adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Zoomed up images of ALMA (Cycle 2 and Cycle 4) 0.88 mm (Band 7 340 GHz) continuum intensity of MG J0414+0434 showing A1 and A2. The contours and colors show intensity larger than 3σ. The images were obtained from the data of Cycle 4 observations (left), and the combined data of Cycle 2 and Cycle 4 observations (right). The imaging was carried out with a Briggs weighting of robust = − 1. The values in the legends show intensity in units of 1σ. The contours start from a 3σ level and increase with a step of 2σ. The small ellipses in the bottom-left corners show the synthesized beam sizes 0.″024 × 0.″016 with P.A. 50.°4 (left) and 0.″025 × 0.″018 with P.A. 49.°5 (right). The 1σ errors are 94 μJy beam−1 (left) and 66 μJy beam−1 (right). Boxes, circles, triangles, and stars correspond to jet components p, q, r, and s at 5 GHz, respectively. The coordinates are J2000 and centered at the centroid of the primary lensing galaxy G.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Peak-subtracted ALMA (Cycle 2 and Cycle 4) 0.88 mm (Band 7, 340 GHz) continuum intensity of MG J0414+0434. Pointlike sources at radio-jet/core components p and q were subtracted off with parameters c p = 0.626, c q = 0.324. The contours and colors show intensity. The imaging was carried out with a Briggs weighting of robust = 0. The ticks in the legend show intensity in units of the background noise of 1σ = 30 μJy beam−1. The contours start from a −5σ level and increase with a step of 3σ. The small ellipses in the bottom-left corners in each panel show the synthesized beam size 0.″038 × 0.″029 with P.A. 42.°5. The symbols represent p, q, r, and s at 5 GHz, as in Figure 14. The coordinates are J2000 centered at the centroid of the primary lensing galaxy G.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Mock simulation of reconstruction of convergence perturbation δ κ. The plotted images are contour maps for the original values (left), the best-fitted reconstructed values obtained with the magnification weighting (middle), and the homogeneous weighting (right). The plots were obtained from the 36 modes that best fit the mock data. Inside the green curves, the “observed” intensity is larger than 4σ. The contour spacing is 0.002. Red “X” symbols show the original positions of the lensed quasar core. Blue circled dots show the positions of object X (upper right) and Y (lower left; see Section 6.5) in each panel. At the boundary of each panel, the potential perturbation is set to zero, and the center of the coordinates is the centroid of observed G.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Difference in de-lensed mean peak-subtracted images in the source plane. The left panel shows the difference in intensity of de-lensed mean peak-subtracted images with the same parity in the unperturbed smooth model. The middle panel shows the difference in intensity of de-lensed mean peak-subtracted images with the same parity in a Type A model obtained with the magnification weighting, L = 3.″6, and c q + c p = 0.95. The right panel shows the change in the difference in intensity between the unperturbed (left) and perturbed (middle) models. The contours begin from a −8σ level and increase with a step of 2σ. The black points show the positions of meshes. The red curves show the caustics. The green X’s show the position of the best-fitted core component q.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Continuum intensity for the original and de-lensed mock sources. Except for the original image in the top left, the bright quasar components (at the position of a blue or red “X”) were subtracted off. The colors show intensity in units of ﹩\mathrm{Jy}\,{\mathrm{arcsec}}^{-2}﹩. The plotted images are the original source (top left), de-lensed source reconstructed with the magnification weighting (top middle), de-lensed source reconstructed with the homogeneous weighting (top right), zoomed up images of the original source (bottom left), differences between the de-lensed source reconstructed with the magnification weighting and the original one (bottom middle), and difference between the de-lensed source reconstructed with the homogeneous weighting and the original one (bottom right).
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Fourier modes used in our analysis. m, n are Fourier mode numbers that specify a Fourier mode function δ ψ defined in Equation (16). A potential perturbation is decomposed into 36 modes, which include six low-frequency modes (light gray), 22 intermediate-frequency modes (middle gray), and eight high-frequency modes (dark gray). We also use three frequency bins: seven low-to-intermediate-frequency modes (circle), 11 intermediate-to-high-frequency modes (star), and seven high-frequency modes (square).
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: The best-fitted positions of four VLBA jet components in the lens plane using the ALMA data, MIR flux ratios, HST positions of galaxies, and VLBA positions of lensed jet component q. The red symbols represent the positions of p, q, r, and s observed at 5  GHz as in Figure 14, and circles indicate their errors. The black “X” symbols represent the best-fitted positions in a Type A model obtained with the magnification weighting with L = 3.″6 and c q + c p = 0.95. The coordinates are J2000 centered at the centroid of the primary lensing galaxy G. North is up and east is left.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Residual error in the reconstructed mock source intensity as a function of S/N. The pixel size is 0.″0066. The red dotted curves show the mean (over a bin width of Δ(S/N) = 1) ratio of the residual error in mock source intensity in units of the 1σ nominal noise as a function of the ratio of the signal to the 1σ nominal noise at a given pixel. The black full curves show the best-fitted polynomial functions ﹩{\left({\rm{S}}/{\rm{N}}\right)}^{\beta }﹩ with β = 0.319 (left) and β = 0.383 (right) for the magnification and homogeneous weightings, respectively.
Paper: ALMA Measurement of 10 kpc Scale Lensing-power Spectra toward the Lensed Quasar MG J0414+0534
Authors: Kaiki Taro Inoue, Takeo Minezaki, Satoki Matsushita, Kouichiro Nakanishi
Figure caption: Contour maps of differences between the original and best-fitted convergence perturbation δ κ obtained with the magnification weighting (left) and homogeneous weighting (right). The contour spacing is 0.002. The red and blue symbols and green curves are the same as in Figure 10. The value are set to be zero in which the “observed” intensity is smaller than 4σ for illustrative purposes.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: 2–10 keV band luminosity vs. that of intrinsic continuum (left hand), and neutral (middle) and ionized (right hand) according to each model. Lines represent the percentage of the quantity in the X-axis with respect to the Y-axis. From bottom to top 100%, 80%, 50%, 10%, and 1% of the intrinsic (left-hand panel) and reflection (right-hand panels) luminosities. Green diamonds, blue squares, and red circles correspond to the hybrid, neutral, and ionized models, respectively. Empty symbols correspond to the sources that equally prefer neutral or ionized model.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: Emission-line diagnostics and spatial maps for GAMA 106717. Each figure in the first row shows the emission-line diagnostics colored according to where each spaxel falls in its respective diagram: green for star-forming, blue for composite or LINER, and red for AGN. Below each diagnostic is the corresponding spatial map showing where in the galaxy the points in the diagram above are located.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: Histograms of the distribution of SMBH mass (top), intrinsic 2–10 keV luminosity (middle), and Eddington ratio (bottom) for the full sample (dotted) vs. the preferred model (dashed). Bars corresponding to the objects that prefer only the neutral or ionized models are given in blue and red colors. The bars of the objects that equally prefer both models are given in cyan and magenta. Note that we do not include the three sources discarded for the analysis in the intrinsic properties of the sample.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: Photon index, Γ, vs. Eddington ratio. Green diamonds, blue squares, red circles, and yellow triangles correspond to the hybrid, neutral, ionized, and nonreflection models, respectively. Symbols of the three sources that equally prefer neutral or ionized models are joined with a dashed-black line. In addition, the name of these sources is written on the side. Note that we do not include the three sources discarded for the analysis on the intrinsic properties of the sample and do not include two nonrefl. sources because we could not get a value for the photon index of these objects.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption: Power-law fit to Mrk 382 (top left-hand panel), IRAS 13224-3809 (top right-hand panel), and MR 2251-178 (bottom panel). We show the best fit (black and red solid lines) to the data in the top panel and the ratio between model and data in the bottom panel. The gold and dark cyan dots show the data from XMM-Newton and NuSTAR, respectively.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption:                         Best fit to the three objects that equally prefer the neutral and ionized models. The description is the same as that given in Figure 4.
Paper: Beyond BPT: A New Multidimensional Diagnostic Diagram for Classifying Power Sources Tested Using the SAMI Galaxy Survey
Authors: Victor D. Johnston, Anne M. Medling, Brent Groves, Lisa J. Kewley, Luca Cortese, Scott Croom, Ángel R. López-Sánchez, Henry Zovaro, Joss Bland-Hawthorn, Julia Bryant, Jon Lawrence, Matt Owers, Samuel Richards, Jesse van de Sande
Figure caption: A flowchart showing a simplified decision tree used by our classification method. The yellow boxes show steps in the classification process while the other colored boxes represent the final classification that a galaxy can fall into.
Paper: Testing Physical Scenarios for the Reflection Features of Type-1 AGNs using XMM-Newton and NuSTAR Simultaneous Observations
Authors: César Ivan Victoria-Ceballos, Omaira González-Martín, Josefa Masegosa, Anna Lia Longinotti, Donaji Esparza-Arredondo, Natalia Osorio-Clavijo
Figure caption:                         Best fit to the object preferring the neutral model. The description is the same as that given in Figure 4.
Paper: Lithium in Turnoff Stars in the Globular Cluster M5: A Quest for Primordial Lithium
Authors: Ann Merchant Boesgaard, Constantine P. Deliyannis
Figure caption: Lithium abundances in turnoff stars in several globular clusters with a range of iron abundances. The results for M5 are from this work, on the Carney temperature scale, shown as filled red circles. The results for M92 from Boesgaard et al. (1998), also on the Carney temperature scale, are shown as blue filled squares; two stars with identical Li values are offset from each other for clarity. The values for NGC 6397 are from Bonifacio et al. (2002) and Pasquini & Molaro (1996), shown as open black circles. The range in values for NGC 6397, shown by the vertical black dashed line, are from Lind et al. (2009) and Gonzalez Hernandez et al. (2009). The orange triangles for NGC 6752 represent nine stars from Pasquini et al. (2005). The range for 217 turnoff stars, shown as the vertical dashed line, is from Gruyters et al. (2014) and Schiappacasse-Ulloa et al. (2022). There are 52 turnoff stars in M4 shown as a range in A(Li) as the purple dashed vertical line from Monaco et al. (2012) and Spite et al. (2016). The values for 47 Tuc (NGC 104) are from Pasquini & Molaro (1997), shown as green filled pentagons, and those by Bonifacio et al. (2007) by open green pentagons. The green dashed line shows the range of values for turnoff stars for 47 Tuc found by Aoki et al. (2021). A typical error bar is shown in the lower left corner. The horizontal line at A(Li) = 2.2 represents the mean abundance of Li found for metal-poor field stars first identified by Spite & Spite (1982). The horizontal line at A(Li) = 2.719 corresponds to the predicted value for primordial Li indicated by the WMAP results (Cyburt et al. 2008 and Cyburt et al. (2016).
Paper: Lithium in Turnoff Stars in the Globular Cluster M5: A Quest for Primordial Lithium
Authors: Ann Merchant Boesgaard, Constantine P. Deliyannis
Figure caption: The equivalent width measurements for two stars in M5. The crosses are for several Fe I lines and the red-circled star is for the Li I line, which is stronger in the star 5323. The line indicates equality in the equivalent widths. An error bar for the line strength measurements is shown in the lower right and corresponds to ±5 mÅ.
Paper: Lithium in Turnoff Stars in the Globular Cluster M5: A Quest for Primordial Lithium
Authors: Ann Merchant Boesgaard, Constantine P. Deliyannis
Figure caption: The spectrum synthesis fits for Li in two of our stars. The black squares are the observed spectra, and the blue solid line is the best fit. The red dashed lines are a factor of 2 more Li and a factor of 2 less Li; the long-dashed red line represents no Li at all. The temperatures and A(Li) values are for the Carney (1983) temperature scale.
Paper: Lithium in Turnoff Stars in the Globular Cluster M5: A Quest for Primordial Lithium
Authors: Ann Merchant Boesgaard, Constantine P. Deliyannis
Figure caption: Examples of spectra of two stars in the Li region. The positions of the Li I and Ca I features are indicated. The Ca I lines are similar in strength in both stars, while the Li I feature is stronger in 5323.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: The LRG fractions in color–magnitude space used to select optical and IR LRG samples from our magnitude-limited mock galaxy catalogs. The first and second columns show optical and IR LRG targets, respectively, in r − z color vs. M  z  magnitude space. The third and fourth columns show optical and IR LRG targets, respectively, in r − W1 color vs. M  W1 magnitude space. Each row shows a different redshift bin. Note that the distributions of optical LRGs in the z-band model (first column) and IR LRGs in the W1-band model (fourth column) are compact by design; i.e., the fraction of galaxies that are LRGs is either ∼zero or ∼1 nearly everywhere in color–magnitude space. In contrast, the distributions of IR LRGs in the z-band model (second column) and optical LRGs in the W1-band model (third column) have a broader gradient between zero and 1, especially toward fainter magnitudes. The boxed region in each panel marks the luminous end of the red sequence, where essentially all galaxies are expected to be LRGs. The LRG fraction in this boxed region is at least 98% for the W1-band model (third and fourth columns) but only 92%–94% for the z-band model (first and second columns).
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Predicted clustering of IR (top row) and optical (bottom row) mock LRGs compared to the clustering of the relevant LRG target samples from the data (black points in each panel). Dotted purple lines in each panel show mock LRGs from the default z-band model (monotonic correspondence between r − z color and z starve at fixed luminosity), while solid purple lines show LRGs from the z-band model with randomized colors. Dashed orange lines in each panel show mock LRGs from the default W1-band model, and solid orange lines show LRGs from the W1-band model with randomized colors. Each column shows a different redshift bin.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: The color-coded points in each panel are bright (M  z  < −23.7) red-sequence objects with photometric redshifts between 0.4 and 0.7 that are not DESI LRG targets, i.e., objects with M  z  < −23.7 in the first two columns of Figure 8 that cause the LRG fraction at the bright end of the red sequence to be <1. The dashed and solid black lines in panels (a), (b), (d), and (e) are the various color–color and color–magnitude cuts that define the optical and IR DESI LRG target samples (Equations (4a) and (5a), respectively). The light blue and gray contours show the distributions of all optical and IR DESI LRG targets with photometric redshifts between 0.4 and 0.7.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Predicted HODs of IR (top row) and optical (bottom row) mock LRGs from both the z-band (thicker purple lines) and W1-band (thicker orange lines) models. Also shown in fainter purple and orange lines are the HODs of the z- and W1-band magnitude-limited mock galaxy catalogs from which mock LRGs are selected. Solid (dotted) lines show results for central (satellite) galaxies and LRGs. Each column shows a different redshift bin. The best-fit values of a standard five-parameter HOD model, as well as the satellite fraction, for each mock LRG sample are given in Table 8.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Distributions of r − z, g − r, and r − W1 colors of optical (shaded histograms) and IR (open histograms) LRGs from above (box A; top three panels) and along (box B; bottom three panels) the red sequence in r − W1 vs. M  W1 color–magnitude space. The regions of color–magnitude space corresponding to boxes A and B are shown in Figure 3. The mean, median, and skewness of each distribution, as well as the number of LRGs in each population, are given in Table 5. Optical and IR LRGs from along the red sequence have similar distributions of each color, while optical LRGs above the red sequence have redder r − z and g − r and bluer r − W1 colors compared to IR LRGs in the same W1-band luminosity range.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Illustration of the model color assignment procedure (Section 3.4), which equates halo z starve with galaxy color at fixed luminosity. The dotted purple curve is the cumulative distribution of 0.43(r − z) color for galaxies in the −23.0 > 0.43 M  z  > −23.05 luminosity bin, while the solid gray curve is the cumulative distribution of halo z starve for mock galaxies in the same luminosity bin. The magenta arrows indicate that a mock galaxy in this luminosity bin in a halo with z starve ≈ 2.6 is assigned a 0.43(r − z) color of 0.96. The faint purple and gray curves are the galaxy color and halo z starve distributions of additional luminosity bins.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Comparison of LRG HOD parameters from this work at z ∼ 0.63 (orange lines) with the analytic HOD fits of Zhou et al. (2021; green lines) and the SAM of Hernández-Aguayo et al. (2021; gray lines) in comparable redshift bins. Solid, dotted, and dashed–dotted lines show results for, respectively, central LRGs, satellite LRGs, and the combination of both.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: The IR (r − W1) vs. optical (r − z) color for IR (left panel) and optical (right panel) LRGs at 0.4 < z phot < 0.5.
Paper: The Galaxy–Halo Connection of DESI Luminous Red Galaxies with Subhalo Abundance Matching
Authors: Angela M. Berti, Kyle S. Dawson, Wilber Dominguez
Figure caption: Projected clustering of the z-band (top panel) and W1-band (bottom panel) absolute magnitude–limited parent galaxy samples and corresponding mock galaxy catalogs, with different colors and line styles representing different redshift bins as denoted by the legend in each panel. Redshift bins are offset by 0.15 dex for clarity.
Paper: FAST Drift Scan Survey for HI Intensity Mapping: I. Preliminary Data Analysis
Authors: Yichao Li, Yougang Wang, Furen Deng, Wenxiu Yang, Wenkai Hu, Diyang Liu, Xinyang Zhao, Shifan Zuo, Shuanghao Shu, Jixia Li, Peter Timbie, Réza Ansari, Olivier Perdereau, Albert Stebbins, Laura Wolz, Fengquan Wu, Xin Zhang, Xuelei Chen
Figure caption: Top panel: The delay spectrum of the bandpass. The delay spectra of the bandpass smoothed with different window function sizes are shown in different colors. Bottom panel: The delay spectrum of the TOD. The gray curve shows the delay spectrum of the TOD before bandpass calibration, while the other curves show the results of bandpass-calibrated data using bandpass measurement smoothed with different window function sizes. All of the delay spectra are estimated using the XX polarization of the central beam data of 20210302. The dashed vertical line marks the delay of τ ∼ 0.92 μ s, associated with the standing wave between the FAST feed and reflector.