adsabs/AstroCLIMB huggingface dataset:
Paper: Environmental Effects in Herschel Observations of the Ionized Carbon Content of Star-forming Dwarf Galaxies in the Virgo Cluster 
Authors: Robert Minchin, Dario Fadda, Rhys Taylor, Boris Deshev, Jonathan Davies
Figure caption: Spectral Energy Distributions of the 14 galaxies in the sample. Measured data points are shown as orange circles; error bars are shown on these data points but may be smaller than the symbol used. The best-fit SED from MAGPHYS is shown as a solid blue line with its χ 2 given in the upper-right.
Paper: Environmental Effects in Herschel Observations of the Ionized Carbon Content of Star-forming Dwarf Galaxies in the Virgo Cluster 
Authors: Robert Minchin, Dario Fadda, Rhys Taylor, Boris Deshev, Jonathan Davies
Figure caption: Herschel [C II] line intensity maps and spatially integrated spectra for the fourteen galaxies in the sample. Spectra show the Herschel spectrum (solid blue line) and the fitted line profile from SOSPEX (orange dashed line).
Paper: Gemini-LIGHTS: Herbig Ae/Be and Massive T Tauri Protoplanetary Disks Imaged with Gemini Planet Imager
Authors: Evan A. Rich, John D. Monnier, Alicia Aarnio, Anna S. E. Laws, Benjamin R. Setterholm, David J. Wilner, Nuria Calvet, Tim Harries, Chris Miller, Claire L. Davies, Fred C. Adams, Sean M. Andrews, Jaehan Bae, Catherine Espaillat, Alexandra Z. Greenbaum, Sasha Hinkley, Stefan Kraus, Lee Hartmann, Andrea Isella, Melissa McClure, Rebecca Oppenheimer, Laura M. Pérez, Zhaohuan Zhu
Figure caption: 33 targets with 1.4 M⊙< stellar Mass <8 M⊙ comparing the Q ϕ /Fstar ratio to the system parameters of WISE 2 (W2, 4.6 μm)–WISE 4 (W4, 22 μm) color (upper right), W2–W4 color of only nonbinary systems (upper left), system age/ZAMS age (bottom left), and stellar mass (bottom right). The target shapes and colors refer to their classification (Group I-blue squares, Group II-orange circles, FS CMa-green diamonds) and the shape filling refers to the binarity (filled shapes: inner and outer binary; edge filled: outer binary; inner filled: inner binary; no filling: no binary). Outer binaries are exterior to the IWA and in the FOV as discussed in Section 3.4. Inner binaries are spectroscopic binaries from the literature. Error bars are plotted under the symbols with down pointing errors indicating the 2σ upper limit uncertainty.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Left: representative haze forward models compared to the measured WFC3 spectrum; models for the clear atmospheres of 1 (dark green line), 10 (orange line), and 100 (purple line) × solar metallicity, and those for the hazy (tholin) atmospheres of 1 (pink line), 10 (light green line), and 100 (yellow line) × solar metallicity. The haze formation efficiency that fits the observed data well is chosen. Right: goodness of fit for the full grid of tholin and soot models. The grid cell shading indicates the reduced χ 2 of the fit to the WFC3 data. The fit has 18 degrees of freedom (21 data points, free parameters for metallicity, f haze, and reference radius).
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: The transmission spectrum of HD 106315c (points with 1σ uncertainties) compared to retrieved spectra from the FULL model (teal shading) with petitRADTRANS. The H2/He atmospheric scale height is indicated on the right y-axis, assuming a solar composition atmosphere at the planet’s equilibrium temperature (the true scale height is likely smaller, due to enhanced metallicity and/or lower temperature). The tentative detection of water absorption is driven by the small increase in transit depth near 1.4 μm.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Pressure–temperature profiles (solid lines) for HD 106315c compared to condensation curves for expected cloud species (dashed lines). The models are assumed to be in radiative–convective and chemical equilibrium. The condensation curves are calculated for a 100× solar metallicity composition; for lower metallicities, the condensation curves shift left (by approximately 100 K per 1 dex metallicity). The shaded region marks the range of pressures that transmission spectroscopy is sensitive to, assuming 100× solar metallicity.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Molecular abundance and cloud property constraints from the SCARLET free retrieval analysis. The top panels in each column show the 1D marginalized posterior distributions of the molecular abundances and cloud properties, with dashed vertical lines in the histograms indicating the marginalized 16th, 50th, and 84th credible intervals. The subjacent 2D panels show the correlations among the gases and cloud properties, with the black, dark gray, and light gray regions corresponding to the 1σ (39.3%), 2σ (86.5%), and 3σ (98.9%) credible intervals. The cloud pressure is given in logarithm (base 10) Pascals, and the abundances are given as the logarithm (base 10) of their volume mixing ratio.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: The retrieved atmospheric properties for the full retrieval with petitRADTRANS. The panels show the posterior distribution of parameters from the nested sampling run. Darker shading corresponds to higher posterior probability. The diagonal shows a one-dimensional histogram for each parameter, with dotted lines denoting the median and 1σ credible interval. The molecular abundances are the logarithm (base 10) of their volume mixing ratio. For reference, a solar composition gas at 1 mbar pressure and 800 K has ﹩{n}_{{{\rm{H}}}_{2}{\rm{O}}}\,=\,﹩−3.65, n CO2 = −6.32, n CO = −3.37, ﹩{n}_{{\mathrm{CH}}_{4}}\,=\,﹩−4.43, and ﹩{n}_{{{\rm{N}}}_{2}}\,=\,﹩−4.23.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: The light curve of HD 106315c observed with the 4.5 μm filter of Spitzer. The left panel shows the best-fit transit model to the binned light curve after removing detector systematics. The blue points with error bars are the data points binned further for visual clarity. The right-hand panel shows the residuals of the best-fit model from the data.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: Allan deviation plots showing the rms variation as a function of bin size for the HST/WFC3 transit light curves. A bin size of 10 points corresponds to 30 minutes. The red dotted lines show the expected ﹩\sqrt{N}﹩ trend for photon-limited, white noise. The black lines show the measured rms for each light curve.
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: A sample of cloud forward models compared to the observed WFC3 spectrum (left) and a goodness of fit for the full grid of cloudy models (right). The grid cell shading indicates the reduced χ 2 of the fit to the WFC3 data. The fit has 18 degrees of freedom (21 data points, free parameters for metallicity, f sed, and reference radius).
Paper: Tentative Evidence for Water Vapor in the Atmosphere of the Neptune-sized Exoplanet HD 106315c
Authors: Laura Kreidberg, Paul Mollière, Ian J. M. Crossfield, Daniel P. Thorngren, Yui Kawashima, Caroline V. Morley, Björn Benneke, Thomas Mikal-Evans, David Berardo, Molly R. Kosiarek, Varoujan Gorjian, David R. Ciardi, Jessie L. Christiansen, Diana Dragomir, Courtney D. Dressing, Jonathan J. Fortney, Benjamin J. Fulton, Thomas P. Greene, Kevin K. Hardegree-Ullman, Andrew W. Howard, Steve B. Howell, Howard Isaacson, Jessica E. Krick, John H. Livingston, Joshua D. Lothringer, Farisa Y. Morales, Erik A. Petigura, Joseph E. Rodriguez, Joshua E. Schlieder, Lauren M. Weiss
Figure caption: HST/WFC3 transmission spectra from two independent pipelines. The black circles are from the model-ramp analysis used by L. Kreidberg, whereas the red squares come from the common-mode error correction from T. Mikal-Evans.
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Our fully reduced, combined, and continuum subtracted moderate-resolution OSIRIS K-band spectra of VHS 1256 b plotted alongside three models of T = 1240 K and logg = 3.2 with varying C/O. The top panel shows the supersolar H2O model with C/O = 0.0142 in blue. The middle panel shows our best-fit model with subsolar H2O and solar CO and CH4, which gives C/O = 0.590. The bottom panel shows a supersolar CO model with C/O = 0.993. This demonstrates how well moderate-resolution spectroscopy can constrain C/O ratios of planetary mass objects.
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Our fully reduced, combined, and flux calibrated moderate-resolution OSIRIS K-band spectra of VHS 1256 b in black, plotted alongside our best-fit model with two different grain sizes, 3 μm in gray and 0.5 μm in pink; and spectra from Miles et al. (2018) in blue; spectra from Gauza et al. (2015) in orange; and magnitudes from Rich et al. (2016) in green, Skrutskie et al. (2006) in magenta, and McMahon et al. (2013) in cyan. The 3 μm grain size model fits the majority of the data except for the red end of the L-band spectra and the Rich et al. (2016) photometry point. The 0.5 μm grain size model underpredicts the flux in the optical, J, and H band, but does fit the L-band spectra and photometry point. We adopt the 3 μm model as the best-fit for the majority of the available data.
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Corner plot from our MCMC fits for our continuum subtracted OSIRIS K-band spectra. The diagonal shows the marginalized posteriors. The covariances between all the parameters are in the corresponding 2-d histograms. The blue lines represent the 50 percentile, and the dotted lines represent the 16 and 84 percentiles. The “flux mult” corresponds to the dilution factor that scales the model by (radius)2(distance)−2. Our fit prefers a value near the edge of the grid for pgs, or, P  cloud .
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Results of T eff = 1240 K, ﹩\mathrm{log}g=3.25﹩, ﹩\mathrm{log}{P}_{\mathrm{cloud}}=6﹩, and grain size = 3 μm model fits with varying mole fractions for both H2O, CO, and CH4 to our continuum-subtracted OSIRIS spectrum. The mole fractions are given in units relative to the ratio in the Sun, such that a value of zero implies the solar value. The scalings of CO prefer solar/subsolar and the scalings of H2O prefer values subsolar. From these fits we find C/O = ﹩{0.869}_{-0.24}^{+0.09}﹩.
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Left: the results of our χ 2 analysis on the first half of our continuum subtracted OSIRIS data. The CO abundances vary minimally during this analysis because of the lack of CO lines in the first half of our spectra. The best-fit water is still subsolar, with the lowest χ 2 values not including solar. Right: the results of our χ 2 analysis on the second half of our continuum subtracted OSIRIS data. The values allowed by the χ 2 analysis include the solar abundance model, with the best-fit H2O molecular abundance being slightly subsolar.
Paper: Moderate-resolution K-band Spectroscopy of the Substellar Companion VHS 1256 b
Authors: Kielan K. W. Hoch, Quinn M. Konopacky, Travis S. Barman, Christopher A. Theissen, Laci Brock, Marshall D. Perrin, Jean-Baptiste Ruffio, Bruce Macintosh, Christian Marois
Figure caption: Our OSIRIS continuum subtracted K-band spectra in black plotted against our MCMC best-fit model in magenta. The bump in the center of the spectrum between 2.1 and 2.2 μm is due to residual telluric. By removing the continuum, we remove uncertainties that were tied to the continuum, thus the residuals for the flatted fit are much smaller.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: The SED of a model galaxy with age = 100 Myr, stellar metallicity, Z ⋆  =  0.2 Z ⊙, and a constant star formation history. The model is generated using BAGPIPES (Carnall et al. 2018) and is redshifted to z = 2.65. Wavelengths corresponding to Lyα and [O II] emission lines at this redshift are marked. The broadband filters BW, R, I, F110W, and F160W that are used in this analysis are shown from left to right in blue below. Similarly, the intermediate-band filters, IA445 and F139M, which probe the Lyα and [O II] lines, respectively, are shown in red.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Example SEDs with their best-fit model. Image cutouts (5″ × 5″) of the LAEs in different bands (BW, IA445, R, I, F110W, F139M, and F160W from left to right) are shown at the top of each panel for each LAE. The green circles on the images are the apertures used for performing photometry. The top, middle, and bottom panels show examples of good, acceptable, and uncertain SED fits, respectively. The blue circles in each panel are flux densities in the BW (corrected for Lyα flux), R, I, F110W, and F160W bands (from left to right in each panel) that are used for the SED fitting. The minimum χ 2 best-fit SED is overplotted, with the χ 2 value shown on the plot. The red points show the IA445 and F139M flux densities, which probe the Lyα and [O II] emission lines, respectively. The pink shaded regions mark the wavelength range of these filter passbands.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Position of LAEs relative to the SFMS on the ﹩\mathrm{log}\,{\text{}}{M}_{\star }﹩ vs. ﹩\mathrm{log}\,\mathrm{SFR}﹩ space. The samples of zLAEs and pLAEs are plotted as filled blue squares and open blue circles, respectively. The MOSDEF comparison SFGs are shown as gray crosses. Previous results of LAEs from Hagen et al. (2016; shown as H16) and Shimakawa et al. (2017; shown as Sh17) are displayed as orange diamonds and magenta stars, respectively. The main-sequence parameterizations computed by Whitaker et al. (2014), Schreiber et al. (2015), and Shivaei et al. (2015) are extended to lower masses and overplotted as dotted, dashed, and solid lines, respectively.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Overlap of the seven HST fields on the distribution of LAEs (shown in gray) from Prescott et al. (2008). The DENS and FIELD fields of view are shown in blue and red, respectively. The LAEs studied in this paper (see Section 3.2) are marked as blue and red points, depending on their HST fields.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Color–magnitude diagram ((IA445 − BW) vs. IA445) of all detected sources from the seven HST fields is shown by the 2D gray-scale histogram. The black dashed line denotes the criterion used for the selection of LAE candidates. The LAEs with confirmed spectroscopic redshifts in the range 2.55 ≤ z ≤ 2.75 are shown as filled blue squares (zLAEs), while the photometric candidates are shown as open blue circles (pLAEs).
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Distribution of stellar mass (top left), SFR (top right), age (bottom left), and dust reddening (bottom right) of the LAEs computed from the SED fitting. In each of the panels, the dark blue shaded bars are the zLAEs, while the light blue shaded bars are the pLAEs. The distributions of typical SFGs are overplotted in hatched gray. The median values of each parameter for the LAEs and SFGs are marked by dotted blue and gray vertical lines, respectively. The histograms in all the panels are normalized by the total number of sources.
Paper: Lyα Escape from Low-mass, Compact, High-redshift Galaxies
Authors: Ragadeepika Pucha, Naveen A. Reddy, Arjun Dey, Stéphanie Juneau, Kyoung-Soo Lee, Moire K. M. Prescott, Irene Shivaei, Sungryong Hong
Figure caption: Redshift distribution of zLAEs and the comparison SFGs studied in this paper. The zLAEs are shown in filled blue, while the SFGs are shown in hatched gray. The median redshift of the zLAEs is ≈2.66, whereas we assume z = 2.65 for the pLAEs.
Paper: ARMADA. II. Further Detections of Inner Companions to Intermediate-mass Binaries with Microarcsecond Astrometry at CHARA and VLTI
Authors: Tyler Gardner, John D. Monnier, Francis C. Fekel, Jean-Baptiste Le Bouquin, Adam Scovera, Gail Schaefer, Stefan Kraus, Fred C. Adams, Narsireddy Anugu, Jean-Philippe Berger, Theo Ten Brummelaar, Claire L. Davies, Jacob Ennis, Douglas R. Gies, Keith J. C. Johnson, Pierre Kervella, Kaitlin M. Kratter, Aaron Labdon, Cyprien Lanthermann, Johannes Sahlmann, Benjamin R. Setterholm
Figure caption: We plot the best-fit inner “wobble” motions due to newly detected companions, with the outer binary motion of Figure 1 subtracted. This motion represents the center of light (i.e., the primary star in cases with negligible secondary flux) of the inner orbit orbiting the center of mass. The “wobbles” here range from ∼50 μas to a few mas, with median residuals to the joint RV+astrometry fit of a few tens of μas. We discover two inner components in HD 5143 (Aa,Ab + Ba,Bb), so in this case the inner orbit measuring Aa to Ba has a “wobble” motion of its own. The shaded gray regions again depict 100 randomly sampled orbits from the MCMC chains. Since the “wobble” motion also depends on the subtraction of the outer orbit, the errors on the inner orbits appear larger than expected from the plotted data in some cases.