adsabs/AstroCLIMB huggingface dataset:
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The top panel shows the synchrotron spectral index map computed from the coeval F560W and F1130W MIRI images. The map is shown on a linear scale with the index scale bar running along the bottom. The ejecta filaments have very flat indices and appear black in the image. The plot in the bottom panel shows the average surface brightness value within the white circular aperture shown in the top panel, a region chosen to avoid filament emission. The uncertainties on the values are dominated by photometric calibration uncertainties. The black line is a power-law model with a best-fit index of α = 0.47 ± 0.10.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: Density diagnostic line ratios in [Fe II] at temperature T = 2400 K (solid), T = 1350 K (long dashed), and T = 4270 K (short dashed). Long and short dashed horizontal lines come from the red and blue velocity components of filament 1, and the dotted and solid horizontal lines come from the red1 and red2 velocity components of filament 2, respectively (see Table 2). All ratios indicate electron density in the range ≃1000–3000 cm−3 for T = 2400 K.
Paper: The Six-planet Resonant Chain of HD 110067
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: The solid curve shows the cumulative unstable fraction of the 1400 HD 110067–like resonant chain systems. The dashed and dotted curves, respectively, show the cumulative unstable fraction of the 278 systems that contain a low-mass planet and the 206 systems that contain a high-eccentricity orbit (i.e., systems with masses or eccentricities outside of the limits reported in Table 2). Systems that contain a low-mass or high-eccentricity planet are significantly more likely to destabilize on long timescales, allowing us to place approximate lower limits on planet masses and upper limits on orbital eccentricities for the HD 110067 system.
Paper: The Six-planet Resonant Chain of HD 110067
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Distributions of three-body resonant angle values in our 1251 stable HD 110067–like resonant chain systems at the outset of the N-body simulations. Horizontal dashed lines mark the observed values, based on measured transit times. For all of the three-body resonant angles except ϕ bcd, the observed value falls comfortably within the range of resonant angles in our simulated resonant systems.
Paper: The Six-planet Resonant Chain of HD 110067
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Transit timing variations (TTVs) over 3000 days for three HD 110067–like resonant chain systems. The predicted TTVs typically evolve over timescales of thousands of days. The predicted amplitudes vary widely across our simulated systems, with a median peak-to-peak amplitude of ﹩{7}_{-6.7}^{+15}﹩ hr.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The top panel shows the position 2 MRS spectrum with the F1800W and F2100W filter transmission curves overlaid and the different emission components shaded in different colors. The brightest lines contributing to the two filters are labeled. The bar chart in the bottom panel shows the contribution of the corresponding emission components to the total surface brightness in the F1800W and F2100W filters within the MRS field of view at position 2 (first two columns). It also shows the contribution of emission components to the weighted residual of the two filters (third column), where Residual = F2100W − 0.65 × F1800W. The dust map (fourth column) is given by subtracting the synchrotron component from the residual (Residual − Synchrotron), and the [S III] image (fifth column) is given by [S III] = F2100W − Synchrotron − 1.65 × Dust. See Section 3.1 for details.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: This figure shows color composites produced from the MIRI line emission images (see Section 3.1). The [O III] emission shown in the top panel was obtained in 1999–2000 with the WFPC2 instrument on board HST (Loll et al. 2013) and does not align on fine scales with the JWST images. See Section 4 for details.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: MIRI MRS spectra from the two observed positions centered on the ejecta filament in the equatorial region (position 1 in orange) and the southern filament (position 2 in blue). The two positions are shown in Figure 1. The detector artifacts that affect the shape of the spectrum are discussed in Section 2.2.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: This image shows the F480M image of the Crab Nebula in blue that traces the PWN’s synchrotron emission and the dust emission map in red. The white arrows indicate the locations of indentations in the PWN that resemble the larger “bays” in the east and west equatorial regions that have been noted previously.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: Enlarged regions on the composite image shown in Figure 6. The [S III] emission is shown in red-orange, [Fe II] emission in blue, dust emission in yellow-white and green, and synchrotron emission from the PWN in smoky white.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: STScI and NASA press release image of the Crab Nebula containing all MIRI and NIRCam images. The composite image shows the [S III] emission in red-orange, [Fe II] emission in blue, dust emission in yellow-white and green, and synchrotron emission from the PWN in smoky white. The colors assigned to different filters are blue (F162M), light blue (F480M), cyan (F560W), green (F1130W), orange (F1800W), and red (F2100W). Credit: NASA, ESA, CSA, STScI, T. Temim, J. DePasquale.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: A color-composite image with the warm dust component from JWST shown in blue and the Herschel 70 μm image dominated by cooler dust shown in pink. We note that the spatial resolution of the JWST/MIRI image of warm dust has a factor of 8 times higher spatial resolution than the Herschel/PACS image (PSF FWHM of 0.″674 vs. 5.″6).
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The NIRCam F480M image of the Crab Nebula shown here is dominated by synchrotron emission from the PWN and has only a minimal contribution from the ejecta filaments. The image is shown on a log scale to maximize the dynamic range. The size of the mosaicked image is 4.′9 × 5.′5, and the orientation is north up.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The left panel shows the original F2100W image that contains synchrotron, [S III], and dust emission. The middle and right panels show the maps of warm dust and [S III] emission that have been derived from the synchrotron-subtracted F1800W and F2100W images (see Section 3.1).
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The NIRCam (panel (a)) and MIRI (panel (b)) imaging mosaic footprints are overlaid in blue on the Spitzer 24 μm image of the Crab Nebula. Panel (c) shows the footprints of the MIRI MRS observations (small yellow squares), along with the fields of view of the two MIRI imaging observations taken simultaneously with the MRS (blue).
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The extraction aperture for position 1 (white rectangle) plotted on images of emission lines in each of the 12 MRS subband cubes. The subband labels and species are shown in the top left-hand corner of each panel. The white lines in the bottom right of each panel represent 1′′ to highlight the increasing size of the field of view from subbands 1A–4C. The decreased spatial resolution from channels 1–4 due to the diffraction limit is also evident. North is up, east is left.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: MIRI two-tile mosaics composed of images observed simultaneously with the MRS and the three-color image that combines all three filters. The position of the footprint relative to the entire Crab Nebula is shown in Figure 1(c). The size of each of the two MIRI mosaic tiles is 1.′2 × 1.′9.
Paper: Dissecting the Crab Nebula with JWST: Pulsar Wind, Dusty Filaments, and Ni/Fe Abundance Constraints on the Explosion Mechanism
Authors: Tea Temim, J. Martin Laming, P. J. Kavanagh, Nathan Smith, Patrick Slane, William P. Blair, Ilse De Looze, Niccolò Bucciantini, Anders Jerkstrand, Nicole Marcelina Gountanis, Ravi Sankrit, Dan Milisavljevic, Armin Rest, Maxim Lyutikov, Joseph DePasquale, Thomas Martin, Laurent Drissen, John Raymond, Ori D. Fox, Maryam Modjaz, Anatoly Spitkovsky, Louis-Gregory Strolger
Figure caption: The NIRCam and MIRI imaging mosaics of the Crab Nebula with the dominant emission components listed in Table 1. The size of each mosaic is 4.′9 × 5.′5, and they are oriented with north up.
Paper: Imprint of “Local Opacity” Effect in Gamma-Ray Spectrum of Blazar Jet
Authors: Sushmita Agarwal, Amit Shukla, Karl Mannheim, Bhargav Vaidya, Biswajit Banerjee
Figure caption: (a) 14 days binned light curve of ≈15 yr of Fermi-LAT observation of PKS 1424−418. The gray region represents high state and white represents low state. (b) The combined spectrum of all “flaring” and “quiescent” epochs marked in panel (a). Intrinsic spectrum is modeled with a log-parabola model up to 10 GeV (solid line with envelope) and then extrapolated up to ∼300 GeV (dotted lines). The significance of detection (﹩\sqrt{{TS}}﹩) for each energy bin is mentioned over the respective bins.
Paper: Imprint of “Local Opacity” Effect in Gamma-Ray Spectrum of Blazar Jet
Authors: Sushmita Agarwal, Amit Shukla, Karl Mannheim, Bhargav Vaidya, Biswajit Banerjee
Figure caption: Observed γ-ray spectrum in 0.1–100 GeV range for the high state and low state. The true intrinsic spectrum in the energy range of 0.110–GeV extrapolated up to 100 GeV for the high and low state is shown in gray dashed and dotted–dashed lines, respectively. The solid red and blue envelope represents the intrinsic high-state and low-state spectrum, respectively, after EBL attenuation using opacity scaling factor (b) ranging from 0.75 to 1.25 across different models indicated in each panel. The mean value of the fit corresponding to b = 1 is indicated by a black dashed line. The quoted reduced χ 2 in each panel is for the mean fitting corresponding to b = 1.
Paper: Imprint of “Local Opacity” Effect in Gamma-Ray Spectrum of Blazar Jet
Authors: Sushmita Agarwal, Amit Shukla, Karl Mannheim, Bhargav Vaidya, Biswajit Banerjee
Figure caption: Orbit-binned light curve of a period of fastest variability in Fermi-LAT of PKS 1424−418. Bayesian Blocks with a false alarm probability of 5% indicating significant points of change are plotted on top. The periods of significant variability are marked with gray dotted lines.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Spitzer-IRS medium resolution spectra obtained from archival data. The blue line shows the spectrum extracted on the science target (AOR 22848256) offset by 0.2 Jy for clarity. The orange line is the spectrum of the dedicated background observation (AOR 22848512). Numerous sharp lines are seen. The strongest lines attributed to the amino acid Trp by IG23 in the OFF spectrum are indicated with vertical gray lines. The green spectrum shows the result of ON–OFF (offset by 0.2 Jy), showing that many lines disappear including those attributed to Trp. The panels below show expansions of the data centered around the wavelengths of the signals attributed to Trp by IG23 (gray dashed lines). Broad features observed at ∼11.2, 12.7, and 16.4 μm are due to PAHs.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Observed spectra of the PRIMOS observations (blue trace) toward Sgr B2(N) near the reported rest frequencies of Trp. Vertical marks near the center of each panel correspond to the Trp laboratory rest frequencies report in Table S2 of Sanz et al. (2014). Transition quantum numbers (without hyperfine splitting and quadrupole coupling) are given in the top left of each panel. Nearby transitions belonging to radio recombination lines (red vertical marks) are labeled.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Comparison of the Spitzer-IRS archival spectrum of IC 348 (orange) with our laboratory spectrum of Trp isolated in p-H2 (blue) and Trp in KBr pellets (red) from the NIST Chemistry WebBook. The wavelengths of the features attributed to Trp by IG23 are shown in the gray dashed lines. The Spitzer spectrum (orange) is of the dedicated background observation (AOR 22848512). Zoomed-in panels are centered around the features attributed to Trp by IG23.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Top: JWST-MIRI IFU spectrum of IC 348. Nearby transitions corresponding to atomic and molecular H2 lines are indicated by vertical colored bars. Bottom: zoomed-in panels of the MIRI spectrum of IC 348 at the wavelengths of the lines reported by IG23 and attributed to Trp.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Structure of L-tryptophan (Trp). In wedge-dash notation, the dark triangle indicates that the amine (-NH2) group is coming out of the page toward the reader. The carbon next to the carboxyl (-COOH) group is called the α carbon, followed by the β carbon and γ carbon.
Paper: On the Origin of Infrared Bands Attributed to Tryptophan in Spitzer Observations of IC 348
Authors: Aditya Dhariwal, Thomas H. Speak, Linshan Zeng, Amirhossein Rashidi, Brendan Moore, Olivier Berné, Anthony J. Remijan, Ilane Schroetter, Brett A. McGuire, Víctor M. Rivilla, Arnaud Belloche, Jes K. Jørgensen, Pavle Djuricanin, Takamasa Momose, Ilsa R. Cooke
Figure caption: Averaged post-BCD frames of the IRS Short-high (SH) observations of IC 438 at OFF position (left) used by the authors and ON position (right). Spectral features of H2 (17 μm) and PAHs (11.2 μm) are clearly seen. Several bright “rogue pixels” of the detector are present in both observations, demonstrating the need to subtract the OFF from the ON position to remove the emission from these pixels.
Paper: Probing the Distinct Extinction Law of the Pillars of Creation in M16 with JWST
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, Jian Gao, 健 高, Xi Chen, 曦 陈
Figure caption: Comparison of the reddening law in M16 with the literature results. Our derived color excess ratios (red points) are plotted alongside results from Weingartner & Draine (2001, WD01) for R  V  = 3.1 in blue dashed and R  V  = 5.5 in blue solid, and from Hensley & Draine (2020, HD20 Cyg OB2-12) in green dashed and Hensley & Draine (2023, HD23 Astrodust) in green solid, respectively. The inset is a zoom-in view of the MIR regime.
Paper: Probing the Distinct Extinction Law of the Pillars of Creation in M16 with JWST
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, Jian Gao, 健 高, Xi Chen, 曦 陈
Figure caption: Color–color diagrams of F090W − λ vs. F090W − F200W for all sources within the Pillars of Creation in M16. Panels display λ = F187N (top left), F335M (top right), F444W (lower left), and F770W (lower right). The red solid lines represent the best-fit linear models to the color indices for each band using LTS_LINEFIT. The 3σ confidence intervals of these fits are indicated by red dashed lines. Outliers are marked as gray points. Best-fit slopes are annotated in the upper left corner of each panel.
Paper: Probing the Distinct Extinction Law of the Pillars of Creation in M16 with JWST
Authors: Jun Li, 军 李, Bingqiu Chen, 丙秋 陈, Biwei Jiang, 碧沩 姜, Jian Gao, 健 高, Xi Chen, 曦 陈
Figure caption: Color–magnitude diagrams for all identified sources within the Pillars of Creation in M16, depicted as black points. Each panel displays data obtained with a different filter λ plotted against the color index F090W − F200W, where λ includes F090W, F187N, F200W, F335M, F444W, and F770W. The total number of sources in each filter is indicated in the upper right corner of each panel.