adsabs/AstroCLIMB huggingface dataset:
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Effect of the SW background estimate on the mass and radius posterior distributions using the W21 data set conditional on the ST-U model. Also, the posteriors for compactness GM/R eq c 2 are shown (hereafter and in the figure referred as M/R eq, i.e., assuming c = 1 and G = 1). Four types of posterior distribution are shown: one conditional on the NICER likelihood function with a smoothed SW background lower bound (STU-W21-0.9xSWs); one similar but with a non-smoothed lower bound (STU-W21-0.9xSW); one conditional on NICER likelihood function without background constraints (STU-W21); and one conditional on the NICER and XMM-Newton likelihood function (STU-W21+XMM). The last two are from R21. The marginal prior PDFs are shown by the dashed–dotted functions. We report the credible intervals and the Kullback–Leibler divergence D KL for the NICER posterior conditional on the smoothed SW estimate lower bound (for the other cases, see Table 6). The shaded intervals contain 68.3% of the posterior mass, and the contours in the off-diagonal panels contain 68.3%, 95.4%, and 99.7% of the posterior mass. See the caption of Figure 5 of R21 for additional details about the figure elements.
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Effect of 3C50 data selection on the mass and radius posterior distributions conditional on the ST-U model. Three types of posterior distribution are shown: one conditional on the NICER likelihood function using 3C50 data set; one conditional on the NICER likelihood function using the W21 data set; one conditional on NICER W21 data and XMM-Newton likelihood function (the latter two are the same as in Figure 5). We report the credible intervals and the divergence estimates for the NICER posterior conditional on the 3C50 data set. See the caption of Figure 5 for additional details about the figure elements.
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Effect of antipodality on the mass and radius posterior distributions conditional on 3C50 with (n l = 3 and n u = ∞) background limits and XMM-Newton likelihood function. Three types of posterior distribution are shown: one conditional on the ST-U model; one conditional on the ST-Ua model; and one conditional on the ST-S model. The credible intervals and the divergence estimates are reported for the NICER posterior conditional on the ST-S model (for the other cases, see Table 10). See the caption of Figure 5 for additional details about the figure elements.
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Prior limits for the background of the W21 data set. The count-rate spectrum and the SW background estimate are shown with blue and red step functions as in Figure 1. The black dashed step function is the estimate multiplied with a factor of 0.9, and a smoothed version of that is shown with a magenta step function. These two rescaled estimates were used as lower limits ﹩\{{\mathfrak{L}}\}﹩ for the joint prior PDF of the expected count-rate variables ﹩\{{\mathbb{E}}[{b}_{{\rm{N}}}]\}﹩ (see Equation (2)).
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: NICER count-rate spectrum of PSR J0740+6620 as a function of detector channel nominal photon energy (i.e., the PI value from the event file divided by 100). The blue solid and the black dashed step functions represent the spectrum for W21 and 3C50 data sets, respectively. The former is the same as used in R21, Miller et al. (2021a). The space weather background estimate (specific for the W21 data) is shown with a red solid step function, and the 3C50 background estimate (specific for the 3C50 data) is shown with an orange dashed step function.
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: Summary of the medians and 68.3% credible intervals for radius using two circular hot spot model ST-U with different data sets and treatments for the background modeling. Purple dots and lines correspond to the results obtained using X-PSI with models described in Tables 6–9 and the associated figures in Section 4. Blue dots and lines correspond to the results obtained using the independent Illinois–Maryland code with the models described in Appendix B, Table 4, and Table 5.
Paper: The Radius of PSR J0740+6620 from NICER with NICER Background Estimates
Authors: Tuomo Salmi, Serena Vinciguerra, Devarshi Choudhury, Thomas E. Riley, Anna L. Watts, Ronald A. Remillard, Paul S. Ray, Slavko Bogdanov, Sebastien Guillot, Zaven Arzoumanian, Cecilia Chirenti, Alexander J. Dittmann, Keith C. Gendreau, Wynn C. G. Ho, M. Coleman Miller, Sharon M. Morsink, Zorawar Wadiasingh, Michael T. Wolff
Figure caption: The 1D posterior probability density of the equatorial circumferential radius of PSR J0740-6620 inferred using the Illinois–Maryland analysis pipeline. Each line is an averaged shifted histogram (e.g., Scott 1985) of the posterior samples from the converged portion of an MCMC analysis. Blue solid lines illustrate the results from Miller et al. (2021a), which analyzed the W21 data set. Green dashed lines illustrate the results from analyses that used the 3C50-selected NICER data, but did not incorporate the 3C50 background estimate as a lower limit; and orange dashed–dotted lines illustrate results from analyses, which used the 3C50-selected NICER data set and incorporated the 3C50 background estimate, with uncertainties, as a lower limit on the NICER background. The top panel includes results from analyses of NICER data alone, while the bottom panel includes results derived using both NICER and XMM data.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Cosmic star formation rate density (SFRD) history. Our SFRD history is shown with filled circles in all panels and is obtained from the combined COSMOS-XS + VLA-COSMOS 3 GHZ data sets (assuming density+luminosity evolution). The study of Madau & Dickinson (2014) is shown as a red line in all panels. All data shown for comparison are indicated in the legend of each panel; see text for details. The comparison of radio- and UV-based SFRDs, integrated down to the same limit, in panel (c), shows that the UV-based SFRD from Bouwens et al. (2020) falls ∼1 dex below the radio SFRD at z  ≳ 2.8. This suggests that the bulk of the star formation contributed by high-luminosity sources at high redshifts is not accounted for by dust corrections.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Radio LFs of SFGs in different redshift bins compared to UV LFs from the literature. Our best-fit luminosity + density function in each redshift bin is shown with the solid black line. The shaded areas show the 1σ confidence interval for the best-fit functions. We compare our data with the UV LFs from Mehta et al. (2017), Ono et al. (2018), and Bouwens et al. (2021). The redshift range and median redshift are given in each panel. The best-fit pure local LF for the data from Bouwens et al. (2021) at z ∼ 4.6 is shown with the dashed red line, while the solid red line shows the joint fit to the UV+radio data discussed in Section 4.3. The comparison of these two fits in the last panel suggests that, at the highest redshifts probed here (3.3  < z < 4.6), the UV data underestimate the integrated LF by at least 22% ± 14% where the LF is integrated from ﹩{L}_{z=3}^{\star }﹩, which corresponds to ﹩{\mathrm{log}}_{10}{L}_{1.4\,\mathrm{GHz}}=21.14\,{\mathrm{WHz}}^{-1}﹩, to ∞ .
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: The best-fit parameters for the luminosity functions as a function of redshift. The upper panel shows the evolution of the luminosity parameter α  L . The lower panel shows the evolution of the density parameter α  D . Open circles correspond to pure luminosity evolution for the COSMOS-XS survey. The red dashed line shows the fitted evolution to these points of the form α  L  + z β. The green dashed line shows the simple pure luminosity evolution model described by Novak et al. (2017). The luminosity parameter shows a similar evolution as the evolution that Novak et al. (2017) described. The filled symbols correspond to the joint COSMOS-XS + VLA-COSMOS 3 GHz data. The red and blue filled symbols correspond to the best-fit parameters found for, respectively, the pure luminosity evolution and the luminosity and density evolution fitted to the joint sample. The density parameter shows a strong evolution while we observe little evolution in the luminosity parameter.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Radio LFs of SFGs in COSMOS-XS in different redshift bins. The best-fit pure luminosity function in each redshift bin is shown by the red lines, and the shaded area shows the 1σ confidence interval. The local radio LF is shown for reference as a solid purple line. We compare our data with the radio LFs from Smolčić et al. (2009), Novak et al. (2017). The redshift range and median redshift are given in each panel.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: The impact of the fitted LF form and assumed FIR–radio correlation on the derived cosmic star formation rate density (SFRD). The left panel shows the effect of fitting pure luminosity evolution compared to the preferred model of density+luminosity evolution (assuming the same FIR–radio correlation). The right panel shows the SFRD obtained from the combined COSMOS-XS + VLA-COSMOS 3 GHZ data sets (assuming density+luminosity evolution) but for different assumed FIR–radio correlations. This gives an indication of the impact an assumed FIR–radio correlation has. The study of Madau & Dickinson (2014) is shown as a red line in both panels. In the remainder of the paper, we convert our radio LFs to SFRD using the Delvecchio et al. (2021) FIR–radio correlation.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Radio LF of SFGs in different redshift bins for the combined COSMOS-XS + VLA-COSMOS 3 GHz data sets derived using SFGS selected with an evolving FIR–radio correlation. Our best-fit density+luminosity function in each redshift bin is shown with solid lines. The redshift range and median redshift are given in each panel. The open circles show the radio LF of SFGs selected with a constant FIR–radio correlation. The small difference between the open and closed circles shows that the influence of our selection criterion used to select SFGs on the derived LF is small. We also show the LFs from Gruppioni et al. (2013), converted as described in Section 4.2 to radio LFs. The open symbols are converted assuming a constant FIR–radio correlation of 2.64 (Bell 2003), and the filled symbols are converted assuming an evolving FIR–radio correlation. The difference between the open and filled symbols shows the influence of the FIR–radio correlation on the comparison between the radio LF and FIR LF. The FIR–radio correlation remains the largest uncertainty in this comparison.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Radio LFs of SFGs in different redshift bins for the combined COSMOS-XS + VLA-COSMOS 3 GHz data sets compared to various FIR LFs from the literature. Our best-fit luminosity + density function in each redshift bin is shown with the black lines. We show FIR LFs from Gruppioni et al. (2013), Koprowski et al. (2017), Gruppioni et al. (2020), and Lim et al. (2020). The LFs of the theoretical study by Casey et al. (2018) for the dust-poor model and the dust-rich model are also shown. The redshift range and median redshift are given in each panel. Our best-fit luminosity + density function is roughly consistent, within the error bars, with the FIR LFs. At z > 2, our LFs are systematically lower than the FIR studies expect for the result from Koprowski et al. (2017). Our best-fit function is most consistent with the dust-poor model from Casey et al. (2018) at z ∼ 4.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: Radio LFs of SFGs in different redshift bins from the combined sample of the COSMOS-XS + VLA-COSMOS 3 GHz data sets compared with the radio LFs from Smolčić et al. (2009), Novak et al. (2017). Our best-fit pure luminosity function and best-fit density + luminosity function in each redshift bin are shown with solid red and blue lines, respectively, where the shaded areas show the 1σ confidence interval for the best-fit functions. The local radio luminosity function is shown as the purple line for reference. The redshift range and median redshift are given in each panel.
Paper: An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History
Authors: D. van der Vlugt, J. A. Hodge, H. S. B. Algera, I. Smail, S. K. Leslie, J. F. Radcliffe, D. A. Riechers, H. Röttgering
Figure caption: X-ray luminosity derived via X-ray stacking vs. FIR luminosity, a proxy for star formation rate, for the star-forming sample, binned in four redshift bins. Circles represent detections whereas the second-highest data point is an upper limits indicated with the upside down triangle. The solid line represents the L X − L IR relation from Symeonidis et al. (2014). The dashed line shows the 2σ scatter around this relation. The binned data fall within the scatter range from the trend from Symeonidis et al. (2014), indicating no appreciable contribution from AGN.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: A schematic picture of the proposed scenario. The 56Ni-rich, Si-rich (including Ca), and C+O-rich materials are (schematically) shown in red, blue, and green, respectively. (a) As the outcome of the initial thermonuclear explosion, 56Ni-rich materials are ejected as the (first) unbound ejecta. The radioactive decay of 56Ni/Co/Fe chain within the bound WD remnant keeps energizing the outer region of the bound WD (or the envelope; indicated by solid arrows). (b) The 56Ni/Co heating creates the second unbound ejecta (i.e., the inner component) in about a month. By this time, the outer ejecta become transparent, and the second ejecta controls the optical output (indicated by dashed arrows). The 56Ni/Co left deep within the WD keeps energizing the bound WD further. (c) The bound WD has further puffed up. When the photons start diffusing out even from the bound WD about 1 yr after the initial explosion, the expansion is virtually stopped. The photons originally emitted from the bound WD start contributing to the optical output.
Paper: The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies
Authors: Huanian Zhang, 华年 张, Dennis Zaritsky
Figure caption: In the top panel we show a cartoon of the orientation of the sightline with respect to the target galaxy. A value of ϕ = 0° represents the alignment along the major axis of the target galaxy, while 90° along the minor axis. In the bottom panels we present two galaxies from our sample, with images drawn from from the DESI Legacy Imaging Surveys (Dey et al. 2019), and the sightline orientation angles (ϕ) indicated with red arcs. The orientation angle of the example on the left is 18.°11. It is 81.°67 for the example on the right. The target galaxy on the left is located at (R.A., decl.) = (1.°61904, +0.°48484) and has z = 0.0622, e = 0.47 and M * = 1010.68 M ⊙. The projected radius to the sightline is 36.8 kpc. The target galaxy on the right is located at (R.A., decl.) = (18.°2994 , +0.°6965) and has z = 0.0846, e = 0.58 and M * = 1010.67 M ⊙. The projected radius to the sightline is 27.5 kpc.
Paper: The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies
Authors: Huanian Zhang, 华年 张, Dennis Zaritsky
Figure caption: The [O III] (top), Hα (middle), and [N II] (bottom) emission line flux as a function of azimuthal angle. The red dot represents the emission flux at the inner radii of 0.05 < r  s  < 0.125 and the blue triangle is for the outer radii of 0.125 < r  s  < 0.25. The horizontal dashed line indicates the zero flux for better visualization.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The (simplified) late-time light-curve model, as compared to the bolometric light curve of SN 2019muj (black squares: Kawabata et al. 2021) as complemented with the bolometric luminosities adopted in the TARDIS late-time spectral models (red squares). The power deposited to the inner ejecta component is shown by a solid-black line, while the full deposition curve is shown by a dashed-black line. In addition, the contribution by the innermost bound WD component is shown by a gray line. The red line shows the combined light curve of the inner ejecta and innermost WD remnant contributions.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: A toy model for the evolution of the 56Ni shell (i.e., the inner component), which is initially within the WD remnant (or its envelope). Shown here are the kinetic energy (red), characteristic velocity (blue-solid), radius (blue-dashed), diffusion timescale (black-solid), and the expansion timescale (black dashed). The vertical gray line shows the timing when the photon diffusion becomes important.
Paper: The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies
Authors: Huanian Zhang, 华年 张, Dennis Zaritsky
Figure caption: The distribution of stellar mass for the primary galaxy sample. We require M * > 1010.4 M ⊙ to match the stellar mass where we found the CGM to have AGN-like properties (Paper III) and to approximately match the Martín-Navarro et al. (2021) study.
Paper: The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies
Authors: Huanian Zhang, 华年 张, Dennis Zaritsky
Figure caption: The [O III], Hα, and [N II] emission line flux for data sample (solid shapes) and control sample (open shapes) as a function of azimuthal angle. The data points are separated in horizontal direction for better visualization. The black dashed line indicates the zero flux for better visualization.
Paper: Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core
Authors: Keiichi Maeda, Miho Kawabata
Figure caption: The individual frames of the late-time spectra of SN 2019muj. The extinction is not corrected in this figure. The combined spectra obtained with the B300 (blue) and R300 (red) grisms are shown, as well as the individual frames (black for the B300 and gray for the R300. The top and bottom portions in each panel are for day 131 and day 480, respectively. In addition to the spectra of SN 2019muj, the sky-line spectra (cyan) and the telluric-absorption spectra (magenta) for the R300 grism on day 480 are shown on an arbitrary scale.
Paper: Repeated Mergers of Black Hole Binaries: Implications for GW190521
Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos
Figure caption: Evolution of the binary period (top panel) and eccentricity (bottom panel) for the various BHBs that Snowball is part of. BHB mergers are displayed as vertical black lines, and three-body exchange events involving the Snowball BHB are displayed as vertical dotted green lines. The eccentricity is given between 0 (circular) and 1 (parabolic), the period in days, and the time in megayears. The time for which Snowball is part of a hierarchical triple BH system is highlighted in red in the bottom panel. Note that there is a sharp upper bound for the periods of 1000 days, as this is the upper cutoff for which NBODY6 regularizes binaries.
Paper: Repeated Mergers of Black Hole Binaries: Implications for GW190521
Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos
Figure caption: Snowball’s position as a function of its mass. The vertical axis displays Snowball’s position, given by the ratio of two distances: Snowball’s distance from the cluster center and the core radius. The horizontal axis displays Snowball’s mass in solar masses. The blue dots represent the mean position for a given mass, and the error bars display the range of positions.