the (τ, δ) parameter space, and black if none are recovered.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Trimmed and cleaned single-sector light curve of the target TIC 1019692. The top plot shows how much of the data is truncated and sigma clipped, resulting in a quasi-continuous light curve shown in the bottom plot. On this bottom plot, the black line corresponds to the mean of the GP model (with hyperparameters optimized here on the cleaned light curve).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Periodic search likelihood ﹩{ \mathcal P }(P)﹩ computed for different trial periods P. Notice how the maximum value of ﹩{ \mathcal P }﹩ for the alias period P = 0.35 day (left plot) is lower than for P = 2 × 0.35 = 0.7 day, a result of combining the log-likelihoods using Equation (8) instead of Equation (7), in favor of individual transits matching a common depth Δ.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Rate of true and false positives for all methods as a fraction of detectable transit signals.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Binned statistics of the injection–recovery of 4000 transit signals in a flat light curve with only white noise using BLS and nuance. The color scale indicates the recovery of transits in the corresponding (period, depth) parameter space, white for a full recovery and black for no detection.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: For each period P, the joint likelihood ﹩{ \mathcal P }(P)﹩ is computed using Equation (8), and the value of the maximum-likelihood transit S/N is retained as ﹩{ \mathcal Q }(P)﹩.
Paper: Dense Outflowing Molecular Gas in Massive Star-forming Regions
Authors: Yani Xu, 雅霓 徐, Junzhi Wang, 均智 王, Shu Liu, 姝 刘, Juan Li, 娟 李, Yuqiang Li, 郁强 李, Rui Luo, 睿 罗, Chao Ou, 超 欧, Siqi Zheng, 思琪 郑, Yijia Liu, 怡嘉 刘
Figure caption: The line wing spatial distributions of HCN 3-2. The source names are shown in the panels. Each panel shows the velocity integrated intensity distribution of blue and/or red wings traced by HCN 3-2. The grayscales illustrate the positions of cloud cores traced by H13CN 3-2. The cyan dotted line boxes indicate signal coverage. The detailed parameters for maps of this and other sources are presented in Table 2.
Paper: Dense Outflowing Molecular Gas in Massive Star-forming Regions
Authors: Yani Xu, 雅霓 徐, Junzhi Wang, 均智 王, Shu Liu, 姝 刘, Juan Li, 娟 李, Yuqiang Li, 郁强 李, Rui Luo, 睿 罗, Chao Ou, 超 欧, Siqi Zheng, 思琪 郑, Yijia Liu, 怡嘉 刘
Figure caption: The left panel presents the outflow mass vs. the cloud core mass for 23 sources. The right panel presents the mass-loss rate vs. the cloud core mass for 15 sources. The solid lines are obtained through linear regression using the least squares method.
Paper: Dense Outflowing Molecular Gas in Massive Star-forming Regions
Authors: Yani Xu, 雅霓 徐, Junzhi Wang, 均智 王, Shu Liu, 姝 刘, Juan Li, 娟 李, Yuqiang Li, 郁强 李, Rui Luo, 睿 罗, Chao Ou, 超 欧, Siqi Zheng, 思琪 郑, Yijia Liu, 怡嘉 刘
Figure caption: The relationship between the outflow mass traced by HCO+ 3-2 and HCN 3-2 for 33 sources. In the left, outflow mass traced by HCO+ 3-2 is obtained with fixed HCO+ abundance, while it is unfixed to derive outflow mass traced by HCO+ 3-2 in the right. The solid lines represent the fitting results.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Point sources from the NIRCam/F356W+F444W image are shown with the MIRI F2550W PSF-subtracted image superimposed in red. Extracted NIRCam sources without HST counterparts are shown as green circles; NIRCam sources with HST-detected background objects (yellow); and instrument artifacts associated with the edge of the coronagraphic mask field of view (white). Source labels correspond to objects listed in Table 3. The red dotted circles denote the expected position of Fomalhaut b (Gáspár & Rieke 2020). No object is seen in this vicinity. We also note the presence of a bright MIRI point source at about 20″ East of Fomalhaut that does not have a NIRCam counterpart. The location of this point source, marked with a white arrow, coincides with the point source marked in Figure 6 of Janson et al. (2015).
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: (Top) PCA reduction of the inner, speckle-dominated, region (inside ∼1.″5). To emphasize the better results in the F444W filter, the images are displayed with the same absolute scale. The residual noise level is worse in the F356W image due to the brighter stellar flux and shorter integration time. (Bottom) S/N map from a forward model match filter (FMMF) analysis of the inner region of the Fomalhaut data. Pixels that yield an S/N of ∼5 are associated with residual bad pixels identifiable in the PSF-subtracted images and/or with residual instrument-related striping (diagonal structures going from the upper right to the lower left). There are no statistically significant peaks that could be ascribed to a planetary companion.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Coronagraphic full array observations of Fomalhaut with NIRCam achieve a 3σ sensitivity below 10−7 contrast at large separations from the star, limited primarily by the background and integration time. At an age of 440 Myr (Mamajek 2012), this contrast limit translates to a detection limit below 1  M Jup outside of 2″, based on either AMES-Cond (Baraffe et al. 2003) or BEX-HELIOS (Linder et al. 2019) evolutionary models.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Zoomed-in F356W+F444W composite image highlighting the NIRCam sources (S1-S7 and one HST source (see Table 3 for details). The negative–positive–negative pattern reflects the effects of the roll subtraction. The image was Gaussian-filtered with a σ = 2 pixel kernel.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Combined F356+F444W full-frame classical ADI-reduced image showing some of the sources detected with NIRCam (labeled S1-S7) within and adjacent to the debris disk system. As discussed later in the text (Section 4) the figure also shows sources identified in Keck H-band imaging (Kennedy et al. 2023) obtained in 2005–2011 when Fomalhaut was ∼5″ from the position at which the NIRCam data were obtained (Epoch = 2022.808). Also shown are background sources detected with Spitzer 4.5 μm imaging from 2006.9 (Marengo et al. 2009).
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: HST/STIS image from 2014 (left) and MIRI F2550W (right) showing the detection of S3 in both the HST and MIRI data. The source is detected at α = 22h57m40.ˢ73, ﹩\delta =-29^\circ 37^{\prime} 32\buildrel{\prime\prime}\over{.} 63﹩ in the HST/STIS image and offset by 0.″39 in the MIRI image at α = 22h57m40.ˢ76, δ = −29°37′32.″53.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Classical ADI reductions for the full-frame data sets for F356W (left) and F444W (right). The negative–positive–negative images surrounding each source are due to the subtraction of the two rolls as discussed in the text.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Coadded full-frame images (﹩2\buildrel{\,\prime}\over{.} 2\times 2\buildrel{\,\prime}\over{.} 2﹩) for F356W (left) and F444W (right) before post-processing to remove residual starlight.
Paper: Searching for Planets Orbiting Fomalhaut with JWST/NIRCam
Authors: Marie Ygouf, Charles A. Beichman, Jorge Llop-Sayson, Geoffrey Bryden, Jarron M. Leisenring, András Gáspár, John E. Krist, Marcia J. Rieke, George H. Rieke, Schuyler Grace Wolff, Thomas L. Roellig, Kate Su, Kevin N. Hainline, Klaus W. Hodapp, Thomas P. Greene, Michael R. Meyer, Douglas M. Kelly, Karl Misselt, John Stansberry, Martha Boyer, Doug Johnstone, Scott Horner, Alexandra Z. Greenbaum
Figure caption: Single F356W full-frame images (﹩2\buildrel{\,\prime}\over{.} 2\times 2\buildrel{\,\prime}\over{.} 2﹩): raw (left) and corrected from horizontal stripes (right).
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Distribution of the Random Forest pseudo-probability P RF for the optimized classifier on the training and validation sets. The purple triangles represent light curves with injected transiting exoplanet signals that passed human vetting and were utilized in the positive training set (Section 4.1). The green diamonds represent the 133 candidates identified in M20 that assisted in optimizing the classifier. The black points indicate random light curves that were given negative class labels; most have P RF values near zero. The orange points represent light curves with injected False Positive signals (Section 4.2). Our chosen threshold for the final classifier is shown as the blue dashed line at P RF = 0.300. The strong performance of the classifier is directly visible: purple and green points lie mostly above the threshold, while the black and orange points lie mostly below the threshold.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Comparison of the orbital parameters found from the best TCF peak with the injected orbital parameters for the synthetic injected planets. Recovered injections are shown as purple triangles. (a) Injected and recovered orbital periods. Dotted lines show integer ratios between the injected and TCF periods. (b) Injected and recovered planet radii. (c) Distribution of the injected planets in period–radius space.
Paper: DIAmante TESS AutoRegressive Planet Search (DTARPS). I. Analysis of 0.9 Million Light Curves
Authors: Elizabeth J. Melton, Eric D. Feigelson, Marco Montalto, Gabriel A. Caceres, Andrew W. Rosenswie, Cullen S. Abelson
Figure caption: Performance of the final Random Forest classifier for every possible threshold choice shown with the Receiver Operator Characteristic (left) and Precision–Recall (right) curves. The solid lines derive from application to the validation set, and the dashed lines are the recall from 133 planet candidates of M20. Our choice of threshold P RF = 0.300 (shown in green) is compared with other possible threshold choices, including the 1% FPR choice used by M20 (purple).