image image | UUID string | Image ID string | Paper DOI string | Paper Title string | Image Caption string | Image Authors string | References DOIs list | Citing DOIs list |
|---|---|---|---|---|---|---|---|---|
10.3847.1538-4357.ac983d_apjac983df5_8 | apjac983df5 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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 ... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df7_9 | apjac983df7 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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 N... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df13_10 | apjac983df13 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df2_11 | apjac983df2 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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. The... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df1_12 | apjac983df1 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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 e... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df18_13 | apjac983df18 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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. Blu... | 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, Mich... | [
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10.3847.1538-4357.ac983d_apjac983df17_14 | apjac983df17 | 10.3847/1538-4357/ac983d | The Radius of PSR J0740+6620 from NICER with NICER Background Estimates | 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 r... | 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, Mich... | [
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10.3847.1538-4357.ac99db_apjac99dbf11_15 | apjac99dbf11 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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 ... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf7_16 | apjac99dbf7 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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. (201... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf4_17 | apjac99dbf4 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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 sh... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf3_18 | apjac99dbf3 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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 ... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf10_19 | apjac99dbf10 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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 sho... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf9_20 | apjac99dbf9 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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.... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf6_21 | apjac99dbf6 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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), Grup... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf5_22 | apjac99dbf5 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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 ... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac99db_apjac99dbf8_23 | apjac99dbf8 | 10.3847/1538-4357/ac99db | An Ultra-deep Multiband Very Large Array (VLA) Survey of the Faint Radio Sky (COSMOS-XS): New Constraints on the Cosmic Star Formation History | 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... | 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 | [
"10.3847/1538-4365/ac3078"
] | [] | |
10.3847.1538-4357.ac9df2_apjac9df2f15_24 | apjac9df2f15 | 10.3847/1538-4357/ac9df2 | Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core | 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 ... | Authors: Keiichi Maeda, Miho Kawabata | [] | [
"10.3847/2041-8213/adf062",
"10.3847/1538-4357/ad037f"
] | |
10.3847.1538-4357.ac9c64_apjac9c64f2_25 | apjac9c64f2 | 10.3847/1538-4357/ac9c64 | The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies | 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 DE... | Authors: Huanian Zhang, 华年 张, Dennis Zaritsky | [
"10.3847/1538-3881/ac69d0"
] | [] | |
10.3847.1538-4357.ac9c64_apjac9c64f4_26 | apjac9c64f4 | 10.3847/1538-4357/ac9c64 | The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies | 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... | Authors: Huanian Zhang, 华年 张, Dennis Zaritsky | [
"10.3847/1538-3881/ac69d0"
] | [] | |
10.3847.1538-4357.ac9df2_apjac9df2f17_27 | apjac9df2f17 | 10.3847/1538-4357/ac9df2 | Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core | 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 soli... | Authors: Keiichi Maeda, Miho Kawabata | [] | [
"10.3847/2041-8213/adf062",
"10.3847/1538-4357/ad037f"
] | |
10.3847.1538-4357.ac9df2_apjac9df2f16_28 | apjac9df2f16 | 10.3847/1538-4357/ac9df2 | Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core | 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... | Authors: Keiichi Maeda, Miho Kawabata | [] | [
"10.3847/2041-8213/adf062",
"10.3847/1538-4357/ad037f"
] | |
10.3847.1538-4357.ac9c64_apjac9c64f1_29 | apjac9c64f1 | 10.3847/1538-4357/ac9c64 | The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies | 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. | Authors: Huanian Zhang, 华年 张, Dennis Zaritsky | [
"10.3847/1538-3881/ac69d0"
] | [] | |
10.3847.1538-4357.ac9c64_apjac9c64f3_30 | apjac9c64f3 | 10.3847/1538-4357/ac9c64 | The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies | 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. | Authors: Huanian Zhang, 华年 张, Dennis Zaritsky | [
"10.3847/1538-3881/ac69d0"
] | [] | |
10.3847.1538-4357.ac9df2_apjac9df2f18_31 | apjac9df2f18 | 10.3847/1538-4357/ac9df2 | Properties of Type Iax Supernova 2019muj in the Late Phase: Existence, Nature, and Origin of the Iron-rich Dense Core | 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 ... | Authors: Keiichi Maeda, Miho Kawabata | [] | [
"10.3847/2041-8213/adf062",
"10.3847/1538-4357/ad037f"
] | |
10.3847.1538-4357.ac9d95_apjac9d95f3_32 | apjac9d95f3 | 10.3847/1538-4357/ac9d95 | Repeated Mergers of Black Hole Binaries: Implications for GW190521 | 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 (circul... | Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos | [
"10.3847/2041-8213/ac7ec4"
] | [
"10.3847/1538-4357/ac9798",
"10.3847/1538-4357/ad90a9"
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10.3847.1538-4357.ac9d95_apjac9d95f2_33 | apjac9d95f2 | 10.3847/1538-4357/ac9d95 | Repeated Mergers of Black Hole Binaries: Implications for GW190521 | 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, a... | Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos | [
"10.3847/2041-8213/ac7ec4"
] | [
"10.3847/1538-4357/ac9798",
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10.3847.1538-4357.ac9c64_apjac9c64f5_34 | apjac9c64f5 | 10.3847/1538-4357/ac9c64 | The Anisotropic Circumgalactic Medium of Massive Early-type Galaxies | The BPT emission line ratios for two azimuthal and two radial bins. The inner bins, 0.05 < r s < 0.125, are represented in red, while the outer, 0.125 < r s < 0.25, are in blue. The symbols designate the azimuthal bins as given in the legend. The blue curve shows the boundary between the H II and AGN regions of the... | Authors: Huanian Zhang, 华年 张, Dennis Zaritsky | [
"10.3847/1538-3881/ac69d0"
] | [] | |
10.3847.1538-4357.ac9d95_apjac9d95f4_35 | apjac9d95f4 | 10.3847/1538-4357/ac9d95 | Repeated Mergers of Black Hole Binaries: Implications for GW190521 | Histogram of the various possible recoil velocities for each of the seven mergers in the Snowball merger chain. For each merger we calculate 10,000 different recoils, randomly assigning the spin directions isotropically, but keeping all other properties such as mass, initial separation, and spin magnitudes fixed. Merge... | Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos | [
"10.3847/2041-8213/ac7ec4"
] | [
"10.3847/1538-4357/ac9798",
"10.3847/1538-4357/ad90a9"
] | |
10.3847.1538-4357.ac9d95_apjac9d95f1_36 | apjac9d95f1 | 10.3847/1538-4357/ac9d95 | Repeated Mergers of Black Hole Binaries: Implications for GW190521 | The BH merger tree of Snowball (seven total BHB mergers). Black hole masses are shown on the vertical axis, and the time of mergers is shown on the horizontal axis. | Authors: Oliver Anagnostou, Michele Trenti, Andrew Melatos | [
"10.3847/2041-8213/ac7ec4"
] | [
"10.3847/1538-4357/ac9798",
"10.3847/1538-4357/ad90a9"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f2_37 | apjac9b23f2 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Mass absorption and scattering coefficients of amorphous olivine (top), amorphous pyroxene (upper middle), crystalline olivine (lower middle), and amorphous carbon (bottom). In the panels of amorphous olivine and pyroxene, the mass absorption and scattering coefficients calculated with different ﹩{f}_{\max }﹩ and ﹩{a}_... | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f3_38 | apjac9b23f3 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Examples of mid-IR spectral fits with models 1 (left), 2 (middle left), 3 (middle right), and 4 (right) to example spectra of IRAS 12127-1412, IRAS 08572+3915, and IRAS15250+3609. The best-fit spectrum by each model is shown with the red solid line. The blue dashed and solid lines represent the AGN-heated dust emission... | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f1_39 | apjac9b23f1 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | An example result of the mid-IR 5–30 μm spectral modeling of heavily obscured AGNs. The black points and the red solid line show the observed spectrum and the best-fit model of IRAS 15250+3609. The blue solid line represents the AGN-heated dust emission components with ice absorption, ﹩{F}_{{\rm{d}}}^{\mathrm{agn}}\exp... | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f8_40 | apjac9b23f8 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Properties of silicate dust as a function of the total infrared luminosity, L IR, shown together with the Pearson’s correlation coefficient and the p-value in the top left corner. | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f4_41 | apjac9b23f4 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Comparison between the results of the four models. The panels at the diagonal positions show the histograms of reduced χ 2 of each model. Black and white bars represent the objects, the fits of which are accepted and rejected, respectively, with a significance level of 5%. The scatter plots at lower diagonal positions ... | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f7_42 | apjac9b23f7 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Correlation plots of the pyroxene mass fraction, r pyr, and the crystallinity, r cry, between the results of the previous studies and ours. Note that Tsuchikawa et al. (2021) defined the pyroxene mass fraction with the total mass of amorphous and crystalline silicate, while the present study defines r pyr with the tota... | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9b23_apjac9b23f6_43 | apjac9b23f6 | 10.3847/1538-4357/ac9b23 | Spitzer/IRS Full Spectral Modeling to Characterize Mineralogical Properties of Silicate Dust in Heavily Obscured AGNs | Histograms of the pyroxene mass fraction, r pyr, and the crystallinity, r cry. Red dashed lines correspond to typical dust properties of the diffuse ISM observed in our Galaxy (Do-Duy et al. 2020). | Authors: T. Tsuchikawa, H. Kaneda, S. Oyabu, T. Kokusho, H. Kobayashi, Y. Toba | [] | [
"10.3847/PSJ/ad0382"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f8_44 | apjac9ea7f8 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Distributions of the χ value for each of our three reconstructions in relation to a single sample. Also plotted is a unit normal Gaussian distribution, showing close agreement. Excess values along the tails indicate model failure, either to estimate proper variance or strong residual biases, or potentially the importan... | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
"10.3847/1538-4365/acbf47"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f7_45 | apjac9ea7f7 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Two-dimensional histogram of temperature and hydrogen density relation in truth compared to the reconstruction. The orange line indicates a best-fit power-law solution, ﹩T={T}_{0}{n}_{{\rm{H}}}^{\gamma }﹩, across the range of 10−4 < n H < 10−6. Red dashed lines indicate the classification of the gas content of the univ... | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
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] | |
10.3847.1538-4357.ac9e57_apjac9e57f2_46 | apjac9e57f2 | 10.3847/1538-4357/ac9e57 | Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC | The split of carbon-rich, fundamental-mode pulsator (C0) AGB stars into “normal” and “extreme” populations is depicted here, using the method found in Blum et al. (2006), Srinivasan et al. (2009), and Boyer et al. (2011), where xAGB stars are those brighter than the 3.6 μm TRGB and with J − [3.6] > 3.1 mag (a), or if t... | Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman | [] | [
"10.3847/1538-4357/adfa2b"
] | |
10.3847.1538-4357.ac9e57_apjac9e57f1_47 | apjac9e57f1 | 10.3847/1538-4357/ac9e57 | Relation of Observable Stellar Parameters to Mass-loss Rate of AGB Stars in the LMC | Plot of [3.6] vs. ﹩\mathrm{log}P﹩ for the stars in the Riebel et al. (2012) data set. M-type stars are in black and C-type stars in blue. M stars brighter than [3.6] = 10.3 are assumed to be red supergiant stars, and are excluded from the analysis. Following the naming convention established in Riebel et al. (2010), se... | Authors: Henry A. Prager, Lee Anne Willson, Massimo Marengo, Michelle J. Creech-Eakman | [] | [
"10.3847/1538-4357/adfa2b"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f9_48 | apjac9ea7f9 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Postage stamp posterior samples of the temperature field from Figure 4. There is high variation in the shocked region, showing the hydrodynamical uncertainty the model has learned, while the areas outside the shocked region are stationary (with some occasional edge effects). | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
"10.3847/1538-4365/acbf47"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f10_49 | apjac9ea7f10 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Performance of HYPHY in terms of the Lyα forest flux in redshift space using Equation (7) as implemented in GIMLET. We show the resulting probability density function of Lyα flux, showing substantial biases in the reconstructed flux at F ∼ 0.25, but good agreement at the extremes. | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
"10.3847/1538-4365/acbf47"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f11_50 | apjac9ea7f11 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Performance of HYPHY in terms of the Lyα forest power spectrum in redshift space using Equation (7) as implemented in GIMLET. We show the resulting power spectra of Lyα flux, finding good agreement across a range of scales up to k ∼ 14 h −1 Mpc. | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
"10.3847/1538-4365/acbf47"
] | |
10.3847.1538-4357.ac9ea7_apjac9ea7f12_51 | apjac9ea7f12 | 10.3847/1538-4357/ac9ea7 | HYPHY: Deep Generative Conditional Posterior Mapping of Hydrodynamical Physics | Figure demonstrating the generation of a light cone using HYPHY. In the top two panels, we show the HYPHY-generated temperature corresponding to the same dark matter distribution as though it was at z = 2.4 and z = 4.0. In the bottom panel we show the same distribution but with a varying redshift across the box, going ... | Authors: Benjamin Horowitz, Max Dornfest, Zarija Lukić, Peter Harrington | [] | [
"10.3847/1538-4357/acfcb5",
"10.3847/2041-8213/ac8f4b",
"10.3847/1538-4365/acbf47"
] | |
10.3847.1538-4357.ac982e_apjac982ef15_52 | apjac982ef15 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | BCES fits to elliptical galaxies. Top: log M • vs. log N GC; bottom: log N GC vs. log M •. Left: no additional scatter; center: additional ϵ y ; right: ϵ y and ϵ x . Solid black lines: best fits; translucent gray lines: range of possible solutions. Solid (red) and open (green) circles represent, respectively, ellip... | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef13_53 | apjac982ef13 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | MW GC system, at the distance and orientation of studied galaxies, projected coordinates +X proj, +Y proj. Top: NGC 3368; bottom: NGC 4395. Left: 3D rotation about the Galactic ﹩X^{\prime} ﹩-axis before projection on the plane of the sky. Right: 3D rotation about Galactic Y-axis. Solid black line: mask; red crosses: so... | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef12_54 | apjac982ef12 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | K s -band luminosity functions of the GCCs. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826. Histograms: number of detected objects; solid red lines: expected Gaussian GCLFs (see Table 4 and Section 7). | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef8_55 | apjac982ef8 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K s ) colors and structural parameters of sources in and closely around the selection region of NGC 4826. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. Symbols as in Figure 5. | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef14_56 | apjac982ef14 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | MW GC system, at the distance and orientation of studied galaxies, projected coordinates + X proj, + Y proj. Top: NGC 4736; bottom: NGC 4826. Symbols as in Figure 13. | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef9_57 | apjac982ef9 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | Spatial distributions of the GCC samples. Top left: NGC 3368; top right: NGC 4395; bottom left: NGC 4736; bottom right: NGC 4826. The GCCs are shown as green-filled circles. Dark blue ellipse: boundary of areas where source confusion is highest (see text); solid cyan line: R 25. | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef11_58 | apjac982ef11 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | Color distributions of GC systems. Top: NGC 3368 GCCs; second row: NGC 4395; third row: NGC 4736; bottom: NGC 4826. From left to right: (﹩u* -g^{\prime} ﹩), (﹩u* -i^{\prime} ﹩), (g′ − r′), (g′ − i′), (g′ − K s ), (r′ − i′). | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef10_59 | apjac982ef10 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | Grayscale images of GC candidates, from HST exposures. Top, left to right: J104635+114912 and J104651+114819, in NGC 3368. Bottom: J125039+410913, J125045+410950, and J125131+410849, in NGC 4736. | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac982e_apjac982ef7_60 | apjac982ef7 | 10.3847/1538-4357/ac982e | The Relation between Globular Cluster Systems and Supermassive Black Holes in Spiral Galaxies. III. The Link to the M •–M * Correlation | (u* – ﹩i^{\prime} ﹩) vs. (﹩i^{\prime} ﹩ – K s ) colors and structural parameters of sources in and closely around the selection region of NGC 4736. Top: FWHM; bottom: 100 × SPREAD_MODEL. Left column: all sources; right column: final sample. Symbols as in Figure 5. | Authors: Rosa A. González-Lópezlira, Luis Lomelí-Núñez, Yasna Ordenes-Briceño, Laurent Loinard, Stephen Gwyn, Karla Alamo-Martínez, Gustavo Bruzual, Ariane Lançon, Thomas H. Puzia | [] | [
"10.3847/1538-3881/adbf0c",
"10.3847/1538-4357/ae0cc0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef2_61 | apjac9fcef2 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Examples of the best-fit SEDs with (blue) and without (orange) the emission-line templates, where IDs are from the ZFOURGE catalog. The Spitzer/IRAC photometry at 3.6 and 4.5 μm bands, which sample rest frame ∼2 μm, cannot be fitted well unless the effects of the emission lines are taken into account. The estimated ste... | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9e5a_apjac9e5af8_62 | apjac9e5af8 | 10.3847/1538-4357/ac9e5a | STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona | Initial configuration (panels (a) and (c)) of a more complex flux distribution with a corrugated PIL and later snapshots during (b) formation and (d) eruption of its filament channel. Magnetic field lines are color-coded and radial velocity is color shaded as in Figure 3. | Authors: J. T. Dahlin, C. R. DeVore, S. K. Antiochos | [
"10.3847/2041-8213/ac64a9"
] | [
"10.3847/1538-4357/ad0229",
"10.3847/1538-4357/aca0ec",
"10.3847/1538-4357/ae2479",
"10.3847/1538-4357/acebeb",
"10.3847/1538-4357/ad7f53",
"10.3847/1538-4357/ae03c5",
"10.3847/1538-4357/ae0297"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef4_63 | apjac9fcef4 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Comparison between the Hα fluxes derived from the NB209 color excesses and the flux excesses in the K s band. Both fluxes are in the units of erg s−1 cm−2. The gray line shows the one-to-one relation, while the regions shaded in gray and light gray indicate factor 2 and 5 intervals, respectively. The color coding of in... | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef3_64 | apjac9fcef3 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | (Left) Changes of the estimated continuum fluxes of our sample when assuming a doubled production rate of the Lyman continuum photons in the SED fitting. (Right) The distribution of the continuum offsets the two models. | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef1_65 | apjac9fcef1 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Combinations of the emission lines and the filters at each redshift. At z > 1, Hα, Hβ, and [O III] emission lines are observed in the near-infrared regime. Especially, at 2.1 < z < 2.5, Hα falls into the K s broadband filter of the ZFOURGE, while Hβ and [O III] are simultaneously observed in the H medium-band filters. | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9e5a_apjac9e5af9_66 | apjac9e5af9 | 10.3847/1538-4357/ac9e5a | STITCH: A Subgrid-scale Model for Energy Buildup in the Solar Corona | Tangential magnetic field injection for a more complex surface flux distribution with a corrugated PIL. Black contours show values of B r = [−30, −20, −10, 0, +10, +20] G. | Authors: J. T. Dahlin, C. R. DeVore, S. K. Antiochos | [
"10.3847/2041-8213/ac64a9"
] | [
"10.3847/1538-4357/ad0229",
"10.3847/1538-4357/aca0ec",
"10.3847/1538-4357/ae2479",
"10.3847/1538-4357/acebeb",
"10.3847/1538-4357/ad7f53",
"10.3847/1538-4357/ae03c5",
"10.3847/1538-4357/ae0297"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef5_67 | apjac9fcef5 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Same as Figure 4, but for the ZFIRE and our method, where the K s-band excesses are derived using the 1.″2 aperture photometry. | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef6_68 | apjac9fcef6 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Same as Figure 4, but for the KMOS3D and our method. | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef16_69 | apjac9fcef16 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | SFMS plot same as Figure 15 but individual observed galaxies are colored according to luminosity ratios between Hα and UV (see Section 3.8). Simulated observations are shown as gray dots, with the scatter in certain stellar mass bins shown as orange bars. The difference between the simulations and observations at ﹩\mat... | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef19_70 | apjac9fcef19 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Same as Figure 17, but only the starburst galaxies are plotted separately according to their stellar masses. Dashed black horizontal lines represent thresholds of the Hα SFR to be classified as the starburst galaxies in our definition, while the dashed–dotted horizontal lines are our Hα emitter selection. As the lumino... | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef18_71 | apjac9fcef18 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Hα/UV ratios of the starburst galaxies as a function of stellar mass. The blue circles represent median values in each stellar mass bin. The gray horizontal line shows the value expected from a constant SFH, while the dashed vertical line indicates the stellar mass completeness limit. | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac9fce_apjac9fcef17_72 | apjac9fcef17 | 10.3847/1538-4357/ac9fce | A Selection of Hα Emitters at z = 2.1–2.5 Using the K s -band Photometry of ZFOURGE | Comparison between the Hα and UV luminosities, which are both corrected for dust attenuation. The color coding reflects the stellar masses of the galaxies. The gray line shows the expected relation from a constant SFH without starbursts within 100 Myr (Faisst et al. 2019). The shaded region indicates a ±0.3 dex region ... | Authors: Yasunori Terao, Lee R. Spitler, Kentaro Motohara, Nuo Chen | [] | [
"10.3847/2041-8213/ad01c0"
] | |
10.3847.1538-4357.ac8d04_apjac8d04f9_73 | apjac8d04f9 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | Time after CC at which the gravitational instabilities in the collapsar disk first set in (top panel) and the period over which the gravitational instabilities are continuously excited during the fallback process (bottom panel), shown in the space of {r b, f K} for the fiducial progenitor model 250.25, with p = 4.5. Th... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
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10.3847.1538-4357.ac8d04_apjac8d04f15_74 | apjac8d04f15 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | A one-zone chemical evolution calculation showing the contribution to the total Galactic r-process content (stars and interstellar medium gas) from superKNe relative to ordinary collapsars and neutron star mergers as a function of Galactic age. The underlying model and parameters for neutron star mergers as well as ord... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f10_75 | apjac8d04f10 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | The disk frequency evolution (Equation (18)) for three progenitor models (250.25, 220.25, and 200.25), with rotation parameters p = 4.5, r b = 1.5 × 109 cm and an overall small (f K = 0.3; top) or large (f K = 0.6; bottom) Keplerian angular momentum parameter. The plots show twice the orbital angular frequency, which... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f13_76 | apjac8d04f13 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | The detection horizons of gravitational waves from our fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, for CE (top), ET (center), and DECIGO (bottom), assuming optimal matched filtering and an S/N of 8. For progenitors with medium to low rotation, these detectors may be able to detect... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f14_77 | apjac8d04f14 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | The same as Figure 12, but for the progenitor model 250.25, with p = 4.5, r b = 1.5 × 109 cm, and different values of the Keplerian fraction, f K = 0.2, 0.4, and 0.6. The relatively low to medium angular momentum models (here, f K ≈ 0.2) generate stronger signals in all detectors (detection horizon ∼400 Mpc with aLIGO ... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f12_78 | apjac8d04f12 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | Amplitude spectral density of the gravitational-wave emission from the collapsar disk, shown for three progenitor models (250.25, 220.25, and 200.25) and the stellar rotation parameters p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, at an assumed source distance of 200 Mpc. The shaded region for each curve shows the unphy... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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"10.3847/2041-82... | |
10.3847.1538-4357.ac8d04_apjac8d04f17_79 | apjac8d04f17 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | Convergence test for model 250.25. Top: the relative error in computing the total mass of the star M ⋆, using a grid discretized in both polar angle and radius, showing that at the fiducial angular resolution of n θ = 1001, the relative error ≲0.0018 is dominated by the radial resolution of the progenitor model. Bott... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f11_80 | apjac8d04f11 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | Plus and cross-polarization strain amplitudes of the l = m = 2 mode of the gravitational waves resulting from the gravitationally unstable collapsar disk in the fiducial model shown in Figure 2, with p = 4.5, f K = 0.3, and r b = 1.5 × 109 cm, assuming a face-on orientation of the accretion disk (ι = 0). The emission s... | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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10.3847.1538-4357.ac8d04_apjac8d04f16_81 | apjac8d04f16 | 10.3847/1538-4357/ac8d04 | “Super-kilonovae” from Massive Collapsars as Signatures of Black Hole Birth in the Pair-instability Mass Gap | The average ratio of p ej/p fb (see Equation (C1)) during the first 100 s for model 250.25, with p = 4.5 and setting θ fb = 45°. Disk winds can overcome the ram pressure of the infalling material in the polar directions and break out of the star, even without the help of the GRB jet. | Authors: Daniel M. Siegel, Aman Agarwal, Jennifer Barnes, Brian D. Metzger, Mathieu Renzo, V. Ashley Villar | [
"10.3847/2041-8213/ac9b41"
] | [
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"10.3847/2041-82... | |
10.3847.1538-4357.aca091_apjaca091f1_82 | apjaca091f1 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Top panel: modeled spectra considering three independent data sets: XRT (in red), BAT+GBM+KW (in orange), and LAT (in blue). The models are shown in the ν F ν representation. Two distinguished time epochs are chosen: the first one dominated fully by the prompt emission (94–118 s; on the left), and the second one (118... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.ac8b78_apjac8b78f11_83 | apjac8b78f11 | 10.3847/1538-4357/ac8b78 | Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups | Hα profile (left) and spectral energy distribution (right) of J1515−2527. The ALLWISE data point at 22 μm, signified as a triangle, is an upper limit. The disagreement between the synthetic spectrum and the optical photometry may be a result of the observations being taken at different times; regardless, our interest i... | Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg | [
"10.3847/1538-3881/ac35e3"
] | [
"10.3847/1538-3881/ad697d"
] | |
10.3847.1538-4357.aca091_apjaca091f2_84 | apjaca091f2 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | The joint X-ray to high-energy spectrum of GRB 220101A at 94–118 s modeled by the Band function with the high-energy spectral cutoff E cutoff (Band+cutoff). We show the spectrum in the count representation (top panel), that in the spectral energy density representation (SED; middle panel), and the residuals between the... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.ac8b78_apjac8b78f12_85 | apjac8b78f12 | 10.3847/1538-4357/ac8b78 | Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups | Same as Figure 11, but for J1915−2847. The left panel shows observations from different nights (red and blue), as well as their mean (black). We estimate A V = 0 for this system as well. | Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg | [
"10.3847/1538-3881/ac35e3"
] | [
"10.3847/1538-3881/ad697d"
] | |
10.3847.1538-4357.ac8b78_apjac8b78f15_86 | apjac8b78f15 | 10.3847/1538-4357/ac8b78 | Follow-up of Young Stars Identified with BANYAN Σ: New Low-mass Members of Nearby Moving Groups | Spectral cutouts of J0542−1535, J0749−0317, and J2004−2342. The target spectrum (black) is depicted alongside a system of similar spectral type for comparison, J1141+4245 (gray). All targets are roughly type M4. | Authors: Asa G. Stahl, Christopher M. Johns-Krull, L. Flagg | [
"10.3847/1538-3881/ac35e3"
] | [
"10.3847/1538-3881/ad697d"
] | |
10.3847.1538-4357.aca091_apjaca091f5_87 | apjaca091f5 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Constraints on the R γ –Γ0 prompt emission region. The gray points are drawn from the R γ –Γ0 distribution after considering only the condition on the cutoff (first scenario), corresponding to the allowed parameter space derived from the opacity argument (requiring τ γ γ = 1 at E cutoff). We show the lower limits o... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.aca091_apjaca091f7_88 | apjaca091f7 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Corner plot showing the parameter marginalized posterior distributions and contours from the MCMC performed for the afterglow analysis. The best-fit values and priors are shown in Table 2. The parameters fitted in the MCMC are the isotropic equivalent energy E kin, the jet opening angle θ j , the circumburst medium de... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
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] | |
10.3847.1538-4357.aca091_apjaca091f4_89 | apjaca091f4 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Optical (r band; in orange), X-ray (0.5–10 keV; in red), and high-energy (0.1–1 GeV; in blue) light curves of GRB 220101A. Lines correspond to the afterglow model by the propagation of the forward shock in a homogeneous circumburst medium. Early X-ray (<134 s) and high-energy data (<118 s) are not considered for the mo... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.aca091_apjaca091f6_90 | apjaca091f6 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Corner plot showing the parameter contours obtained from the MCMC of the prompt fit parameters, namely the low- and high-energy slopes α and β, respectively, the characteristic energy E ch, the cutoff energy E cutoff, and the flux integrated between 0.1 keV and 0.25 GeV. The 1σ contour region is shown in dark blue, whi... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.aca091_apjaca091f3_91 | apjaca091f3 | 10.3847/1538-4357/aca091 | Constraints on the Physics of the Prompt Emission from Distant and Energetic Gamma-Ray Burst GRB 220101A | Distribution of simulated test statistics, obtained by fitting 103 fake spectra during the prompt time bin (930–118 s) with Band (null model) and Band+cutoff (alternative model). Fake spectra are produced by using as an input the Band model and its relative best-fit parameters obtained from the fit of the real data. Th... | Authors: Alessio Mei, Gor Oganesyan, Anastasia Tsvetkova, Maria Edvige Ravasio, Biswajit Banerjee, Francesco Brighenti, Samuele Ronchini, Marica Branchesi, Dmitry Frederiks | [
"10.3847/1538-4357/ac85b7"
] | [
"10.3847/1538-4357/acf4fe",
"10.3847/1538-4357/ad05c8"
] | |
10.3847.1538-4357.aca09d_apjaca09df6_92 | apjaca09df6 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | Microlensing parallax vs. Einstein crossing time for OGLE-detectable microlensing events (described in the first paragraph of Section 4.3) as a function of lens type. Regardless of IFMR, black hole (BH) lensing events are characterized by their long t E and low π E as compared to other types of lenses. The addition... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
"10.3847/2041-8213/ac7442"
] | [
"10.3847/1538-3881/adcd7a"
] | |
10.3847.1538-4357.aca09d_apjaca09df9_93 | apjaca09df9 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of Einstein crossing times for OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The solid lines indicate all lens types while the dashed lines indicate the distribution of the blac... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
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] | [
"10.3847/1538-3881/adcd7a"
] | |
10.3847.1538-4357.aca09d_apjaca09df11_94 | apjaca09df11 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of Einstein crossing times for microlensing events detectable by a Roman-style survey. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The solid lines indicate all lens types while the dashed lines indicate ... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
"10.3847/2041-8213/ac7442"
] | [
"10.3847/1538-3881/adcd7a"
] | |
10.3847.1538-4357.aca09d_apjaca09df12_95 | apjaca09df12 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of microlensing parallaxes for microlensing events detectable by a Roman-style survey. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The solid lines indicate all lens types while the dashed lines indicate ... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
"10.3847/2041-8213/ac7442"
] | [
"10.3847/1538-3881/adcd7a"
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10.3847.1538-4357.aca09d_apjaca09df10_96 | apjaca09df10 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of microlensing parallax for OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The solid lines indicate all lens types while the dashed lines indicate the distribution of the black ... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
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10.3847.1538-4357.aca09d_apjaca09df7_97 | apjaca09df7 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of Einstein crossing times for OGLE-detectable microlensing events as a function of lens type for each IFMR. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The largest differences between the IFMRs are found at long... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
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10.3847.1538-4357.aca09d_apjaca09df8_98 | apjaca09df8 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | A histogram of microlensing parallax for OGLE-detectable microlensing events as a function of lens type for each IFMR. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The largest differences between the IFMRs are found at small ... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
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10.3847.1538-4357.aca09d_apjaca09df13_99 | apjaca09df13 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | Einstein crossing time distributions for microlensing events detectable by a Roman-style survey, for constant-valued vs. Maxwellian NS/BH birth kicks. The number of events is scaled to the number of events Roman is expected to detect during its 5 yr microlensing survey, as described in Section 4.5. The effect of the di... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
"10.3847/2041-8213/ac7442"
] | [
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10.3847.1538-4357.aca09d_apjaca09df5_100 | apjaca09df5 | 10.3847/1538-4357/aca09d | The Impact of Initial–Final Mass Relations on Black Hole Microlensing | Mass distribution of black hole lenses from OGLE-detectable microlensing events. The number of events is scaled to the number of events an OGLE-like survey would observe over a span of 10 yr, as described in Section 4.4. The Spera15 IFMR produces much more massive BHs than the Raithel18 and SukhboldN20 IFMRs, and this ... | Authors: Sam Rose, Casey Y. Lam, Jessica R. Lu, Michael Medford, Matthew W. Hosek, Natasha S. Abrams, Emily Ramey, Sergiy S. Vasylyev | [
"10.3847/2041-8213/ac90bb",
"10.3847/1538-4365/ac5969",
"10.3847/2041-8213/ac7442"
] | [
"10.3847/1538-3881/adcd7a"
] | |
10.3847.1538-4357.ac9fcb_apjac9fcbf10_101 | apjac9fcbf10 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Fractional difference α 1 − 1 between the average diameter of peak brightness in a 1.3 mm black hole image and the diameter of the black hole shadow (i.e., twice the critical impact parameter) shown against the fractional FWHM of the bright ring in the image, for a broad range of black hole spins, observer inclinations... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
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10.3847.1538-4357.ac9fcb_apjac9fcbf9_102 | apjac9fcbf9 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Demonstration of the image characterization algorithm employed in Section 5. (Upper left) Sample 1.3 mm black hole image for a spin of a = 0.6, an observer inclination of 30°, and the analytic plasma model described in Section 3. (Upper right) Same image after a 15 G λ, n = 2 Butterworth filter has been applied to mimi... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
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10.3847.1538-4357.ac9fcb_apjac9fcbf5_103 | apjac9fcbf5 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | (Left) Equatorial radial velocity, (middle) density, and (right) comoving 230 GHz synchrotron emissivity profiles of accretion flows around Kerr black holes with spins equal to (top) a = 0 and (bottom) a = 0.7. In all panels, the region inside the horizon is shown with a gray-filled area, and the coordinate radii of th... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
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10.3847.1538-4357.ac9fcb_apjac9fcbf4_104 | apjac9fcbf4 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Brightness cross sections of images around a nonspinning black hole with the simple emissivity model but for profiles arbitrarily truncated at various radii r in. (a) Images where r in = 3M and r in = 4M show extremely little difference from those with the horizon boundary condition, even for small values of the disk t... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
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"10.3847/2041-8213/ac6674"
] | |
10.3847.1538-4357.ac9fcb_apjac9fcbf7_105 | apjac9fcbf7 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Radial and azimuthal components of the velocity in the flow as a function of the polar angle θ. The top panels show the velocity components at constant cylindrical radii ϖ and the bottom panels at constant spherical radii r for a GRMHD simulation with a black hole spin a = 0.7. The shaded bands in the left panels show ... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
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10.3847.1538-4357.ac9fcb_apjac9fcbf8_106 | apjac9fcbf8 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Images of black holes at 1.3mm calculated using the analytic plasma model described in Section 3, for different black hole spins, observer inclinations, and parameters of the radial velocity profile. In all panels, we have set R = 5 and B 0 = 20 G. The outline of the black hole shadow on each image is shown as a dashed... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
"10.3847/1538-4357/ad8dd5",
"10.3847/2041-8213/ac6756",
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10.3847.1538-4357.ac9fcb_apjac9fcbf6_107 | apjac9fcbf6 | 10.3847/1538-4357/ac9fcb | Black Hole Images as Tests of General Relativity: Effects of Plasma Physics | Comparison of the radial profiles of various flow properties in the analytic model to an example GRMHD simulation with a black hole spin a = 0.7. Top left shows the azimuthal velocity, top right the equatorial density, bottom left the ion temperature, and bottom right the magnetic field strength. GRMHD simulation resul... | Authors: Feryal Özel, Dimitrios Psaltis, Ziri Younsi | [] | [
"10.3847/1538-4357/ac9ab7",
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