adsabs/AstroCLIMB huggingface dataset:
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Summary of the 34 line ratio ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ radial profiles in our sample. Absolute values of ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ are shown in the left panel, the middle panel shows the ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ normalized by each galaxy’s global line ratio ﹩{{ \mathcal R }}_{12/13}^{\mathrm{gal}}﹩, and the right panel shows ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ divided by ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ at the central radial bin (﹩{{ \mathcal R }}_{12/13}^{0}﹩). Interacting galaxies are shown in red star symbols, and barred, noninteracting galaxies are shown in green crosses. The other unbarred, noninteracting galaxies are shown in blue lines. Within a noninteracting, unbarred galaxy, ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ are fairly constant as a function of radius, with a possible tendency toward a slight increase beyond 0.2–0.3r 25;  outliers from the general trend are exclusively found in barred or interacting galaxies.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Integrated line ratio ﹩{{ \mathcal R }}_{12/13}^{\mathrm{gal}}﹩ as functions of global galaxy parameters for the 105 galaxies in which F 12 is detected with S/N > 3. Blue symbols show the isolated galaxies and the red symbols show the interacting galaxies. The circles with error bars show the ﹩{{ \mathcal R }}_{12/13}^{\mathrm{gal}}﹩ and its uncertainty for the 41 galaxies with F 13 detected with S/N > 4. The lower limits of ﹩{{ \mathcal R }}_{12/13}^{\mathrm{gal}}﹩ of the other 64 galaxies with F 12 detected but F 13 below the detection limits are shown as triangles. The Spearman rank correlation test results are shown in Table 3.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption:  13CO emissions, measured on individual grids (left panel), radial annulus (middle), and the entire galaxy (right panel), as functions of their 12CO counterparts. The blue dots show the 13CO detections with S/N > 4 in the noninteracting galaxies, while the red ones are those in the interacting galaxies. The blue and red solid lines show the median ﹩{{ \mathcal R }}_{12/13}﹩ of the noninteracting and interacting galaxies, with shaded regions showing the first and third quartiles of the corresponding measurements. Constant ﹩{{ \mathcal R }}_{12/13}﹩ values of [4, 8, 16, 32] are shown as gray dotted lines in each panel. The typical detection limits of the resolved I 13 and I 12 are shown as horizontal and vertical solid lines, respectively, in the left and middle panels. Note in the middle panel, the azimuthally stacked ﹩{I}_{13}^{\mathrm{stack}}﹩ approaches ranges well below this limit. All three types of measurements are closely distributed around constant values of ﹩{{ \mathcal R }}_{12/13}﹩.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption:  13CO intensity maps of the 30 galaxies with resolved 13CO detected from the EDGE survey. The black contours overlaid show the 13CO intensity observed with S/N > 4, while the white contours levels show the 12CO intensity with S/N > 3. The black circles in the first panel of each row show the beam size. We use a single color palette for all the galaxies, and the color scale is adjusted to emphasize the 13CO emission.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption:  13CO flux spectra for the 41 galaxies with F 13 detected. The blue lines show the 13CO flux in each channel obtained using the dilated 12CO masks, and the red lines are the 12CO flux resulting from the same masks scaled down by a factor of 8. The light-blue-shaded regions represent the 1σ uncertainty of the 13CO flux.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 1, but for WASP-136 b, WASP-166 b, WASP-178 b, and WASP-189 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Corner plot showing the posterior distribution of the directly estimated transit parameters from the MCMC sampling for KELT-3 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 7, but for WASP-18 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 1, but for KELT-17 b, KELT-19 A b, KELT-20 b, KELT-24 b, and HAT-P-1 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 1, but for HAT-P-2 b, HAT-P-11 b, HAT-P-22 b, HAT-P-69 b, and HAT-P-70 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 1, but for MASCARA-4 b, XO-3 b, WASP-7 b, WASP-8 b, and WASP-14 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 1, but for WASP-18 b, WASP-33 b, WASP-69 b, WASP-76 b, and WASP-99 b.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Same as Figure 7, but for KELT-20 b.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Azimuthally stacked line ratio ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ as functions of azimuthally averaged properties in the 41 galaxies from our sample. The explanations of the x-axis labels and the Spearman rank correlation test results are shown in Table 4. In panels (h), (i), (j), and (l), we exclude the radius bin if it contains less than 50% of the grids identified as star-forming regions with the BPT diagnostics. The filled circles show the individual azimuthally averaged ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ measurements for annuli with stacked 13CO detected with S/N > 4 in noninteracting (blue) and interacting (red) galaxies. The lower limits of ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ for annuli with stacked 13CO undetected are shown in triangles.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Stacked line ratio ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ vs. azimuthally averaged SFR (left) and sSFR (right) surface density in galaxy centers (within 0.2r 25). The labels and colors are the same as in Figure 6. In the left panel, the dashed line shows the empirical relation derived by Davis (2014). In the right panel, the solid line is the fitting based on our sample, and the dotted line shows the fitting by Morokuma-Matsui et al. (2020). The Spearman rank coefficients are shown in black and blue at the bottom for all the galaxies and for noninteracting galaxies, respectively.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Azimuthally averaged ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ profiles of the 41 galaxies with ﹩{I}_{13}^{\mathrm{stack}}﹩ detected with S/N >4 in our sample. The galactocentric radius for each galaxy is normalized to its r 25. Spectra of 13CO and 12CO are shifted and stacked at each normalized radius bin to derive ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩. Interacting galaxies are highlighted with star symbols. Cross symbols show the noninteracting galaxies with bars, and filled circles show the other noninteracting galaxies. The lower limit of ﹩{{ \mathcal R }}_{12/13}^{\mathrm{stack}}﹩ in the bins with ﹩{I}_{13}^{\mathrm{stack}}﹩ below the detection threshold of 4 is shown in triangles. We are able to detect stacked 13CO out to a radius of ∼0.4r 25 in most galaxies.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Resolved line ratio ﹩{{ \mathcal R }}_{12/13}﹩ as functions of local parameters for regions where I 13 is detected with S/N > 4. The Spearman rank correlation test results are shown in Table 6. The gray line in panel (a) corresponds to the upper boundary of our ﹩{{ \mathcal R }}_{12/13}﹩ measurements imposed by a constant I 13 detection of the sample (corresponding to the horizontal gray line in panel (a) of Figure 3). In panels (h), (i), (j), and (l), we exclude the grids that are identified as star-forming regions with the BPT diagnostics. The filled circles show the individual ﹩{{ \mathcal R }}_{12/13}﹩ measurements for noninteracting (blue) and interacting (red) galaxies.
Paper: Precise Transit Photometry Using TESS: Updated Physical Properties for 28 Exoplanets around Bright Stars
Authors: Suman Saha
Figure caption: Observed and best-fit model lightcurves (one transit event) for KELT-2 A b, KELT-3 b, KELT-4 A b, and KELT-11 b. For each observed transit, the three sections in each panel show (top) the unprocessed lightcurve (cyan), the lightcurve after wavelet denoising (magenta), and the best-fit transit model (blue); (middle) the residual after modeling without GP regression (magenta), and the mean (blue) and 1σ interval (cyan) of the best-fit GP regression model; (bottom) mean residual flux (blue).
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: Azimuthally stacked spectra of IC 0944 (top) and NGC 2906 (bottom). Each panel shows the results of a radial bin adjusted following the method described in Section 3.3. In the top-left corner of each panel, we show the radial bin ranges in units of r/r 25 and the number of spectra used in the stacking. The blue lines are the 13CO spectra, and the red lines are the 12CO spectra scaled down by a factor of 4. The blue vertical lines show the channel noise of the 13CO stacked spectrum. The red- and blue-shaded regions show the Gaussian-fitted integrated fluxes of 12CO and 13CO used for the stacked line ratios.
Paper: The EDGE-CALIFA Survey: Spatially Resolved 13CO(1–0) Observations and Variations in 12CO(1–0)/13CO(1–0) in Nearby Galaxies on Kiloparsec Scales
Authors: Yixian Cao, Tony Wong, Alberto D. Bolatto, Adam K. Leroy, Erik Rosolowsky, Dyas Utomo, Sebastián F. Sánchez, Jorge K. Barrera-Ballesteros, Rebecca C. Levy, Dario Colombo, Leo Blitz, Stuart N. Vogel, Johannes Puschnig, Vicente Villanueva, Monica Rubio
Figure caption: The peak signal-to-noise map of 13CO for the 30 galaxies with resolved 13CO detected from the EDGE survey. The black contours overlaid show the 13CO intensity observed with S/N > 4.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The extinction variations in the effective temperature T eff vs. colors of the SAGES for different log g with solar metallicity and comparisons of the β  n  − β  w  and α  n  − α  w  for the extinction variations. The gravity log g = 4.5 for panels (a), (b), (c), and (d), while it is log g = 2.0 for panels (e), (f), (g), and (h); panels (a), (c), (e), and (g) are for the SC system, and panels (b), (d), (f), and (e) are for SAGES.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The image of the Bok telescope in the SAGES v  s  band. The CCD mosaic is composed of four CCDs, and for each one, there are four amplifiers.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Spectra of typical F- (red), G- (blue), and K-type (green) stars from MILES overplotted with the SAGES filter passbands.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The effective temperature vs. colors for different metallicities with two given gravities of log g = 2.0 (a) and 4.5 (b).
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Metallicity vs. colors of the SC system (left panel) and SAGES (right panel) for different effective temperatures with a given gravity log g = 2.0 and 4.5.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: Gravity vs. colors of the SC system (left panel) and SAGES (right panel) for different effective temperatures with solar metallicity.
Paper: The Stellar Abundances and Galactic Evolution Survey (SAGES). I. General Description and the First Data Release (DR1)
Authors: Zhou Fan, Gang Zhao, Wei Wang, Jie Zheng, Jingkun Zhao, Chun Li, Yuqin Chen, Haibo Yuan, Haining Li, Kefeng Tan, Yihan Song, Fang Zuo, Yang Huang, Ali Luo, Ali Esamdin, Lu Ma, Bin Li, Nan Song, Frank Grupp, Haibin Zhao, Shuhrat A. Ehgamberdiev, Otabek A. Burkhonov, Guojie Feng, Chunhai Bai, Xuan Zhang, Hubiao Niu, Alisher S. Khodjaev, Bakhodir M. Khafizov, Ildar M. Asfandiyarov, Asadulla M. Shaymanov, Rivkat G. Karimov, Qudratillo Yuldashev, Hao Lu, Getu Zhaori, Renquan Hong, Longfei Hu, Yujuan Liu, Zhijian Xu
Figure caption: The sky coverage of the SAGES project covers most of the northern sky area except the Galactic plane, for which the Galactic latitude ∣b∣ > 10°, and the decl. is from −5° to +90°. The total survey area is ∼12,000 deg2.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Historical MWL light curves from the observations with different instruments. (a) XRT, (b) MAXI, (c) BAT, (d) LAT, (e) FACT, and (f)–(k) UVOT UVW2 − V bands. While the XRT, FACT, and UVOT data are derived by using the 1 day integration, the BAT, MAXI, and LAT light curves are based on data binned every 2 weeks. In panels (b)–(c), the black and gray data points correspond to the detections of the source with 5σ and 3σ–4σ significances, respectively. In panel (d), the downward gray triangles show the upper limits to the 0.3–300 GeV flux when TS < 9 and/or N pred < 8. The vertical dashed line denotes a boundary between the different time intervals listed in Table 1.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption:                         Same as Figure 1 in the subintervals of 2021–2022. Due to the strong correlation between the UVOT-band variabilities (see Section 4.1.2), only the plots from the shortest and longest wavelength bands are presented here.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: The XRT-band flares of Mrk 501 showing different profiles: fast brightening and slower decline (A), slow brightening and faster decline (B), two-peak (C), and nearly symmetric (D).
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Distribution of spectral parameter values in different time intervals (histograms and corresponding normalized cumulative distribution in the last panel of each row): curvature parameter (panel (A)), photon index at 1 keV (panel (B)), synchrotron SED peak position (panel (C)), and 0.3–10 keV photon index describing the power-law spectra (panel (D)).
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Fastest 0.3–10 keV IDVs detected at the 99.99% confidence level. The instances are arranged in order of increasing observation duration.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: 0.3–10 ke IDVs from the densely sampled XRT observations of Mrk 501.
Paper: Long-term X-Ray Outburst in the TeV-detected Blazar Mrk 501 in 2021–2022: Further Clues for the Emission and Unstable Processes
Authors: B. Kapanadze, A. Gurchumelia, M. Aller
Figure caption: Correlation between the spectral parameters and MWL fluxes. (a)–(c) Curvature parameter b plotted vs. the unabsorbed 0.3–10 keV flux, the photon index a and the position of the synchrotron SED peak E p, respectively. Parameters a and E p are plotted vs. the unabsorbed 0.3–10 keV flux in panels (d)–(e). The scatter plot E p–﹩\mathrm{log}{S}_{{\rm{p}}}﹩ is presented in panel (f). The 0.3–10 keV photon index from the power-law spectra is plotted vs. the unabsorbed 0.3–10 keV flux in panel (g); the scatter plot with the LAT-band photon index and photon flux (1-weekly integration) is presented in the last panel. The black, red, and blue points correspond to the data from Intervals 1a, 1b, and 1c, respectively.