adsabs/AstroCLIMB huggingface dataset:
Paper: “CY1” Chondrites Produced by Impact Dehydration of the CI Chondrite Parent Body
Authors: Ke Zhu, 柯 朱, Nao Nakanishi, Jan Render, Quinn R. Shollenberger, Tetsuya Yokoyama, Akira Ishikawa, Lu Chen
Figure caption: (a) Mass-independent Cr, Fe, and Ti isotope data comparison between CY chondrites, Ryugu, CI chondrites, and CM chondrites. Literature data sources: Cr (A. Trinquier et al. 2007; L. Qin et al. 2010; E. M. M. E. Van Kooten et al. 2016; K. Zhu et al. 2021b; T. Yokoyama et al. 2023b, 2023c), Fe (M. Schiller et al. 2020; T. Hopp et al. 2022) ,and Ti (A. Trinquier et al. 2009; J. Zhang et al. 2012; T. Yokoyama et al. 2023c). For the μ54Cr data of Ryugu, we only included the data with sample masses more than 10 mg to avoid sample heterogeneities associated with small sample sizes (T. Yokoyama et al. 2023c; R. Tanaka et al. 2024). Also note that before T. Yokoyama et al. (2023c), other studies did not find the low μ54Cr values for CI chondrites, which are down to ∼80 ppm. (b) Mass-independent Cr and Ti data comparison for the same CY chondrites reported in D. L. Schrader et al. (2025) and here. Big blue and yellow circles indicate data from this study, while the small gray squares are data from D. L. Schrader et al. (2025). Cr isotope data between the two studies are consistent, but the data in this study are of higher (2–4 times) precision. Note that the two distinct μ53Cr values of Y 980115 in this study are due to their different 55Mn/52Cr ratios (1.43 and 0.85, respectively). As for the μ50Ti values, we find that the CY1 samples investigated in this study are more homogeneous, whereas the μ50Ti values of CY2 samples are more heterogeneous than those in D. L. Schrader et al. (2025).
Paper: “CY1” Chondrites Produced by Impact Dehydration of the CI Chondrite Parent Body
Authors: Ke Zhu, 柯 朱, Nao Nakanishi, Jan Render, Quinn R. Shollenberger, Tetsuya Yokoyama, Akira Ishikawa, Lu Chen
Figure caption: Comparison of mass-independent Fe, Ti, and Cr isotope data of CY chondrites and other groups of CCs with literature data (A. Trinquier et al. 2007, 2009; L. Qin et al. 2010; J. Zhang et al. 2012; M. Schiller et al. 2020; K. Metzler et al. 2021; K. Zhu et al. 2021b; T. Hopp et al. 2022; M. Rüfenacht et al. 2023; T. Yokoyama et al. 2023b, 2023c). For μ54Cr data, we did not include two anomalously low values in T. Yokoyama et al. (2023c). The areas of ellipses represent the 2SD variation of the average isotope values of each group. Abbreviations: TA—Tarda; TL—Tagish Lake.
Paper: “CY1” Chondrites Produced by Impact Dehydration of the CI Chondrite Parent Body
Authors: Ke Zhu, 柯 朱, Nao Nakanishi, Jan Render, Quinn R. Shollenberger, Tetsuya Yokoyama, Akira Ishikawa, Lu Chen
Figure caption: Schematic diagram illustrating the impact (a) and disruption (b) events on the CI chondrite parent body. In panel (a), this impact results in metamorphism that transforms a part of the CI lithology into a lithology that resembles “CY1” chondrites, now with the recommended name of “CI1T.” Note that Ryugu has highly similar Fe, Cr, and Ti isotope compositions as CI1 and CI1T chondrites. The red region on the CI parent body represents the area directly impacted, while the pink region indicates the surrounding area affected by heat conduction from the impact. This pink region underwent metamorphism and dehydration, leading to the formation of a CI1T lithology. The resulting heat caused the evaporation of water and volatile elements, including Au, In, Bi, Tl, and Cd. In panel (b), we show that the CI parent body could be disrupted, especially considering its small size and fragility. Also, based on similar CREAs of CI and CI1T meteorites, it can be predicted that this parent-body impact and disruption can eject both CI and CI1T1 samples, and they finally fell to Earth.
Paper: “CY1” Chondrites Produced by Impact Dehydration of the CI Chondrite Parent Body
Authors: Ke Zhu, 柯 朱, Nao Nakanishi, Jan Render, Quinn R. Shollenberger, Tetsuya Yokoyama, Akira Ishikawa, Lu Chen
Figure caption: (a) Measured abundances of major and trace elements in CY chondrites normalized to CI chondrite values (K. Lodders 2021) and plotted on a logarithmic scale and as a function of 50% condensation temperature (B. J. Wood et al. 2019). Circles with cool colors represent four CY1 chondrites, while triangles with warm colors indicate the three CY2 chondrites. (b) Measured abundances of HSEs in CY chondrites (we plot the average data of each sample of repeated measurements) normalized to CI chondrite values and plotted on a logarithmic scale and as a function of 50% condensation temperature (B. J. Wood et al. 2019). Ryugu and Bennu data are from T. Yokoyama et al. (2023b) and D. S. Lauretta et al. (2024), respectively, and the CM data are from the literature (M. Fischer-Gödde et al. 2010; K. Lodders 2021).
Paper: “CY1” Chondrites Produced by Impact Dehydration of the CI Chondrite Parent Body
Authors: Ke Zhu, 柯 朱, Nao Nakanishi, Jan Render, Quinn R. Shollenberger, Tetsuya Yokoyama, Akira Ishikawa, Lu Chen
Figure caption: Re–Os data for CY chondrites. The Re–Os isochron for the IIIA iron meteorite is from M. I. Smoliar et al. (1996). The gray dashed line means the Os composition of CI chondrites (R. J. Walker et al. 2002).
Paper: Characterizing the Impact of Alfvén Wave Forcing in Interplanetary Space on the Distribution of Near-Earth Solar Wind Speeds
Authors: B. L. Alterman
Figure caption: Probability density function (PDF) of the solar wind speed during the declining phase of solar activity. The turquoise regions are the slow and fast wind peaks, labeled vslow and vfast. The pink regions indicate vσ and vi. vσ is the range of speeds over which ﹩{{\rm{\nabla }}}_{{v}_{{\rm{sw}}}}{A}_{{\rm{He}}}﹩ decreases as the Alfvénicity increases. vi is the range of speeds over which Gaussians fit to the slow and fast wind distributions intersect. The range of speeds near Earth predicted from observations of the near-Sun kinetic energy flux is highlighted in orange and labeled vK. Green regions indicate the speeds derived using the isopoly model without (vIP) and with (vIPW) Alfvén wave forcing. Table 2 summarizes these values.
Paper: Characterizing the Impact of Alfvén Wave Forcing in Interplanetary Space on the Distribution of Near-Earth Solar Wind Speeds
Authors: B. L. Alterman
Figure caption: A 2D heat map showing the frequency of observations as a function of solar wind speed and kinetic energy flux observed near Earth. Because slow solar wind is observed more frequently than fast solar wind (Figure 1), each column in the heat map is normalized to its maximum value to remove this sampling artifact. The black dashed–dotted line is the central value in each column; the black solid lines are the spread of values. The region highlighted with a thick black line corresponds to vfast. The orange horizontal band is the range of kinetic energy fluxes predicted near Earth from Probe observations of the radial scaling of the total and kinetic energy fluxes during Encounters 1, 2, 4, and 5.
Paper: Characterizing the Impact of Alfvén Wave Forcing in Interplanetary Space on the Distribution of Near-Earth Solar Wind Speeds
Authors: B. L. Alterman
Figure caption: An example of the log-normal distribution fit to observations of solar wind speeds observed near Earth in the range of speeds 620–630 km s−1. The binned observations are in black. The fit is plotted in a dashed–dotted orange line.
Paper: On the Origin of Long-term Modulation in the Sun’s Magnetic Activity Cycle
Authors: Chitradeep Saha, Suprabha Mukhopadhyay, Dibyendu Nandy
Figure caption: Top and middle panels: plot of reconstructed decadal sunspot group number (C. J. Wu et al. 2018, blue curve), with annually resolved reconstructed sunspot number series (I. G. Usoskin et al. 2021, orange curve). Bottom panel: power spectral density corresponding to the above time series. In each cases, the red dashed curves mark the upper threshold of the 3σ significance level of power spectra generated out of 5000 noise-based surrogate realizations of the original data. We estimate the first-order autoregressive parameters (M. R. Allen & L. A. Smith 1996) to model the colored noise in the time series. The autoregressive model of first order should be sufficiently good over higher orders in this context as we are mainly probing the longer timescale regime where the autocorrelation in the time series becomes weaker. The gray-shaded region signifies the periodicity interval that corresponds to amplitude modulation beyond decadal timescale, i.e., supradecadal modulation.
Paper: On the Origin of Long-term Modulation in the Sun’s Magnetic Activity Cycle
Authors: Chitradeep Saha, Suprabha Mukhopadhyay, Dibyendu Nandy
Figure caption: Power spectrum of simulated sunspot time series without any stochastic fluctuation in the poloidal sources. Results are from 2D solar dynamo model simulations (panel (a), (c), and (e)) and time delay dynamo model simulations (panel (b), (d), and (f)). Top panels ((a) and (b)) show results for second-order nonlinearity incorporated in the poloidal sources, whereas middle panels are similar to top panels but with the order of nonlinearity, portrayed in Equations 3 and 4, increased to four. Bottom panels demonstrate the results for the highly supercritical regime of dynamo operation. The red dashed curve denotes the statistical 3σ threshold. The gray-shaded regions in all the panels denote the periodicity regime that corresponds to supradecadal modulation. In all of these nonstochastic simulations, there is no trace of statistically significant spectral peak in the supradecadal regime. Refer to the Appendix for the exact amplitudes of poloidal sources used in these simulations.
Paper: On the Origin of Long-term Modulation in the Sun’s Magnetic Activity Cycle
Authors: Chitradeep Saha, Suprabha Mukhopadhyay, Dibyendu Nandy
Figure caption: Distributions of cumulative power contained in 50 yr wide bands of periodicities for statistically significant spectral peaks lying above the 3σ threshold in the decadal-averaged time series of (a) reconstructed data (blue), (b) stochastic 2D solar dynamo model simulations (orange), and (c) stochastic time delay dynamo model simulations (red crosshatch). Each of these three distributions is normalized to unity with respect to the bins containing the highest spectral power.
Paper: On the Origin of Long-term Modulation in the Sun’s Magnetic Activity Cycle
Authors: Chitradeep Saha, Suprabha Mukhopadhyay, Dibyendu Nandy
Figure caption: Variation of the simulated mean toroidal flux with αBL in the absence of stochastic forcing for the 2D model (left panel) and the reduced model (right panel).
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Panel (a): the first of four o-band ATLAS, Rio Hurtardo telescope discovery images of 2024 YR4  from 2024 December 27 05:42:49 UTC. The asteroid moved at a rate of 22﹩\mathop{.}\limits^{{\rm{^{\prime} }}}﹩8 per hour (9﹩\mathop{.}\limits^{\unicode{x000b0}}﹩11 per day) in the northwest direction. The asteroid makes a ​​​​​​∼6 pixel trail (∼11″) in the 30 s ATLAS exposures, indicated by the red circle. Panel (b): the 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. Panel (c): the same as panel (a), but the second of four o-band images containing 2024 YR4 taken on 2024 December 27 05:46:04 UTC. Panel (d): the same as panel c but shows the image after subtracting static sources. The asteroid was detected with an apparent magnitude of o = 16.54 in panel (a) and o = 15.80 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 Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Top panel: the r-band-filter-equivalent time-series lightcurve g, r, i, and Z observations of 2024 YR4  taken by GMOS on 2025 February 7 UTC. The g, i, and Z data were converted to an equivalent r-band brightness by using the colors g − r = 0.70 ± 0.10, r − i = 0.25 ± 0.06, r − Z = −0.02 ± 0.10. The error bars on the data points equal their 1σ photometric uncertainties. Center panel: the same as in the top panel, but the data have been phased by a double-peaked rotation period of 1172 s. A sinusoudal lightcurve model with a double-peaked period of ∼1172 s and amplitude of 0.40 mag is plotted in black. Bottom panel: the same as in the center panel, except that the data have been rebinned with 0.075 wide bins in phase-dimensional space.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Reflectance photometric spectrum of 2024 YR4 consisting of g, r, i, and Z observations of 2024 YR4 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 YR4 have been offset slightly from their location in the wavelength direction. The error bars on the spectrum data points correspond to 1σ uncertainty. The red cross indicates the spectrum has been normalized to unity at 550 nm. The spectral range of R-, Sr-, Sa-, and C-type asteroids from the Bus–DeMeo asteroid taxonomic catalog (F. E. DeMeo et al. 2009) are overplotted with the R-type spectrum most closely resembling the spectra of 2024 YR4. The flat C-type spectrum serves as a baseline to contrast with the other asteroid spectra.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: The a* parameter vs. i − z(Z) colors of 2024 YR4 from our measurements and the a* and i − z(Z) of C-, S-, and V-complex asteroids from Ž. Ivezić et al. (2001) and M. Jurić et al. (2002). We use the scheme of Ž. Ivezić et al. (2002) that sets the color of data points as a function of a* and i − z, where blue symbol colors correspond to C-complex asteroids, red symbol colors correspond to S-complex asteroids, and green symbol colors correspond to V-complex asteroids. We note we use the Z magnitude of 2024 YR4 in place of its Z magnitude for its i − z color calculation used in this plot. We also include the a* and i − z determined with the mean S-, V-, and C-complex spectra taken from F. E. DeMeo et al. (2009) and the a* and i − z determined from the Sun’s colors (C. N. A. Willmer 2018).
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Top left panel: a coadd stack of 11 × 200 s g-filter images of 2024 YR4 with a red 5″ wide double arrow for scale. The cardinal directions are shown with yellow arrows. Top right panel: a coadd stack of 12 × 200 s r filter images of 2024 YR4. Bottom left panel: a coadd stack of 8 × 200 s i filter images of 2024 YR4. Bottom right panel: a coadd stack of 8 × 60 s Z filter images of 2024 YR4. The scale and orientation of the r-, i-, and Z-band panels are the same as in the g-band panel.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Top panel: edge-on ecliptic view of the orbits and positions of 2024 YR4 (black), Mercury (red), Venus (blue), Earth (purple), and Mars (green) at the time of the discovery of 2024 YR4 on 2024 December 27 05:42:49. Bottom panel: the same as the top panel, except from the ecliptic pole. A close-up of the positions of 2024 YR4 and the Earth is shown in an inset. This orbital diagram was generated using REBOUND (H. Rein & S.-F. Liu 2012; H. Rein & D. S. Spiegel 2015).
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Left panel: LS 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 power is located at a single-peaked lightcurve period of 587 s. Right 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 LS.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Convex shape model of 2024 YR4 in three orthogonal views obtained using publicly available photometry of 2024 YR4 from the MPS archive, VLT archive, and Gemini. The X-vs.-Z and Y-vs.-Z views show the edge-on view of the asteroid with the spin axis pointing in the Z-direction (ecliptic longitude and latitude equal to 42∘ and −25∘). The asteroid is viewed from a pole-on view in the X-vs.-Y view.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: The periodogram of 2024 YR4, computed near the suspected synodic period. The minimum at Psid = 0.32439 hr, indicated by the vertical line, corresponds to the global minimum. The horizontal line represents the rms threshold, indicating the statistical significance of the minimum.
Paper: The Discovery and Characterization of Earth-crossing Asteroid 2024 YR4
Authors: Bryce T. Bolin, Josef Hanuš, Larry Denneau, Roberto Bonamico, Laura-May Abron, Marco Delbo, Josef Ďurech, Robert Jedicke, Leo Y. Alcorn, Aleksandar Cikota, Swayamtrupta Panda, Henrique Reggiani
Figure caption: Lightcurve fit of 2024 YR4, showing dense photometric observations from VLT and Gemini in the r and g filters (top panels) and sparse data sets from ATLAS, Catalina Sky Survey, and Pan-STARRS (bottom three panels). The best-fit model is overlaid.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: RML and CLEAN comparison for continuum-subtracted observations of AA Tau in 12CO J = 3–2, 13CO J = 3–2, and CS J = 7–6. Shown are three adjacent channels, centered at v = 7.8 km s−1 where the 12CO J = 3–2 non-Keplerian feature appears most prominently. All six panels for each molecular line (the three RML panels and three CLEAN panels) are plotted on the same color scale, and the color bars for each molecule are in units of Jy arcsec−2. The white arrows indicate the NKF, which can be seen in the 12CO J = 3–2 emission; while the feature is present in all three channels shown, we only place the arrows in one RML image and one CLEAN image to highlight the location of the feature.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Five channels of LkCa 15 selected for thorough CV testing (RML images pictured). Channels were selected arbitrarily across the range of velocity space where gas emission is prominent in all three molecular lines, testing channels that varied in the spatial extent and general morphology of the emission. We intentionally include a channel with a prominent NKF at v = 6.9 km s−1. The color bar has units of Jy arcsec−2.
Paper: exoALMA. IX. Regularized Maximum Likelihood Imaging of Non-Keplerian Features
Authors: Brianna Zawadzki, Ian Czekala, Maria Galloway-Sprietsma, Jaehan Bae, Marcelo Barraza-Alfaro, Myriam Benisty, Gianni Cataldi, Pietro Curone, Stefano Facchini, Daniele Fasano, Mario Flock, Misato Fukagawa, Himanshi Garg, Cassandra Hall, Thomas Hilder, Jane Huang, John D. Ilee, Andrea Isella, Andrés F. Izquierdo, Kazuhiro Kanagawa, Geoffroy Lesur, Cristiano Longarini, Ryan A. Loomis, Ryuta Orihara, Christophe Pinte, Daniel J. Price, Giovanni Rosotti, Jochen Stadler, Richard Teague, Hsi-Wei Yen, Gaylor Wafflard-Fernandez, David J. Wilner, Andrew J. Winter, Lisa Wölfer, Tomohiro C. Yoshida
Figure caption: Three different image products showing continuum-subtracted 12CO J = 3–2 emission in AA Tau at v = 7.8 km s−1. We estimate the noise by taking the rms of a signal-free region, shown with the cyan circles. Before beam convolution, the native RML images are in units of Jy arcsec−2 (left). To enable a more direct comparison of the noise properties between RML and CLEAN images, we calculate the rms in the RML image convolved with a circular 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 beam (center) along with the fiducial CLEAN image, which also has a circular 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 beam (right). The rms in the 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 RML image is nearly 2 orders of magnitude lower than the rms in the 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩15 fiducial CLEAN image (0.043 mJy beam−1 and 3.953 mJy beam−1, respectively), demonstrating that regularization can suppress the background noise far below what is expected from instrumental thermal noise.