adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Figure shows distribution of radio power (Log(P 150 W/Hz)) with redshift (z). The 24 new GRGs (left) and 10 new GRQs (right) are shown with the filled red circles. The plot also includes GRGs from Dabhade et al. (2017; with dark orange points) and from Dabhade et al. (2020c; with green points); GRQs from Kuźmicz & Jamrozy (2021; with gray points) and from Dabhade et al. (2020c; with green points).
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Histogram showing radio power (P 150) distribution of GRSs presented in the current paper for GRGs (left) and GRQs (right). For completeness of the study, the radio powers of GRGs and GRQs are calculated at 150 MHz in TGSS-ADR1. GRGs from Dabhade et al. (2020b, 2020c) and Simonte et al. (2022), and GRQs from Dabhade et al. (2020b, 2020c) and Kuźmicz & Jamrozy (2021) are also included in the plot.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Plot displays how radio power at 1400 MHz varies with the linear size of compact symmetric objects (CSOs), medium-sized symmetric objects (MSOs), and large symmetric objects (LSOs). Black dashed lines represent the evolutionary paths of high radio power sources. This plot includes TGSS-GRSs (with magenta open circles; present work), large size FR-II sources from Bhukta et al. (2022a; with yellow squares), high-power compact steep spectrum radio sources from Fanti et al. (2001; with the green plus), high-power GHz peaked-spectrum sources from Xiang et al. (2006), Liu et al. (2007; with the magenta asterisks), and high-power CSOs from Kunert-Bajraszewska et al. (2006; with the red crosses).
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Histogram showing spectral index distribution of the reported GRGs (left) and GRQs (right). We also included GRGs presented in Dabhade et al. (2020b, 2020c) and Simonte et al. (2022), and GRQs presented in Dabhade et al. (2020b, 2020c) and Kuźmicz & Jamrozy (2021). For uniformity, we calculate the spectral index of GRS using TGSS-ADR1 flux and NVSS flux.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Histogram showing the projected linear size distribution of the reported GRGs (left) and GRQs (right). We also included GRGs presented in Dabhade et al. (2020b, 2020c) and Andernach et al. (2021), and GRQs presented in Kuźmicz et al. (2018), Dabhade et al. (2020b, 2020c), Kuźmicz & Jamrozy (2021), and Simonte et al. (2022).
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Red, green, and blue image of the host galaxy of GRG J1138+4540 in BCG environment. This image uses Pan-STARRS with y band (magenta), i band (green), and g band (red). The host galaxy is elliptical in shape, which is marked in the figure.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Plot shows the radio power at 1.4 GHz with absolute R-band magnitude for GRS. The Owen–Ledlow division line (Wold et al. 2007) is drawn by using ﹩\mathrm{log}\ {{P}}_{1.4\ \,{\rm{GHz}}}=-0.67{{M}}_{R}+10.13﹩.
Paper: Discovery of Giant Radio Sources from TGSS Alternative Data Release 1: Radio, Optical, and Infrared Properties
Authors: Netai Bhukta, Souvik Manik, Sabyasachi Pal, Sushanta K. Mondal
Figure caption: Plot showing linear size vs. redshift of GRSs presented in the current paper. For completeness, we included GRS from Kuźmicz et al. (2018), Dabhade et al. (2020c), and Andernach et al. (2021).
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Comparison of resulting Sérsic indices, effective radii, and model magnitudes obtained by Nedkova et al. (2021) and this work.
Paper: Self-consistent Combined HST, K-band, and Spitzer Photometric Catalogs of the BUFFALO Survey Fields
Authors: Amanda Pagul, F. Javier Sánchez, Iary Davidzon, Anton M. Koekemoer, Bahram Mobasher, Mathilde Jauzac, Charles L. Steinhardt, Hakim Atek, Renyue Cen, Iryna Chemerynska, Lukas J. Furtak, David J. Lagattuta, Guillaume Mahler, Mireia Montes, Mario Nonino, Keren Sharon, John R. Weaver
Figure caption: Comparison of the second-best photometric redshift estimate (ZSECOND) and our nominal best-fit photometric redshift (ZPDF).
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: Comparison of light curves to the publicly available codes BoxFit and afterglowpy. We assume a top-hat jet with an isotropic equivalent energy of 1052 erg, a half-opening angle of 0.045 radians (3 degrees), and a symmetric counterjet. The initial Lorentz factor is infinite and the external medium is ISM-like. The rest of the parameters are: n 0 = 1 cm−3, E iso = 1052 erg, ϵ e = 0.1, ϵ B = 0.01, p=2.5, d L = 1028 cm, and z = 0. The viewing angle θ v and the frequency ν are labeled in the figure. Top panel: Radio and optical light curves. Bottom panel: Relative differences as compared to BoxFit.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: An image of a jet with a Gaussian profile traveling in an ISM environment. From top to bottom are the images at the coasting phase, deceleration phase, and spreading phase. The intensity distributions are normalized by maximum intensity. The markers “⋆” and “+” represent the burst origin and the flux centroid, respectively. The white contour is the 1 − σ size assuming Gaussian-equivalent intensity distribution. The parameters for the calculation are: n 0 = 1 cm−3, E 0 = 1052 erg, γ 0 = 1000, θ c = 0.1 rad, θ v = 0.3 rad, ϵ e = 10−2, ϵ B = 10−3, p = 2.2, ν = 3 × 109 Hz, d L = 44 Mpc, and z = 0.01.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: Comparison of light curves to the publicly available code afterglowpy. The jet structures are assumed to be Gaussian profiles with core width θ c labeled in the figure. The rest of the parameters for the light curves are n 0 = 1 cm−3, E 0 = 1051 erg, γ 0 = 1000, θ v = 0.3, ϵ e = 0.1, ϵ B = 0.01, p=2.5, ν = 1018 Hz, d L = 474.33 Mpc, and z=0.1. Top panel: light curves with spreading effect and calibration disabled (γ 0 = ∞ and s = 1). Bottom panel: light curves with these effects enabled.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: Same as Figure 7, but for a wind-like environmental medium profile: ﹩{n}_{0}=1{(r/{10}^{17}\,\mathrm{cm})}^{-2}﹩ cm−3. The counterjet is absent in this comparison.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: Best fitting light curves for multiwave band observation of GRB 170817A afterglow with flux centroid data included or not. The data points are normalized to 3 GHz, 5.06 × 1014 Hz, and 1 keV, respectively. The shadow regions represent a 68% confidence interval of the flux density.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The posterior distribution of flux centroid position with respect to the measurement data. The contour lines represent 68% and 95% confidence regions. The measurement at 8 days is assumed to be the burst origin.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: Same as the last figure, but for a top-hat jet with a half-opening angle of 0.1 radians (6°) traveling in a wind medium.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The posterior probability distribution of the parameters in the MCMC study with the centroid offset data included.
Paper:  jetsimpy: A Highly Efficient Hydrodynamic Code for Gamma-Ray Burst Afterglow
Authors: Hao Wang, 灏 王, Ranadeep G. Dastidar, Dimitrios Giannios, Paul C. Duffell
Figure caption: The posterior probability distribution of the parameters in the MCMC study without the centroid offset data.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Panels (a), (b), (c), and (d) show, respectively, the distributions of the total D  L  estimation errors, the sky localization errors, the numbers of candidate host galaxies, and the expected numbers of candidate host AGNs. All results are derived based on the M1 population model. The colors indicate TianQin (black), TianQin I+II (blue), and TianQin+LISA (red). And in panels (c) and (d), the solid and dashed lines, respectively, represent the conditions in which the cosmological parameters are fixed and freely varying within a prior range, when transforming the range of luminosity distances into the range of redshifts.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Minimum number ﹩{N}_{\mathrm{GW},3\sigma }^{\mathrm{threshold}}﹩ of detected EMRI events required to confirm the EMRI–AGN correlation with a 3σ significance. The black, blue, and red error bars and lines correspond to TianQin, TianQin I+II, and TianQin+LISA observations. The solid lines represent the case in which both H 0 and Ω M  are fixed to the true values, and the dashed lines with corresponding error bars represent the case in which both H 0 and Ω M  are freely variable within the prior. The error bars correspond to 1σ CIs.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Constraints on h and Ω M  given by the EMRIs detectable by TianQin (black), TianQin I+II (blue), and TianQin+LISA (red). The horizontal axis represents the different EMRI population models. The error bars correspond to a 1σ CI. The gray-shaded area represents the 1σ equivalent error of the prior, and the green-shaded region represents an error scale of 2% (10%) for h (Ω M ).
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Typical example of fitting the D  L –z relation that is derived from the EMRI dark sirens detectable by the TianQin+LISA network. Here we use the fiducial EMRI population model. The horizontal colored serial squares represent the probability distribution of redshift (normalized by the maximum) derived from the observed candidate host galaxies, and the color hues from white to red show the probability of redshift. The luminosity distances shown here represent the mean values, and their errors (1σ CI) are indicated by the black error bars. The solid green line represents the true cosmological model adopted by our simulations. The dotted–dashed red line represents the best-fit cosmological model, while the two shaded regions represent the 1σ and 2σ CIs.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: The error in constraining f agn as a function of the number of detected EMRIs. Here we fix the cosmological parameters to their true values. The black, blue, and red error bars correspond to TianQin, TianQin I+II, and TianQin+LISA. The thick and thin error bars correspond to 1σ and 2σ CIs, respectively. The dots in the middle of the error bars represent the expectations. The green dashed horizontal line represents the injected f agn in the simulations.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: An example comparing the signal likelihood ratio λ s(f agn) (vertical green dashed line) with the conditional PDFs of λ for four different values of f agn. In this example, ﹩{f}_{\mathrm{agn}}^{0}=0.1﹩, ﹩{f}_{\mathrm{agn}}^{{\prime} }=0.55﹩, ﹩{f}_{\mathrm{agn}}^{{\prime\prime} }=0.7﹩, and ﹩{f}_{\mathrm{agn}}^{\prime\prime\prime }=0.85﹩.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Same as Figure 4, but for w 0 and w  a . The green shades represent error scales of Δw 0 = 0.1 and Δw  a  = 0.1.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: Scaling tests for the 3D VSI setup performed using the Intel Haswell nodes. The environment variable MPI_IB_RAILS used by the IB network was set to 2 for all runs. (a) Efficiency, η, for the weak scaling test where the problem size per processor is fixed. (b) Efficiency for the strong scaling test where the total problem size is fixed at n  r  × n  z  × n  ϕ  = 512 × 512 × 1024. (c) Efficiency, η, with Fargo deactivated. The measure, η, accounts for the decrease in time step when Fargo is deactivated.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: A portion of the horizontal plane (r, ϕ) cutting through the disk at z/H 0 = 2 comparing the perturbation vertical vorticity, δ ω  z , for a 3D VSI run with and without Fargo. Each run was started at t/T 0 = 300.27 and run for 0.5T 0 up to t/T 0 = 300.77. (a) With Fargo. (b) Without Fargo.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: Counterrotating Taylor–Couette flow at ﹩{\mathrm{Re}}_{{\rm{i}}}\,=\,-{\mathrm{Re}}_{{\rm{o}}}\,=\,500﹩ following Dong (2008). The mesh is 48 × 962(n  r  × n  z  × n  ϕ ). (a) and (b) radial velocity contours at U i t/d = 798.8. (a) The meridional plane ϕ = 0. (b) Horizontal plane at midheight (z = π) to show that the flow is three dimensional. (c) Torque coefficients (black) compared with curves (red) digitized from Dong (2008, Figure 3) and shifted backward in time by U iΔt/d = 802. The negative of the torque coefficient is plotted for the outer cylinder.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: (a) Effective wavenumber for various difference schemes. (b) Transfer function, T(k), for the Padé filter. The grid spacing is h. The limit kh = π corresponds to the Nyquist mode, which has wavelength 2h.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: Effect of varying the strength of the Padé filter, ϵ filter when the Padé filter is used as an implicit subgrid scale treatment for an axisymmetric VSI simulation. Completely white pixels are where ω  ϕ  exceeds the range of the legend. The mesh size is 5122. The plots in the right-hand column are intended to show the level of numerical 2Δ oscillations, which appear as sawtooth features.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: 1D Euler equation tests. (a)–(c) Shock tube. (a) Density. (b) Pressure. (c) Velocity. (d) A Mach 3 shock propagating into density waves (Shu & Osher 1989). The result of the present code is compared with the WENO5–Roe method. For both tests the coefficient of artificial pressure C ap = 2 and Pade/compact filter strength ϵ filter = 0.05 (applied at the end of every step). CFL = 1.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: (a) Vertical velocity for the axisymmetric VSI simulation using a 5122 mesh. The units of velocity are scale heights (H 0) per orbit time (T 0). (b) Similarly, the perturbation azimuthal velocity.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: Density field at t = 6 for the KH instability benchmark of L2016. (a) PADÉ code with n  x  = 1024. (b) Pseudospectral DEDALUS code with n  x  = 4096. Data provided by D. Lecoanet.
Paper:  P ADÉ: A Code for Protoplanetary Disk Turbulence Based on Padé Differencing
Authors: Karim Shariff
Figure caption: Convergence for 2D advection.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: Photometry results (I vs. V − I) of starlike objects brighter than I < 23.1 and located beyond the radial distances of 6 kpc from the center of M33 are shown in panel (a). The location of stars selected to determine the TRGB magnitude is marked with the yellow parallelogram in panel (a). The histogram of the selected RGB star magnitudes (I passband) is shown in panel (b). The determined TRGB magnitude, I TRGB = 20.64, is marked with the magenta line in panel (a) and the dashed magenta line in panel (b). The isochrones of 16, 32, and 100 Myr (the blue, cyan, and green lines, respectively; the arrows of corresponding colors mark the MS tips of isochrones) are provided for reference. The candidate MS stars (presumably younger than 100 Myr) are marked with red symbols in panels (a) and (c). The deprojected XY distribution of bright MS stars (I < 23.1) is shown in panel (c); the circles mark radial distances of 6 kpc (cyan), 9 kpc (blue), and 11.5 kpc (black); two red lines indicate the 90° segment omitted from the analysis of radial profiles. The radial surface-number density profiles of MS stars are shown in panel (d). The profile colors correspond to the ages of populations: red—≲100 Myr; cyan—≲30 Myr; blue—≲15 Myr. The solid black line is fitted to the profile of the MS star (≲100 Myr) surface-number density; the dashed black line represents an expected level of the background object surface-number density.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: Number densities of detected starlike objects within the surveyed field (62′ × 95′) of the M33 galaxy are displayed. In the left-hand panel, all (803,095) objects from the catalog are shown. The right-hand panel displays 463,414 objects with V < 23.5. In the left-hand panel, positions of eight overlapping Suprime-Cam mosaics are marked with lines of different styles and colors. In the right-hand panel a red line marks an approximate area observed by Massey et al. (2006), a black line marks an approximate area observed by HST (Williams et al. 2021), and blue and magenta ellipses mark radial distances of 6 and 9 kpc, respectively. North and east directions are indicated by arrows inside the right-hand panel.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: Photometry results of starlike objects from the present M33 survey, residing within the ranges of radial distances (in kiloparsecs) indicated in the rightmost panels. The CMDs V vs. B − V and I vs. V − I include all available objects; the TCDs V − I vs. B − V show only bright objects (V < 23.5) in corresponding annuli. The red circle in panel (l) indicates a prominent group of main-sequence (MS) stars younger than ∼100 Myr residing at large radii.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: (a)–(c) Photometry results of starlike objects in M33 from Massey et al. (2006) and (d)–(f) from the present survey. The CMDs V vs. B − V [(a) 146,622, (d) 638,072] and I vs. V − I [(b) 133,258, (e) 726,312] include all objects; the TCDs V − I vs. B − V [(c) 132,529, (f) 375,455] show only bright objects (V < 23.5). Numbers in square brackets indicate counts of objects displayed in the respective panels: the first one represents data from Massey et al. (2006), while the second one represents data from our catalog.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: Photometry parameters for starlike objects in the M33 galaxy. Parameters plotted vs. B (638,072 objects), V (803,095 objects), and I (726,312 objects) magnitudes are as follows: (a)–(c) photometric errors, σ; (d)–(f) object-profile sharpness in respect to PSF, sharpness; (g–(i) accuracy of object-profile fitting with PSF, χ 2.
Paper: Subaru Suprime-Cam Wide-field BVI Stellar Photometry of the M33 Galaxy
Authors: Rima Stonkutė, Vladas Vansevičius
Figure caption: Differences of calibrated magnitudes from the M33 Suprime-Cam catalog minus magnitudes from Massey et al. (2006) vs. the latter magnitudes. The numbers of stars (N) used for calibration and the scatterings (σ, rms) of differences are indicated in the panels.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Constraints on (h, Ω M ) (left panel) and (w 0, w  a ) (right panel) by combining the EMRIs detected by TianQin with AGN catalogs. The eccentricities at plunges are set to zero, and the other parameters are derived from the M1 model. The blue contours represent the constraints derived from candidate host galaxies and the red contours represent the constraints from candidate host AGNs. The two levels of contours correspond to 1σ and 2σ CIs, respectively. The cyan crosses mark the injected cosmological parameters in our simulations.
Paper: Improving Cosmological Constraints by Inferring the Formation Channel of Extreme-mass-ratio Inspirals
Authors: Liang-Gui Zhu, 良贵 朱, Hui-Min Fan, 会敏 范, Xian Chen, 弦 陈, Yi-Ming Hu, 一鸣 胡, Jian-dong Zhang, 建东 张
Figure caption: Typical background distribution P bg(λ) (dashed line) and probability distribution P(λ) (solid line) of the likelihood ratio λ in Equation (18) for 100 EMRIs detected by TianQin+LISA, assuming our fiducial cosmological parameters. The black, blue, cyan, and red colors correspond to four fractions of f agn = 0.1, 0.3, 0.6, 1.0, respectively.