adsabs/AstroCLIMB huggingface dataset:
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Top: comparison of the griz-band light curves of SN2025ulz and AT2017gfo. The downward-facing triangles correspond to 3σ upper limits for SN2025ulz. Bottom: KN model fits for SN2025ulz. Both models presented have dynamical (low-opacity) ejecta, with 0.025 M⊙ and 0.3c, and disk wind (higher-opacity) ejecta, with 0.05 M⊙ and 0.15c. The model on the left possesses no shock heating, whereas the model on the right is generated invoking maximum shock heating. The hollow symbols correspond to 3σ upper limits.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Top: comparison of SN2025ulz gri-band evolution to the early light curves of SNe 1993J (BRI), 2008ax (gri), 2011dh (gri), and 2016gkg (gri)—all SNe IIb that possess early-time observations. The evolution of SN2025ulz closely resembles the evolution of these transient events. Bottom: bolometric luminosity (LBOL) light-curve property comparisons between SN2025ulz and SNe 1993J, 2008ax, 2011dh, and 2016gkg and the KN AT2017gfo. The LBOL evolution of SN2025ulz closely mirrors the comparison sample of SNe IIb, whereas it exhibits a stark difference to that of AT2017gfo. A similar trend exists for the temperature comparison.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: Left: illustration of the limiting magnitude reached by each PS pointing and the corresponding fraction of the distance posterior for which AT2017gfo-like KN emission can be ruled out. Right: histogram highlighting the fraction of pointings that rule out different fractions of the distance posterior of S250818k. Only a few of the pointings enable the ruling out of a substantial fraction (≳0.8) of the distance posterior.
Paper: Pan-STARRS Follow-up of the Gravitational-wave Event S250818k and the Light Curve of SN2025ulz
Authors: J. H. Gillanders, M. E. Huber, M. Nicholl, S. J. Smartt, K. W. Smith, K. C. Chambers, D. R. Young, J. W. Tweddle, S. Srivastav, M. D. Fulton, F. Stoppa, G. S. H. Paek, A. Aamer, M. R. Alarcon, A. Andersson, A. Aryan, K. Auchettl, T.-W. Chen, T. de Boer, A. K. H. Kong, J. Licandro, T. Lowe, D. Magill, E. A. Magnier, P. Minguez, T. Moore, G. Pignata, A. Rest, M. Serra-Ricart, B. J. Shappee, I. A. Smith, M. A. Tucker, R. Wainscoat
Figure caption: SNIFS spectrum of the host galaxy of SN2025ulz. We mark the location of prominent Hα, [N II] λ6583.46, and [S II] λλ6716.44 & 6730.81 emission, which allows us to measure a host galaxy redshift z = 0.0849 ± 0.0003.
Paper: Understanding the Origin and Dynamical Evolution of the Unique Open Star Cluster Berkeley 20 Using FIRE Simulations
Authors: Alessa I. Wiggins, Jamie R. Quinn, Micah Oeur, Sarah R. Loebman, Peter M. Frinchaboy, Kathryne J. Daniel, Fiona McCluskey, Jonah M. Otto, Hannah R. Woodward, Elena D'Onghia, Andrew Wetzel, Hanna Parul, Binod Bhattarai, Maximilian Cozzi
Figure caption: BOB undergoes major orbital changes. Panel (a) shows the ratio of the local to annular stellar (blue) and median gas (dark orange) densities over time. Blue/dark orange vertical dotted lines indicate when BOB encounters a significant stellar/gaseous overdensity. We identify stellar density peaks after the disk settles at ∼9.25 Gyr (S. Yu et al. 2021) and before the merger event. The black, rightmost dashed–dotted line at ∼12.4 Gyr indicates the merger event with a ∼Sgr dSph–mass satellite, after which BOB’s vertical amplitude increases dramatically. Panel (b) tracks BOB’s height above/below the midplane, while panel (c) shows its instantaneous and guiding radius over time. Panel (d) shows BOB’s virial ratio, which stays ≲1 after 10 Gyr, indicating the cluster remains bound. Panel (e) shows the cluster’s angular momentum, Lz, with blue/red points indicating BOB’s location on the leading/trailing edge of a dominant spiral arm, respectively, otherwise BOB is in an interarm region.
Paper: Cospatial Multiwavelength Observations of an Eruptive Prominence as the Bright Core of a Coronal Mass Ejection
Authors: Bin Zhuang, Tingyu Gou, Noé Lugaz, Manuela Temmer, Brian E. Wood, Yara De Leo, Shaheda Begum Shaik, Phillip Hess, Carlos R. Braga, Cecilia Mac Cormack, Xiaolei Li
Figure caption: EUV and WL observations of the 2022 September 23 event. The top-left two panels show the 3.8 minutes corrected SolO/EUI-FSI 174 and 304 Å composite image and the total-brightness Metis image in visible light processed by the running-difference technique. The bottom three panels show the EUVI 171 and 304 Å composite image, background-subtracted COR1 and COR2 images obtained from STEREO-A, respectively. The top-right panel shows the locations of SolO and STEREO-A relative to the Sun and Earth in the ecliptic plane in the heliocentric Earth ecliptic coordinate system. The CME propagation direction is indicated by the gray arrow.
Paper: Cospatial Multiwavelength Observations of an Eruptive Prominence as the Bright Core of a Coronal Mass Ejection
Authors: Bin Zhuang, Tingyu Gou, Noé Lugaz, Manuela Temmer, Brian E. Wood, Yara De Leo, Shaheda Begum Shaik, Phillip Hess, Carlos R. Braga, Cecilia Mac Cormack, Xiaolei Li
Figure caption: Cospatial observations of the prominence in EUV and WL wavelengths at three different times. In each row, from left to right, the four panels show the scaled and mirrored SolO image in 174 and 304 Å channels, the background-subtracted COR1 image, and the COR1 image overplotted with the bright data points identified in FSI. The dashed contours indicate the heliocentric distances ranging from 1 to 3.5 R⊙ in increments of 0.5 R⊙.
Paper: Cospatial Multiwavelength Observations of an Eruptive Prominence as the Bright Core of a Coronal Mass Ejection
Authors: Bin Zhuang, Tingyu Gou, Noé Lugaz, Manuela Temmer, Brian E. Wood, Yara De Leo, Shaheda Begum Shaik, Phillip Hess, Carlos R. Braga, Cecilia Mac Cormack, Xiaolei Li
Figure caption: Testing the overlay SolO/EUI-FSI (3.8 minutes corrected) and STEREO-A/EUVI images. The left, middle, and right panels show the scaled and mirrored SolO/FSI image in 304 Å, the STEREO-A/EUVI image in 304 Å, and their overlay in the helioprojective Cartesian coordinates, respectively. The two dashed contours in the figure indicate the projected heliocentric distances of 1 and 1.5 R⊙.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: Radio 10 GHz light curve of SN 2023fyq with various model fits. We show the best-fit SSA and FFA models at 10 GHz (where these are fits from Equations (1) and (3) to the entire dataset derived in Section 3) along with a model taken from S. C. Wu & D. Tsuna (2025; the “merger model”) described in Section 3.1. This merger model has a similar shock speed ∼9000 km s−1 but a different α = 0.55 and slightly different ϵe and ϵB. The merger model cuts off at ∼220 days, as this is when D. Tsuna et al. (2024) constrain the mass loss to begin for these merger models. The 3σ upper limits in black are not taken into account for the fits for any of the models.
Paper: The First Radio View of a Type Ibn Supernova in SN 2023fyq: Understanding the Mass-loss History in the Last Decade before the Explosion
Authors: Raphael Baer-Way, Nayana A. J., Wynn Jacobson-Galán, Poonam Chandra, Maryam Modjaz, Samantha C. Wu, Daichi Tsuna, Raffaella Margutti, Ryan Chornock, Craig Pellegrino, Yize Dong, Maria R. Drout, Charles D. Kilpatrick, Dan Milisavljevic, Daniel Patnaude, Candice Stauffer
Figure caption: A view of all previous radio-observed SNe Ibn and the upper limits on luminosities, including 10 GHz detections and nondetections for SN  2023fyq. The nondetections are shown with downward-facing triangles and are all 3σ limits. SNe 2006jc, 2019qav, 2019aajs, and 2020bgq were observed quite early, and thus their radio evolution could still be consistent with SN 2023fyq, but SN 2015G clearly shows upper limits that are much deeper than the observed radio emission from SN 2023fyq. Future deep observations between 50 and 500 days post-explosion will be key to constraining the subclass.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Evolution of Alfvén and fast magnetosonic waves at early times, t < 100r*/c, where r* is the stellar radius. This is illustrated by the perturbations of the toroidal magnetic field δBtor (top row) and the toroidal electric field δEtor (bottom row), normalized to the poloidal magnetic field Bpol, respectively. Both waves enter a nonlinear regime. In the case of Alfvén waves, forming a nonlinear Alfvén wave packet, opening the magnetosphere and ejecting it, and forming equatorial current sheets, (kilohertz) fast magnetosonic waves will ultimately enter a monster shock stage, indicated by the characteristic shape (A. M. Beloborodov 2023), e.g., of the leading waves in the lower rightmost panel. The black square indicates the area shown in Figure 7.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Time evolution (top row) and corresponding frequency spectrum (bottom row) of crustal surface motion (left column) and magnetospheric (right column) perturbations. We quantify surface motion via an effective normalized surface kinetic energy ﹩{e}_{\mathrm{cru}}=\tfrac{1}{2{c}^{2}}\int ({v}_{\theta }^{2}+{v}_{\varphi }^{2})\sin \theta d\theta d\varphi ﹩ and MPs via the normalized EM energy ﹩{e}_{\mathrm{mag}}=\tfrac{1}{c{r}_{* }^{2}{B}_{* }^{2}}\int {r}^{2}{S}_{r}\sin \theta d\theta d\varphi ﹩, where Sr is the radial component of Poynting vector at r = 12 r*, with r* and B* being the stellar radius and surface magnetic field strength, respectively.
Paper: The First Triple Radio Active Galactic Nucleus in an Ongoing Galaxy Merger
Authors: Emma Schwartzman, Ryan W. Pfeifle, Tracy E. Clarke, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, Miranda McCarthy, Daniel Stern, Peter G. Boorman, Joanna Piotrowska
Figure caption: Optical DeCaLS grz images and radio VLA images of J1218/J1219+1035. (A): DeCaLS grz image of the interacting system J1218+1035 NW/SE and J1219+1035. The two other galaxies to the north of J1218+1035 NW and to the northeast of J1218+1035 SE reside at higher redshifts and are not associated with this system. (B), (C), and (D): VLA 3, 10, and 15 GHz images, respectively, of the interacting system. In each main panel, J1218+1035 NW/SE and J1219+1035are marked with dashed, dashed–dotted, and dotted white circles, the band is given in the top-left corner, and a 30″  scale bar is given in the bottom-left corner. In each of the VLA panels, the thumbnails in the bottom-right corner show the 10″  × 10″ field of view centered on the individual AGN and better exhibit the radio emission associated with those nuclei.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Meridional x–z-plane slice at late time t = 275 r*/c, illustrating the perturbations of the toroidal magnetic field δBtor normalized to the poloidal magnetic field Bpol, the rescaled Alfvén waves energy density ﹩{r}^{2}\delta {U}_{A}/{r}_{* }^{2}{B}_{* }^{2}﹩, and the rescaled current density δj/r*B*, where r* and B* are the radius and surface magnetic field strength of the neutron star.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Magnetospheric state during a magnetar quake event. Shown is a meridional x–z-plane slice at late times, t = 275, r*/c, illustrating the perturbations of the toroidal magnetic field δBtor (top part) and the toroidal electric field δEtor (bottom part), normalized to the poloidal magnetic field Bpol in the full simulation, corresponding to Alfvén and fast magnetosonic waves, respectively. We can see several cycles of wave injection, most of which nonlinearly steepen, combing out part of the initially dipolar magnetosphere. The black square indicates the area shown in Figure 5.
Paper: The First Triple Radio Active Galactic Nucleus in an Ongoing Galaxy Merger
Authors: Emma Schwartzman, Ryan W. Pfeifle, Tracy E. Clarke, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, Miranda McCarthy, Daniel Stern, Peter G. Boorman, Joanna Piotrowska
Figure caption: VLA radio spectrum of all cores in J1218/1219+1035. Square, circular, and triangular points represent J1219+1035, J1218+1035 NW, and J1218+1035 SE, respectively. Purple, green, and brown points represent 3, 10, and 15 GHz measurements, respectively. Each source is fit with a standard power law. The solid red line, dotted pink line, and dotted–dashed blue line are fit to J1219+1035, J1218+1035 NW, and J1218+1035 SE, respectively. Each power-law spectral index is shown in the upper left-hand corner.
Paper: The First Triple Radio Active Galactic Nucleus in an Ongoing Galaxy Merger
Authors: Emma Schwartzman, Ryan W. Pfeifle, Tracy E. Clarke, Kimberly A. Weaver, Nathan J. Secrest, Barry Rothberg, Miranda McCarthy, Daniel Stern, Peter G. Boorman, Joanna Piotrowska
Figure caption: Keck LRIS long-slit spectra for J1218+1035 NW and SE.
Paper: Crustal Quakes Spark Magnetospheric Blasts: Imprints of Realistic Magnetar Crust Oscillations on the Fast Radio Burst Signal
Authors: Louis Burnaz, Elias R. Most, Ashley Bransgrove
Figure caption: Velocity profiles of the CPs at the base of the magnetosphere. The top row displays the polar velocity vθ/c, and the bottom row displays the azimuthal velocity vφ/c, both shown at various times during the evolution of the perturbation.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: Per-galaxy propagated uncertainties on the δDGR accounting for only measurement errors (orange), only αCO and R31 systematics (violet), and both (gray). Dots represent the median of the derived per-galaxy δDGR distribution, while error bars are the 16th and 86th percentile levels. Red cross markers show the fiducial values adopted in the Letter. The dashed line corresponds to the reference value of δDGR = 1/100, and the light-blue band represents the 0.15 dex dispersion measured for SFGs (G. E. Magdis et al. 2012).
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: For each QG: left: ALMA Band 6 primary-beam corrected moment-zero map (5″ × 5″ size) overlaid with dust continuum contours (white dashed) and CO(3–2) contours (blue solid) increasing from 2σ with 1σ step. Typical beam size of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩85 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩7 and 1″ scale (corresponding to ∼5 kpc) are shown; right: stellar emission from JWST F277W (or Hubble Space Telescope F160W for sources hCOS-d7 and hCOS-d9) with basic physical properties annotated in the lower-right corner.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: Comparison of fiducial dust properties with alternative dust-mass estimates (upper: versus modified blackbody fits; lower: versus N. Scoville et al. 2016). We consider 12 QGs with direct ALMA estimates. From left to right: comparisons of our fiducial values versus alternative methods to estimate Mdust, fdust, and ﹩\mathrm{log}({\delta }_{{\rm{DGR}}})﹩.
Paper: Analyses of the Ancient Chinese Report on the Total Solar Eclipse in 709 BCE: Implications for the Contemporaneous Earth’s Rotation Speed and Solar Cycles
Authors: Hisashi Hayakawa, Mathew J. Owens, Meng Jin, Mitsuru Sôma, Mike Lockwood
Figure caption: Contextualization of the total solar eclipse in −708 (dashed vertical black line) upon contemporaneous solar cycles on the basis of radiocarbon data sets (U+25). The first and second panels show U+25’s open solar flux (OSF) and SSN. The third and fourth panels show the full streamer belt width (SB width) and inclination (Inc.) using the methods and coefficients of M. Lockwood & M. J. Owens (2014), while their loss rate coefficient is adjusted according to SILSO SSN version 2 (F. Clette et al. 2023). On their basis, the bottom panel schematically shows how streamer belts look from Qūfù upon the said total solar eclipse in these three scenarios.
Paper: Analyses of the Ancient Chinese Report on the Total Solar Eclipse in 709 BCE: Implications for the Contemporaneous Earth’s Rotation Speed and Solar Cycles
Authors: Hisashi Hayakawa, Mathew J. Owens, Meng Jin, Mitsuru Sôma, Mike Lockwood
Figure caption: Solar disk orientation at the eclipse maximum on −708 July 17, as seen from Qūfù, with lower-limit, optimal, and upper-limit ΔT values of 20,264 s, 21,180 s, and 21,204 s, respectively.
Paper: Analyses of the Ancient Chinese Report on the Total Solar Eclipse in 709 BCE: Implications for the Contemporaneous Earth’s Rotation Speed and Solar Cycles
Authors: Hisashi Hayakawa, Mathew J. Owens, Meng Jin, Mitsuru Sôma, Mike Lockwood
Figure caption: Comparison of M+21’s ΔT spline curve (black line) and our ΔT constraints based on total solar eclipses (red bars), as discussed in Appendix E. We show two error margins for the −647 eclipse, owing to two candidate sites for the observation.
Paper: Analyses of the Ancient Chinese Report on the Total Solar Eclipse in 709 BCE: Implications for the Contemporaneous Earth’s Rotation Speed and Solar Cycles
Authors: Hisashi Hayakawa, Mathew J. Owens, Meng Jin, Mitsuru Sôma, Mike Lockwood
Figure caption: Excerpts of records of the −708 total solar eclipse in CQ-NAJ (v. 2, ff. 6b–7a) and HS-NAJ (v. 27, ff. 2b–3a), reproduced courtesy of the National Archives of Japan (see Appendix A). The red and blue squares show records of the total solar eclipse and mentions of the possible coronal structure.
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: “Isopoly” wind profiles and data statistics. From top to bottom, the panels show isopoly profiles of proton density, proton velocity, and proton temperature, colorized as in Figure 1 according to the wind speed at 1 au. These models are superimposed on statistics of the 15 minute cadence data set of each quantity as a function of radial distance. In each panel, the solid line shows the median as a function of distance, while two progressively fainter regions annotate the interquartile range and the 1st/99th percentile ranges. Black (blue) lines and shading indicate Parker and Solar Orbiter statistics, respectively. In the middle panel, scatter points provide additional context depicting conjunction results on solar wind acceleration from Y. J. Rivera et al. (2024, 2025). A dashed vertical line indicates Parker’s closest perihelion distance.
Paper: Multispacecraft Measurements of the Evolving Geometry of the Solar Alfvén Surface over Half a Solar Cycle
Authors: Samuel T. Badman, Michael L. Stevens, Stuart D. Bale, Yeimy J. Rivera, Kristopher G. Klein, Tatiana Niembro, Rohit Chhiber, Ali Rahmati, Phyllis L. Whittlesey, Roberto Livi, Davin E. Larson, Christopher J. Owen, Kristoff W. Paulson, Timothy S. Horbury, Jean Morris, Helen O'Brien, Jean-Baptiste Dakeyo, Jaye L. Verniero, Mihailo Martinovic, Marc Pulupa, Federico Fraschetti
Figure caption: Effect of SPAN-i temperature correction. A 2D heat map of the “gyrocorrected” scalar proton temperature vs. the original SPAN-i moment 15 minute medians. A red diagonal line indicates y = x. A blue contour shows that the corrected temperature is systematically hotter in general. A green contour shows that the distribution and correction is less severe after selecting for good FOV intervals; however, at the highest temperatures, the systematic increase is still observed.
Paper: ALMA Reveals Diverse Dust-to-gas Mass Ratios and Quenching Modes in Old Quiescent Galaxies
Authors: G. Lorenzon, D. Donevski, A. W. S. Man, M. Romano, K. E. Whitaker, S. Belli, D. Liu, M. M. Lee, D. Narayanan, A. Long, I. Shivaei, A. Nanni, K. Lisiecki, P. Sawant, G. Rodighiero, I. Damjanov, Junais, R. Davé, C. Pappalardo, C. Lovell, M. Hamed
Figure caption: (a) Selected QGs in the UVJ plane, color-coded by sSFR. (b) Evolution of δDGR with sSFR, tq, and M⋆. Large circles mark QGs detected with ALMA (10 in both CO and dust, 1 in either CO or dust); triangles show nondetections in both CO and Band 6 dust continuum. Small points are literature QGs at z ∼ 1 (J. S. Spilker et al. 2025). For all symbols, the lower or upper limits of δDGR are denoted with arrows. Solid lines show fast and slow quenching tracks for z ∼ 0.4 QGs from SIMBA  (G. Lorenzon et al. 2025). The horizontal line marks the canonical δDGR ∼ 1/100.