adsabs/AstroCLIMB huggingface dataset:
Paper: GalCEM. I. An Open-source Detailed Isotopic Chemical Evolution Code
Authors: Eda Gjergo, Aleksei G. Sorokin, Anthony Ruth, Emanuele Spitoni, Francesca Matteucci, Xilong Fan, Jinning Liang, Marco Limongi, Yuta Yamazaki, Motohiko Kusakabe, Toshitaka Kajino
Figure caption: [X/Fe]–[Fe/H] relation abundance plots for the elements up to atomic number 32. To facilitate the navigation of the table, the atomic number is shown right before the element symbol. The total abundance in the one-zone run is enriched by BBN (Galli & Palla 2013), SNIa (Iwamoto et al. 1999), AGB/LIMs (Cristallo et al. 2015, with zero initial rotational velocity), and SNCC (Limongi & Chieffi 2018, set R, with zero initial rotational velocity). The observational data scatter is labeled according to the legend on top.
Paper: GalCEM. I. An Open-source Detailed Isotopic Chemical Evolution Code
Authors: Eda Gjergo, Aleksei G. Sorokin, Anthony Ruth, Emanuele Spitoni, Francesca Matteucci, Xilong Fan, Jinning Liang, Marco Limongi, Yuta Yamazaki, Motohiko Kusakabe, Toshitaka Kajino
Figure caption: Log‒log time-dependent returned mass rates (in units of M ⊙ yr−1) for each enrichment channel included in the one-zone run presented in this work—which include BBN, SNIa, LIMs, and SNCC as outlined in the Methods, Section 2. The number preceding the atomic symbol represents the atomic mass. To improve readability, we only show the first 120 isotopes, even though the full simulation computes 451 species. This cut includes every zinc nuclide (atomic number of 30), consistent with Figure 12. The full table will be shown in E. Gjergo et al. (2023b, in preparation) with the inclusion of r-process enrichment channels.
Paper: GalCEM. I. An Open-source Detailed Isotopic Chemical Evolution Code
Authors: Eda Gjergo, Aleksei G. Sorokin, Anthony Ruth, Emanuele Spitoni, Francesca Matteucci, Xilong Fan, Jinning Liang, Marco Limongi, Yuta Yamazaki, Motohiko Kusakabe, Toshitaka Kajino
Figure caption: The age‒metallicity relation with respect to the metallicity (upper figure) and iron abundance (lower figure) normalized to solar values. The orange lines cross at the solar age and abundance. The observational scatter comes from the APOKASC sample. Stellar age and abundances are taken from Silva Aguirre et al. (2018), while the iron abundance is taken from Pinsonneault et al. (2014).
Paper: A Spatially Resolved X-Ray Polarization Map of the Vela Pulsar Wind Nebula
Authors: Kuan Liu, Fei Xie, Yi-han Liu, Chi-Yung Ng, Niccolò Bucciantini, Roger W. Romani, Martin C. Weisskopf, Enrico Costa, Alessandro Di Marco, Fabio La Monaca, Fabio Muleri, Paolo Soffitta, Wei Deng, Yu Meng, En-wei Liang
Figure caption: Chandra (left), ATCA (middle, 6 cm), and IXPE (right) images of the Vela PWN. In the ATCA image, the contour from the Chandra observation is overlaid. The white box in the right panel is the region analyzed in Xie et al. (2022), and the white circle marks the boundary of a radius of 300″ centered at the pulsar. The red panda region and three black squared boxes identify the background and the source regions in the analysis in Section 3, respectively. Each black box is 90″ × 90″, and the background region extends from an inner radius of 140″ up to an outer radius of 300″ centered on the pulsar, with an open angle of 160°. The white (black) lines in the middle (right) panel show the magnetic field direction revealed by the radio (X-ray) polarization.
Paper: A Spatially Resolved X-Ray Polarization Map of the Vela Pulsar Wind Nebula
Authors: Kuan Liu, Fei Xie, Yi-han Liu, Chi-Yung Ng, Niccolò Bucciantini, Roger W. Romani, Martin C. Weisskopf, Enrico Costa, Alessandro Di Marco, Fabio La Monaca, Fabio Muleri, Paolo Soffitta, Wei Deng, Yu Meng, En-wei Liang
Figure caption: (Top) The PD map of the Vela PWN in the 2–5 keV energy range with a pixel size of 45″ overlaid with the Chandra contour. Pixels with X-ray PD > MDP99 have polarization vectors on top. The length of the black (white) lines indicates the PD measure in X-ray (radio), and orientation indicates the projected magnetic field. (Bottom) The polarization protractor plot for pixels with the polarization vector overlaid on the top panel, covering the same region, with radius and polar angle indicating the PD and PA, respectively.
Paper: A Spatially Resolved X-Ray Polarization Map of the Vela Pulsar Wind Nebula
Authors: Kuan Liu, Fei Xie, Yi-han Liu, Chi-Yung Ng, Niccolò Bucciantini, Roger W. Romani, Martin C. Weisskopf, Enrico Costa, Alessandro Di Marco, Fabio La Monaca, Fabio Muleri, Paolo Soffitta, Wei Deng, Yu Meng, En-wei Liang
Figure caption: The relationship between the upper limit of the ratio between the random and ordered magnetic field strength and the angle between the light of sight and the magnetic field direction, with given PD of 55% (blue), 60% (orange), and 65% (green).
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: We show MIRI pointing 1 (right panel) alongside the Spitzer/IRAC (middle) and MIPS (left) observations of the same region. The apertures show the location of detected sources in each image (MIRI region only). For the MIPS (IRAC) image, the apertures are 6″(2″), corresponding to the instrument beam size. In the IRAC image, blue corresponds to channel 1 (3.6 μm), green corresponds to channel 2 (4.5 μm), and red corresponds to channel 3 (5.8 μm). In the MIRI image, the 770W filter is blue, F1000W is green, and F1280W is red.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption:  L 6.2/L IR vs. L IR for the MIRI galaxies falling in the redshift ranges in Equation (8). L 6.2 has been estimated by calculating what percentage of the photometric point could be due to the 6.2 μm feature using the 5MUSES sample of star-forming galaxies from Kirkpatrick et al. (2014; black stars). The mid-IR weak galaxies are shown as the open symbols, while the filled symbols correspond to the dust-rich galaxies. Lower-luminosity galaxies have higher ratios of L 6.2/L IR, in line with local trends. Interestingly, the higher-redshift sources seems to have higher L 6.2/L IR, which could indicate a shift in the star-forming conditions at higher redshift. Spectroscopy is required to accurately measure L 6.2 and confirm this trend.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: Left panel: MIRI color selection of AGN. Dust-rich galaxies (circles) are colored according to f(AGN)MIR. Galaxies with f(AGN)MIR> 0.5 are shown as filled circles. The mid-IR weak galaxies are the gray squares. The proposed AGN selection region (Equation (1)) is shown as the solid line. We illustrate how the dust-rich star-forming galaxies (purple dashed line; K15 template) and mid-IR weak galaxies (magenta and pink dotted–dashed lines; this work) move with redshift. AGN do not strongly evolve with redshift. Dust-rich galaxies separate by f(AGN)MIR, while the mid-IR weak galaxies contaminate the AGN regions. Right panel: mid-IR weak SEDs compared with a K15 AGN template. The IRAC Ch 1 (3.6 μm) bandpass is shown alongside the MIRI bandpasses. All bandpasses have been redshifted to z = 1. At this redshift, the mid-IR weak and AGN templates have similar mid-IR colors, but the inclusion of a near-IR data point will help to separate them.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: Redshift vs. ν L  ν  for the full MIPS population (ν = 24 μm; black crosses) and the MIRI population (ν = 18 μm; orange squares). The surprising lack of high-z MIRI sources is attributable to the lack of bright dust features at λ rest ≤ 5μm and the much smaller survey area. MIRI is capable of detecting fainter sources than MIPS at all redshifts in a fraction of the time. We show the final sample (S/N > 3 in at least two bands and well fit by a mid-IR template; 385 18 μm galaxies meet these criteria) in orange. We also show the sources that have S/N > 3 in only the F1800W filter (14 sources; blue circles with crosses) and the sources that are not well fit with a mid-IR template (34 sources; blue triangles). Our selection criteria are not biasing the final sample toward brighter sources. The histograms in the side panels have been arbitrarily normalized due to the stark difference in the number of sources.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: Left panel: average SEDs from Figure 4. The PAH features clearly become stronger with increasing luminosity. At low luminosities, the mid-IR emission is much weaker than the near-IR emission. Right panel: average SEDs are plotted alongside the CE01 template of the same L IR. Arbitrary normalization is applied to templates of the same luminosities. The CE01 templates have more emission around λ ∼ 1.6 μm, which may be attributable to their older stellar populations.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: MIRI + near-IR color selection of AGN. Symbols and lines are the same as in Figure 6. Dust-rich galaxies separate from mid-IR weak galaxies, in contrast with Figure 6. The solid lines show our proposed AGN selection region. The main contaminant in this region is the dust-rich star-forming galaxies at z < 1.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: The fraction of galaxies that are mid-IR weak (i.e., fit with CE01 templates rather than K15; blue squares) or AGN (f(AGN)MIR> 0.5; red triangles) as a function of L IR (left) and redshift (right). The small number statistics make it difficult to narrow down the true distribution of AGN with redshift, although it seems to be increasing.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: Optical vs. IR SFRs, where symbol color and shape correspond to redshift. Mid-IR weak galaxies are shown as open symbols. At lower luminosities, the bulk of star formation is unobscured, which is reflected by the optical SFRs being systematically higher than the IR SFRs. This is mainly an issue for the mid-IR weak galaxies.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: 10 μm cumulative number counts for all sources with S/N > 3 in F1000W (open stars) and the final sample (filled stars). Our selection criteria mainly affected sources at the faintest F1000W fluxes. We also show the number counts for the mid-IR weak galaxies (blue squares), star-forming galaxies (f(AGN)MIR≤ 0.5; filled green circles), and AGN (f(AGN)MIR> 0.5; red triangles). AGN predominantly have brighter F1000W fluxes. The 8 μm number counts from Fazio et al. (2004) are shown in pink. The discrepancy between the 8 and 10 μm counts may be due to the large differences in field sizes. The number of sources in one MIRI FOV is shown on the right axis.
Paper: CEERS Key Paper. VII. JWST/MIRI Reveals a Faint Population of Galaxies at Cosmic Noon Unseen by Spitzer
Authors: Allison Kirkpatrick, Guang Yang, Aurélien Le Bail, Greg Troiani, Eric F. Bell, Nikko J. Cleri, David Elbaz, Steven L. Finkelstein, Nimish P. Hathi, Michaela Hirschmann, Benne W. Holwerda, Dale D. Kocevski, Ray A. Lucas, Jed McKinney, Casey Papovich, Pablo G. Pérez-González, Alexander de la Vega, Micaela B. Bagley, Emanuele Daddi, Mark Dickinson, Henry C. Ferguson, Adriano Fontana, Andrea Grazian, Norman A. Grogin, Pablo Arrabal Haro, Jeyhan S. Kartaltepe, Lisa J. Kewley, Anton M. Koekemoer, Jennifer M. Lotz, Laura Pentericci, Nor Pirzkal, Swara Ravindranath, Rachel S. Somerville, Jonathan R. Trump, Stephen M. Wilkins, L. Y. Aaron. Yung
Figure caption: To create average SEDs (shown in black), we separated galaxies by luminosity and normalized to the median luminosity in each bin. Individual galaxies are plotted by color.
Paper: Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
Authors: Theodore Kareta, Cristina Thomas, Jian-Yang Li, Matthew M. Knight, Nicholas Moskovitz, Agata Rożek, Michele T. Bannister, Simone Ieva, Colin Snodgrass, Petr Pravec, Eileen V. Ryan, William H. Ryan, Eugene G. Fahnestock, Andrew S. Rivkin, Nancy Chabot, Alan Fitzsimmons, David Osip, Tim Lister, Gal Sarid, Masatoshi Hirabayashi, Tony Farnham, Gonzalo Tancredi, Patrick Michel, Richard Wainscoat, Rob Weryk, Bonnie Burrati, Jana Pittichová, Ryan Ridden-Harper, Nicole J. Tan, Paul Tristram, Tyler Brown, Mariangela Bonavita, Martin Burgdorf, Elahe Khalouei, Penelope Longa, Markus Rabus, Sedighe Sajadian, Uffe Graae Jorgensen, Martin Dominik, Jean-Baptiste Kikwaya, Elena Mazzotta Epifani, Elisabetta Dotto, Prasanna Deshapriya, Pedro Hasselmann, Massimo Dall'Ora, Lyu Abe, Tristan Guillot, Djamel Mékarnia, Abdelkrim Agabi, Philippe Bendjoya, Olga Suarez, Amaury Triaud, Thomas Gasparetto, Maximillian N. Günther, Michael Kueppers, Bruno Merin, Joseph Chatelain, Edward Gomez, Helen Usher, Cai Stoddard-Jones, Matthew Bartnik, Michael Bellaver, Brenna Chetan, Emma Dugan, Tori Fallon, Jeremy Fedewa, Caitlyn Gerhard, Seth A. Jacobson, Shane Painter, David-Michael Peterson, Joseph E. Rodriguez, Cody Smith, Kirill V. Sokolovsky, Hannah Sullivan, Kate Townley, Sarah Watson, Levi Webb, Josep M. Trigo-Rodríguez, Josep M. Llenas, Ignacio Pérez-García, A. J. Castro-Tirado, Jean-Baptiste Vincent, Alessandra Migliorini, Monica Lazzarin, Fiorangela La Forgia, Fabio Ferrari, Tom Polakis, Brian Skiff
Figure caption: Top: a zoomed-in section of Figure 1 highlighting the change in photometric dimming in the Swope (“x”s), LCOGT (diamonds), and Danish 1.54 m (squares) data sets which have fast enough cadences to detect and characterize it. The dimming appears to “pause” seven to eight days after impact and then continue approximately a day or two later at very similar rates (often within 1σ of each other). The Danish data set had mutual event contamination masked out, while Swope and LCOGT did not. This suggests that mutual events do not play a significant role in this photometric event. The three sites also used slightly different filters which each peak at red wavelengths (Swope utilized Sloan r, LCOGT used the broadband PanSTARRS w (close to Sloan g+r+i), and the Danish 1.54 m utilized the Johnson R filter). While the retrieved dimming rates for identical apertures are really very similar, this may explain some of the vertical offsets between the observatories. Bottom: the same timeframe but focusing on photometry with different aperture radii from the Swope and Danish telescopes, with aperture size indicated by color (pink for 1.″5, blue for 2′–2.″5, black for 5.″0, and orange for 7.″5). Smaller apertures dim faster, but the change in photometric behavior at the eight-day mark is similar among aperture sizes.
Paper: Ejecta Evolution Following a Planned Impact into an Asteroid: The First Five Weeks
Authors: Theodore Kareta, Cristina Thomas, Jian-Yang Li, Matthew M. Knight, Nicholas Moskovitz, Agata Rożek, Michele T. Bannister, Simone Ieva, Colin Snodgrass, Petr Pravec, Eileen V. Ryan, William H. Ryan, Eugene G. Fahnestock, Andrew S. Rivkin, Nancy Chabot, Alan Fitzsimmons, David Osip, Tim Lister, Gal Sarid, Masatoshi Hirabayashi, Tony Farnham, Gonzalo Tancredi, Patrick Michel, Richard Wainscoat, Rob Weryk, Bonnie Burrati, Jana Pittichová, Ryan Ridden-Harper, Nicole J. Tan, Paul Tristram, Tyler Brown, Mariangela Bonavita, Martin Burgdorf, Elahe Khalouei, Penelope Longa, Markus Rabus, Sedighe Sajadian, Uffe Graae Jorgensen, Martin Dominik, Jean-Baptiste Kikwaya, Elena Mazzotta Epifani, Elisabetta Dotto, Prasanna Deshapriya, Pedro Hasselmann, Massimo Dall'Ora, Lyu Abe, Tristan Guillot, Djamel Mékarnia, Abdelkrim Agabi, Philippe Bendjoya, Olga Suarez, Amaury Triaud, Thomas Gasparetto, Maximillian N. Günther, Michael Kueppers, Bruno Merin, Joseph Chatelain, Edward Gomez, Helen Usher, Cai Stoddard-Jones, Matthew Bartnik, Michael Bellaver, Brenna Chetan, Emma Dugan, Tori Fallon, Jeremy Fedewa, Caitlyn Gerhard, Seth A. Jacobson, Shane Painter, David-Michael Peterson, Joseph E. Rodriguez, Cody Smith, Kirill V. Sokolovsky, Hannah Sullivan, Kate Townley, Sarah Watson, Levi Webb, Josep M. Trigo-Rodríguez, Josep M. Llenas, Ignacio Pérez-García, A. J. Castro-Tirado, Jean-Baptiste Vincent, Alessandra Migliorini, Monica Lazzarin, Fiorangela La Forgia, Fabio Ferrari, Tom Polakis, Brian Skiff
Figure caption: Evolution of the brightness of the Didymos system plus the ejecta from the Double Asteroid Redirection Test (DART) impact over time measured from several days before impact to approximately one month after. Different observatories are given their own symbol, and each observation is plotted with errorbars—though these are frequently smaller than the markers themselves. The dimming was more rapid at first and slowed over time. These brightness measurements were only corrected for heliocentric and geocentric distances, but we also plot an HG1G2 model (Muinonen et al. 2010) of the system's brightness using in situ derived values (H = 18.16, G1 = 0.84, G2 = 0.05; Hasselmann et al. 2023) as a black line for context. This indicates that some of the dimming is due to phase angle effects, but certainly not all. Only the Danish (squares) and Lowell 42″ (circles) have had mutual events removed from their nightly averages, which may move them slightly above contemporaneous observations. A pause in dimming at seven-to-eight days post impact (highlighted in Figure 2) and the time-dependence of the dimming makes ascertaining the bulk wavelength dependence of the dimming rates challenging.(The data used to create this figure are available.)