adsabs/AstroCLIMB huggingface dataset:
Paper: Radio Active Galactic Nuclei Activity in Low Redshift Galaxies Is Not Directly Related to Star Formation Rates
Authors: Arjun Suresh, Michael R. Blanton
Figure caption:  M ⋆ model predictions for the absolute fraction of AGN with λ > λ  c , where we will take λ  c  = 0.001. To the curve, we fit a cubic polynomial in log–log space, as shown by the dashed line. We quote the coefficients of this fit as a specification of our M ⋆ model. Note that this relationship between F AGN and M ⋆ is constrained only in the range ﹩10\leqslant \mathrm{log}\left({M}_{\star }/{M}_{\odot }\right)\leqslant 12﹩.
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Faraday rotation for azimuthal (left), radial (middle), and vertical (right) magnetic field configurations. For azimuthal and radial fields there is circular symmetry so there is rotation of different sign. In the vertical field there is constant rotation across the flow.
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: The depolarization caused by Faraday rotation for a homogeneous ordered field in either B  ϕ  or B  r .
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Cyg X-1 polarization angle as a function of energy (black data) showing its general alignment with the radio jet axis (magenta line), though there is a marginally significant linear trend (green line). The red line shows the predicted Faraday rotation angle from a homogeneous field of B  z  = 106 G. Adapted from H. Krawczynski et al. (2022).
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Same as Figure 3 but for constant vertical field.
Paper: Making the Invisible Visible: Magnetic Fields in Accretion Flows Revealed by X-Ray Polarization
Authors: Samuel Barnier, Chris Done
Figure caption: Same as Figure 3 but for constant radial field.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Scattering delays at 1500 MHz predicted by NE2001 and measured for pulsars in both J. E. Turner et al. (2021; blue circles) and this work (red stars). Arrows on some of the blue circles indicate lower limits. The dashed red line represents one-to-one correspondence. The high correlation coefficient for the data as a whole indicates general agreement with the model along the LOSs used in these analyses.
Paper: Modeling the Multiwavelength Detection of Protoclusters. I. An Excess of Submillimeter Galaxies in Protocluster Cores
Authors: Pablo Araya-Araya, Rachel K. Cochrane, Christopher C. Hayward, Robert M. Yates, Laerte Sodré, Marcelo C. Vicentin, Douglas Rennehan, Roderik Overzier, Marcel van Daalen
Figure caption: SFR vs. stellar mass relation for galaxies in protocluster cores (points), protocluster outskirts (contours), and the field (colored hexbin maps) at z ∼ 2.0, 3.0, and 4.0 (first, second, and third rows, respectively) for Fornax-, Virgo, and Coma-type protoclusters (first, second, and third columns, respectively). For all redshifts and protocluster types, the locus of galaxies in the SFR–Stellar mass plane (i.e.,  the SFMS) is independent of the environment. In all panels, the colored points at the high-mass tip of the SFMS indicate that protocluster cores host very high-mass star-forming galaxies that are not represented in less-dense environments.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Log–log plot of ﹩{\chi }_{r}^{2}﹩ and the corresponding dispersion measures for pulsars in both J. E. Turner et al. (2021; blue circles) and this work (red stars). The modest Pearson (r  p ) and Spearman (r  s ) correlation coefficients suggest a notable relationship between these two quantities.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: (a) A dynamic spectrum for PSR J1645–0317 on MJD 60137. (b) The corresponding 2D autocorrelation function. (c) The 1D frequency slice (orange) of the 2D autocorrelation function with corresponding fits. (d) The 1D time slice of the 2D autocorrelation function (red) with its corresponding fits.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example dynamic spectrum for PSR J0332+5434 on MJD 60237.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Example secondary spectrum for PSR J0332+5434 on MJD 60237.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: Scintillation bandwidth (left) and timescale (right) timeseries for pulsars with at least 10 measurements for both quantities.
Paper: The Pulsar Science Collaboratory: Multiepoch Scintillation Studies of Pulsars
Authors: Jacob E. Turner, Juan G. Lebron Medina, Zachary Zelensky, Kathleen A. Gustavson, Jeffrey Marx, Manvith Kothapalli, Luis D. Cruz Vega, Alexander Lee, Caryelis B. Figueroa, Daniel E. Reichart, Joshua B. Haislip, Vladimir V. Kouprianov, Steve White, Frank Ghigo, Sue Ann Heatherly, Maura A. McLaughlin
Figure caption: An example scintillation arc with its corresponding fit (dashed red line) for PSR J2022+5154 on MJD 60306. The color bar is in units of log power (dB).
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: The SED profiles of galaxies mapped onto the SOM with 5 times fewer cells. The gray SED curves represent the training set from the CANDELS survey, encompassing a variety of galaxy types, with the shading indicating the photometric errors. Overlaid in purple are the SEDs of normal star-forming galaxies from the MOSDEF survey, while the cyan SEDs correspond to AGNs from the same survey. All galaxies included in this analysis fall within the redshift range of 1.37 < z < 1.7. As illustrated, SED shapes gradually change from cell to cell, with similar SEDs in neighboring cells and higher photometric errors at the edges of the SOM. The X and Y axes represent the positions of galaxies as mapped into different cells of the SOM. The SEDs in each cell are normalized to the mean magnitude value within that cell, resulting in a magnitude range of 0.85–1.15. The wavelength range of the SEDs in each cell spans from 370 to 1800 nm.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: MOSDEF galaxies mapped onto the trained SOM. The top panel displays the first redshift bin at 1.37 < z < 1.7. The bottom panel depicts the redshift range 2.0 < z < 2.6. The background color represents the median stellar mass of CANDELS galaxies within each redshift bin. Normal star-forming MOSDEF galaxies are indicated by purple circles, while MOSDEF AGNs are marked by cyan “x” symbols.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Similar to Figure 6 on the redshift range of 2.0 < z < 2.6.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Distribution of MOSDEF AGNs mapped on SOM in the second redshift bin at (2.0 < z < 2.6), shown as cyan “x.” Blue squares around the cyan “x” mark represent MOSDEF AGNs in each respective group. The optical (Kauffmann ≪ Kewley) AGN group refers to the AGNs that lie between the G. Kauffmann et al. (2003) and L. Kewley et al. (2001) lines in the BPT (A. Baldwin et al. 1981) diagram. The optical (above Kewley) AGN group refers to AGNs that are located above the L. Kewley et al. (2001) line on the BPT diagram (A. Baldwin et al. 1981). Normal star-forming MOSDEF galaxies are indicated by purple circles.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: SEDs of two SOM cells at an enlarged scale, covering a redshift range of 2.0–2.6. SEDs are normalized to the mean magnitude values at each wavelength within its corresponding cell. The gray curves represent the training set from the CANDELS survey, covering various galaxy types with shading indicating photometric errors. Overlaid in purple are the SEDs of star-forming galaxies from the MOSDEF survey, while the cyan curves represent AGNs from the same survey. As illustrated, galaxies within the same SOM cell exhibit nearly similar SED shapes.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Distribution of MOSDEF AGNs mapped on SOM in the first redshift bin at (1.37 < z < 1.7), shown as cyan “x.” Blue squares around the cyan “x” mark represent MOSDEF AGNs in each respective group. The optical (Kauffmann ≪ Kewley) AGN group refers to the AGNs that lie between the G. Kauffmann et al. (2003) and L. Kewley et al. (2001) lines in the BPT (A. Baldwin et al. 1981) diagram. Normal star-forming MOSDEF galaxies are indicated by purple circles.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Nebular emission line ratios of the MOSDEF galaxies in the 1.37 < z < 1.7 (top row) and 2.0 < z < 2.6 (bottom row) redshift ranges. From left to right, the Hα/Hβ, [O III]/[O II], and [O III]/Hβ are plotted. The scatterplots show the relation between the median stellar mass of each cell (blue circles) and individual MOSDEF galaxies (black crosses).
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: Hα flux mapped to the SOM cells for two redshift bins: Left: 1.37 < z < 1.7. Right: 2.0 < z < 2.6. Each blue point in the scatterplots represents a SOM cell. Stellar mass values are derived from the CANDELS training sample, while Hα flux is obtained from the MOSDEF spectroscopic sample.
Paper: The Application of Manifold Learning to a Selection of Different Galaxy Populations and Scaling Relation Analysis
Authors: Sogol Sanjaripour, Shoubaneh Hemmati, Bahram Mobasher, Gabriela Canalizo, Barry C. Barish, Irene Shivaei, Alison L. Coil, Nima Chartab, Marziye Jafariyazani, Naveen A. Reddy, Mojegan Azadi
Figure caption: The gas-phase metallicity distribution on a 15 x 15 SOM.
Paper: Jet Interaction with Galaxy Cluster Mergers
Authors: P. Domínguez-Fernández, J. ZuHone, R. Weinberger, E. Bellomi, L. Hernquist, P. Nulsen, G. Brunetti
Figure caption: Visualization of the merger and AGN jet-material evolution. The upper, middle, and lower panels depict the early, mid, and late phases of run R = 1:5, θ = 20°, t jet,0 = 50 Myr at high resolution. The lower panels show density projection maps with a width of 8 Mpc. The upper left insets show a zoom-in dashed lines) where the AGN jet material is (contour lines). At the top of the middle panel, we additionally show six examples of different morphologies drawn by the CR jet pressure for different runs. The complete set of projection maps of the CR pressure with colorbars can be found in Appendix A.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: A portion of the approximate source-plane reconstruction of the Sunburst Arc from K. Sharon et al. (2022) with ray-traced non-LyC-leaking apertures overlaid in red and labeled in the top left of each panel. The numbered circles and square correspond to the unique source-plane regions identified in K. Sharon et al. (2022). Region 1 boxed in red is the LyC leaker.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: The rest-LyC (F275W) and Lyα maps of the north (N) and northwest (NW) segments of the Sunburst Arc, with the MagE slit apertures overlaid in magenta and the identified images of the Sunburst Arc marked and labeled following the color and naming scheme of K. Sharon et al. (2022). Boxes mark images of the LyC-leaking region, and circles mark all other images. The filter in parentheses in the Lyα map labels indicates the filter used to estimate the background continuum contribution to the count rate of F410M, which includes the Lyα line.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Lyα profiles of the stacked LyC-leaking and non-LyC-leaking MagE slit apertures with fits. Top: Lyα profiles of the stacked LyC leaker (above in blue) and non-LyC-leaking regions (below in red). The shaded regions indicate the 3σ uncertainty of the flux density. Center: stacked Lyα profile of the non-LyC-leaking apertures with the total fit in dashed black and individual peak fits in dotted black. Bottom: stacked LyC leaker Lyα profile with the total fit in dashed black and individual peak fits in dotted black.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Cartoon of the Lyα mirror hypothesis. The LyC-leaking region (bottom) produces a prodigious amount of Lyα (red) and LyC (blue) photons compared to the older non-LyC-leaking regions (top). Some photons from the LyC-leaking region directly escape out of a highly ionized channel oriented toward us. These photons constitute the observed LyC and central Lyα peak. Additional Lyα emission resonantly scatters off the expanding H I surrounding the LyC-leaking region until it escapes the galaxy along the observer's sight line, which constitute the redshifted and blueshifted Lyα peaks (bottom box). In the non-LyC-leaking regions, which have much less LyC flux due to their older age, the surrounding H I (gray) is thicker, preventing any LyC escape and direct Lyα escape. Thus, only a redshifted Lyα peak emerges (first box from the top). However, Lyα photons from the LyC-leaking region preferentially reflect into the observer's sight line incident upon the thick H I around the non-LyC-leaking regions (second box from the top), forming a central Lyα peak superimposed upon the redshifted Lyα peak emerging from the non-LyC-leaking regions.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Corner plot of the Lyα measurements, as well as ﹩{f}_{\mathrm{esc}}^{\mathrm{LyC}}﹩. Red squares are non-LyC-leaking apertures, blue circles are LyC-leaking apertures, and the pink star is slit M3. Filled markers are the stacked spectra. The value annotated in each plot indicates the Pearson correlation coefficient between the two quantities. Table 5 also lists the Pearson correlation coefficients and type “b” Kendall rank correlation coefficients.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Cartoon sketch of the spatially variable absorption hypothesis. The Lyα and LyC photons directly escaping through an ionized channel produce the LyC and the central Lyα peak observed from the LyC-leaking region. Lyα photons from the LyC-leaking region also resonantly scatter with either side of the surrounding, expanding H I shell, forming the redshifted and blueshifted Lyα peaks (bottom box). In this picture, the triple-peaked Lyα profile from the LyC-leaking region originates from a large source-plane area, and an intervening, outflowing absorber with higher H I column density attenuates the blueshifted Lyα peak and varying amounts of the central Lyα peak across the face of the galaxy.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Lyα maps centered on slit M3 created from the schemes discussed in Section 3.3. The top and bottom rows show the maps with the F390W and F555W filters as the off-band filter, respectively. The dashed magenta line is the on-sky aperture of slit M3. There are systematic differences between the two continuum subtraction bands, with the F555W-based subtraction removing marginally more continuum flux than the F390W-based subtraction.
Paper: Connecting Lyα and Ionizing Photon Escape in the Sunburst Arc
Authors: M. Riley Owens, Keunho J. Kim, Matthew B. Bayliss, T. Emil Rivera-Thorsen, Keren Sharon, Jane R. Rigby, Alexander Navarre, Michael Florian, Michael D. Gladders, Jessica G. Burns, Gourav Khullar, John Chisholm, Guillaume Mahler, Håkon Dahle, Christopher M. Malhas, Brian Welch, Taylor A. Hutchison, Raven Gassis, Suhyeon Choe, Prasanna Adhikari
Figure caption: Results of using GALFIT to remove a foreground galaxy over an image of the LyC leaker (image 1.5 in Figure 1) from the F275W and F814W images. Each column uses the same color map with a cube root scale, with minima (maxima) of the masked median of the cutout minus 2× (plus 100×) the standard deviation of the source-masked cutout. The GALFIT models have a flat background of zero.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Event timeline for the prominence observations. Time intervals are labeled 1–5, with filament intervals listed first. The time range is divided—at relative time t = 200 hr—into (a) Quiescent and (b) Precursor stages. A shaded region from t = 300 hr onward denotes a phase where rapid rise in the prominence is observed, with the approximate start time of the eruption marked at 328 hr (red, dashed–dotted line), corresponding to March 27 at 16:00 UT. Time is expressed in hours from 2011 March 14 00:00 UT.
Paper: A Precursor to Solar Prominence Eruptions: Detection and Analysis of EUV Prominence Oscillations
Authors: William Beckwith-Chandler, Claire Foullon, Erwin Verwichte
Figure caption: Evolution with time (Interval 4) over the northeast limb from SDO (top) the prominence height, h  B , corresponding to (bottom) the average limb angle, B*. Time is expressed in hours from 2011 March 14 00:00 UT.