adsabs/AstroCLIMB huggingface dataset:
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: White light-curve analysis of the two LHS 1140 b transits. The white 							light curve of each visit and each detector is normalized. The left 							panel shows the white light curves from the NRS1 and NRS2 detectors 							using the G235H grating. The middle panel shows the same information as 							the left panel, but for the G395H grating. The starspot crossing can be 							seen here. The right panel shows the residuals of the fit for each of 							the four white light curves. The relative rms is also noted.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Raw spectroscopic light curves from the NIRSpec/G235H (left) and G395H 							(right) modes. Both modes show a gap that separates the data from the 							NRS1 and NRS2 detectors. The white horizontal stripe in the G235H data 							are points affected by the high-gain antenna move.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Transmission spectrum of LHS 1140 b. The two transit observations are 							color-coded, i.e., blue for the G235H grating and green for the G395H 							grating. The models shown are randomly selected solutions from the 							posterior distributions of Scenario 4 (Table 5, corresponding to 								N2–H2O atmospheres with deep clouds). We have 							applied the best-fit offsets to the data. The offset between the two 							visits is ∼50 ppm, while the offset between the two detectors within 							each of the two visits is negligible (see Figure 4 and Table 6).
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Comparison of the 1D posterior distribution functions of Scenarios 1 and 							4 (i.e., including N2, H2O, CO2, 							clouds, and with and without the stellar heterogeneity).
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Posterior distribution functions of the Bayesian analysis of all the LHS 							1140 b data sets combined. The posterior distribution functions suggest 							a H2O-rich atmosphere with a nonnegligible presence of 							hydrogen. The offsets are defined as follows: offset1 is 							related to G235H-NRS2, and offset2 and offset3 are 							instead related to G395H-NRS1 and NRS2, respectively; offset4 							is between the HST data (Edwards et al. 2020) and G325H-NRS1 data set, and 								offset5 is between the Magellan data set (Diamond-Lowe et 							al. 2020) and the 							G325H-NRS1 data. The numeric values above each panel indicate the median 							and 1σ uncertainty of the 							distribution.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Available data sets for LHS 1140 b. The MAP solution from the Bayesian 							retrieval process is shown in black. The individual contribution from 							the spectral components is also shown. The data are plotted by taking 							into consideration the offsets value calculated by the Bayesian 							analysis. The offset values are reported in the posterior distribution 							functions in Figure 10. 							HST data are adopted from Edwards et al. (2020), and the Magellan data are 							adopted from Diamond-Lowe et al. (2020).
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: The transmission spectrum obtained in this work compared with the HST 							data adopted from Edwards et al. (2020). The green model, i.e., maximum a 							posteriori (MAP) solution of Scenario 4 in Table 5, extended to the HST data wavelength. 							The blue model is the best-fit model for the HST data (a 							H2-dominated atmosphere with water vapor absorption). In this 							model we injected a CH4 and CO2 10−6 							VMR and we extended the wavelength range to cover the JWST data. The 							JWST data set is incompatible with the blue model.
Paper: LHS 1140 b Is a Potentially Habitable Water World
Authors: Mario Damiano, Aaron Bello-Arufe, Jeehyun Yang, Renyu Hu
Figure caption: Potential processes that partition C and N species between the 							atmosphere, the ocean, and the HP ices in a cold water world like LHS 							1140 b. Summarized based on Levi et al. (2017), Ramirez & Levi (2018), Levi & Cohen 								(2019), Marounina 							& Rogers (2020), 							Kovačević et al. (2022), and Vazan et al. (2022).
Paper: Low-mass Galaxy Interactions Trigger Black Hole Activity
Authors: Marko Mićić, Jimmy A. Irwin, Preethi Nair, Brenna N. Wells, Olivia J. Holmes, Jackson T. Eames
Figure caption: AGN frequency in paired/grouped dwarfs in both N AGN,low = 6 and N AGN,high = 10 limits compared to the occupation fraction in isolated control sample and occupation fraction from the literature as a function of the median stellar mass of dwarfs hosting an AGN. Uncertainties from our work are estimated at 1σ assuming Poissonian statistics. Latimer et al. (2021) do not provide the list of galaxies in their sample; thus, the median stellar mass of the sample is set to log (M */M ⊙) = 9.0
Paper: Low-mass Galaxy Interactions Trigger Black Hole Activity
Authors: Marko Mićić, Jimmy A. Irwin, Preethi Nair, Brenna N. Wells, Olivia J. Holmes, Jackson T. Eames
Figure caption: Demographics of paired/grouped dwarfs. Upper left: redshift distribution of paired/grouped dwarf systems. Upper right: stellar mass distribution of all dwarfs from paired/grouped dwarf systems. Lower left: distribution of projected separation between the most massive dwarf and their neighbor(s). Lower right: distribution of the mass ratios of the most massive dwarf and their neighbor(s).
Paper: Low-mass Galaxy Interactions Trigger Black Hole Activity
Authors: Marko Mićić, Jimmy A. Irwin, Preethi Nair, Brenna N. Wells, Olivia J. Holmes, Jackson T. Eames
Figure caption: Top: distribution of interacting and isolated control dwarf galaxies in redshift–stellar mass space. Middle: redshift distribution of interacting and isolated control dwarf galaxies. Bottom: stellar mass distribution of interacting and isolated control dwarf galaxies.
Paper: Low-mass Galaxy Interactions Trigger Black Hole Activity
Authors: Marko Mićić, Jimmy A. Irwin, Preethi Nair, Brenna N. Wells, Olivia J. Holmes, Jackson T. Eames
Figure caption: GOODS color images of nine randomly selected dwarf systems. The identification number of each system is given in the upper left corner. The white horizontal lines in the lower right corner represent ≈10 kpc. The galaxies of interest are labeled with red rectangles.
Paper: Low-mass Galaxy Interactions Trigger Black Hole Activity
Authors: Marko Mićić, Jimmy A. Irwin, Preethi Nair, Brenna N. Wells, Olivia J. Holmes, Jackson T. Eames
Figure caption: GOODS color images of the six dwarf pairs/groups hosting an AGN. The identification number of each system is given in the upper left corner. Horizontal white lines in the lower right corner represent ≈10 kpc. Galaxies of interest are located in red rectangles. Red star symbols represent the location of Chandra X-ray-detected AGN.
Paper: JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4
Authors: Vicki Kuhn, Yicheng Guo, Alec Martin, Julianna Bayless, Ellie Gates, AJ Puleo
Figure caption: The left panel shows the fraction of spiral galaxies as a function of redshift from our subsample with varying intrinsic spiral fractions. The big black points show the results of our probability decision. The x and y errors are the median of the redshift in each bin and 3σ standard error, respectively. Each of the different colored lines shows how the observed spiral fraction of a sample with different intrinsic spiral fraction at z = 0.5–0.8 would change when the sample was shifted to different redshifts. The intrinsic fraction that matches the observed spiral fraction at a given redshift would be considered the true spiral fraction. The right panel shows the intrinsic fraction of the real sample (teal squares) across different redshifts compared with the fraction of disk galaxies (brown and gray lines) that have been reported in the literature.
Paper: JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4
Authors: Vicki Kuhn, Yicheng Guo, Alec Martin, Julianna Bayless, Ellie Gates, AJ Puleo
Figure caption: Examples of galaxies in our sample. Redshifts increase from left to right as indicated by the labels. Galaxies in the top three rows (outlined in the large blue box) were classified as spirals by all inspectors (except for the top right corner with an asterisk, which only had five inspectors vote spiral). The two blank cutouts signify no other spiral galaxies identified in that redshift bin. The middle three rows (outlined in the large cyan box) show galaxies with spiral votes of three to four. The bottom three rows (outlined in the large red box) show nonspiral galaxies.
Paper: JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4
Authors: Vicki Kuhn, Yicheng Guo, Alec Martin, Julianna Bayless, Ellie Gates, AJ Puleo
Figure caption: Fraction of spiral galaxies as a function of redshift. The blue points represent the galaxies in our sample that had at least three voters (i.e., more than 50%) classify them as spirals; the green points represent those with more than five spiral votes (i.e., more than 75% of the voters); and the orange points represent those that all six voters classified as spirals. The black points represent the average score of our sample (probability decision). The gray hexagon represents the fraction found from Delgado-Serrano et al. (2010). The thin and thick diamonds show the uncorrected and corrected fractions after taking into account redshift effects from Margalef-Bentabol et al. (2022), respectively. The error bars in the right panel shows 3σ standard error in the y-axis and the 16th and 84th percentile values in the x-axis.
Paper: JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4
Authors: Vicki Kuhn, Yicheng Guo, Alec Martin, Julianna Bayless, Ellie Gates, AJ Puleo
Figure caption: The top row shows the SFR as a function of stellar mass in separate redshift bins. Blue points show spiral galaxies with six “yes” votes; cyan triangles show spiral galaxies with three to five “yes” votes; and red squares show nonspiral galaxies, two or less “yes” votes. Nonspiral galaxies below the star-forming region are shown as open red squares. The black line shows the star-forming main-sequence line (Whitaker et al. 2014), and the gray line (0.9 dex below the black line) shows the lower boundary of the star-forming region. The bottom row shows the half-light radius as a function of stellar mass.
Paper: JWST Reveals a Surprisingly High Fraction of Galaxies Being Spiral-like at 0.5 ≤ z ≤ 4
Authors: Vicki Kuhn, Yicheng Guo, Alec Martin, Julianna Bayless, Ellie Gates, AJ Puleo
Figure caption: Examples of galaxies within our artificially redshifted sample. Each row shows one galaxy at differing redshifts. The number of classifiers that designated the galaxy as spiral is indicated in the top right corner of each image. The top four rows show examples of galaxies with a clear spiral structure across all the redshift bins. The bottom four show galaxies whose spiral structure is not detectable at higher redshifts.
Paper: Probing the C IV Continuum Size–Luminosity Relation in Active Galactic Nuclei with Photometric Reverberation Mapping
Authors: Swayamtrupta Panda, Francisco Pozo Nuñez, Eduardo Bañados, Jochen Heidt
Figure caption: Left: recovered distributions of delays (τ*) for CT286 (top) and CT406 (bottom). Right: time-delay spectrum τ  c (λ) ∝ λ 4/3 (black line) as predicted from the transfer functions. The black circles represent the median values of the recovered distributions. The associated error bars reflect the upper and lower uncertainties, corresponding to the distributions’ 16th and 84th percentiles, respectively. For comparison, we show the results for different sampling intervals using different symbols: filled circles for Δt = 2 days, empty circles for Δt = 3 days, and empty squares for Δt = 5 days. A small offset in λ was used for better visualization. The dashed red lines show the delay spectrum obtained for a black hole mass with 30% uncertainty.
Paper: Probing the C IV Continuum Size–Luminosity Relation in Active Galactic Nuclei with Photometric Reverberation Mapping
Authors: Swayamtrupta Panda, Francisco Pozo Nuñez, Eduardo Bañados, Jochen Heidt
Figure caption: Spectrum of the sources CT286 (top) and CT406 (bottom) from Lira et al. (2018). The colored line shows the transmission of the WFI medium-band filters, which were convolved with the quantum efficiency of the camera. The filters trace mainly the AGN emission-line-free continuum variations around the C IV and C  III] emission lines.
Paper: Probing the C IV Continuum Size–Luminosity Relation in Active Galactic Nuclei with Photometric Reverberation Mapping
Authors: Swayamtrupta Panda, Francisco Pozo Nuñez, Eduardo Bañados, Jochen Heidt
Figure caption: The R BLR–L 1350 Å relation from Kaspi et al. (2021) (black) and the expected R AD–L 1350 Å relation (blue). The solid red and blue lines indicate the mean values of the posterior probability distributions for both relationships. The shaded areas around these lines reflect the 1σ uncertainty. The dashed lines delineate the mean predictions for the upper and lower bounds when the intrinsic scatter in the sources is considered. The positions of CT286 (z = 2.556) and CT406 (z = 3.178) are marked with red circles. The time lag is given in the rest frame.
Paper: Probing the C IV Continuum Size–Luminosity Relation in Active Galactic Nuclei with Photometric Reverberation Mapping
Authors: Swayamtrupta Panda, Francisco Pozo Nuñez, Eduardo Bañados, Jochen Heidt
Figure caption: Recovered R BLR–R AD relationship. The solid black line indicates the mean value of the posterior probability distributions. The shaded area reflects the 1σ uncertainty. The best-fit slope (α), intercept (β), and scatter (σ) are reported with 1σ uncertainties. The dotted lines delineate the mean predictions for the upper and lower bounds when the intrinsic scatter in the data is considered. Blue and red circles denote the positions of CT286 and CT406, respectively.
Paper: Probing the C IV Continuum Size–Luminosity Relation in Active Galactic Nuclei with Photometric Reverberation Mapping
Authors: Swayamtrupta Panda, Francisco Pozo Nuñez, Eduardo Bañados, Jochen Heidt
Figure caption: AD transfer functions for CT406 (bottom) and CT286 (top) sources. The transfer functions centroids are indicated in the observer frame and denoted by vertical dotted lines.
Paper: The Six-planet Resonant Chain of HD 110067
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Evolution of adjacent planet period ratios, orbital eccentricities, and three-body resonant angles during an example convergent migration simulation (in this case, K = 114). Adjacent planet pairs are captured into two-body MMRs outside-in, beginning with planets f–g and ending with planets b–c. Each planet obtains a non-zero eccentricity through this process, and three-body resonant angles librate with small amplitudes (two-body resonant angles also librate). Before carrying out our long-term N-body simulations, we adiabatically remove the eccentricity and semimajor axis damping and provide a random kick to the planets’ eccentricities.
Paper: The Six-planet Resonant Chain of HD 110067
Authors: Caleb Lammers, Joshua N. Winn
Figure caption: Cumulative fraction of 350 systems that destabilized within 25 Myr. 99% of the nonresonant systems with properties consistent with the observations were unstable, as opposed to 11% of systems initialized in a six-planet resonant chain (via a disk migration simulation). Systems in which only a subset of the planets are captured into a resonant chain were also mostly unstable.
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 plot shows a comparison between the measured Ni/Fe ratios for the Crab Nebula and the predictions from some of the available explosion nucleosynthesis models. The green band represents the JWST-measured Ni/Fe ratios (relative to the solar ratio of 0.053 from Scott et al. 2015), including the estimated uncertainty of 50%. The near-IR measurements from Hudgins et al. (1990) and the optical ratios rederived in this work are shown as the gray bands. We note that the range of optical values does not include uncertainties in the measurements but represents a range of values measured at different positions in the Crab Nebula. These optical values are likely to be lower if dust in the filaments is accounted for (see Section 7 for details). The yields of the 3D models of Wang & Burrows (2024a) and Wang & Burrows (2024b) are shown as orange and blue solid vertical lines, respectively. The vertical lines reflect the variation in the expected ratio due to mixing with the stellar envelope (the dots are Ni/Fe values assuming no mixing with the envelope, and the crosses are values that assume the ejecta are mixed with the stellar envelope). The explosion energy (in units of Bethes) and resulting neutron star kick velocity are also labeled for each model (Burrows et al. 2024a; Wang & Burrows 2024a) and can be compared to the ∼160 km s−1 kick velocity of the Crab’s pulsar (Hester 2008; Kaplan et al. 2008). Nucleosynthetic yields from the 1D Fe core-collapse models of Sukhbold et al. (2016) are shown as blue diamonds for comparison. The orange dashed line connecting open orange circles represents the range of Ni/Fe ratios for the 1D ECSN models of Wanajo et al. (2009) that assume no mixing with the envelope. The orange dashed line connecting the orange pluses shows how these values might shift if we use a dilution factor of ∼4 (similar to what is found for the ECSN-like models). For more details, please see Section 8.1.
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: Left: the plot shows the [Fe II] 5.340 μm (solid lines) and [Ni II] 6.636 μm (dashed lines) line profiles as a function of the velocity shift with respect to the rest wavelength. The line profiles from position 1 and position 2 are shown in the green and orange colors, respectively. The solid gray curve shows the best-fit two-component Gaussian model to the [Ni II] 6.636 μm at position 2, with the dotted and dashed gray curves showing the individual model components. The locations of the MRS pointings are shown in Figure 1. Right: this figure shows line emission maps for the [Fe II] 5.340 μm and [Ni II] 6.636 μm lines extracted from the MIRI MRS data. The maps are produced by integrating the MRS cubes over the wavelength range that spans the detected line. While position 2 shows two distinct redshifted components (see left panel), position 1 contains distinct blue- and redshifted components with different spatial distributions. The white rectangles represent the spectral extraction regions used in the analysis.
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 first three panels are images of the inner pulsar region showing the structure of the synchrotron wisps, with a field-of-view size of 40″ across and the scale in units of MJy sr−1. The F560W and F1130W images were taken on the same day, while the F480M image was obtained 4 months before. The last panel shows the synchrotron spectral index map between the F560W and F1130W images. The spectral index values are labeled for several regions. While the absolute values of the spectral indices have an average 3σ uncertainty on the order of ∼0.15, the relative values in the index map have 3σ uncertainties of only ∼0.025.
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: Left: schematic diagrams (not to scale) of assumed PWN geometry. The thermal gas in a Rayleigh–Taylor finger resides in a cone cut out of the otherwise assumed spherical PWN. Synchrotron emission from the nebula irradiates thermal gas in the cone. The lower panel shows the geometry for the calculation. Right: ionization balance for Ni (top), Fe (middle), and variation of electron density and temperature (bottom) used in the Ni/Fe abundance ratio determination.
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: Left panel: spectral index of synchrotron emission due to pairs having an energy distribution given by a broken power law with lower energy index 1.35 and high energy index 2.35 as a function of the break Lorentz factor γ br, comoving magnetic field (orthogonal to the line of sight) ﹩{B}_{\perp }^{{\prime} }﹩, and Doppler boosting term D boost (where γ is the bulk Lorentz factor of the emitting plasma and β is the component of the bulk velocity along the line of sight). The solid blue line is the analytical value at λ = 8.3 μm; orange dots are values obtained from the ratio of integrated flux in the F560W and F1130W JWST filter bands. Right panel: difference in spectral index between a boosted (toward the observer) and unboosted emitting region as a function of the comoving magnetic field for two different values of the break Lorentz factor and two values of the bulk velocity of the boosted region at the effective wavelength of 8.3 μm.