adsabs/AstroCLIMB huggingface dataset:
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: J1359+5726 (AGBT/19A-301): The archival 21 cm observations of J1359+5726 have insufficient S/N to characterize the H I properties. The upper limit on S H I  corresponds to a low gas fraction (μ < 0.25).
Paper: CLASSY. XI. Tracing Neutral Gas Properties Using UV Absorption Lines and 21 cm Observations 
Authors: Kaelee S. Parker, Danielle A. Berg, Simon Gazagnes, John Chisholm, Bethan L. James, Matthew Hayes, Timothy Heckman, Alaina Henry, Michelle A. Berg, Karla Z. Arellano-Córdova, Xinfeng Xu, Dawn K. Erb, Crystal L. Martin, Weida Hu, Evan D. Skillman, Kristen B. W. McQuinn, Zuyi Chen, Dan P. Stark
Figure caption: J1148+2546 (AGBT/19A-301): J1148+2546 has a broad 21 cm profile (FWHM ∼170 km s−1), in particular as compared with other CLASSY galaxies of a similar mass (M ⋆ ∼ 108 M ⊙).
Paper: Visual Orbits of Wolf–Rayet Stars. I. The Orbit of the Dust-producing Wolf–Rayet Binary WR 137 Measured with the CHARA Array
Authors: Noel D. Richardson, Gail H. Schaefer, Jan J. Eldridge, Rebecca Spejcher, Amanda Holdsworth, Ryan M. Lau, John D. Monnier, Anthony F. J. Moffat, Gerd Weigelt, Peredur M. Williams, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: The orbital solution for the CHARA measurements presented in this analysis along with the measurements of the W-R star’s radial velocities published by L. Lefèvre et al. (2005). For the visual orbit, the model is shown in blue with the measurements shown as black dots. The red ellipses show the measurement errors of the interferometry (typically 10–50 μas). We have noted the year for observations with the CHARA Array including CLIMB (2013) and the MIRC-X combiner (2019–2023), with the MYSTIC observations taken simultaneously blending in with the MIRC-X observations. The IOTA observations were at a similar phase as our 2019 observations, which are shown with their larger error ellipses. The visual orbit shows the path of the WC star around the O star. We used the data from L. Lefèvre et al. (2005) for the radial velocities, who did not include formal errors on the points but rather stated that the error for each measurement was σ ∼ 5–10 km s−1. We also show the potential orbital solutions in gray with the adopted solution in blue. Note that the uncertainty in the visual orbit is almost negligible, while work remains to improve upon the spectroscopic orbit.
Paper: Visual Orbits of Wolf–Rayet Stars. I. The Orbit of the Dust-producing Wolf–Rayet Binary WR 137 Measured with the CHARA Array
Authors: Noel D. Richardson, Gail H. Schaefer, Jan J. Eldridge, Rebecca Spejcher, Amanda Holdsworth, Ryan M. Lau, John D. Monnier, Anthony F. J. Moffat, Gerd Weigelt, Peredur M. Williams, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: Different aspects of evolution of the WR 137 system are shown in these three panels. The blue (W-R star) and red (O star) thick lines represent the model with the best matching initial parameters, with thinner lines representing models that are within the 1σ uncertainties in initial mass, initial mass ratio, initial period, and initial metallicity. The mean model is shown as a dashed line, while the mode model is shown as a thick line. In the left panel we show the Hertzsprung–Russell diagram for the past and future evolution of the W-R star. In the middle panel we show the primary radius in light/dark blue and the orbital separation in yellow/red. In the right panel we show the mass of the primary in light/dark blue and the mass of the secondary in yellow/red.
Paper: Visual Orbits of Wolf–Rayet Stars. I. The Orbit of the Dust-producing Wolf–Rayet Binary WR 137 Measured with the CHARA Array
Authors: Noel D. Richardson, Gail H. Schaefer, Jan J. Eldridge, Rebecca Spejcher, Amanda Holdsworth, Ryan M. Lau, John D. Monnier, Anthony F. J. Moffat, Gerd Weigelt, Peredur M. Williams, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: The recent infrared light curve of WR 137 from M. J. Peatt et al. (2023) is shown for the H- and K-bands as + symbols, shifted to △mag being around 0 for the times prior to the current dust formation episode (2020–late 2021). The blue/red circles represent the incoherent flux fitted in the CHARA measurements in the H/K-band. In the bottom panel, we show the ratio of the WR and O star fluxes, which are nearly constant within our errors.
Paper: Visual Orbits of Wolf–Rayet Stars. I. The Orbit of the Dust-producing Wolf–Rayet Binary WR 137 Measured with the CHARA Array
Authors: Noel D. Richardson, Gail H. Schaefer, Jan J. Eldridge, Rebecca Spejcher, Amanda Holdsworth, Ryan M. Lau, John D. Monnier, Anthony F. J. Moffat, Gerd Weigelt, Peredur M. Williams, Stefan Kraus, Jean-Baptiste Le Bouquin, Narsireddy Anugu, Sorabh Chhabra, Isabelle Codron, Jacob Ennis, Tyler Gardner, Mayra Gutierrez, Noura Ibrahim, Aaron Labdon, Cyprien Lanthermann, Benjamin R. Setterholm
Figure caption: A corner plot showing the interdependencies of fitted parameters in the combined visual and spectroscopic orbital fit.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Example images produced with the standard pipeline, and following two different background removal methods, as described in Section 2.2. The image median (in counts/second/pixel) are given in the bottom-left of each panel. Left: the FLS6 image from the standard pipeline. Middle: the FLS6 image where we have subtracted a median background constructed from all six FLS fields, with the sources masked out. Right: the FLS6 image with super-background subtraction (S. Alberts et al. 2024; P. G. Pérez-González et al. 2024).
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: An example of our MIRI images (for the FLS6 field) highlighting the number of sources clearly detected within the imager’s FOV of only 2.3 arcmin2. The angular resolution is also illustrated in the zoomed-in insets, both measuring 9″ × 9″, where we see both resolved morphology as illustrated by the detected spiral structure (top inset) as well as resolved closely spaced sources (that would have been blended in the Spitzer IRAC images, middle inset). The 2″ scale bars are comparable to IRAC channel 3 FWHM, which is 1.″88.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Left: the combined integral number counts with Poisson errors along with the counts for our individual eight fields. The field-to-field variation is roughly a factor of 2—well above the Poisson errors on the combined counts. The vertical dashed line is our 5σ limit. Lastly, we overlay the IRAC channel 3 counts from M. L. N. Ashby et al. (2009). These do not have the stars removed, which explains the difference between the counts at the bright end. Right: our integral number counts for our eight fields (orange symbols), with the Poisson and field-to-field variation uncertainties added in quadrature. We overlay for comparison both the published CEERS counts (G. Yang et al. 2023, blue crosses, include only Poisson error) and the SMILES counts (M. A. Stone et al. 2024, open green circles, include only Poisson error), as well as model predictions MIRI F560W counts from W. I. Cowley et al. (2018) (black curves) where the dotted–dashed curve is their fiducial model and the upper (dashed) one is the same but with evolving supernovae feedback (“EVOLFB”). We also overlay the 5σ limit as a vertical dashed line.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Noise map for the FLS1 field. Produced by computing the standard deviation of the FLS1 image inside a 3 × 3 pixel square centered on each pixel. The science image used in producing the noise map was first multiplied by the field’s segmentation map, removing the sources. We then applied a mask, shown here in orange, that removes edges and residual stripes as additional sources of noise. After both steps, we produced the noise map. A thin orange line on the color bar indicates the median value of the pixels in the noise map.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Source completeness for our images. The x-axis is trimmed to show detail. We overlay, as thin orange lines, an arbitrary sample of the computed completeness curves in order to show their spread. The vertical dotted line shows the 5σ depths of the images as determined by the empty apertures method, detailed in Section 2.4.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: The COSMOS1 field with all COSMOS2020 Classic catalog (J. R. Weaver et al. 2022a) sources overlaid as the open green circles. The COSMOS2020 sources, which have IRAC channel 3 (5.8 μm) detections, are shown as filled green triangles. The open orange diamonds are all our MIRI-detected sources in this field. Note that we have greater than three times more MIRI 5.6 μm m detections in the field relative to the prior Spitzer IRAC 5.8 μm detections.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Photometry cross check for the matched sources with the available IRAC channel 3 measurements applying an SNR > 1 cut on the IRAC channel 3 data, leaving us with 119 sources. The dashed diagonal line is the 1:1 line. The vertical dashed line represents the 3σ IRAC channel 3 limit (J. R. Weaver et al. 2022a). The quoted median offset is computed for the SNR > 3 sources.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Comparison of the position centroids of the 582 matched sources between MIRI and the COSMOS2020. The histograms (top and right) represent the offsets in both fields combined, with the mean absolute deviation (MAD) (calculated as the mean of ∣ΔR.A.∣ and ∣Δdec∣., respectively) labeled.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: Representative examples of sources we flagged as “fake,” see Section 3.4. The stripe in the left-hand panel is due to the mask around the Lyot coronograph. See the text for further details regarding fake source flagging.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: A comparison between the flux distributions of our MIRI sources that are matched to COSMOS2020 sources vs. those that are unmatched.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: The 16 × 16 pixel source model used in the Monte Carlo simulations to determine source completeness. The FWHM of the best-fit Gaussian is 0.″341 in the x-direction and 0.″330 in the y-direction.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: The upper panel depicts the 7 day binned γ-ray light curve of PKS 0805-07, integrated over the energy range of 0.1–100 GeV [flux (E > 100 MeV)] in units of  10−6 photons cm−2 s−1 from MJD 54684 to 60264. The lower panel showcases the corresponding values of the spectral index for the source during the same period. The red horizontal lines in the upper and lower panels represent the flux and index reported in the 4FGL catalog, respectively. The shaded regions represent the HOPs, and HOP 8 is designated as “active state.” The different colors representing HOPs are solely for demarcation purposes.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: We compare the 5σ mag limit of our images (in red) with the izYJHK+IRAC 5σ mag limits for the COSMOS2020 catalog (in gray), based on J. R. Weaver et al. (2022a). We suggest two potential explanations for the MIRI detections that are not in the COSMOS catalog: either a low-mass intermediate (z ∼ 1) redshift galaxy or a galaxy closer to M * at z ∼ 3 or beyond with high dust content. See Section 4.4 for more details on the models.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: Correlation plot between index and flux in 7 day binned light curve. The filled yellow circles represent the individual flux-index pairs, and the filled black circles represent the flux-index pairs based on the BB analysis. Flux is measured in units of 10−6 photons cm−2 s−1.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: 3 day binned γ-ray light curve of PKS 0805-07 fitted with the SOE function defined in Equation (1). Yellow strips denote the peak time (MJD) of the significant peaks, as mentioned in Table 2. The horizontal red line denotes the baseline flux. Flux is measured in units of in units of 10−6 photons cm−2 s−1.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: 3.″3 × 3.″3 cutouts of the 31 sources detected in MIRI 5.6 μm but are not present in the COSMOS2020 Classic catalog. The red contours represent the 2σ and 3σ levels from the COSMOS IRAC channel 1 image from M. Annunziatella et al. (2023), with an applied Gaussian blur (σ = 0.8). We label each source with our catalog ID and its MIRI 5.6 μm flux.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: Normalized histogram of the γ-ray light curve. Upper panel: normalized histogram fitted using the Gaussian function. Lower panel: normalized histogram fitted using the log-normal function. Flux is measured in units of  10−6 photons cm−2 s−1.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: The redshift distribution of our COSMOS2020-matched MIRI 5.6 μm sources. These are LEPHARE redshifts from the classic COSMOS2020 catalog.
Paper: Halfway to the Peak: The JWST MIRI 5.6 μm Number Counts and Source Population
Authors: Leonid Sajkov, Anna Sajina, Alexandra Pope, Stacey Alberts, Lee Armus, Duncan Farrah, Jamie Lin, Danilo Marchesini, Jed McKinney, Sylvain Veilleux, Lin Yan, Jason Young
Figure caption: The stellar mass vs. SFR relation for the same sources presented in Figure 12. The overlaid lines are the main-sequence relations at the indicated redshifts based on M. P. Koprowski et al. (2024).
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: Multiwavelength light curves of PKS 0805-07 obtained using Fermi-LAT, Swift-XRT, and UVOT observations. The observations spanned the period from MJD 54684 to 60264. The top panel represents the 3 day binned γ-ray light curve (flux is measured in units of 10−6 photons cm−2 s−1), and the second, third, and fourth panels depict the X-ray, UV, and optical light curves. Colored vertical stripes indicate the regions where broadband spectral modeling is performed. The γ-ray light curve with simultaneous X-ray and optical/UV data is zoomed in and is shown at the top of the plot, with arrows indicating their location in the multiwavelength plot.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: MaNGA SED fits on (a) quiescent, (b) star-forming, and (c) AGN galaxies. The gray lines are the total SED fit to broadband photometry, the green lines are the estimated AGN component. The fuchsia points are the GALEX NUV and FUV and the LS grz bands (from left to right). The red points are the four WISE magnitudes: W1, W2, W3, and W4. Each panel is labeled by its MaNGA identifier plate-IFU. Only the galaxy dominated by the AGN component in mid-IR demonstrates an increase in W2 flux, therefore contributing to a redder W1 − W2 color.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Observed W2 variance across all epochs (Equation (8)) vs. the expected W2 variance across all epochs calculated from within-epoch variances (Equation (10)) for MaNGA galaxies. Galaxies in red are defined to be “variable in the mid-IR” in Section 2.4.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: The broadband SED of PKS 0805-07 acquired during the flux states S1 (on the top left panel), Q1 (on the top right panel), S2 (on the bottom left panel), and S3 (on the bottom right panel). The flux points denoted by open diamonds correspond to Swift-UVOT, filled circles correspond to Swift-XRT, and filled squares correspond to Fermi-LAT. The solid red curve illustrates the combined best-fit synchrotron, SSC, and EC spectra.
Paper: Insights into the Long-term Flaring Events of Blazar PKS 0805-07: A Multiwavelength Analysis Over the Period of 2009–2023
Authors: Sikandar Akbar, Zahir Shah, Ranjeev Misra, Naseer Iqbal
Figure caption: Variation of F var with different time binning of γ-ray light curve.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Light curves of galaxies that are variable in the mid-IR (in blue), and galaxies that are not classified as variable in the mid-IR (in orange). Each panel is labeled by its MaNGA plate-IFU (top right) and its location in our variability space given by ﹩{\mathrm{log}}_{10}\mathrm{Var}({\rm{W}}2)﹩ and ﹩{\mathrm{log}}_{10}{\varsigma }^{2}﹩ (top left). The gray band indicates when the object was observed by MaNGA.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Comparing the expected variance derived from within-epoch variances (Equation (10)) to the expected variance derived from within-epoch uncertainties (Equation (9)); 81% of the MaNGA sample lies above the one-to-one line (ς 2 > σ 2). We therefore conservatively use ς 2 as our true errors.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Distribution of predicted points using Monte Carlo simulations vs. the observed ﹩{\mathrm{log}}_{10}\mathrm{Var}({\rm{W}}2)﹩, only using points with ﹩{\mathrm{log}}_{10}{\varsigma }^{2}\lt -2.5﹩.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Images and spectra of galaxies 11981–6104 and 9870–1902. For each galaxy, the top left panel shows the SDSS optical image of the galaxy and the top center panel shows the Hα (red) and [O III] (green) maps overlaid on the r-band flux (gray). The top right panel shows the W2 light curve (the gray line indicates when it was observed by MaNGA). The bottom panel shows the MaNGA spectra with emission lines marked. Lines from the same element are of the same color.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Panel (a) compares ﹩{\mathrm{log}}_{10}{\varsigma }^{2}﹩ vs. W2, with the black line plotting the vertical edge of the variable cut in panel (b). The galaxies in blue have W2 < 16.5 and ﹩{\mathrm{log}}_{10}{\varsigma }^{2}\lt -2.5﹩. Panel (b) shows the population with W2 < 16.5. It is also labeled with “count,” which is the number of variable objects that remain after the magnitude cut.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Showing where galaxies mentioned in Section 3 lie in our variability space (left panel) and in W1 − W2 vs. sSFR space (right panel). Each galaxy is labeled by a diamond and labeled by its plate-IFU.
Paper: Mid-infrared Variability in Nearby Galaxies from the MaNGA Sample
Authors: Aashay Pai, Michael R. Blanton, John Moustakas
Figure caption: Depicting where our variable galaxies lie in the P1 vs. P3 space, with the gray points being the MaNGA galaxies. The red crosses are variable objects from our catalog that are identified as narrow-line AGN based on the criterion from X. Ji & R. Yan (2020). The black crosses are the remaining objects that we identify to be variable in the mid-infrared.