adsabs/AstroCLIMB huggingface dataset:
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Comparison of the 11.2 μm PAH feature in T Cha’s continuum-subtracted spectra from different epochs (left) and the 11.2 μm PAH feature normalized to its peak amplitude (right): Spitzer SH (blue) in 2004, Spitzer SL (black) in 2005, and JWST/MIRI (red) in 2022. Left: all spectra plotted in absolute flux units, revealing a factor of ∼3 increase in feature strength in the JWST epoch compared to the two Spitzer observations. Right: the same data normalized to the peak flux of the PAH feature, showing no appreciable change in profile shape.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Location of T Cha observed by JWST (black star) and Spitzer (brown triangle) on the PAH charge–size diagnostic grid constructed using data from A. Maragkoudakis et al. (2020). The grid shows model tracks for PAH populations with varying neutral-to-cation ratios (colored curves), and dashed gray curves indicate PAH sizes. T Cha lies outside the model grid at both epochs, suggesting a low ionization fraction (75% neutral) and small PAH sizes, with NC < 30 based on extrapolation from the nearest model tracks.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Gaussian decomposition of the 6 μm PAH emission in T Cha. The median-filtered spectrum is shown in black. The colored lines indicate individual Gaussian components, and the red line marks the total fitted model. The lower panel plots residuals (data minus model). The primary emission peak at 6.273 μm is significantly shifted relative to the more commonly reported 6.2 μm feature, characteristic of border class B/class C PAH spectra.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Comparison of the JWST/MIRI MRS spectrum of T Cha (red) with two Spitzer/IRS data sets: the 2004 SH module (blue) and the 2005 SL module (black). The 2005 data cover the 5–15 μm range, while the 2004 SH observation starts at 10 μm. The “seesaw” effect is evident, with the JWST continuum showing diminished flux below 10 μm but enhanced emission at longer wavelengths, compared to the 2005 Spitzer spectra. Forbidden lines ([Ar II], [Ar III], [Ne II], [Ne III]) and the main PAH bands are marked with vertical dashed lines.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Continuum-subtracted mid-IR spectra of T Cha from JWST/MIRI (red) and archival Spitzer SL observations (black). Top panel: continuum-subtracted spectral comparison showing prominent emission features between 5 and 14 μm in both JWST and Spitzer. Bottom panel: same spectra normalized to the peak of the 11.2 μm PAH feature, emphasizing the ratios have not changed significantly over the 18 yr timescale.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Continuum-subtracted JWST/MIRI (left panel) and Spitzer (right panel) spectra of T Cha highlighted with integrated PAH regions. The final flux in the 12.7 μm PAH band is estimated after the subtraction of fitted [Ne II] flux in the case of the JWST spectrum.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Variation of the 6.2 μm peak position (left) and the 6.0/6.2 ratio (right) with Teff for T Cha and reference stars.
Paper: When the Wall Fell: Study of Polycyclic Aromatic Hydrocarbons in T Chamaeleontis Using JWST
Authors: R. Arun
Figure caption: Continuum-subtracted ISAAC L-band spectrum of T Cha highlighting 3.3 μm integrated PAH regions taken from V. C. Geers et al. (2007).
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Selected pixels inside a dense area in Region A (top two panels) and a diffuse area in Region B (bottom two panels). The α means from Monte Carlo resampling, with the labeled pixel and pixel number in red, is shown on the left column, while the power-law fit is shown on the right. The mean and median of the Monte Carlo simulated distributions are given as the solid and dotted lines, respectively. The 68% confidence band of the Monte Carlo distribution is shown in blue.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: AV, ﹩{R}_{\widetilde{VI}}﹩, and α distributions (filled histograms) from regions A, B, and C (regions shown in Figure 8) of VV 191b. Region A most resembles a typical spiral arm, Region B is similar to a tendril branch of a spiral arm, and Region C is the edge of the galaxy disk. The best-fit model of the pdf of the distributions of the entire overlap of VV 191b (see Figure 6) is overlaid in black, scaled to roughly match the histogram peaks of the three regions.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Regions of predominantly noise for AV (top) and EV−F090W = AV − AF090W (bottom), shown to demonstrate the distribution of these respective values when no expected signal is present. The chosen areas of noise (in red) are well outside the outer arms of VV 191b and on the back side of the background elliptical galaxy, VV 191a. The right column shows the distribution of the low-S/N pixels. Both show a near-Gaussian distribution centered at zero. It is calculated that ﹩{A}_{V}^{{\mathrm{mean}}}=-0.01﹩, ﹩{\sigma }_{{A}_{V}}=0.05﹩, ﹩{E}_{V-{{\rm{F}}}090{{\rm{W}}}}^{{\mathrm{mean}}}=-0.003﹩, and σEV−F090W = 0.09 for these selected regions shown in red. Thus, the lower-limit threshold used in the Monte Carlo simulation, such that AV and EV−F090W ≤ 0.1 must equal 0.1, is a reasonable choice.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: Top left: the modeled foreground spiral galaxy, VV 191b, determined by effectively subtracting out the modeled background elliptical galaxy. One can see the subtle outline of the background elliptical in this image. A radius of ∼14 kpc is overlaid in dotted black to show the extent of the rms annular profile. Top right: the JWST F090W image of VV 191 with the sampled sky with low S/N used to calculate its rms outlined in red. Bottom left: the annular rms profile of VV 191. Each annulus has a bin width of 5 pixels. Bottom right: histogram of the sigma-clipped sky region whose sample is shown above in the F090W image. The units are in megajanskys per steradian.
Paper: Mapping Interstellar Dust in the Foreground Outer Disk of Overlapping Galaxy Pair VV 191 with HST and JWST
Authors: Clayton D. Robertson, Benne W. Holwerda, Jessica M. Berkheimer, Trevor Butrum, Ian Castellano, Kyle W. Cook, William C. Keel, Anton M. Koekemoer, Divya Patel, Maria del Carmen Polletta, Rogier A. Windhorst
Figure caption: The attenuation from the long-wavelength filters from JWST/NIRCam, AF356W and AF444W, over the same area of overlap as all the other dust maps. The Petrosian radius (RP = 12 kpc) is overlaid in black.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Example data for three Kepler stars with high SNR (top panels, KIC  ID 4554810), moderate SNR (middle panels, KIC  ID 11673802), and low SNR (bottom panels, KIC  ID 12314973). Column A: critically sampled power density spectrum (in units of ppm2 μHz−1). The blue band is centered on the pySYD’s estimated νmax value. Column B: background-corrected power density spectrum in linear scale centered on pySYD’s estimate of νmax. Column C: autocorrelation function of the data shown in column B. The blue line corresponds to the expected Δν value given the input νmax, and the red dotted line corresponds to the measured Δν using pySYD’s analysis. Column D: Échelle diagram of the background-corrected power spectrum (shown in column B) using pySYD’s measurement of Δν.
Paper: Gravity-sensitive Spectral Indices in Ultracool Dwarfs: Investigating Correlations with Metallicity and Planet Occurrence Using SpeX and Fire Observations
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Julien de Wit, Jan Toomlaid, Michaël Gillon, Amaury H. M. J. Triaud, Adam J. Burgasser, Christopher A. Theissen
Figure caption: ECDF plots for eight gravity indices, comparing stars with and without detected planets using the Kolmogorov–Smirnov (KS) test. Each panel shows the ECDFs for the two samples, with the KS statistic (D) indicated by a solid vertical line representing the maximum vertical difference between the distributions. Panel (a) shows FeHz, where a significant difference is observed between the two groups, as indicated by the larger KS statistic. For all other indices, including FeHJ, VOz, K IJ, and metallicity, the distributions do not show significant differences (p > 0.05). The x-axis represents the spectral index values, and the y-axis represents the cumulative probability.
Paper: Gravity-sensitive Spectral Indices in Ultracool Dwarfs: Investigating Correlations with Metallicity and Planet Occurrence Using SpeX and Fire Observations
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Julien de Wit, Jan Toomlaid, Michaël Gillon, Amaury H. M. J. Triaud, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Gravity indices (FeHz, FeHJ, K IJ and H-cont) vs. NIR spectral type for M dwarfs in our sample. The color-coded regions represent different gravity classifications: Very Low Gravity (VL-G, pink), Intermediate Gravity (INT-G, green), and Field Gravity (FLD-G, purple). SPECULOOS-2 (S2), SPECULOOS-3 (S3), LHS 3154 (L), and the FIRE and SpeX spectra measurements of TRAPPIST-1 (T1F and T1S) are highlighted as red stars.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: Comparison of νmax (top row) and Δν (bottom panel) measurements from this work and previous catalogs, including A. Serenelli et al. (2017), W. J. Chaplin et al. (2014), S. Mathur et al. (2022), L. A. Balona (2020), D. Huber et al. (2013), M. S. Lundkvist et al. (2016), and others (summarized in Section 2.1). The bottom panel of each subplot shows the residuals.
Paper: A Homogeneous Catalog of Oscillating Solar-type Stars Observed by the Kepler Mission and a New Amplitude Scaling Relation Including Chromospheric Activity
Authors: Maryum Sayeed, Daniel Huber, Ashley Chontos, Yaguang Li
Figure caption: H-R diagram showing 765 stars with detected oscillations in white circles, new detections in blue, planet hosts in yellow, and new planet hosts in orange. The complete Kepler sample is shown in gray for reference, using stellar parameters from T. A. Berger et al. (2020b).
Paper: Gravity-sensitive Spectral Indices in Ultracool Dwarfs: Investigating Correlations with Metallicity and Planet Occurrence Using SpeX and Fire Observations
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Julien de Wit, Jan Toomlaid, Michaël Gillon, Amaury H. M. J. Triaud, Adam J. Burgasser, Christopher A. Theissen
Figure caption: EWs for the K I lines in the J band vs. NIR spectral type for M dwarfs in our sample. The figure elements are the same as in Figure 3. The panels display: (a) NIR spectral type vs. K I 1.169 μm EW, (b) NIR spectral type vs. K I 1.177 μm EW, and (c) NIR spectral type vs. K I 1.253 μm EW.
Paper: Gravity-sensitive Spectral Indices in Ultracool Dwarfs: Investigating Correlations with Metallicity and Planet Occurrence Using SpeX and Fire Observations
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Julien de Wit, Jan Toomlaid, Michaël Gillon, Amaury H. M. J. Triaud, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Near-IR SpeX/SXD spectra (R ∼ 2000) of the M dwarfs in our sample. Spectral types and positions of significant gravity-sensitive features are indicated. These spectra are publicly available on Zenodo, DOI: 10.5281/zenodo.16420633.
Paper: Gravity-sensitive Spectral Indices in Ultracool Dwarfs: Investigating Correlations with Metallicity and Planet Occurrence Using SpeX and Fire Observations
Authors: Fatemeh Davoudi, Benjamin V. Rackham, Julien de Wit, Jan Toomlaid, Michaël Gillon, Amaury H. M. J. Triaud, Adam J. Burgasser, Christopher A. Theissen
Figure caption: Near-IR FIRE spectra (R ∼ 6000) of the M dwarfs in our sample. Spectral types and positions of significant gravity-sensitive features are indicated. These spectra are publicly available on Zenodo, DOI: 10.5281/zenodo.16420633.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Similar to Figure 6, but shown for all spectral templates that included a single opacity source at an artificially high chemical abundance of ﹩{{\rm{log}}}_{10}{\rm{VMR}}=-4﹩.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Similar to Figure 6, but shown for all the atmospheric species with an artificial exoplanet signal injected at a velocity offset of Δvsys = ΔKp = −30 km s−1 at nominal scale a = 1. Recovery of the injected signal depends on the atmospheric species involved, where titanium (Ti) and iron (Fe) have the highest-S/N detections at the injected velocity offset.
Paper: First Results from WINERED: Detection of Emission Lines from Neutral Iron and a Combined Set of Trace Species on the Dayside of WASP-189 b
Authors: Lennart van Sluijs, Emily Rauscher, Eliza M.-R. Kempton, Thomas Kennedy, Isaac Malsky, Noriyuki Matsunaga, Michael Meyer, Andrew McWilliam, John D. Monnier, Shogo Otsubo, Yuki Sarugaku, Tomomi Takeuchi
Figure caption: Similar to Figure 17, but shown for all spectral templates that included a single opacity source at an artificially high chemical abundance of ﹩{{\rm{log}}}_{10}{\rm{VMR}}=-4﹩.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: TNO discovery completeness by absolute magnitude for the nonresonant subpopulations. There is no size range on which most subpopulations have discovery completeness near 100%. TNOs do not complete a large fraction of their orbits in 10 yr, so many eccentric scattering and detached objects that would be easily observed at perihelion stay at high distances throughout the survey. Meanwhile, high-inclination members of the hot classical population can stay farther north than LSST observes for the entire survey. Cold Classicals, with circular, low-inclination orbits, all lie within the survey footprint and reach high completeness for Hr < 6.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Cumulative distribution of detections by band for MBAs, as in Figure 7. LSST will produce catalogs of Jupiter Trojans with hundreds of detections, and even the least-observed objects usually still have several detections in griz.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: The differential number density and cumulative number of MBAs (top and bottom panels, respectively), analogous to Figure 5. Loss of completeness at the bright end is due to the mr ∼ 16 saturation limit assumed for the LSST camera. Nearly all MBAs with 12.5 ≲ Hr ≲ 17 will have well-determined colors, while about 75% of objects with 12.5 ≲ Hr ≲ 15 will have sufficient observations for high-quality light curves.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Model TNOs by absolute magnitude, similar to Figure 5. Due to the cut made on apparent magnitude at perihelion, the “simulated objects” population shown in blue does not strictly increase with Hr, despite our model having a strictly increasing size distribution.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Cumulative distribution of detections by band for NEOs. Note the change in x-axis scale to display the tail of the overall detection distribution. Most objects receive only a few dozen detections, and small objects are not always detected in the u, g, or y bands.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Cumulative distribution of detections by band for Trojans, as in Figure 7. LSST will produce catalogs of Jupiter Trojans with hundreds of detections (median), and even the least-observed objects usually still have several detections in gri.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: The differential number density and cumulative number of Jupiter Trojans (top and bottom panels, respectively). The Trojan population is generally very well-measured, with large size ranges receiving high discovery completeness, color completeness, and light-curve completeness.
Paper: Predictions of the LSST Solar System Yield: Near-Earth Objects, Main Belt Asteroids, Jupiter Trojans, and Trans-Neptunian Objects
Authors: Jacob A. Kurlander, Pedro H. Bernardinelli, Megan E. Schwamb, Mario Jurić, Joseph Murtagh, Colin Orion Chandler, Stephanie R. Merritt, David Nesvorný, David Vokrouhlický, R. Lynne Jones, Grigori Fedorets, Samuel Cornwall, Matthew J. Holman, Siegfried Eggl, Drew Oldag, Maxine West, Jeremy Kubica, Peter Yoachim, Joachim Moeyens, Kathleen Kiker, Laura E. Buchanan
Figure caption: Cumulative distribution of detections by band for TNOs, analogous to Figure 7.
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: The final F444W image produced via classical RDI optimized for extended source emission retrieval (FULL and Subarray combined), shown at a larger field of view to include the outer ring in the left hand panel and zoomed in to the inner regions in the right panel. While the outer ring is not detected in our observations, the inner regions exhibit a marginal (1σ), low level of asymmetric extended emission. The background sources are “doubled” where the FULL images overlap that were taken 6 months apart).
Paper: Searching for Planets Orbiting ϵ Eridani with JWST/NIRCam
Authors: Jorge Llop-Sayson, Charles Beichman, Geoffrey Bryden, Marie Ygouf, Andras Gaspar, William Thompson, Aniket Sanghi, Dimitri Mawet, Tiffany Meshkat, Alexandra Z. Greenbaum, Jarron Leisenring, Schuyler Wolff, Marcia Rieke, George Rieke
Figure caption: Contrast curves comparing the performance of the 3-roll strategy (black) with respect to pair-wise combinations (blue) from the same data set. These observations of ϵ Eridani were the first to test a three-roll observation strategy. The three-roll combination performs generally better beyond the inner working angle of the coronagraph (vertical line). However, the gains are modest: the three-roll curve never outperforms all three two-roll combinations by a wide margin. At small separations, the small roll angle differences result in self subtraction, which favors the pair-wise combinations over the three-roll combination.