adsabs/AstroCLIMB huggingface dataset:
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Luminosity–metallicity relation for nearby satellites. Metallicities of satellites from this work are converted to [Fe/H] using D. Streich et al. (2014) assuming an [α/Fe] = 0.3. All other data points are from the Local Volume Database. Error bars include errors from bootstrapping and errors on age. If the combined mean metallicity error for a particular galaxy was less than the average combined mean error of all four galaxies, we set the error to 0.3 dex.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Radial density profiles for each satellite. Black dots are derived from counting the number of RGB stars in bins of elliptical annuli around each satellite and dividing by the total nonzero area in each bin, accounting for pixels that are masked out in each image. Error bars show Poisson uncertainties. The best-fit profile from the MCMC is shown as a colored line, with 100 random draws from the posterior distribution shown in gray.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Distribution of point sources in each ACS field. The 2 and 3a  h  best-fit ellipses are shown in black. Only the RGB stars used to fit each satellite are shown. The x- and y-scales are identical in each plot.
Paper: Exploring the Diversity of Faint Satellites in the M81 Group
Authors: Katya Gozman, Eric F. Bell, In Sung Jang, Jose Marco Arias, Jeremy Bailin, Roelof S. de Jong, Richard D'Souza, Oleg Y. Gnedin, Antonela Monachesi, Paul A. Price, Vaishnav V. Rao, Adam Smercina
Figure caption: Completeness curve for one galaxy in our sample, D1009+68.
Paper: Unveiling the Emission Mechanisms of Blazar PKS 1510-089. I. Multiwavelength Variability
Authors: Alfredo Amador-Portes, Abigail García-Pérez, Vahram Chavushyan, Victor M. Patiño-Álvarez
Figure caption: Example decomposition of the Hβ and Hγ emission lines from a spectrum observed at SO on 2010 March 19. Top panel: the rest-frame spectrum with the best-fit model overlaid. The continuum is represented by a power-law function. Middle panel: the broad and narrow components used to fit Hβ and Hγ, along with the Fe II template, [O III] doublet, and telluric absorptions. Bottom panel: residuals from the subtraction of the best-fit model from the observed spectrum.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The signatures in ﹩\angle (\bar{m})﹩ and Re ﹩(\breve{v})﹩ for the four polarimetric best-bet models at 230 GHz for M87*. The “open stars” represent the transition radii obtained from the change in sign (denoted by ﹩{ \mathcal S }﹩) from the n = 0 to the n = 1 image domain polarization quantity. The “dots” represent the values obtained from the geometric formulae developed in the paper. For MAD, a * = 0, R h = 80, no transition is reported in LP since the physical transitions are posited to occur beyond 30 Gλ. For MAD, a * = +0.94, R h = 160 since ﹩{ \mathcal S }({v}_{1})=1﹩ and the signal only has positive values, the inference for the CAA-based analysis is that the signal is always photon ring dominated. The nan represents the mathematical fact that for this model, ﹩{ \mathcal F }\times {v}_{r}\lt 1﹩, and so Equation (17) has an undefined numerical value.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The transition values ρ  T  in the Fourier plane obtained via CAA of time-averaged GRMHD images of M87* at 230 GHz. The data points denote the first instance at which the photon ring signal begins to dominate. For LP, this is noted by identifying the value of ρ at which the sign of arg(﹩{\bar{m}}_{01}﹩) swings from positive to negative or vice versa, with the “correct” swing being decided by whether the corresponding change in signs of arg (β 2,0) to arg (β 2,1) (which are image domain quantities) is positive to negative or vice versa. For CP, a similar prescription is provided for noting the sign change in the real part of ﹩{\breve{v}}_{01}﹩, with the correct convention based on the signs of v 0 and v 1. Markers in the black rectangle on the right indicate images for which the direct and indirect images have the same polarimetric signs and therefore do not show a clear photon ring transition in the indicated polarized interferometric quantity.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The maximum permitted thermal noise in ﹩\breve{m}﹩ and ﹩\breve{v}﹩ for the four best models for M87* at 230 GHz. The plots are obtained by sampling the Fourier domain signals of the models along the u and v axes. For both σ ngEHT and σ BHEX, the reference baseline is formed with ALMA in conjunction with the new site/orbiter parameters given in Table 1. The SEFD of ALMA is assumed to be 74 Jy (Event Horizon Telescope Collaboration et al. 2019c). The horizontal dashed lines represent the thermal noise for the ngEHT/BHEX-ALMA baseline, with the subscripts 9 and 13 signifying the 9 m and 13 m antenna diameters, respectively. These lines are terminated at the vertical dashed lines, which represent the maximum baselines achievable with the corresponding mission at 230 GHz.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The antenna diameter requirements for an ngEHT site ALMA baseline. For the site, the putative parameters considered are system temperature T  s  = 110 K and antenna efficiency η  A  = 0.8. For the baseline, the bandwidth considered is Δv = 16 GHz with an integration time of Δt = 600 s and (2 bit) quantization efficiency η  Q  = 0.88. The SEFD of ALMA is assumed to be 74 Jy.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The demonstration of the CAA scheme on a time-averaged GRMHD image of a MAD model with a * = +0.5 and R h = 160 which contains contributions from both n = 0 and n = 1 images. The left panel shows Re(﹩\breve{v}﹩) for a grid of points in the (u,v) plane out to 30 Gλ, while the right panel shows the coherently averaged results after implementing CAA with a bin width of 4 Gλ.
Paper: Photon Ring Polarimetry with Next-generation Black Hole Imaging. I. M87*
Authors: Aditya Tamar, Daniel C. M. Palumbo
Figure caption: The antenna diameter requirements for the BHEX forming an Earth-Space baseline with ALMA. The orbiter parameters are given in Table 1.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: Purity (left column) and completeness (right column) as a function of redshift for the three protocluster classes (top: Fornax type; middle: Virgo type; bottom: Coma type) when using the spatially based criteria to select protocluster members; whether a galaxy is actually a protocluster member is known from its dark matter halo merger history. The lines indicate the median value for the protocluster sample, and the shaded region indicates the 25–75th-percentile range. The results for R  e  and 2R  e  consider all protocluster members, whereas those for R 200c consider only members within the core region. Using a radius of 2R  e  to select protocluster galaxies yields an overall completeness of 80%, while with R  e , this quantity is generally less than ∼50%. The purity is ≳80% when R  e  is used, whereas it is ∼50%–80% when 2R  e  is employed, depending on redshift and protocluster type. When selecting core galaxies within R 200c, the purity drops with decreasing redshift, mainly due to R 200c becoming comparable with R  e  and thus enclosing increasingly many galaxies that will not merge with the main halo by z = 0.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The predicted S 870 differential number counts for our Millennium+L-GALAXIES mock, computing submillimeter flux densities using both the R. K. Cochrane et al. (2023) scaling relation (blue dashed line) and the template approach (red solid line). We overplot observational results from J. E. Geach et al. (2017) and S. M. Stach et al. (2018). For reference, colored areas represent the predicted number counts from the R. K. Cochrane et al. (2023) scaling relation if we arbitrarily divide or multiply the SFR (top panel) or M dust (bottom panel) by a factor of 2.5. Note that multiplying M dust by 2.5 implies that all metals in the cold gas would be dust. The two approaches for computing submillimeter flux density yield similar number counts. As is the case with most models that assume a standard IMF, the predicted counts are less than those observed, though only by a factor of a few.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The evolution of the effective radius (R  e ) and the most massive dark matter halo’s radius (R 200c) as a function of redshift. We show Fornax-, Virgo- and Coma-type progenitors from left to right. Colored areas represent the 25th and 75th percentiles, respectively, while the lines are the medians. As shown in Y.-K. Chiang et al. (2013), R  e  increases with increasing redshift. On the other hand, R 200c decreases with increasing redshift and becomes comparable to R  e  at z ∼ 1. Thus, we will focus our analysis at z ≳ 1.5 since our galaxy member selection depends on both quantities.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The number counts (deg−2) of protoclusters (solid lines) and clusters (dashed lines) as a function of redshift. Once a protocluster reaches a virial mass of 1014  M ⊙, it is subsequently classified as a cluster. Fornax-, Virgo-, and Coma-type progenitors are shown in the top, middle, and bottom panels, respectively. The redshift at which the numbers of protoclusters and clusters are the same is z ∼ 0.7, 1.2, and 1.7 for Fornax-, Virgo-, and Coma-type progenitors, respectively.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: Example SED of a galaxy at z=3.23 with ﹩{{\rm{log}}}_{10}({{M}}_{\star }/{{M}}_{\odot })=11.14﹩, SFR = 400.27 M ⊙ yr−1, and ﹩{\mathrm{log}}_{10}({{M}}_{\mathrm{dust}}/{{M}}_{\odot })=9.19﹩ computed using the template approach. Red dots indicate the flux densities computed using the R. K. Cochrane et al. (2023) scaling relations. The template and scaling relation approaches yield similar results.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: The stellar mass formed between two epochs with (dashed line) and without (solid) the SFH refinement for the disk (blue) and bulge (red) components. This example shows the SFH of a z = 0.4 galaxy with M ⋆ = 1.6 × 1011 M ⊙ and SFR=34.23 M ⊙ yr−1. Our SFH refinement technique splits the stellar mass in the youngest (age ∼20 Myr for this snapshot) SFH bin into five bins with younger ages.
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Distribution of Faraday rotation for 105 photons crossing the τ LoS = 1 photosphere with a turbulent magnetic field. The results depends on the typical scale of the turbulence d compared to the length of the photosphere ℓ. In blue, orange, green, and red are represented the cases of N = d/ℓ = 1, 3, 10, and 30, respectively. The larger the number of cells in the photosphere, the smaller the effects of Faraday rotation become.
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Depolarization caused by Faraday rotation for a turbulent field with different length scales of turbulence ℓ  relative to the mean free path d. The more distinct the cells, the more random fields along the line of sight, but each one is over a smaller length scale so counterintuitively the depolarization is reduced by multiple turbulent cells.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Diagram showing screens relative to their distance between Earth and the pulsar PSR J1645−0317. The labels “G” and “L” represent screens derived from transverse velocities using Gaussian and Lorentzian fits to ACFs, respectively. A scenario in which x = 1 represents the halfway point between Earth and the pulsar, as defined in Equation (4). Lighter shaded bars indicate uncertainties on the associated distances.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J0922+0638 on MJD 60286.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example secondary spectrum for PSR J0826+2637 on MJD 60384.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J2018+2839 on MJD 60265.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J0826+2637 on MJD 30372.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J2022+5154 on MJD 60145.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example secondary spectrum for PSR J1645–0317 on MJD 60270.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J1645–0317 on MJD 60146.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J2022+2854 on MJD 60265.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Left: the redshift distribution of the MOSDEF spectroscopic sample on top of the underlying photometric data from the five CANDELS fields. The black dashed lines show the three redshift bins asserted by the MOSDEF team (M. Kriek et al. 2015). Right: distribution of the sample on the star formation rate vs. stellar mass plane. The underlying 2D histogram shows CANDELS galaxies in the redshift range of 0.6 < z < 3.6 to match that of MOSDEF. Black circles are the MOSDEF targets and the colored crosses are the identified AGNs with different techniques. The light green, purple, and gold dashed lines show the main sequence of star-forming galaxies at z = 1, 2, and 2.5, respectively, from E. Daddi et al. (2007), K. G. Noeske et al. (2007), and I. Shivaei et al. (2015).
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: The top two rows represent the component maps of the trained SOM at 1.37 < z < 1.70, resulting from learning the 8D color manifold. The color bars represent the respective colors for individual SOMs. In the bottom row, the SOM cells are color-coded based on the median of normalized stellar mass, normalized star formation rate (SFR), and galaxy redshift of CANDELS galaxies used in the training process, respectively, from left to right. These parameters are derived from the SEDs of galaxies, involving all nine colors (eight dimensions).
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Augmenting a missing band in the photometric catalog using linear interpolation (left) and the SOM (right). The top panels show contours on the scatterplots of the predicted vs. real F098W magnitudes for a test subsample, and the bottom panels show a Gaussian regression fit to the delta magnitudes. Both methods predict the missing fluxes with reasonable accuracy comparable to photometric uncertainties.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Illustration of the arms of the Milky Way produced by the electron density model NE2001 (S. K. Ocker & J. M. Cordes 2024), with the dot representing the location of our solar system and the line extending to the potential scattering screen distance of PSR J2313+4253 within the error of our estimations.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example secondary spectrum for PSR J2313+4253 on MJD 60169.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J2313+4253 on MJD 60169.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Similar to Figure 2, trained on the 2.0 < z < 2.6 galaxies.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example secondary spectrum for PSR J2022+5154 on MJD 60283.
Paper: AstroSat View of the Neutron Star Low-mass X-Ray Binary GX 5-1
Authors: V. P. Shyam Prakash, Vivek K. Agrawal
Figure caption: The evolution of spectral parameters from the XSPEC model tbabs(diskbb+nthComp) for the SXT and LAXPC combined spectral modeling of GX 5-1. The flux depicted in figure is the unabsorbed flux calculated using the cflux model in XSPEC in the energy range 0.3–50 keV.