adsabs/AstroCLIMB huggingface dataset:
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN trajectory on 2014 December 29, shown in three projections: (a) X–Z plane, (b) Y–Z plane, and (c) X–R plane, where ﹩R=\sqrt{{Y}^{2}+{Z}^{2}}﹩. In panels (a) and (c), the nominal bow shock (BS) and induced magnetosphere boundary (IMB) are shown as black lines based on the model by D. Vignes et al. (2000). The red star marks the location of the CS crossing.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN crossing of the Martian induced magnetosphere on 2015 September 3. The time series of the magnetic field in MSO coordinates, the energy–time spectrogram of ions, electrons, and solar wind ions. The position of MAVEN in MSO is given below the panels. The crossings of the bow shock and the tail CS are labeled by vertical black and red dashed lines, respectively.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN crossing of the Martian induced magnetosphere on 2016 February 2. The time series of the magnetic field in MSO coordinates, the energy–time spectrogram of ions and solar wind ions. The position of MAVEN in MSO is given below the panels. The crossings of the bow shock and the tail CS are labeled by vertical black and red dashed lines, respectively.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN’s trajectory on 2015 September 3. The format is the same as Figure 3.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: The distribution of the BX component in the modified Mars-Solar-Electric-field (MSE) coordinates (−3RM < XMSE < − 0.5RM) when the average upstream IMF ((B1 + B2)/2) is significantly (a) sunward (cone angle <60°) and (b) tailward (cone angle >120°); (c) cross-flow (70° <  cone angle <110°). The average configurations of the tail current sheet structure are marked by the solid black lines. (a)–(c) represent the current sheet configurations without crustal magnetic field effects. (d)–(f) represent the current sheet configurations with crustal magnetic fields effects.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: The distribution of the BX component in the modified Mars-Solar-Electric-field (MSE) coordinates (−1.5RM < XMSE < −0.5RM) when the average upstream IMF ((B1 + B2)/2) is significantly (a) sunward (cone angle <60°) and (b) tailward (cone angle > 120°); (c) cross-flow (70° < cone angle < 110°). The average configurations of the tail current sheet structure are marked by the solid black lines. (a)–(c) represent the current sheet configurations without crustal magnetic field effects. (d)–(f) represent the current sheet configurations with crustal magnetic fields effects.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Treatment of blended sources, to avoid biased measurement of structural parameters contaminated by neighboring sources. In the surface brightness profile, the black points with error bars are measured by aperture photometry, the red dashed line shows the single-component model profile, the green dashed line the multicomponent model, which includes the target galaxy and the contaminating neighbor, and the blue dashed line represents the PSF, scaled to match the model profile. It is clear that the outer region of the target galaxy is heavily contaminated by the neighbor, and the additional component is necessary to measure the structural parameters of the target galaxy accurately. The images show, from left to right, the original image, the single-component model, the multicomponent model, and the respective residuals for the two models.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: Scatterplot represents the shifted distance of the CS as a function of the IMF cone angle. The lengths of the horizontal error bars represent the IMF cone angle deviation between the IMF for inbound and outbound bow shock crossings. The lengths of the vertical error bars represent the uncertainty of the shifted distance from the uncertainty of the CS normal estimated by the MVA.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Simultaneous, multiband fitting of the galaxy EGS−20408 (M. Stefanon et al. 2017) at z = 5.373. Rows from top to bottom are the results for the F115W, F150W, F200W, F277W, F356W, F410M, and F444W bands. Columns from left to right are the surface brightness profile, input science image, model image (convolved with the PSF), and residual image. The ﹩{\chi }_{\nu }^{2}﹩ for each band is given in the residual image, and the structural parameters are shown in the lower-left corner of the model image. In the surface brightness profile, the black points with error bars are measured by aperture photometry, the red dashed line shows the model profile, and the blue dashed line represents the PSF, scaled to match the model profile.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: The distribution of the BX component in the modified Mars-Solar-Electric field (MSE) coordinates under high and low solar EUV conditions.
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: Magnetic maps of the average BX component in the Martian magnetotail, separated +BY IMF (a) and −BY IMF (b) conditions in the same format as G. A. DiBraccio et al. (2022).
Paper: Statistical Investigations of the Radial Interplanetary Magnetic Field Component Impact on the Magnetotail Current Sheet Structure of Mars: MAVEN Observations
Authors: Yuanzheng Wen, Zhaojin Rong, Hans Nilsson, Chi Zhang, Han-Wen Shen, Jiawei Gao
Figure caption: MAVEN’s trajectory on 2016 February 2. The format is the same as Figure 3.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Dependence on galaxy properties of the color gradient, quantified using the variation of the effective radius ﹩{ \mathcal R }﹩ (Equation (3); top), variation of the Sérsic index ﹩{ \mathcal N }﹩ (Equation (2); middle), and the color gradient ∇ (Equation (4); bottom). From left to right, the columns show the dependence on galaxy optical effective radius (﹩{R}_{e}^{{\rm{opt}}}﹩), stellar masses (M*), and the rest-frame UV-to-optical color. The white contours denote the density distribution of the data points, the stars show the running median of the data binned so that each bin contains at least 60 galaxies, and the error bars indicate the standard deviation. The solid line gives the best-fit linear regression of the individual measurements. The background gradient denotes the region where the color gradient is positive (blue) or negative (red).
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Distribution of redshift and stellar mass of our final sample of 441 galaxies (orange points). Blue points correspond to galaxies with blending flag 1 or 2 in the initial sample. The stellar mass spans a wide range, from M* = 107.5 to 1011 M⊙. The extreme massive galaxies with M* > 1011 M⊙ at z ≳ 4 should be treated with caution; they are likely to be low-redshift interlopers introduced by errors in their photometric redshifts.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Example of galaxies with (a) negative and (b) positive color gradient in our sample. In each panel, the left column shows the best-fit Sérsic model profile for the rest-frame UV and optical bands (top) and the UV−optical color profile (bottom), where the blue shaded area shows the 16th and 84th percentile of the color profile derived by sampling the structural parameter according to its uncertainty. The right column of each panel shows the two-dimensional visualizations of the color gradients: from top to bottom, the panels show the science images from the rest-frame UV and optical, the pseudocolor image (red = F444W, green = F277W, blue = F150W), and the PSF-matched UV−optical color image.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: The stellar mass vs. size and stellar mass vs. specific SFR (sSFR) distributions of our sample. From left to right, the columns quantify the color gradient using ﹩{ \mathcal R }﹩, ﹩{ \mathcal N }﹩, and ∇, whose strength is indicated by the color bar on the top. The squares denote median values of at least five objects within a box of size 0.25 dex in ﹩\mathrm{log}{M}_{\star }﹩ and 0.11 dex in ﹩\mathrm{log}{R}_{e}^{{\rm{opt}}}﹩ or 0.13 mag in rest-frame UV-to-optical color, after performing a locally weighted regression smoothing using the Python package LOESS (M. Cappellari et al. 2013).
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: The redshift evolution of the color gradient, quantified using the variation of the effective radius ﹩{ \mathcal R }﹩ (Equation (3); top), variation of the Sérsic index ﹩{ \mathcal N }﹩ (Equation (2); middle), and the color gradient ∇ (Equation (4); bottom). The x-axis stands for the median redshift of each redshift bin. The open white points correspond to individual measurements. The black stars indicate the median value for each redshift bin, with the error bars giving the 16th and 84th percentile of the distribution. The background gradient describes the region where the color gradient is positive (blue) or negative (red).
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Pseudocolor (red = F444W, green = F277W, blue = F150W) images of galaxies with positive color gradients that show evidence of hosting a central point-like source.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: The distribution of mass-weighted ages of galaxies with AV < 0.4 mag of (a) all stellar masses, (b) M⋆ ≥ 109 M⊙, and (c) M⋆ < 109 M⊙ having negative (red) and positive (blue) color gradient. The p-value of the KS test is shown on the upper left corner of each panel.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: The correlation between dust attenuation and ∇ in our sample. Dusty systems (AV > 1 mag) are highlighted in red stars. The blue contours display the distribution of all sample galaxies, with the black solid line indicating the best-fit linear regression.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Statistics of color gradients for the 441 galaxies in our sample, given separately for the three methods (﹩{ \mathcal R }﹩, ﹩{ \mathcal N }﹩, ∇) used to measure color gradient.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Influence of a “blue nucleus” on the measurements, for F150W (top) and F444W (bottom). In the surface brightness profile, the black points with error bars are measured by aperture photometry, the red dashed line shows the single-Sérsic model, the green dashed line refers to the Sérsic+point source model, and the blue dashed line represents the PSF, scaled to match the model profile. The lower panel of the left column shows the residuals between the Sérsic+point source model and the data. The images show, from left to right, the original image, the single-Sérsic model, the Sérsic+point source model, and the respective residuals for the two models. It is clear that including the nucleus component improves the quality of the fit, and that the additional component is necessary to measure accurately the structural parameters of the host galaxy.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: The bias of ﹩{ \mathcal R }﹩ as a function of F150W magnitude, for ﹩{ \mathcal R }=0.53﹩ (top), 1.00 (middle), and 1.87 (bottom), and, for columns from left to right, different values in input ﹩{R}_{e}^{{\rm{F444W}}}﹩. The colors indicate the input values of the Sérsic index n at F444W. The gray-shaded region marks the magnitude range below 5σ detection at HST/WFC3 F160W.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: Dependence of the variation in effective radius ﹩{ \mathcal R }﹩ on galaxy effective radius Re measured in F115W (left), the median of different bands (middle), and F444W (right). The solid line gives the best-fit linear regression. The error bars indicate the median uncertainty of the data points. The blue-filled contour shows the density distribution of the data points, where the darker color signifies higher density.
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: As in Figure B1, but for the bias of ﹩{ \mathcal N }﹩, for ﹩{ \mathcal N }=0.66﹩ (top), 1.00 (middle), and 1.53 (bottom).
Paper: A High Incidence of Central Star Formation Inferred from the Color Gradients of Galaxies at z > 4
Authors: Bingcheng Jin, 秉诚 金, Luis C. Ho, Wen Sun, 文 孙
Figure caption: As in Figure B1, but for the bias of ∇, for ﹩{ \mathcal N }=0.66﹩ (top), 1.00 (middle), and 1.53 (bottom).
Paper: A Gigaparsec-scale Hydrodynamic Volume Reconstructed with Deep Learning
Authors: Cooper Jacobus, Roger de Belsunce, Solène Chabanier, Peter Harrington, J. D. Emberson, Zarija Lukić, Salman Habib
Figure caption: Visualization of the 960 h−1 Mpc wide baryon density volume we have reconstructed using our machine learning model. The dashed box highlights a region 80 h−1 Mpc wide, which is the size of our training data and comparable to existing simulations used for DESI (M. Walther et al. 2021, 2025) and other surveys.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Mode amplitudes, with f-modes displayed as the large filled circles and p-modes displayed as the open circles, with the symbol size decreasing as n increases (from n = 1 to n = 10), vs. angular degree ℓ. Top: mode amplitudes just after a merger with a Neptune-mass impactor mimp = MNep (Equation (12), no damping applied). Bottom: maximum mode amplitude set by shocks (Equation (14)). Notice ∣cmom∣ and ﹩| {c}_{{\rm{\max }}}| ﹩ have opposite trends with ℓ and n. The mode amplitude after impact is given by ﹩c={\rm{\min }}({c}_{{\rm{mom}}},{c}_{{\rm{\max }}})﹩.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Profiles of different quantities with optical depth τ inside the super-Jupiter. Top: ratio of radiative to total internal luminosity Lrad/L and thermal time tth (Equation (2)) multiplied by the mode frequency ω, for the (ℓ, n) = (0, 1) p-mode. Energy transport by radiation dominates only near the photosphere (τ ≲ 1), and oscillations are approximately adiabatic everywhere (tthω ≫ 1). Bottom: comparing how the mode perturbs the radiative luminosity ﹩{\rm{\Delta }}\widetilde{L}/{L}_{{\rm{rad}}}﹩, compared to the radial displacement ﹩{\widetilde{\xi }}_{r}/{R}_{{\rm{p}}}﹩ and Lagrangian pressure perturbation ﹩{\rm{\Delta }}\widetilde{P}/P﹩. Jumps in ﹩{\rm{\Delta }}\widetilde{L}/{L}_{{\rm{rad}}}﹩ at large optical depths (τ ≫ 1) occur because of variations in the opacity. The transition of hydrogen from ionized to neutral near τ ∼ 1010 affects the adiabatic sound speed, causing the small dip in ﹩{\rm{\Delta }}\widetilde{P}/P﹩.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Mode periods Pmode = 2π/ω, vs. angular degree ℓ and radial node number n. The f-modes are displayed by the large filled circles, while the p-modes are the open circles, whose size decreases as n increases from n = 1 to n = 10. Notice ℓ < 2 do not have f-modes. The mode periods Pmode decrease as ℓ and n increase.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: We display ﹩{\widetilde{\xi }}_{r}﹩ profiles for f-modes (n = 0) and p-modes (n > 0), for the angular degrees ℓ and radial node numbers n indicated. The number of radial nodes n equals the number of times ﹩{{ \mathcal Y }}_{1}﹩ crosses zero in the radial direction (Equation (1)), excepting the origin. When the mode’s self-gravity is small (﹩\delta \widetilde{{\rm{\Phi }}}\approx 0﹩), n counts the nodes in the radial displacement ﹩{\widetilde{\xi }}_{r}﹩. We normalize ﹩{\widetilde{\xi }}_{r}﹩ using Equation (7).
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Visualizations of f-modes (n = 0) and p-modes (n > 0), for the angular degrees ℓ indicated. The interior colors display a temperature excess (ΔT > 0; red) or deficit (ΔT < 0; blue) due to the oscillation. The color scale is linear in all diagrams, although the maximum and minimum ΔT/T values vary, clipping the color scale to retain detail closer to the planet’s center.
Paper: Effects of Dark Matter Self-interactions on Sagittarius and its Stream
Authors: Connor Hainje, Oren Slone, Mariangela Lisanti, Denis Erkal
Figure caption: Results from the best-fit simulations of the CDM (black) and SIDM (blue) IC suites, for the MDM,s = 1010M⊙ progenitor. The SIDM model assumes a velocity-independent cross section of σ/mχ = 30 cm2 g. The left panel shows the final positions of the satellite star particles in the orbital plane, rotated to place the progenitor on the x-axis. The middle and right panels show the mass from stars and dark matter enclosed within 5 kpc of the progenitor position as a function of time, with pericenter times marked by squares, and the time axis shifted to place present day at time = 0. The radius 5 kpc is chosen for comparison with the mass estimates of E. Vasiliev & V. Belokurov (2020), indicated by gray circles. The gray triangle (with black outline) in the left panel marks the target position of the progenitor. This SIDM model exhibits significantly enhanced mass loss relative to CDM in stars and especially in dark matter.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Mode damping timescales 1/γ, with f-modes displayed as the large filled circles and p-modes displayed as the open circles, with the symbol size decreasing as n increases (from n = 1 to n = 10), vs. angular degree ℓ. Top: damping from radiative diffusion. Bottom: damping from turbulent convection. Notice that the two damping timescales tend to be comparable in magnitude.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Fractional bolometric luminosity variation (top panels), radial displacement (middle panels), and fractional temperature perturbation (bottom panels) at the surface after a merger with a Neptune-mass body, for modes with radial node numbers n = 0 (larger closed circles) and n = 1 (smaller open circles), with varying angular degree ℓ. Modes with n > 1 vary surface ∣ΔL/L∣, ∣ξr/r∣, and ∣ΔT/T∣ at amplitudes smaller than 10−4. The different columns display different lengths of time after the merger. After impact, numerous normal modes persist over timescales comparable to the age of β Pic b.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Observed luminosity variation from β Pic b oscillations after a merger with a Neptune-mass body, for modes with radial node numbers n = 0 (larger closed circles) and n = 1 (smaller open circles), with varying angular degree ℓ. The modes with n > 1 vary the planet’s luminosity with amplitudes smaller than 10−4. The different panels display different lengths of time after the merger. Planetary normal modes cause brightness variations whose amplitudes can exceed a percent for several million years.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: The radial displacement (top panel) and temperature variation (bottom panel) at the surface just after impact (no damping applied) vs. angular degree. The large filled circles denote f-modes, while the open circles denote p-modes, with the symbol size decreasing as n increases (from n = 1 to n = 10). Modes with high ℓ, n are strongly nonlinear (∣∂ξr/∂r∣ ∼ 1), with order-unity variations in ∣ΔT/T∣.
Paper: Seismic Oscillations Excited by Giant Impacts in Directly Imaged Giant Planets
Authors: J. J. Zanazzi, Eugene Chiang, Yifan Zhou
Figure caption: Injecting a ℓ = 0, n = 1 p-mode oscillation with period Pmode = 0.76 hr into synthetic JWST data for β Pic b, with amplitudes, random noise, and systematic noise levels indicated. Left columns: injected signals (orange solid lines) and simulated measurements (blue dots). Right columns: Lomb–Scargle periodograms with 3σ (dashed lines) and 5σ (solid lines) FAP upper limits indicated.