adsabs/AstroCLIMB huggingface dataset:
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Optical light curves of V1515 Cyg between 2006 and 2022. Most of the BVR  C  I  C  data were obtained at the Piszkéstetö Observatory, while the rest of the data taken in the V and g band are from the ASAS-SN database. The vertical dashed dark gray lines mark the BOAO and NOT optical/IR observations between 2012 and 2021 as well as the 2015 spectrum of V1515 Cyg by Connelley & Reipurth (2018). Yellow dashed–dotted lines indicate the TESS Sector 14, 15, and 41 observations of the source.
Paper: Observational Constraints on Cosmic-Ray Escape from Ultrahigh-energy Accelerators
Authors: Quentin Luce, Sullivan Marafico, Jonathan Biteau, Antonio Condorelli, Olivier Deligny
Figure caption: Energy flux at Earth as a function of energy, as modeled by the best-fit parameters for a variation around the benchmark scenario using the Sibyll2.3c hadronic interaction model. The all-particle spectrum and proton component are shown as black circles and red squares, respectively. Lighter points are not included in the fit. The best-fit components obtained for the five detected mass groups are displayed with solid colored lines, as labeled in the figure.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Light curves of V1515 Cyg gathered by TESS in 2019 and 2021, aligned to our I  C  light curves.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Upper panel: detrended 2021 data indicated in different filters. TESS coverage is indicated by two parallel dashed lines. Bottom panel: color–magnitude diagrams for the detrended light curve. Evolutionary paths obtained from accretion disk modeling (Section 4.2) are indicated by lines of different colors.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Comparison of the profiles of lines with P Cygni shape in V1515 Cyg in 2021 May.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Source-plane reconstructions of the [O II] emission, Fe II* emission, and the Mg II emission doublet surface brightness map around the counter arc. Top row: the reconstructions of the MUSE surface brightness maps for the emission lines in the source plane. The white contours represent the 3σ significance levels (see Table: 2). The Δx and Δy represent the distance along the R.A. α direction and decl. δ direction, respectively. The yellow ellipses in the top panels represent the maximum seeing in the source plane for the counter arc. Bottom row: source-plane reconstruction of the HST image for the counter arc. We plot the 3σ contours from the top row over these HST reconstructions.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Mean surface brightness radial profiles for the [O II] (red diamonds), Fe II* (purple circles), and Mg II emission (black squares) in the source plane for image 3 (first panel), the star-forming regions U (second panel), E (third panel), and B (fourth panel). All the data points are representatives of radial bins with surface brightness pixels greater than 3σ. The dashed lines represent the fitted models from Section 3.5. The best-fit parameters are summarized in Table B1 in Appendix B. The Fe II* and Mg II are bright and more extended than the [O II] nebular emission.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Source-plane reconstruction of the [O II] emission (top row), the Fe II* emission (middle row), and the Mg II emission doublet λ λ2796, 2803 emission (bottom row) surface brightness maps in images 1 (left column), 2 (middle column), and 3 (right column), respectively. The white contours represent the 3σ significance levels. We label the four individual star-forming regions as shown in Figure 1. The reconstructed maximum seeing is shown as a filled yellow region in the left corner of each subplot.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Source-plane surface brightness spatial extents of the [O II] emission (left), Fe II* emission (middle), and the Mg II full emission (right) in the counter arc. The top row and bottom row represent the spatial extent of the surface brightness along the x (R.A. α) and y directions (decl. δ), respectively. The open circles with arrows represent the 2σ upper limit for nondetections. All the surface brightness data points are normalized by dividing by the value of the pixel with maximum surface brightness. The yellow dashed lines in the top and bottom rows represent the normalized seeing profile extents along the x and y directions, respectively.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Surface brightness maps in the image plane for the continuum-subtracted [O II] emission (Left), Fe II* emission (Middle), and Mg II emission (right) around the main arc (top row) and the counter arc (bottom row), respectively. The white contours correspond to 3σ surface brightness significance levels (Table 2). The yellow dashed rectangles in the top row correspond to the three images of the main arc from Figure 1 from left to right, respectively. The yellow circles in the top right of each subplot represent the maximum seeing during observation.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Surface brightness radial profiles for the [O II] emission (left), Fe II* emission (middle), and Mg II emission (right). The radial profiles are measured from the center of the galaxy. The filled black squares represent radial bins with significance greater than 3σ. The open black squares represent the 2σ upper limits in radial bins with nondetections. The dashed gold line represents the radial profile for the seeing for the counter-arc image in the source plane.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Gas covering fraction C  f (r) as a function of distance for Mg II emission (black squares), Fe II* emission (purple circles), and [O II] emission (red diamonds), respectively. The detection limit is 3σ for the surface brightness of a pixel to be counted as a detection. A value of C  f (r) = 1 means the radial bin area is totally covered by emission, and a value of C  f (r) = 0 means that there is no emission covering any area of that radial bin.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Mg II continuum-subtracted emission surface brightness maps for the Mg II 2803 primary (left) and secondary (right) components, respectively. The white contours represent the 3σ surface brightness limits. The yellow circles in the top left of each subplot represent the maximum seeing during observation. Both the primary and secondary Mg II emission peaks are spatially extended. The primary component and the secondary component are redshifted and have mean velocities of 100 km s−1 and 500 km s−1 with respect to the galaxy redshift, respectively.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Panel A: Mg II 2803 primary emission component surface brightness map in the source plane. The white contour corresponds to a 3σ significance level. The yellow ellipse represents the shape and the size of the seeing in the source plane. Panel B: mean surface brightness radial profile. Panels C and D show the spatial extent of the surface brightness along the x-axis and y-axis, respectively. The filled black squares represent mean surface brightness greater than 3σ. The open black squares are 2σ upper limits for bins with surface brightness below 3σ. The orange dashed lines in the panels represent seeing in the source plane.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Required Q in photons s–1 vs. light-travel time. This represents the luminosity required to ionize the gas at each radius, while the projected distance from the center is converted into time considering the light-travel time. In black circles we show the values derived from model 1 for every arm. In red we show the lower limit of Q as shown in Figure 5 of Keel et al. (2017), and the solid light-blue line represents the data obtained by Gagne et al. (2014). The gray lines come from Figure 7 in Keel et al. (2017), and they represent the peak Q values in every 1000 lt-yr bin for different objects. The Q values from Keel et al. (2017) are derived from a recombination balance method that provides a lower limit to the ionizing flux at different radii of the EELR. They use the highest surface brightness observed in Hα as a function of projected distance to estimate the required (isotropic) emission rate of ionizing photons (Q ion). Our results are consistent with the results from Keel et al. (2017), as they show a similar tendency of increasing Q ion but with higher values, which is expected, as Keel et al. (2017) values represent a lower limit.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Bolometric luminosity vs. projected distance from the center. The different symbols represent apertures over different arms. The shaded areas represent the error for each measurement from MC simulations to the data. The blue shaded area corresponds to the data obtained from model 1. Model 1 corresponds to the bolometric luminosity obtained assuming that the gas density is equivalent to the electron density derived from the [S II] line ratio, fixing this parameter in the fitting to the photoionization simulations, using the code CLOUDY. In model 2 we leave as free parameters the ionization parameter and the gas density in the fitting to our photoionization simulations, which results in different L bol values for both approaches. There is a clear tendency of increasing L bol with projected distance from the center for both models. This implies a change of ∼120 (for model 1) and ∼160 (for model 2) times in luminosity over the past 5 × 104 yr.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Top: velocity maps from two Gaussian component fit to the inner region, where the left corresponds to the broad component and the right to the narrow component. The black contours correspond to the respective flux for each component, while the magenta contours correspond to the extinction from a single component fit. The two points marked as “A” and “B” show the spaxels where example spectra are extracted from. Bottom: spectral profiles extracted from points “A” (left) and “B” (right); overplotted in red is the total fitted profile, with the two components marked in blue.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: BPT diagram; black dots are derived from the fluxes coming from the apertures to each arm. Colored dots come from the CLOUDY simulations, where the color indicates different ionization parameter values (U) and from left to right covers 1–4.5 dex of hydrogen density. The gray dots correspond to the CLOUDY simulations assuming solar metallicity.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: CLOUDY model over data ratios for the emission lines; solid lines show the model obtained assuming a density from the [S II] emission-line ratio, while dashed lines show a model assuming the density as a free parameter. The different colors represent the different metallicity scenarios. The top panel corresponds to an aperture over the “A” arm, while the bottom panel shows an aperture over the “AT” arm.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Top panel: SF for the magnitude difference of every radius (black circles) and the total magnitude difference (red triangle). We add in gray the variability data summarized in Figure 2 of Sartori et al. (2018) for comparison. Gray circles represent the quasar SF. Squares represent the Δm for changing-look quasars. Downward-pointing triangles show the data for Voorwerpjes from Keel et al. (2017; filled triangles) and from X-ray data (open triangles). For more details see Sartori et al. (2018). Bottom panel: zoomed-in version of the top panel.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Example of double Gaussian component fit to an aperture in the “C” arm. Top panels: zoom-in of the spectral windows, containing the emission lines, from left to right, Hβ, [O III], [N II] and Hα, and [S II]. In blue are the two Gaussian components, and in red the sum of both components. Bottom panel: fit to the complete spectra, trimmed at 7400 Å. Gaussian components are in blue, and the final fit of the summed components is represented by the dashed red line.
Paper: Detailed Accretion History of the Supermassive Black Hole in NGC 5972 over the Past ≳104 yr through the Extended Emission-line Region
Authors: C. Finlez, E. Treister, F. Bauer, W. Keel, M. Koss, N. Nagar, L. Sartori, W. P. Maksym, G. Venturi, D. Tubín, T. Harvey
Figure caption: Velocity profiles extracted from the two Gaussian component fit velocity maps along PA = 110°. The points in red represent the broad component, while the points in blue represent the narrow component.
Paper: Examining AGN UV/Optical Variability beyond the Simple Damped Random Walk
Authors: Weixiang Yu, Gordon T. Richards, Michael S. Vogeley, Jackeline Moreno, Matthew J. Graham
Figure caption: Top left: DHO fits of S82 quasars in the ξ, ω 0 space (LHS of Equation (3)). Underdamped DHOs are located to the left of the solid vertical line (ξ = 1), and overdamped DHOs are located to the right of this same line. The dashed–dotted line further (empirically) separates underdamped DHOs into QPOs and oscillatory DHOs. Both underdamped and overdamped DHOs are colored by their decorrelation timescales (τ decorr) but using two different color maps. The purple dotted lines on the underdamped population show the evolution of τ rise across the parameter space, where the numbers give the τ rise in the unit of days. Top right: DHO fits of S82 quasars in the σ  ϵ , τ perturb space (RHS of Equation (3)). Same as in the top left panel, colors show the corresponding τ decorr for each object, and different color maps are used for the underdamped and overdamped populations. Bottom left: the driving process (RHS of Equation (3)) PSDs of the three selected points A, B, and C shown in the top two panels (see footnote 11). Bottom middle: the response functions (LHS of Equation (3)) due to a delta function impulse of the dynamical systems described by the same selected points A, B, and C. Bottom right: DHO light curves simulated using A, B, and C as the input model parameters. Superimposed are the versions down-sampled using the best (magenta) and the worst (orange) cadences of our SDSS light curves (in terms of the number of observations, baseline duration, and photometric accuracy) for each classification. Median photometric uncertainties are used for error bars.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Motion of the stars within the isophotal contour shown in Figure 8. The left panel shows the motions of the UMS stars, while the right panel is for the PMS stars. Each arrow indicates the average direction of the stars found within a 200 × 200 pixel grid, after subtracting the total NGC 346 motion. The arrow length, increased 10,000 times, corresponds to the measured displacement. In the left panel the contamination of the SMC young field was statistically removed. Green, blue, and magenta colors were used to highlight different directions. Yellow star symbols mark the positions of the YSOs identified by Sewiło et al. (2013). The green plus symbols highlight the positions of the photometric center, while the rotation center is marked with a red x. The density contours highlight the spatial distribution of the PMS stars.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Spatial distribution of the stars found within 0.5σ from the three Gaussian peaks found in the side histogram of Figure 9. The left panel shows the distribution of the stars associated with the broader green Gaussian, the central panel the distribution of the stars associated with the narrow magenta Gaussian, and the right panel the distribution of the stars found under the blue Gaussian. The arrows indicate the average motion of the stars found in the higher density regions, after the mean motion of NGC 346 has been subtracted.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Left panels: v  θ  (upper panel) and v  ρ  (lower panel) components of the velocity as a function of the distance from the rotation center. Sources that lie within 2σ from (v  θ , v  ρ  = 0, 0) are shown in blue, and the remaining sources are in gray. The continuous yellow line marks the mean value of the distribution. The dashed yellow lines mark the + and -1 standard deviation. Right panels: zoomed in views of the v  θ  and v  ρ  1σ variations as a function of the distance from the rotation center.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Spatial distribution of NGC 346 UMS stars. The arrows indicates the direction of the motion with the respect of the rotation center, while their length is proportional to their velocity. As in Figure 10 the yellow stars mark the positions of the massive YSOs. The red logarithmic spiral, described by the equation ﹩x=\cos (\theta ){e}^{0.21\theta }﹩                       ﹩y=\sin (\theta ){\exp }^{0.21\theta }﹩, is not a fit, and has been superimposed only to guide the eye. The dashed line connects the stars in the center to the tail of stars that appear to escape NGC 346 from the southwest. The dashed blue line highlights the stream of stars that connect the small cluster to the west to the southern tail.