adsabs/AstroCLIMB huggingface dataset:
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: Sample of Gaussian fits (solid orange) to molecular lines in normalized EXES spectra (solid black) toward NGC 7538 IRS 1 for A-type CH3OH (top row), E-type CH3OH (second row), the ν5 band of C2H2 (third row), and the ν4 + ν5 band of C2H2 (bottom row). All CH3OH lines displayed belong to the 2ν12 band. We have overlaid the vLSR systemic to IRS 1 (dotted green, −58.5 km s−1; G. Sandell et al. 2020), and those of the binary protostars IRS 1a and IRS 1b (dashed purple, −59.50; and dashed–dotted pink, −56.39 km s−1; L. Moscadelli & C. Goddi 2014). Note the different y-axis scales for CH3OH and C2H2.
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: Rotation diagrams for A-type (top left) and E-type (top right) CH3OH; ortho (center left) and para (center right) states of the ν5 band of C2H2; and ortho (bottom left) and para (bottom right) states of the ν4 + ν5 band of C2H2. The ν12 band CH3OH are the transitions with El/kB > 600 K and 2ν12 band CH3OH with El/kB < 500 K. The P, Q, and R branch transitions are indicated with purple triangles, yellow squares, and blue circles, respectively.
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: Several CH3OH lines in normalized flux as observed by EXES toward NGC 7538 IRS 1. Transition labels are indicated, all of which are 2ν12 and A-type, except Q14R1, which is E-type. Note the two blended lines. There are no telluric lines present in this plot. Other features are instrumental noise.
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: The colored boxes represent the beam configurations for EXES observations described in Table A1. The grayscale map of the NGC 7538 IRS 1 region is SOFIA/FORCAST archival data at 25.3 μm, as described in Figure 1.
Paper: The Discovery of 25 μm Interstellar Methanol
Authors: Sarah L. Nickerson, Naseem Rangwala, Keeyoon Sung, Xinchuan Huang, Edward J. Montiel, Curtis DeWitt, Valentin J. M. Le Gouellec, Sean W. J. Colgan, Jason Dittmann, José Pablo Fonfría, Graham M. Harper, Kathleen E. Kraemer, Jialu Li, Conor A. Nixon, Maisie Frances Rashman, Clara Sousa-Silva, Alexander G. G. M. Tielens, William D. Vacca
Figure caption: Curve of growth plots for absorption lines measured by SOFIA/EXES toward NGC 7538 IRS 1 for separate CH3OH and C2H2 groups.
Paper: Magnetic Webs in Stellar Radiative Zones
Authors: Valentin A. Skoutnev, Andrei M. Beloborodov
Figure caption: Evolution of the rotation period of the envelope Pe (black curve) and the core Pc (colored curves) in a 1.6M⊙ star. On the horizontal axis, we use the growing radius of the star R⋆ as a proxy for its age. The stellar model includes AM transport by the magnetic web and turbulent transport outside the web (Tayler–Spruit dynamo model). Two evolution histories (red and green) are calculated assuming different values for the convective overshoot parameter fov. The dotted portions of the curves indicate the late evolutionary phase when the web is completely buried in the growing helium core below the hydrogen burning shell. The models are compared with asteroseismic data for Pc (B. Mosser et al. 2012; C. Gehan et al. 2018), indicated by the blue shaded region.
Paper: Magnetic Webs in Stellar Radiative Zones
Authors: Valentin A. Skoutnev, Andrei M. Beloborodov
Figure caption: Schematic picture of a red giant hosting a magnetic web deposited during MS evolution. The magnetic web encloses the helium core and the lower radiative mantle, enforcing their corotation. The web-free, upper radiative mantle is free to rotate differentially, with a profile of Ω(R) regulated by turbulent transport. Surrounding the mantle is a large, slowly rotating, convective envelope.
Paper: Magnetic Webs in Stellar Radiative Zones
Authors: Valentin A. Skoutnev, Andrei M. Beloborodov
Figure caption: A 1.6M⊙ stellar model with a magnetic web spanning the mass shells 0 ≤ m ≤ mt = 0.23M⊙ (hatched) and with AM transport disabled in radiative regions outside the web. Top: Kippenhahn diagram including the MS and RGB phases. Bottom: rotation profiles Ω(m) at different evolutionary points on the RGB, with the growing helium core mass mHe indicated next to each profile.
Paper: Magnetic Webs in Stellar Radiative Zones
Authors: Valentin A. Skoutnev, Andrei M. Beloborodov
Figure caption: Rotation profiles Ω(R) of the 1.6M⊙ star, calculated with different prescriptions for AM transport (see the main text). Profiles are taken when mHe = 0.2M⊙, representative of the evolutionary point of KIC 11515377. Shaded and hatched regions are the same as in Figure 3.
Paper: Magnetic Webs in Stellar Radiative Zones
Authors: Valentin A. Skoutnev, Andrei M. Beloborodov
Figure caption: Toy model of an evolving core and mantle connected by a radial magnetic field.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: Left: a grz cutout of our sky-corrected coadd centered on the midpoint between BCG1 (green) and BCG2 (blue). An intermediate galaxy whose profile we study, LEDA 64218, is also labeled (yellow). Right: a cutout of the same field from the sky-corrected and star-subtracted coadd with masked pixels (detections and stars) rendered in grz. The pixels rendered in grayscale show the r-band coadd with an aggressive stretch to showcase LSB features. Note the presence of cirrus clouds (red) and two cluster members that are enveloped by ICL (purple), LEDA 64290 in the southeast, and LEDA 95791 in the west.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: Detector 42 from DECam visit 1110874, binned into 8 px × 8 px superpixels with an aggressive stretch, shown during different steps of skycorr. From left to right: the default calexp produced by the LSP with an aggressive background subtraction, the same calexp with the background restored, calexp-bg1, calexp-bg1-sky, and calexp-bg1-sky-bg2. The default background model has a pronounced dark ring around a pair of merging galaxies. Without any model, there is a gradient across the detector. This is corrected by bg1 and the sky frame while preserving the LSB features such as the extended profile of the merging galaxy and the wings of a bright star outside the field of view (top left). bg2 does not noticeably flatten the background further and removes light from the LSB features.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: LSB contours of the central region of our coadds in g band (right) and r band (left) drawn at surface brightnesses of 26, 28, and 30 mag arcsec–2. These are drawn over the corresponding inverted star-subtracted coadd for each band. The eastern LSB feature is the extended PSF of a bright star outside the central region; the northernmost, northwestern, and southernmost 30 mag arcsec–2 contours are cirrus (the last two are also highlighted in Figure 1). BCG1 (green), BCG2 (blue), and LEDA 64218 (orange) are labeled in the right panel. Additionally, the blue square shows the field of view from Figure 1, and the orange rectangle shows the region displayed in Figure 6.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: Left: the rest-frame g − r color and r-band surface brightness profiles; the dashed red curves in the bottom-left panel enclose the profile of LEDA 64218 minus the profile of the bridge. The color profiles have been truncated at smaller central distances for ease of viewing. Right: a cropped cutout of the sky-corrected and star-subtracted image from Figure 1 with statistically significant (SN ≳ 3) isophotes and annuli rendered; these are colored per the (g − r)0 color as in Figure 4.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: The calibrated surface brightness and color profiles for BCG1 (top), BCG2 (middle), and the bridge (bottom). The red shaded region in the color profiles covers the red sequence of A3667 (S. Fu et al. 2024). The isophotes and annuli are drawn over grz RGB cutouts and colored according to (g − r)0. BCG1 is cropped to the core with the mask built in Section 2 applied. We have rendered BCG2 without the mask and central isophotes to showcase the shells surrounding its core. The bridge has the modified LSP mask (detections, bad pixels, stars, and intermediate galaxies) applied and the center contour (h = 0), is rendered with a dashed line.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: Detector 42 from DECam visit 1110874, shown with the default mask produced by the LSP and the final mask created by skycorr overlaid in red. The final mask is significantly more aggressive but still fails to mask the most extended features, such as the wings of bright stars and the extended profile of the merging galaxies. This leaves them susceptible to oversubtraction by bgmodel2.
Paper: The Intracluster Light of Abell 3667: Unveiling an Optical Bridge in LSST Precursor Data
Authors: Anthony M. Englert, Ian Dell'Antonio, Mireia Montes
Figure caption: The signal-to-noise (SN) of the ICL signal as a function of central distance for different features. The signal for LEDA 64218 is truncated because, beyond ∼100″, its outer profile blends into the bridge. Due to the small number of pixels used to fit isophotes near the cores of BCG1, BCG2, and LEDA 64218, the SN profile fluctuates and can have a peak offset from center of the object.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The top row shows the measured AH for the morning and evening limbs for each planet vs. planet equilibrium temperature with best-fit picaso model tracks overplotted (See Figure 14 for full spectra). The top left includes Na2S, MnS, and MgSiO3 clouds, and the top right only includes MgSiO3 clouds. The bottom row shows temperature–pressure (TP) profiles for the evening limb for each planet; the morning limb TP profiles have the same parameterization except temperature being 0.66x(Teq-500K) lower. The cloud condensation lines are overplotted in dashed lines. The water band averaged peak contribution function pressure levels are shown in dotted lines for both limbs.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The morning (blue) and evening (red) limb spectra for the nine-planet sample used in this study. We normalize the spectra by their corresponding atmospheric scale heights (H) and apply a 13 H offset between planets, which are sorted by temperature. The water opacity is shown at the bottom. The vertical gray (0.9−1.3 μm) and light blue (1.35−1.5 μm) shaded areas represent the baseline and 1.4 μm water band regions, respectively. To eliminate spectral overlap between planets, the morning limb spectra are offset to be one scale height above the evening limb spectra based on the averaged inside of the water band transit depth values. We first measured the band average for both blue and gray regions for both limbs for each planet, and then calculated the relative differences between them (AH).
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: Transit light curves from inside the 1.4 μm water band vs. the outside baseline are shown in the top panels for each of the nine planets. The differences between the two light curves are shown in the middle panels. This direct empirical comparison visualizes the wavelength-dependent asymmetric signals in the transit light curves. Residuals (Red) between two bands should be symmetric around ingress and egress if the planet has the same morning and evening limb spectral shapes, regardless of limb-darkening, midtransit time, and eccentricity. The spot crossings are removed from the light curves. The best-fit one-circle (Teal) and two semicircle (Black) transit models are overplotted in the middle panels. The midtransit times are both fixed to the white-light midtransit times. The respective residuals for both fits are shown in the bottom panels. The two semicircle models can better fit ingress and egress for especially three planets, WASP-39 b, WASP-94 Ab, and WASP-17 b, where we see strong morning and evening limb spectra difference in Figure 2.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: Day–night temperature difference is the main driver for large-scale flows on hot Jupiter atmospheres. We assumed two empirically motivated (T. D. Komacek et al. 2017) day–night ΔT vs. Teq correlation (top panel) and then derived the expected vertical wind speeds (second panel; T. D. Komacek et al. 2019) and the time needed to cross 1 scale height (H) vertically (third panel). Then we calculated the number of H downwelling flows that can travel in half of the planet’s period (P/2) time (bottom panel) with planet-specific estimates (gray) and compared to measured δAH values. Downwelling flows can remove aerosols on a similar timescale as day–night flow, leading to clearer evening than morning limb spectra.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: Calculated total fall time from 0.01 to 1 mbar as a function of particle size based on V. Parmentier et al. (2013) for two temperatures and surface gravity. The effect of stellar radiation pressure is estimated by scaling up the gravity term based on β as a function of grain size. To qualitatively match the observed muted morning and clear evening limbs, the total fall time should be comparable to or shorter than the advection timescale (∼days). For large particles (>∼10 μm), gravitational settling alone is sufficient. For small grains (<∼1 μm), settling is not enough; additional mechanisms such as evaporation and vertical flow are needed.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: Comparison between morning and evening spectra for WASP-39 b using NIRISS/SOSS (this work) vs. NIRSpec PRISM (this work; top panel). Comparison between NIRSpec PRISM (this work) evening (middle panel) and morning (bottom panel) limbs spectra to three reductions in Extended Figure 1 from N. Espinoza et al. (2024), where the labels (NE, MM, and tiberius) are kept consistent from N. Espinoza et al. (2024) representing the three reductions. Beyond the constant vertical offsets introduced by T0 uncertainties, both NIRISS/SOSS and NIRSpec PRISM show consistent wavelength-dependent spectral shapes with muted morning limbs and clear evening limbs. This shows that the observed limb–limb spectral shape difference is not introduced by any SOSS instrument-specific systematics.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The measured δAH for each planet in the planet equilibrium temperature vs. surface gravity space. Planets with high δAH appear to cluster around the bottom right of the parameter space. We propose the asymmetry horizon (gray line), which outlines the transition region where aerosol-induced limb–limb asymmetry is expected to appear in the hot Jupiter atmosphere population. The line is empirically derived by fitting a 2D sigmoid function to the data and represents the contour where the function reaches half of its maximum value. The shaded gray area represents the 1, 2, and 3σ regions of uncertainties.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The top row shows the measured AH for the morning and evening limbs for each planet vs. planet equilibrium temperature (left) and surface gravity (right). The bottom row shows the evening–morning difference (δAH) for each planet. Neither planet temperature nor gravity appears to exhibit a simple relationship with AH or δAH.
Paper: Overcast Mornings and Clear Evenings in Hot Jupiter Exoplanet Atmospheres
Authors: Guangwei Fu, Sagnick Mukherjee, Kevin B. Stevenson, David K. Sing, Reza Ashtari, Nathan Mayne, Joshua D. Lothringer, Maria Zamyatina, Stephen P. Schmidt, Carlos Gascón, Natalie H. Allen, Katherine A. Bennett, Mercedes López-Morales
Figure caption: The absolute transit depth for the morning and evening limbs is sensitive to the exact T0 value used for the spectroscopic light-curve fits. However, the relative shapes of the spectra remain consistent. We demonstrated this with the WASP-39 b SOSS data set by varying the T0 by one σ before and after the best-fit white-light T0. The corresponding AH value is insensitive to the T0 variation.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Marginalized likelihood on the Mg II column density, Doppler parameter, and O I column density for the z = 7.368 (left), z = 7.443 (right), and z = 7.476 (bottom) absorption systems. The crosses mark the maximum of the three-dimensional likelihood that we adopt as our fiducial absorber parameters. The dashed line in the lower-left subpanels shows where the O I/Mg II ratio would be equivalent to the solar abundance ratio of O/Mg from E. Magg et al. (2022). The measured Mg IIλλ2796, 2803 and O Iλ1302 equivalent widths are shown in the upper right of each absorber panel, along with the corresponding values from our best-fit parameters in brackets.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Left: posterior pdfs of the IGM neutral fraction 〈xHI〉 from the Lyα transmission analysis. The black curve shows the posterior, assuming that the signal is entirely intergalactic, while the blue and orange curves include the presence of H I absorbers corresponding to the z > 7.3 low-ionization absorption systems found by C23, assuming they have relatively high metallicity ([O/H] =  −2.5) or low metallicity ([O/H] = −3.5). The points with error bars show the medians and central 68% credible intervals; for the [O/H] = −3.5 case we elect to present them as an upper limit for clarity. Right: the same for the posterior pdfs of the quasar lifetime tq.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Spectrum of J1342 (black + noise vector in red) and a prediction for its unabsorbed continuum (blue). The top panels show the individual H I absorbers corresponding to the three absorption systems from C23, while in the bottom panel the absorbers are combined along with a complete Gunn–Peterson trough at wavelengths shortward of Lyα in the frame of the highest-redshift system (z = 7.476). The left panels show the H I column densities, assuming an absorber metallicity of [O/H] = −2.5, while the right panels assume [O/H] = −3.5. The transparent swarm of curves in the lower panels show draws from the quasar continuum prediction uncertainty and their resulting impact after absorption.
Paper: Possible Contamination of the Intergalactic Medium Damping Wing in ULAS J1342+0928 by Proximate Damped Lyα Absorption
Authors: Frederick B. Davies, Eduardo Bañados, Joseph F. Hennawi, Sarah E. I. Bosman
Figure caption: Best-fit absorption models in the absorber-free case with only IGM absorption (left; 〈xHI〉 = 0.90), the [O/H] = −2.5 case (middle; 〈xHI〉 = 0.85), and the [O/H] = −3.5 case (right; 〈xHI〉 = 0.1), where the latter two include both the effect of the foreground absorbers and the IGM. The purple curves and shaded regions show the median and 68% scatter of the Lyα transmission of the maximum pseudolikelihood model. The gray and black curves show the unbinned quasar spectrum and the 500 km s−1-binned spectrum, respectively, while the red curve shows the unbinned noise vector. The blue curve shows the prediction for the intrinsic continuum, with a swarm of transparent curves showing draws from its covariant uncertainty. The green curves in the middle and right panels show the corresponding model of the absorption from the three foreground absorbers.