adsabs/AstroCLIMB huggingface dataset:
Paper: Erratum: “UVIT Observations of the Small Magellanic Cloud: Point-source Catalog” (2023, ApJ, 946, 65)
Authors: A. Devaraj, P. Joseph, C. S. Stalin, S. N. Tandon, S. K. Ghosh
Figure caption: Distribution of AB magnitudes of the point sources in the SMC field for the three FUV (left panel) and four NUV (right panel) filters.
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: Color–magnitude and color–color diagrams using JWST filters expected to be commonly used for brown dwarfs. Gray dots represent the photometric sample from Leggett et al. (2021) converted to the JWST system. Green squares represent recently published JWST data. Yellow circles and stars indicate the observed and synthesized colors, respectively, for the 260 K Y dwarf WISE 0855. Black lines are ATMO2020++ model sequences with parameters as given in the upper legend. Purple lines are disequilibrium chemistry sequences from Lacy & Burrows (2023), for 250 ≤ T eff (K) ≤ 350, and other parameters as given in the lower legend. See text for further discussion. WISE 0535, like WISE 1828, is an unresolved apparently overluminous system (e.g., Leggett et al. 2021).
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: The black line is the observed spectrum of WISE 0359 from Beiler et al. (2023). Black points represent their photometric measurements. The pink line and dots are the best-fit Sonora model spectrum and photometry, respectively, from Beiler et al. (2023). The blue line and data points are the spectrum and photometry from the best-fit model of the ATMO2020++ grid, respectively. The green line is the same model where PH3 has been removed from the atmospheric composition. The ATMO2020++ model is scaled by the known distance to WISE 0359 (Kirkpatrick et al. 2021) and the radius inferred from evolutionary models (Marley et al. 2021), and has not been scaled to fit. Principal opacity species are indicated. The lower panel shows the difference between the observed spectrum and the spectra generated by the three models (note the difference in y-axis scale in the upper and lower panels). The inset shows the near-infrared flux region. See Section 3 for discussion.
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: Relationships between colors and T eff, calculated from the grid of ATMO2020++ colors. See also Table 1. For T eff ≲ 350 K the F162M − F480M and F360M − F480M colors are less reliable indicators of T eff than M F480M (see Figure 2 and Section 4).
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: The black line is the observed spectrum of WISE 0359 from Beiler et al. (2023). Yellow and orange lines are synthetic spectra generated by model atmospheres with T eff = 450 K, log g = 4.5, and solar metallicity from the BT-Settl suite (Allard 2014, 2016) and by Lacy & Burrows (2023), respectively. Principal opacity species are indicated along the top axis.
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: Additional color transformations for longer wavelengths, calculated from the ATMO2020++ grid, with surface gravity and metallicity as in the legend. The color corresponding to x is indicated by the color of the sequence and identified along the x-axis. The color corresponding to y is identified in each panel. Approximate spectral types are indicated along the top axis.
Paper: The First Y Dwarf Data from JWST Show that Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: Color transformations calculated from the ATMO2020++ grid, with surface gravity and metallicity as in the legend. Colors corresponding to x:y are identified in the colored legends. Approximate spectral types are indicated along the top axis.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: The linear model evidences ﹩\mathrm{ln}Z﹩ and ﹩{\chi }_{\mathrm{red}}^{2}﹩ for fits to different numbers of LST bins and regions N  r . The models shown here (solid, dashed, and dotted) are when the model inputs (BM, PM) are the same as those in the REACH mock, the ideal case, but the number of nonlinear parameters included varies. Each LST bin tends to saturate at a maximum number of regions, with greater LST bin mock foregrounds requiring greater spatial resolution. The solid, colored dots in the bottom panel correspond to the expectation value ﹩E[{\chi }_{\mathrm{red}}^{2}]﹩ for each model input and number of LST bins. Similar analyses are carried out when the model inputs differ from the REACH mock.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Simulated mock spectra (REACH mock, top panel) and noise levels (bottom panel) plotted for various numbers of LST bins: one spectrum at LST 12 hr (magenta), two spectra at 6 and 18 hr (green), five spectra at 2.4, 7.2, 12, 16.8, and 21.6 hr (cyan), and 10 spectra at 1.2, 3.6, 6, 8.4, 10.8, 13.2, 15.6, 18, 20.4, and 22.8 hr (red). The vertical black lines delineate each LST bin. We also plot the radiometer noise levels for the mock data (bottom panel), as well as flat 20 and 100 mK noise levels in black-dashed lines for comparison. Black vertical lines delineate different spectra when the number of bins is greater than one, and channels refer to a particular frequency in the bandwidth for a particular LST spectrum. Thus, channel zero corresponds to 51 MHz for the first spectrum, while channel 93 refers to 51 MHz for the second spectrum, and so on.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Mollweide view and histogram of the difference between the temperature BM used to create the REACH mock (T 408) and the model input (T 300). The right panel shows the temperature difference per pixel, which peaks around 12–17 K, while the left panel shows the view of the galactic-centered sky. Pixels that are cyan have model input values very close to the REACH mock, while those in magenta are more different. Note that these errors still trace out the features of the galaxy, and thus, are indicative of errors that are proportional to the temperatures in each pixel. Hence, the pixel errors near the Galactic Center, which is brighter, are larger.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Approximation of the intrinsic spectral index map by dividing the sky into N  r  equal percentile bin regions. Each region j is then assigned parameters that are constant throughout the region. This particular map is generated from the spectral index map used in the intrinsic mock foreground, β  R .
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Mollweide view (left panel) and histogram (right panel) of the difference between the spectral index PM used to create the REACH mock (408/230) and the PM used as a model input (300/130). Each region in ascending order is assigned a number between zero and seven, before the difference is taken. Pixels that are in the same region in both the mock and model input are shown in cyan in the left panel and have a difference value of zero, while those that differ by one region have a value of one, and so on.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Residuals from the best-fitting (BF) cases from Table 2 for the linear and nonlinear models. Each panel is denoted by the number of LST bins in the fit. Nonlinear models use dotted lines and have NL in their label, while linear models use solid lines and are denoted by L.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: E and H plane polar cuts of the EDGES antenna beam used to convolve the intrinsic mock foreground. The units shown are normalized, absolute units, such that the integral of the beam over the entire sky is unity at every frequency. The different colors represent the beam at various frequencies, as shown in the legend, from roughly 50–90 MHz.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Base temperature map and spectral index map for the intrinsic foreground in the simulated data. The latter map is calculated by forming the natural logarithmic ratio of the two temperature maps generated by the GSM at 408 and 230 MHz, modulated by their reference frequency ratio.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Relationships between intrinsic properties (age, metallicity, and color in the top, middle, and bottom panels, respectively) of the centrals (or satellites, diffuse light) and dark matter halo mass M 200. Each panel shows the results for the centrals, satellites, and diffuse light, represented by the red, green, and blue open circles, respectively. The panels from left to right to show the results at redshifts z = 0.1, 0.3, 0.5, and 1.0. The error bars represent the standard deviations.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: A comparison of the reconstructed intrinsic foreground as determined by the best-fit nonlinear parameters from fits to the convolved spectra. The left panel shows the rms error in the reconstruction (as computed with respect to the input intrinsic foreground) as a function of frequency, where the different colors (red, purple, and cyan) label the different LST bin cases (1, 2, and 5, respectively). The triangle symbols label models that were selected as best fits via the K-S test, whereas the squares denote models selected using the Bayesian evidence. The black lines correspond to the ideal case, without the beam or averaging over the sky, by using the mean spectral index in the input intrinsic foreground for each spectral region, with the number of regions N  r  = 4, 8, and 9, for 1, 2, and 5 LST bins, respectively. The right panel shows the reconstructions of the foreground as a function of LST for the models selected via the K-S test. The gray band shows the input intrinsic foreground. The top (bottom) of the band corresponds to the lowest (highest) frequencies.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Number distributions of galaxy properties are shown in each panel, with the fraction normalized by dividing by the maximum number in the value bins. The solid lines represent Gaussian fits to the distributions. In each panel, the red, green, and blue open circles represent the results for the centrals, satellites, and diffuse light, respectively. The panels from left to right correspond to the results at redshifts z = 0.1, 0.3, 0.5, and 1.0.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Bayesian evidence as a function of the number of regions of the sky N  r  and the number of LST bins (compare to the top panel of Figure 5). For each line style, the legend shows the relative size of the FWHM of the analytical Gaussian beam as a quadratic function of the band. The first number refers to the degree of the FWHM of the beam in the low band, while the second number shows the high band. The dotted and dashed lines therefore have smaller beams across the band than the solid line. For the 1 and 2 LST bins (blue and orange contours), the best-fit number of regions saturates to the same value of N  r  quickly, regardless of the size of the beam. However, when the number of LST bins increases to 5 or 10, the best-fit (according to the highest evidence) number of regions N  r  increases dramatically for beams that have smaller FWHMs across the band (dotted and dashed lines).
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Example triangle plot for the 2 LST bin case, showing the best-fit spectral indices for each region, N  r  = 1–8. The blue contours correspond to the best-fit model selected by the evidence, while the orange contours correspond to the model selected by the K-S test. The black contours show the input mock distribution for the intrinsic foreground, as generated from the GSM. Contours that are closer to the center of the mock distribution represent better fits to the intrinsic foreground, but not necessarily to the spectra that result from convolving the foreground with a beam.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Illustration of the luminosity profile of a dark matter halo with a virial radius of around 1.15h −1 Mpc and mass M 200 of .96 × 1014  M ⊙ at redshift z = 0.1. The projection of this halo is shown on the x–y plane, with each side of the square being approximately 1.0h −1 Mpc and centered at the center of mass. Left: total luminosity profile of the halo; right: luminosity of the halo after applying a mask that excludes the galaxies defined by the SBLSP method. The color bar represents the surface brightness in the V band.
Paper: Fitting and Comparing Galactic Foreground Models for Unbiased 21 cm Cosmology
Authors: Joshua J. Hibbard, David Rapetti, Jack O. Burns, Nivedita Mahesh, Neil Bassett
Figure caption: Panel (a) shows several example residuals produced from fitting polynomial models to the REACH mock. The solid (dashed) lines denote 5 (9) term fits. The input noise level is shown as a solid black line, while the red, cyan, and magenta lines denote the linear physical, linear-logarithmic, and linear polynomial models, respectively. Panel (b) shows similar example residuals for the maximally smooth polynomials, with solid (dashed) lines for 5 (10) parameter fits. Blue denotes the difference in the polynomial model and the orange line denotes the difference in the log-log polynomial model.
Paper: Mock Observations: Formation and Evolution of Diffuse Light in Galaxy Groups and Clusters in the IllustrisTNG Simulations
Authors: Lin Tang, Weipeng Lin, Yang Wang, Jing Li, Yanyao Lan
Figure caption: Relationships between the dark halo mass M 500 and the stellar masses of the centrals (left panel), total satellites (middle panel), and diffuse light (right panel) within dark matter halos at redshift z = 0.1. The gray points represent the results for each component in the dark matter halos. The open circles with error bars indicate the average values within the mass bins, and the solid lines represent the fitting results. The error bars show the standard deviations of the data points.
Paper: The Effect of Magnetic Field Line Topology on ICME-related GCR Modulation
Authors: Emma E. Davies, Camilla Scolini, Réka M. Winslow, Andrew P. Jordan, Christian Möstl
Figure caption: In situ data for the ICME on 2022 March 31–April 1. The first panel shows the Wind magnetic field data in RTN coordinates, with B  R  in red, B  T  in green, and B  N  in blue. The magnetic field magnitude B and its negative −B are in black. The same color-coding for the magnetic field data is used in the following figures as well. The second panel shows the SOPO neutron monitor data. The linear fits to the FD steps, initial recovery, and second recovery are presented by the light-blue, red, and dark-orange lines, respectively. The third, fourth, and fifth panels show the Wind proton bulk speed, number density, and proton β, respectively. The sixth and seventh panels show the Wind suprathermal electron PAD between 136 eV and 2 keV in normal and normalized forms (normalizing the maximum intensity at each time stamp to 1). The eighth plot reports the periods of BDE detection (in black), while data gaps in PAD are indicated in pink. The vertical magenta lines denote the shock time (dashed line) and the FR (solid lines) boundaries, while the orange vertical lines denote the SOPO FD start, step times, and the end of the initial recovery associated with the passage of the FR (solid), respectively, and the minimum of the FD (dashed). Wind data and ICME boundaries have been time-shifted to Earth as described in Section 2.2.
Paper: The Effect of Magnetic Field Line Topology on ICME-related GCR Modulation
Authors: Emma E. Davies, Camilla Scolini, Réka M. Winslow, Andrew P. Jordan, Christian Möstl
Figure caption: In situ data for the ICME on 2002 September 30–October 1. The first panel shows the ACE magnetic field data in RTN coordinates, using the same colors as in Figure 1. The second panel presents the SOPO neutron monitor data and fits to the FD steps and recoveries, as in Figure 1. The third, fourth, fifth, and sixth panels show the ACE proton bulk speed, number density, temperature, and proton β, respectively. The seventh, eighth, and ninth panels show the ACE suprathermal electron PAD at 272 eV and the BDE detection in a similar format to that in Figure 1. The vertical magenta lines denote the shock time (dashed line) and the FR (solid lines) boundaries, while the orange vertical lines denote the SOPO FD start and the end of the initial recovery associated with the passage of the FR (solid), respectively, and the minimum of the FD (dashed). ACE data and ICME boundaries have been time-shifted to Earth as described in Section 2.2.
Paper: The Effect of Magnetic Field Line Topology on ICME-related GCR Modulation
Authors: Emma E. Davies, Camilla Scolini, Réka M. Winslow, Andrew P. Jordan, Christian Möstl
Figure caption: In situ data for the ICME on 2005 May 15–17. ACE data and SOPO neutron monitor data are shown in the same format as in Figure 2. ACE data and ICME boundaries have been time-shifted to Earth as described in Section 2.2.
Paper: The Effect of Magnetic Field Line Topology on ICME-related GCR Modulation
Authors: Emma E. Davies, Camilla Scolini, Réka M. Winslow, Andrew P. Jordan, Christian Möstl
Figure caption: In situ data for the ICME on 2004 November 9–10. ACE data and SOPO neutron monitor data are shown in the same format as in Figure 2. ACE data and ICME boundaries have been time-shifted to Earth as described in Section 2.2.
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: [X/Fe] derived abundances for J0117 (black square) compared to the abundances of UFD galaxies (colored dots; see text for references 4) and stars from the MW halo (gray dots; Roederer et al. 2014). J0117 follows the general abundance trends of what is seen in most UFD galaxy stars.
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: Left: LTE [K/Fe] abundances for J0117 (black square), UFDs (colored dots; see Figure 2 for the legend), and MW halo (gray dots) stars. Middle: NLTE-corrected [K/Fe] abundances for J0117, UFDs, and MW halo stars. Right: NLTE-corrected [K/Fe] abundances for J0117, MW halo stars, GC stars (colored x), and stars from stellar streams with GC progenitor (colored diamonds). There is an offset in [K/Fe] abundance between some UFD galaxies and the average value for MW halo stars. The GC and stellar stream [K/Fe] abundances also mostly overlap with the MW halo stars and are lower than what is seen in UFD galaxy stars.
Paper: Chemical Analysis of the Brightest Star of the Cetus II Ultrafaint Dwarf Galaxy Candidate 
Authors: K. B. Webber, T. T. Hansen, J. L. Marshall, J. D. Simon, A. B. Pace, B. Mutlu-Pakdil, A. Drlica-Wagner, C. E. Martínez-Vázquez, M. Aguena, S. S. Allam, O. Alves, E. Bertin, D. Brooks, A. Carnero Rosell, J. Carretero, L. N. da Costa, J. De Vicente, P. Doel, I. Ferrero, D. Friedel, J. Frieman, J. García-Bellido, G. Giannini, D. Gruen, R. A. Gruendl, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, J. Mena-Fernández, F. Menanteau, R. Miquel, R. L. C. Ogando, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, E. Sanchez, B. Santiago, J. Allyn Smith, M. Smith, E. Suchyta, G. Tarle, C. To, N. Weaverdyck, B. Yanny
Figure caption: [X/Fe] derived neutron-capture element abundances for J0117 (black square) compared to the abundances of other UFD galaxies (colored dots; see text for references and Figure 2 for the legend) and stars from the MW halo (gray dots; Roederer et al. 2014). The upper limits are designated with downward-pointing triangles. J0117 has low abundances of neutron-capture elements, which is characteristic of most UFD galaxies.