adsabs/AstroCLIMB huggingface dataset:
Paper: Linear Mode Decomposition in Magnetohydrodynamics Revisited
Authors: G. P. Zank, L.-L. Zhao, L. Adhikari, M. Nakanotani, A. Pitňa, D. Telloni, H. Che
Figure caption: The assumed coordinate system with the mean flow vector  U  0 aligned along the ﹩\hat{x}﹩-axis. The 2D wavenumber coordinates are also illustrated.
Paper: Characterizing the Emission Region Properties of Blazars
Authors: Junhui Fan, Hubing Xiao, Wenxin Yang, Lixia Zhang, Anton A. Strigachev, Rumen S. Bachev, Jianghe Yang
Figure caption: The distributions of B and γ p. The left panels give the distributions of the two parameters, with the dashed curve standing for the Gaussian fit of the histogram. The right panels give the corresponding cumulative probability distributions. The red color stands for FSRQs and the blue color stands for BL Lacs throughout this paper.
Paper: Characterizing the Emission Region Properties of Blazars
Authors: Junhui Fan, Hubing Xiao, Wenxin Yang, Lixia Zhang, Anton A. Strigachev, Rumen S. Bachev, Jianghe Yang
Figure caption: The distribution of ﹩\mathrm{log}{d}_{\mathrm{em}}﹩.
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: Total transmission curves of relevant HSC filters based on the area-weighted mean measurements, including the transmission of the atmosphere, the prime focus unit, and the dewer window; the primary mirror reflectivity; average CCD quantum efficiency; and the effect of vignetting. Colored thick curves show the transmission of NB filters, from left to right: NB387, NB527, NB718, NB816, NB921, NB973, and NB1010. Black curves show the transmission of HSC broadband filters, from left to right: g, r2, i2, z, and y. Note that the r- and i-band filters were replaced with the new r2 and i2 filters in 2016, but hereafter we simply refer to them as r and i bands.
Paper: Characterizing the Emission Region Properties of Blazars
Authors: Junhui Fan, Hubing Xiao, Wenxin Yang, Lixia Zhang, Anton A. Strigachev, Rumen S. Bachev, Jianghe Yang
Figure caption: The distribution of ﹩\tan \phi ﹩.
Paper: Characterizing the Emission Region Properties of Blazars
Authors: Junhui Fan, Hubing Xiao, Wenxin Yang, Lixia Zhang, Anton A. Strigachev, Rumen S. Bachev, Jianghe Yang
Figure caption: The distributions of ﹩\mathrm{log}{U}_{{\rm{e}}}﹩ and ﹩\mathrm{log}({U}_{{\rm{e}}}/{U}_{{\rm{B}}})﹩.
Paper: Characterizing the Emission Region Properties of Blazars
Authors: Junhui Fan, Hubing Xiao, Wenxin Yang, Lixia Zhang, Anton A. Strigachev, Rumen S. Bachev, Jianghe Yang
Figure caption: The comparison of ﹩\mathrm{log}{d}_{\mathrm{em}}﹩ from this work and from Ghisellini & Tavecchio (2015).
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: Integrated exposure times T exp for all merged event files reduced in our analysis. The black histogram refers to radio sources having an X-ray-detected counterpart while the red one represents those for which no X-ray source is spatially coincident with the radio core. A total of 624 observations were retrieved from the Swift-XRT archive and analyzed to investigate the X-ray emission of 89 G4Jy-3CRE radio sources. The two dashed vertical lines mark the thresholds of 5 ks and 12 ks, respectively. We found an X-ray counterpart for all radio sources with integrated T exp larger than ∼12 ks and for 85% of the sample (i.e., 35 out of 41) observed for more than 5 ks.
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: Radio maps for G4Jy 1518 retrieved from the TGSS, NVSS, and VLASS archives (left to right panels) at 150 MHz, 1.4 GHz, and 3 GHz, respectively. The frequency of the radio map from which contours were drawn is reported together with the intensity of the first level. All radio contours increase in level by a binning factor as indicated. The radio morphology of G4Jy 1518 shows a classical double-double radio structure similar to “restarted” radio galaxies.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Model IR emission spectra of neutral aliphatic PAHs of N H,ali = 0, 2, 6, 10 aliphatic H atoms and N C,aro = 24 aromatic C atoms illuminated by an M2V star of T eff = 3500 K (orange lines), a solar-type star of T eff = 6000 K (purple lines), an A2V star of T eff = 10,000 K (magenta lines), a B1.5V star of T eff = 22,000 K (blue lines), a B0V star of T eff = 30,000 K (cyan lines), and the MMP83 ISRF (black lines). The starlight intensities are all set to be U = 1. The 3.4 and 6.85 μm aliphatic C–H features are clearly seen in the spectra of aliphatic PAHs with N H,ali = 2, 6, 10, while the 7.25 μm aliphatic C–H feature is less prominent. For clarity, their spectra are vertically shifted.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Model-calculated intensity ratios ﹩{\left({I}_{3.4}/{I}_{3.3}\right)}_{\mathrm{mod}}﹩ as a function of N H,ali/N H,aro for neutral aliphatic PAHs of N C,aro = 24. These molecules are illuminated by an M2V star of T eff = 3500  K (orange lines), a solar-type star of T eff = 6000  K (purple lines), an A2V star of T eff = 10,000 K (magenta lines), a B1.5V star of T eff = 22,000 K (blue lines), a B0V star of T eff = 30,000 K (cyan lines), and the MMP83 ISRF (black lines). The starlight intensities are all set to be U = 1.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: The aromatic and aliphatic C–H stretches at ∼3.3 and 3.4 μm, respectively, from SPT0418-47, a galaxy at z ≈ 4.22, detected by JWST/MIRI (Spilker et al. 2023). The MIRI spectrum has been smoothed to a resolution of R ≈ 600. Also shown is the JWST/NIRCam spectrum of GOODS-S 9883, a moderately distant galaxy at z ∼ 0.36 (J. W. Lyu et al. 2023, in preparation). To facilitate comparison, the JWST/NIRCam spectrum has been multiplied by a factor of 3.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figures 2 and 3 but highlighting the aromatic and aliphatic C–H bands in the 3.2–3.6 μm wavelength range.
Paper: Aliphatics and Aromatics in the Universe: The Pre-JWST Era
Authors: X. J. Yang, Aigen Li
Figure caption: Same as Figure 2 but for aliphatic PAH cations.
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: Spatiotemporal distributions (colored plus signs) of the central reversal of the Si IV, C II, and Mg II h line profiles at the southern part of the flare region overplotted on the Doppler velocity maps. The relative depth (R  d ) is indicated in the color bar. The contours indicate the flare regions with levels of (2%, 18%), (3%, 11%), and (18%, 35%) of the peak total intensities for the Si IV, C II, and Mg II h lines, respectively, with the black contour marking the main ribbon. The colored diamonds indicate the selected positions and time steps for the line profiles as shown in Figure 5. There is an intensity threshold of 15 DN for the Si IV and C II lines.
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 4. Different colors represent different time steps. (j)–(l) Si IV line profiles (black) at the three selected positions when the Doppler velocity is relatively larger for the selected time steps. For the Si IV line profile at the first position, we use a single-Gaussian fitting (red) to obtain the Doppler velocity (V  s ). For the other two profiles, the bisector method is applied to derive the Doppler velocity (V  b ). The velocities by using different methods (including the one by the moment method, V  m ) are given in the panels. Note that V  b  is the velocity at the 20% level of the peak intensity. The vertical dashed line in each of the panels denotes the reference wavelength of the spectral line.
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: Spatiotemporal distributions (colored plus signs) of the central reversal of the Si IV, C II, and Mg II k line profiles at the southern part of the flare region overplotted on the Doppler velocity maps. The relative depth (R  d ) is indicated in the color bar. The contours indicate the flare regions with levels of (2%, 18%), (3%, 11%), and (18%, 35%) of the peak total intensities for the Si IV, C II, and Mg II k lines, respectively, with the black contour denoting the main ribbon. The colored diamonds mark the selected positions and time steps for the line profiles as shown in Figure 9. There is an intensity threshold of 5 DN for the three lines.
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 8. Different colors represent different time steps. (j)–(l) Si IV line profiles (black) at the three selected positions when the Doppler velocity is the largest among the selected time steps. For the Si IV profile at the first position, we use a single-Gaussian fitting (red) to obtain the Doppler velocity (V  s ). For the other two profiles, the double-Gaussian fitting (red) is applied to derive the Doppler velocities for different components (V 1 and V 2, in magenta and orange, respectively). The velocities by using different methods (including the one by the moment method, V  m ) are given in the panels. The vertical dashed line in each of the panels denotes the reference wavelength of the spectral line.
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: Spatiotemporal distributions (colored plus signs) of the central reversal of the Si IV, C II, and Mg II k line profiles at the southern part of the flare region overplotted on the Doppler velocity maps. The relative depth (R  d ) is indicated in the color bar. The contours indicate the flare regions with levels of (2%, 18%), (3%, 11%), and (18%, 35%) of the peak total intensities for the Si IV, C II, and Mg II k lines, respectively, with the black contour marking the main ribbon. The colored diamonds indicate the selected positions and time steps for the line profiles as shown in Figure 13. There is an intensity threshold of 5 DN for the Si IV and C II lines.
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: Observation overview of the M1.5 flare on 2022 January 18. (a) GOES 1–8 Å flux and SJI 2796 Å flux (integrated over the flare region as shown in panel (d)). (b) STIX fluxes at different energy bands. The vertical magenta dotted lines in panels (a) and (b) indicate the start, peak, and end times of the flare. (c)–(e) HMI LOS magnetogram, SJI 2796 Å, and AIA 94 Å images around the flare peak time. The red contours mark the flare ribbons as seen in the SJI 2796 Å image with a level of 40% of the maximum intensity. The vertical yellow dashed line indicates the IRIS slit position. (f)–(h) The spectra of Mg II k, C II, and Si IV along the slit at 17:44:01 UT (i.e., the flare peak time). The olive dashed lines mark the reference wavelengths of these spectral lines.
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: Observation overview of the C1.6 flare on 2015 December 19. (a) GOES 1–8 Å flux and SJI 2796 Å flux (integrated over the flare region as shown in panel (d)). (b) RHESSI fluxes at different energy bands. The vertical magenta dotted lines in panels (a) and (b) indicate the start, peak, and end times of the flare. (c)–(e) HMI LOS magnetogram, SJI 2796 Å, and AIA 94 Å images around the flare peak time. The red contours mark the flare ribbons as seen in the SJI 2796 Å image with a level of 15% of the maximum intensity. The vertical yellow dashed line indicates the IRIS slit position. (f)–(i) The spectra of Mg II k, C II, Si IV, and Fe XXI along the slit at 10:46:20 UT. The olive dashed lines mark the reference wavelengths of these spectral lines.
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: Spatiotemporal variations of the total intensity (in units of log(DN)), Doppler velocity (kilometers per second), and line width (kilometers per second) of the Si IV and Mg II k lines along the IRIS slit obtained from the moment analysis. The contours indicate the flare regions with levels of (2%, 18%) and (18%, 35%) of the peak total intensities for the Si IV and Mg II k lines, respectively, with the black contour marking the main ribbon. Note that for these two lines, we set an intensity threshold of 5 DN for a reliable S/N.
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: Spatiotemporal variations of the total intensity (in units of log(DN)), Doppler velocity (kilometers per second), and line width (kilometers per second) of the Si IV and Mg II k lines along the slit obtained from the moment analysis. The contours indicate the flare regions with levels of (2%, 18%) and (18%, 35%) of the peak total intensities for the Si IV and Mg II k lines, respectively, with the black contour marking the main ribbon. Note that for the Si IV line we set an intensity threshold of 5 DN for a reliable S/N.
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. The first panel represents the result for the calibration. Blue and orange points are Tycho-2 and GSPC data points, respectively. Outliers for the fitting are marked with a red square. The two vertical dashed lines mark the range of Tycho-2 data points used for the fitting procedure. The lower horizontal dashed line represents the COI saturation limit at a zero background, while the upper horizontal dashed line is for the readout streak method. For sources brighter than this value, the uncertainty derived with the readout streak method is comparable to or smaller than the typical value ∼20% of the PSF method. The horizontal dotted line marks the lower limit for GSPC data points, for which the theoretical residual of this dotted line is shown in the second panel to illustrate that the strange shape of the GSPC residuals is not induced by any physical reasons. The gray region represents 1, 2, and 3 times the rms of residuals, which is also shown in the second panel. For the V band, measurements of GRB 080319B, labeled with black points, are plotted but not fitted. Fitting residuals are shown in the second panel, where outliers are not plotted for clarity. The third panel represents the weighted bright residual distribution. The vertical axis represents the fraction of sources brighter than the fitted model weighted by reciprocals of uncertainties of data points. The domination of bright residuals at low count rate is due to the lower limit in photometries of Tycho-2 sources. While for the high count rate, the wing is strongly influenced by the coincidence loss. The last panel represents the systematic uncertainty for the PSF method. Solid, dashed, and dotted lines represent the 1σ, 2σ, and 3σ uncertainties for each bin, respectively. The dotted–dashed line is the mean value of the 1σ uncertainties; please see Table 1 for exact values.
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: Color transformation from the Johnson–Kron–Cousin system to the UVOT system. From left to right, the three panels show color transformation of the V, B, and U bands, respectively. Since the main peaks of the V and B bands of the Johnson–Kron–Cousins system and UVOT system are very close (see Figure 4), B UVOT − B JKC and V UVOT − V JKC are very close to 0, i.e., <0.06 mag, as is shown. For the U band, the difference between the two systems reaches a maximum of ∼0.25 mag. Note that in this figure, color terms are under Vega system, and AB magnitudes of Vega in the UVOT V, B, and U bands are −0.01, −0.13, and 1.02 mag, respectively. M-type stars are not plotted in this figure, due to their large scatter.
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: An example for measurement of the wing. This figure is generated by the algorithm to measure the count rate of the wing. The two panels in the top row are the normalized sky image and the statistical information for the background. The four panels in the middle row, from left to right, are the magnified image of the source, the fitted model for the wing, the residual image for the wing, and the bad pixel map created with the sigma-clipping method, with a threshold of 5. Some true background pixels are clearly marked as bad pixels, and they should be removed from the bad pixel map to avoid their influence on the generation of the mask for the wing. For the bottom row, four panels from left to right are the smoothed bad pixel map, the clean bad pixel map, the mask for the wing, and the masked magnified image of the wing. Please note that the mask for sources in the wing should be composed with sector annuli instead of source shapes, or Equation (2) is wrong.
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 light curve of GRB 080319B in the V band. The black solid line represents RAPTOR-T measurements (taken from Woźniak et al. 2009). The red dashed line shows measurements obtained with UVOT FTOOLS uvotsource. The uncertainties of measurements of RAPTOR-T and uvotsource are not plotted for clarity (they are compared with other points), as they are very small <0.07 mag. Black points show the photometries restored by the PSF method with the same time bins of Woźniak et al. (2009). Blue points show restored photometries by the readout streak method (Page et al. 2013), and photometries restored by the PSF method with same time bins of Page et al. (2013) are plotted with orange points (for clarity, time uncertainties of blue points are not plotted since they are the same as those of the orange points).
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 flow chart for the procedures described in Section 3.3. A simple summary: (1) The UVOT observation list is crossmatched with the reference catalog with a search radius of 12′. (2) Each extension of PP images is checked with the corresponding matched star, because the pointing coordinate and the field of view of each extension could be different, though the extensions are in one exposure sequence. (3) Measure the count rate of the wing for each star that passed all selection criteria.
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. Please refer to the caption of Figure 9 for the meaning of all notations, except for the dashed line in the first panel, which represents the COI saturation limit of UVOT.
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. 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: An illustration of the uncertainty weighted residual distribution for the V-band event 1 × 1 data set. The GSPC data will have a higher weight than the Tycho-2 data. With the scaling factor, GSPC and Tycho-2 have an approximate influence on the fitting for the calibration of zero-points.
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 spatial distribution of calibration sources in the V-band event 1 × 1 data set. This figure shows the detector position of each sources used for the calibration of ﹩{\mathrm{ZP}}_{\mathrm{wing},\mathrm{evt}1\times 1}^{\mathrm{AB},V}﹩. Points with darker colors are the result that several individual points coincides with each other.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Illustration of the KMTNet/SEP field observed in the BVRI bands. Each red box corresponds to an FOV of ∼2° ×  2°, and the entire area covered by 7 × 7 patches is ∼14.5 × 14.5 deg2. The dotted red boxes indicate areas excluded from this study due to the poor quality of the B- and R-band data. The blue boxes represent the nine subfields of 1° ×  1° used for standardization and background estimation.
Paper: Photometric Selection of Unobscured QSOs at the Ecliptic Poles: KMTNet in the South Field and Pan-STARRS in the North Field
Authors: Woowon Byun, Minjin Kim, Yun-Kyeong Sheen, Dongseob Lee, Luis C. Ho, Jongwan Ko, Kwang-Il Seon, Hyunjin Shim, Dohyeong Kim, Yongjung Kim, Joon Hyeop Lee, Hyunjin Jeong, Jong-Hak Woo, Woong-Seob Jeong, Byeong-Gon Park, Sang Chul Kim, Yongseok Lee, Sang-Mok Cha, Hyunmi Song, Donghoon Son, Yujin Yang
Figure caption: Histograms of magnitudes of all the detected sources (blue) and pointlike sources with a stellarity index higher than 0.9 (red). The shaded regions represent saturated magnitudes, and the dashed vertical lines represent the 5σ detection limit for point sources.