adsabs/AstroCLIMB huggingface dataset:
Paper: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds (DAVOS): Properties of Variability-selected AGN in the Dark Energy Survey Deep Fields
Authors: Yichen Liu, Colin J. Burke, Diego Miura, Xin Liu, Qian Yang, Priyamvada Natarajan, Charlotte A. Ward
Figure caption: Demonstration of absolute flux calibration of our spectra. Each data point is a single DES-SN variable AGN with one spectrum from SDSS and at least one from another source. The bolometric luminosity from SDSS spectral continua is plotted against the bolometric luminosity from other spectra (see Table 1 for the data source list) before (left) and after (right) performing absolute flux calibration to the W. G. Hartley et al. (2022) photometry. Although AGN variability can contribute to some of the scatter across surveys, our resulting flux-calibrated spectra appear to be more consistent, as evidenced by the significantly reduced scatter. The right panel only includes those with successful flux calibration.
Paper: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds (DAVOS): Properties of Variability-selected AGN in the Dark Energy Survey Deep Fields
Authors: Yichen Liu, Colin J. Burke, Diego Miura, Xin Liu, Qian Yang, Priyamvada Natarajan, Charlotte A. Ward
Figure caption: Host galaxy stellar mass vs. redshift for DES-SN variable AGNs with stellar mass estimates from broadband SED fitting using CIGALE. Gray circles: unreliable stellar mass (﹩{\chi }_{\nu }^{2}\gt 5﹩ or star formation excess <1.2). Colored circle symbols with black border: reliable stellar mass calculated from spectroscopic redshift. Colored circle symbols without a black border: reliable stellar mass calculated from the photometric redshift. Gray curve: theoretical detection limit.
Paper: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds (DAVOS): Properties of Variability-selected AGN in the Dark Energy Survey Deep Fields
Authors: Yichen Liu, Colin J. Burke, Diego Miura, Xin Liu, Qian Yang, Priyamvada Natarajan, Charlotte A. Ward
Figure caption: Comparison of the photometric redshifts from C. J. Burke et al. (2022) and the spectroscopic redshifts obtained in this work. The photometric redshifts are determined using the approach outlined in Q. Yang et al. (2017). The root mean square error values of all the sources and zspec < 1.5 sources are displayed in the upper left corner of the figure panel. A gray y = x line is included for reference.
Paper: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds (DAVOS): Properties of Variability-selected AGN in the Dark Energy Survey Deep Fields
Authors: Yichen Liu, Colin J. Burke, Diego Miura, Xin Liu, Qian Yang, Priyamvada Natarajan, Charlotte A. Ward
Figure caption: Updated redshifts in this work from SIMBAD, OzDES, and DESI vs. original redshifts from C. J. Burke et al. (2022). The redshifts updated from photometric to spectroscopic are labeled using orange triangle symbols, and the unchanged or updated photometric and spectroscopic redshifts are shown as gray crosses and blue dots, respectively. A number of previous catastrophically underestimated photometric redshifts have been updated
Paper: Dwarf Active Galactic Nuclei from Variability for the Origins of Seeds (DAVOS): Properties of Variability-selected AGN in the Dark Energy Survey Deep Fields
Authors: Yichen Liu, Colin J. Burke, Diego Miura, Xin Liu, Qian Yang, Priyamvada Natarajan, Charlotte A. Ward
Figure caption: The bolometric AGN luminosity, estimated as 10 times the 2–10 keV X-ray luminosity (following F. Duras et al. 2020), is plotted against our updated redshifts. The distributions of redshift and bolometric luminosity are displayed in the upper and right panels, respectively.
Paper: α-MC: Self-consistent α-enhanced Stellar Population Models Covering a Wide Range of Age, Metallicity, and Wavelength
Authors: Minjung Park, Charlie Conroy, Benjamin D. Johnson, Joel Leja, Aaron Dotter, Phillip A. Cargile
Figure caption: Comparison between α-enhanced (red) and solar-scaled (blue) SSP spectra with different ages at a fixed total metallicity. The ratios between the two spectra are given in Figure 13.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Blue lines show the nVF time series from simulations described in Table 1, orange and green lines represent fits using the sigmoid function, S(t), defined according to Equation (23). Red dots represent where S(t) = 5% and red crosses where S(t) = 95%. The fit was used to quantify the time lag shown in Figure 6.
Paper: Time-dependent Turbulent Electron Acceleration and Transport in Solar Flares
Authors: Luiz A. C. A. Schiavo, Natasha L. S. Jeffrey, Gert J. J. Botha, James A. McLaughlin
Figure caption: Exponential damping timescale extracted from Figure 13, for cases 19–22 in Table 1.
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: UMAP of final features of the DESA model. All points are in gray. Colored points correspond to samples with Prot < 30 days in one of the latest period catalogs (A. McQuillan et al. 2014; A. R. G. Santos et al. 2019, 2021; T. Reinhold et al. 2023; I. Kamai & H. B. Perets 2025a).
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Result of few-shot learning of a linear regression model. The two upper panels show the predicted labels vs. the true labels. The lower left panel shows the true CMD. The lower right panel shows the predicted CMD. Colors on the lower right panel correspond to the MAE.
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Ablation study results. Upper panel: different attention mechanisms. Lower panel: different uses of A—with and without AT for one of the projections (refer to Section 3.2 for details).
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: UMAP of the final features of different models. In the upper panel, color represents luminosity. In the lower panel, the color represents CMD classes from D. Godoy-Rivera et al. (2025).
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Histograms of UMAP distance of stars with multiple spectra. The legend shows the model name and the mean and standard deviation of the distribution in parentheses.
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Upper panel—results of the spectra encoder on LASP labels. Lower panel—results on the labels from APOGEE. The purple and gray lines represent prediction intervals of 80% and 50%.
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Example of the preprocessing steps for Kepler Light curve. The upper row shows the raw light curve normalized by absolute magnitude (left) and mean and standard deviation (right). The lower row shows the ACF (left) and FFT (right).
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Example of the preprocessing steps for LAMOST spectra. The left column is the blue range, and the right column is the red range.
Paper: Machine Learning Inference of Stellar Properties Using Integrated Photometric and Spectroscopic Data
Authors: Ilay Kamai, Alex M. Bronstein, Hagai B. Perets
Figure caption: Results of the light-curve encoder. Gray and purple lines represent 50% and 80% intervals.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: TPR (or recall) as a function of magnitude relative to 5σ limiting magnitude. Black and blue lines show TPR with score > 0.35 and > 0.70, respectively. In our analysis, we adopt the threshold score of 0.70 (blue).
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Volume density profiles, centered on the stellar COM, for the N-body merger remnant models of NGC 1600, NGC 6166, and IC 1101, using binned SPH profiles. The inset plots use spherical shells centered on the SMBH to show the formation of the nucleus. Columns from left to right are for GW recoil kicks of vk/vesc = 0.1, 0.3, and 0.5, respectively. tk is the time when the N-body simulation is paused for the SMBH merger and the GW recoil kick is given; “An” and “Pn” indicate the nth apocenter and pericenter passages of the kicked SMBH; “Br” indicates that the SMBH has settled into Brownian motion. Increases in central density are seen in Brownian motion in almost all cases, with varying degrees of core formation outside them.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: (Top) Survey footprints of our observations in the equatorial coordinate. The color represents the total exposure time for each part of the sky. (Bottom) Distribution of the detected glints. The blue points show all the glints, while the orange points show those associated with cataloged objects. Note that the coordinates of the glints are given as viewed from the Kiso observatory.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Volume (top three rows) and surface density (bottom three rows) profiles when the SMBH remnant has settled to Brownian motion for A2147-BCG, 4C+74.13, and A2261-BCG. Columns from left to right are for kicks with a vk/vesc of 0.1, 0.3, and 0.5, respectively. Profiles labeled “nucleus” indicate those for particles that were within the influence radius of the SMBH at first apocenter (blue), and all other particles as “remainder” (orange). The combined profiles are labeled “total” (green dotted).
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: NSC relations: NSC mass–radius relation (top left); SMBH mass relation with NSC radius (top right); NSC mass (bottom left); and velocity dispersion (bottom right). Blue points are observations from B. T. Dullo (2019), R. Schödel et al. (2014), A. Feldmeier et al. (2014), A. W. Graham & L. R. Spitler (2009), A. C. Seth et al. (2010), and M. Den Brok et al. (2015), red points are simulations from this study, and green points are refitted observations from B. T. Dullo (2019).
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: Trajectory of the SMBH remnant (recentered on the COM) from the time the GW kick recoil is applied. Rows (from top to bottom) correspond to galaxies NGC 1600, A2147-BCG, NGC 6166, 4C+74.13, A2261-BCG, and IC 1101, respectively. Columns (from left to right) show results for a vk/vesc of 0.1, 0.3, and 0.5, respectively. In contrast to the higher speed kicks in Paper I, the SMBH in general makes just one or two passages through the nucleus before being damped to Brownian motion.
Paper: Second-timescale Glints from Satellites and Space Debris Detected with Tomo-e Gozen
Authors: Masaomi Tanaka, Ichiro Takahashi, Naoki Yoshida, Naonori Ueda, Akisato Kimura, Kazuma Mitsuda, Hirofumi Noda, Shigeyuki Sako, Noriaki Arima, Mitsuru Kokubo, Tomoki Morokuma, Yuu Niino, Nozomu Tominaga, Kenzo Kinugasa, Naoto Kobayashi, Sohei Kondo, Yuki Mori, Ryou Ohsawa, Hidenori Takahashi, Satoshi Takita
Figure caption: Cumulative areal exposure (deg2 hr) of our survey as a function of 5σ limiting magnitude.
Paper: Black Hole Dragging: A New Mechanism for Forming Nuclear Star Clusters in Giant Elliptical Galaxies
Authors: Nader Khonji, Alessia Gualandris, Justin I. Read, Walter Dehnen
Figure caption: As for Figure 13, but for A2147-BCG, 4C+74.13, and A2261-BCG
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Fast EUV wave, CME, and associated SEPs for E4 on 2014 March 28. (a1)–(a4) AIA 211 Å running-difference images showing a large-scale EUV wave associated with a filament eruption. (b1)–(b4) LASCO C2 (2–6 R⊙) and STEREO-A COR2 (2–15 R⊙) images depicting the CME and shock. FR is the flux rope. CME (E3) is the preceding CME from the earlier eruption E3. (c1) TD intensity plot along the slit (marked in panel (b3)) using STEREO-A COR2 white-light images. (c2) Dynamic radio spectrum in 0.2–16 MHz from STEREO-A/WAVES. “F” and “H” indicate the fundamental and harmonic bands of the Type II burst, respectively. (c3) Electron flux (12 s cadence) measured by Wind/3DP at different energies ranging from 28 to 523 keV.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: Quasiperiodic Type III bursts during breakout reconnection near the inner and outer nulls. (a)–(d) The wavelet analysis of the radio flux density from RSTN Sagamore Hill observatory for E1. Left: (a) radio flux density (410 MHz) in solar flux units (1 sfu = 10−22 W m−2 Hz−1) vs. time (UT). (b) The detrended light curve after subtracting the red trend shown in (a) from the original light curve. (c) Wavelet power spectrum of the detrended signal. Red contours outline the 95% significance level. (d) Global wavelet power spectrum. The dashed line is the 95% global confidence level. Right and bottom left: (a)–(d) the same plots for E2 and E3.
Paper: Solar Eruption Onset and Particle Acceleration in Nested-null Topologies
Authors: Pankaj Kumar, Judith T. Karpen, Peter F. Wyper, David Lario, Spiro K. Antiochos, C. Richard DeVore
Figure caption: VDA for the onset of SEPs for E1 on 2014 March 29. Inverse beta vs onset time plot for electrons (26–307 keV) detected by Wind/3DP at 1 au. The red dashed lines indicate the onset and end times of decimetric–metric Type III bursts, while the blue line marks the onset time of the metric Type II radio burst.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Continuum and line emission images matching the wavelength range of the F1000W MIRI filter constructed from MRS observations. MIRI (first column), “MIRI-like” (second column), continuum (third column), and line (fourth column) images of the central 1 kpc of ESO137-G0134 (first row), MCG-05-23-016 (second row), NGC 3081 (third row), NGC 5506 (fourth row), NGC 5728 (fifth row), and NGC 7172 (sixth row). Contours (white lines) increase in steps of [1, 5, 10, 30, 50, 70]% from the peak flux. The contour at a 10% level (thick white line) from the peak flux is shown for reference. The orientations of the radio jet (black dashed line), dust lane (blue dotted line), and stellar bar (red line; only for NGC 5728) axes are shown. The beam (yellow circle) of the observations is shown.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: MIR spectra of the AGN in our sample. The spectra of the extended emission without the core (>39 pc; red) and only the core (≤39 pc; blue) are shown. The black solid line shows the extrapolated continuum used to determine the silicate feature, ﹩{\tau }_{9.7\mu {\rm{m}}}=-\mathrm{ln}({F}_{9.7\mu {\rm{m}}}/{F}_{{\rm{c}}})﹩, from the extended MIR emission without the core.
Paper: Dynamical Properties and Velocity Dispersion–Mass Relation of z ∼ 1 Galaxy Clusters from the GOGREEN and GCLASS Surveys
Authors: Shrouk Abdulshafy, Mohamed H. Abdullah, Gillian Wilson, Michael L. Balogh, Raouf H. Mabrouk
Figure caption: Spectroscopic incompleteness test for two representative clusters: SpARCS0034 and SpARCS1613. Top panels show the weight functions in projected distance–stellar mass plane (rp–﹩{\mathrm{log}}{{M}}_{* }﹩), derived as the inverse of the completeness function (see Appendix). Bottom panels compare the measured velocity dispersion from the incomplete sample (σincomp, bottom left) and the weighted-corrected sample (σweighted, bottom right) against the true dispersion (σtrue) from fully sampled simulated clusters. Gray points represent the mean values across 500 Monte Carlo realizations, each randomly sampled based on the completeness function. The error bars show the standard deviation across those trials. Magenta points show the binned mean of the gray points with 1σ error bar; the dashed black line marks the one-to-one relation. While σincomp remains consistent with the true value, σweighted shows a slight systematic bias.
Paper: Dynamical Properties and Velocity Dispersion–Mass Relation of z ∼ 1 Galaxy Clusters from the GOGREEN and GCLASS Surveys
Authors: Shrouk Abdulshafy, Mohamed H. Abdullah, Gillian Wilson, Michael L. Balogh, Raouf H. Mabrouk
Figure caption: Velocity dispersion σ200 vs. virial mass M200. Left: the distribution of the cluster sample in the σ200–M200 plane, where red and blue points represent the results from our work and Biv21, respectively. Note that for Biv21, the σ values correspond to σlos (the velocity dispersion for all members), since they did not provide σ200 values. Right: the red and blue solid lines represent the best fit at z = 1 for our work and Biv21, respectively. For comparison, we include relations from N-body dark matter simulations, specifically those derived by A. E. Evrard et al. (2008; dashed black) and E. Munari et al. (2013; dashed cyan), as well as from simulations incorporating baryonic effects, including E. Munari et al. (2013)-AGN (dashed violet) and T. J. Armitage et al. (2018)-Eagle simulations (dashed green). The three shaded red areas indicate 1σ, 2σ, and 3σ uncertainties for our best-fit line, and the blue shaded area is 1σ for Biv21.
Paper: Dynamical Properties and Velocity Dispersion–Mass Relation of z ∼ 1 Galaxy Clusters from the GOGREEN and GCLASS Surveys
Authors: Shrouk Abdulshafy, Mohamed H. Abdullah, Gillian Wilson, Michael L. Balogh, Raouf H. Mabrouk
Figure caption: A comparison that shows our results (the red triangles on the solid black line, representing 1:1 relation) in contrast with those from Biv16 (cyan squares) and Biv21 (blue dots) for M200. The bottom panel presents the scatter between the masses reported by Biv16 and Biv21 and our results, defined as ﹩{\rm{\Delta }}{\rm{log}}{{M}}_{200}={\rm{log}}{{M}}_{200}({\rm{Biviano}})-{\rm{log}}{{M}}_{200}({\rm{ours}})﹩.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: SEDs of the continuum emission within the MIRI imaging filters of the AGN in our sample. The SEDs of the nucleus (<75 pc; blue dotted line with circles), the full FOV including the nucleus (<450 pc; gray solid line with squares), and without including the nucleus (75–450 pc; red dashed line with open squares) are shown. The best fit of the blackbody function (black line) to the continuum extended emission in the 10–25 μm wavelength range, excluding the nucleus (r < 75 pc; red dashed line) and the first interquartile (25%–75%; gray shadowed area) are displayed. In each panel, we show the characteristic dust temperature, Td, dust mass, Md, and emissivity index, β.
Paper: GATOS. VIII. On the Physical Origin of the Extended Mid-infrared Emission in Active Galactic Nuclei
Authors: Enrique Lopez-Rodriguez, Cristina Ramos Almeida, Miguel Pereira-Santaella, Ismael García-Bernete, Robert Nikutta, Almudena Alonso-Herrero, Anelise Audibert, Enrica Bellocchi, Andrew Bunker, Steph Campbell, Françoise Combes, Richard Davies, Tanio Diaz-Santos, Lindsay Fuller, Poshak Gandhi, Santiago García-Burillo, Omaira González-Martín, Erin K. S. Hicks, Sebastian Hönig, Kohei Ichikawa, Masatoshi Imanishi, Takuma Izumi, Alvaro Labiano, Nancy A. Levenson, Christopher Packham, David Rosario, Dimitra Rigopoulou, Daniel Rouan, Taro Shimizu, Marko Stalevski, Martin Ward, Lulu Zhang, Claudio Ricci, Donaji Esparza-Arredondo, Begoña García-Lorenzo
Figure caption: Normalized correlation coefficients between line emission and the total MIR and continuum emission images. For all galaxies with detected extended MIR emission, we show the mean and standard deviation (shadowed regions) of the normalized correlation coefficients, ρ, between the line and total MIR emission (solid line), and line and continuum (dashed line) emission in the F1000W (left), F1500W (middle), and F2100W (right) filters. The ranges for strong, moderate, and uncorrelated coefficients are displayed. The correlations for each galaxy and filter are shown in Appendix D (Figure 14).