adsabs/AstroCLIMB huggingface dataset:
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: The impact of adding the remaining JWST medium bands (F140M, F210M, F250M, F300M, F335M, and F480M) to the existing set of PRIMER filters on the inferred stellar masses at each redshift (different panels). Stellar masses derived from SED fits including all broad and medium bands are shown in black in each panel, and the original fits (using just the PRIMER filter coverage) are shown in color. All fits use the double power-law SFH parameterization. Particular improvement is seen for low-mass galaxies at z = 5 (where the addition of the F250M, F335M, and F480M data enable continuum constraints) and at z = 7 and z = 8 (where the F480M measurement provides an important constraint against a rising continuum).
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: (a) The first of four o-band ATLAS-Sutherland telescope discovery images of 2024 PT5 from 2024 August 7 21:11:57 UTC. The asteroid moved at a rate of 34﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩3 hr−1 (13﹩\mathop{.}\limits^{\unicode{x000b0}}﹩7 day−1) in the northwest direction. The asteroid makes a ~9 pixel trail in the 30 s ATLAS exposures, indicated by the red circle. (b) Same as panel (a) but shows the image after subtracting static sources. Despite the presence of nearby stars, the asteroid is detected cleanly in the subtracted images. (c) Same as panel (a), but the second of four o-band images containing 2024 PT5 taken on 2024 August 7 21:16:35 UTC. (d) Same as panel (c) but shows the image after subtracting static sources. The asteroid was detected with an apparent magnitude of o= 17.13 in panel (b) and o = 16.99 in panel (c). The large black areas in the subtracted images are regions of saturated pixels from bright stars. The direction of the asteroid and cardinal directions are indicated in each figure.
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: Reflectance photometric spectrum of 2024 PT5 consisting of g, r, i, and Z observations of 2024 PT5 on 2024 September 27 UTC. The λeff locations of the g, r, i, and Z filters have been plotted as vertical dashed lines. The data points for the normalized reflectivity of 2024 PT5 have been offset slightly from their location in the wavelength direction. The error bars on the spectrum data points correspond to 1σ uncertainty. The spectrum has been normalized to unity at 550 nm, as indicated by the red cross. The spectral range of S-, V- and C-type asteroids from the Bus–DeMeo asteroid taxonomic catalog (F. E. DeMeo et al. 2009) are overplotted with the V-type spectrum most closely resembling the spectra of 2024 PT5. The average spectrum of Apollo program coarse bulk lunar rock samples is plotted for reference (P. J. Isaacson et al. 2011).
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: Top panel: side view of the Earth corotating frame orbital trajectory of 2024 PT5 as it enters and leaves the Earth–Moon system between 2024 June and 2025 April in Cartesian Earth–Moon barycentric x- and z-coordinates. The daily position of 2024 PT5 is represented as blue points except the portion of its trajectory when it had eg < 1 plotted in red. The position of the Earth is plotted with a cyan circle. The circular green-shaded region indicates the Hill sphere of Earth. The position of 2024 PT5, when it was discovered, is marked by a green circle, and the position of 2024 PT5 when Gemini observed it is marked with a green X. A blue arrow indicates the direction of motion of 2024 PT5 along its orbital path. Bottom panel: the same as the top panel, except in Cartesian Earth–Moon barycentric x- and y-coordinates.
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: a* vs. i − z(Z) colors of 2024 PT5 plotted with a* vs. i − z colors of C-, S-, and V-type asteroids from Ž. Ivezić et al. (2001) and M. Jurić et al. (2002); active comets (M. Solontoi et al. 2012); Kuiper Belt objects (E. O. Ofek 2012); and bulk lunar rock samples (P. J. Isaacson et al. 2011). The colorization scheme of data points as a function of a* and i − z is adapted from Ž. Ivezić et al. (2002), where blue symbol colors correspond to C-type asteroids, red symbol colors correspond to S-type asteroids, and green symbol colors correspond to V-type asteroids. We note that in this case, the measured Z magnitude of 2024 PT5 is plotted as a substitute for its z magnitude, i − z. The a* and i − z range of average S-, V-, and C-type asteroids are shown computed from the average spectra from F. E. DeMeo et al. (2009).
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: Top left panel: a median combination stack of 11 × 75 s g-filter images of 2024 PT5. An arrow indicating the width of 10″ is shown for scale, and the cardinal directions are indicated. Top right panel: a median combination stack of 5 × 50 s r-filter images of 2024 PT5. Bottom left panel: a median combination stack of 2 × 60 s i-filter images of 2024 PT5. Bottom right panel: a median combination stack of 2 × 60 s Z-filter images of 2024 PT5. The image scale and cardinal directions in the r, i, and Z stacks are the same as in the g-image stack.
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: Top panel: Lomb–Scargle periodogram of lightcurve period vs. spectral power (N. R. Lomb 1976) for the g-filter data from the 2024 September 27 UTC Gemini N/GMOS observations. A peak in the power is located at single-peaked lightcurve period of 1320 s. Bottom panel: phase-dispersion minimization analysis of lightcurve rotation period vs. Θ metric (R. F. Stellingwerf 1978). The Θ metric is minimized at single-peaked rotation periods of 1150 s similar to the 1320 ± 227 s period found with the Lomb–Scargle periodogram.
Paper: The Discovery and Characterization of Minimoon 2024 PT5
Authors: Bryce T. Bolin, Larry Denneau, Laura-May Abron, Robert Jedicke, Kristin Chiboucas, Carl Ingebretsen, Brian C. Lemaux
Figure caption: Top panel: g-filter lightcurve from 2024 September 27 GMOS observations of 2024 PT5. The error bars on the data points are equal to their 1σ photometric uncertainties. A model lightcurve is plotted in black with a double-peaked period of  ~2600 s and amplitude of 0.28 mag. Bottom panel: phased g-filter lightcurve data of 2024 PT5 using a lightcurve period of  ~1300 s and amplitude of 0.28 mag.
Paper: Alpha–Proton Relative Drift: Implications for the Origins and Dynamics of the Solar Wind
Authors: Joseph H. Wang, Timothy S. Horbury, Lorenzo Matteini, Domenico Trotta
Figure caption: Radially binned means and standard errors of (a) the rms velocity fluctuation amplitudes of the proton and alpha populations and (b) the ratio of alpha fluctuation amplitudes to proton amplitudes.
Paper: Alpha–Proton Relative Drift: Implications for the Origins and Dynamics of the Solar Wind
Authors: Joseph H. Wang, Timothy S. Horbury, Lorenzo Matteini, Domenico Trotta
Figure caption: Velocity variations for multiple species due to an Alfvén wave. Vectors for background (subscript 0) and wave magnetic field and velocity directions have been drawn, with circles representing the spherically polarized velocity fluctuations and magnetic field.
Paper: Alpha–Proton Relative Drift: Implications for the Origins and Dynamics of the Solar Wind
Authors: Joseph H. Wang, Timothy S. Horbury, Lorenzo Matteini, Domenico Trotta
Figure caption: 1D histograms comparing alpha drift and Alfvén speed, colors normalized in vertical columns.
Paper: Relativistic Electron Acceleration and the “Ankle” Spectral Feature in Earth’s Magnetotail Reconnection
Authors: Weijie Sun, Mitsuo Oka, Marit Øieroset, Drew L. Turner, Tai Phan, Ian J. Cohen, Xiaocan Li, Jia Huang, Andy W. Smith, James A. Slavin, Gangkai Poh, Kevin J. Genestreti, Dan Gershman, Kyunghwan Dokgo, Guan Le, Rumi Nakamura, James L. Burch
Figure caption: Overview of a magnetic reconnection event observed by MMS1 on 2018 June 2 in Earth’s magnetotail plasma sheet. (a) Magnetic field components in the local coordinate of the cross-tail neutral sheet: BL (blue), BM (green), and BN (red). (b) Energy spectrogram for electrons with energies from ∼10 eV to 560 keV from FPI and FEEPS. (c) Ion density from HPCA and electron density from FPI. (d) Electron temperature from FPI, perpendicular (Teperp, red) and parallel (Teparp, blue) components. (e) Ion bulk velocity measured by FPI and HPCA; solid lines are from FPI with VL (blue), VM (green), and VN (red), and crosses are from HPCA. (f), (g) Energy spectra of electrons from FPI with electrons moving parallel to magnetic field subtracting those moving antiparallel and vice versa, respectively. (h) The magnetic field intensity in the lobe derived through pressure balance. (i) A schematic figure of MMS’s trajectory of the magnetic reconnection event. The green segments represent the separatrix regions, corresponding to time intervals represented by green bars between panels (e) and (f). In panels (a) to (h), the first and fourth vertical dashed lines indicate the start and the end of the reconnection event, the second vertical dashed line indicates the sharp enhancement in ion bulk velocity, and the third dashed line marks the primary X-line location.
Paper: Relativistic Electron Acceleration and the “Ankle” Spectral Feature in Earth’s Magnetotail Reconnection
Authors: Weijie Sun, Mitsuo Oka, Marit Øieroset, Drew L. Turner, Tai Phan, Ian J. Cohen, Xiaocan Li, Jia Huang, Andy W. Smith, James A. Slavin, Gangkai Poh, Kevin J. Genestreti, Dan Gershman, Kyunghwan Dokgo, Guan Le, Rumi Nakamura, James L. Burch
Figure caption: (a), (c) Kappa function modeling of electron phase-space densities obtained from 18:29:36.6 to 18:29:39.67 UTC. The blue dots with error bars represent measured phase-space densities. The red and magenta lines correspond to two Kappa modelings for electrons, respectively. The black line represents the derived Maxwellian function for the relatively low-energy Kappa function. Residuals in (b) are normalized (see Appendix B for details). The orange lines indicate the one-count-level phase-space densities for FPI and FEEPS. (d), (e) Three spectral distributions are shown. One is during pre-active phase (18:28:59.71 to 18:29:02.78 UTC, marked as triangles, and the fittings are in green), one is during the energy dispersion (18:29:36.6 to 18:29:39.67 UTC, marked as circles, and the fittings are in magenta), and one is in the separatrix layer during active phase (18:29:58.12 to 18:30:01.19 UTC, marked as crosses, and the fittings are in orange). Their locations are marked as diamonds in Figure 2(e). Relativistic effects were considered during conversion to phase-space densities (R. V. Hilmer et al. 2000).
Paper: Relativistic Electron Acceleration and the “Ankle” Spectral Feature in Earth’s Magnetotail Reconnection
Authors: Weijie Sun, Mitsuo Oka, Marit Øieroset, Drew L. Turner, Tai Phan, Ian J. Cohen, Xiaocan Li, Jia Huang, Andy W. Smith, James A. Slavin, Gangkai Poh, Kevin J. Genestreti, Dan Gershman, Kyunghwan Dokgo, Guan Le, Rumi Nakamura, James L. Burch
Figure caption: Differential particle flux variations of electrons with energies from ∼1.86 to 523.2 keV from MMS1 for the reconnection event. (a) and (b) Magnetic field and ion bulk velocity under the local coordinate of the neutral sheet. (c) Electron density. (d), (e) Electron flux intensities measured by FPI and FEEPS. The horizontal line in (e) represents the background flux of the 523.2 keV energy channel. (f), (g) Pitch-angle distribution and fluxes in parallel (0°–32°, red), perpendicular (65°–115°, blue) and antiparallel (147°–180°, green) of electrons with energies between 294 and 355 keV. (h), (i) Electrons with energies between 401 and 560 keV, in a similar format to (f) and (g).
Paper: Relativistic Electron Acceleration and the “Ankle” Spectral Feature in Earth’s Magnetotail Reconnection
Authors: Weijie Sun, Mitsuo Oka, Marit Øieroset, Drew L. Turner, Tai Phan, Ian J. Cohen, Xiaocan Li, Jia Huang, Andy W. Smith, James A. Slavin, Gangkai Poh, Kevin J. Genestreti, Dan Gershman, Kyunghwan Dokgo, Guan Le, Rumi Nakamura, James L. Burch
Figure caption: Number and energy densities of thermal, suprathermal, and relativistic “ankle” electrons between 18:28:00 and 18:34:00 UTC. (a) Magnetic field components (BL in blue, BM in green, and BN in red). (b) Spectral slope indices (﹩{\boldsymbol{\kappa }}﹩) of suprathermal (red) and the “ankle” (magenta and black) electrons. The red and magenta indices are obtained through the Kappa distributions, and the black indices are obtained from power-law distributions. (c) Densities of thermal (black) and suprathermal (red) electrons. (d) Density fractions of thermal and suprathermal electrons. (e) Density (blue) and density fraction (magenta) of the “ankle” electrons. (f)–(h) are similar to (c)–(e) but are energy densities for thermal, suprathermal, and relativistic electrons. (i) Normalized residuals from the function modelings.
Paper: Relativistic Electron Acceleration and the “Ankle” Spectral Feature in Earth’s Magnetotail Reconnection
Authors: Weijie Sun, Mitsuo Oka, Marit Øieroset, Drew L. Turner, Tai Phan, Ian J. Cohen, Xiaocan Li, Jia Huang, Andy W. Smith, James A. Slavin, Gangkai Poh, Kevin J. Genestreti, Dan Gershman, Kyunghwan Dokgo, Guan Le, Rumi Nakamura, James L. Burch
Figure caption: Overview of the enhancements of electrons with energies from ∼47.2 to 523.2 keV at ∼18:29:30 UTC when ion bulk velocity suddenly increased. (a), (b) Magnetic field and ion bulk velocity in the local coordinate. (c) Electron flux intensities measured by FEEPS. The asterisks indicate the time when electron fluxes start to sharply increase in each energy channel. (d) The fitting between ﹩t﹩ and ﹩1/{V}_{\mathrm{para}}\left(t\right)﹩. The fitting includes the asterisks during the interval that MMS moved toward the neutral sheet as indicated by the shaded region. The ﹩{V}_{\mathrm{para}}﹩ is the parallel velocity of the dispersed electrons.
Paper: Radial Evolution of MHD Turbulence Anisotropy in Low Mach Number Solar Wind
Authors: Xingyu Zhu, Gary P. Zank, Lingling Zhao, Ashok Silwal
Figure caption: Left panels: time series of the sub-Alfvénic solar wind observed by PSP. Right panels: time series of the modestly super-Alfvénic solar wind observed by Wind spacecraft. (a) and (f) Magnetic field BT and ion velocity VT in RTN coordinates. (b) and (g) Magnetic field BN and ion velocity VN in RTN coordinates. (c) and (h) Scaled proton number density nR2 and the Mach number MA measured by PSP. (d) and (i) Angle between the 30 minutes moving-averaged mean magnetic field and mean plasma velocity, θBV. The dotted horizontal lines indicates the average values in the corresponding intervals. (e) and (j) Proton plasma beta βp.
Paper: Radial Evolution of MHD Turbulence Anisotropy in Low Mach Number Solar Wind
Authors: Xingyu Zhu, Gary P. Zank, Lingling Zhao, Ashok Silwal
Figure caption: Decomposition of the observed ﹩{z}_{{\rm{obs}}}^{+}.﹩ (green) and ﹩{z}_{{\rm{obs}}}^{-}.﹩ (orange) spectra into the inferred contribution by the 2D and NI/slab components using the NI MHD theory for (a) sub-Alfvénic and (b) modestly super-Alfvénic solar wind turbulence. The blue solid line represents the inferred 2D turbulence spectrum (z∞), the red solid line denotes the inferred NI/slab turbulence spectra z*+ for z+, and the red dashed line the inferred NI/slab turbulence spectra z*− for z−. The black solid line and dashed line are theoretical z+ and z− spectra predicted by the NI MHD theory, respectively.
Paper: Radial Evolution of MHD Turbulence Anisotropy in Low Mach Number Solar Wind
Authors: Xingyu Zhu, Gary P. Zank, Lingling Zhao, Ashok Silwal
Figure caption: (a) Trace PSDs of a sub-Alfvénic flow observed by PSP. Different colors correspond to the PSD of the velocity v (blue line), the magnetic field in units of fluctuating Alfvén velocity b (red line), and the two Elsässer variables z+ (green line) and z− (orange line). The black lines indicate the power-law fits to the z+ and z− spectra. (b) Similar to panel (a) but for the Wind observations. (c) Normalized cross helicity (σc) and normalized residual energy (σr) spectra observed by PSP. (d) σc and σr spectra observed by Wind spacecraft.
Paper: Radial Evolution of MHD Turbulence Anisotropy in Low Mach Number Solar Wind
Authors: Xingyu Zhu, Gary P. Zank, Lingling Zhao, Ashok Silwal
Figure caption: (a) The spacecraft frequency spectra of the inferred contribution of 2D and NI/slab turbulence to the observed spectrum, derived from PSP observations. (b) The wavenumber spectra of the inferred 2D and NI/slab turbulence converted from the frequency spectra. (c) The power ratios of each component in the frequency domain. (d) The power ratios of each component in the wavenumber domain.
Paper: Radial Evolution of MHD Turbulence Anisotropy in Low Mach Number Solar Wind
Authors: Xingyu Zhu, Gary P. Zank, Lingling Zhao, Ashok Silwal
Figure caption: (a) The spacecraft frequency spectra of the inferred contribution of 2D and NI/slab turbulence to the observed spectrum, derived from Wind observations. (b) The wavenumber spectra of the inferred 2D and NI/slab turbulence converted from the frequency spectra. (c) The power ratios of each inferred component in the frequency domain. (d) The power ratios of each component in the wavenumber domain.
Paper: Ultradiffuse Dwarf Galaxies Hosting Pseudobulges
Authors: Yu Rong, Hong-Xin Zhang, Cheng Cheng, Qi Guo, Weiyu Ding, Zichen Hua, Huiyuan Wang, Xu Kong
Figure caption: (a) Stellar mass–size relationship for galaxies and GCs, including UDGs. (b) Color–stellar mass diagram for DESI galaxies with radial velocities v < 18,000 km s−1, based on data from Z. L. Wen & J. L. Han (2024). (c) Comparison of effective radius Rh,d vs. r-band mean surface brightness 〈μ〉h,d for the outer disk components of the five chosen UDGs (red), the LSB hosts of typical BCDs from H. T. Meyer et al. (2014; blue), the stellar disks of typical UDGs from H.-J. Hu et al. (2023; black), and the stellar disks of typical LSB galaxies from Z. Hua et al. (2024; light green). (d) Comparison of baryonic bTFR for the five chosen UDGs hosting pseudobulges (red), typical UDGs (H.-J. Hu et al. 2023; orange), as well as typical LSB galaxies (Z. Hua et al. 2024; light green). The black dashed line depicts the best-fit bTFR for typical galaxies by F. Lelli et al. (2016). In these panels, the central bulge and outer disk components of the five selected UDGs are represented by red stars and triangles, respectively. The stellar masses of the bulge and disk components of the chosen UDGs are derived from mass-to-light ratios of E. F. Bell et al. (2003), with ﹩\mathrm{log}{({M}_{\star }/{L}_{\star })}_{g}=1.519\times (g-r)-0.499-0.093﹩, adjusting the masses by 0.093 dex to transition from a “diet” Salpeter to Chabrier initial mass function (A. Gallazzi et al. 2008).
Paper: The NANOGrav 15 yr Data Set: Running of the Spectral Index
Authors: Gabriella Agazie, Akash Anumarlapudi, Anne M. Archibald, Zaven Arzoumanian, Jeremy G. Baier, Paul T. Baker, Bence Bécsy, Laura Blecha, Adam Brazier, Paul R. Brook, Sarah Burke-Spolaor, J. Andrew Casey-Clyde, Maria Charisi, Shami Chatterjee, Tyler Cohen, James M. Cordes, Neil J. Cornish, Fronefield Crawford, H. Thankful Cromartie, Kathryn Crowter, Megan E. DeCesar, Paul B. Demorest, Heling Deng, Lankeswar Dey, Timothy Dolch, David Esmyol, Elizabeth C. Ferrara, William Fiore, Emmanuel Fonseca, Gabriel E. Freedman, Emiko C. Gardiner, Nate Garver-Daniels, Peter A. Gentile, Kyle A. Gersbach, Joseph Glaser, Deborah C. Good, Kayhan Gültekin, Jeffrey S. Hazboun, Ross J. Jennings, Aaron D. Johnson, Megan L. Jones, David L. Kaplan, Luke Zoltan Kelley, Matthew Kerr, Joey S. Key, Nima Laal, Michael T. Lam, William G. Lamb, Bjorn Larsen, T. Joseph W. Lazio, Natalia Lewandowska, Rafael R. Lino dos Santos, Tingting Liu, Duncan R. Lorimer, Jing Luo, Ryan S. Lynch, Chung-Pei Ma, Dustin R. Madison, Alexander McEwen, James W. McKee, Maura A. McLaughlin, Natasha McMann, Bradley W. Meyers, Patrick M. Meyers, Chiara M. F. Mingarelli, Andrea Mitridate, Cherry Ng, David J. Nice, Stella Koch Ocker, Ken D. Olum, Timothy T. Pennucci, Benetge B. P. Perera, Nihan S. Pol, Henri A. Radovan, Scott M. Ransom, Paul S. Ray, Joseph D. Romano, Jessie C. Runnoe, Alexander Saffer, Shashwat C. Sardesai, Ann Schmiedekamp, Carl Schmiedekamp, Kai Schmitz, Tobias Schröder, Brent J. Shapiro-Albert, Xavier Siemens, Joseph Simon, Magdalena S. Siwek, Sophia V. Sosa Fiscella, Ingrid H. Stairs, Daniel R. Stinebring, Kevin Stovall, Abhimanyu Susobhanan, Joseph K. Swiggum, Stephen R. Taylor, Jacob E. Turner, Caner Unal, Michele Vallisneri, Rutger van Haasteren, Sarah J. Vigeland, Richard von Eckardstein, Haley M. Wahl, Caitlin A. Witt, David Wright, Olivia Young
Figure caption: Bounds on the RPL parameters β and γ in scenarios where the NANOGrav signal is identified with an RPL-like signal of inflationary origin. The bounds labeled CMB, ΔNeff, and LVK are derived from the upper limits on the (i) tensor-to-scalar ratio, (ii) amount of dark radiation, and (iii) GWB amplitude at LVK frequencies, respectively. Parameter values below any of the three solid lines are excluded.
Paper: Ultradiffuse Dwarf Galaxies Hosting Pseudobulges
Authors: Yu Rong, Hong-Xin Zhang, Cheng Cheng, Qi Guo, Weiyu Ding, Zichen Hua, Huiyuan Wang, Xu Kong
Figure caption: H I spectra of the five UDGs with bulges from ALFALFA are presented. Each panel displays the positions used for calculating W50 for the respective galaxy. The inset in each panel compares the rotation velocity (with the gray region indicating the 1σ uncertainty range, estimated from the errors of W50 and inclination) of the galaxy with the rotation velocity distribution (shown as a black histogram) of all H I-bearing dwarf galaxies with ﹩8\lt \mathrm{log}{M}_{{\rm{st}}}/{M}_{\odot }\lt 9﹩ in ALFALFA.
Paper: Ultradiffuse Dwarf Galaxies Hosting Pseudobulges
Authors: Yu Rong, Hong-Xin Zhang, Cheng Cheng, Qi Guo, Weiyu Ding, Zichen Hua, Huiyuan Wang, Xu Kong
Figure caption: The left four columns of panels depict images of the five chosen UDGs with bulges. The panels, from left to right, display the colored DECaLS images, g-band images, double-Sérsic profile fitting outcomes, and residuals. The right three columns of panels showcase DESI images of 15 BCD examples from H. T. Meyer et al. (2014) for comparison.
Paper: The Galactic Disk North–South Asymmetry in Metallicity May Be a New Tracer for the Disk Warp
Authors: Weixiang Sun, Han Shen, Biwei Jiang, Xiaowei Liu
Figure caption: Left panel: spatial distribution of the LAMOST RC sample stars, in the R–Z plane, color-coded by stellar number densities. There are no less than two stars in a bin, with both axes spaced by 0.1 kpc. Right panel: spatial distribution of the LAMOST RC sample stars, in the X–Y plane, overplotted by the ϕ angle line. There is a minimum of five stars per bin, with both axes spaced by 0.25 kpc. The RC sample stars are distributed between 4.0 ≤ R ≤ 15.0 kpc and ∣Z∣ ≤ 3.0 kpc and cover a range from ϕ = −20° to ϕ = 40°.