adsabs/AstroCLIMB huggingface dataset:
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Log-scale posterior distributions for the gap depth inferred from five mock catalogs containing a mass gap, each with 250 perfectly measured events (see Figure 5). Note that the posterior support for A = 0 is vanishingly small in the purple catalog, explaining the extreme values of ﹩\mathrm{ln}{{ \mathcal B }}_{A}﹩ and ﹩\mathrm{ln}{{ \mathcal B }}_{\mathrm{empty}}﹩.
Paper: No Evidence for a Dip in the Binary Black Hole Mass Spectrum
Authors: Christian Adamcewicz, Paul D. Lasky, Eric Thrane, Ilya Mandel
Figure caption: Posterior distributions for gap-related population hyperparameters inferred using GWTC-3 data, including the edge sharpness. The values listed above give the median and 90% credible intervals on these posteriors. The contours on the two-dimensional panels give the 50%, 90%, and 99% credible intervals. The priors are overplotted in gray.
Paper: Alleviating H 0 and S 8 Tensions Simultaneously in K-essence Cosmology
Authors: Seyed Ali Hosseini Mansoori, Hossein Moshafi
Figure caption: Alleviating the Hubble Tension in ϕ 2/3 model. (Upper) One-dimensional posteriors of the H 0 parameter are shown for the different combination of the data set. (Lower) 68% and 95% confidence level constraints on H 0 vs. Ω m  for the model. The shaded area shows the measurement of H 0 done by the SH0ES team and its 1σ and 2σ errors (A. G. Riess et al. 2022).
Paper: Alleviating H 0 and S 8 Tensions Simultaneously in K-essence Cosmology
Authors: Seyed Ali Hosseini Mansoori, Hossein Moshafi
Figure caption: Marginalized joint 68% and 95% CL regions for the cosmological parameters in the ϕ 2/3 model with PlanckTT, EE, and TE, with the EE likelihood at low multipoles joint with R21 prior on H 0 and BAO+SN data. The shaded area depicts the 1σ and 2σ error bars of the Hubble parameter measured by A. G. Riess et al. (2022).
Paper: Alleviating H 0 and S 8 Tensions Simultaneously in K-essence Cosmology
Authors: Seyed Ali Hosseini Mansoori, Hossein Moshafi
Figure caption: Marginalized joint 68% and 95% CL regions for n  s  and r for the ϕ 2/3 and ϕ 2 models from Planck 2018+lensing in comparison with BK18+BAO data (P. A. R. Ade et al. 2021).
Paper: Alleviating H 0 and S 8 Tensions Simultaneously in K-essence Cosmology
Authors: Seyed Ali Hosseini Mansoori, Hossein Moshafi
Figure caption: Two-dimensional contour plots at 1σ and 2σ confidence levels for S 8 vs. Ω m  for the ϕ 2/3 model to compare analyses based on CMB data and DES data.
Paper: Ultraviolet Flux and Spectral Variability Study of Blazars Observed with UVIT/AstroSat
Authors: M. Reshma, Aditi Agarwal, C. S. Stalin, Prajwel Joseph, Akanksha Dagore, Amit Kumar Mandal, Ashish Devaraj, S. B. Gudennavar
Figure caption: Comparison plot of FUV light curve for the source 1ES 1218+304 in F148W filter with top panel denoting Photutils light curve, middle panel denoting Curvit light curve, and bottom panel denoting the difference between Photutils and Curvit light curves.
Paper: Ultraviolet Flux and Spectral Variability Study of Blazars Observed with UVIT/AstroSat
Authors: M. Reshma, Aditi Agarwal, C. S. Stalin, Prajwel Joseph, Akanksha Dagore, Amit Kumar Mandal, Ashish Devaraj, S. B. Gudennavar
Figure caption: The observed FUV field images of the ten blazar sources. The target sources are shown in green circles. The source name and the corresponding filter name are given in each field image. Each image has a field of view of ∼28′ diameter.
Paper: Ultraviolet Flux and Spectral Variability Study of Blazars Observed with UVIT/AstroSat
Authors: M. Reshma, Aditi Agarwal, C. S. Stalin, Prajwel Joseph, Akanksha Dagore, Amit Kumar Mandal, Ashish Devaraj, S. B. Gudennavar
Figure caption: CMDs for the sources that are variable and have more than four simultaneous FUV and NUV photometric data points. The best-fit line from Bayesian analysis using LINMIX _ ERR is shown by the dashed blue line, and the uncertainty range on the best fit is shown by the blue shaded region. The intrinsic scatter (σ) is given in the respective plots. The names of the sources are given on the top of each panel (see also Tables 5 and 6).
Paper: Ultraviolet Flux and Spectral Variability Study of Blazars Observed with UVIT/AstroSat
Authors: M. Reshma, Aditi Agarwal, C. S. Stalin, Prajwel Joseph, Akanksha Dagore, Amit Kumar Mandal, Ashish Devaraj, S. B. Gudennavar
Figure caption: FUV and NUV light curves of sources. Here, red dots denote FUV light curves, and green dots denote NUV light curves. The respective source name and observation ID are mentioned on top of each plot. Also, the names of the filters used for the light curves are given in each panel.
Paper: Ultraviolet Flux and Spectral Variability Study of Blazars Observed with UVIT/AstroSat
Authors: M. Reshma, Aditi Agarwal, C. S. Stalin, Prajwel Joseph, Akanksha Dagore, Amit Kumar Mandal, Ashish Devaraj, S. B. Gudennavar
Figure caption: FUV and NUV light curves (represented by red and green circles, respectively) of sources. The observation ID and source name are labeled in each plot. The name of the filters used for the light curves is given in each panel.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Lifetime SFH metrics vs. in-plane distance from the center of the LMC, assuming viewing angles from Y. Choi et al. (2018a) and the LMC center location based on H I kinematics. From top to bottom, the plots show the trend in look-back time by which 90%, 75%, and 50% of the cumulative stellar mass had formed. In the left column, individual fields are color-coded by their position angle east of north, with symbols as in Figure 7. In the right column, our fields are shown in gray and values for M33 (M. K. Barker et al. 2007, 2011; B. F. Williams et al. 2009) are overplotted in red, with deprojected radial distances normalized to the disk scale length h  r  for each galaxy. These results assume PARSEC evolutionary models, and in Appendix C we demonstrate that the inversion in radial age trends, as well as its constancy over the range of look-back times shown here, is robust to choice of stellar evolutionary models and adopted LMC center location.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Top row: comparison between the best-fitting distance from our MATCH SFH fits and the distance (and uncertainty) measured independently from the red clump in SMASH photometry as in Y. Choi et al. (2018a). Differences are plotted as a function of median line-of-sight extinction to the LMC red clump in each field from Y. Choi et al. (2018a), and points are color-coded by the line-of-sight extinction internal to the LMC = (σ 1 + σ 2) from D. M. Skowron et al. (2021). Distance offsets, shown for three different evolutionary models from left to right, are smaller than the red clump distance uncertainties and uncorrelated with total or differential extinction. The dashed line and dark colored shading in each panel represent the (inverse-square-weighted) mean and its standard deviation, and the lighter shading indicates the standard deviation of the individual offsets. Bottom row: difference between the best-fit extinction from MATCH and the median extinction measured using LMC red clump stars as in Y. Choi et al. (2018a). Because MATCH fits for both the foreground Galactic extinction A  V,fg and additional internal differential extinction δ A  V , the vertical location of the filled circles corresponds to the best-fit foreground Galactic extinction A  V,fg and the vertical lines represent the best-fitting additional differential extinction δA  V  internal to the LMC for each field from our SFH fits, illustrated in the box in the bottom-left panel. When considering both foreground and internal extinction resulting from our SFH fits with MATCH, our results are in good agreement with the independent red-clump-based measurements of the median extinction, with outliers at the ≲0.3 mag level (see text for discussion).
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Left: radial profiles of cumulative stellar mass surface density color-coded by three example look-back times, including the present day. Exponential fits to fields inside R break (dashed lines) are essentially identical to fits to the full sample (solid lines), but fits to the fields at R > R break (dotted lines) are flatter. Middle: the evolution of the best-fit exponential disk scale length h  r  with look-back time, shown for fits to the full sample (solid line) and fields inside R break (dashed line), offset by intervals of 0.15 Gyr to avoid overlapping error bars. Fits to LMC fields with R > R break are not shown since they all yield h  r  > 2.6 kpc owing to the flattening of the profile seen in the left panel, with large (>25%) uncertainties (see Table 6). Values for M33 (B. F. Williams et al. 2009) and NGC 300 (S. M. Gogarten et al. 2010) are overplotted. When viewed globally, the LMC, M33, and NGC 300 all show approximately constant h  r  over time, but unlike the LMC, the inner disk of M33 has grown over time, possibly due to its different interaction history. Right: the evolution of the best-fitting central surface density, using the same symbols as in the middle panel. Trends for the LMC are similar to those for M33 when fit as a single sample across R break, but the outer region of the LMC disk and the inner region of M33's disk deviate from these trends, also possibly reflecting different interaction histories.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: The look-back time to form 90% of each field’s cumulative stellar mass (denoted τ 90) as a function of in-plane distance from the center of the LMC. We compare trends assuming the R. P. van der Marel & M.-R. L. Cioni (2001) isopleth-based center location (left panel) vs. the H I kinematic center we adopt (right panel). Individual fields from this study are shown as filled circles, color-coded by their position angle east of north relative to the adopted center. The subset of our fields located in the southeast disk (corresponding to the magenta dashed lines in Figure 1) are circled in magenta. Literature results from the ground-based fields of L. Monteagudo et al. (2018) and I. Meschin et al. (2014) are overplotted as green diamonds and stars, respectively. The location of the inversion in radial age trends R inv is shown as a vertical dashed brown line. Radial profiles of H I column density (S. Kim et al. 2003) in azimuthal slices are shown as lines, also color-coded by position angle, corresponding to the right-hand vertical axis. Radial trends for both the per-field τ 90 values from our SFH fitting and the H I column density profiles show less scatter when adopting the H I kinematic center, consistent with models predicting that LMC–SMC-like interactions can produce an offset photometric distribution.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Results of SFH fits for two example fields with data quality typical of our sample, LMC_9 (top row) and LMC_M26 (bottom row). These fits assume PARSEC stellar evolutionary models, although we also perform SFH fits for all fields assuming two additional sets of evolutionary models. Each row shows, from left to right, Hess diagrams (i.e., two-dimensional binned color–magnitude histograms) of the observed sample used for SFH fitting (including only stars brightward of the 80% completeness limit, ascertained from artificial star tests), the best-fit model, and the statistical significance of the fit residuals in terms of Poisson standard deviations, in the sense (observed − model). The middle panel in each row shows the best-fit AMR, and the right panel shows the best-fit CSFH, with 1σ uncertainties enclosed by gray shading, including both random and systematic uncertainty contributions. In the right panel, the CSFH metrics we use are illustrated, using a different color for each: the vertical solid lines indicate the look-back times τ 50, τ 75, and τ 90, by which 50%, 75%, and 90% of the total stellar mass ever formed had already been formed. The shading around each vertical line indicates the uncertainties on these CSFH metrics, inferred directly from the uncertainties on the CSFH.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Photometric completeness vs. magnitude in the bluer of the two filters (top) and F814W (middle). Completeness curves are shown for each individual field, color-coded to indicate whether that field was observed as part of our Scylla program, or incorporated from archival METAL or LGSPA imaging. The panels in the bottom row illustrate the distribution of the faint magnitude limits imposed for SFH fitting (C80, corresponding to the 80% faint completeness limit) compared to the metal-poor oMSTO (13 Gyr, [M/H] = −1) from a PARSEC isochrone, calculated using per-field distance and extinction values.
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Fraction of total mass formed from 0.1 to 2.5 Gyr ago in each field, as a function of deprojected in-plane radius from the kinematic center of the LMC. Fields located in the northern spiral arm are shown in orange (and enclosed by the orange dashed line in Figure 1), supporting the stability of the arm on a ∼2.5 Gyr timescale observed by T. Ruiz-Lara et al. (2020).
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Comparison of combined CSFH for all WFC3/UVIS (i.e., Scylla and METAL) fields (purple) and all archival WFPC2 LGSPA fields (orange), showing no apparent dependence of recovered SFHs on observing setup for any of the three assumed evolutionary libraries (shown from left to right).
Paper: Scylla. II. The Spatially Resolved Star Formation History of the Large Magellanic Cloud Reveals an Inverted Radial Age Gradient
Authors: Roger E. Cohen, Kristen B. W. McQuinn, Claire E. Murray, Benjamin F. Williams, Yumi Choi, Christina W. Lindberg, Clare Burhenne, Karl D. Gordon, Petia Yanchulova Merica-Jones, Karoline M. Gilbert, Martha L. Boyer, Steven Goldman, Andrew E. Dolphin, O. Grace Telford
Figure caption: Comparison of CSFH (top row) and AMR (bottom row) for two fields (LMC_20 and LMC_24) that were observed, reduced, and analyzed separately but have >90% spatial overlap. Both the CSFHs and AMRs agree to within their 1σ uncertainties, represented by the shaded regions, for all three assumed isochrone libraries (shown from left to right).
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Best-fit two-temperature H2O model parameters for each disk in our sample. Error bars correspond to the 0.16 and 0.84 percentiles. Observable masses are calculated as the product of column density, emitting area, and molecular weight. The disks are listed in ascending R dust order from left to right, and the dashed lines separate compact and extended disks . Note that sometimes the error bars are smaller than the marker.
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The velocity field distributions of the seven identified ARs. The horizontal velocity is drawn by the purple arrows in these ARs. The obvious saturation effect is shown in these sunspots at the center of NOAA 8375, 9236, and 10930 due to filter magnetic measurements. The magnetic field saturates at ±0.06 Ic of polarization degree for NOAA 10930 and at ±1000 G for the other ARs. The spatial scale of 20″ and the velocity of 0.1 km s−1 are shown by the lengths of the black line and the purple arrow in the left lower corner.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Power-law H2O column density (top) and excitation temperature (bottom) profiles fit to each disk in the sample. The solid lines correspond to the median profiles generated from posterior samples, while the shaded regions indicate the 0.16 and 0.84 percentiles at each radius. The profiles are truncated at 150 K. The dashed-line portions correspond to the regions where the modeled H2O emission lies below the detection threshold (see Section 4.1).
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The relationship between flares and BMEs. Panels ((a1)–(a4)), ((b1)–(b4)), and ((c1)–(c4)) show the UV image evolutions for three flares in NOAA 12158, and the initial brightening associated with the BMEs are indicated by the green arrows. The light curve of the soft X-ray in 1.0–8.0 A is displayed in the bottom panel, and the three flares are plotted by the vertical lines with different colors. In addition, the different vertical lines in the same color correspond to the times of UV images shown in the upper panels. The vertical fields are shown by the contour lines of 300 G and 1000 G, and the red and purple contour lines indicate the positive and negative fields, respectively.
Paper: Are There Local Dynamos Acting in Sunspot Regions?
Authors: Chunlan Jin, Guiping Zhou, Haisheng Ji, Jingxiu Wang
Figure caption: The cartoon of twisting-reconnecting dynamo model in the sunspot region. The stars in panel (C) indicate the interaction regions between these peculiar BMEs and the sunspot radial fields. The dark gray region indicates the sunspot area on the solar surface, and the light gray region represents the peripheral area of the sunspot. The e  z  indicates the direction from the solar interior to the solar surface.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Best-fit two-temperature H2O model to the compact disk of GQ Lup. The data are shown in black, the total model is shown in violet, and the individual contributions of the cold and hot H2O components are shown in blue and magenta, respectively, shifted vertically for clarity. Regions where the emission is blended with OH or organics are labeled.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Same as Figure 3, but for the extended disk of CI Tau. Note that, unlike GQ Lup, the spectrum of CI Tau is dominated by the hot H2O component even at longer wavelengths.
Paper: Retrieval of Thermally Resolved Water Vapor Distributions in Disks Observed with JWST-MIRI
Authors: Carlos E. Romero-Mirza, Andrea Banzatti, Karin I. Öberg, Klaus M. Pontoppidan, Colette Salyk, Joan Najita, Geoffrey A. Blake, Sebastiaan Krijt, Nicole Arulanantham, Paola Pinilla, Feng Long, Giovanni Rosotti, Sean M. Andrews, David J. Wilner, Jenny Calahan
Figure caption: Continuum-subtracted MIRI-MRS spectra of each of the disks in the sample, vertically shifted for clarity. The blue shaded regions indicate the wavelength regions excluded from our analysis owing to rovibrational emission (<12 μm) or larger noise (>27 μm).
Paper: To High Redshift and Low Mass: Exploring the Emergence of Quenched Galaxies and Their Environments at 3 < z < 6 in the Ultra-deep JADES MIRI F770W Parallel
Authors: Stacey Alberts, Christina C. Williams, Jakob M. Helton, Katherine A. Suess, Zhiyuan Ji, Irene Shivaei, Jianwei Lyu, George Rieke, William M. Baker, Nina Bonaventura, Andrew J. Bunker, Stefano Carniani, Stephane Charlot, Emma Curtis-Lake, Francesco D'Eugenio, Daniel J. Eisenstein, Anna de Graaff, Kevin N. Hainline, Ryan Hausen, Benjamin D. Johnson, Roberto Maiolino, Eleonora Parlanti, Marcia J. Rieke, Brant E. Robertson, Yang Sun, Sandro Tacchella, Christopher N. A. Willmer, Chris J. Willott
Figure caption: Properties of robust poststarburst galaxies selected via B19. Top rows for each source: F606W, F090W, F200W, F444W, F770W cutouts, 1.″2 on a side. Bottom rows for each source: the SEDs (left), SSFR posterior distributions (middle), and SFHs (right).