adsabs/AstroCLIMB huggingface dataset:
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Plots of the center distances of the complexes as a function of area A compl (left), AR (central), and radius of the largest matched resolved clump (right). We plot the median profiles of the center distances as golden dots for ΔHα−opt, magenta squares for ΔUV−opt, and black triangles for ΔUV−opt, noHα . Error bars show the quartiles of the distribution in the bin. On the top right, we show the Pearson coefficient for each quantity and for Hα- and UV-matched clumps. We also plot our resolution limit as a horizontal gray dashed line.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Violin plots of the AR distributions of the star-forming clumps and complexes of our sample. Median values are plotted as stars, and the dark vertical line shows the interquartile region. Left plot: distribution of the whole UV- (magenta) and Hα- (golden) resolved clumps. Middle plot: UV- (magenta) and Hα- (golden) resolved clumps are divided into spatial categories (disk, extraplanar, and tail from left to right). Right plot: distribution of the resolved star-forming complexes.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Images of three star-forming complexes (in dark violet) together with the matched UV- (in purple) and Hα- (in golden, when present) selected trunk clumps. Geometrical centers of the complex and the brightest Hα- and UV-selected matched clumps are plotted as violet, purple, and golden stars, respectively. The underlying images are in the optical F606W band.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: As Figure 5, but for Hα-selected clumps filling factor f A(Hα) (golden dots) and UV-selected clumps filling factor f A(UV) (magenta squares).
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Images of three UV-resolved clumps. The solid contour defines the area of the clump, and the dashed ellipse is defined by the major and minor axis. The dashed line represents the major axis. The cross represents the geometric center of the clump. The arrow points to the center of the hosting galaxy. The clumps are selected as examples of the variety of elongation we have: from left to right, the AR (defined as the ratio of the semiminor to the semimajor axes of the clump) decreases from 0.92 to 0.60 to 0.24.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: F275W maps of the six galaxies of our sample. Top row (from left to right): JO175, JO201, and JO204; bottom row (from left to right): JO206, JW39, and JW100. In different colors, we plot the sub-tails we defined for each galaxy: the dots denote the UV-selected clumps we used to trace the regions (solid, closed regions) defining the sub-tails; the best-fitting trajectories of the sub-tails are plotted as solid lines (as straight lines or spiral arms, according to the choice made in Section A). The red dots denote the zero-points of the sub-tails, from which the distances of the clumps along the sub-tails are computed. Each sub-tail is flagged with a number.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Trends with the projected Galactocentric distance of the complex properties related to the matched clumps: golden dots when related to matched Hα-selected clumps, magenta squares to matched UV-selected clumps, and black triangles, when present, to UV-selected clumps in complexes with no Hα-selected clumps. Median profiles are plotted as dark golden dots for Hα-selected clumps and magenta squares for UV-selected clumps. Error bars show the quartiles of the distribution in the bin. From top to bottom: number of matched clumps; filling factor f  A ; radius of the brightest matched resolved clump r bc; and geometric center displacements (defined in Section 5.1, with our resolution limit of ∼0.055 kpc plotted as the horizontal dashed gray line).
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Plots of resolved clump and complex area A (top) and AR (bottom) as a function of the projected galactocentric distance. Yellow-to-red and magenta contours are the Hα- and UV-selected/resolved clump density distributions, respectively. Star-forming complexes are plotted as violet triangles. Golden dots, purple squares, and violet triangles represent the median profiles of the Hα-selected/resolved clump, UV-selected/resolved clump, and star-forming complex properties for bins containing an equal number of clumps/complexes, where the bars indicate the quartiles of the distribution.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Cumulative distribution of tail Hα- and UV-selected clumps (solid golden and dashed purple, respectively) and star-forming complexes (dashed–dotted violet) as a function of the distance. The median distances for each sample of clumps/complexes are plotted as vertical lines with the same color and style as the corresponding cumulative distribution.
Paper: Morphology of Star-forming Clumps in Ram-pressure Stripped Galaxies as Seen by HST
Authors: Eric Giunchi, Bianca M. Poggianti, Marco Gullieuszik, Alessia Moretti, Ariel Werle, Anita Zanella, Benedetta Vulcani, Stephanie Tonnesen, Daniela Calzetti, Callum Bellhouse, Claudia Scarlata, Cecilia Bacchini
Figure caption: Same as Figure 2, but for tilt angle distributions of resolved clumps and complexes.
Paper: Effect of Spherical Polarization on the Magnetic Spectrum of the Solar Wind
Authors: Corina Dunn, Trevor A. Bowen, Alfred Mallet, Samuel T. Badman, Stuart D. Bale
Figure caption: Panel (A): the perpendicular variance isotropy, Ψ, along the x-axis, and compressibility, ﹩\mathrm{log}({C}_{B})﹩, along the y-axis, form a basis to describe the geometry of observed structures. Each depicted structure is the hodogram of an interval of the magnetic field chosen to be as close as possible in Ψ and ﹩\mathrm{log}({C}_{B})﹩ values to its marked position. Hodograms are color-coded by the distance into the page, with the lightest points closest to the viewer. Each square is color-coded by the average α  B  in the Ψ–C  B  space contained. This α  B  value is also recorded in white at the top of each square. The white and purple curves, respectively, show contours for observations inside 30 R ⊙ and outside 200 R ⊙. The solid, dashed, and dotted lines show, respectively, the 90th, 70th, and 50th percentiles of counts in a 100 bin 2D histogram. Panels (B), (C), and (D) show, respectively, the probability densities of ﹩\mathrm{log}({C}_{B})﹩, Ψ, and α  B . The distributions of all studied intervals are shown in blue, for only data inside 30 R ⊙ in orange, and for data outside 200 R ⊙ in green.
Paper: Effect of Spherical Polarization on the Magnetic Spectrum of the Solar Wind
Authors: Corina Dunn, Trevor A. Bowen, Alfred Mallet, Samuel T. Badman, Stuart D. Bale
Figure caption: Panels (A), (B), and (C) show joint probability distributions of Ψ and α  B , with data column-normalized. Panels (D), (E), and (F) likewise show column-normalized joint probabilities of ﹩\mathrm{log}({C}_{B})﹩ and α  B . Panels (A) and (D) show all studied data, while panels (B) and (E) show data only in a 5 R ⊙ bin centered around 177.5 R ⊙. Panels (C) and (F) similarly show a 5 R ⊙ bin at 37.5 R ⊙. The dashed black line in each panel marks 2/3 scaling, while the dotted black line marks 1/2 scaling.
Paper: Effect of Spherical Polarization on the Magnetic Spectrum of the Solar Wind
Authors: Corina Dunn, Trevor A. Bowen, Alfred Mallet, Samuel T. Badman, Stuart D. Bale
Figure caption: The figure shows the effect of the “discontinuity conditioning” described on those extremely one-dimensional observations where Ψ < 0.05. Panels (A), (B), and (C) show the effect on α  B , Ψ, and ﹩\mathrm{log}{C}_{B}﹩, respectively, where orange shows unconditioned values for Ψ < 0.05, blue shows the conditioned distribution, and green shows the distribution for all intervals across the whole range of Ψ (the “parent distribution”). Panel (D) plots the average α  B  for Ψ values in each of the 15 bins, with error bars showing the standard deviation. Conditioned α  B  is plotted vs. conditioned Ψ in blue, while all unconditioned α  B  values are plotted against all unconditioned Ψ values in green.
Paper: Effect of Spherical Polarization on the Magnetic Spectrum of the Solar Wind
Authors: Corina Dunn, Trevor A. Bowen, Alfred Mallet, Samuel T. Badman, Stuart D. Bale
Figure caption: Panel (A) shows the evolution of Ψ with solar distance as a column-normalized joint probability. Panel (B) shows a column-normalized joint probability between the solar distance and ﹩\mathrm{log}({C}_{B})﹩. In Panels (A) and (B), the average values in 10 R ⊙ bins of Ψ and ﹩\mathrm{log}({C}_{B})﹩, respectively, are plotted in black, with error bars giving the standard deviation in each bin. Panel (C) shows a column-normalized joint probability between the solar distance and α  B , with dashed and dotted black lines indicating, respectively, 2/3 and 1/2 scalings.
Paper: Effect of Spherical Polarization on the Magnetic Spectrum of the Solar Wind
Authors: Corina Dunn, Trevor A. Bowen, Alfred Mallet, Samuel T. Badman, Stuart D. Bale
Figure caption: Panels (A) and (C) show hodograms of the magnetic field for a compressible arc-like interval (A) and for an incompressible spherically polarized interval (C). The mean field vector is shown as a black line from the origin. Panel (B) shows the perpendicular magnetic field of the structure in panel (A), with its directions of maximum and minimum variance shown as arrows scaled by the size of the corresponding eigenvalue. Panel (D) likewise shows the perpendicular magnetic field of panel (C).
Paper: Prospects for Detecting γ-Ray Bursts at Very High Energies with the HADAR Experiment
Authors: Yu-Hua Yao, Zhen Wang, Shi Chen, Tian-Lu Chen, You-Liang Feng, Qi Gao, Quan-Bu Gou, Yi-Qing Guo, Hong-Bo Hu, Ming-Ming Kang, Hai-Jin Li, Chen Liu, Mao-Yuan Liu, Wei Liu, Fang-Sheng Min, Hui-Ying Sun, Bing-Qiang Qiao, Xiang-Li Qian, Xu Wang, Guang-Guang Xin, Qiang Yuan, Yi Zhang
Figure caption: Key parameters utilized in generating GRB populations, with red lines representing standard distributions and blue and dark-green lines representing test distributions used to evaluate differences resulting from varying parameter distributions. Top left: E iso, derived by using the redshift-observed data of 400 GRBs. The fluence measurements are obtained from the Swift-BAT instrument, and the data are sourced from the GRB table available at https://swift.gsfc.nasa.gov/archive/grb_table/fullview/. The observations included in the analysis extend up to GRB 230506C. Top right: distribution of Lorentz factor, as reported by Ghirlanda et al. (2018). Middle: distributions of microphysical parameters ϵ  e  and ϵ  B , adapted from Santana et al. (2014). Bottom left: distribution of redshift, adopted from Wanderman & Piran (2010). Bottom right: distribution of electron index p (Wang et al. 2015).
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Left: HST WFC3/F438W image of the M81 bulge overlaid with the CAHA/PPAK FoV (black hexagon). Right: PPAK-measured Hα line intensity after Voronoi tessellation binning (Paper I). The Hα intensity contours from an HST narrowband image (Devereux et al. 1997) delineate the nuclear spiral at a higher angular resolution. The black cross marks the position of M81*, and the ellipse outlines the region with a deprojected radius of 800 pc.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: A schematic view of the adopted geometry. The radially equally spaced clouds are located in the same plane as defined by the stellar disk, illuminated by the central LLAGN and a combination of bulge+disk stars.
Paper: Prospects for Detecting γ-Ray Bursts at Very High Energies with the HADAR Experiment
Authors: Yu-Hua Yao, Zhen Wang, Shi Chen, Tian-Lu Chen, You-Liang Feng, Qi Gao, Quan-Bu Gou, Yi-Qing Guo, Hong-Bo Hu, Ming-Ming Kang, Hai-Jin Li, Chen Liu, Mao-Yuan Liu, Wei Liu, Fang-Sheng Min, Hui-Ying Sun, Bing-Qiang Qiao, Xiang-Li Qian, Xu Wang, Guang-Guang Xin, Qiang Yuan, Yi Zhang
Figure caption: The observed count of GRBs using HADAR is investigated, employing a methodology similar to that demonstrated in Figure 2, to explore the impact of varying a specific parameter on the distribution. Each panel is accompanied by the Poisson fit results of the respective distribution. The red line corresponds to the result obtained in Figure 2. In the top left panel, the standard distribution of Γ0 is replaced with an alternative test distribution. Similarly, in the top right panel, the standard ϵ  B  distribution is varied by utilizing a test distribution. Moving to the bottom left panel, the standard p distribution is substituted with a test distribution. Lastly, the density mediums are represented by different colored regions in the bottom right panel, where red, blue, and green correspond to density values of 1, 0.1, and 10 cm−3, respectively.
Paper: Prospects for Detecting γ-Ray Bursts at Very High Energies with the HADAR Experiment
Authors: Yu-Hua Yao, Zhen Wang, Shi Chen, Tian-Lu Chen, You-Liang Feng, Qi Gao, Quan-Bu Gou, Yi-Qing Guo, Hong-Bo Hu, Ming-Ming Kang, Hai-Jin Li, Chen Liu, Mao-Yuan Liu, Wei Liu, Fang-Sheng Min, Hui-Ying Sun, Bing-Qiang Qiao, Xiang-Li Qian, Xu Wang, Guang-Guang Xin, Qiang Yuan, Yi Zhang
Figure caption: Right: the detected count of GRBs utilizing HADAR's observation sensitivity, considering an intrinsic average annual burst of 600. GRBs are generated with standard parameter distributions. A total of 1000 simulated experiments were conducted, and a Gaussian fit is employed for analysis. Gilmore et al. (2012) is considered. Left: four different EBL models are considered; they are from the works of Inoue et al. (2013), Stecker et al. (2012), Finke et al. (2010), and Helgason & Kashlinsky (2012).
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The three traditional BPT diagrams plotting the flux ratios of emission-line pairs [O III]λ5007/Hβ vs. [N II]λ6584/Hα, [S II]λ λ6716, 31/Hα, and [O I]λ6300/Hα. The data points are derived from each Voronoi bin and are color coded by the deprojected distance from the galactic center. The dividing lines are from Kewley et al. (2006), which divide the line ratios into Seyfert, LINER, H II, and composite regions. In all three diagrams, the circumnuclear region of M81 exhibits a mixture of LINER and Seyfert characteristics.
Paper: Prospects for Detecting γ-Ray Bursts at Very High Energies with the HADAR Experiment
Authors: Yu-Hua Yao, Zhen Wang, Shi Chen, Tian-Lu Chen, You-Liang Feng, Qi Gao, Quan-Bu Gou, Yi-Qing Guo, Hong-Bo Hu, Ming-Ming Kang, Hai-Jin Li, Chen Liu, Mao-Yuan Liu, Wei Liu, Fang-Sheng Min, Hui-Ying Sun, Bing-Qiang Qiao, Xiang-Li Qian, Xu Wang, Guang-Guang Xin, Qiang Yuan, Yi Zhang
Figure caption: Light curve (left) and spectra (right) of a single GRB are presented as the black lines. The parameters used are E  k  = 6 × 1053 erg, Γ0 = 300, ϵ  e  = 0.07, ϵ  B  = 4 × 10−5, p = 2.5, n 0 = 0.3 cm−3, and z = 0.2. The sensitivity curves (green lines) of HADAR are plotted, which are determined by calculating them with the GRB located at R.A. = 288.°26 and decl. = 9.°8, assuming the burst time at MJD = 59863.491. The Moon and Sun orbits have also been tracked.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Left: the adopted SED of the LLAGN (M81*) and stellar populations at ∼20 pc from the galactic center. The difference between the jet-dominated (solid black line) and ADAF-dominated (dotted blue line) models of M81* is small within the range of the ionizing UV band (100–912 Å). The default AGN model in CLOUDY is also plotted as a dashed magenta line. The dashed red line is the default bulge stellar population (SP), while the dashed–dotted green and dotted yellow lines represent alternative bulge SPs with different ages and metallicities. The dashed–dotted cyan line shows the SED from 10,000 pAGB stars, each with a blackbody temperature of 105 K and a luminosity of 103 L ⊙, following the same deprojected Sérsic distribution as the bulge. The dashed orange line shows the SED of 200 XRBs following an L −1 luminosity function and the deprojected Sérsic bulge distribution. The vertical black dashed line marks the Lyman limit at 912 Å. Right: the radial distribution of ionization parameter U, by M81* (dashed red line), the default bulge SP (solid blue line), the disk SP (orange dotted line), and the XRBs (solid tomato line), respectively.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The radial distribution of the observed line intensities (black points) and the simulated line intensities from the CLOUDY models (colored lines) of the most prominent emission lines: Hα, Hβ, [N II], [O III], [O II] and [O I]. The units are ﹩\mathrm{erg}\,{{\rm{s}}}^{-1}\,{\mathrm{cm}}^{-2}\,{\mathrm{arcsec}}^{-2}﹩. The observed line intensities are derived from a single Gaussian fit to each Voronoi bin. The error bar of the y-axis represents the standard deviation of the fitting results from 100 iterations of Monte Carlo simulations. The error bar of the x-axis represents the range of the deprojected radius of each Voronoi bin. The dashed black line represents a CLOUDY model with M81* as the only ionizing source, whereas the green solid line represents a similar model but using the built-in AGN SED of CLOUDY. The solid blue line represents a model with the 8 Gyr old bulge SP as the only ionizing source, and the dotted orange line represents a model with the 2 Gyr old disk SP as the only ionizing source. The combination of the AGN and the two SPs (i.e., model A) is shown by the solid red line.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Left: the radial distribution of electron density. The black points are computed with the observed [S II] doublet line ratio of each Voronoi bin. Some data points have their line ratio falling below the density-sensitive range and are thus plotted as an upper limit at a value of 10 cm−3. The default radial distribution of hydrogen density n H ∝ r −1 is shown as a solid red line. Another radial distribution, n H ∝ r −1.5, is shown by a dashed–dotted blue line. Right: the observed [S II] doublet line ratio as a function of radius (black points), in comparison with model predictions based on the different hydrogen density profiles (Table 1). The horizontal dashed line indicates the line ratio above which the resultant electron density is lower than 10 cm−3, which is beyond the valid range of the [S II] doublet line ratio.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: Left: similar to Figure 10, but comparing models with different density distributions. The default model A with a density profile n H ∝ r −1 is shown with a solid red line. Model F, with a density profile of n H ∝ r −1.5 is shown with a dashed blue line, and models G, H, and I, with a constant density of 1, 10, and 100 cm−3 are shown with a dotted, dashed, and solid orange line, respectively. In the left panel, the line ratio predicted by model G is below the range presented here due to a significantly lower [N II], resulting in this model.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The radial distribution of observed [N II]/Hα (Left) and [O III]/Hβ (Right) line ratios are shown as black points. For clarity, error bars are not displayed for the x-axis. The line ratio measurements of ground-based spectroscopic observations extracted from an aperture of ∼4″ × 2″ (Ho et al. 1996) are also plotted as a black diamond. The AGN, SP (bulge plus disk), and AGN+SP models are shown by the black dashed, blue dashed–dotted, and red solid lines, respectively.
Paper: CAHA/PPAK Integral-field Spectroscopic Observations of M81. II. Testing Photoionization Models in a Spatially Resolved LINER
Authors: Zongnan Li, Zhiyuan Li, Rubén García-Benito, Yifei Jin
Figure caption: The radial distribution of the observed [N II]/Hα (left) and [O III]/Hβ (right) line ratios, in comparison with models with different AGN luminosities. The default model (A) is shown by a solid red line, while model B with the ADAF-dominated SED is shown by the dashed–dotted cyan line, and model C with a 10 times higher AGN luminosity is shown by the dotted blue line.