adsabs/AstroCLIMB huggingface dataset:
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: V701 Per and its potential birthplaces in three groups, each marked. Top left: the proper motions and 3σ uncertainties of IC 348 members (gray points and green shadow), walkaway star limit of 5 km s–1 (red circle), V701 Per (red square), and members of the three groups that are the potential birthplaces of V701 Per (blue, cyan, and orange symbols). Top right: R.A. vs. parallax. Middle left: the current position of V701 Per and other stars. Black vectors show the proper motion relative to IC 348 with the direction toward the past. A length of 0.1 represents a proper motion of 1 mas yr−1. The proper motion of a visual binary is represented by their individual proper motions. Middle right to bottom right: the trace to past positions relative to IC 348, indicating overlaps and possible ejections at −0.07, −0.23, and −0.45 Myr. The uncertainty cone of V701 Per corresponds to 3σ and that of other group members is 1σ. The past positions of group members are calculated via their individual proper motions, except 2MASS J03415745+3148365 in Group 3 (see Section 4.1.1 for details). The past positions of other IC 348 members are held constant with time, since these stars represent the bulk of IC 348 and IC 348 is used as the frame of reference.
Paper: Walkaway Star Candidates in IC 348 and Their Possible Birthplaces
Authors: Xingyu Zhou, Gregory J. Herczeg, Min Fang, Xiaolong Wang, Bin B. Ren
Figure caption: Past motions for LRL 170 (left) and LRL 70 (right), relative to IC 348 and with 1σ uncertainties. The position of IC 348 members (gray point) remains unchanged, since the trace-back proper motion is relative to the IC 348 frame of reference.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Comparison of the chemical abundance pattern in our two Ret II stars. Top: comparison to the PISN yields from Takahashi et al. (2018). Bottom: comparison to the metal-free CCSN (faint SNe, E51 = 1) yields from Nomoto et al. (2013). The color coding is the same as in Figure 7, and models of different masses are shown in grayscale (reported in solar masses).
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Chemical abundance patterns scaled to Fe for CEMP-no stars with known light-element enhancements in UFDs. These stars cover a range of metallicities with Car III 1120 being the most metal-poor at [Fe/H] = −3.9, Segue 1 7 at [Fe/H] = −3.6, Boo I 119 at [Fe/H] = −3.3, and Psc II 10694 at [Fe/H] = −2.6, similar to GDR3 0928 at [Fe/H] = −2.5.
Paper: GHOST Commissioning Science Results: Identifying a New Chemically Peculiar Star in Reticulum II
Authors: Christian R. Hayes, Kim A. Venn, Fletcher Waller, Jaclyn Jensen, Alan W. McConnachie, John Pazder, Federico Sestito, André Anthony, Gabriella Baker, John Bassett, Joao Bento, Trystyn Berg, Gregory Burley, Jurek Brzeski, Scott Case, Edward Chapin, Timothy Chin, Eric Chisholm, Vladimir Churilov, Adam Densmore, Ruben Diaz, Jennifer Dunn, Michael Edgar, Tony Farrell, Veronica Firpo, Joeleff Fitzsimmons, Juan Font-Serra, Javier Fuentes, Colin Ganton, Manuel Gomez-Jimenez, Tim Hardy, David Henderson, Alexis Hill, Brian Hoff, Michael Ireland, Venu Kalari, Neal Kelly, Urs Klauser, Yuriy Kondrat, Kathleen Labrie, Sam Lambert, Lance Luvaul, Jon Lawrence, Jordan Lothrop, G. Scott Macdonald, Slavko Mali, Steve Margheim, Richard McDermid, Helen McGregor, Bryan Miller, Felipe Miranda, Rolf Muller, Jon Nielsen, Ryan Norbury, Oliver Oberdorf, Naveen Pai, Gabriel Perez, Pablo Prado, Ian Price, Carlos Quiroz, Vladimir Reshetov, Gordon Robertson, Roque Ruiz-Carmona, Ricardo Salinas, Kim M. Sebo, Andrew Sheinis, Matthew Shetrone, Keith Shortridge, Katherine Silversides, Karleyne Silva, Chris Simpson, Greg Smith, Kei Szeto, Julia Tims, Eduardo Toro, Cristian Urrutia, Sudharshan Venkatesan, Lewis Waller, Ivan Wevers, Ramunas Wierzbicki, Marc White, Peter Young, Ross Zhelem
Figure caption: Residual abundances (using LTE) from a scaled solar r-process abundance pattern in HD 122563, GDR3 1760, and GDR3 0928, fit to the heavier neutron-capture elements (see the text for details).
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The Zernike moments vs. the n index for the MAD (top) and SANE simulations (bottom). From left to right, we increase the BH spin a = (−0.94, −0.5, 0.0, +0.5, +0.94). In each panel, we sum over all of the nonzero m indices for a given n splitting the positive and negative terms with the solid-magenta and dashed-green lines, respectively. Different simulations show distinct patterns in C  n  (as defined in Equation (15)) vs. n that can eventually be used to distinguish them from one another. In each panel, the subplot refers to the case with an extended value of ns, indicating that in most cases we do not need to consider n orders above 20.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The time-averaged phase map for the EB correlation for the MAD simulations (top row), the reconstructed phase map using the Zernike polynomials (middle row), and the MAD simulations with NFR (bottom row). To infer the phase map we adopt the M 1 method presented in Section 2.2.1 in which we first compute the time-averaged E and B modes and then compute the correlation phase using these averaged quantities. The Zernike expansion is truncated at n = 40 order. As the Zernike polynomials are defined on a unit circle, we have multiplied them to 8 to be similar to the original phase map from the GRMHD simulations.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The time-averaged phase map for the EB correlation for SANE simulations (top row), the reconstructed phase map using the Zernike polynomials (middle row), and for SANE simulations with NFR (bottom row). To infer the phase map we adopt the M 1 method presented in Section 2.2.1 in which we first compute the time-averaged E and B modes and then compute the correlation phase using these averaged quantities. The Zernike expansion is truncated at n = 40 order. As the Zernike polynomials are defined on a unit circle, we have multiplied them to 8 to be similar to the original phase map from the GRMHD simulations.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The Zernike moments vs. the absolute value of the m index for the MAD (top) and SANE (bottom) simulations. From left to right, we increase the BH spin in a = (−0.94, −0.5, 0.0, +0.5, +0.94). In each panel, we compute the summed C  nm  for all n indices that include the associated m index, splitting the positive and the negative terms with solid-magenta and dashed-green lines, respectively. Different simulations show different patterns in their C ∣m∣ (as defined in Equation (16)) vs. ∣m∣ that might be used to distinguish them from one another. In each panel, the subplot refers to the case with an extended value of ∣m∣s that again indicates we do not need to consider m orders above 20.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The time-averaged images of SANE simulations with different BH spins. From top to bottom, we present the total intensity (I), fractional linear polarization (P/I), and the Stokes Q parameter. As the system is controlled by turbulence, there is no clear handedness in the EVPAs.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The time-averaged phase map for the EB correlation in the MAD simulations from the GRMHD simulations of IHARM. To infer the phase map we follow the M 1 method presented in Section 2.2.1. It is clearly seen that the phase map is very similar to that of the MAD simulations from H-AMR simulations, which demonstrates that the observed patterns in the MAD simulations are robust and rather independent of initial conditions.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The time-averaged phase map for the EB correlation for the MAD and SANE simulations using the M 2 method presented in Section 2.2.2, where we first compute the EB correlation at every snapshot and then calculate the time-averaged phase map. Comparing the results with Figures 7 and 8, it can be seen that both maps are qualitatively similar.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The phase map for the EB-correlation function in the visibility space from the time-averaged GRMHD simulations using the EHT 2017 coverage for M87*. In the top (bottom) panel, we have used the MAD (SANE) simulations to create the synthetic data.
Paper: The EB Correlation in Resolved Polarized Images: Connections to the Astrophysics of Black Holes
Authors: Razieh Emami, Sheperd S. Doeleman, Maciek Wielgus, Dominic Chang, Koushik Chatterjee, Randall Smith, Matthew Liska, James F. Steiner, Angelo Ricarte, Ramesh Narayan, Grant Tremblay, Douglas Finkbeiner, Lars Hernquist, Chi-Kwan Chan, Lindy Blackburn, Ben S. Prather, Paul Tiede, Avery E. Broderick, Mark Vogelsberger, Charles Alcock, Freek Roelofs
Figure caption: The comparison between the real part of the EB correlation in the MAD simulations from the full numeric as well as the m-order cut. From top to bottom, we present the full numeric, the case with m cut = 2, m cut = 3, and m cut = 4, respectively.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: (Left): Rest-frame UVJ diagram used to classify galaxy populations. U − V and V − J colors are calculated by SED fitting. The solid orange lines represent the boundaries defined in Williams et al. (2009). The dark orange circles represent all MIRI-selected sources, and the green squares indicate unresolved galaxies that were excluded from the morphology analysis, as explained in Section 3.3.1, UVJ-selected quiescent galaxies are marked as open red circles. (Right): Stellar mass vs. SFRs plot for our samples. The symbols used in this panel are the same as in the left panel. The error bars for SFR are computed based on the Bayesian probability distribution of CIGALE. The blue shaded region indicates the ±0.4 dex range of the star formation main sequence at 1 < z < 1.5 derived by Whitaker et al. (2014).
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Same as Figure 5, but as a function of sSFR (left) and SFRIR/SFRUV (right). The error bars for the sSFR are computed based on the Bayesian probability distribution of CIGALE. The large blue and gray squares with error bars denote the median values and associated uncertainties (calculated using the normalized median absolute deviation with N − 1° of freedom) in each bin.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Postage stamps of the selected galaxies we used for the compactness analysis. Each column shows the galaxy centered in the F160W, F200W, F770W, and F1000W filters from left to right, with a size of 3.″2 × 3.″2. The stellar mass and SFR calculations are detailed in Section 3.2, and both values are corrected for the lensing magnification. The two white ellipses in the middle columns represent r in and r out, which are used to calculate the compactness. The lensing magnification factor (μ) for each galaxy, as calculated in Section 3.1, is also provided.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: A schematic view of our dust decomposition method. (Top left): an example SED from our galaxy sample at redshift 1.32 features the 3.3 μm PAH emission captured by the F770W filter. (Bottom left): dust decomposition using the observed F770W and observed F200W. The δ denotes the stellar flux density ratio between two filters. (Right): from top to bottom, the flux profile of the F200W filter (representing the stellar continuum), the F770W filter (capturing a mixture of stellar continuum and dust emission), and the extracted dust emission.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Distribution of the dust-to-stellar compactness ratio (c dust/c stellar) as a function of stellar mass (M *). The symbol colors represent measurements obtained from nonparametric morphology (blue) and galfit parametric morphology (gray). The subset of UVJ-selected quiescent galaxies are indicated by open red circles.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Histogram showing the distribution of the dust-to-stellar compactness ratio of our sample (blue for the ratio calculated by the nonparametric approach, and gray for the parametric approach). The median values derived from the two techniques (dashed blue and gray lines, respectively) are shown. The dashed red line corresponds to c dust/c stellar = 1, which suggests a coherent distribution of dust and stellar compactness.
Paper: A Multiwavelength Investigation of Dust and Stellar Mass Distributions in Galaxies: Insights from High-resolution JWST Imaging
Authors: Zhaoran Liu, Takahiro Morishita, Tadayuki Kodama
Figure caption: Comparison of the flux-based compactness c derived by nonparametric method (horizontal axis) and parametric method based on galfit best-fit model (vertical axis). The symbol color represents dust (red) and stellar (blue) components.
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Diagram showing the trends of quenching since infall (i.e., a continuous increase of Dn4000 with infall time proxy) across redshift and luminosity bins. In all panels, different colors indicate different redshift bins: black, all z (0.26 < z < 1.13); blue, low-z (0.26 < z < 0.53); and red, high-z (0.53 < z < 1.13). Different panels show different luminosity bins: left, all (faint+bright); middle, faint (sub-L*; L  i /L* < 1); and right, bright (super-L*; L  i /L*  > 1). The diamonds with error bars indicate the bootstrapped mean Dn4000 and associated standard deviation of sample galaxies in each infall zone, which also accounts for Dn4000 measurement uncertainties. The formats are the same as in Figure 4. By comparing the blue and red points in each panel, it is clearly shown that low-z galaxies have a larger mean Dn4000 than their high-z counterparts at a fixed infall zone (fixed environmental effect), regardless of luminosity. This is due to the redshift dependence of the star-forming main sequence (Section 4.3). Also, by comparing the middle and right panels for the same colored points, it is shown that bright galaxies have a larger mean Dn4000 than their faint counterparts at a fixed infall zone across redshift, which is due to the mass-dependent quenching effect (Section 4.2). Thus, by dividing sample galaxies into specific redshift and luminosity bins, this figure clearly shows that environmental quenching does exist and impact galaxies since their infall into cluster, at all redshifts and luminosities, yet the exact age (Dn4000) depends on both redshift and luminosity at a fixed environment (infall zone; Section 4.3).
Paper: A Gradual Decline of Star Formation since Cluster Infall: New Kinematic Insights into Environmental Quenching at 0.3 < z < 1.1
Authors: Keunho J. Kim, Matthew B. Bayliss, Allison G. Noble, Gourav Khullar, Ethan Cronk, Joshua Roberson, Behzad Ansarinejad, Lindsey E. Bleem, Benjamin Floyd, Sebastian Grandis, Guillaume Mahler, Michael A. McDonald, Christian L. Reichardt, Alexandro Saro, Keren Sharon, Taweewat Somboonpanyakul, Veronica Strazzullo
Figure caption: Diagram showing that environment and luminosity are the two main drivers of galaxy quenching, where the environmental effect is kinematically measured from the phase space of cluster galaxies (Figure 3 and Section 3.2). The color indicates the mean Dn4000 strength of the nearest 100 sample galaxies at a given luminosity and infall proxy location with a grid spacing of 0.025 L  i /L* and 0.05 ﹩\mathrm{log}[({r}_{\mathrm{proj}}/{r}_{500})\,\times \,({\rm{\Delta }}v/{\sigma }_{\mathrm{cl}})]﹩. The white dashed lines are the contours of several Dn4000 values tracing the mean Dn4000 distributions of sample galaxies. It is clear that the mean Dn4000 typically increases with infall proxy for any luminosity, which suggests that environmental quenching affects galaxies regardless of luminosity (Section 4.2).
Paper: Late-time Hubble Space Telescope Observations of AT 2018cow. I. Further Constraints on the Fading Prompt Emission and Thermal Properties 50–60 days Post-discovery
Authors: Yuyang Chen, Maria R. Drout, Anthony L. Piro, Charles D. Kilpatrick, Ryan J. Foley, César Rojas-Bravo, Kirsty Taggart, Matthew R. Siebert, M. R. Magee
Figure caption: Final multiband UVOIR light curves of AT 2018cow used in this study. The HST photometry is shown as stars, and the HST epochs are marked with dashed lines. Magnitudes are shifted for visual clarity. The UVOT photometry is included only if they are above the 3σ detection level. The photometry shown is available as data behind the Figure.(The data used to create this figure are available.)