adsabs/AstroCLIMB huggingface dataset:
Paper: Adaptive Weighted Multi-image Shape from Shading for Precise Topographic Reconstruction at the Lunar South Pole
Authors: Zhen Ye, Jia Qian, Yusheng Xu, Hong Zhang, Tao Tao, Rong Huang, Shijie Liu, Huan Xie, Xiaohua Tong
Figure caption: Surface slope maps for the MI-AW-SFS DEM (panels (a) and (c)) and LOLA DEM (panels (b) and (d)) for experimental data sets 1 and 2.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Insolation flux vs. planet mass, with the Hot Neptune Desert (T. Mazeh et al. 2016) labeled on the left. Small black dots are confirmed exoplanets; large dots colored by planet radius are confirmed planets with mass (or M﹩\sin (i)﹩) and radius uncertainties <10% and bright host stars (J < 9). A rough outline of the Hot Neptune Desert is designated by the gray triangular region (to guide the eye only, not to serve as a sharp delineation). WASP-166b (large and labeled “W”) is on the edge of the desert. LTT 9779b (“L”) is deep within the desert and labeled for comparison; see Section 5.2 for further discussion.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Examples of the Eureka! (T. J. Bell et al. 2022) Stage 5 spectroscopic light curves and dynesty (J. S. Speagle 2020) fits for the NIRSpec G395M constant (∼0.01797 μm) bin-width data reduction. Left panel: data corrected with polynomial systematics models (colored points), and overplotted with the best-fit transit models (black curves). Wavelengths for each spectral channel are shown above the corresponding transit light curve. Right panel: residuals for the corresponding data, with rms scatter in black text. Data and best-fit transit curves are offset for each spectral channel for clarity.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: The spectral decomposition of the Reference retrieval (R1) of WASP-166b with the absorption contributions of the key atmospheric constituents shown. Our reduced NIRISS and NIRSpec observational data (fixed 0.01797 μm bins) are plotted as gray circles and “x” markers, respectively. Post-retrieval, we have subtracted the median transit depth offset value (14.4 ppm) for the plotted NIRISS SOSS data (the NIRSpec data are the relative zero anchor). Spectra are plotted at R = 100 for clarity. The combined forward model, shown as a heavy black line, is the median Reference retrieval (R1) result (see Table 5). The colored lines correspond to the individual opacity/absorption contributions (including Rayleigh scattering and collision absorption) of the various constituent molecules and clouds at specific wavelengths. (H2S is plotted but is not distinguishable from the bulk species line.) The transmission spectrum is dominated by contributions from H2O (15.2σ), and CO2 (14.7σ). The more subtle effects of NH3 (2.3σ) may be apparent at ∼2.3 μm, and possibly at ∼3.9 μm. The effects of the cloud deck (dashed gray line at a transit depth of ∼2740 ppm) are apparent in clipping the troughs of the water features from 0.85–1.7 μm.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectrum from POSEIDON equilibrium chemistry retrieval (E1). Top panel: observational data shown for NIRISS SOSS (orange circles) and NIRSpec G395M (blue squares), for the case of fixed (0.01797 μm) bins. The retrieval is using an isothermal P–T profile with an opaque cloud deck. The 31 molecular species that are included in our POSEIDON equilibrium chemistry model are shown in Table 2. The plotted NIRISS data have been adjusted down (post-retrieval) by a small retrieved instrument offset (see plotted δrel value). The median retrieved spectrum for this case is shown as a fine black line with the 1σ and 2σ confidence intervals shown in dark- and light-gray shading, respectively. Bottom-left panel: residuals between observational data and retrieval model from the top panel plot. Bottom-right panel: histogram of residuals for each instrument wavelength range, with orange for NIRISS data and blue for NIRSpec data.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectrum from POSEIDON Baseline free chemistry retrieval (B1). Top panel: observational data shown for NIRISS SOSS (orange circles) and NIRSpec G395M (blue squares), for the case of fixed (0.01797 μm) bins. The retrieval is using an isothermal P–T profile with an opaque cloud deck. Fill gases (H2 and He) are present at the primordial solar ratio. The trace gases H2O, CO2, and NH3 are included in the model. The plotted NIRISS data have been adjusted down (post-retrieval) by a small retrieved instrument offset (see plotted δrel value). The median retrieved spectrum for this case is shown as a fine black line with the 1σ and 2σ confidence intervals shown in dark- and light-gray shading, respectively. Bottom-left panel: residuals between observational data and retrieval model from the top panel plot. Bottom-right panel: histogram of residuals for each instrument wavelength range, with orange for NIRISS data and blue for NIRSpec data.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Examples of our Eureka! (T. J. Bell et al. 2022) Stage 5 spectroscopic light curve emcee (D. Foreman-Mackey et al. 2013) fits to the NIRISS SOSS Ahsoka data reduction for constant (∼0.01797 μm) bin widths. Left panel: data corrected with polynomial systematics models (colored points), and overplotted with the best-fit transit models (black curves). Wavelengths for each spectral channel are shown above the corresponding transit light curve. Right panel: residuals for the corresponding data, with rms scatter in black text. Data and best-fit transit curves are offset for each spectral channel for clarity.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: The aligned spectral trace and residual background are shown as part of the Eureka! Stage 3 reduction of the NIRSpec data set. The background region is outside the bg8 lines (solid orange), and the spectral extraction aperture is inside the ap4 lines (dashed green). Outlier pixels can be seen with certain bad pixels identified via the CRDS shown in black. The color bar on the far right is a one-to-one mapping of the flux value (x-axis) in the right panel.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for POSEIDON Reference retrieval case, R1.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Trace Curvature. The measured (blue points), smoothed (yellow line), and integer-rounded (green points) relative position of the spectral trace on the NIRSpec G395M (NRS1) detector determined with the Eureka! data reduction and analysis pipeline (T. J. Bell et al. 2022). The majority of the measured (blue) data agree closely with the smoothed (yellow) line. Significant curvature is evident; however, the aspect ratio of the plot is significantly compressed along the horizontal/column axis.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for POSEIDON equilibrium chemistry case, E1.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for POSEIDON Baseline retrieval case, B1.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Eureka! (T. J. Bell et al. 2022) Stage 5 white light curve emcee (D. Foreman-Mackey et al. 2013) fit to the NIRISS SOSS Ahsoka data reduction. The top panel shows the Order 1 data corrected with the polynomial systematics model (blue points), and overplotted with the best-fit transit model (black curve). The center panel indicates residuals with rms scatter in black text. Mean error bars in the top and center plots are 146 ppm. The bottom panel shows the histogram distribution of residuals in terms of number of standard deviations σ overplotted with a Gaussian curve of the same mean and standard deviation as the residuals. The Gaussian trend of our distribution indicates the systematics are well managed.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Comparison of NIRISS SOSS 1D stellar spectra (flux vs. wavelength) before (top) and after (bottom) correcting for 5σ outliers. Stellar spectra for all integrations are overplotted, with each individual stellar spectrum plotted in partially transparent color, such that the most opaque region corresponds to the expected stellar spectrum, while the more transparent regions indicate outlying values of flux. An excessive number of outliers were evident in the stellar spectra from our initial box extraction (top). These outliers are no longer visible after our correction (bottom).
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Median image of our NIRISS SOSS F277W integrations. The F277W filter blocks those wavelengths ≲2.6 μm, and thus allows only the longest wavelengths of the order 1 spectrum to be dispersed upon the subarray. These longest wavelengths are visible left of column 500. The F277W exposure may be used to find the locations of any order 0 field star contaminants, which would appear as bright chevron shapes if present. Our observations have no significant order 0 contaminants.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: NIRISS SOSS raw white light curve for the 30 pixel width nirHiss box extraction before (left) and after (right) correcting the stellar spectra for 5σ outliers. We normalized the flux for each integration by the median flux of the out-of-transit integrations. For this computation, we used integration indices [0, 1750] and [4000, 4835] as the out-of-transit points.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: 1D spectrum, with flux vs. absolute pixel position for an arbitrarily chosen early integration (in this case Integration 4) in our NIRSpec data set. We use the “Optimal” spectrum (K. Horne 1986) shown in green, although it is almost an exact match to the Standard spectrum, shown in orange. The vertical spikes along the spectral profile indicate suspect pixel columns that were, in some cases, masked in Stage 4.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Broadband (white) light curve from our NIRSpec observation of WASP-166b, showing the fitted central transit time (t0), and showing the exposure-long downward linear trend in normalized flux (−137 ppm hr−1). We saw no other indication of unusual events or trends in the light curve.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Comparison of the NIRISS SOSS CRDS spectral trace, the PASTASOSS-derived spectral trace, and the PASTASOSS trace shifted by 10 pixels, all overplotted on our BadPix output frame from integration 0. A portion of Order 2 is visible near the top center of SUBSTRIP96. The PASTASOSS trace shifted vertically by 10 pixels aligns best with our data.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for POSEIDON Reference retrieval case, R3, with CO and SO2 added to the Baseline model. We see some hints of SO2, but it is very poorly constrained.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Posterior distributions of free parameters (corner plot) for POSEIDON Reference retrieval case, R2, with Na and K added to the Baseline model. We see some faint hints of Na, but it is very poorly constrained.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectra from POSEIDON free chemistry retrievals, based on the NIRISS SOSS data set alone (B3; top panels) and based on the NIRSpec data set alone (B4; bottom panels). Top panel: observational data shown for NIRISS SOSS (orange circles) for the case of fixed (0.01797 μm) bins. The retrieval is using an isothermal P–T profile with an opaque cloud deck. Fill gases (H2 and He) are present at the primordial solar ratio. The trace gases H2O, CO2, and NH3 are included in the model. The median retrieved spectrum for this case is shown as a fine black line with the 1σ and 2σ confidence intervals shown in dark- and light-gray shading, respectively. Below the primary top panel is a smaller panel with residuals between observational data and retrieval model, with an orange histogram of NIRISS residuals on the right. Retrieval results are as expected; they show that the water abundance and cloud-top pressure are similar to the Baseline (B1) values, but that the CO2 abundance is understated, and NH3 is missed altogether. Bottom panel: same as the top panel, but the observational data shown is for NIRSpec G395M (blue squares) for the case of fixed (0.01797 μm) bins. Retrieval results are as expected. Water is seen but at a lower abundance than the Baseline (B1). Since we are missing the shorter-wavelength data, the cloud effects are not captured, leaving the cloud-top pressure essentially unconstrained. The CO2 is reasonably well captured, and NH3 appears slightly higher in abundance than the Baseline. Again, below the primary bottom panel is a smaller panel with residuals between observational data and retrieval model, with a blue histogram of NIRSpec residuals on the right.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectrum from TauREx free chemistry retrieval (B6). We used the same free parameter priors (see Table 4) here as in the POSEIDON Baseline retrieval case (B1). Top panel: observational data shown for NIRISS SOSS (orange circles) and NIRSpec G395M (blue squares), for the case of fixed (0.01797 μm) bins. The retrieval is using the native TauREx “isothermal” P–T profile with the TauREx opaque cloud deck model. Fill gases (H2 and He) are present at the primordial solar ratio (same ratio as used by POSEIDON, ﹩{X}_{{\rm{He}}}/{X}_{{{\rm{H}}}_{2}}﹩ = 0.17). The trace gases H2O, CO2, and NH3 are included in the model. Since TauREx does not directly retrieve an instrument offset, the actual data was adjusted here (all NIRISS transit depth values had the estimated B1 retrieval offset of ∼8.4 ppm subtracted). Posteriors of the free parameters for this case are compiled in Table 8. The median retrieved spectrum for this case is shown as a fine black line with the 1σ confidence interval shown in dark-gray shading. Bottom-left panel: residuals between observational data and retrieval model from the top panel plot. Bottom-right panel: histogram of residuals for each instrument wavelength range, with orange for NIRISS data and blue for NIRSpec data.
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: Top three panels: the signal power ﹩{ \mathcal S }﹩, noise rms ﹩{ \mathcal N }﹩, and the resulting signal-to-noise ratio (﹩{ \mathcal S }/{ \mathcal N }﹩) recovered as a function of the coordinates of the delay center for pulsar B2310+42 calibrated to J0117+8928. With the basic correlator (black curves), the sensitivity drops significantly at around ﹩\pm \,\rm{20}^{\prime} ﹩, which corresponds to a half-integer residual delay of Δt/2. Using the S/N2 search correlator (green; Equation (46)), the sensitivity can be recovered near the integer lag boundaries. Bottom panel: We plot the signal and noise power ratios ﹩({ \mathcal S }/{{ \mathcal S }}_{0})﹩ and ﹩({ \mathcal N }/{{ \mathcal N }}_{0})﹩ as well as the S/N ratio (﹩({ \mathcal S }/{ \mathcal N })/{({ \mathcal S }/{ \mathcal N })}_{0}﹩) to reduce the pointing-to-pointing sample variance in the top three panels, finding a ≈30% improvement at half-integer delays fully consistent with our simulations. This demonstrates our ability to mitigate the sensitivity losses arising from upstream PFB windowing effects.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: Retrieved P–T profile for the atmosphere of WASP-166b using the POSEIDON 2-parameter “gradient” model (B2). The observational data for this case has been reduced to fixed 0.01797 μm bins. As with the Baseline (B1) case, the fill gases, H2 and He are present at the primordial solar ratio. Trace gas abundances for H2O, CO2, and NH3, as well as cloud-top pressure are free parameters in the retrieval. There is a retrieved transit depth offset between the instruments of ∼11 ppm. The median temperature (dark-purple line) is consistent with the Baseline isothermal temperature of 697 K (white dashed line) at low pressures, but there is a small increase in temperature at pressures above ∼0.01 mbar. The temperature is very poorly constrained in the deep atmosphere.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectrum from POSEIDON free chemistry retrieval; the observational data are for the case of constant R = 100 binning (B5). Top panel: observational data shown for NIRISS SOSS (orange circles) and NIRSpec G395M (blue squares). The retrieval is using an isothermal P–T profile with an opaque cloud deck. Fill gases (H2 and He) are present at the primordial solar ratio. The trace gases H2O, CO2, and NH3 are included in the model. The plotted NIRISS data have been adjusted down (post-retrieval) by a small retrieved instrument offset (see plotted δrel value). The median retrieved spectrum for this case is shown as a fine black line with the 1σ and 2σ confidence intervals shown in dark- and light-gray shading, respectively. Bottom-left panel: residuals between observational data and retrieval model from the top panel plot. Bottom-right panel: histogram of residuals for each instrument wavelength range, with orange for NIRISS data and blue for NIRSpec data.
Paper: A VLBI Software Correlator for Fast Radio Transients
Authors: Calvin Leung, Shion Andrew, Kiyoshi W. Masui, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Victoria Kaspi, Kholoud Khairy, Adam E. Lanman, Mattias Lazda, Juan Mena-Parra, Gavin Noble, Aaron B. Pearlman, Mubdi Rahman, Pranav Sanghavi, Vishwangi Shah
Figure caption: We show the delay autocorrelation function Gd (defined formally later in Equation (20)) calculated from cross-correlation visibilities computed before (blue) and after (red) applying the fractional sample correction in VLBI observations on the CHIME-KKO baseline of a Crab giant pulse (left) and the NCP source (right). This validates our implementation of the fractional sample correction part of our delay compensation.
Paper: Detection of H2O and CO2 in the Atmosphere of the Hot Super-Neptune WASP-166b with JWST
Authors: Andrew W. Mayo, Charles D. Fortenbach, Dana R. Louie, Courtney D. Dressing, Emma V. Turtelboom, Steven Giacalone, Caleb K. Harada
Figure caption: WASP-166b transmission spectrum from PLATON equilibrium chemistry retrieval (E2). Top panel: observational data shown for NIRISS SOSS (orange circles) and NIRSpec G395M (blue squares), for the case of fixed (0.01797 μm) bins. The retrieval is using an isothermal P–T profile with an opaque cloud deck, and 31 molecular species (M. Zhang et al. 2020). The plotted NIRISS data have been adjusted down (post-retrieval) by a small retrieved instrument offset (see plotted δrel value). The median retrieved spectrum for this case is shown as a fine black line with the 1σ confidence interval shown in dark-gray shading. Bottom-left panel: residuals between observational data and retrieval model from the top panel plot. Bottom-right panel: histogram of residuals for each instrument wavelength range, with orange for NIRISS data and blue for NIRSpec data.