adsabs/AstroCLIMB huggingface dataset:
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: The γ-ray SED of nova V407 Cyg, with Fermi-LAT detections in yellow and VERITAS limits in magenta. Also plotted is the SED for V392 Per, with HAWC limits using the same Γ = 2.5 PL index as VERITAS.
Paper:  γ-Ray Emission from Classical Nova V392 Per: Measurements from Fermi and HAWC
Authors: A. Albert, R. Alfaro, C. Alvarez, J. C. Arteaga-Velázquez, D. Avila Rojas, H. A. Ayala Solares, R. Babu, E. Belmont-Moreno, C. Blochwitz, K. S. Caballero-Mora, T. Capistrán, A. Carramiñana, S. Casanova, O. Chaparro-Amaro, U. Cotti, J. Cotzomi, E. De la Fuente, C. de León, S. Coutiño de León, R. Diaz Hernandez, B. L. Dingus, M. A. DuVernois, M. Durocher, J. C. Díaz-Vélez, K. Engel, C. Espinoza, K. L. Fan, K. Fang, N. Fraija, J. A. García-González, F. Garfias, M. M. González, J. A. Goodman, J. P. Harding, S. Hernandez, J. Hinton, D. Huang, F. Hueyotl-Zahuantitla, P. Hüntemeyer, A. Iriarte, V. Joshi, A. Lara, W. H. Lee, J. T. Linnemann, A. L. Longinotti, G. Luis-Raya, J. Lundeen, K. Malone, V. Marandon, O. Martinez, J. Martínez-Castro, J. A. Matthews, P. Miranda-Romagnoli, J. A. Morales-Soto, E. Moreno, M. Mostafá, A. Nayerhoda, L. Nellen, M. Newbold, M. U. Nisa, R. Noriega-Papaqui, N. Omodei, A. Peisker, Y. Pérez Araujo, E. G. Pérez-Pérez, C. D. Rho, D. Rosa-González, E. Ruiz-Velasco, D. Salazar-Gallegos, F. Salesa Greus, A. Sandoval, J. Serna-Franco, A. J. Smith, Y. Son, R. W. Springer, O. Tibolla, K. Tollefson, I. Torres, R. Torres-Escobedo, R. Turner, F. Ureña-Mena, L. Villaseñor, X. Wang, E. Willox, A. Zepeda, H. Zhou, L. Chomiuk, E. Aydi, K. L. Li, B. D. Metzger, I. Vurm
Figure caption: The spectral lines used to estimate the reddening taken 6 days after t 0. Left: the Na I D interstellar absorption lines at 5895.9 Å (D1) and 5889.9 Å (D2). Right: the diffuse interstellar bands used to estimate the reddening.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Radial profiles of w rms (a), u rms (b), the total U rms (c), and the perturbations of potential temperature (d). The profile of the latitudinal component v rms is similar to u rms. The averaging was performed in the horizontal directions and time. The thin vertical lines show the bottom of the unstable layer.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Luminosity carried by the enthalpy flux, ﹩{L}_{{\rm{e}}}=4\pi {r}^{2}{R}_{g}{c}_{p}\rho \langle w{{\rm{\Theta }}}^{{\prime} }{\rangle }_{\phi \theta }﹩ (solid lines), and the kinetic energy flux, L k = 4π r 2 ρ〈w(u 2 + v 2 + w 2)〉 ϕ θ  (dotted lines), for the nonrotating simulations presented in Table 1. The color-coding of the lines is the same as in Figure 3. The inset shows the overshooting region with negative values of L e.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Instantaneous snapshots of the velocity components for simulations R1 to R8, from top to bottom. The radial velocity, w, is presented in the orthographic projection (panels a, e, i, and m) and in the meridional plane (b, f, j, and n). The latitudinal, v (panels c, g, k, and o), and the longitudinal, u (panels d, h, l, and p), components are presented in the meridional plane. The thin dashed red line shows the transition between the stable and unstable layers.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Kinetic power spectra for the spheroidal (blue lines), toroidal (yellow), and radial (black) components of the velocity field at r = 0.95R ⊙ for simulations (a) R1 to (d) R8. The dashed lines in panel (c) correspond to simulation R1x. The results of panels (c) and (d) indicate strongly anisotropic convection with divergent flows more energetic than the radial flows. The black and red dashed lines in panel (d) show the Kolmogorov (1941) and Rincon et al. (2017) predictions, respectively, for the spectra of turbulent motions.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: (a) Radial profile of the ambient potential temperature, Θ a . The insert shows a close-up for 0.7 < r/R ⊙ < 0.96 depicting a negative radial gradient of Θ a . The difference between the bottom and top of the unstable layer is 62 K. (b) Radial profiles of the ambient density (black line) and temperature (red line). The dotted lines correspond to the solar structure model of Christensen-Dalsgaard et al. (1996). From the bottom to the top of the domain, there are ∼4.5 density scale heights. From the base of the convection zone, r > 0.7R ⊙, there are ∼3.7 density scale heights. The vertical red lines show the bottom of the unstable layer located at r = 0.725R ⊙.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Turbulent kinetic power spectra for simulations with different resolutions R1–R8 (see color correspondence in the legend), at three different depths, from left to right. The black dashed line corresponds to a simulation with the same horizontal resolution as R1 but with 256 grid points in the radial direction. The dotted line shows the ℓ −5/3 Kolmogorov scaling.
Paper: Implicit Large-eddy Simulations of Global Solar Convection: Effects of Numerical Resolution in Nonrotating and Rotating Cases
Authors: G. Guerrero, A. M. Stejko, A. G. Kosovichev, P. K. Smolarkiewicz, A. Strugarek
Figure caption: Same as Figure 2, but for simulations R1x24, R2x24, and R4x24, from top to bottom.
Paper: Estimating the Convective Turnover Time
Authors: Wei-Chun Jao, 惟君 饒, Andrew A. Couperus, Eliot H. Vrijmoet, Nicholas J Wright, Todd J. Henry
Figure caption: (Left) Stars in Wright et al. (2011) used to generate the τ–mass relation are shown on an observational H-R diagram using Gaia photometry and parallaxes. The central black line represents a fit to the distribution of stars on the main sequence in Gaia EDR3 within 100 pc, and the upper and lower black lines encompass 90% of the population at a given color (W. C. Jao 2022, in preparation). The short, thick black line represents the location of the main-sequence gap (Jao & Feiden 2020), corresponding to the transition between partially and fully convective M dwarfs. (Center) Yellow dots are stars in the mass bin of 1.02–1.16 M ⊙ in Wright et al. (2011) and an orange dot represents a G2V dwarf as a reference. Red dots are stars with masses included in the lowest-mass bin with masses of 0.09–0.14 M ⊙ in Wright et al. (2011), and blue dots are supplemental low-mass stars presented in Wright et al. (2018). Three masses of 1.0, 0.37, and 0.16 M ⊙ are labeled at their corresponding spectral types of G2V, M3V, and M5V based on the stellar parameters table in Pecaut & Mamajek (2013). (Right) A comparison between distances from Gaia EDR3 and distances used in Wright et al. (2011) to derive their fundamental parameters; most distances were underestimated.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Dispersion properties of resonantly damped oblique quasi-kink modes in an asymmetric slab configuration. Plotted here are the oscillation frequency (ω, the upper row) and the ratio of the damping rate to the oscillation frequency (−γ/ω, lower) against the dimensionless TL width (l/d). A fixed combination [ρ i/ρ L, k  y  d, k  z  d] = [10, 0.5, π/50] is adopted, whereas a number of ρ i/ρ R are examined as discriminated by the line styles. The black curves represent our resistive computations (labeled “Resis”). Also presented are two groups of solutions to the dispersion relation (Equation (22)) in the thin-boundary limit, one found numerically (labeled “TB num,” the red curves in the left column) and the other found analytically in an approximate manner (“TB analytic,” the blue curves in the right column). See text for more details.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Effects of density asymmetry on resonantly damped oblique quasi-kink modes in an asymmetric slab configuration. Plotted are the dependencies on ρ i/ρ R of (a) the oscillation frequency ω, (b) the ratio of the damping rate to oscillation frequency −γ/ω, and (c) the damping rate −γ. The combination [ρ i/ρ L, l/d, k  y  d, k  z  d] is fixed at [10, 0.5, 0.5, π/50]. The red asterisks in (a) and (b) are obtained with the approximate expressions for the “Fully Asymmetric” and “Fully Symmetric” configurations in the thin-boundary limit. Furthermore, the blue dashed–dotted curve in (a) represents the upper end of the right Alfvén continuum (k  z  v AR). The open triangles (boxes) in (c) correspond to the contribution to the gross damping rate from the left (right) resonance, as evaluated with the relevant eigenfunctions. The sum of the individual contributions is further given by the filled circles. See text for more details.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Eigenfunctions of resonantly damped oblique quasi-kink modes in an asymmetric slab configuration. A fixed combination [ρ i/ρ L, l/d, k  y  d, k  z  d] = [10, 0.5, 0.5, π/50] is adopted, whereas two values are examined for ρ i/ρ R, one being 5 (the left column) and the other being 1.2 (right). The portions shaded green and blue correspond to the left and right transition layers, respectively. The magnetic Reynolds number R m is taken to be 105. Plotted from top to bottom are the Fourier amplitudes of the transverse speed (﹩{\tilde{v}}_{x}﹩), the out-of-plane speed (﹩{\tilde{v}}_{y}﹩), and the total pressure perturbation (﹩{\tilde{p}}_{\mathrm{tot}}﹩). The eigenfunctions are scaled such that ﹩{\tilde{p}}_{\mathrm{tot}}=1﹩ at x = − 2d, their real (imaginary) parts represented by the solid (dashed) curves.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Dependencies on the dimensionless TL width (l/d) of the critical density contrast ﹩{({\rho }_{{\rm{i}}}/{\rho }_{{\rm{R}}})}_{\mathrm{crit}}﹩, only above which is the right Alfvén resonance relevant. The combination [ρ i/ρ L, k  z  d] is fixed at [10, π/50], whereas a number of k  y  d are examined as labeled.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Dependencies of the damping efficiency on the magnetic Reynolds number R m for oblique quasi-kink modes in asymmetric coronal slabs. The damping efficiency is measured by ω/∣γ∣, with ω being the oscillation frequency and γ the damping rate. A fixed combination [ρ i/ρ L, l/d, k  y  d, k  z  d] = [10, 0.5, 0.5, π/50] is adopted, whereas a number of values are examined for ρ i/ρ R as labeled.
Paper: Oblique Quasi-kink Modes in Solar Coronal Slabs Embedded in an Asymmetric Magnetic Environment: Resonant Damping, Phase and Group Diagrams
Authors: Shao-Xia Chen, Bo Li, Mingzhe Guo, Mijie Shi, Hui Yu
Figure caption: Transverse density profile ρ 0(x) for the examined asymmetric slab system. Two transition layers (TLs, the shaded portions), centered around the nominal slab boundaries (∣x∣ = d) and both of width l, are placed symmetrically about the nominal slab axis (x = 0). Some smooth profile is adopted to connect the interior density ρ i to ρ L(ρ R), the density in the left (right) exterior (see, Equation (1)). A pair [ρ i/ρ L, l/d] = [10, 0.5] is adopted, while a number of ρ i/ρ R are examined as labeled.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: The emissivity with small-scale fluctuations and its known smooth component (top panels), and the reconstructed electron density profiles for the LOS with l = 2.°0 on the Galactic plane (bottom panels). For left panels we adopt ﹩{k}_{\min }=5.0﹩ kpc−1 and for right panels we adopt ﹩{k}_{\min }=0.5﹩ kpc−1. All density profiles, including the NE2001, have been smoothed by a Gaussian kernel with radius equal to 1 bin.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: Top: the face-on view of the electron distribution on the Galactic plane reconstructed from 900 equally separated LOS. To suppress the noise and highlight the large-scale structures, the density fields are smoothed by a Gaussian kernel with a radius 0.25 kpc. Bottom: the electron density in the NE2001 model. For comparison purposes, the NE2001 data are binned and smoothed the same as to the reconstructed density. To guide the eye we plot the locations of spiral arms modeled in NE2001.
Paper: A New Method of Reconstructing Galactic 3D Structures Using Ultralong-wavelength Radio Observations
Authors: Yanping Cong, 艳平 丛, Bin Yue, 斌 岳, Yidong Xu, 怡冬 徐, Yuan Shi, 嫄 施, Xuelei Chen, 学雷 陈
Figure caption: The ∣f err∣ vs. n  e  in the reconstructed 3D Cartesian coordinate density field. Color bar indicates the probability density with normalization ﹩\int \mathrm{PD}d| {f}_{\mathrm{err}}| {{dn}}_{e}=1﹩.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: Van der Wel et al. (2014)'s size mass relation for ETGs at z = 0.75 and z = 1.25 shown with red and purple x’s at the median, respectively, with black lines connecting each point. CJ 1323 is shown with a deep purple star. The color of each object corresponds to its redshift, as defined in the color bar to the right. The other symbols represent ETGs; triangles are quiescent galaxies at z = 0.6–1 reported in Bezanson et al. (2018), drawn from the LEGA-C survey (van der Wel et al. 2016); plus signs are 75 massive quiescent galaxies from z = 1.0–1.3 from the VANDELS survey (Carnall et al. 2019); circles are 17 spheroidals at z = 1.05–1.60 from Newman et al. (2010), diamonds are 40 massive quiescent galaxies at z = 1.0–1.6 from Belli et al. (2014) (the original sample is 56 galaxies; the 16 also in Newman et al. 2010 have been removed), and squares are 13 strongly lensed massive compact ETGs at z = 0.4–0.7 from Oldham et al. (2017). It is clear that, on average, lower redshift galaxies have larger radii, despite there not being as significant a trend for mass. Furthermore, CJ 1323 is one of the most compact galaxies.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: (Left) Coadded reconstructions of COOL J1323+0343 in the source plane. (Right) The GALFIT model of the arc in the image plane based on the FOURSTAR H-band data.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption:  gr(z + H) image of COOL J1323+0343. This image was constructed using grz-band imaging from DECaLS and H-band imaging from FOURSTAR on Magellan. The lensed galaxy is seen as a bright red multiply imaged source, with three images. We refer to the images by number throughout the Paper, corresponding to the labels in this figure. The foreground cluster has two similarly bright central galaxies. The bright blue source between the two brightest cluster galaxies is a foreground star.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: (Left) FOURSTAR H-band image of CJ 1323 showing the tangential critical curve from the lens model (red) trisecting the arc and the caustic (yellow). The lens model was made using the positional constraints indicated with small circles. The positional constraints are derived from the H-band model, not convolved with the PSF, and each color represents locations of matching surface brightness on the lensed images. (Right) The LDSS3 grz-band image, with the central stellar contaminant subtracted, revealing a fourth image. The blue arrow points to the fourth image.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: (Top left) The posterior distribution of the demagnified stellar mass of CJ 1323 in the source plane. (Top right) The posterior distribution of the star formation rate (SFR) in the source plane. Both the stellar mass and SFR are the results of the model utilizing the Kriek & Conroy (2013) attenuation curve. The median and uncertainties are reported above each plot and shown as dashed lines. (Bottom) The specific star formation rate for each age bin. Both models show that CJ 1323 was quiescent at the epoch of observation and, within error, show the same rate of star formation.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: (Top) Residual between the best-fit Prospector model and the observed photometry (blue). (Middle) Best-fit SED model using the Kriek & Conroy (2013) dust attenuation curve (black) and other fits from the posterior distribution (gray) calculated via Prospector using grzH photometry (purple) and optical/NIR Nordic Optical Telescope/ALFOSC spectroscopy (green), with the 1σ uncertainty on the spectra shown as a light green envelope. Best-fit photometry is shown as black squares. (Bottom) A zoom in on the black box in the middle plot showing the spectra in more detail, with the H-delta emission line, Calcium H and K absorption lines, and the center of the G band in the rest frame labeled.
Paper: COOL-LAMPS. II. Characterizing the Size and Star Formation History of a Bright Strongly Lensed Early-type Galaxy at Redshift 1.02
Authors: Ezra Sukay, Gourav Khullar, Michael D. Gladders, Keren Sharon, Guillaume Mahler, Kate Napier, Lindsey E. Bleem, HÅkon Dahle, Michael K. Florian, Katya Gozman, Jason J. Lin, Michael N. Martinez, Owen S. Matthews Acuña, Elisabeth Medina, Kaiya Merz, Jorge A. Sanchez, Emily E. Sisco, Daniel J. Kavin Stein, Kiyan Tavangar, Katherine E. Whitaker
Figure caption: Corner plot with posterior distributions and correlations for inferred parameters in the Prospector SED fitting analysis for the lensed source in the image plane, with contours corresponding to 1σ (dark) and 2σ (light). We show results from the models using the Kriek & Conroy (2013) attenuation curve (blue) and the Calzetti et al. (2000) attenuation curve (red). In the model using the C+00 curve, dust_index is fixed to zero and dust2 is the only normalization factor. The best-fit values for the model using the K&C13 curve are shown with gray dashed lines. This plot clearly shows the results for mass and metallicity are similar regardless of model choice.