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Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Understanding the details of the MZR is fundamental for theories of galaxy evolution. Left: arrows show that (1) metal abundance increases with the nucleosynthetic yields of star formation, (2) accretion of metal-poor gas both dilutes metals and can trigger star formation, and (3) outflows remove enriched gas with an efficiency that is inversely proportional to the galaxy gravitational well. The purple line and swath show the MZR and its scatter measured from synthetic NIRISS spectra, derived from our simulations: NGDEEP will significantly extend the MZR mass coverage by ∼2 dex. Right: the diversity in the evolution of the MZR slope predicted by simulations with different assumptions about feedback (with color scheme as in the left panel); NGDEEP will measure this slope and scatter and thereby constrain the physics of feedback.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: Full simulated NGDEEP-NRC F277W 22.3 hr mosaic, displaying the footprint of the proposed observations, including all instrumental effects and sensitivities. The main input for this simulation is the ultradeep Santa Cruz SAM light cone (Yung et al. 2022). The central inset zooms in on a 10.″7 region, demonstrating the increase in depth compared with CEERS. On the upper left we show composite NGDEEP-NRC images of z = 1.5 and z = 3 galaxies from the VELA simulation (Simons et al. 2019), with faint tidal features (indicated by white dashed lines) clearly detected in the planned exposure times. By resolving low-mass galaxies at early times, NGDEEP will probe a new frontier in galaxy assembly. On the lower left we show 2″ postage stamps of two massive galaxies at z = 4 generated from the SIMBA simulation (Davé et al. 2019), with the NGDEEP-NRC images on top and stamps of the same sources imaged at the CEERS depth on the bottom. Extended emission and complicated morphologies are evident in all filters at the NGDEEP-NRC depth. We also show 1″ postage stamps of four z > 9.5 galaxies, again compared with CEERS imaging, highlighting the power of NGDEEP-NRC imaging to detect m > 30 galaxies to z = 13.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: The layout of NGDEEP. The background grayscale image is the exposure time map of HST/ACS F814W imaging, shown with logarithmic scaling as given by the scale bar. The NGDEEP NIRISS (NGDEEP-NIS) pointing is shown by the magenta region (in the HUDF), while NGDEEP NIRCam (NGDEEP-NRC) is shown by the red regions (in the HUDF-Par2 parallel field). Extremely deep HST/ACS F435W imaging exists in the HUDF (Illingworth et al. 2013), achieving depths of 29.6 AB mag (5σ; Illingworth et al. 2013), while the deepest HST/ACS F814W imaging anywhere in the sky is in the HUDF-Par2 field. The inset tables show our expected line flux sensitivities for NGDEEP-NIS and continuum sensitivities for NGDEEP-NRC. The image inset shows a portion of the ACS F435W imaging, with sources near the detection limit indicated by white boxes. At z = 2 the m 435 magnitudes correspond to rest-frame UV magnitudes of M UV = −16.7, or an unattenuated SFR of 0.12 M ⊙ yr−1 (Kennicutt & Evans 2012). This SFR would produce Hα fluxes detectable by our NIRISS spectroscopy.
Paper: The Next Generation Deep Extragalactic Exploratory Public (NGDEEP) Survey
Authors: Micaela B. Bagley, Nor Pirzkal, Steven L. Finkelstein, Casey Papovich, Danielle A. Berg, Jennifer M. Lotz, Gene C. K. Leung, Henry C. Ferguson, Anton M. Koekemoer, Mark Dickinson, Jeyhan S. Kartaltepe, Dale D. Kocevski, Rachel S. Somerville, L. Y. Aaron Yung, Bren E. Backhaus, Caitlin M. Casey, Marco Castellano, Óscar A. Chávez Ortiz, Katherine Chworowsky, Isabella G. Cox, Romeel Davé, Kelcey Davis, Vicente Estrada-Carpenter, Adriano Fontana, Seiji Fujimoto, Jonathan P. Gardner, Mauro Giavalisco, Andrea Grazian, Norman A. Grogin, Nimish P. Hathi, Taylor A. Hutchison, Anne E. Jaskot, Intae Jung, Lisa J. Kewley, Allison Kirkpatrick, Rebecca L. Larson, Jasleen Matharu, Priyamvada Natarajan, Laura Pentericci, Pablo G. Pérez-González, Swara Ravindranath, Barry Rothberg, Russell Ryan, Lu Shen, Raymond C. Simons, Gregory F. Snyder, Jonathan R. Trump, Stephen M. Wilkins
Figure caption: NGDEEP-NIS WFSS Simulations. Bottom left: the NIRISS grism covers a wide range of emission lines over a wide range of redshifts. Bottom right: zoomed-in simulated WFSS observations using the F115W cross filter where emission lines are clearly visible. The insets show full images and the region in F115W that is zoomed in. All known instrumental and WFSS-related effects are included in the simulated data. Top: the GRISMR (orange) and GRISMC (green) extracted NIRISS spectra of a galaxy at z = 2.21 with F(Hα)  =  10−17 erg s−1 cm−2 (S/N = 22), 107.7 M ⊙. We will measure σ > 5 emission lines in over 1500 galaxies in the HUDF.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: Simulated acceleration parameters X(z) based on the future DECIGO, and the corresponding uncertainties σ  X  are shown in gray. The inset figure shows the effect of binning. Red bars represent the weighted mean of X(z) in redshift bins of width Δz = 0.1 with the corresponding uncertainties. The black solid line with the corresponding blue uncertainty band displays the ANN-reconstructed X(z) relation. The advantage of binning is noticeable.
Paper: Comprehensive Analysis of a Filament-embedding Solar Active Region at Different Stages of Evolution
Authors: Jie Zhao, Fu Yu, Sarah E. Gibson, Yuhong Fan, Yang Su, Ying Li, Jun Dai, Hui Li, Chuan Li, Pengfei Chen, Ming-De Ding, Cheng Fang
Figure caption: Spectroscopic observations from IRIS are displayed at different time ranges. A sit-and-stare model is carried out for the observations in the top three panels. The FOV of the slit-jaw imager (SJI) is displayed for 2796 Å as a vertical red line in the left panels, and the evolution of the obtained Doppler velocity at the location of the slit are displayed in the top right panels, with time on the X-axis. A 16-step raster scanning mode is carried out for the observations as shown in the bottom panels. The FOV of the SJI is shown as a black vertical line in the left panel (d1) in 1400 Å, and the scanning results are displayed in the right panels in (d2). The intensity in the scanning region are displayed in the left five panels from chromosphere to the corona in 2796 Å (∼104.15 K), C II (∼104.4 K), Si IV 1394/1403 Å (∼104.9 K), and Fe XII (∼106.2 K); the Doppler velocities obtained through the shift of the line center (k3) as well as the blue (k2v) and red peak (k2r) of Mg II k line are displayed in the following three panels respectively, and the velocity gradient of the upper chromosphere (Δv  k3 –Δv  h3) is shown next. The Si IV line ratio, which is usually used to indicate the plasma opacity, is shown in the last panel. The intensity enhancement in the south part of the sigmoidal filament is annotated with plus signs in the panels in (d2).
Paper: Comprehensive Analysis of a Filament-embedding Solar Active Region at Different Stages of Evolution
Authors: Jie Zhao, Fu Yu, Sarah E. Gibson, Yuhong Fan, Yang Su, Ying Li, Jun Dai, Hui Li, Chuan Li, Pengfei Chen, Ming-De Ding, Cheng Fang
Figure caption: Panels (a1)–(a2) show the vector magnetic field, with vertical magnetic field (B ver) in the background and the horizontal field (B hor) overlaid on top as arrows. Red arrows show B hor at positive polarity, and blue arrows show B hor at negative polarity. Pink and green contours of ±5 G of the B ver are overlaid. Horizontal flows at the photosphere obtained from DAVE4VM are displayed in panels (b1)–(b2) with purple arrows showing the velocity at positive polarity and green arrows at the negative polarity. Gray and black contours of ±100 G of the B ver are also overlaid. Same vertical magnetic field and the contours of ±5 G of the B ver as in panels (a1) and (a2) are shown in panels (c1) and (c2). Rectangle boxes in white show the regions around PIL where the magnetic flux is calculated. The magnetic flux evolution during February 14–15 is displayed in panel (d); points in pink and green show the positive and negative magnetic flux respectively.
Paper: Comprehensive Analysis of a Filament-embedding Solar Active Region at Different Stages of Evolution
Authors: Jie Zhao, Fu Yu, Sarah E. Gibson, Yuhong Fan, Yang Su, Ying Li, Jun Dai, Hui Li, Chuan Li, Pengfei Chen, Ming-De Ding, Cheng Fang
Figure caption: Overview of the observations on February 14 (panels (a1)–(f1)) and 15 (panels (a2)–(f2)). Hα line center images from NVST and CHASE are displayed in panels (a1)–(a2) and (b1)–(b2), respectively. Panels (c1)–(c2) show the images from AIA/304 Å, and Doppler velocities obtained from CHASE are displayed in panels (d1)–(d2). The contours show the LOS magnetic field (B los) with threshold values of ±100 G. Doppler velocity and AIA/171 Å with a larger FOV are shown in panels (e1)–(e2) and (f1)–(f2), respectively.
Paper: Discovery of a Rare Eclipsing Be/X-Ray Binary System, Swift J010902.6-723710 = SXP 182
Authors: Thomas M. Gaudin, Jamie A. Kennea, M. J. Coe, I. M. Monageng, Andrzej Udalski, L. J. Townsend, David A. H. Buckley, Phil A. Evans
Figure caption: Truncated OGLE IV, Swift UVOT, and Swift XRT light curves for Swift J010902.6-723710 showing emission from MJD 60100 to MJD 60300. The times of optical eclipse, calculated using Equation (1), are shown as vertical gray lines. Blue arrows show the calculated XRT flux upper limit during S-CUBED observations where Swift J010902.6-723710 is not detected.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: Magnetic amplification rate as a function of RI fraction. The color scale represents the Alfvén Mach number of the shocks. The black squares are binned density averages with associated standard error within each bin shown with error bars. The histogram in the background shows the number of events in each bin. Data points are distinguished by upside-down triangle and circle markers for the analysis method based on “RI Track” and “SW Subtract,” respectively.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: Ion reflection rate as a function of Alfvén Mach number. Data are color coded by the upstream plasma temperature. The black squares are averages of binned densities. The associated standard error within each bin is shown with error bars. The horizontal dashed line is drawn at n RI/n  U  = 1.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: Simulation results for the density of RIs n  p,ref normalized by the mean upstream solar wind density ﹩\left\langle {n}_{p,\mathrm{SW}}\right\rangle ﹩, as a function of distance x upstream of the shock ramp. Panels are as follows: (a) comparison of the density of RIs to the density of inflowing solar wind ions for the run U6T65, (b) comparison of the normalized density of RIs for all of the simulations, and (c) magnetic field strength in the shock layer for run U6T65 at a single time step, showing upstream enhancements and nonplanar shock morphology.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: An example of spacecraft measurements of a quasiperpendicular shock for which we track the RIs (“RI Track”) in the FPI FOV. Panels show time series data of (a) magnetic field strength and components in GSE coordinates, (b) ion energy flux spectrogram, (c) ion energy flux in the polar angle (θ) in the FPI FOV, and (d) ion energy flux along the azimuth ϕ. The shock layer is at 16:43:55 UT. On panel (c) we mark the FOV angles associated with RIs with white rectangles, which are used in calculation of partial moments. The solar wind beam is evident at θ ∼ 0°.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: The distribution of the Earth’s bow shock crossing events. The events are projected on the XY plane of the geocentric solar ecliptic (GSE) coordinates, in which the +X-axis is toward the Sun, the +Y-axis points opposite to the planetary orbital motion, and the +Z-axis completes the right-hand triple. Nominal bow shock (dashed line) and magnetopause (solid line) boundaries are shown for reference (Farris & Russell 1994; Shue et al. 1998). The axes are in units of Earth radii (R E).
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: RI temperatures as a function of upstream ion plasma temperature. Both axes are in units of electronvolt (eV). The linear fit on the data (blue line) and 95% confidence intervals (red lines) are overplotted with the fit function annotated in blue. The R 2 goodness of fit is 0.506. RI temperatures can be obtained for “RI Track” events only.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: An example of spacecraft measurements of a quasiperpendicular shock for which we track the solar wind beam and subtract it from the total ion density to obtain the RI densities (“SW Subtract”). The format of the figure is similar to Figure 7. The shock layer is at 12:01:06 UT for this event. A substantial overlap between the solar wind ion beam and nonsolar wind ions is evident in panels (c) and (d). In panel (d) we mark the angles associated with the solar wind beam with white dashed rectangles, which are used in calculation of partial moments.
Paper: Drivers of Magnetic Field Amplification at Oblique Shocks: In Situ Observations
Authors: Hadi Madanian, Imogen Gingell, Li-Jen Chen, Eli Monyek
Figure caption: Magnetic amplification rate as a function of P Dyne./P  B  (1/σ). Data points are color coded by the upstream plasma temperature. Events with low upstream plasma temperatures occur in weaker magnetic field strengths.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: The 2D plots and 1D marginalized distributions with 1σ and 2σ contours of the cosmological parameters (H 0 and Ω k ) from the simulated QSO and GW data. Dashed lines represent the fiducial parameters that we used in our simulation, i.e., H 0 = 67.4 km s−1 Mpc−1 and Ω k  = 0.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: The precision on Ω k  as a function of the number of simulated QSOs. The blue polyline represents the free H 0 parameter case. The red polyline represents the fixed H 0 = 67.4 km s−1 Mpc−1 parameter case. For the illustration of the uncertainty floor observed, standard statistical ﹩1/\sqrt{N}﹩ curves have been overplotted.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: The precision on H 0 as a function of the number of simulated QSOs. The blue polyline represents the case of the free Ω k  parameter. The red polyline represents the case of the fixed Ω k  = 0 parameter. For the illustration of the uncertainty floor observed, standard statistical ﹩1/\sqrt{N}﹩ curves have been overplotted.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: 1D and 2D marginalized probability distributions of H 0 and Ω k  as in Figure 3 but corresponding to doubling the uncertainties from the GW or QSO data, respectively, while keeping the other unchanged. Dashed lines represent the fiducial parameters that we used in our simulation, i.e., H 0 = 67.4 km s−1 Mpc−1 and Ω k  = 0.
Paper: Model-independent Way to Determine the Hubble Constant and the Curvature from the Phase Shift of Gravitational Waves with DECIGO
Authors: Tonghua Liu, Shuo Cao, Marek Biesiada, Yilong Zhang, Jieci Wang
Figure caption: Simulated sample of 1000 angular size measurements of ultracompact structure in radio quasars from the future VLBI observations.
Paper: NICER, NuSTAR, and Insight-HXMT Views to Black Hole X-Ray Binary SLX 1746–331
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Yu-Peng Chen, Ling-Da Kong, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Ming-Yu Ge, Jin-Lu Qu, Lian Tao, Zhi Chang, Jian Li, Zhao-sheng Li, Zhe Yan
Figure caption: The light curve of SLX 1746–331 for NICER 1–10 keV during the 2023 outburst. The three red bars represent the three NuSTAR observations. The yellow bar represents the Insight-HXMT observation.
Paper: NICER, NuSTAR, and Insight-HXMT Views to Black Hole X-Ray Binary SLX 1746–331
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Yu-Peng Chen, Ling-Da Kong, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Ming-Yu Ge, Jin-Lu Qu, Lian Tao, Zhi Chang, Jian Li, Zhao-sheng Li, Zhe Yan
Figure caption: The disk unabsorbed flux (1–100 keV) vs. the disk inner temperature (T in). Flux is found to correlate with temperature in the form of proportional ﹩{T}_{\mathrm{in}}^{3.974\pm 0.003}﹩. The red points represent the results of the joint fit.
Paper: NICER, NuSTAR, and Insight-HXMT Views to Black Hole X-Ray Binary SLX 1746–331
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Yu-Peng Chen, Ling-Da Kong, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Ming-Yu Ge, Jin-Lu Qu, Lian Tao, Zhi Chang, Jian Li, Zhao-sheng Li, Zhe Yan
Figure caption: The simultaneous broadband spectrum of SLX 1746–331 is observed from NICER (black), NuSTAR/FPMA (red), and NuSTAR/FPMB (green).
Paper: NICER, NuSTAR, and Insight-HXMT Views to Black Hole X-Ray Binary SLX 1746–331
Authors: Jing-Qiang Peng, Shu Zhang, Qing-Cang Shui, Shuang-Nan Zhang, Yu-Peng Chen, Ling-Da Kong, Zhuo-Li Yu, Long Ji, Peng-Ju Wang, Ming-Yu Ge, Jin-Lu Qu, Lian Tao, Zhi Chang, Jian Li, Zhao-sheng Li, Zhe Yan
Figure caption: The NICER hardness–intensity diagram of SLX 1746–331, where the hardness is defined as the ratio of 6–10 to 1–6 keV count rate.
Paper: Comprehensive Analysis of a Filament-embedding Solar Active Region at Different Stages of Evolution
Authors: Jie Zhao, Fu Yu, Sarah E. Gibson, Yuhong Fan, Yang Su, Ying Li, Jun Dai, Hui Li, Chuan Li, Pengfei Chen, Ming-De Ding, Cheng Fang
Figure caption: Overview of AR 12946 on 2022 February 15. Intensity images of AIA/171, 193, 335 Å are displayed in the top panels. Emission measures at different temperature ranges, i.e., 0.7–0.9 MK and 2.5–3.2 MK, are displayed in middle panels and bottom panels, respectively. Three-dimensional magnetic field lines of different systems are overlaid at the emission measure plots. The gray contours with a value of 0 G are from the Gaussian-smoothed magnetogram to show the PIL.
Paper: Comprehensive Analysis of a Filament-embedding Solar Active Region at Different Stages of Evolution
Authors: Jie Zhao, Fu Yu, Sarah E. Gibson, Yuhong Fan, Yang Su, Ying Li, Jun Dai, Hui Li, Chuan Li, Pengfei Chen, Ming-De Ding, Cheng Fang
Figure caption: Different FOVs are displayed in the top panel for the following demonstrations: DEM analysis (green box), CHASE Doppler velocity analysis (blue box), NVST observations (red box), DAVE4VM analysis (purple box), and IRIS observations (white rectangle). The background is AIA/171 Å image on 2022 February 15. Time coverage of observations from NVST (green), CHASE (pink), and IRIS (blue) on 2022 February 14–15 is displayed in the bottom panel.
Paper: The Optical to Infrared 0.6–5.3 μm Dust Extinction Law of the Milky Way with JWST NIRSpec: Westerlund 2
Authors: Shu Wang, Xiaodian Chen
Figure caption: The distribution of RMSE with different prior α for 1251 extinction pairs, where RMSE is the minimum rms error of each extinction pair.