adsabs/AstroCLIMB huggingface dataset:
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 10955 and its associated solar wind. The full-disk image taken by EIT 195 Å and the subregion map inside the rectangle (outline of the region scanned by the EIS) are presented in (a) and (b), the photospheric magnetic field measured by MDI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 10955 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of the open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Magnetic Field Structure, Doppler Shift, and Intensity of Active Regions and Their Connections with the Solar Wind
Authors: Chi Ma, Hui Fu, Zhenghua Huang, Lidong Xia, Jinmei Zheng, Xinzheng Shi, Bo Li
Figure caption: Remote sensing of AR 10938 and its associated solar wind. The full-disk image taken by EIT 195 Å and the subregion map inside the rectangle (outline of the region scanned by EIS) are presented in (a) and (b), the photospheric magnetic field measured by MDI is given in (c), the EIS Fe XII 195.12 Å intensity and Doppler maps of AR 10938 are shown in panels (d) and (e), the parameters of the solar wind are shown in (f). The red and blue crosses represent the footpoints of open magnetic field lines derived from the PFSS model. The sky-blue lines contour the magnetically concentrated area and the red lines outline the footpoint areas of blueshift.
Paper: Genesis and Coronal-jet-generating Eruption of a Solar Minifilament Captured by IRIS Slit-raster Spectra
Authors: Navdeep K. Panesar, Sanjiv K. Tiwari, Ronald L. Moore, Alphonse C. Sterling, Bart De Pontieu
Figure caption: Thermal and dynamical properties of the minifilament eruption. Panels (a) and (e), (b) and (f), and (c) and (g) show the maps of temperature, LOS velocity (V LOS), and electron density (log(n  e )), respectively, evaluated at log(τ) = −5.0. Panels (d) and (h) show the spectroheliograms of the Mg II k line at 2796.38 Å. The black and white arrows in (a)–(c) point to the JBP. In panel (f) the upper black arrow points to the weak redshifts and the lower arrow points to the blueshifts along the jet spire; these Doppler shifts confirm the Doppler shift evidence in Figure 6(f) for clockwise spin of the spire.
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: Simulated altitude profiles for the densities of ions and electrons (left column), neutral (T  n ), ion (T  i ), and electron (T  e ) temperatures (middle column), and magnetic field (right column) for a solar zenith angle of 60° at Earth, Venus, and Mars. Panel (c) represents the Earth’s internal magnetic fields, and Panels (f, i) show the induced magnetic fields with evolution times of 0, 2, and 4 hr at Venus and Mars, respectively. The gray triangles in panel (d) show the measured electron density in the interval 65° ± 5° by the PV (Pioneer Venus) ORPA (Orbiter Retarding Potential Analyzer) instrument (after Miller et al. 1984). The orange squares and green triangles in panel (e) display the measured ion and electron temperatures by the PV ORPA and OETP (Orbiter Electron Temperature Probe) instruments, respectively (after Cravens et al. 1980). The orange squares, red circles, blue stars and gray triangles in panel (g) are the measured densities of ﹩{{\rm{O}}}_{2}^{+},{\mathrm{CO}}_{2}^{+},{{\rm{O}}}^{+}﹩ and electrons by the MAVEN (Mars Atmosphere and Volatile EvolutioN) NGIMS (Neutral Gas and Ion Mass Spectrometer) and LPW (Langmuir Probes and Waves) instruments, respectively (after Fox et al. 2021). The olive squares, cyan circles, and dark triangles in panel (h) represent the measured electron temperatures by the LPW and NGIMS (after Flynn et al. 2017; Fox et al. 2021).
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: (a, c, e) The relative changes (ratio) in electron density between simulations with and without flares, at Earth, Venus, and Mars, respectively. The vertical lines indicate the onset of two flares. (b, d, f) Altitudinal variations of the corresponding relative changes at the time of the X9.3 flare peak (12:02 UT). Note that for the right panels the relative changes larger than 1.25 are shown in the bottom X-axis (blue), otherwise in the top one (orange) for better visualization.
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: Flare-induced absolute changes in electron (left) and ion (right) temperatures at Earth, Venus, and Mars. The vertical lines indicate the onset of two flares.
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: The changes of vertical plasma velocity between simulations with and without flares at Earth, Venus, and Mars. The vertical lines indicate the onset of two flares.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Euler rotations for 3D orbital model: (a) initial coordinate frame, (b) rotation accounting for argument of pericenter, (c) rotation accounting for orbital inclination, and (d) rotation accounting for R.A. of ascending node.
Paper: A Comparative Study of Ionospheric Response to Solar Flares at Earth, Venus, and Mars
Authors: Maodong Yan, Tong Dang, Yu-Tian Cao, Jun Cui, Binzheng Zhang, Zerui Liu, Jiuhou Lei
Figure caption: Solar X-ray irradiance in the 0.1–0.8 nm band as measured by the GOES-15 satellite for the event of 2017 September 6.
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Histogram of the ratio of the emission frequencies calculated using the magnetic moment scaling laws given by Stevenson (1983) (S83) and Mizutani et al. (1992) (M92).
Paper: Detecting Magnetospheric Radio Emission from Giant Exoplanets
Authors: Reza Ashtari, Anthony Sciola, Jake D. Turner, Kevin Stevenson
Figure caption: Illustration of 3D orbital model.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The VUO-old (1994–2007) V light curves (open circles; Hrivnak et al. 2010) plotted together with the VUO-new (2008–2018) V light curves from this study (filled circles). In addition to seasonal variations, they allow us to see longer-term trends in the light curves.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The differential color curves for the target objects based on our new VUO data: Δ(V−R  C ) vs. ΔV. There exists a clear trend of the stars appearing redder when fainter.
Paper: Variability in Protoplanetary Nebulae. IX. Evidence for Evolution in a Decade
Authors: Bruce J. Hrivnak, Wenxian Lu, William C. Bakke, Peyton J. Grimm
Figure caption: The differential VUO V light curves from 2008−2018 for nine of the program objects. The uncertainties in the data are small, ± 0.005–0.010 mag. Note that there are large differences among the brightness ranges of the objects (e.g., IRAS 05113+1347 and 05341+0852).
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: An overview of the Sgr E region. The red shows the 870 μm 12CO (J = 3–2) emission integrated over the entire line-of-sight velocity range of ±300 km s−1 (CHIMPS2; Eden et al. 2020), the green shows 70 μm (Herschel Hi-GAL; Molinari et al. 2010), and the blue shows 8 μm (Spitzer GLIMPSE; Benjamin et al. 2003). The white circle is the field of view of the ALMA observation.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Spatially masked moment 0 maps generated from data in the velocity range of −197 km s−1 to −231 km s−1 for 12CO (top), 13CO (middle), and C18O (bottom). In the 12CO image, the orange line represents the filament 1 p–v slice path, while the blue line represents the filament 2 p–v slice path. For each image, the beam is indicated in the lower right corner.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Integrated intensity (moment 0) maps from the 13CO data cube. Each image shows the integrated intensity over a range of 5 km s−1. The specific velocity ranges are indicated above each image. The top—orange—contour indicates the region that we define for filament 1, while the bottom—blue—contour indicates the filament 2 region. The beam is indicated in the lower right corner of each channel map.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: The filament 2 p–v diagrams for 12CO (top), 13CO (middle), and C18O (bottom), respectively. The p − v slice starts at the end of the filament that is closer to the Galactic center, so the offset represents the distance along the p − v slice as we move from left to right along the filament 2 spine (see Figure 5).
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: The filament 1 p–v diagrams for 12CO (top), 13CO (middle), and C18O (bottom), respectively. The p − v slice starts at the end of the filament that is closer to the Galactic center, so the offset represents the distance along the p − v slice as we move from left to right along the filament 1 spine (see Figure 5).
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Velocity profiles generated from the C18O p − v diagrams (see Figures 8 and 9). Top left: the profile for velocity component 1A, centered at approximately −223 km s−1. Top right: the profile for velocity component 1B, centered at approximately −208 km s−1. Bottom left: the velocity profile for velocity component 2A, centered at approximately −220 km s−1. Bottom right: the profile for velocity component 2B, centered at approximately −203 km s−1. The blue lines in each figure are the Gaussian fits for each velocity profile, made using a fitting distance of 1.3 km s−1 from the central velocity. The FWHM velocity line widths for each velocity component are reported in Table 3.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: The full-resolution velocity channel maps for the spectral line 13CO used to identify filaments 1 and 2, with channel widths of ∼0.3 km s−1. The channel maps on the top row span the velocity range of −222.0 km s−1 to −224.0 km s−1. The channel maps on the bottom row span the velocity range of −202.0 km s−1 to −204.0 km s−1. In each image, the top—orange—contour indicates the region that we define for filament 1, while the bottom—blue—contour indicates the filament 2 region. The beam is indicated in the lower right corner of each channel map.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: An overview of the inner Galaxy in l–v space, as seen in the 12CO (J = 3–2) emission (CHIMPS2; Eden et al. 2020). The black box indicates the longitude range of the CMZ (l = 2° to −1.°1). The blue box represents the line-of-sight velocity range (−170 km s−1 > v LOS > −220 km s−1) and the longitude range (−0.°7 > l > −1.°7) of the Sgr E region. The red circle represents the (l,v) coordinate of the H II region, which our data is centered on.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Spatially masked moment 1 maps generated from data subcubes in the velocity range of −197 km s−1 to −231 km s−1 for 12CO, 13CO, and C18O, respectively. In the 12CO image, the black contours indicate the filament 1 and filament 2 regions. For each image, the beam is indicated in the lower right corner.
Paper: ALMA Uncovers Highly Filamentary Structure toward the Sgr E Region
Authors: J. Wallace, C. Battersby, E. A. C. Mills, J. D. Henshaw, M. C. Sormani, A. Ginsburg, A. T. Barnes, H. P. Hatchfield, S. C. O. Glover, L. D. Anderson
Figure caption: Top: the brightness temperature profile for filament 1, taken from the −223.0 km s−1 C18O channel image. Bottom: the brightness temperature profile for filament 2, taken from the −203 km s−1 C18O channel image. The blue lines plotted in both figures are the Gaussian fits for each filament profile, made using a fitting distance of 0.05 pc from the center of the filament. The radial distance is the distance from the center of the filament.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Left panel: UV–optical flux offset for each CLASSY galaxy, obtained from the comparison of extended-UV stellar-continuum fitting and optical stellar-continuum fitting of SDSS (blue circles), MUSE (red triangles), KCWI (gold pentagon), VIMOS (purple square), LBT (green hexagons), and MMT (gray diamond) data. Right panel: UV–optical flux offset as a function of the average half-light radius (r 50) taken from Paper I and calculated from Pan-STARRS imaging. The solid magenta horizontal lines are centered at the ratio of the COS/SDSS aperture (i.e., (2.″5/3″)2), while the dashed–dotted blue, dotted red, and dashed green horizontal lines show the median UV–optical flux offsets for the SDSS, MUSE, and LBT spectra, respectively. The uncertainties are shown for all the displayed quantities.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Upper panels: COS, SDSS, and MUSE spectra of galaxy J0021+0052. The COS spectrum is shown with a black solid line, while the original SDSS and MUSE optical spectra with a dotted gray and black line, respectively. The UV–optical flux offset is estimated comparing the UV-extended stellar-continuum fitting (dashed blue line) and optical stellar-continuum fitting (dashed red line for SDSS and magenta for MUSE) in several featureless wavelength ranges of 40 Å between 4000 and 5600 Å, highlighted in cyan. The UV–optical flux offset corrected spectra are shown from the green and orange solid lines, for SDSS and MUSE, respectively. The bottom panel shows a zoom on the optical region of the spectra. Lower panels: same for galaxy J1144+4012.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Fit of the N IV] λλ1483,87 emission-line doublet, with one of the lines detected with a S/N > 3 in 6 out of 44 galaxies. The observed flux and the best-fit model are shown in black and red, respectively, while their uncertainties are given by the gray and red shades. The black dashed vertical lines indicate the line positions, taking z lit. into account.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Same as Figure 19 for [O III] λλ1661,6 emission line in the CLASSY survey detected with a S/N > 3 in 22 out of 44 galaxies.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Same as Figure 19 for the He II λ1640 emission line in emission, detected with a S/N > 3 in 19 out of 44 galaxies.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Same as Figure 19 for the Si III] λλ1883,92 doublet, with one of the lines detected with a S/N > 3 in 6 out of 44 galaxies.
Paper: CLASSY IV. Exploring UV Diagnostics of the Interstellar Medium in Local High-z Analogs at the Dawn of the JWST Era 
Authors: Matilde Mingozzi, Bethan L. James, Karla Z. Arellano-Córdova, Danielle A. Berg, Peter Senchyna, John Chisholm, Jarle Brinchmann, Alessandra Aloisi, Ricardo O. Amorín, Stéphane Charlot, Anna Feltre, Matthew Hayes, Timothy Heckman, Alaina Henry, Svea Hernandez, Nimisha Kumari, Claus Leitherer, Mario Llerena, Crystal L. Martin, Themiya Nanayakkara, Swara Ravindranath, Evan D. Skillman, Yuma Sugahara, Aida Wofford, Xinfeng Xu
Figure caption: Same as Figure 19 for the [N III] λ1750 multiplet in the CLASSY survey detected with a S/N > 3 in 2 out of 44 galaxies.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Optical spectra of PKS 1222+216 from SO SPOL observations. Observed and de-reddened (Cardelli et al. 1989) mean spectra are plotted as dashed–dotted red and solid blue lines, respectively, along with the de-reddened spectra at high- (black solid line) and low-flux (solid gray line) states. The prominent emission lines, Hβ (λ rest = 4861.3 Å), Hγ (λ rest = 4340.48 Å), Hδ (λ rest = 4101.75 Å), and Mg II (λ rest = 2795.50 and 2802.7 Å), in the observed frame are also identified in the plot. The shaded region shows the spectral region local to Hγ emission line that we used for the analysis.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Best-fit parameters from the analysis of the optical spectral region (6024–6452 Å) local to Hγ line using the models powerlaw and Gaussian. The left panels show the power-law properties such as the continuum flux (F C,opt) in the 6024–6092 Å and 6380–6452 Å wave bands (observer’s frame), spectral index (α) and amplitude (ampl) of the model. The right panels give the emission line properties of Hγ, say, line flux (F Hγ ), FWHM, best-fit central wavelength (λ pos), and the equivalent width (EW) of the emission line.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Light curves of Hγ emission line flux (upper), optical continuum fluxes for two wavelength regions (red: 6024–6092 Å and blue: 6380–6452 Å; middle), and γ-ray flux (Fermi-LAT: 3σ detection; lower). Different markers for the optical light curves (upper and middle panels) represent various cycles used in the analysis. The error bars for the optical continuum flux values are smaller than the size of the markers, hence are not visible in the plot.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Variation in the Hγ flux (left), the equivalent width (middle), and the flux density ratio between 5044 and 6064 Å (right) with the narrowband optical continuum flux.
Paper: Long-term Optical and γ-Ray Variability of the Blazar PKS 1222+216
Authors: Savithri H. Ezhikode, Amit Shukla, Gulab C. Dewangan, Pramod K. Pawar, Sushmita Agarwal, Blesson Mathew, Akhil Krishna R.
Figure caption: Spectral fitting plots of local continuum and Hγ line emission with powerlaw and Gaussian (after ignoring the region of atmospheric absorption feature) at high- (left) and low-optical-flux (right) states. The upper panel in each plot shows the de-reddened spectrum and the best-fit model. The lower panels show the residuals associated with the spectral fits.