adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of a Pair of Galaxies with Both Hosting X-Ray Binary Candidates at z = 2.544
Authors: Sijia Cai, Zheng Cai, Jianwei Lyu, Yunjing Wu, Xiaojing Lin, Mingyu Li, Junjie Mao, Jiayi Chen, Pengjun Lu
Figure caption: The evolution of LX/SFR with redshift. The galaxy pair UDF3 and UDF3-2 are represented by star markers. Additionally, stacked LX/SFR values from previous studies in different redshift bins are marked. The metallicity, indicated by oxygen abundance, is shown by different colors. These include measurements at z = 0 from B. Lehmer et al. (2010) and S. Mineo et al. (2012), as well as from the full sample of F. M. Fornasini et al. (2019), and measurements from galaxies dominated by HMXBs (﹩{\mathrm{log}}\,\rm{sSFR}\,\gt -8.8﹩). Measurements from F. M. Fornasini et al. (2020) in the hCOSMOS and zCOSMOS surveys are also displayed. The dark gray dashed line shows the redshift evolution of LX/SFR for HMXBs from B. Lehmer et al. (2016): LX = β(1 + z)δSFR. The light gray dashed line represents the relation measured by J. Aird et al. (2016): LX = β(1 + z)δSFRθ, normalized at SFR = 30 M⊙ yr−1.
Paper: Discovery of a Pair of Galaxies with Both Hosting X-Ray Binary Candidates at z = 2.544
Authors: Sijia Cai, Zheng Cai, Jianwei Lyu, Yunjing Wu, Xiaojing Lin, Mingyu Li, Junjie Mao, Jiayi Chen, Pengjun Lu
Figure caption: SED fitting of the two galaxies. The red hexagons, circles, and diamonds represent the photometric data from HST, NIRCam, and MIRI, respectively. The blue solid line and square markers denote the model spectrum and model photometry predicted by the SED fitting. The green solid line corresponds to the stellar component predicted by the FSPS model, while the orange solid line represents the fitted B. T. Draine & A. Li (2007) dust emission component. The AGN component is omitted in the plot due to its negligible contribution. The transmission curves of each filter are shown by the gray line.
Paper: Discovery of a Pair of Galaxies with Both Hosting X-Ray Binary Candidates at z = 2.544
Authors: Sijia Cai, Zheng Cai, Jianwei Lyu, Yunjing Wu, Xiaojing Lin, Mingyu Li, Junjie Mao, Jiayi Chen, Pengjun Lu
Figure caption: RGB and multiband images of galaxies UDF3 and UDF3-2, each with a cutout size of 5″ × 5″ and a pixel scale of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩05 pixel–1. (a) RGB composite image created using the F444W, F277W, and F115W filters. (b) Full-band (0.5–7 keV) Chandra X-ray image (0﹩\mathop{.}\limits^{\unicode{x02033}}﹩5 pixel–1) with [2σ, 3σ, 4σ, 5σ] brightness contours overlaid on the JWST/NIRCam F444W filter image. (c)–(i) NIRCam images in various filters, each smoothed with a 1σ Gaussian kernel.
Paper: Discovery of a Pair of Galaxies with Both Hosting X-Ray Binary Candidates at z = 2.544
Authors: Sijia Cai, Zheng Cai, Jianwei Lyu, Yunjing Wu, Xiaojing Lin, Mingyu Li, Junjie Mao, Jiayi Chen, Pengjun Lu
Figure caption: The BPT diagram, with the UDF3 plotted as a blue filled circle and 1σ error bar. The solid black lines show the maximum starburst boundaries from L. J. Kewley et al. (2001), while the dashed black line in the left panel show the empirical maximum starburst line from G. Kauffmann et al. (2003) and the right panel displays the Seyfert-LINER separation lines from L. J. Kewley et al. (2006).
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: Time–distance stack plots are generated for 12 slices in Figure 3(a2), with each slice spaced at 15° intervals and centered on the filament mass F2, using 171 Å raw images. The third row is the oscillation of filament F2 in the directions of slices 6, 7, and 8 in Figure 3 panel (a2), where the green and red curves are the oscillation curves that manually marked the positions using fore fitting, and their corresponding fitting results are listed with corresponding colors in each panel. The box in panel (S7) is the field of view for Figure 3(b2).
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: Measurement of the Doppler velocity of the oscillation filaments. The Doppler velocities obtained from sampling points on filaments F1, F2, and F3 are shown in (a1)–(a4), (b1)–(b4), and (c1)–(c4), respectively. In each panel, the blue curve with filled circles is the derived Doppler velocity, while the red curve with open diamonds is the detrended velocity. The back curve is a fit to the detrended velocity using the formula ﹩f(t)=A{e}^{(-t/\tau )}{\rm{\cos }}(2\pi /T+\phi )﹩. The fitted velocity amplitude (A), oscillation period (T), and damping time (τ) are listed in the corresponding panel.
Paper: 3D Fast-mode Wave Propagation from Corona to Chromosphere: Triggering Mechanism for 3D Oscillations of Filaments
Authors: Yunxue Huang, Qin Feng, Yuhu Miao, Zhining Qu, Ke Yu, Hongfei Liang, Yu Liu, Xinping Zhou
Figure caption: The time–distance stack plots for filaments F1 and F3 along the slices marked 0, 1, and 2 in panels (a1) and (a3) of Figure 3, using the AIA 171 Å raw images. The green curves in the top row are the oscillation curves that manually marked the positions used for fitting, and the fitting results are listed in the corresponding panels. The boxes are the fields of view of panels (b1) and (b3) in Figure 3.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Spectrum and model of Hα line for CEERSP7:8486. The best model selected is a double-component Gaussian with an absorption feature. The FWHM of the components is ∼1980 km s−1 and ∼560 km s−1 for the broad and narrow components, respectively. We note that the supposed detection of an absorption feature may instead be due to the presence of [N II] emission creating a small secondary peak. This was the only spectrum that displayed a possible hint of [N II] emission.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Spectrum and model of Hα line for CEERSP9:7426. The best model selected is a double-component Gaussian with an absorption feature. The FWHM of the components is ∼1700 km s−1 and ∼320 km s−1 for the broad and narrow components, respectively.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Spectrum and model of Hα line for CEERSP2:2580. The best model selected for this LRD is a single-component Gaussian with an FWHM of ∼240 km s−1.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: The redshift distribution for our LRD sample. The distribution peaks around z ∼ 5 and contains most LRDs in the range 4 ≲ z ≲ 6, similar to D. D. Kocevski et al. (2023), V. Kokorev et al. (2024), and I. Labbe et al. (2025).
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: The number density evolution of our LRD sample. The errors on the number density are calculated assuming a Poissonian error on the count of LRDs in each bin.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Comparison of the BIC with the fraction of AGN IR luminosity to total IR luminosity. Note that a jitter has been added to distinguish data points. Around ∼70% of the pairs of AGN and non-AGN models have a positive ΔBIC value. For LRDs with MIRI data, this is ∼9. In comparison, CEERS and NEP-TDF LRDs tend to have a lower ΔBIC than JADES LRDs. Most of the values for CEERS and NEP-TDF LRDs with lower AGN fractions are ∼6.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Comparison of Δχ2 across CEERS, NEP-TDF, and JADES with the fraction of AGN IR luminosity to total IR luminosity. Note that a jitter has been added to distinguish data points. The red symbol is the LRD in JADES without MIRI data. Note that some values of χ2 remain effectively the same. The LRDs with the highest AGN fractions tend to have a considerably improved χ2 compared to non-AGN models.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: AGN (top) and non-AGN (bottom) CIGALE models for JADES:32344 (z = 5.82), which has MIRI coverage. Note that six of the longest-wavelength model flux points corresponding to MIRI data are treated as upper limits, while the F2550W band is treated as an observed flux. Both models produce a stellar mass of ∼109.3 M⊙. The AGN IR luminosity fraction for this LRD is fAGN = 0.9.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: The stellar mass calculated by CIGALE for non-AGN models compared to the difference in stellar mass for AGN and non-AGN models, expressed logarithmically. The average error is included in the bottom left corner. The stellar mass of the non-AGN model is higher for all but two LRDs in JADES and two LRDs in CEERS.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Distributions of LRD and galaxy redshifts for the 4.75 < z < 6.5 and 6.5 < z < 8.25 bins. Note that the LRD histograms are weighted to be normalized compared to the galaxy histograms for ease of visual comparison. The redshift distribution of LRDs and galaxies is roughly similar, especially for the 4.75 < z < 6.5 bin.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: AGN (top) and non-AGN (bottom) CIGALE models for CEERS:2580, which has redshift z = 5.43.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Distribution of FWHM in km s−1 of the broadest component of each Hα line for LRDs.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Comparison of the stellar mass with the fraction of AGN IR luminosity to total IR luminosity fAGN. The fraction fAGN is quantized because of the choice of values allowed. We find no correlation between the fraction of AGN and stellar mass.
Paper: Lonely Little Red Dots: Challenges to the Active Galactic Nucleus Nature of Little Red Dots through Their Clustering and Spectral Energy Distributions
Authors: María Carranza-Escudero, Christopher J. Conselice, Nathan Adams, Thomas Harvey, Duncan Austin, Peter Behroozi, Leonardo Ferreira, Katherine Ormerod, Qiao Duan, James Trussler, Qiong Li, Lewi Westcott, Rogier A. Windhorst, Dan Coe, Seth H. Cohen, Cheng Cheng, Simon P. Driver, Brenda Frye, Lukas J. Furtak, Norman A. Grogin, Nimish P. Hathi, Rolf A. Jansen, Anton M. Koekemoer, Madeline A. Marshall, Rosalia O'Brien, Norbert Pirzkal, Maria Polletta, Aaron Robotham, Michael J. Rutkowski, Jake Summers, Stephen M. Wilkins, Christopher N. A. Willmer, Haojing Yan, Adi Zitrin
Figure caption: Stack plot of the dust extinction calculated by CIGALE for AGN models. Most AGN models are fit by a dust extinction close to the extremes (0.1 and 6) of the allowed values.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Images of the dual-cone model from fits to the 2017 April 6 observations of M87 (left) and the 2018 April 21 observations of M87 (right). The top row shows the mean images of posterior chain samples at the native resolution, and the middle row shows the samples blurred to the nominal EHT resolution. For the EHT resolution, we use a Gaussian beam with an FWHM of 20 μas. The bottom row shows the corresponding consensus images from the EHT.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Normalized log-closure amplitude (top row) and closure phase (bottom row) residuals of mF-ring and dual-cone model fits to the 2018 observations of M87* by the EHT. Each panel shows residuals of posterior samples (gray) and the maximum a posteriori estimate (blue) from our dual-cone model fits. Residuals pertaining to fits of the 2017 and 2018 observations of M87* are shown in the left and right columns, respectively. We also show residuals from a maximum aposterior estimate of the fiducial mF-ring model to both the 2017 and 2018 observations of M87* in orange.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Full corner plot of posterior samples for the dual-cone model fits to data from EHT observations of M87* on 2017 April 6 (blue) and 2018 April 11 (orange). Vertical lines show independent mass measurements of M87* from K. Gebhardt et al. (2011; red), J. L. Walsh et al. (2013; pink), Event Horizon Telescope Collaboration et al. (2019a; black dotted), E. R. Liepold et al. (2023; yellow), and D. A. Simon et al. (2023; green). We also show the measured position angle and inclination of the large-scale jet in M87* (R. C. Walker et al. 2018). See Table 1 for a description of the model parameters. Both the blue and orange sets of histograms have been normalized.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Best fits (i.e., the MAP estimates) for the dual-cone model (blue) and the fiducial mF-ring model (orange) to log-closure amplitudes (top row) and closure phases (bottom row) constructed from data acquired during observations of M87* by the EHT (gray). The fits to the the 2017 and 2018 data products are shown in the left and right columns, respectively.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Images of the MAP estimates of the mF-ring model and the dual-cone model for fits to EHT observations of M87* in 2017 (left) and in 2018 (right). The top row shows images at their native resolutions; the bottom row shows images blurred to the nominal EHT resolution. For the latter, we use a Gaussian beam of 20 μas FWHM.
Paper: Assessing the Role of Intrinsic Variability in Black Hole Parameter Inference Using Multiepoch EHT Data
Authors: Dominic O. Chang, Michael D. Johnson, Paul Tiede
Figure caption: Baseline coverage (u, v) from the EHT observations of M87*. EHT observations from 2017 April 6 and 2018 April 21 are shown in blue and orange, respectively. The gray circle shows a fringe spacing of 25 μas, corresponding to ﹩\sqrt{{u}^{2}+{v}^{2}}\approx 8.25\,{\rm{G}}\lambda ﹩.
Paper: The Kick Velocity Distribution of Isolated Neutron Stars
Authors: Paul Disberg, Ilya Mandel
Figure caption: Velocity distributions for the pulsar samples of A. P. Igoshev (2020) and F. Verbunt et al. (2017), together with their kick distributions (light dashed lines) and our double-Maxwellian fits (dark dotted lines) through Equation (9). The parameters of our fits and those from the literature are listed in the figure as well, along with quoted uncertainties on the latter in parentheses.