adsabs/AstroCLIMB huggingface dataset:
Paper: Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Romeel Davé, Shy Genel
Figure caption: The z = 0.1 mass-weighted mean temperature projections for the SIMBA feedback variations and the CAMELS TNG runs. Each projection is over a depth of 525 kpc h−1 (corresponding to the absorber length discussed in Section 2.4). The top rows display the fiducial runs, and the bottom rows display the runs without the AGN jet and kinetic feedback modes for SIMBA (left) and TNG (right). The SIMBA projection is a 25 by 25 Mpc h−1 portion of the full (50 by 50 Mpc h−1) box while the CAMELS TNG projection is the full 25 by 25 Mpc h−1 box.
Paper: Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Romeel Davé, Shy Genel
Figure caption: The z = 0.1 CDDs for the SIMBA runs (black lines) and the IllustrisTNG runs (red lines), compared to the D16 observational data (blue points). The solid lines are the fiducial runs while the dashed lines are the no-jet and no-kinetic runs. The observational data is from Table 6 of D16.
Paper: Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Romeel Davé, Shy Genel
Figure caption: The SIMBA z = 0.1 CDDs corresponding to the raw simulation results (black lines) and when correcting the UVB post-processing to find the best fit (green lines). Results are shown for both the fiducial (solid lines) and no-jet runs (dashed lines). The ﹩{\chi }_{R}^{2}﹩ values and the UVB correction factors (relative to the Haardt & Madau 2012 UVB) for the fits are in the legends.
Paper: Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Romeel Davé, Shy Genel
Figure caption: The same as Figure 1 but, instead of a temperature projection, a Lyα column density projection over a single 525 kpc h−1 slice is shown. These projections show how rare column densities of N H I ≳ 1015 cm−2 are.
Paper: No Need for Extreme Stellar Masses at z ∼ 7: A Test-case Study of COS-87259
Authors: Sophie E. van Mierlo, Karina I. Caputi, Vasily Kokorev
Figure caption: Best-fit SEDs corresponding to the five SED fitting setups presented in Table 2. In each panel, the SED is shown in a black line. The observed fluxes and flux upper limits are shown in dark and light blue diamonds, respectively. The template fluxes in each band are shown in red points. Each panel reports the SED fitting setup, the spectroscopic redshift from Endsley et al. (2022b), the reduced χ 2 value of the fit, and the stellar mass. For the LEPHARE run using STARBURST99 models, shown in the lower left panel, the yellow dotted line represents the contribution of nebular emission to the total SED.
Paper: No Need for Extreme Stellar Masses at z ∼ 7: A Test-case Study of COS-87259
Authors: Sophie E. van Mierlo, Karina I. Caputi, Vasily Kokorev
Figure caption: Best-fit SED of COS-87259 obtained with STARDUST on the observed UV to millimeter photometry from Endsley et al. (2022a) and Endsley et al. (2022b). The flux measurements are shown in red, where the arrows correspond to flux upper limits. The individual components of the stellar, AGN, and dust emission are shown in blue, green, and red curves respectively.
Paper: The Influence of Tidal Heating on the Habitability of Planets Orbiting White Dwarfs
Authors: Juliette Becker, Darryl Z. Seligman, Fred C. Adams, Marshall J. Styczinski
Figure caption: For the two objects under consideration (Earth and TRAPPIST-1 e), we show the section of parameter space where the habitable time during the white dwarf phase due to tidal heating is greater than 3, 6, and 9 Gyr. For comparison, the Earth has a habitable lifetime of 6.3–7.8 Gyr around the main-sequence Sun (Rushby et al. 2013). Planets with physical parameters outside the range considered in this work will occupy slightly different locations in parameter space.
Paper: The Influence of Tidal Heating on the Habitability of Planets Orbiting White Dwarfs
Authors: Juliette Becker, Darryl Z. Seligman, Fred C. Adams, Marshall J. Styczinski
Figure caption: (Top panel) The computed amount of time that a planet like TRAPPIST-1 e (with physical parameters given in Table 1) around a white dwarf maintains habitable surface temperatures when both tidal heating and radiative heating are considered. (Bottom panel) The difference between the time that the same planet remains in the habitable zone while including tidal heating as compared to when ignoring tidal heating. Both quantities are shown for a range of initial semimajor axis and eccentricity values for the orbiting planet. In both plots, the solid black line denotes the threshold eccentricity above which planets will be tidally disrupted; the parameter space where planets may be habitable is safely below this limit. The habitable lifetime of a planet increases when including tidal heating for all but a very narrow range of parameter space.
Paper: First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70
Authors: Teppei Okumura, Atsushi Taruya
Figure caption: Monopole and quadrupole correlation functions of SDSS galaxies in redshift space, ﹩{\xi }_{{gg},{\ell }}^{s}﹩, ﹩{\xi }_{g+,{\ell }}^{s}﹩, ﹩{\xi }_{+,{\ell }}^{s}﹩, and ﹩{\xi }_{-,{\ell }}^{s}﹩ from top to bottom panels. The results for LRG, LOWZ, and CMASS samples are shown from the left to right panels, respectively. The error bars are estimated from jackknife resampling. The solid curves are the best-fit nonlinear alignment and RSD models jointly fitted for these four statistics, where the data points enclosed by the vertical lines are used. The dotted curves are the linear predictions as references.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: Top panel: radial profile of self-similar acceleration close to the jet axis at θ = 0.°0446 is shown in self-similar coordinates v  r /v 0 vs. r/v 0 t for the cases of M A = 1.2, 1.5, 2, 3, 6, 18, and 30 winds (distinguished by line styles) with n = 1, 2, 4, and 6 toroids (distinguished by color hues). The inset shows the plot of v  f /v 0 as a function of M A (Equation (21)). The v  f /v 0 values corresponding to the illustrated M A values are shown as red dots in the inset. Lower panel: radial velocity v  r /v 0 vs. r/v 0 t profiles for different θ are shown for the cases with n = 1, 2, 4, and 6 toroids. Data are shown together, for each n, for these θ: 0.°13, 0.°4, 1°, 4°, and 8°, with line styles showing M A = 1.2, 1.5, 2, 3, 6, 18, and 30 winds, identical to the top panel.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: The 2D spatial profiles of ﹩{\mathrm{log}}_{10}\left(-{ \mathcal C }/{b}_{0}\right)﹩ for winds of M A = 1.2, 1.5, 2, 3, 6, 18, 30 with n = 1, 2, 4, and 6 toroids and ambient poloidal field strengths of α  b  = 1 (left) and α  b  = 0 (right), in which ﹩{b}_{0}\equiv {v}_{0}\sqrt{{D}_{0}}/{M}_{{\rm{A}}}﹩. The black contours are loci of v  r /v 0 = 1, and the gray contours are loci of ﹩-{ \mathcal C }/{b}_{0}=1﹩. The spatial axes are labeled in units of v 0 t. The horizontal ϖ axes have been exaggerated by factors of 3.5, 2.3, 1.4, and 1.0 for n = 1, 2, 4, and 6, respectively.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: The 2D spatial profiles of ﹩{\mathrm{log}}_{10}\left(h/{h}_{0}\right)﹩, a specific magnetic enthalpy within the acceleration region, for winds of M A = 1.2, 1.5, 2, 3, 6, 18, and 30 with n = 1, 2, 4, and 6 toroids and ambient poloidal field strengths of α  b  = 1 (left) and α  b  = 0 (right), in which ﹩{h}_{0}\equiv {v}_{0}^{2}/{M}_{{\rm{A}}}^{2}﹩. The black contours are loci of v  r /v 0 = 1, and the brown contours are loci of h/h 0 = 1. The spatial axes are labeled in units of v 0 t, with horizontal ϖ axes exaggerated by factors as in Figure 3.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: Top: variation along θ = 0.°0446 of ﹩\tilde{b}/{b}_{0}=-{ \mathcal C }/{b}_{0}﹩ against v  r /v 0. Bottom: ﹩\tilde{b}/{b}_{0}﹩ vs. v  r /v 0 for θ of 0.°13, 0.°4, 1°, 4°, and 8°. The same line styles and colors as in Figure 2 are used.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: Schematic plots of the outflow lobes with magnetic acceleration for a case with a strong ambient magnetic field (left) and without an ambient magnetic field (right).
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption:                         (a) PV diagrams of column density (rescaled for ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ contrast) produced by winds with M                      A = 1.2, 1.5, 2, 3, 6, 18, and 30 (left to right) for the strongly magnetized α                                               b                       = 1 (top) and nonmagnetized α                                               b                       = 0 (bottom) toroids of n = 1, 2, 4, and 6 (top to bottom) at an inclination angle of 45°. The column density is integrated for material with v                                               p                       > a                      ambient. The spatial position is convolved with a Gaussian profile of 0.01v                      0                      t for smoother appearance as in Paper II. (b) PV diagrams of column density (rescaled for ﹩\mathrm{log}{N}_{{\rm{H}}}﹩ contrast) as in Figure 6(a), while the matter is integrated for wind mass fraction 0 < f < 1.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: The 2D spatial profiles of the quantity ﹩{\mathrm{log}}_{10}\left(\mu /{\mu }_{0}\right)﹩ for winds of M A = 1.2, 1.5, 2, 3, 6, 18, and 30 with n = 1, 2, 4, and 6 toroids and ambient poloidal field strengths of α  b  = 1 (left) and α  b  = 0 (right), in which ﹩{\mu }_{0}\equiv {v}_{0}/{M}_{{\rm{A}}}\sqrt{{D}_{0}}﹩. The black contours are loci of v  r /v 0 = 1, and the brown contours are loci of ﹩-{ \mathcal C }/{b}_{0}=1﹩. The spatial axes are labeled in units of v 0 t. The horizontal ϖ axes have been exaggerated by factors of 3.5, 2.3, 1.4, and 1.0 for n = 1, 2, 4, and 6, respectively.
Paper: A Unified Model for Bipolar Outflows from Young Stars: Apparent Magnetic Jet Acceleration
Authors: Hsien Shang, 賢 尚, Ruben Krasnopolsky, Chun-Fan Liu, 君帆 劉
Figure caption: The 2D spatial profiles of number density (n H, the left halves) and column density (N H, the right halves) for winds of M A = 1.2, 1.5, 2, 3, 6, 18, and 30; toroids of n = 1, 2, 4, and 6; and ambient poloidal field strengths of α  b  = 1 (left) and α  b  = 0 (right). The spatial axes are labeled in units of v 0 t, with horizontal ϖ axes exaggerated by factors as in Figure 7.
Paper: Coplanar Circumbinary Planets Can Be Unstable to Large Tilt Oscillations in the Presence of an Inner Polar Planet
Authors: Anna C. Childs, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Aaron M. Geller
Figure caption: Phase diagrams for various semimajor axes of the outer planet and inclinations of the inner planet. Green and blue orbits are circulating orbits with initial inclinations less than and greater than 90°, respectively. Red and cyan orbits are librating orbits with initial inclinations less than and greater than the stationary polar inclination, respectively. The black crosses show the stationary polar inclination found with Equation (8).
Paper: Coplanar Circumbinary Planets Can Be Unstable to Large Tilt Oscillations in the Presence of an Inner Polar Planet
Authors: Anna C. Childs, Rebecca G. Martin, Stephen Lepp, Stephen H. Lubow, Aaron M. Geller
Figure caption: Numerical results for the inclination evolution of an outer planet orbiting an equal mass binary star with binary eccentricity e b = 0.8 with an inner Jupiter-mass polar planet orbiting with semimajor axis a p1 = 5 a b. The outer planet begins coplanar to the binary orbit with i p2 = 0° for different outer planet semimajor axis.
Paper: Multicomponent Activity Cycles Using Hilbert–Huang Analysis
Authors: E. N. Velloso, F. Anthony, J.-D. do Nascimento, L. F. Q. Silveira, J. Hall, S. H. Saar
Figure caption: Result of our analysis for 61 Cyg A. The colored vertical lines indicate the epochs for which its large-scale magnetic geometry was reconstructed using ZDI (Boro Saikia et al. 2016, 2018). The background colors indicate predicted polarities for a hypothesis of a complete magnetic reversal taking three times cycle 1 (shown in the Cycle 2 panel) or two times cycle 1 (as in the Sun, shown in the Cycle 1 panel).
Paper: Multicomponent Activity Cycles Using Hilbert–Huang Analysis
Authors: E. N. Velloso, F. Anthony, J.-D. do Nascimento, L. F. Q. Silveira, J. Hall, S. H. Saar
Figure caption: Result of CEEMDAN for the Sun. The sunspot number is shown in blue and the K-index is in orange. The top-left panel shows the preprocessed input data. The right-side panels show the Hilbert spectra corresponding to their respective time-domain components.
Paper: Multicomponent Activity Cycles Using Hilbert–Huang Analysis
Authors: E. N. Velloso, F. Anthony, J.-D. do Nascimento, L. F. Q. Silveira, J. Hall, S. H. Saar
Figure caption: Same as Figure 2, however for a smoothed-out version of the signal using 150 day bins during downsampling.
Paper: Efficient Long-range Active Galactic Nuclei (AGNs) Feedback Affects the Low-redshift Lyα Forest
Authors: Megan Taylor Tillman, Blakesley Burkhart, Stephanie Tonnesen, Simeon Bird, Greg L. Bryan, Daniel Anglés-Alcázar, Romeel Davé, Shy Genel
Figure caption: The z = 0.1 CDD for the original SIMBA and TNG runs vs. the small box runs studied in this work. The results are converged exhibiting that the box size and resolution of these runs are converged for the Lyα statistics presented within this study.
Paper: The Influence of Tidal Heating on the Habitability of Planets Orbiting White Dwarfs
Authors: Juliette Becker, Darryl Z. Seligman, Fred C. Adams, Marshall J. Styczinski
Figure caption: Evolution of the habitable zone (HZ) for planets around a white dwarf with contributions to total planetary heating (dashed) from tidal heating (blue) and incident stellar radiation (red). Each panel shows a different mode of evolution with a different selection of initial physical and orbital parameters. In the top panel, we show the evolution of an Earth analog with initial semimajor axis of a = 0.2 and eccentricity of e = 0.7. This planet initially resides within the tidal habitable zone. The subsequent semimajor axis evolution caused by tidal circularization does not follow the location of the habitable zone at late times. In the bottom panel, we show the evolution of a TRAPPIST-1 e-analog with initial semimajor axis of a = 0.2 and eccentricity of e = 0.8. Its semimajor axis evolution traces the location of the habitable zone for the first 10 Gyr of the white dwarf phase. The physical parameters of each planet are presented in Table 1.
Paper: The Influence of Tidal Heating on the Habitability of Planets Orbiting White Dwarfs
Authors: Juliette Becker, Darryl Z. Seligman, Fred C. Adams, Marshall J. Styczinski
Figure caption: The semimajor axis spanned by the habitable zone for two white dwarfs with masses of 1.1 M ⊙ (dashed yellow lines) and 0.54 M ⊙ (solid red lines), neglecting tidal heating within the planet. As the white dwarf luminosity decreases over time, the location of the habitable zone moves inward and shrinks. The white dwarf cooling curves used to compute the location of the habitable zone are from Salaris et al. (2022) and use the opacity models of Cassisi et al. (2007).
Paper: The Influence of Tidal Heating on the Habitability of Planets Orbiting White Dwarfs
Authors: Juliette Becker, Darryl Z. Seligman, Fred C. Adams, Marshall J. Styczinski
Figure caption: The total power received via tidal heating as a function of the orbital semimajor axis and eccentricity for a planet with an Earth-like composition and tidal parameters. This power is computed using Equation (4). Contours for the orbital locations where the planet receives Io- and Earth-like levels of tidal heating are marked.
Paper: First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70
Authors: Teppei Okumura, Atsushi Taruya
Figure caption: Constraints on model parameters as a function of the minimum separation, ﹩{r}_{\min }﹩, obtained from clustering-only analysis and combined analysis of clustering and IA for LRG (left), LOWZ (middle), and CMASS (right) samples. We show the results for f σ 8, b σ 8, b  K  σ 8, and σ  v  from the top to bottom rows. Theoretical prediction with 68% C. L. based on the Planck experiment is shown as the yellow regions in the top row.
Paper: First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70
Authors: Teppei Okumura, Atsushi Taruya
Figure caption: Constraints on (f σ 8, b σ 8, b  K  σ 8, σ  v ) obtained from clustering-only analysis and combined analysis of clustering and IA, determined by the correlation functions of LRG sample at 10 ≤ r ≤ 100 h −1 Mpc. The contours show the 68%, 95%, and 99% C. L. from inward.
Paper: First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70
Authors: Teppei Okumura, Atsushi Taruya
Figure caption: Same as Figure 2, but for LOWZ (top) and CMASS (bottom) samples. For these samples, the II correlations only at 10 ≤ r ≤ 25 h −1 Mpc are used, and the GG and GI correlations at 10 ≤ r ≤ 100 h −1 Mpc are used.
Paper: First Constraints on Growth Rate from Redshift-space Ellipticity Correlations of SDSS Galaxies at 0.16 < z < 0.70
Authors: Teppei Okumura, Atsushi Taruya
Figure caption: Upper panel: constraints on growth rate f(z)σ 8(z) from three SDSS galaxy samples compared to the best-fitting ΛCDM model from the Planck experiment. We adopt ﹩{r}_{\min }=10\,{h}^{-1}\,\mathrm{Mpc}﹩. Lower panel: 1σ error of the growth rate constraints, Δ(f σ 8)/f σ 8.
Paper: Discovery of the Exceptionally Short Period Ultracool Dwarf Binary LP 413-53AB
Authors: Chih-Chun Hsu, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Radial velocity measurements for primary (circles) and secondary (triangles) components for individual UT epochs 2007 October 26, 2007 October 27, and 2022 March 13 (top row); 2022 July 10, 2022 October 16, and 2022 December 2 (middle row); and 2023 January 8 (bottom left), and the phase-folded RV curve (bottom right). Measurement uncertainties are smaller than the symbol size. In each panel, the best-fit orbit indicating primary (blue lines) and secondary (orange lines) RVs are indicated, as well as the center-of-mass (systematic) RV (gray dashed lines). The measurements from J-band data on 2007 October 26 and 2007 October 27 shown here have been corrected for the RV offset term σ  J . Four epochs in 2022 December 2 and three epochs in 2023 January 8 were excluded from the orbit fit due to their unresolved spectra (open circles); these are nevertheless included in the phase-folded RV curve (see Section 4).
Paper: Discovery of the Exceptionally Short Period Ultracool Dwarf Binary LP 413-53AB
Authors: Chih-Chun Hsu, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Forward-model fit to the 2.29–2.33 μm (order 33) Keck/NIRSPEC spectrum of LP 413-53 obtained on 2022 March 13 at 05:02:59.43 UT (59,651.20898 MJD; black line). The forward model consists of primary (orange) and secondary (magenta) spectra, with the combined spectrum (blue) modulated by telluric absorption (red). The residual (data − model) and uncertainty are depicted by the black line and gray-shaded region along the bottom, respectively. The legend provides the final fit parameters for component temperatures (T eff in K), log surface gravities (﹩\mathrm{log}g﹩ in log cm s−2), rotational velocities (﹩v\sin i﹩ in km s−1), and radial velocities (RV in km s−1) with their uncertainties, as well as the best-fit χ 2 and degrees of freedom (DOF).
Paper: Discovery of the Exceptionally Short Period Ultracool Dwarf Binary LP 413-53AB
Authors: Chih-Chun Hsu, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Sequence of LP 413-53 spectra over a 2 hr period on 2022 December 2 (UT), centered on the 2.312–2.316 μm region. Time increases from top to bottom, and UT times (hour and minute) are indicated next to each spectrum. The topmost spectrum shows equivalent data for the M9 dwarf LP 666-9 (C. Hsu et al. 2023, in preparation). Absorption features arising from CO are initially consistent with a single-line source, but become clearly doubled over the observing sequence, with the line centers of the stronger features drifting to the right and the line centers of the weaker features drifting to the left. Vertical lines mark line center positions at the start (solid) and end (dashed) of the sequence for the stronger (magenta) and weaker (blue) lines.
Paper: Multipoint Turbulence Analysis with HelioSwarm
Authors: Francesco Pecora, Sergio Servidio, Leonardo Primavera, Antonella Greco, Yan Yang, William H. Matthaeus
Figure caption: Estimations of cascade rate, for isotropic (a) and anisotropic (b) simulations. Insets show ϵ(ℓ, θ, ϕ) computed from Yaglom’s law, Equation (2), over all grid points, plotted as a function of lag. The maximum value within the inertial range is highlighted with a dashed horizontal line and reported as ﹩{\epsilon }_{{sim}}﹩ in the legend. Histograms are obtained from computing the divergence using tetrahedra in lag space (see text and Figure 4). We discarded values larger than +1 and smaller than −1.
Paper: A Dwarf Galaxy Debris Stream Associated with Palomar 1 and the Anticenter Stream
Authors: Yong Yang, Jing-Kun Zhao, Xian-Hao Ye, Gang Zhao, Ke-Feng Tan
Figure caption: The left and right panels present the dust extinction map extracted from Schlegel et al. (1998) and Gaia's scanning pattern covered by the DR3, respectively. The middle panel presents the weighted sky map for stars fainter than G = 18 mag. The green areas are two moving masks used to generate the stream’s lateral and longitudinal profiles in Figure 2. The red dashed line of the three panels indicates the trajectory of the stream.
Paper: A Dwarf Galaxy Debris Stream Associated with Palomar 1 and the Anticenter Stream
Authors: Yong Yang, Jing-Kun Zhao, Xian-Hao Ye, Gang Zhao, Ke-Feng Tan
Figure caption: Left: the lateral distributions for weighted (red solid line) and unweighted (blue dashed line) numbers of stars fainter than G = 18 mag, obtained by moving the left mask in Figure 1 across the stream. Right: similar to the left panel but for the longitudinal profile obtained by moving the bottom mask along the stream.