adsabs/AstroCLIMB huggingface dataset:
Paper: The Orbital Eccentricities of Directly Imaged Companions Using Observable-based Priors: Implications for Population-level Distributions
Authors: Clarissa R. Do Ó, Kelly K. O'Neil, Quinn M. Konopacky, Tuan Do, Gregory D. Martinez, Jean-Baptiste Ruffio, Andrea M. Ghez
Figure caption: Same as Figure 14, but for HD 49197 B.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Reproduced from Rimmer et al. (2021b). Primary spectral features of a selection of prebiosignature molecules at JWST-probable wavelengths. The icons represent major physical and geochemical sources of the molecules, with primary prebiosignatures being directly associated with prebiotic chemistry. The species included are carbon monoxide (CO), hydrogen sulfide (H2S), sulfur dioxide (SO2), imidazole (C3N2H4), cyanamide (CH2N2), nitric oxide (NO), methane (CH4), acetylene (C2H2), and hydrogen cyanide (﹩\mathrm{HCN}﹩). We include all of these except imidazole and cyanamide in our study. We also investigate ammonia and formaldehyde as potential prebiosignatures. Transparency indicates the strength of the features, with weaker features being more transparent. CME = Coronal Mass Ejection.
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Transmission spectra of model exoplanets, calculated using petitRADTRANS. Top left: Hycean planet, with planetary and atmospheric properties chosen to match those described by Madhusudhan et al. (2021) for K2-18b. Top right: Super-Earth with thin hydrogen envelope, with planetary properties chosen to match those of HD 88512b, and atmospheric properties based on the modeling of Hu et al. (2012). Middle left: Ultra-reduced volcanic planet, both with (blue) and without (orange) a gray cloud layer at 10 mbar, with planetary and atmospheric properties chosen to match those described by Swain et al. (2021) for GJ 1132b. Middle right: Post-impact planet transmission spectra 100 kyr (blue) and 10 Myr (orange) after the impact, with atmospheric properties chosen to match those described by Zahnle et al. (2020) for a Hadean Earth. Bottom: Model TRAPPIST-1e with an atmosphere to emulate an early epoch of Earth history (Kaltenegger et al. 2007).
Paper: Prebiosignature Molecules Can Be Detected in Temperate Exoplanet Atmospheres with JWST
Authors: A. B. Claringbold, P. B. Rimmer, S. Rugheimer, O. Shorttle
Figure caption: Detection threshold of C2H2 as a function of the atmosphere’s mean molecular weight (top left), transmission spectrum noise (top right), temperature of the isothermal atmosphere (middle left), surface atmospheric pressure (middle right), planet radius (bottom left), and cloud-top pressure (bottom right). In each case only a single parameter is varied, with other parameters given by a model Hycean planet with noise from observing GJ 1132b for three transits. The noise floors for NIRSpec is given by Rustamkulov et al. (2022).
Paper: Autoencoding Galaxy Spectra. I. Architecture
Authors: Peter Melchior, Yan Liang, ChangHoon Hahn, Andy Goulding
Figure caption: Top left: direct attention weights  a  of the SPENDER LR-10 model for the spectrum shown in the lower subpanel. Marker sizes are proportional to weight activations. Top right: Grad-FAM attention weights  g   a  responsible for the peak height of the Hα line (see Equation (4)). Colors indicate gradient amplitudes, marker sizes increased for clarity. Attention channel 149 is most highly activated, especially in the wavelength segment that contains the Hα line. Bottom left: same as top right, but for a higher-redshift galaxy. Channel 149 remains most highly activated, finding Hα in a larger wavelength segment. Bottom right: six galaxies from the same SDSS plate, ordered by Grad-FAM activation of channel 149, which serves as a proxy for Hα line strength.
Paper: Autoencoding Galaxy Spectra. I. Architecture
Authors: Peter Melchior, Yan Liang, ChangHoon Hahn, Andy Goulding
Figure caption: UMAP embedding of the SPENDER LR-10 latent variables for 20,480 spectra. Galaxy subpopulations (starburst, star-forming, and broadline AGN) form clusters in latent space (top left, bolder colors indicate higher redshifts). Color coding by Hα line strength (top right) and stellar mass (bottom right) reveals the two main dependencies of the spectrum embeddings, with the redshift dependence (emphbottom left) being a result of the magnitude cut of the survey.
Paper: Autoencoding Galaxy Spectra. I. Architecture
Authors: Peter Melchior, Yan Liang, ChangHoon Hahn, Andy Goulding
Figure caption: Left: 5 pixel wide SDSS-II LSF kernel learned from the data. Right: SDSS spectrum in the regions of the [O II]λλ3726,3729 and [S II]λλ6716,6731 doublets. The SPENDER SR model resolves the [O II] doublet that is heavily blended in the observation by increasing the restframe resolution by a factor of 2 and deconvolving from the LSF model.
Paper: Autoencoding Galaxy Spectra. I. Architecture
Authors: Peter Melchior, Yan Liang, ChangHoon Hahn, Andy Goulding
Figure caption: Example restframe spectra, ordered by redshift (top to bottom), and their reconstruction by 5 SPENDER LR models with different latent space dimensionality S. The left column shows the entire spectrum. Other columns zoom in to specific emission and absorption lines. Wavelengths that are unobserved or masked by the processing pipeline are shown in light blue shading.
Paper: Autoencoding Galaxy Spectra. I. Architecture
Authors: Peter Melchior, Yan Liang, ChangHoon Hahn, Andy Goulding
Figure caption: The autoencoder architecture of SPENDER with an attentive convolutional encoder and an explicit redshifting, resampling, and convolution transformation after the decoder.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Left: sky positions of all stars in a 12′ ×12 ′ region about Boötes V, projected onto the tangent plane centered at R.A., decl. = (14h15m38.ˢ6, +32° 54′ 42″). Dark blue sources are those that meet the isochrone selection criterion (see right panel). Yellow points are stars identified in Gaia DR3 as sources with complete astrometric information, and are selected as high-confidence (probability > 90%) members by our maximum-likelihood membership selection algorithm (see Section 4.1). The concentric black ellipses indicate 1 ×, 3 ×, and 5 × the half-light radius (r h) as determined by the Markov Chain Monte Carlo (MCMC) fit (see Section 3.1). Right: CMD of extinction-corrected CFIS-r and Pan-STARRS-i for all stellar sources in a 12′ × 12′ region about Boötes V. We overlay an old (13 Gyr), metal-poor ([Fe/H] = −2.2) isochrone, shifted to a distance of 100 kpc. We use a broad color selection criterion, selecting all stars with (r − i)0≤0.1 from the isochrone, and we add, in quadrature, the empirical photometric errors from each band. Stars consistent with this selection criterion are highlighted in dark blue.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Left: 8′ × 8′ cutout from CFIS-r imaging tiles. Bright sources with diffraction spikes are likely Milky Way foreground stars. The clustering of stars and light in the center of this image is Boötes V. Upper right: smoothed spatial density plot of all stellar sources on the 8′ × 8′ tile. No stellar population filtering has been applied to the stars in this smoothed distribution. Lower right: smoothed spatial density plot of all galaxies in the 8′ × 8′ tile, normalized with respect to the stellar density. There are many more galaxies than stars in this field of view, but there is no discernible overdensity.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Two-dimensional and marginalized probability distribution functions (PDFs) from the MCMC analysis. The fit was run on all stellar sources within a 9′ radius, circular region around the initial satellite’s centroid estimate that are consistent with the isochrone selection criteria. This corresponds to all of the stars that are highlighted in blue in Figure 2. The quantities x 0, y 0, and r h are the projected R.A. centroid offset, projected decl. centroid offset, and half-light radius, respectively. All three are presented in arcminutes. Ellipticity is denoted as ϵ = 1 − b/a, where b/a is the minor-to-major axis ratio, while θ is the position angle (denoted east from north in degrees), and N* is the estimated number of member stars. In each marginalized PDF, dashed lines should be interpreted as the 16th, 50th, and 84th quantiles, from left to right.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Left: CMD of all stars within 3 elliptical r h of the satellite’s centroid; 92 stars meet this spatial criterion. A 13 Gyr, [Fe/H] = −2.2 isochrone shifted to 100 kpc is overlaid as a solid line. Isochrones shifted to 80 and 120 kpc, the lower and upper distance bounds as determined in Section 3.2, are shown as dashed lines. A possible TRGB star (red triangle) and three possible BHB stars (blue squares), which were used for distance estimates, are shown as well. Note that the two brightest BHB stars are nearly directly atop each other on the CMD. Right: CMD of stars within an equivalent area offset by 12′ to the south of the satellite’s centroid, with the same isochrone overlaid; 48 stars meet this spatial criteria.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Yellow sources are those selected as high-confidence (probability > 90%) members by our maximum-likelihood membership selection algorithm. Gray sources/shading are all five-parameter Gaia detections in a 2° circle around Boötes V. Left: sky positions of stars in a 12′ × 12′ region about Boötes V, projected onto the tangent plane centered at R.A., decl. of (14h15m38.ˢ6, +32° 54′ 42″). Center: CMD with a 13 Gyr, [Fe/H] = −2.2 isochrone overlaid. Right: proper motions of members overlaid on Milky Way foreground stars.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Absolute V-band magnitude (M  V ) vs. half-light radius (r h) plane showing both the dwarf galaxy (black markers) and globular cluster (blue “X” marks) populations. We show both candidate and spectroscopically confirmed dwarf galaxies within 300 kpc of the Milky Way. Boötes V is shown as a yellow triangle.
Paper: Discovery of a New Local Group Dwarf Galaxy Candidate in UNIONS: Boötes V
Authors: Simon E. T. Smith, Jaclyn Jensen, Joel Roediger, Federico Sestito, Christian R. Hayes, Alan W. McConnachie, Jean-Charles Cuillandre, Stephen Gwyn, Eugene Magnier, Ken Chambers, Francois Hammer, Mike J. Hudson, Nicolas Martin, Julio Navarro, Douglas Scott
Figure caption: Resulting 1D distributions of key parameters from orbital MCMC analysis. It is estimated to take ∼1.4 Gyr for Boötes V to travel between pericenters, and it has been ∼0.5 Gyr since last pericenter.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Diagram of the SETI Ellipsoid, which has its foci at the source event (purple dot) and Earth (green dot). The blue dashed line represents the information front of the source event; stars outside this sphere (blue dot 1) have not yet observed the event. Stars outside the ellipsoid (orange dot 2) have observed the event, and if they transmitted a signal upon observation, such a signal would arrive at Earth in the future. For stars on the ellipsoid (pink dot 3), their synchronized transmission would be observable on Earth now; at any time, these are the current technosignature candidates. Signals from stars inside the ellipsoid (red dot 4) would have been received on Earth in the past.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: The angles of observation for the Seto scheme. Synchronized signals from stars along the four blue lines, which correspond to two conical shells when rotated about the horizontal axis, will be observable on Earth now; these systems are the current technosignature candidates for this signaling framework. The path from the source event through the potentially transmitting civilization to Earth, through a pair of red and blue lines, forms a right angle at a point on the SETI Ellipsoid, where the technosignature candidate is located.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: The top panel shows the spatial distribution of all 868 candidates selected via the SETI Ellipsoid and Seto methods for all four SNe, with crossing times within the date range of available Gaia light curves, combining the targets from Figures 8 and 6. The bottom panel displays the color–magnitude diagram of these targets, each marked with its Gaia variable type classification.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Current SETI Ellipsoid with SN 1987A as the source event, in galactocentric Y and Z coordinates. The red dots are stars that have not yet seen SN 1987A; the blue dots have seen it, but are outside the SETI Ellipsoid. The pink dots are stars inside the SETI Ellipsoid, and the black dots are those within 0.1 ly of the SETI Ellipsoid.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Seto scheme crossing time diagram with SN 1054 as the source event. This scheme covers half the sky, centered at SN 1054, with two rings, one expanding with time and one contracting. The contour lines show the progression of these two rings. For SN 1054, the search window closes at around the year 3620, corresponding to a normal time of ﹩\sqrt{2}-1﹩.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Crossing time diagram for the SETI Ellipsoid with SN 1987A as the source event, in galactocentric Y and Z coordinates, with ﹩\left|X\right|\lt 150﹩ pc. The vast majority of stars will not be on the SETI Ellipsoid for thousands of years. The contour lines show the growth of the Ellipsoid.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Stars with Seto scheme crossing times within dates of available Gaia light-curve data for SNe 1604, 1572, and 1054. Each supernova has two rings of candidates, corresponding to the θ + and θ − rings. There are 403 candidates total.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Two-dimensional histogram of the distance uncertainties for the variable stars in Gaia DR3, with distances less than 5000 lyr. The median and mode distance uncertainties are shown in the dashed and solid lines, respectively. Stars with a distance uncertainty less than 1 lyr are the most ideal; there are 43,237 such stars total, mostly at low distances.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: SETI Ellipsoid target selection for SNe 1987A, 1604, 1572, and 1054, in galactocentric X and Z coordinates. The red dots are the 465 stars with SETI Ellipsoid crossing times, including error bounds, within the dates of available Gaia epoch photometry. The light blue dots are background stars.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: (a) Full, left, and right light curves and their Lomb–Scargle Periodograms for two eclipsing binaries. The left panel has the highest-interest index and the right panel is near the middle of the interest rankings. The analysis seems to successfully fold the data both before and after the crossing time, and there is a small but noticeable change in the double Gaussian eclipsing binary fit between the left and right light curves, though this is most likely due to sparse sampling. It is difficult to distinguish between eclipsing binaries with high interest, as we do not normally expect the variability parameters for an eclipsing binary to change, so the left and right light curves should be similar. (b) Lomb–Scargle Periodograms and light curves for two eclipsing binaries with some of the lowest-interest indices. The periodograms are unable to find strong peak frequencies and the double Gaussian fit fails in these two panels, indicating that the analysis and ranking system successfully assigns low interest to targets that do not have clean data.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Sample candidate light curve with SN 1987A light curve overlain in green. The red dots show the SN light curve interpolated to match the Gaia light-curve data points; the orange dots are the same for a top-hat function with width equal to the FWHM of the SN light curve, a baseline equal to a normalized flux of 1, and a peak equal to the maximum normalized flux of the stellar light curve. The vertical blue line indicates the crossing time of the star, which is where the supernova light curve and top-hat function begin. The timescale of the SN, on the order of hundreds of days, is close to that of the Gaia epoch photometry sampling and is also longer than the periods of most stars that are classified as variable by Gaia. This approach would be better suited to a data set that has denser time sampling and is not limited to only variable stars.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Sample light curve for one of the selected targets, with solar-like variable type classification, in the three Gaia bands: G, BP, and RP. The solid vertical line marks the crossing time, via either the SETI Ellipsoid or the Seto scheme. The solid horizontal lines denote the median flux, calculated separately before and after the crossing time, and the dashed horizontal lines are the ±3 × median absolute deviation (MAD) levels. This target is a candidate from the SETI Ellipsoid method, so we include the crossing time error due to the stellar distance uncertainty, which is denoted by the vertical dashed lines. The data are noticeably sparse and incomplete, consisting of only three years of Gaia observations, but have long-term stability.
Paper: Signal Synchronization Strategies and Time Domain SETI with Gaia DR3
Authors: Andy Nilipour, James R. A. Davenport, Steve Croft, Andrew P. V. Siemion
Figure caption: Light curves in all three Gaia bands for the most (top panel) and least (bottom panel) interesting targets not classified as variable stars, formatted in the same manner as in Figure 10. The most interesting candidate displays a nonsignificant but noticeable shift in the median flux before and after the crossing time, as well as possible increase in the scatter. The best-fit slope also appears to be strongly negative before the crossing time but near-horizontal afterward. On the other hand, the least interesting candidate shows almost zero change in the median flux, and seemingly small change in the scatter and best-fit slope.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Histograms showing the BB magnitudes and colors for the full sample of SFACT emission-line candidates from the three pilot-study fields (N = 533). Upper left: r-band magnitude distribution, with a median value of r = 22.51 and a faint limit of r ∼ 25.8. Upper right: i-band magnitude distribution, with a median value of i = 22.15. Lower left: g-band magnitude distribution, with a median value of r = 23.18 and a faint limit of g ∼ 26.3. Lower right: g−r color distribution, with a median value of 0.65. While the bulk of the galaxies have observed colors between 0.2 <g−r 1.2, many objects with extreme colors are present in the sample.
Paper: The Star Formation Across Cosmic Time (SFACT) Survey. I. Survey Description and Early Results from a New Narrowband Emission-line Galaxy Survey
Authors: John J. Salzer, David J. Carr, Jennifer Sieben, Samantha W. Brunker, Alec S. Hirschauer
Figure caption: Left: filter tracings of the three NB filters currently in use with SFACT. Right: plot showing the wavelength coverage of the SFACT NB filters as well as the redshift ranges associated with the detection of strong optical nebular emission lines. Each vertical column represents a specific NB filter, while the vertical location of each rectangular box represents the redshift range for the emission line indicated. We show the redshift windows only for Hα, [O III]λ5007, and [O II]λ3727; the majority of the SFACT candidates are detected via one of these three lines. Also shown are the two additional filters that we plan to add to the survey. The plot on the right-hand side compresses the wavelength scale in order to better illustrate the distribution of the redshift windows covered by the survey.