adsabs/AstroCLIMB huggingface dataset:
Paper: The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Authors: ZiQian Shang, 自乾 尚, Zhao Wu, 昭 武, Yan Liu, 岩 刘, Yu Bai, 宇 白, Guang Lu, 光 路, YuanYuan Zhang, 园园 张, Lei Zhang, 磊 张, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The structure of a typical total-power radiometer with a matched load and the input–output relationship of the SLD. The nonlinearity of the SLD causes errors since the antenna output is T1 when the Sun is quiet and T2 when it is in burst.
Paper: The Calibration of the 35–40 GHz Solar Radio Spectrometer with the New Moon and a Noise Source
Authors: ZiQian Shang, 自乾 尚, Zhao Wu, 昭 武, Yan Liu, 岩 刘, Yu Bai, 宇 白, Guang Lu, 光 路, YuanYuan Zhang, 园园 张, Lei Zhang, 磊 张, YanRui Su, 艳蕊 苏, Yao Chen, 耀 陈, FaBao Yan, 发宝 严
Figure caption: The noise factor of the upgraded calibration unit. It is reduced by 70 K compared to the pre-upgrade stage.
Paper: Spectral Features of the Solar Transition Region and Chromospheric Lines at Flare Ribbons Observed with IRIS
Authors: L. F. Wang, Y. Li, Q. Li, X. Cheng, M. D. Ding
Figure caption: (a)–(i) Si IV, C II, and Mg II line profiles at the selected positions and time steps marked by the colored diamonds in Figure 12. Different colors represent different time steps. (j)–(l) Example profiles (black) and the single-Gaussian fittings (red) for the Si IV line at the three selected positions. The velocities by using the moment method (V  m ) and single-Gaussian fitting (V  s ) are given in the panels. The vertical dashed line in each of the panels denotes the reference wavelength of the spectral line.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The maximum influence of nonuniformity. From left to right, the three panels are for the V, B, and U bands (labels are at the upper-right corner of each panel). Thin solid, dashed, dotted–dashed, dotted, and thick solid lines in all three panels represent the NU﹩{}_{\max }﹩ calculated with the raw background count rate densities CRD﹩{}_{\mathrm{raw}}^{\mathrm{bkg}}﹩, which are 0, 0.005, 0.01, 0.03, and 0.05 count s−1 pixel−1, respectively. The rapid drop at high rates is because the scaled count rate used to calculate the COI and the EXT factors for the inner edge of the wing is larger than the valid threshold for the fitted model of the EXT factor.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: Difference between UVOT photometries and converted photometries from Tycho-2 and GSPC sources. The left panel shows the V band, and UVOT photometries are systematically fainter than converted photometries by ∼0.08 mag, which can be clearly seen for GSPC data points. However, due to the large scatter of Tycho-2 points, the offset is not obvious. For the B band, the difference is ∼0.13 mag between UVOT photometries and converted photometries, but due to lack of GSPC points and the large scatter of Tycho-2 points, the figure for the B band is not shown. However, as shown in the right panel, the difference is negligible (∼0.026 mag) for the U band. Dashed lines in both panels represent the COI saturation limit. As for points above the COI limit, they are actually not saturated, but after the LSS and the SEN correction, their corrected count rates are beyond the limit. For example, the COI corrected count rate is 360 count s−1 for a point source, which is smaller than the COI limit ∼372, but the LSS and the SEN factors are both 1.1. As a result, the corrected count rate is 435.6 count s−1, which is greater than the COI limit.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The fitted template of the count density distribution (CDD). Red, green, and blue points/lines represent extracted CDD/fitted templates for the V, B, and U bands, respectively. The cyan region represents the wing of the PSF, and the background is estimated from the gray region. For the region with r < 15″, the coincidence loss strongly affected the PSF.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The V-band calibration for the PSF method in different sub-data sets. From left to right, the three panels show the calibration for event 1 × 1, image 1 × 1, and image 2 × 2 data sets, respectively. Please refer to the caption of Figure 9 for the meaning of all notations.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The U-band calibration for the PSF method in different sub-data sets. From left to right, the three panels show the calibration for event 1 × 1, image 1 × 1, and image 2 × 2 data sets, respectively. Please refer to the caption of Figure 9 for the meaning of all notations.
Paper: A Method to Measure Photometries of Moderately Saturated UVOT Sources
Authors: Hao Zhou, Zhi-Ping Jin, Stefano Covino, Yi-Zhong Fan, Da-Ming Wei
Figure caption: The B-band calibration for the PSF method in different sub-data sets. From left to right, the three panels show the calibration for event 1 × 1, image 1 × 1, and image 2 × 2 data sets, respectively. Please refer to the caption of Figure 9 for the meaning of all notations.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The optimized hyperparameters of a network in reconstructing an observable process with the number of hidden layers N  hl  and the number of neurons N  ne  for (a) Hubble expansion rate H(z), N  hl  = 1, N  ne  = 512; (b) growth history of the Universe f σ 8(z), N  hl  = 1, N  ne  = 128; and (c) the angular diameter distance D  A (z), N  hl  = 1, N  ne  = 128.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The reconstructed functions of (a) H(z), (b) f σ 8(z), and (c) D  A (z) labeled by the black solid lines and the corresponding 1σ error with neural networks that have one hidden layer shown by the blue error areas. The yellow circles with black error bars represent the observational data, and the red dashed lines with orange error areas correspond to the fiducial flat ΛCDM models ﹩\left\{H(z),f{\sigma }_{8}(z),{D}_{A}(z)\right\}﹩ with parameters ﹩\left\{{H}_{0},{{\rm{\Omega }}}_{m0},{\sigma }_{8}\right\}﹩ inferred from Planck 2018 results, respectively.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of Ω m0 and σ 8 that are estimated from parameter constraints with (a) the total mock data z ∈ [0, 4], (b) the part of mock data ordering before the transition point z ∈ [0, z  ep ], (c) the part of mock data containing the transition point z ∈ [0.2, 0.6], and (d) the part of mock data ordering after the transition point z ∈ [3.6, 4].
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The Gaussian sampling results of (a) Hubble constant H 0, (b) matter density parameter Ω m0, and (c) matter fluctuation amplitude σ 8, and the joint mock data sets of (d) ﹩\left(H(z),f{\sigma }_{8}(z)\right)﹩, (e) ﹩\left(f{\sigma }_{8}(z),{D}_{A}(z)\right)﹩, and (f) ﹩\left(H(z),{D}_{A}(z)\right)﹩.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The relative errors in the Taylor expansion of f σ 8 vary with redshift z, which are colored corresponding to each expansion point z  ep , respectively.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: Observable curves in 3D ﹩\left(H,f{\sigma }_{8},{D}_{A}\right)﹩ space and 2D projections. Data points and errors are simulated based on a fiducial flat ΛCDM model assuming the Planck 2018 cosmological parameters.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The theoretical curves of f σ 8(z) vary with redshift z from 0 to 4, which are colored corresponding to Ω m0 = 0.1, 0.2, 0.3, 0.4, 0.5, and 0.6, respectively.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The transition point curve of f σ 8 as a function of matter density parameter Ω m0 from 0 to 1.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The construction of the observable space and parameter inference.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of H 0, Ω m0, and σ 8 that are estimated from our joint constraint method with the interval of the redshift bin (a) z ∈ [0, 0.8], (b) z ∈ [0.8, 1.5], (c) z ∈ [1.5, 2.3], and (d) z ∈ [2.3, 4].
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of H 0, Ω m0, and σ 8 that are estimated from (a) our joint constraint method with redshift and redshift error, (b) our joint constraint method with redshift but no redshift error, and (c) the traditional combined method without redshift.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of H 0, Ω m0, and σ 8 that are estimated from our joint constraint method (a) with 10 points in the observational data, (b) with 15 points in the observational data, and (c) with 20 points in the observational data.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of H 0, Ω m0, and σ 8 that are estimated from (a) our joint constraint method with the mock data, (b) observational data, and (c) the traditional combined method with observational data.
Paper: Novel Cosmological Joint Constraints in Multidimensional Observable Space with Redshift-free Inferences
Authors: Wei Hong, Kang Jiao, Yu-Chen Wang, Tingting Zhang, Tong-Jie Zhang, 同杰 张
Figure caption: The 68%, 95%, and 99% confidence regions of the joint and marginal posterior probability distributions of H 0, Ω m0, and σ 8 that are estimated from our joint constraint method with the interval of the redshift bin (a) z ∈ [0.11, 0.8], (b) z ∈ [0.8, 1.5], and (c) z ∈ [1.5, 1.944].
Paper: Catalog of the Galactic Population of X-Ray Pulsars in High-mass X-Ray Binary Systems
Authors: Vitaliy Kim, Ildana Izmailova, Yerlan Aimuratov
Figure caption:  P s–﹩| \dot{P}| ﹩ diagram for Galactic X-ray pulsars in HMXBs. In the spin-up diagram (left panel), the lines correspond to the maximal possible spin-up for Kd scenario, with B ns = 1013 G, L x = 1037 erg s−1 (dashed blue line) and with B ns = 1012 G, L x = 1037 erg s−1 (solid orange line). In the spin-down diagram (right panel), the lines correspond to the maximal possible spin-down for the Kd scenario, with B ns = 1013 G, L x = 1037 erg s−1 (horizontal dashed–dotted magenta line) and with B ns = 1012 G, L x = 1037 erg s−1 (horizontal dotted line). The dashed blue line corresponds to the maximal possible spin-down for QSp, with B ns = 1013 G, L x = 1037 erg s−1, and the solid orange line corresponds to QSp with B ns = 1012 G, L x = 1037 erg s−1. Due to the high precision of the measurements, the error bars for some objects are within data points.
Paper: Catalog of the Galactic Population of X-Ray Pulsars in High-mass X-Ray Binary Systems
Authors: Vitaliy Kim, Ildana Izmailova, Yerlan Aimuratov
Figure caption: Distribution of the Galactic HMXB sources in Aitoff projection. The inset resolves the dense central region. Crosses indicate objects from the catalog by Neumann et al. (2023), while empty diamonds show the objects from the catalog by Fortin et al. (2023). Transient (red) and persistent (blue) pulsars in HMXBs are indicated by the coloring of the corresponding crosses, diamonds, or both. Crosses and diamonds without coloring indicate HMXBs with a black hole as the main X-ray active component. Candidates of pulsars are colored green. All HMXB X-ray pulsars (except X Per) have absolute values of galactic latitude not exceeding 4.°1.
Paper: Catalog of the Galactic Population of X-Ray Pulsars in High-mass X-Ray Binary Systems
Authors: Vitaliy Kim, Ildana Izmailova, Yerlan Aimuratov
Figure caption: Venn diagram of the coordinate crossmatch of the three catalogs (not to scale). Each colored sector indicates the number of unique objects present either in the single catalog (3, 19, and 826), in two catalogs (2, 3, and 49), or in all three catalogs (98).
Paper: Catalog of the Galactic Population of X-Ray Pulsars in High-mass X-Ray Binary Systems
Authors: Vitaliy Kim, Ildana Izmailova, Yerlan Aimuratov
Figure caption: Evolution of the spin period (frequency) of some Galactic X-ray pulsars in HMXBs within the time range from the 1970s to 2022 received by HEAO-1, Tenma, Ginga, Einstein, OSO-8, Ariel V, and Granat (red; Nagase 1989), the CGRO (black; CGRO Collaboration 2000), INTEGRAL (magenta; Integral Collaboration 2022), and Fermi-GBM (blue; Fermi Collaboration 2022). The error bars for later missions are within data points due to the increase in instrumental precision.
Paper: Catalog of the Galactic Population of X-Ray Pulsars in High-mass X-Ray Binary Systems
Authors: Vitaliy Kim, Ildana Izmailova, Yerlan Aimuratov
Figure caption: Observed flux (in keV cm−2 s−1) for a time in Modified Julian Date (MJD) by Fermi-GBM (Fermi Collaboration 2022) from some persistent (left column) and transient (right column) X-ray pulsars in the range 12–50 keV.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Similar to Figure 6, but the mean number counts of our LAEs are compared with those of similar previous LAE surveys. From top to bottom, results for NB387, NB816, and NB921 are shown. Here we use total magnitude (MAG_AUTO of SExtractor) for the x-axis value for a fair comparison. References for the NB387 results: Nakajima et al. (2012); Hao et al. (2018). References for the NB816 results: Ouchi et al. (2008); Shibuya et al. (2018a); Ono et al. (2021). References for the NB921 results: Ouchi et al. (2010); Shibuya et al. (2018a); Ono et al. (2021).
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Similar to Figure 7, but showing the result for the CHORUS NBs. From top to bottom, results for NB527, NB718, and NB973 are shown. Here we use total magnitude (MAG_AUTO of SExtractor) for the x-axis value for a fair comparison. References for the NB527 results: Ouchi et al. (2008); Ono et al. (2021). References for the NB718 results: Zhang et al. (2020); Ono et al. (2021). References for the NB973 results: Itoh et al. (2018); Ono et al. (2021).
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Number counts of our LAEs in each subfield. From top to bottom, results for NB387, NB816, and NB921 are shown. Here we use total magnitude (MAG_AUTO of SExtractor) for the x-axis value. Symbols for the same x-axis value are slightly offset for clarity.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Redshift distribution of spectroscopically confirmed LAEs in our catalogs. Thick colored curves show the normalized transmission curves of HSC NB filters (Figure 1) with wavelength converted to Lyα redshift, while thin colored curves show the shifted ones.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Limiting magnitude maps (5σ, 2.″0 aperture) for the NB387 images.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: From left to right, sky distribution of NB527, NB718, and NB973 LAEs (z = 3.3, 4.9, and 7.0). Thick (thin) blue dots indicate the locations of objects brighter (fainter) than NB527 or NB718 = 25.75 mag, while all sources are plotted with thick blue dots in the NB973 map. North is up, and east is to the left. Masked regions are shown in gray.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Sky distribution of NB387 LAEs (z = 2.2). Thick (thin) blue dots indicate the locations of objects brighter (fainter) than NB387 = 24.0 mag, respectively. North is up, and east is to the left. Masked regions are shown in gray.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Sky distribution of NB816 LAEs (z = 5.7). Thick (thin) blue dots indicate the locations of objects brighter (fainter) than NB816 = 25.5 mag, respectively. North is up, and east is to the left. Masked regions are shown in gray.
Paper: SILVERRUSH. XIII. A Catalog of 20,567 Lyα Emitters at z = 2−7 Identified in the Full-depth Data of the Subaru/HSC-SSP and CHORUS Surveys
Authors: Satoshi Kikuta, Masami Ouchi, Takatoshi Shibuya, Yongming Liang, Hiroya Umeda, Akinori Matsumoto, Kazuhiro Shimasaku, Yuichi Harikane, Yoshiaki Ono, Akio K. Inoue, Satoshi Yamanaka, Haruka Kusakabe, Rieko Momose, Nobunari Kashikawa, Yuichi Matsuda, Chien-Hsiu Lee
Figure caption: Sky distribution of NB921 LAEs (z = 6.6). Thick (thin) blue dots indicate the locations of objects brighter (fainter) than NB921 = 24 mag, respectively. North is up, and east is to the left. Masked regions are shown in gray.
Paper: Powerful Radio Sources in the Southern Sky. II. A Swift X-Ray Perspective
Authors: F. Massaro, S. V. White, A. Paggi, A. Jimenez-Gallardo, J. P. Madrid, C. Mazzucchelli, W. R. Forman, A. Capetti, C. Leto, A. García-Pérez, C. C. Cheung, V. Chavushyan, N. P. H. Nesvadba, I. Andruchow, H. A. Peña-Herazo, E. Sani, R. Grossová, V. Reynaldi, R. P. Kraft, B. Balmaverde, S. Cellone
Figure caption: Left panel: the X-ray image of G4Jy 1136 obtained from the merged XRT event file as in Figure 2, smoothed with a Gaussian kernel of 10 pixels (i.e., 23.″57) and with radio contours drawn from the TGSS radio map overlaid. These were computed starting at level of 0.1 Jy beam−1 and increasing in level by a binning factor of 4. Right panel: the same field but observed as part of the WISE All-sky survey at 12 μm. The magenta dashed circle in the right panel is centered on the location of the X-ray counterpart to mark its position and that the mid-IR associated source (position indicated by the red cross in the right panel). According to our previous analysis (Paper I) this radio source lacks an optical counterpart but the Swift-XRT analysis revealed that the mid-IR counterpart assigned in the G4Jy catalog is correct as it overlaps with its X-ray counterpart. It is worth highlighting the presence of a relatively bright star located in the northwestern direction with respect to the position of G4Jy 1136. However it appears fainter in the 12 μm WISE image, shown here, rather than in that at 3.4 μm used in Paper I. A cyan cross, if present, marks the location of the radio source (i.e., brightness-weighted radio centroid as reported in the G4Jy catalog) while the red one that of the assigned mid-IR counterpart associated in the analysis of the G4Jy sample.