adsabs/AstroCLIMB huggingface dataset:
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: HELIOS output for 2021 November 19 at 22:30 UT illustrates the global configuration of the HCS and the CME (green points), reconstructed using the GCS model, relative to PSP’s position and the FOV of the WISPR inner telescope. The top-left panel (a) presents the configuration from the perspective of a hypothetical observer located behind PSP, while the bottom-left panel (b) shows a side view along PSP’s orbital plane, looking toward the Sun. The extended CH boundaries are depicted in orange, located beneath the CME. As initially suggested, this configuration—combined with the CME’s propagation nearly parallel to the HCS—likely facilitated the development of KHIs, as discussed in E. Paouris et al. (2024). The right panel (c) shows the CME as observed by WISPR on 2021 November 19 at 22:33 UT. The extent of the CH is overlaid on the WISPR image, highlighting its presence as described in E. Paouris et al. (2024). This supports the initial hypothesis that the ambient solar wind beneath the CME was faster than the CME itself.
Paper: HELIOS: A Visualization Tool to Decipher the Locations and Dynamical Properties of Expanding Small Magnetic Flux Ropes in the Corona
Authors: Evangelos Paouris, Angelos Vourlidas, Guillermo Stenborg
Figure caption: Summary plots showing (a) the blob area derived from ellipse fitting, (b) the ratio of major to minor axis lengths of the ellipse, and (c) the expansion rate, as functions of the heliocentric distance of the ellipse center. Each blob is represented by a distinct symbol and color. In all cases, the blobs exhibit acceleration. All five blobs show a tendency to circularize (axis ratio trending toward unity), increasing the distance from the Sun.
Paper: Active Young Stars in the LAMOST–Kepler Survey
Authors: FuKun Xu, Shenghong Gu, Yue Xiang
Figure caption: rmscont versus Teff for the LRS sample.
Paper: Active Young Stars in the LAMOST–Kepler Survey
Authors: FuKun Xu, Shenghong Gu, Yue Xiang
Figure caption: The Gaia DR3 CMD for identified aYSs (red dots) and the probability distribution of all LAMOST objects with Teff < 7000 K and ﹩\mathrm{log}g﹩> 4.0 (blue contours, using https://seaborn.pydata.org/). The isochrones (dashed lines) and tracks (solid lines), from the PARSEC v1.2s model (A. Bressan et al. 2012) at the solar metallicity, are shown in colors of blue and black corresponding to the cases of 3.5 < ﹩\mathrm{log}g﹩ ≤ 4.0 and ﹩\mathrm{log}g﹩ > 4.0, respectively.
Paper: Active Young Stars in the LAMOST–Kepler Survey
Authors: FuKun Xu, Shenghong Gu, Yue Xiang
Figure caption: Distribution of the EWLi versus Teff for the LRS (a) and the MRS (b) datasets. The points are color coded by the EWHαs and their sizes are proportional to the log(SNR)s. The Li envelopes for some clusters, including the IC 2264 (4 Myr), IC 2602 (30 Myr), Pleiades (78–125 Myr), NGC 3532 (300–399 Myr), Hyades (750 Myr), and NGC 752 (2000 Myr), are shown with lines adopted from P. Sestito et al. (2004) and M. L. Gutiérrez Albarrán et al. (2024).
Paper: Active Young Stars in the LAMOST–Kepler Survey
Authors: FuKun Xu, Shenghong Gu, Yue Xiang
Figure caption: The coincidence of our results (panels (a)–(c)) and the comparison to the literature (panels (d) and (e)). In panels (a)–(c), we depict the coincidence of results for stars with multiple observations based on the LRS and MRS datasets, and the comparison between the different datasets. In panels (d) and (e), the comparison to the MRS results of F22 and to the LRS results of W21 is shown. Records with either eLi > 0.05 Å or eHα > 0.05 Å are hidden for an easier view. The red dashed lines represent one-to-one relationships.
Paper: Active Young Stars in the LAMOST–Kepler Survey
Authors: FuKun Xu, Shenghong Gu, Yue Xiang
Figure caption: Examples for identified “TTS,” “ROT,” “EP,” and “EB” (from top to bottom). For each target, the left panel depicts the LAMOST spectrum (blue), template (red), and residual spectrum+1.05 (black), overlaid by horizontal red dotted lines at 1.0 and 1.05 and vertical black dotted lines denoting the Hα and Li line centers. The middle and right panels show the LC and phase-folded LC, respectively, colored by every 300 days.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: A demonstration of the ability of medium bands to starkly differentiate between z > 15 galaxies and z ∼ 5 interlopers. Starting from the photometry of the CEERS z ≈ 16 candidate (C. T. Donnan et al. 2023) scaled fainter to S/N = 7 in F277W and F356W in our survey field, we perform fits to the Cycle 1 wide-band photometry, first for z ∼ 16 solutions and then for z ∼ 5 solutions, using the Prospector galaxy spectrum modeling code (B. D. Johnson et al. 2021). With the Cycle 1 bands alone, one can get acceptable fits at either redshift (Δχ2 = 0.6); these best-fit smoothed spectra are plotted. We then predict the medium-band photometry from each model. These results clearly distinguish the two hypotheses: the F182M and F210M bands indicate a well-localized break, while the F250M and F300M bands completely exclude the emission lines that the z ∼ 5 solution requires. Our photometric depth yields Δχ2 = 43, an overwhelming confirmation.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: Layout of JADES Cycle 3 observations in the GOODS-South field. Cycle 1 JADES NIRCam imaging observations are shown as the background image. The JOF regions are shown with solid magenta lines. The regions of spectral coverage of the Cycle 3 NIRCam WFSS GRISMC observations are shown as the green shaded area (for complete spectral coverage at 3–5 μm) and as solid orange lines (for partial spectral coverage across 2.4–5 μm), respectively. The dispersion direction of GRISMC is indicated by the gray arrow. To the west of the NIRCam footprints, the coordinated MIRI imaging parallel observations are indicated by the solid orange (F560W), red (F770W and F1000W) and maroon lines (F1500W and F2100W). For comparison we also plot the footprints of CANDELS HST F160W imaging (dotted gray lines; K. E. Whitaker et al. 2019), SMILES MIRI multiwavelength imaging (Cycle-1 GTO 1207; S. Alberts et al. 2024, G. H. Rieke et al. 2024), and FRESCO NIRCam imaging and F444W GRISMR WFSS (P. A. Oesch et al. 2023).
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: We compare two filter strategies in their ability to reject a low-redshift hypothesis for a high-redshift galaxy. The first strategy is the Cycle 1 strategy of program 1210, focused on wide bands. The second strategy is the wide+medium-band strategy adopted with programs 1210 and 3215. We have rescaled the errors from the first strategy so as to match the total exposure time of the second, i.e., 2.68 times what program 1210 actually provides. In both, we take the high-redshift fit from Figure 2 and shift it in redshift, holding the F277W S/N constant (at 7, for the wide+medium strategy). At each true redshift, we fit with Prospector and report Δχ2 between the best low-redshift false solution and the best high-redshift true solution. This quantifies the rejection of the low-redshift hypothesis. We find that at z > 15, the wide+medium strategy provides a clear advantage, nearly 4 times better Δχ2 at fixed exposure time than the strategy of a typical wide-band survey.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: The layout of data sets in the GOODS-S field most immediate to this paper, overlaid on a background F160W image from HST CANDELS (K. E. Whitaker et al. 2019). JADES DR1 and DR2 are shown in green and gray, using the F356W exposure map. The parallel imaging in 1210 is the deepest portion; program 3215 extends this with six medium bands. The location of the 3215 secondary field lies to the northwest; it overlaps other JADES NIRCam imaging from program 1286 (not shown). The NIRSpec MSA footprints for the two 3215 pointings are shown. We also display the footprints of the HUDF ACS field (S. V. W. Beckwith et al. 2006), FRESCO grism (P. A. Oesch et al. 2023, program 1895), and JEMS medium-band (C. C. Williams et al. 2023, program 1963), as these are immediately supportive of the target selection for the 3215 NIRSpec observations. There are many other powerful data sets in this region, not shown for brevity!
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: Exposure maps of the JADES NIRCam F090W, F115W, F150W, F200W, F277W, F335M, F356W, F410M, and F444W imaging. The 1180 Deep program comprises the rectangle in the northeast and 1180 Medium the wider, shallower rectangular exposure area to the southwest. The JADES 1210 imaging of the JOF appears as a deep module pair in the southwest. The F335M filter is only used in 1180 Deep and 1210. The F444W image includes the wide-area FRESCO imaging (P. A. Oesch et al. 2023). Not shown are the F182M and F210M exposure maps from the JEMS (C. C. Williams et al. 2023) and FRESCO program data, or the F430M, F460M, and F480M JEMS imaging.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: A rendering of the JADES GOODS-S data release image, combining filters 0.9–1.9 μm in blue, 2–3 μm in green, and 3–5 μm in red. The green boundary indicates the region new to this release; the yellow boundary indicates the region also in the first JADES release (M. J. Rieke et al. 2023). The region where the imaging is solely from the FRESCO survey (P. A. Oesch et al. 2023) is tinted brown to distinguish it.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: F444W magnitude versus photometric redshift for the galaxies for which shutters were allocated for NIRSpec observations in program 3215. The color coding indicates the exposure time with the prism for each target.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: A small portion of the deep imaging from the JOF, illustrating some of the opportunities of the medium-band data. The background mosaic shows an F444W/F200W/F090W RGB image with three galaxies highlighted. A disk galaxy at redshift z ∼ 1 (center) shows star-forming regions that glow distinctively in various JADES filter combinations. Emission from Hα and [N II] appears as green in an F200W/F150W/F115W RGB image, and Paα appears as red in an F410M/F356W/F335M RGB image. The redshifts of line-emitting galaxies can be easily identified using the JADES medium bands. At z ∼ 6, Hβ + [O III] appear as green in an F356W/F335M/F277W RGB image. At z∼5, the presence of Hβ + [O III] in F277W, Hα in F356W, and no strong line in F335M will cause a line-emitting galaxy to appear purple in an F356W/F335M/F277W RGB image. As is common in JWST mosaics of data taken at multiple position angles, chip gaps in some of the input images produce disjoint diffraction spikes in the bright star at the top.
Paper: The JADES Origins Field: A New JWST Deep Field in the JADES Second NIRCam Data Release
Authors: Daniel J. Eisenstein, Benjamin D. Johnson, Brant Robertson, Sandro Tacchella, Kevin Hainline, Peter Jakobsen, Roberto Maiolino, Nina Bonaventura, Andrew J. Bunker, Alex J. Cameron, Phillip A. Cargile, Emma Curtis-Lake, Ryan Hausen, Dávid Puskás, Marcia Rieke, Fengwu Sun, Christopher N. A. Willmer, Chris Willott, Stacey Alberts, Santiago Arribas, William M. Baker, Stefi Baum, Rachana Bhatawdekar, Stefano Carniani, Stephane Charlot, Zuyi Chen, Jacopo Chevallard, Mirko Curti, Christa DeCoursey, Francesco D'Eugenio, Anna de Graaff, Eiichi Egami, Jakob M. Helton, Zhiyuan Ji, Gareth C. Jones, Nimisha Kumari, Nora Lützgendorf, Isaac Laseter, Tobias J. Looser, Jianwei Lyu, Michael V. Maseda, Erica Nelson, Eleonora Parlanti, Bernard J. Rauscher, Tim Rawle, George Rieke, Hans-Walter Rix, Wiphu Rujopakarn, Lester Sandles, Aayush Saxena, Jan Scholtz, Katherine Sharpe, Irene Shivaei, Charlotte Simmonds, Renske Smit, Michael W. Topping, Hannah Übler, Giacomo Venturi, Christina C. Williams, Joris Witstok, Charity Woodrum
Figure caption: The depth in the F115W, F200W, and F356W bands, expressed as the 5σ AB magnitude for a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15 radius aperture, measured from the rms scatter from empty regions of the mosaic and corrected for the point-source curve of growth. We quote this aperture for comparison with R23 and previous HST work, but we note that a 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩1 aperture yields yet deeper limits, by about 0.3 mag in F200W.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: Two examples of plotting all identified flare events on the corresponding light curves. The color of the points on the light curve represents the average prediction values of the 10 CNN models, with the color bar indicating the corresponding values. The color mapping in Figure 1 is the same as the color bar in Figure 4. The vertical green dashed lines mark the peak times of the corresponding flares. Flares identified near gaps through traditional flare identification methods but not processed by the CNN models (true flares with CNN prediction values less than 0.5) are also marked in the figures, such as the first flare on the two segments of the light curve in the upper panel.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: Two flare events identified through the flare search method described in this paper. The two panels on the left depict the location of a single flare on the light curve, with data points in different colors representing the average prediction values of the CNN models. The two panels on the right provide the corresponding zoomed-in views of the flares, where red points indicate the confirmed flare and blue points represent the stellar background flux.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: An example of a flare originating from the target source. This figure reproduces the results of Figure 1 from the work by Z.-L. Tu et al. (2022), including the flare flux variation (first row, two subplots), the pixel brightness changes at the preflare and flare peak moments (first two subplots in the second row), and the pixel-level light-curve variations (last two subplots in the second row).
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: An example of a flare originating from a faint nearby source rather than the target star. The content of each subplot is the same as in Figure 2.
Paper: Properties of Flare Quasiperiodic Pulsations Based on a New TESS Flare Catalog
Authors: Yinpeng Wang, Li-yun Zhang, Tianhao Su, Prabhakar Misra, Xianming L. Han
Figure caption: An example of identifying QPPs in the flare sample of this work using the method provided by S. A. Belov et al. (2024). The first column in the figure represents the data file of an individual flare, the second column shows the confidence values of QPP events predicted by the FCN model, the third column indicates whether the event is classified as a QPP, and the fourth column provides the corresponding flare profile.