adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Masses and Star Formation Rates of Galaxies and AGNs in the eFEDS GAMA09 Field
Authors: Zhibo Yu, 知 博 喻, Fan Zou, 凡 邹, William N. Brandt
Figure caption: Top-left: Comparison between our M ⋆ and M ⋆ from existing catalogs in eFEDS. Top-right: Comparison between our SED-based SFRs and FIR-based SFRs. The dashed lines indicate 0.5 dex deviations. Note that we only plot sources with i-mag <22. Bottom: Number of good bands (with S/N > 5) vs. i-mag. Each blue point represents a source, and the red error bars represent the median, 25th, and 75th percentile of the number of good bands in each magnitude bin.
Paper: Improved Redshifts for DESI EDR Quasars
Authors: Qiaoya Wu, Yue Shen
Figure caption: Median composite spectra around several emission/stellar absorption lines of DESI EDR quasars with large discrepancies between the EDR redshift and the new systemic redshift, generated using the EDR redshifts (left panels) and the improved systemic redshift (right panels). The number of quasars contributing to the coadds for each particular line is listed in the upper right corner of each. The new systemic redshifts for high-redshift quasars (z > 1) perform much better than z EDR in the statistical sense.
Paper: Dataset of Classified Chandra Sources in Globular Clusters
Authors: Steven Chen, Oleg Kargaltsev, Hui Yang, Jeremy Hare, George Pavlov
Figure caption: Screenshot of the visualization tool, showing two plots with different features selected. The inset table shows a summary of classified sources per cluster, with color shading corresponding to number of sources per cluster, normalized by class.
Paper: Citizen Science Discovery of a Recurrently Active Jupiter-Family Comet: (551023) 2012 UQ192
Authors: Jarod A. DeSpain, Colin Orion Chandler, William J. Oldroyd, Henry H. Hsieh, Chadwick A. Trujillo, William A. Burris, Jay K. Kueny, Kennedy A. Farrell, Mark Jesus Mendoza Magbanua, Nima Sedaghat, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes
Figure caption: Two images of 2012 UQ192. The fields of view are 126″ × 126″, with north up and east left. Left: UT 2014 April 30, 90 s VR-band image taken with the DECam on the 4 m Blanco telescope (Cerro Tololo Inter-American Observatory, Chile; Prop. ID 2014A-0283, PI Trilling, observers D. Trilling, L. Allen, J. Rajagopal, T. Axelrod). A clear tail is present, oriented on-sky roughly toward the anti-motion (red −v) direction and pointed toward 2 o’clock. Right: UT 2020 November 12, 30 s r-band ZTF image taken by the 1.22 m Samuel Oschin Telescope (Palomar Observatory, USA) shows a diffuse tail pointed toward the coinciding anti-motion and anti-solar (yellow −⊙) vectors.
Paper: Activity in Centaur-like Jupiter-family Comet 2023 RN3 
Authors: Henry H. Hsieh, Michael S. P. Kelley, Tim A. Lister, Helen Usher, Edward Gomez, Joseph P. Chatelain, Sarah Greenstreet
Figure caption: Single-exposure (90 s) ﹩r^{\prime} ﹩-band images from FTN of 2023 RN3 and a nearby field star with corresponding contour plots. Panels are 15″ × 15″.
Paper: Custom JWST NIRSpec/IFU and MIRI/MRS Data Reduction Pipelines for Solar System Targets
Authors: Oliver R. T. King, Leigh N. Fletcher, Jake Harkett, Michael T. Roman, Henrik Melin
Figure caption: Example cube slices showing JWST/MIRI observations of Saturn (Fletcher et al. 2023) at different stages of our custom data reduction process. The first column shows the output of the standard JWST pipeline, which contains saturation (missing data around Saturn’s North Pole in panel i), partial saturation (dark pixels on Saturn in i), significant flat fields effects (a and g), and limb darkening caused by the instrument PSF (m). The second column shows the data after the application of the desaturation step, the third column shows the data after flat field correction, and the fourth column shows the “final” version of the data after PSF correction. The application of the custom data reduction steps significantly improves the data quality, such as revealing banded structure of Saturn’s atmosphere (panels d and h) that is impossible to see in the standard pipeline output. This figure is an extended version of Figure 3 from Fletcher et al. (2023).
Paper: A Pipeline for Modeling Rapidly Rotating Stars
Authors: Jackson L. Sackrider, Jason P. Aufdenberg
Figure caption: (a) A synthetic image for β CMi at a position angle of 143°, (b) corresponding synthetic visibilities for VERITAS baselines, (c) a synthetic spectrum compared to an archival spectrum (elodie:20020328/0018), (d) a model spectral energy distribution compared to archival absolute spectrophotometry.
Paper: A Dark Siren Measurement of the Hubble Constant with the LIGO/Virgo Gravitational Wave Event GW190412 and DESI Galaxies
Authors: W. Ballard, A. Palmese, I. Magaña Hernandez, S. BenZvi, J. Moon, A. J. Ross, G. Rossi, J. Aguilar, S. Ahlen, R. Blum, D. Brooks, T. Claybaugh, A. de la Macorra, A. Dey, P. Doel, J. E. Forero-Romero, S. Gontcho A Gontcho, K. Honscheid, A. Kremin, M. Manera, A. Meisner, R. Miquel, J. Moustakas, F. Prada, E. Sanchez, G. Tarlé, Z. Zhou
Figure caption: Upper left: GW190412 skymap. The spatial probability is given by the color map and the 50% and 90% CI are shown by the green dashed and solid lines. Each black point is a DESI galaxy. The blue circles represent the bright-time DESI pointings in the region. The red circles are the DESI pointings taken as part of secondary target GW follow-up program. Bottom left: DESI galaxies’ redshift distribution subtracted by that of a uniform-in-comoving-volume distribution, to highlight the presence of overdensities along the GW190412 line-of-sight. Right: H 0 posteriors from this analysis. 1σ constraints from Riess et al. (2022) and Planck Collaboration (2020) are also shown. The vertical lines to indicate the 68% CI of our combined GW170817+GW190412 fiducial result.
Paper: Instrumental Effects of Lyα Properties in CLASSY and Implication for HETDEX and JWST
Authors: Zorayda Martinez, Simon Gazagnes, Danielle A. Berg
Figure caption: Row 1: Presents the evolution of the Errabs for each Lyα property (EW, v red, and v blue) as a function of velocity resolution. Row 2: Shows similar insights for the Errrel, which is the percent difference from the CLASSY measurements. Solid lines show the averaged errors on double peak profiles, dotted lines show the averaged errors on double peak plus absorption profiles, dashed–dotted lines show the averaged errors on single peak profiles, and dashed lines show the averaged errors on absorption-only profiles. From these plots, we see that systematic error increases as velocity resolution increases dramatically, making measurements of some Lyα properties at higher velocity resolutions more unreliable.
Paper: AT 2023prq: A Classical Nova in the Halo of the Andromeda Galaxy
Authors: Michael W. Healy-Kalesh, Daniel A. Perley
Figure caption: Top left: light curve of AT 2023prq. Top right: 4.°5 × 4.°5 DSS image of M31 and its surroundings. AT 2023prq is shown (star) with the two tidal stream CNe (AT 2016dah and AT 2017fyp) from Darnley et al. (2020) for comparison. Bottom: spectra of AT 2023prq with emission lines labeled.
Paper: Using Mg II Doublet to Predict the Lyman Continuum Escape Fraction from 14 HETDEX Galaxies
Authors: Victoria Salazar, Floriane Leclercq, John Chisholm, Gary J. Hill, Gregory R. Zeimann
Figure caption: (a): Comparison of our sample (red) to literature (black: Flury et al. 2022; green: Izotov et al. 2016a, 2016b, 2018a, 2018b, 2021). The red circled points show our LyC leaker candidates from the O32 (crosses) and R (squares) methods (Sections 3 and 2.3). (b): Mg II doublet (black) with best-fit in orange and continuum in blue (Section 2.1). (c): The predicted LyC values from the R and O32 methods are compared to the dust values (Section 2.2). (d): Relation between the predicted ﹩{f}_{\mathrm{esc}}^{\mathrm{LyC}}﹩ and dust, with points color coded by the Mg II escape fraction.
Paper: WRAP: A Tool for Efficient Cross-Identification of Proper Motion Objects Spanning Multiple Surveys
Authors: Hunter Brooks, J. Davy Kirkpatrick, Dan Caselden, Adam C. Schneider, Aaron M. Meisner, Yadukrishna Raghu, Farid Cedeno, Jacqueline K. Faherty, Federico Marocco, Marc J. Kuchner, S. L. Casewell
Figure caption: A flowchart illustrating the WRAP procedure. Here we utilize 2MASSI J1721039+334415 (Bardalez Gagliuffi et al. 2014). It is highlighted in red for CatWISE, WFCAM, and PanSTARRS. The process begins by opening WRAP in a terminal window. Then, the user inputs the coordinates, sets the search radius, and chooses the catalogs for their search. WRAP executes API queries, interacting with the chosen catalog APIs to retrieve relevant data. If the designated region is found through the API, WRAP displays an image of the area with catalog detections overlaid. Users interact by clicking on the image, prompting WRAP to identify the nearest object and writing pertinent information from the catalog into an output file.
Paper: The Jets and the Neutron Star Kick Velocity of the Supernova Remnant CTB 1
Authors: Ealeal Bear, Noam Soker
Figure caption: Upper left panel: An image adapted from Reyes-Iturbide et al. (2024) based on Tomasz Zwolinski (http://astrozdjecia.pl/); white circle from their image. Red and blue are for Hα and [O III]. We added the double-headed arrow to signify the main jets’ axis. Upper right panel: Our identification of morphological features on a picture adapted from Kimberly Sibbald (https://www.flickr.com/photos/spacepaparazzi/51748096139/in/dateposted-public/). Lower left panel: A radio image from Schinzel et al. (2019). We added the jets’ axis and the kick velocity. Lower right panel: Observed cumulative distribution function (black step-function) and four different theoretical cumulative distribution functions.
Paper: False Alarms Revealed in a Planet Search of TESS Light Curves
Authors: Michelle Kunimoto, Steve Bryson, Tansu Daylan, Jack J. Lissauer, Michael R. B. Matesic, Susan E. Mullally, Jason F. Rowe
Figure caption: Period histograms of TCEs and invTCEs identified in various input TESS light curves by our detection pipeline, with insets showing inverted eleanor CORR_FLUX light curves with planet-like false alarms. Transits in the insets are indicated by short blue vertical lines, and the red vertical dashed lines delineate sectors. The filled histograms are TCEs and the line histograms are invTCEs. The vertical gray lines are aliases of the 13.7 days TESS orbital period. Most signals are false alarms. We see that, in all cases, pileups in TCEs correspond to pileups in invTCEs, indicating that many detections in the observed data are false alarms. Top panel: CORR_FLUX light curves, comparing two- and three-transit thresholds for transit detection. Middle panel: Comparing three-transit detections from CORR_FLUX and PCA_FLUX light curves. Lower panel: Comparing three-transit detections from CORR_FLUX and QLP light curves. The lower panel also shows “no sines” TCEs and invTCEs after the removal of sinusoidal signals identified by the SWEET test (see text).
Paper: No Compact Radio Emission from the Proposed Blazar Candidate Counterpart for the Fermi Source 4FGL J1848.7–0129
Authors: Sándor Frey, Krisztina Perger, Krisztina Éva Gabányi
Figure caption: 3 GHz VLASS image cutouts around the position of the proposed blazar source on 2017 November 13 (left) and 2020 August 5 (right). The field is dominated by spurious linear features caused by a nearby bright source southwards, the ultracompact H II region GPSR5 31.243–0.110 (Giveon et al. 2007). The 1σ image noise values in the empty field within a ﹩4^{\prime} \times 4^{\prime} ﹩ region centered on the GMRT source position are 0.26 and 0.25 mJy beam−1 at the first and second epochs, respectively. The corresponding elliptical Gaussian restoring beams are 2.″4 × 2.″9 at 3.°3 major axis position angle and 2.″1 × 2.″8 at −3.°6.
Paper:  FluxCT: A Web Tool for Identifying Contaminating Flux in Kepler and TESS Target Pixel Files
Authors: Jessica Schonhut-Stasik, Keivan Stassun
Figure caption: Returned plot for KIC 11860814. The pink star shows the target source in R.A. (hour angle) and decl. (degrees); gray dotted lines represent on-sky coordinates. Each colored square depicts a pixel. Gray pixels constitute areas without data, dark purple represents pixels not included in the TPA, and Lighter shades of purple through white correspond to the source’s TPA, scaled toward white as flux values increase. White lines around the TPA show the smallest possible polygon, with R.A. and decl. values in each corner. KIC 11860814 has one additional source within the TPA, with a target magnitude of 11.16 and 13.50 for the accompanying source, giving a magnitude difference of ∼2. There is a flux ratio (F 2/F 1) of ∼0.1, resulting in a total flux contamination of 10%. The secondary source has a RUWE of 1.7, suggesting an unresolved double system.
Paper: Recent Updates of Gas-phase Chemical Reactions and Molecular Lines of SiS in CLOUDY
Authors: Gargi Shaw, Gary Ferland, M. Chatzikos
Figure caption: Panel 1: Variation of SiS density as a function of A V for an H II and PDR model (“h2_Orion_hii_pdr.in” from the CLOUDY download under the directory tsuite.) Panel 2: Variation of temperature across the cloud. Panel 3: Model predicted intensities of various SiS rotational lines.
Paper: Possible Disintegration of Main-belt Asteroid 2008 BJ22 
Authors: Sam Deen, Henry H. Hsieh
Figure caption: Left: a ﹩1^{\prime} \times 1^{\prime} ﹩ stack of 2 × 120 s ﹩r^{\prime} ﹩-band images of 2008 BJ22 taken with the Subaru Telescope on 2008 March 4. Right: a ﹩3^{\prime} \times 1^{\prime} ﹩ stack of 2 × 150 s r-band images of 2008 BJ22's expected location taken with DECam on 2013 March 10. The antisolar (− ⊙ ) and antivelocity (−v) vectors are marked in yellow and red, respectively, with the nominal predicted position of the object marked with red crosshairs and the faint linear East-West haze discussed in the text marked with short red lines.
Paper: First Ejection from the PSR B1259-63/LS 2883 High Mass Gamma-Ray Binary Detected During the 2021–2024 Binary Cycle
Authors: Jeremy Hare, George G. Pavlov, Oleg Kargaltsev, Gordon P. Garmire
Figure caption: Chandra ACIS-I images of B1259 with pixel size of 0.″246 648 days after he 2021 periastron passage (left) and 610 days after the 2017 persiastron passage (right).
Paper: Early Galaxy Formation and the Hubble Constant Tension
Authors: Stacy S. McGaugh
Figure caption: Left: The covariance between the density parameter and Hubble constant in CMB fits, Ω m  h 3 = 0.09633 ± 0.00029 (Planck Collaboration et al. 2020a, red line). Also shown are best-fit values from CMB experiments over time, as labeled. These all fall along the line of constant Ω m  h 3, but have diverged from concordance with local data (examples from Cole et al. 2005; Mohayaee & Tully 2005; Tully et al. 2016; Riess et al. 2021) as higher multiples ℓ have been observed. Right: Unbinned Planck data (Planck Collaboration et al. 2020b, points) with the best-fit power spectrum (red line) and a model (blue line) with h = 0.73 and Ω m  adjusted to maintain constant Ω m  h 3. The ratio of the models is shown at bottom, illustrating the subtle need for slightly greater power with increasing ℓthan provided by the model with h = 0.73.
Paper: Discovery of Dust Emission Activity Emanating from Main-belt Asteroid 2015 FW412
Authors: Colin Orion Chandler, Chadwick A. Trujillo, William J. Oldroyd, Jay K. Kueny, William A. Burris, Henry H. Hsieh, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz
Figure caption: 2015 FW412 (green dashed arrow) displays a tail (white arrows) in the anti-motion (−v) direction in these images from the DECam on the Blanco 4 m telescope (Cerro Tololo Inter-American Observatory, Chile). Also indicated is the anti-solar (-⊙) direction. The FOV is about 126″ × 126″. Left: 430 s VR-band, UT 2015 April 13 (Program 2015A-0351, PI Sheppard, observers S. Sheppard, C. Trujillo). Right: 40 s VR-band, 2015 April 18 (Program 2013B-0536, PI Allen, observers L. Allen, D. James).
Paper: Magneto-convective Modeling of Low-mass Pre-main Sequence Stars: Postponing the Depletion of Lithium
Authors: D. J. Mullan, J. MacDonald
Figure caption:  A(7Li) as a function of stellar mass at age 16 Myr in MM10 models. Solid lines: isochrones with different B  v . Empirical data for 2M1222-57A/B are plotted in red and blue respectively.
Paper: New Recurrently Active Main-belt Comet 2010 LH15
Authors: Colin Orion Chandler, William J. Oldroyd, Henry H. Hsieh, Chadwick A. Trujillo, William A. Burris, Jay K. Kueny, Jarod A. DeSpain, Kennedy A. Farrell, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano
Figure caption: 2010 LH15 (green dashed arrows) with a tail (white arrows) oriented on sky roughly toward the anti-solar (yellow −⊙) direction, and counter-clockwise from the anti-motion (red −v) vector. The FOV of each image is 126″ × 126″. Left: UT 2020 September 27 45 s i-band GigaPixel1 exposure on the 1.8 m Pan-STARRS 1 (Haleakala). Center: UT 2019 August 31 Zwicky Transient Facility (ZTF) camera on the 48″ Samuel Oschin telescope (Mt. Palomar) 30 s r band exposure. Right: UT 2019 September 30 90 s Dark Energy Camera (DECam) on the 4 m Blanco telescope (Cerro Tololo Inter-American Observatory, Chile); Prop. ID 2019B-1014, PI Olivares, observers F. Olivares, I. Sanchez. This was the image classified as active by Active Asteroids volunteers.
Paper: Recent Extragalactic Nova Rate Determinations and their Implications
Authors: Massimo Della Valle, Allen W. Shafter, Sumner Starrfield
Figure caption: Measured K-band luminosity-specific nova rates, ν  K , as a function of galaxy color. The black point indicates the Milky Way assuming a nova rate of 40 ± 15 yr−1, which represents an average of recent measurements. The red squares are based on HST nova rate determinations for M49, M51 and M87 made by Ferrarese et al. (2003), Mandel et al. (2023) and Shara et al. (2016), respectively.(The data used to create this figure are available.)
Paper: Observational Constraints on the Metagalactic Lyα Photon Scattering Rate at High Redshift
Authors: Avery Meiksin
Figure caption: Evolution of the galactic UV luminosity density at 1500A (erg s−1 Hz−1 Mpc−3) (upper panel) and the Lyα scattering rate P  α , normalized by the thermalization rate P th (lower panel). The curves correspond to the indicated minimum halo mass thresholds required for star formation.
Paper: Diffusion Coefficients of 56Fe in C–O and O–Ne White Dwarfs
Authors: Matthew E. Caplan
Figure caption: (Top) Dimensionless diffusion coefficients for nuclei in our simulations and (bottom) residuals between the MD and the proposed fits. While ﹩{D}_{\mathrm{Fe}}^{* }﹩ is over-predicted for both (left) C–O and (right) O–Ne mixtures, I find that the fit is marginally better for the O–Ne mixture due to the smaller charge ratio between the 56Fe nuclei and the background.
Paper: DRAGONS—A Quick Overview
Authors: K. Labrie, C. Simpson, R. Cardenes, J. Turner, M. Soraisam, B. Quint, O. Oberdorf, V. M. Placco, D. Berke, O. Smirnova, S. Conseil, W. D. Vacca, J. Thomas-Osip
Figure caption: Screenshots of a raw GMOS longslit spectroscopic observation (top-left), a 2D spectrum from a corrected and stacked 4-frame sequence with spatial and wavelength offsets (top-right), and the final extracted spectrum of the central source (bottom). The source is a DB white dwarf candidate.
Paper: The Distribution of High-excitation OCS Emission Around the Cep A-East Protostellar Cluster
Authors: C. Codella, R. Bachiller, S. Viti
Figure caption: Left: Countour maps of the integrated emission (in the −20, +5 km s−1 range) of the OCS(17–16), and OCS(18–17) emission toward CepA-East. The triangles stand for the VLA 2 cm continuum components which trace strings of shocked regions (Garay et al. 1996). The maps are centered at the HW2 position (see text). The circles show the beam (HPBW), while the crosses mark the observed positions. The first contours and steps correspond to 3σ (0.30 K km s−1). Right: OCS spectra (T MB scale) observed at the map center. The dashed lines stand for the LSR velocity (–10.7 km s−1, Codella et al. 2005).
Paper: Anthropogenic Coal Ash as a Contaminant in a Micro-meteoritic Underwater Search
Authors: Patricio A. Gallardo
Figure caption: Beryllium, lanthanum, uranium and nickel concentrations in BeLaU (green) samples. Histogram shows frequencies obtained from COALQUAL. Concentrations are within expectation for all elements.
Paper: Parallelization of the Symplectic Massive Body Algorithm (SyMBA) N-body Code
Authors: Tommy Chi Ho Lau, Man Hoi Lee
Figure caption: Benchmarking results of SyMBAp with the 4 conditions. Top: Wall clock times with respect to the number of threads. Arrows on the y-axis indicate the wall clock times using the original SyMBA. Bottom: Normalized wall clock times for SyMBAp.
Paper: SNART: Synchrotron Self Absorption Model For Non-relativistic Transients
Authors: Lindsay DeMarchi, Daniel Finstad, R. Margutti
Figure caption: An example of SNART outputs on the test case of SN 2004C (DeMarchi et al. 2022). The power of SNART is its calculation of physical parameters after modeling radio data (see top left corner for an example model). Different models can be compared on shared plots of physical parameters (see varying color and markertypes) or viewed alone (see bottom right panel). Changes to microphysical parameters such as ϵ are also comparable (green circular points vs. other marker styles). Single sided power laws in the modeling stage become upper limits of physical parameters (down-pointing arrows).
Paper: Observations of GRB 230307A by TESS
Authors: Michael M. Fausnaugh, Rahul Jayaraman, Roland Vanderspek, George R. Ricker, Christopher J. Burke, Knicole D. Colón, Scott W. Fleming, Hannah M. Lewis, Susan Mullally, Allison Youngblood, Thomas Barclay, Eric Burns, David W. Latham, S. Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: TESS light curve of GRB 230307A. The large star shows the prompt emission coincident with the Fermi discovery at BJD−2,460,000 = 11.15549 days (vertical red line). The gray marks show the 200 s cadence light curve, and the black points show the light curve binned to 1600 s. The limiting magnitude in 1600 s is 18.63, based on the scatter of the light curve prior to the GRB discovery. All timestamps are given relative to 2,460,000 BJD. Fits for two models of the afterglow are shown: a double power law (PL) and a fast-rise exponential-decay (FRED) model. For both fits, we excluded the prompt emission at the time of the Fermi trigger. Models were fit to the original light curve sampled at 200 s—data are binned here only for display purposes. The horizontal dashed line shows the residual background of the FRED model, which is a nuisance parameter in our fits. The vertical blue line shows the break time t break of the double power law. The TESS light curve is available at https://tess.mit.edu/public/tesstransients/light_curves/lc_grb230307A_cleaned.txt.
Paper: On the Recent Discovery of Coronal [Fe X]λ6374 Emission in the Low-metallicity Dwarf Galaxy SDSS J0944-0038
Authors: E. C. Herenz, G. Micheva, P. M. Weilbacher, A. Monreal-Ibero, M. Hayes, F. Anders, T. Rivinius
Figure caption: Spectral excerpt from “Nucleus 1” of J0944 from VLT/MUSE observations and the two modeling steps to subtract emission lines other than [Fe X]λ6374 and the continuum. The expected positions of the emission lines are marked and labeled by dotted lines that are colored according to species, with the rightmost black dotted line marking [Fe X]λ6374. The top panel shows the spectrum and the Gaussian models for the [O I]λ λ6300, 6363 and [S III]λ6313 lines. The inset shows a synthesized R-band from the MUSE datacube and the position of the circular 1″ extraction aperture. The middle panel shows the residual after subtracting this model. We modeled the Si II λ6371 line based on the Gaussian fit to the Si II λ6347 line (magenta line). The residual after subtraction of this model is shown in the bottom panel. The blue line indicates the noise.