adsabs/AstroCLIMB huggingface dataset:
Paper: A Luminous Dust-obscured Tidal Disruption Event Candidate in a Star-forming Galaxy at 42 Mpc
Authors: Christos Panagiotou, Kishalay De, Megan Masterson, Erin Kara, Michael Calzadilla, Anna-Christina Eilers, Danielle Frostig, Viraj Karambelkar, Mansi Kasliwal, Nathan Lourie, Aaron M. Meisner, Robert A. Simcoe, Robert Stein, Jeffry Zolkower
Figure caption: The Galactic-extinction-corrected rest-frame u − r color of NGC 7392 (red square) vs its best-fit stellar mass, obtained through reproducing the broadband photometry of the galaxy. The errors are not distinguishable due to their small value. Magenta diamonds denote the values for TDEs discovered by SRG/eROSITA (Sazonov et al. 2021), while blue squares correspond to TDEs found in the ZTF survey (Hammerstein et al. 2022). The contours enclose a comparison sample of nearby (z < 0.1) SDSS galaxies (Mendel et al. 2014). The green dashed lines denote the limits of the green valley parameter space, as given by van Velzen et al. (2021), where most of the optically and X-ray selected TDEs are found. Contrarily, NGC 7392 sits in a very different region of parameter space, where star-forming galaxies reside.
Paper: A Luminous Dust-obscured Tidal Disruption Event Candidate in a Star-forming Galaxy at 42 Mpc
Authors: Christos Panagiotou, Kishalay De, Megan Masterson, Erin Kara, Michael Calzadilla, Anna-Christina Eilers, Danielle Frostig, Viraj Karambelkar, Mansi Kasliwal, Nathan Lourie, Aaron M. Meisner, Robert A. Simcoe, Robert Stein, Jeffry Zolkower
Figure caption: Optical and NIR follow-up spectroscopy of the nucleus of NGC 7392. The gray lines show the raw spectra in the lower two panels while the black lines show the binned spectrum. Prominent spectral features are marked. Regions of telluric absorption and low atmospheric transmission are masked with gray boxes. The insets show profiles of the major emission and absorption features of H, He, N, and Na together with best-fit Gaussian profiles. The spectral regions used for the PPXF fitting of the Ca II IR triplet and CO band heads are indicated.
Paper: Scary Barbie: An Extremely Energetic, Long-duration Tidal Disruption Event Candidate without a Detected Host Galaxy at z = 0.995
Authors: Bhagya M. Subrayan, Dan Milisavljevic, Ryan Chornock, Raffaella Margutti, Kate D. Alexander, Vandana Ramakrishnan, Paul C. Duffell, Danielle A. Dickinson, Kyoung-Soo Lee, Dimitrios Giannios, Geoffery Lentner, Mark Linvill, Braden Garretson, Matthew J. Graham, Daniel Stern, Daniel Brethauer, Tien Duong, Wynn Jacobson-Galán, Natalie LeBaron, David Matthews, Huei Sears, Padma Venkatraman
Figure caption: Optical photometry of AT 2021lwx. Left: ZTF forced photometry in ztf-g and ztf-r bands from the ZTF survey. The data in orange and cyan bands are from ATLAS forced photometry. The inset highlights the evidence of minor fluctuations in the otherwise smooth light curve. The light curve presented is as measured in the observed frame, and the measurements are not corrected for extinction. The ATLAS photometry is plotted using an offset for the purpose of clarity. Right: rest-frame ztf-r absolute light curve of AT 2021lwx plotted in comparison with other transients. The light curve of AT 2021lwx is corrected for Milky Way foreground extinction in addition to K correction. The light curves of other transients except ASASSN-15lh (V band) are in r/R passbands plotted with respect to the days from peak or days from discovery (see Section 6 for references).
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Left: average spectra of the 3.°3 × 2.°5 region of Cygnus X North with the black, blue, and green lines indicating the H I, 12CO, and 13CO emissions, respectively. Middle: line-integrated maps of H I (colors in the backgrounds), 12CO (black contours), and 13CO (purple contours) emissions of the first velocity component. The minimal level and the interval of the black contours are 30 K km s−1 and 45 K km s−1, respectively. The minimal level and the interval of the purple contours are both 21 K km s−1. The dashed lines indicate the coverage of the 12CO and 13CO data. Right: line-integrated maps of H I, 12CO, and 13CO emissions of the second velocity component. The minimal level and the interval of the black contours are 50 K km s−1. The minimal level and the interval of the red contours are 24 K km s−1.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Average H I (T on), HISA, and 12CO spectra over 5′ × 5′ centered on the DR21 filament region. The dashed red lines show the fitted curves (T off) to the absorption-free channels of the H I spectrum using different methods. The HISA curve (solid red line) is estimated by subtracting the H I spectrum from the fitted curve.
Paper: Scary Barbie: An Extremely Energetic, Long-duration Tidal Disruption Event Candidate without a Detected Host Galaxy at z = 0.995
Authors: Bhagya M. Subrayan, Dan Milisavljevic, Ryan Chornock, Raffaella Margutti, Kate D. Alexander, Vandana Ramakrishnan, Paul C. Duffell, Danielle A. Dickinson, Kyoung-Soo Lee, Dimitrios Giannios, Geoffery Lentner, Mark Linvill, Braden Garretson, Matthew J. Graham, Daniel Stern, Daniel Brethauer, Tien Duong, Wynn Jacobson-Galán, Natalie LeBaron, David Matthews, Huei Sears, Padma Venkatraman
Figure caption: Top panel: (left) multiband light-curve fits from MOSFiT TDE model; (right) pseudo-bolometric light curve of AT 2021lwx. Later epochs of AT 2021lwx are reasonably fit with a t −5/3 or a t −4/3 power law. Bottom panel: (left) g - r color evolution of AT 2021lwx; (right) blackbody temperature evolution of AT 2021lwx.
Paper: Scary Barbie: An Extremely Energetic, Long-duration Tidal Disruption Event Candidate without a Detected Host Galaxy at z = 0.995
Authors: Bhagya M. Subrayan, Dan Milisavljevic, Ryan Chornock, Raffaella Margutti, Kate D. Alexander, Vandana Ramakrishnan, Paul C. Duffell, Danielle A. Dickinson, Kyoung-Soo Lee, Dimitrios Giannios, Geoffery Lentner, Mark Linvill, Braden Garretson, Matthew J. Graham, Daniel Stern, Daniel Brethauer, Tien Duong, Wynn Jacobson-Galán, Natalie LeBaron, David Matthews, Huei Sears, Padma Venkatraman
Figure caption: Top: spectra of AT 2021lwx obtained from Lick (brown), Keck (black), and Palomar (blue) with UT dates of observations and phase with respect to the first detection in ztf-r (MJD 59025.38) provided. Our highest-quality spectrum from November 2022 is enlarged with line identifications. Bottom: comparison with various transients including a composite quasar (QSO; Vanden Berk et al. 2001), the TDE (AT 2019qiz, Hung et al. 2021), the Type IIn (SN 2010jl, Fransson et al. 2014), and the ANT (ASSASN-17jz, Holoien et al. 2022). Wavelength regions of telluric contamination are marked with “⊕” symbol.
Paper: Scary Barbie: An Extremely Energetic, Long-duration Tidal Disruption Event Candidate without a Detected Host Galaxy at z = 0.995
Authors: Bhagya M. Subrayan, Dan Milisavljevic, Ryan Chornock, Raffaella Margutti, Kate D. Alexander, Vandana Ramakrishnan, Paul C. Duffell, Danielle A. Dickinson, Kyoung-Soo Lee, Dimitrios Giannios, Geoffery Lentner, Mark Linvill, Braden Garretson, Matthew J. Graham, Daniel Stern, Daniel Brethauer, Tien Duong, Wynn Jacobson-Galán, Natalie LeBaron, David Matthews, Huei Sears, Padma Venkatraman
Figure caption: Left: ZTF image of the field surrounding AT 2021lwx in ztf-r band obtained on 2020 December 16 and retrieved from the Infrared Science Archive (IRSA). The red circle shows the position of AT 2021lwx. Green circles are catalog stars obtained from Gaia DR2 (Van Leeuwen et al. 2018). Middle: composite r − i − z image of the same field made from images obtained from the PanSTARRS archive. Right: zoom-in at the location of AT 2021lwx. No underlying host galaxy is detected.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Left: 1.4 GHz radio continuum emission from the Effelsberg Galactic plane survey (Reich et al. 1990, 1997). The circle sizes approximate the radius of the H II regions from Anderson et al. (2014). The purple line indicates the distribution of the Cygnus X North filament. The green stars indicate the O-type stars in Cygnus OB2 from Comerón & Pasquali (2012). Middle: the sketch map of H II regions Cygnus OB2 and G081.920+00.138 in the three-dimensional coordinate system. Right: position–velocity map of H I (colors in the backgrounds) and 12CO (contours) emission along the decl. in the left panel.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption:  N(H I) and N(H2) as a function of time for the DR21 filament. The black dotted line indicates the calculated time from the N(H I) and N(H2) of the DR21 filament.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Left: 12CO integrated intensity overlaid on the line-integrated H I emission. The purple line indicates distribution of the Cygnus X North filament. The intensities are integrated over a velocity range from −8 to −2 km s−1. The minimal level and the interval of the overlaid contours are 0.2× peak and 0.15× peak of 12CO brightness. Middle: position–velocity map of H I (color) and 12CO (contours) emission along the purple line in the left panel. Right: map of HISA intensity integrated from −8 to −2 km s−1.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Left: column density map of the H I cloud derived from HISA, assuming the spin temperature T HISA = 40 K and P = 0.7. Middle: column density map of the molecular cloud derived from 13CO emission. Right: ratio of the H2-to-H I column densities.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: A pixel-by-pixel comparison between the line center velocity (relative to the local standard of rest) of the extracted HISA features vs. that of the observed 12CO emissions. As indicated in the top right corner of each panel, we show the comparisons for the HISA features derived with the second-order, third-order, and fourth-order polynomial fittings and with the Gaussian fittings. The solid line in each panel indicates the relation where the HISA velocity equals the 12CO velocity.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Top row: peak velocity of the HISA data (left panel) and the 12CO data (right panel), respectively. The HISA are extracted by using a third-order polynomial to estimate the background emissions. Bottom row: FWHM of the HISA emission (left panel) and the 12CO feature (right panel), respectively.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Velocity channel maps of H I (gray scale and gray contours) and 12CO (red contours) emissions between −12 and 24 km s−1. The minimal level of the gray contours is 0.55 times the emission peak, and the interval is 0.25 times the peak. The minimal level of the red contours is 0.15 times the emission peak. Note that for display purposes, we have binned the original channels into velocity windows of a width of 4 km s−1.
Paper: H I Self-absorption toward the Cygnus X North: From Atomic Filament to Molecular Filament
Authors: Chong Li, Keping Qiu, Di Li, Hongchi Wang, Yue Cao, Junhao Liu, Yuehui Ma, Chenglin Yang
Figure caption: Left: T cont from the Effelsberg 21 cm radio continuum emission. Right: counts histogram of the derived optical depth at all the pixels.
Paper: M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population
Authors: Jae-Woo Lee
Figure caption: (a) A chromosome map of the primordial population of our study. The gray dashed line shows the border line between the FG and SG populations by Milone et al. (2017). (b) The simulated chromosome map for our primordial population. The orange plus signs (P2) are for (ΔY, Δ[O/Fe], Δ[Mg/Fe]) = (+0.028, −0.30, −0.80) with respect to the P1 (blue plus signs). (c) Same as (a) but for the intermediate population. (d) The simulated chromosome map for our intermediate population, with (ΔY, Δ[C/Fe], Δ[N/Fe], Δ[O/Fe]) = (+0.028, −0.30, +0.60, −0.20) with respect to the P1. (e) Same as (a) but for the extreme population. (f) The simulated chromosome map for our intermediate population, with (ΔY, Δ[C/Fe], Δ[N/Fe], Δ[O/Fe]) = (+0.028, −0.60, +1.20, −0.40) with respect to the P1. (g) Cumulative radial distributions (CRDs) of the FG (the blue solid line) and SG (the red solid line) classified by using the border line by Milone et al. (2017). (h) CRDs of the primordial (the blue solid line), intermediate (the gold solid line), and extreme (the red solid line) populations. The magenta dashed line is for the enhanced population.
Paper: M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population
Authors: Jae-Woo Lee
Figure caption: (a) The [C/Fe] ch  vs. V magnitude of M92 RGB stars with −2.5 mag ≤ V − V HB ≤ −3.0 mag. The gray dashed line indicates the V magnitude of the RGBB (≈14.6 mag). (b) Same as (a) but for the [N/Fe] nh  vs. V magnitude. (c) The [C/Fe] ch  vs. [N/Fe] nh  of RGB stars with −2.5 mag ≤ V − V HB ≤ 3.0 mag. (d) The [C/Fe] ch  vs. [N/Fe] nh  of RGB stars fainter than the RGBB, V ≥ 14.6 mag. (e) The [C/Fe] ch  vs. [N/Fe] nh  of MP RGB stars fainter than the RGBB. The blue, gold, and red crosses denote the primordial, intermediate, and extreme subpopulations, respectively. (f) The [C/Fe] ch  vs. [N/Fe] nh  of MR RGB stars fainter than the RGBB. The colors are the same as (e).
Paper: M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population
Authors: Jae-Woo Lee
Figure caption: (a) Metallicity distributions of individual RGB stars with −2.5 mag ≤ V − V HB ≤ 3.0 mag. The blue and red colors denote the MP and MR populations in M92. The measurement uncertainties (±1σ) are shown. We show stars V-45 (open gray circle), XII-8 (open orange triangle), and XI-19 (open green square) studied by Langer et al. (1998). (b) Generalized histograms returned from our EM estimator for each population along with the normalized observed histogram. The blue and red lines are for the MP and MR populations, while the gray line is for the all RGB stars. (c) Cumulative distributions. The MP population is more centrally concentrated than the MR population is.
Paper: M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population
Authors: Jae-Woo Lee
Figure caption: A comparison of our photometric metallicity [Fe/H] hk  to that of high-resolution spectroscopic study by Roederer & Sneden (2011). (a) A plot of our photometric [Fe/H] vs. spectroscopic [Fe/H] by Roederer & Sneden (2011), showing a good correlation with [Fe/H]RS11  ∝ 1.656×[Fe/H] hk . The error bar in the bottom right corner denotes the typical measurement errors in both studies. (b) Residuals around the fitted line against the visual magnitude, showing a substantial gradient. (c) A plot of our photometric [Fe/H] vs. magnitude-gradient-corrected [Fe/H] by Roederer & Sneden (2011), showing [Fe/H]RS11,c  ∝ 0.794×[Fe/H] hk . (d) Residuals around the fitted line against the visual magnitude using (c).
Paper: M92 (NGC 6341) Is a Metal-complex Globular Cluster with an Atypical Primordial Population
Authors: Jae-Woo Lee
Figure caption: (Top) CMDs for proper-motion membership stars in M92. We also show the mean measurement uncertainties at a given V magnitude bin with red error bars. (Bottom) Parallelized CMDs of RGB stars with −2.5 mag ≤ V − V HB ≤ −3.0 mag. In each panel, we show stars V-45 (open gray circles), XII-8 (open orange triangles), and XI-19 (open green squares).
Paper: JWST Reveals a Population of Ultrared, Flattened Galaxies at 2 ≲ z ≲ 6 Previously Missed by HST
Authors: Erica J. Nelson, Katherine A. Suess, Rachel Bezanson, Sedona H. Price, Pieter van Dokkum, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Ivo Labbé, Laia Barrufet, Gabriel Brammer, Daniel J. Eisenstein, Justus Gibson, Abigail I. Hartley, Benjamin D. Johnson, Kasper E. Heintz, Elijah Mathews, Tim B. Miller, Pascal A. Oesch, Lester Sandles, David J. Setton, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Ken-ichi Tadaki, Hannah Übler, John. R. Weaver
Figure caption: Physical Properties. Left: effective (half-light) semimajor radius in F444W vs. stellar mass. The gray points show the F444W sizes from Suess et al. (2022) for 1.0 < z < 2.5 galaxies at M * > 109 M ⊙, and the red symbols show UFOs, which are the subject of this paper. To guide the eye, the black lines show the relationship between half-mass–radius and stellar mass at z ∼ 2 for star-forming galaxies (upper relation) and quiescent galaxies (lower relation) (Suess et al. 2019), and the blue lines show the size–mass relation for S0s and fast rotators from Bernardi et al. (2023). Center: distribution of observed axis ratios and example population models with various intrinsic 3D shapes. Assuming axisymmetry, the UFOs could have intrinsic disk geometries, with the peaked distribution at q ∼ 0.5 caused by a preferential edge-on orientation for these objects. Without this assumption, prolate shapes also provide a reasonable fit to the data. Right: redshifts and stellar masses for the galaxies in our sample in red. Our galaxies have 2 < z < 6 and M * ∼ 1010–1011 M ⊙.
Paper: JWST Reveals a Population of Ultrared, Flattened Galaxies at 2 ≲ z ≲ 6 Previously Missed by HST
Authors: Erica J. Nelson, Katherine A. Suess, Rachel Bezanson, Sedona H. Price, Pieter van Dokkum, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Ivo Labbé, Laia Barrufet, Gabriel Brammer, Daniel J. Eisenstein, Justus Gibson, Abigail I. Hartley, Benjamin D. Johnson, Kasper E. Heintz, Elijah Mathews, Tim B. Miller, Pascal A. Oesch, Lester Sandles, David J. Setton, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Ken-ichi Tadaki, Hannah Übler, John. R. Weaver
Figure caption: Three color images for all of the UFOs in F150W, F200W, and F444W filters, with a 1″ bar indicated. Most of these galaxies are red throughout and consistently elongated. We note that a number of the objects include nearby sources, at least in projection. For two in particular, 8459 and 38,711, there are ambiguous patches with slightly bluer colors that may be associated with the primary objects, but may also be chance superpositions.
Paper: JWST Reveals a Population of Ultrared, Flattened Galaxies at 2 ≲ z ≲ 6 Previously Missed by HST
Authors: Erica J. Nelson, Katherine A. Suess, Rachel Bezanson, Sedona H. Price, Pieter van Dokkum, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Ivo Labbé, Laia Barrufet, Gabriel Brammer, Daniel J. Eisenstein, Justus Gibson, Abigail I. Hartley, Benjamin D. Johnson, Kasper E. Heintz, Elijah Mathews, Tim B. Miller, Pascal A. Oesch, Lester Sandles, David J. Setton, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Ken-ichi Tadaki, Hannah Übler, John. R. Weaver
Figure caption: (Top row): a sample of 29 galaxies (black points and red stars) are selected to be bright at the reddest wavelengths JWST/NIRCam can detect (4.4 μm), and not formally detected at the wavelengths previously visible with HST, namely <1.6 μm (black points). Finally, we isolate the 12 most extended galaxies with a cut on R e  > 0.″17 (extended galaxies indicated by red stars). (Bottom row): an example color image of one extended galaxy (black star in top left panel) to demonstrate that while these objects are nearly or completely invisible HST/WFC3 imaging (bottom left: color composite of F606W, F125W, and F160W), these galaxies are extremely red and prominent in JWST/NIRCam imaging (bottom right: color composite of F150W, F277W, and F444W).
Paper: JWST Reveals a Population of Ultrared, Flattened Galaxies at 2 ≲ z ≲ 6 Previously Missed by HST
Authors: Erica J. Nelson, Katherine A. Suess, Rachel Bezanson, Sedona H. Price, Pieter van Dokkum, Joel Leja, Bingjie Wang, 冰洁 王, Katherine E. Whitaker, Ivo Labbé, Laia Barrufet, Gabriel Brammer, Daniel J. Eisenstein, Justus Gibson, Abigail I. Hartley, Benjamin D. Johnson, Kasper E. Heintz, Elijah Mathews, Tim B. Miller, Pascal A. Oesch, Lester Sandles, David J. Setton, Joshua S. Speagle, 佳士 沈, Sandro Tacchella, Ken-ichi Tadaki, Hannah Übler, John. R. Weaver
Figure caption: Spectral energy distributions (SEDs) spanning from 0.4 to (in some cases) 24 μm. Black points show observed JWST photometry, while gray points show HST and Spitzer photometry. Red shows the best-fit model from parrot. In each case, the SEDs are very red, attributable to a combination of redshift, dust, and age.
Paper: Novel Approach to Forecasting Photospheric Emergence of Active Regions
Authors: S. S. A. Silva, M. Lennard, G. Verth, I. Ballai, E. L. Rempel, J. Warnecke, H. Iijima, H. Hotta, S.-H. Park, A. C. Donea, K. Kusano, V. Fedun
Figure caption: Evolution of the simulated solar surface, z = 0.0 Mm, before and after the AR emergence time, t = 0.0 hr, colored by: (a) continuum intensity, I, normalized by the average of the continuum intensity over the field of view, I  c ; (b) vertical component of the magnetic field, B  z .
Paper: Novel Approach to Forecasting Photospheric Emergence of Active Regions
Authors: S. S. A. Silva, M. Lennard, G. Verth, I. Ballai, E. L. Rempel, J. Warnecke, H. Iijima, H. Hotta, S.-H. Park, A. C. Donea, K. Kusano, V. Fedun
Figure caption: Selected region from the original domain colored by (a) bFTLE field starting at t 0 = − 25 hr for τ = 20 minutes; (b) Same as panel (a), but for τ = 1 hr 40 minutes; (c) fFTLE field starting at t 0 = − 25 hr for τ = 20 minutes; (d) Same as panel (c), but for τ = 1 hr 40 minutes; (e) ridges of the bFTLE field showed in panel (a) superimposed on the v  z  at t = t 0 = − 25 hr; (f) ridges of the bFTLE field showed in panel (b) superimposed on the v  z  at t = t 0 = − 25 hr; (g) ridges of the fFTLE field showed in panel (c) superimposed on the v  z  at t = t 0 = − 25 hr; (h) ridges of the fFTLE field showed in panel (d) superimposed on the v  z  at t = t 0 = − 25 hr.
Paper: Novel Approach to Forecasting Photospheric Emergence of Active Regions
Authors: S. S. A. Silva, M. Lennard, G. Verth, I. Ballai, E. L. Rempel, J. Warnecke, H. Iijima, H. Hotta, S.-H. Park, A. C. Donea, K. Kusano, V. Fedun
Figure caption: Evolution of the simulated solar surface, z = 0.0 Mm, before and after the AR emergence time, t = 0.0 hr, colored by the fFTLE field. The time t 0 indicates the initial time used for the calculation of fFTLE. The white rectangle indicates the location and time of the first local signature prior to the AR emergence.