adsabs/AstroCLIMB huggingface dataset:
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: Subsample of low-redshift galaxies with Hubble types from Nair & Abraham (2010), shown on sSFR–M * (left) and ΣSFR–M * diagrams (right). Upper panels are color-coded by the Hubble type, and lower panels by the Sérsic index (from Meert et al. 2015). Galaxies on the main sequence are mostly later types and have lower Sérsic indices. The SFR surface density provides a cleaner demarcation between early and late types than the sSFR.
Paper: ΣSFR–M ∗ Diagram: A Valuable Galaxy Evolution Diagnostic to Complement (s)SFR–M ∗ Diagrams
Authors: Samir Salim, Sandro Tacchella, Chandler Osborne, S. M. Faber, Janice C. Lee, Sara L. Ellison
Figure caption: The effects on the ΣSFR–M * relation arising from defining the SFR surface density using the effective (half-light) radius. This figure is to be compared to the right panel of Figure 2, which uses the isophotal sizes, our nominal choice. Effective-radius-based ΣSFR are significantly noisier, leading to a broader main sequence (width, in dex, given in the lower panel). The effective radius, being dependent on the galaxy light profile, is not as good an indicator of the extent over which SF is (or was) taking place as is the isophotal radius.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Median log luminosity in erg s−1 for PSFs of this sample (blue bar) and the median predicted 1.03 μm luminosity for the PSFs of the Georgiev et al. (2009) sample (red bars) at varying ages. Black lines indicate the range from minimum to maximum luminosity.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Log luminosity in erg s−1 of the central PSF components of this sample (red) and the Kimbrell et al. (2021) sample of AGN hosts (black). The PSFs in the AGN hosts are, on average, more than 2 orders of magnitude more luminous than those in the non-AGN hosts, suggesting the PSFs in the AGN hosts are dominated by AGN light.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Morphologies of the galaxies analyzed in this work (red) compared to the general population of dwarfs in the same mass range (109 < M */M ⊙ < 109.5) discussed in Reines (2022; black). This demonstrates that our sample of non-AGN-hosting dwarf galaxies provides a good representation of the general population of dwarf galaxies.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Morphologies of the galaxies analyzed in this work (red) compared to the AGN hosts analyzed in Kimbrell et al. (2021; black). The first and second options indicate a single-component galaxy best fit as a dwarf elliptical or a pure disk, respectively. The third option indicates a dwarf galaxy best fit with two Sèrsic components.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Left: UKIRT image, GALFIT model, and the residuals obtained by subtracting the GALFIT model from the image. Images are shown on a log scale, and the residuals are very stretched to show faint details. Right: surface brightness profiles. Data are black circles and the model is shown as a black line; the GALFIT components are shown as dashed lines in color. The bottom panels contain the radial residuals.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: The star used for PSF creation for galaxy UK6 (left); model PSF created using GALFIT (middle); residuals resembling random noise after subtracting the model PSF from the image of the star (right).
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: B/T ratios of the two-component galaxies in this work (red) compared to the two-component AGN hosts analyzed in Kimbrell et al. (2021; black). Dashed vertical lines indicate median values.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Inner Sèrsic indices of all two-component galaxies studied in this work (red) compared to the AGN hosts analyzed in Kimbrell et al. (2021; black).
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: UKIRT images of the eight irregular/disturbed galaxies in our sample. All images are shown on a log scale.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: Upper panels: evolution of the radiative parameter in the stellar-wind (left) and uniform-density (right) medium considering the synchrotron and expansion timescales. Lower panels show the evolution of energy radiated away (left) and the relation between the radiative parameters ϵ and s (right panel). The uniform-density and stellar-wind environments are shown in red solid and green dashed lines, respectively. The term E 0 corresponds to the initial equivalent kinetic energy. We use the values of Γ0 = 60, E 0 = 1052 erg, ε  e  = 0.5, ε  B  = 5 × 10−2, χ e = 1, and A  W  = 0.1, n = 1 cm−3.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The 4D parameter space (for the forward-shock model with k = 0) of the expected values of ε B as a function of typical values of ε e, n, and E 0,j  with two different values of p, for the cooling break of synchrotron (row 1) and SSC emission (row 2). We consider typical values in the ranges of 10−2 ≤ ε e ≤ 1, 10−3 ≤ n ≤ 1 cm−3 and 1047 ≤ E 0,j ≤ 1051 erg for p = 2.2 (columns (1) and (3)) and 2.6 (columns (2) and (4)). Columns (1) and (2) correspond to q = 0.7 and columns (3) and (4) to q = 0.3.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The panels show the CR of the synchrotron off-axis scenario in all regimes for the constant-density (above) and stellar-wind (below) environments for ϵ = 0.5 without energy injection with the spectral and temporal indexes from 2FLGC. The purple ellipses are displayed when the CRs are satisfied within 1σ error bars and lines in red and cyan colors correspond to the expected CRs.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The panels show the CRs of the synchrotron off-axis model in all regimes for the ISM (above) and wind (below) environment in the adiabatic regime with energy injection (q = 0.5) with the spectral and temporal indexes from 2FLGC. The purple ellipses are displayed when the CR are satisfied within 1σ error bars and lines in red and cyan colors correspond to the expected CRs.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The same as Figure 6, but for a wind-like scenario (k = 2) with 10−3 ≤ A W ≤ 1.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The same as Figure 2, but for the SSC off-axis scenario.
Paper: A Comparison between the Morphologies and Structures of Dwarf Galaxies with and without Active Massive Black Holes
Authors: Seth J. Kimbrell, Amy E. Reines, Jenny E. Greene, Marla Geha
Figure caption: Median log luminosity in erg s−1 for the PSFs of the Kimbrell et al. (2021; blue bar) and the median predicted 1.15 μm luminosity for the PSFs of the Jiang et al. (2011) sample (red bar). Black lines indicate the range from minimum to maximum luminosity.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The same as Figure 4, but for the SSC off-axis scenario.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The 3D parameter space of the expected values of t pk as a function of Δθ and the parameter b with two distinct values of ϵ and E 0 for k = 0 (above) and k = 2 (below). Columns (1) (ϵ = 0.8) and (2) (ϵ = 0.2) are for E 0 = 5 × 1051 erg and column (3) (ϵ = 0.8) and column (4) (ϵ = 0.2) are for E 0 = 5 × 1053 erg. We consider the parameter b in the range of 0.3 ≤ b ≤ 3 for n = 1 cm−3 and A w = 0.1.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: Upper panel: multiwavelength observations of GRB 160625B with the best-fit light curves. The light curves that describe the early observations (LAT and optical for t < 103 s) are generated with the synchrotron and SSC off-axis afterglow model, and the light curves that explain the late observations (X-ray and optical for t > 103 s) are taken from Fraija et al. (2017b). Lower panel: all the photons with energies >100 MeV and probabilities >90% of being associated with GRB 160625B. The magenta line denotes the maximum photon energy radiated by the synchrotron afterglow model.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The 3D parameter space of the expected values of t pk/t j as a function of Δθ/θ j and the parameter b with two distinct values of ϵ for k = 0 (above) and k = 2 (below). For each value of ϵ we consider the ranges of 0.3 ≤ b ≤ 1 and 1 < b ≤ 3. Columns (1) and (2) correspond to ϵ = 0.8 and columns (3) and (4) to ϵ = 0.2.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The same as Figure 8, but for two values of q. Column (1) (q = 0.8) and 2 (q = 0.2) are for E 0 = 5 × 1051 erg and column (3) (q = 0.8) and 4 (q = 0.2) are for E 0 = 5 × 1053 erg.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The corner plot displays the outcomes of our MCMC parameter estimate for the synchrotron and SSC off-axis models applied to GRB 160625B. The histograms on the diagonal display the marginalized posterior densities for each parameter and the median values are shown by red lines.
Paper: Off-axis Afterglow Closure Relations and Fermi-LAT Detected Gamma-Ray Bursts
Authors: N. Fraija, M. G. Dainotti, D. Levine, B. Betancourt Kamenetskaia, A. Galvan-Gamez
Figure caption: The same as Figure 9, but for two values of q. Columns (1) and (2) correspond to q = 0.8 and columns (3) and (4) to q = 0.2.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The contour of (a) ﹩{\tau }_{{{\rm{N}}}_{2}}/{\tau }_{\mathrm{mix}}\,=\,1﹩ and (b) ﹩{\tau }_{{\mathrm{NH}}_{3}}/{\tau }_{\mathrm{mix}}\,=\,1﹩ for assorted parameters are shown. The color bar (each value represents one metallicity contour) represents the metallicity value for the plotted quenched curve. The three sets of lines are for different values of K  zz  coefficients; solid, dashed, and dashed–dotted lines are for K  zz  = 104, 108, and 1012 cm2 s−1, respectively. In panel (b), the quenched curves of N2 are shown in faded lines with the same color and the equal-abundance curves for 0.1 × solar metallicity ([M/H] = −1) are also shown.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The color bar shows the mole fraction of NH3 in the log10 scale as a function of pressure and temperature. The region between the solid blue lines represents the retrieval constraint of HD 209458 b taken from MacDonald & Madhusudhan (2017), the black dashed line represents the T–P profile adopted for effective temperature T eff = 1000 K, g surface  =  3000 cm s−2, which is adopted from MacDonald & Madhusudhan (2017). The solid black lines represent the quench lines for different K  zz  values (labeled in the plots). The four plots represent the different values of atmospheric metallicity.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The top panel shows the T–P profile overplotted with the quenched curve of N2 (left), NH3 (middle), and HCN (right) for 20 different metallicities (green to red lines range from 0.1 to 1000× solar metallicity). The quenched curve is calculated for K  zz  = 109 cm2 s−1 and assuming the mixing length is equal to 0.1 × (upper triangles) and 1 (lower triangles) atmospheric scale height. The bottom panel shows the mixing ratio of N2 (left), NH3 (middle), and HCN (right), for the same set of metallicities. The colored lines represent the output of the chemical kinetics model and the corresponding faded colored lines the equilibrium abundances. The “+” symbol is the quench level calculated using the Smith method (Smith 1998).
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The timescale of the conversion of ﹩\mathrm{HCN}\to {\mathrm{NH}}_{3}﹩ (﹩{\tau }_{\mathrm{HCN}}﹩) for four different temperatures (750, 1250, 1750, and 2250 K) with five different metallicities (0.1, 1, 10, 100, and 1000× solar metallicity). The colored lines represent the timescale of the RLS in the corresponding temperature-pressure value, and the black dashed lines represent ﹩{\tau }_{{{\rm{H}}}_{2}}\,\times \,\tfrac{3[\mathrm{HCN}]}{{{\rm{H}}}_{2}}﹩. The solid black line represents ﹩{\tau }_{\mathrm{HCN}}﹩, labeled with the respective metallicity.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The left panel shows the contour of the chemical timescale of HCN (following the same convention as that used in Figure 6). The right panel shows the quenched curve of HCN (following the same convention as that used in Figure 7).
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The exoplanets whose atmosphere are probed and at least one H–C–N–O bearing molecule is found are plotted in their mass and orbital separation parameter space. Each colored circle denotes one H–C–N–O bearing molecule. The different markers refer to their detection method, given in the legend (exoplanet.eu).
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: Same as Figure 11 but for HD 189733 b. The solid circles (bottom right panel) represent the abndance of HCN calculated from Equation (7), where [NH3q ] and [CO q ] are taken from photochemistry transport. The solid circles are plotted until the quench level (for the mixing length = 0.1  ×  H) of HCN.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The ratio of the chemical kinetics model (with only transport) output mixing ratio at 100 mbar with the output of quenching approximation mixing ratio is shown. The vertical mixing timescale is calculated using the mixing length, which is calculated using the Smith method.
Paper: Using a Quench Level Approximation to Estimate the Effect of Metallicity on the Abundances of N-bearing Species in H2-dominated Atmospheres
Authors: Vikas Soni, Kinsuk Acharyya
Figure caption: The pressure–temperature range of different RLSs is shown for three different metallicities. Each color corresponds to the different RLSs in Figure 3.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Evolution of the magnetic toroid pattern during CR 2112 (2011 July 3–July 30), CR 2113 (2011 July 30–August 26), and CR 2114 (2011 August 26–September 22), i.e., from one CR before through the storm to one CR after, during which AR 11263, located at 300° longitude in the north (yellow circled region), produce the second-biggest flare (X-6.9) of cycle 24. Another AR (AR 11266, marked by pink circled region) in the same toroid, located at a longitude of about 55° left of AR 11263, did not flare.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Evolution of the magnetic helicity imbalance (top) and magnetic winding imbalance (bottom) for AR 12673. Negative values indicate the injection of potential-dominated magnetic structure and positive values indicate current-carrying-dominated magnetic field structure. Purple and beige backgrounds indicate first and second major emergences, respectively.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Evolution of the magnetic helicity imbalance (top) and magnetic winding imbalance (bottom) for AR 11263. Negative values indicate the injection of potential-dominated magnetic structure and positive values indicate current-carrying-dominated magnetic field structure. Purple and beige backgrounds indicate first and second major emergences, respectively.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Accumulation of magnetic helicity (top) and magnetic winding (bottom) for AR 11263. Purple and beige backgrounds indicate first and second major emergences, respectively. We note that after the X-class flare the AR approaches the limb, therefore the data become less reliable and are omitted. Here the start time is 2011 July 27, 12:00.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Evolution of the magnetic helicity imbalance (top) and magnetic winding imbalance (bottom) for AR 11266. Negative values indicate the injection of potential-dominated magnetic structure and positive values indicate current-carrying-dominated magnetic field structure.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Accumulation of fluxes magnetic helicity (top) and magnetic winding (bottom) for AR 11266. Here, the start time is 2011 August 2, 10:00.
Paper: Deciphering the Pre–solar-storm Features of the 2017 September Storm From Global and Local Dynamics
Authors: Breno Raphaldini, Mausumi Dikpati, Aimee A. Norton, Andre S. W. Teruya, Scott W. McIntosh, Christopher B. Prior, David MacTaggart
Figure caption: Summary of the maximal deviation of the helicity imbalance (right) and the magnetic winding imbalance (right).
Paper: A Low-mass line-rich Core Found in Massive Star-forming Region IRAS 16351-4722
Authors: Meizhu Liu, Sheng-Li Qin, Tie Liu, Mengyao Tang, Sheng-Yuan Liu, Li Chen, ChuanShou Li, HongQiong Shi, Xiaohu Li, Tianwei Zhang, Ken'ichi Tatematsu, Fengwei Xu, Yuefang Wu
Figure caption: Fractional abundances of different molecules relative to CH3OH in the I16351 low-mass line-rich core and the other hot corinos listed in Table B2.
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: Top: the GALFA-H I LVC column density image, divided into 10 equal subregions named as G0–G9, where each region is 36° × 36° in size. Bottom: the corresponding H I SPS calculated for the above G0–G9 regions. The gray area shows the range of angular scales used for fitting the SPS (between 18° and 16′, which corresponds to spatial frequencies k = 10−3 arcmin–1 to ∼6 × 10−2 arcmin−1).
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The H I column density images for three regions: inner Galactic plane (left), high Galactic latitude (middle), and outer Galactic plane (right). Each region has a size 40° × 40°. The three regions are centered at R.A. ∼19h30m (left), R.A. ∼12h45m (middle), and R.A. ∼06h00m (right), with decl. centered at 18.°5 for each.
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Light curves in three SDO/AIA channels (171, 211, and 304 Å) at the point marked with a small green circle in Figure 9(a).
Paper: High-altitude Spider-type Prominence above the Magnetic Null Point
Authors: Boris Filippov
Figure caption: Distance-time diagram along the slit AB shown in Figure 1(b).
Paper: Neutral Hydrogen (H I) 21 cm as a Probe: Investigating Spatial Variations in Interstellar Turbulent Properties
Authors: Amit Kumar Mittal, Brian L. Babler, Snežana Stanimirović, Nickolas Pingel
Figure caption: The H I column density calculated by integrating the H I brightness temperature from the GALFA-H I survey over the velocity range −40 km s−1 ≤v ≤ 40 km s−1. The Galactic coordinate grid is overlaid.