adsabs/AstroCLIMB huggingface dataset:
Paper: A Photometric and Spectroscopic Study of the Short-period Algol EW Boötis with a δ Sct Pulsator
Authors: Hye-Young Kim, Kyeongsoo Hong, Chun-Hwey Kim, Jae Woo Lee, Min-Ji Jeong, Jang-Ho Park, Mi-Hwa Song
Figure caption: The TESS photometric data of Sector 23 and 24 for EW Boo. The gray circles in the upper panel indicate the original SAP flux. In the bottom panel, the black circles represent the SAP magnitudes after detrending.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Comparison of the space densities of various phases of massive galaxy evolution. The black star represents the modeled space density for compact starburst galaxies like those in our observed sample. Its error bar along the redshift axis represents the size of the redshift range of our sources, and the error bar along the space density axis is the statistical uncertainty calculated via bootstrapping as described in Section 5.2. We note that there are additional systematic errors, including uncertainty with model assumptions, that make this statistical error a lower limit. The blue squares represent the space density evolution of massive, compact star-forming galaxies from the CANDELS survey (Barro et al. 2013), the red points represent massive (﹩\mathrm{log}{M}_{* }/{M}_{\odot }\sim 11﹩), compact quiescent galaxies (van der Wel et al. 2014), the green triangle represents low-z PSBs (Pattarakijwanich et al. 2016), and the purple hexagon represents low-z ULIRGs (Kim & Sanders 1998). The gray, red, purple, and green shaded regions depict the Lotz et al. (2011) observed merger rate density, the Stott et al. (2013) observed merger rate density (calculated using merger observability timescales), ULIRG space density (Magnelli et al. 2011), and intermediate-z PSB space density (Wild et al. 2016) ranges, respectively. The Barro et al. (2013) points, Lotz et al. (2011) region, and Stott et al. (2013) region have been adjusted to account that our sources have masses ﹩\mathrm{log}{M}_{* }/{M}_{\odot }\gt 10.5﹩, while most of the other populations shown include galaxies ﹩\mathrm{log}{M}_{* }/{M}_{\odot }\gt 10﹩. While only a relatively small fraction of intermediate-z major mergers will result in an extreme compact starburst similar to those in our sample, it is likely that sources like ours are the more extreme, lower-z analogs to compact star-forming galaxies more common in the early universe and are closely related to intermediate-z PSBs.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Panel (a): Best-fit SED for galaxy J01713+2817. The red points and error bars are the observed photometry and ±0.25 mag uncertainty region, respectively. The open black squares are the modeled photometry. The blue, violet, and green curves are the modeled SED for the total galaxy system, nuclear burst, and host galaxy, respectively. Panel (b): Triangle plot of parameter posterior distributions for galaxy J01713+2817. We calculate the mean and covariances of these posterior distributions in order to model them as 4D-Gaussian distributions. We then randomly draw sets of parameter values from the Gaussian-modeled posterior in order to construct a mock population of compact starbursts. Panel (c): Galaxy cutout as seen in Figure 1.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Panel (a): Best-fit SED for galaxy J1613+2834. The red points and error bars are the observed photometry and ±0.25 mag uncertainty region, respectively. The open black squares are the modeled photometry. The blue, violet, and green curves are the modeled SED for the total galaxy system, nuclear burst, and host galaxy, respectively. Panel (b): Triangle plot of parameter posterior distributions for galaxy J1613+2834. We calculate the mean and covariances of these posterior distributions in order to model them as 4D-Gaussian distributions. We then randomly draw sets of parameter values from the Gaussian-modeled posterior in order to construct a mock population of compact starbursts. Panel (c): Galaxy cutout as seen in Figure 1.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Panel (a): Best-fit SED for galaxy J1506+6131. The red points and error bars are the observed photometry and ±0.25 mag uncertainty region, respectively. The open black squares are the modeled photometry. The blue, violet, and green curves are the modeled SED for the total galaxy system, nuclear burst, and host galaxy, respectively. Panel (b): Triangle plot of parameter posterior distributions for galaxy J1506+6131. We calculate the mean and covariances of these posterior distributions in order to model them as 4D-Gaussian distributions. We then randomly draw sets of parameter values from the Gaussian-modeled posterior in order to construct a mock population of compact starbursts. Panel (c): Galaxy cutout as seen in Figure 1.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Panel (a): Best-fit SED for galaxy J1558+3957. The red points and error bars are the observed photometry and ±0.25 mag uncertainty region, respectively. The open black squares are the modeled photometry. The blue, violet, and green curves are the modeled SED for the total galaxy system, nuclear burst, and host galaxy, respectively. Panel (b): Triangle plot of parameter posterior distributions for galaxy J1558+3957. We calculate the mean and covariances of these posterior distributions in order to model them as 4D-Gaussian distributions. We then randomly draw sets of parameter values from the Gaussian-modeled posterior in order to construct a mock population of compact starbursts. Panel (c): Galaxy cutout as seen in Figure 1.
Paper: The Space Density of Intermediate-redshift, Extremely Compact, Massive Starburst Galaxies
Authors: Kelly E. Whalen, Ryan C. Hickox, Alison L. Coil, Aleksandar M. Diamond-Stanic, James E. Geach, John Moustakas, Gregory H. Rudnick, David S. N. Rupke, Paul H. Sell, Christy A. Tremonti, Julie D. Davis, Serena Perrotta, Grayson C. Petter
Figure caption: Panel (a): Best-fit SED for galaxy J2118+0017. The red points and error bars are the observed photometry and ±0.25 mag uncertainty region, respectively. The open black squares are the modeled photometry. The blue, violet, and green curves are the modeled SED for the total galaxy system, nuclear burst, and host galaxy, respectively. Panel (b): Triangle plot of parameter posterior distributions for galaxy J2118+0017. We calculate the mean and covariances of these posterior distributions in order to model them as 4D-Gaussian distributions. We then randomly draw sets of parameter values from the Gaussian-modeled posterior in order to construct a mock population of compact starbursts. Panel (c): Galaxy cutout as seen in Figure 1.
Paper: The Upper Edge of the Neptune Desert Is Stable Against Photoevaporation
Authors: Shreyas Vissapragada, Heather A. Knutson, Michael Greklek-McKeon, Antonija Oklopčić, Fei Dai, Leonardo A. dos Santos, Nemanja Jovanovic, Dimitri Mawet, Maxwell A. Millar-Blanchaer, Kimberly Paragas, Jessica J. Spake, Samaporn Tinyanont, Gautam Vasisht
Figure caption: Transiting exoplanets with fractional mass uncertainties of less than 30%, with the dashed lines indicating the Neptune desert boundaries from Mazeh et al. (2016). Planets orbiting stars with 4000 K < T eff < 5400 K are outlined in red, and the seven targets constituting our sample are outlined in blue. The point color denotes the host star’s J magnitude, and the point size is proportional to the logarithm of the predicted signal-to-noise ratio (S/N) in the Wide-field InfraRed Camera (WIRC) helium bandpass from Section 2.1.
Paper: Fragment Dynamics in Active Asteroid 331P/Gibbs
Authors: Man-To Hui, 文韜 許, David Jewitt
Figure caption: Upper three panels: separation velocities decomposed into radial, transverse, and normal components (color coded) of Fragments A (left), B (middle), and C (right) split from the primary of 331P needed in order to best fit the astrometry as functions of fragmentation epoch (here expressed as number of years past J2000). Lower panel: normalized rms residuals (the goodness of fit divided by twice the number of observations) of the best fits for Fragments A, B, and C (distinguished by colors) varied with split epoch. The shaded region represents the range of possible impulsive activation epochs of 331P inferred from the tail morphology by Stevenson et al. (2012; 2011 July 7 ± 20), with the nominal value marked by the vertical line. The dotted lines in gray in the upper panels indicate split epochs rendering solutions with corresponding local minimum normalized rms residual. Note the best normalized rms for Fragment C is worse than those for the other two fragments by an order of magnitude.
Paper: Fragment Dynamics in Active Asteroid 331P/Gibbs
Authors: Man-To Hui, 文韜 許, David Jewitt
Figure caption: Schematic diagram showing plausible relations between the four brightest components of 331P. Texts in dark red and blue respectively label the fragmentation epoch and the separation speed with respect to the pairwise parent components. Dotted arrows indicate the existence of more than a single possible pairwise relationship. Two plausible split scenarios were found for the pair of Fragments B and C, with the major difference in the split epoch.
Paper: Fragment Dynamics in Active Asteroid 331P/Gibbs
Authors: Man-To Hui, 文韜 許, David Jewitt
Figure caption: Same as Figure 2 but for pairwise combinations between the fragments themselves. The normalized rms residuals all have two local minima in the investigated split epoch range, but only in the pair of Fragments B and C are the local minima comparable to each other, as well as to those for Fragments A and B in Figure 2.
Paper: Fragment Dynamics in Active Asteroid 331P/Gibbs
Authors: Man-To Hui, 文韜 許, David Jewitt
Figure caption: Identification of the primary body, 331P, and the three brightest fragments 331P-A, -B, and -C, analyzed in this work. A dust trail is evident spanning the image and other fragments are visible in the figure but are not studied here. The region shown is ∼7.5  ×  104 km in width projected to the distance of the object. J2000 equatorial north is up and east is left. A scale bar of 10″ in length is given on the lower right corner.
Paper: Fragment Dynamics in Active Asteroid 331P/Gibbs
Authors: Man-To Hui, 文韜 許, David Jewitt
Figure caption: Ephemeris positional differences between the possible fragmentation scenarios of Fragments A (red) and C (blue) from 2020 to 2030. The sawtooth features in the curve of Fragment A are artifacts due to the fact that the positional difference approaches the output precision limit of the computed J2000 equatorial coordinates in the ephemerides.
Paper: Dynamical Star-forming History of Per OB2
Authors: Marina Kounkel, TingYan Deng, Keivan G. Stassun
Figure caption: HR diagram for all the groups in the sample. The solid black line shows the best-fitted MIST isochrone (Choi et al. 2016) from Table 2. The dashed lines show the isochrone 0.2 dex younger and 0.2 dex older. The thin gray line shows the main sequence, and the thin dotted line is the field binary sequence, included for reference to estimate contamination. In the California cloud, gray sources have PMS probabilities <90% as measured by Sagitta. (Note that the classifier may also exclude the youngest stars with ages ≲0.5 Myr, due to their rarity in the training set)
Paper: Dynamical Star-forming History of Per OB2
Authors: Marina Kounkel, TingYan Deng, Keivan G. Stassun
Figure caption: Top left: Distribution of candidate members identified toward the California Cloud, color-coded by the age estimated via Sagitta (McBride et al. 2021). Top right: proper motions of stars in the reference frame of the California cloud, color-coded by their parallax. Bottom left: Kernel density estimate of the overall distribution of parallaxes of stars within the California cloud, shown in blue. Red curve shows the simulated distribution of parallaxes for a compact population at a distance typical of the California cloud, broadened by the parallax uncertainties of the stars. Bottom right: velocity gradients with distances of all three dimensions of motion.
Paper: Dynamical Star-forming History of Per OB2
Authors: Marina Kounkel, TingYan Deng, Keivan G. Stassun
Figure caption: Spatial distribution on the sky of 810 stars in the identified groups toward Per OB2, color-coded by their age. Gray dots correspond to 1171 PMS stars from McBride et al. (2021) with PMS probability >90% within the same volume of space.
Paper: Dynamical Star-forming History of Per OB2
Authors: Marina Kounkel, TingYan Deng, Keivan G. Stassun
Figure caption: Distribution of individual young stars toward Perseus along the three-dimensional projection. Sources are color-coded by the age of their parent group, similarly to those in Figure 1. The size of each symbol is inversely correlated with the parallax uncertainty (ranging from <0.02 mas to 0.3 mas), with larger symbols having a firmer distance measurement.
Paper: Dynamical Star-forming History of Per OB2
Authors: Marina Kounkel, TingYan Deng, Keivan G. Stassun
Figure caption: A comparison of spatial distribution candidate members for five groups presented in Pavlidou et al. (2021; down to G < 18 mag) and the corresponding groups in this work.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: BTFR for normal galaxies (black circles, from the AGES Virgo background fields) and a selection of optically dark H I clouds, using the W50 (left) and W20 (right) estimates for the line width. The line widths are corrected for inclination for the galaxies but not the H I clouds. The baryonic mass for the clouds is computed using their H I mass multiplied by a factor 1.36 to account for the presence of helium. The dashed line is the best fit to the optically bright galaxies. Our main sample of Leo clouds are shown with red squares, while additional objects in Leo are shown as open red squares (highlighted with orange circles in Figure 3; cloud 7 is shown in Figure 5). Clouds from the Virgo surveys of AGES are shown with open blue circles, while other clouds in the Virgo Cluster are shown as labeled open blue squares. Other clouds in green are described in Section 4.6. The solid line in the left panel shows the completeness line for an integrated S/N of 6.5.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: BTFR using more sophisticated corrections for velocity width (derived for our sample from W20) and stellar mass, following the prescriptions of McGaugh (2012) and Springob et al. (2005)—for full details see Appendix. The color scheme is as for Figure 6, except that the open circles show the sample of McGaugh (2012, his Table 1). The black solid line shows the best-fit relation according to McGaugh (2012), with the dashed and dotted lines showing the 1σ (0.24 dex in mass) and 2σ scatter, respectively, again according to McGaugh (2012). Clouds from non-AGES samples are not included, as we lack the data needed to make the appropriate corrections to velocity width, which is corrected for inclination, spectral resolution, and cosmological expansion.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: Clouds 1–3. The top row shows renzograms with the contour at 3.5σ and the Arecibo 3.′5 beam (equivalent diameter 11.3 kpc) as a green line, overlaid on an a RGB image from the SDSS. The middle row shows the spectra—red dashed lines show the profile window used for computing the H I parameters, blue circles show the positions of the W50 measurement, and blue squares show the W20 values. The bottom row shows the stacked g, r, i bands from the SDSS, with the black circle showing the Arecibo beam size, centered on the coordinates of the H I detections.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: Renzogram of the M95–M96 region. The thick contours are from the standard AGES cube at 3.5σ. The thin contours are from a cube with additional Hanning smoothing (width 15) at 4σ. The green circle in the upper right corner shows the AGES beam. An additional feature tentatively identified as cloud 7 is also shown.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: Same as Figure 1, but for clouds 4−6.
Paper: The Arecibo Galaxy Environment Survey. XII. Optically Dark H I Clouds in the Leo I Group
Authors: Rhys Taylor, Joachim Köppen, Pavel Jáchym, Robert Minchin, Jan Palouš, Jessica L. Rosenberg, Stephen Schneider, Richard Wünsch, Boris Deshev
Figure caption: PV diagram of the M95–M96 region with a linear color stretch, highlighting clouds 1−4.
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Published estimates of the libration amplitudes of three critical resonant angles (ϕ  cb,c , ϕ  cb,c , ϕ Lap) in the GJ 876 system, plotted as a function of the number of radial velocity measurements used in the analysis. These results are taken from Laughlin et al. (2005), Rivera et al. (2005, 2010), Nelson et al. (2016), and Millholland et al. (2018). Measurements from ELODIE, CORALIE, or Lick Observatory are not included in the number of RVs. (Figure adapted from Millholland et al. 2018.)
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Evolution of two critical resonant angles resulting from a numerical integration of the GJ 876 system. The two angles correspond to the 2:1 MMR between planets c and b.
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Phase-space portrait of the approximate first-order resonant motion of HD 128311. The action-angle variables are complicated functions of the planetary orbital elements, but roughly speaking, Ψ is proportional to ∼e 2, and ψ is a combination of the critical angles. The level curves correspond to energy levels of the integrable one-degree-of-freedom Hamiltonian from Batygin & Morbidelli (2013). The dashed line indicates the separatrix, which encloses the crescent-moon-shaped resonant domain. The gray and brown regions indicate several trajectories derived from integrations of the system with parameters drawn from the true posterior distribution (gray) and the simulated distribution with γ = 2 (brown).
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Libration amplitude distributions for the critical angle ϕ 1  =  2λ 2 − λ 1 − ϖ 1 in a synthetic system closely resembling HD 128311. These results correspond to the posterior distributions resulting from the fits to the synthetic radial velocity data with varying levels of Gaussian noise with standard deviation, σ noise. The top and bottom panels correspond to normalized histograms and cumulative histograms, respectively. The dashed black line corresponds to the “true” libration amplitude of the synthetic system.
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Libration amplitude distributions for the critical angle ϕ 1  =  2λ 2 − λ 1 − ϖ 1 in a synthetic system closely resembling HD 128311. The top panel is a duplicate of the Figure 5 top panel for convenience. The bottom panel corresponds to the posterior distributions resulting from the MCMC sampling with a Gaussian-like penalty term included in the prior. The dashed black line corresponds to the “true” libration amplitude of the synthetic system. The medians of the σ noise = 10 m s−1, 20 m s−1, and 40 m s−1 distributions are 23°, 27°, and 37° for the top panel and 22°, 23°, and 21° for the bottom panel.
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: Libration amplitude distributions for the critical angle ϕ 1  =  2λ 2 − λ 1 − ϖ 1 in the HD 128311 system. The result corresponding to the true posterior distribution from Rein (2015) is shown in gray. Additionally, we show the results from four simulated posterior distributions with broadening factors, γ, indicated in the legend. The top and bottom panels correspond to normalized histograms and cumulative histograms, respectively.
Paper: Inferred Properties of Planets in Mean-motion Resonances are Biased by Measurement Noise
Authors: David Jensen, Sarah C. Millholland
Figure caption: One example subplot (﹩\sqrt{{e}_{2}}\cos {\omega }_{2}﹩ vs. P 1) of the full corner plot of the posterior distribution, with the three panels indicating three versions of the simulated distribution with different broadening factors γ. The black (yellow) points correspond to data from the true (simulated) distributions. The simulated distribution in the left panel (γ = 1, no broadening) agrees well with the true distribution.
Paper: ACCESS: Tentative Detection of H2O in the Ground-based Optical Transmission Spectrum of the Low-density Hot Saturn HATS-5b
Authors: Natalie H. Allen, Néstor Espinoza, Andrés Jordán, Mercedes López-Morales, Dániel Apai, Benjamin V. Rackham, James Kirk, David J. Osip, Ian C. Weaver, Chima McGruder, Kevin Ortiz Ceballos, Henrique Reggiani, Rafael Brahm, Florian Rodler, Nikole K. Lewis, Jonathan Fraine
Figure caption: All of the atmospheric models that we tested against our transmission spectrum. The Flat and Flat + Stellar Contamination models are from Exoretrievals, and all the rest are from petitRADTRANS. Their corresponding ﹩\mathrm{ln}Z﹩ values are given in Table 6.