adsabs/AstroCLIMB huggingface dataset:
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Particle energization in 2D pair-plasma MRI simulations. Top row: average Lorentz factor for electrons and positrons for simulations with a small box/large ω C/Ω0 (left), medium box/medium ω C/Ω0 (center), large box/small ω C/Ω0 (right). In each case, the difference between 〈γ〉 of the two species is shown as a dashed green line, and the end of the nonlinear stage is marked with a vertical dashed–dotted line (notice the difference in timescales between different runs). Bottom row: evolution of energy distributions in time (including both species) for the three runs. In each case, the distributions are shown until the same final time as in the top row. The dotted lines indicate the average and cutoff Lorentz factors γ ∼ qB λ MRI/(mc 2) (with B = B c or B = B e; see text) characterizing the quiescent end state of each run.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Isotropic power spectrum of the in-plane (red lines) and out-of-plane (blue lines) magnetic field for a 2D pair-plasma MRI simulation with parameters ω C/Ω0 = 60, β 0 = 624, and box size ﹩8\times 8{\lambda }_{\mathrm{MRI}}^{2}﹩. The spectra during the linear stage (dashed lines) are peaked around the most-unstable MRI wavenumber k MRI. At late times during the nonlinear stage (solid lines), the spectra feature characteristic slopes indicating an inertial range, and a clear spectral break in the vicinity of the average Larmor-radius wavenumber k  ρ .
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Evolution of the change in the in-plane magnetic energy for our parameter-space exploration of the 2D pair-plasma MRI. Top left and top right: varying ω C/Ω0 at a fixed β 0 for a small- and a medium-size simulation box, respectively. Bottom left: varying the box size at a fixed ω C/Ω0 and β 0. Bottom right: varying β 0 at a fixed ω C/Ω0 for a medium-size box.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Comparison of 2D pair-plasma simulations of the MRI with variable box aspect ratio. Top: spatial distribution of the in-plane field strength at t = 4.2P 0 for a simulation with box size ﹩4\times 4{\lambda }_{\mathrm{MRI}}^{2}﹩ (left) and ﹩16\times 4{\lambda }_{\mathrm{MRI}}^{2}﹩ (right), with ω C/Ω0 = 30, β 0 = 624. The elongated-box case shows turbulent structures that do not develop in the corresponding square-box case. Bottom left: evolution of the change in magnetic energy for runs with variable box size and aspect ratio at fixed ω C/Ω0 and β 0. Bottom right: evolution of the volume-averaged β ∥ and β ⊥ for the square-box case ﹩4\times 4{\lambda }_{\mathrm{MRI}}^{2}﹩ and for the elongated-box case ﹩16\times 4{\lambda }_{\mathrm{MRI}}^{2}﹩.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Evolution of the pair-plasma MRI in a small 3D box (﹩2\times 2\times 2{\lambda }_{\mathrm{MRI}}^{3}﹩). Left: spatial distribution of the radial (B  x ) and toroidal (B  y ) magnetic field at subsequent times during the simulation. Right: evolution of the change in magnetic energy in all three components of  B  (top), and evolution of the volume-averaged β ∥ and β ⊥ (bottom).
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Left column: evolution of the α-parameter and of the volume-averaged Maxwell, Reynolds, and anisotropic stresses for a small box/large ω C/Ω0 (top), medium box/medium ω C/Ω0 (center), and large box/small ω C/Ω0 (bottom) simulation of the 2D pair-plasma MRI. Right column: evolution of the volume-averaged pressure anisotropy and β ∥, β ⊥ for the same simulations.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Evolution of the in-plane magnetic-energy variation for several 2D pair-plasma simulations of the MRI with zero net magnetic flux. Left: simulations with varying box size and fixed ω C/Ω0, β 0. Right: simulations with varying ω C/Ω0 and fixed box size and β 0.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Estimate for injection of magnetic energy and conversion into kinetic energy assuming Alfvénic turbulence, for the three simulations presented in Section 4.5. In each case, the end of the nonlinear phase is marked with a black cross.
Paper: Fully Kinetic Shearing-box Simulations of Magnetorotational Turbulence in 2D and 3D. I. Pair Plasmas
Authors: Fabio Bacchini, Lev Arzamasskiy, Vladimir Zhdankin, Gregory R. Werner, Mitchell C. Begelman, Dmitri A. Uzdensky
Figure caption: Comparison of 2D pair-plasma simulations of the MRI with variable β 0 in a medium-size box and fixed ω C/Ω0. Left: in-plane magnetic-energy variation normalized over the initial field strength. Right: corresponding evolution of the volume-averaged β in time.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Velocity-integrated-intensity maps of (a–d) four HOCO+ transitions, (e) H13CO+(1-0), and (f) CH3OH(2 k −1  k ). Contour levels are (a–d) [2, 4, 8, 12], (e) [9.0, 18.0, 36.0, 72.0], and (f) [25.0, 50.0, 100.0, 200.0] K km s−1. A beam size of 1.″6 × 1.″6 (27 pc × 27  pc) is shown at the bottom left corner in each panel as a blue circle. Locations of the GMCs identified by Leroy et al. (2015) are shown as black crosses and labeled in panel (f). The coordinates of these GMCs are given in Table 3. The kinematic center known as “TH2” (Turner & Ho 1985) with the revised coordinates of Cohen et al. (2020) is shown as a yellow star with orange edges in panel (f). GMCs with Class I methanol maser detection by Humire et al. (2022) are labeled with red numbers in panel (f).
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Left: the IRAC 8 μm image is shown with contours, while the integrated-intensity image of CO(2-1) is shown with color in the logarithmic scale. The contour levels are 25, 50, 100, 200, and 500 MJy msr−1. The approximate positions of the bar orbits (x 1 orbits) and inner orbits that form the CMZ (x 2 orbits) are shown with magenta and red ellipses, respectively. The beam size is shown as a blue ellipse in the left-bottom corner. The area shown in Figure 2 and the right panel are indicated with a white dashed rectangle in Figure 2 (left). For more detailed orbit models, we refer the reader to other works (e.g., Sorai et al. 2000; Das et al. 2001; Levy et al. 2022). Right: the integrated-intensity image of CO(1-0) overlaid with the same orbits as the left panel.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Maps of (a) the HOCO+ column density, (b) the excitation temperature of HOCO+derived from CASSIS, (c) the total H2 column density derived from the dust continuum shown in a logarithmic scale, and (d) the fractional abundance of HOCO+ shown in the logarithmic scale. The black contours show the HOCO+ (50,5−40,4) integrated intensities, as in Figure 2.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Integrated intensity ratios of (left) HOCO+(50,5−40,4)/CH3OH (2 k −1 k ) and (right) HOCO+(50,5−40,4)/H13CO+(1-0). Only pixels with an integrated intensity of >3σ for each transition and ratio are shown. The ranges of the color scales are set to 0.003–0.15 (left) and 0.03–1.5 (right). Because the maximum/minimum ratios of the color scales are 50 for both images, the variations in color scales between the left and right panels represent variations in the HOCO+(50,5−40,4)/CH3OH (2 k −1 k ) and HOCO+(50,5−40,4)/H13CO+(1-0) ratios.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Left: the column densities of CO2 ice reported by Yamagishi et al. (2015) are shown for selected slits in color. The integrated-intensity image of HOCO+ (50,5−40,4) is shown both in contours and gray scale. Right: the fractional abundances of CO2 ice (i.e., CO2 ice column density divided by the averaged total H2 column density inside the rectangular regions) are shown in log scale with colored rectangles. The continuum image at 361.5 GHz is shown in contours and gray scale.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: The following modeled quantities are shown as functions of the density and cosmic-ray ionization rate: (a) gas temperatures from the Meudon code used for Nautilus chemical modeling, (b) abundance ratios HOCO+/CO2, (c) fractional abundances of HOCO+, (d) CO2 ice (surface + mantle), and (e) CO2 gas, and (f) HCO+.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Examples of observed spectra (blue) vs. modeled spectra from CASSIS (orange) at (x offset, y offset) of (Left) (-17.″3,-10.″4) and (Right) (2.″0,2.″1) relative to the phase center of our observations.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: Left: ratios of errors in the derivation of HOCO+ column densities over the derived HOCO+ column densities at corresponding hexagonal pixels. Right: errors of the excitation temperatures.
Paper: ALCHEMI Finds a “Shocking” Carbon Footprint in the Starburst Galaxy NGC 253
Authors: Nanase Harada, Sergio Martín, Jeffrey G. Mangum, Kazushi Sakamoto, Sebastien Muller, Víctor M. Rivilla, Christian Henkel, David S. Meier, Laura Colzi, Mitsuyoshi Yamagishi, Kunihiko Tanaka, Kouichiro Nakanishi, Rubén Herrero-Illana, Yuki Yoshimura, P. K. Humire, Rebeca Aladro, Paul P. van der Werf, Kimberly L. Emig
Figure caption: AKARI spectra for the regions used in our analysis. As in Figure 1 of Yamagishi et al. (2015), the blue curve represents the best-fit continuum emission while the red curve shows the overall spectral profiles.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Merged ACIS images of the central region of NGC1167 in different energy bands, with overlaid 22 GHz radio contours (Giroletti et al. 2005). The images are presented with a subpixel of one-eighth of the native ACIS pixel size and smoothed with a Gaussian kernel of σ = 2 image pixels.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Images from the CO observations presented in Murthy et al. (2022). Left: CO total intensity with superposed the Chandra full band (0.3–7 keV) contours derived from the 0.3–3.0 keV image shown in Figure 2. Right: CO velocity dispersion. The black contours are from the 22 GHz radio image (Giroletti et al. 2005); the blue and cyan contours identify the outer boundaries of the regions of soft and hard emission in the HR map. The magenta ellipses represent the beam of the CO observations.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Left: hardness Ratio (HR) map (see the text for definition), with 22 GHz contours superimposed. North is to the top and east is to the left. Note the lower HR pixels (blue) along the jet and to the south of the bend of the jet. Right: HR map with 0.3–3.0 keV isointensity contours from the X-ray image in Figure 2. The soft (blue pixel) region to the south of the radio jet is a region of intense X-ray emission.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Top: radial profiles of the 0.3–3.0 keV surface brightness, in two 90° quadrants in the jet direction (top left), and in the cross-jet direction (top right). The PSF is indicated by red dots. Bottom: the same for the 3.0–7.0 keV band.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Left: 0.3–7.0 KeV image with the 22 GHz radio contours overplotted in cyan. The regions used for spectral extraction are shown with white dashed lines. The “All” region is a circle of 4″ radius, encompassing the entire X-ray emission. Right: HR image with extraction regions. Note the different spatial scales.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Left: the 12 azimuthal sectors used to extract the average surface brightness. Right: azimuthal surface brightness profile, with bins starting from the west and going counterclockwise. The jet emission regions are in the colored areas between the two sets of vertical lines.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Spectrum and best-fit model for the region encompassing the entire diffuse emission (the unbinned spectrum and best-fit model using Cash statistics is on the left; the binned spectrum and the χ 2 best-fit model and residuals are on the right).
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Binned spectrum of the entire X-ray emission extracted from a circle of 4″ radius centered on the nucleus, with a χ 2 best-fit model and residuals. Left: the best-fit APEC model is shown in orange. Right: the best-fit CLOUDY model is shown in orange. In both cases, the fit residuals are displayed in the lower panels.
Paper: Jet–ISM Interaction in NGC 1167/B2 0258+35, an LINER with an AGN Past
Authors: G. Fabbiano, A. Paggi, R. Morganti, M. Baloković, M. Elvis, D. Mukherjee, M. Meenakshi, A. Siemiginowska, S. M. Murthy, T. A. Oosterloo, A. Y. Wagner, G. Bicknell
Figure caption: Unbinned spectrum from the nucleus with best-fit Cash power-law model shown in orange.
Paper: Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Data Sets
Authors: Andrew R. Kaiser, Nihan S. Pol, Maura A. McLaughlin, Siyuan Chen, Jeffrey S. Hazboun, Luke Zoltan Kelley, Joseph Simon, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt
Figure caption: Hypermodel A on an injected density ratio of ΩPGW/ΩSMBHB = 0.5 corresponding to an SMBHB GWB (α = − 2/3, γ = 13/3) at an amplitude of A SMBHB,Inj = 2 × 10−15 and a PGW GWB (α = −1, γ = 5) at A PGW,Inj = 1.4 × 10−15 both at f ref = 1/yr. All parameter amplitude panels correspond to the re-parameterized posteriors in terms of a lower reference frequency of f ref = 1/(10 yr). The second-from-the-top plot more closely examines the narrow region of the fixed-PL-only signal model shown in the top panel.
Paper: Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Data Sets
Authors: Andrew R. Kaiser, Nihan S. Pol, Maura A. McLaughlin, Siyuan Chen, Jeffrey S. Hazboun, Luke Zoltan Kelley, Joseph Simon, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt
Figure caption: Examples of various base models used in this analysis. Power laws (PLs) for the injected SMBHB (solid gray line), example WN (dark pink dashed–dotted line), and PGW (solid orange line) with the range in spectral indices for the three early universe models covered in the orange region. An example broken PL encapsulating the combination of SMBHB and WN PLs (cyan dashed line) with the bend frequency is marked with the dashed light blue line, and an example EPBL combining the PGW, SMBHB, and WN PLs (dotted dark blue line) with the low- and high-frequency breaks is marked by the dashed olive green and light blue lines, respectively. Amplitudes are quoted at f ref = 1/yr.
Paper: Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Data Sets
Authors: Andrew R. Kaiser, Nihan S. Pol, Maura A. McLaughlin, Siyuan Chen, Jeffrey S. Hazboun, Luke Zoltan Kelley, Joseph Simon, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt
Figure caption: Logarithmic fractional uncertainties on the amplitude at f ref = 1/(10 yr) for 50 realizations of an additional process on top of an SMBHB GWB fixed PL with respect to injected strain amplitudes at f ref = 1/yr (left axis) and GW density fraction (right axis) versus the timing baseline of the PTA.
Paper: Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Data Sets
Authors: Andrew R. Kaiser, Nihan S. Pol, Maura A. McLaughlin, Siyuan Chen, Jeffrey S. Hazboun, Luke Zoltan Kelley, Joseph Simon, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt
Figure caption: Fractional uncertainties on the spectral index for 50 realizations of an additional process on top of an SMBHB GWB fixed PL with respect to injected strain amplitudes at f ref = 1/yr (left axis) and GW density fraction (right axis) versus the timing baseline of the PTA.
Paper: Disentangling Multiple Stochastic Gravitational Wave Background Sources in PTA Data Sets
Authors: Andrew R. Kaiser, Nihan S. Pol, Maura A. McLaughlin, Siyuan Chen, Jeffrey S. Hazboun, Luke Zoltan Kelley, Joseph Simon, Stephen R. Taylor, Sarah J. Vigeland, Caitlin A. Witt
Figure caption: Median BFs for 50 realizations of an additional process in addition to an SMBHB GWB PL with respect to injected strain amplitudes at f ref = 1/yr (left axis) and GW density fraction (right axis) versus the timing baseline of the PTA.
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 12 but for the dynamical systems metrics computed on daily minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 1 but for minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 11 but for minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 3 but for minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 7 but for minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 8 but for minimum temperature (T min in °C).
Paper: Greater Climate Sensitivity and Variability on TRAPPIST-1e than Earth
Authors: Assaf Hochman, Paolo De Luca, Thaddeus D. Komacek
Figure caption: Same as Figure 5 but for minimum temperature (T min in °C).