adsabs/AstroCLIMB huggingface dataset:
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Calculated TSM for transiting, long-period, mini-Neptunes from NASA’s Exoplanet Archive (as of 2021 October 29). The log of the TSM is plotted as a function of equilibrium temperature, T eq. Each planet is colored based on the effective temperature of the host star, T eff. The dashed lines denote the suggested JWST TSM cutoff for mini-Neptunes as described in Kempton et al. (2018). We show the calculated TSM for planets in the range of 2.0 R ⊕ ≤ R  P  ≤ 4.0 R ⊕. TOI-712 b, TOI-712 c, and TOI-712 d are shown by the starred points, with a black border. There are very few temperate planets with a high TSM, so while TOI-712 c and TOI-712 d fall below the suggested threshold, they are promising targets for studying atmospheric evolution in the absence of strong irradiation.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Known validated small planets (R  P  ≤ 6.0 R ⊕) in multiplanet systems (as of 2021 October 29, via NASA’s Exoplanet Archive). The host stars’ K-magnitudes are plotted against the orbital periods. The points are colored based on the planet radius. TOI-712 d is one of the longest-period small planets orbiting a bright star. The brightness of the host allows for the planetary radii to be well constrained through photometric observations with relatively few observed transits and also enables future characterization with other facilities.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Results of the dynamical simulations, described in Section 6. Top: the eccentricity variations of the known planets for a period of 300,000 yr, showing the stability of the system and the high-frequency eccentricity oscillations of planets c and d. Bottom: the dynamical simulation results for an Earth-mass planet located in the semimajor axis range 0.3–0.9 au, shown as percentage survival of the simulation as a function of semimajor axis (solid line). As for Figure 7, the CHZ and OHZ are shown in light green and dark green, respectively. The vertical dashed line indicates an example stable resonance location (3:2).
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Ratio of NUV to J-band flux plotted against spectral type for Hyades members (light-purple circles) according to Friend Finder. Younger stars are expected to exhibit enhanced NUV fluxes, while older stars should produce less high-energy flux. The dark-purple star shows the location of TOI-712, which suggests an age consistent with that of the Hyades (∼625  Myr).
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: A top-down view of the TOI-712 system, where the known planets are plotted in black and the candidate planet TOI-712.05 is plotted in gray. The CHZ (purple) spans 0.436–0.802 au, and the OHZ (pink) spans 0.344–0.846 au, coinciding with the orbit of TOI-712 d at its inner edge.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: Young planets (≲1 Gyr) shown with insolation flux received from the host star, in terms of Earth’s insolation flux. The planetary radii for the TOI-712 system (age ≈ 830 Myr) are smaller than most of the youngest planets, though there are no young planets with comparable insolation fluxes.
Paper: TOI-712: A System of Adolescent Mini-Neptunes Extending to the Habitable Zone
Authors: Sydney Vach, Samuel N. Quinn, Andrew Vanderburg, Stephen R. Kane, Karen A. Collins, Adam L. Kraus, George Zhou, Amber A. Medina, Richard P. Schwarz, Kevin I. Collins, Dennis M. Conti, Chris Stockdale, Bob Massey, Olga Suarez, Tristan Guillot, Djamel Mekarnia, Lyu Abe, Georgina Dransfield, Nicolas Crouzet, Amaury H. M. J. Triaud, François-Xavier Schmider, Abelkrim Agabi, Marco Buttu, Coel Hellier, Elise Furlan, Crystal L. Gnilka, Steve B. Howell, Carl Ziegler, César Briceño, Nicholas Law, Andrew W. Mann, Alexander Rudat, Knicole D. Colon, Mark E. Rose, Michelle Kunimoto, Maximilian N. Günther, David Charbonneau, David R. Ciardi, George R. Ricker, Roland K. Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins
Figure caption: A TLS analysis of the three-planet EXOFASTv2 global fit residuals reveals an additional transit signal, with a period of ∼4.32 days. The phase-folded, binned light curve from TESS is shown with a normalized flux.
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Reproduction of the optical red, filter I 8040 Å, continuum image that has been convolved with a Gaussian beam FWHM ∼ 1.″5 × 1.″5 in gray scale and in contours (Garcia-Barreto et al. 1996). The image had not been calibrated in intensity scale, thus the gray-scale stretch is in relative units proportional to noise from 5σ up to 37.7σ, where 1σ = 45 in arbitrary units. Contours are 5, 7, 11, 15, 20, 25, 30, 34, 40, 60, 80, 100, 200, 300, 400, 500, 750, 900 × 1σ. Note the boxy isophotes at radii larger than 5.″0 that delineate a structure straddling the nucleus elongated in P.A. ∼ 52° EofN.
Paper: Ωbar in NGC 5597 from Very Large Array H I 21 cm Observations
Authors: J. Antonio Garcia-Barreto, Emmanuel Momjian
Figure caption: Reproduction of the optical blue continuum image (glass plate 103aO) of the close-pair disk galaxies NGC 5597 at the southeast and NGC 5595 at the northwest, obtained with the OAN-SPM 2.1 m optical telescope in Mexico (Diaz-Hernández et al. 2009). The flux density scale is not calibrated. Gray scale is from 2 → 27.8σ, where σ is the noise in arbitrary units.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: Top: Sky positions for 278 galactic novae with cross-matches from Gaia EDR3 and distances from Bailer-Jones et al. (2021). These events are predominantly located within the galactic midplane. Bottom: Distance versus time since discovery for the 278 novae in our sample. Large uncertainties in distance are the result of faint quiescent luminosities for the novae systems in Gaia, and high extinction.
Paper: Searching the SETI Ellipsoid with Gaia
Authors: James R. A. Davenport, Bárbara Cabrales, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: SETI Ellipsoid diagram for Novae Cygnus 1975 in galactocentric X,Y coordinates, centered on the Earth. Colors for points are the same as in Figure 4. 142 sources with the GCNS are presently located within 0.1 lyr of the SETI Ellipsoid for N Cyg 1975.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Mock reflected light phase curve of the cloudless Earth expanded to spherical harmonic degree l = 25, viewed along the ecliptic. The main plot shows the phase curve over the course of one year. The images at the top show the corresponding progression of the phases of the Earth, from new phase to full phase and back to new phase. Below each image we show a normalized 24 hr segment of the light curve at that phase (blue). Orange dots correspond to the flux computed from brute force numerical integration on a grid of ∼105 points.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Mock secondary eclipse ingress light curves of the cloudless Earth expanded to spherical harmonic degree l = 25, viewed from an orientation where the Earth is occulted behind a solar latitude of 30°. Black curves show the analytic solution; orange dots correspond to brute force numerical integration on a grid of ∼105 points. The top panel shows the light curve in emitted light and is similar to Figure 13 in Luger et al. (2019a). The middle panel (this work) shows the same light curve in reflected light. The bottom panel shows the difference between the normalized reflected and emitted light curves.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Mock light curves of the Moon occulting a rotating, cloudless Earth expanded to spherical harmonic degree l = 25. Black curves show the analytic solution; orange dots correspond to brute force numerical integration on a grid of ∼105 points. The top panel shows the light curve in emitted light and is the same as in Figure 7 in Luger et al. (2019a). The bottom panel (this work) shows the same light curve in reflected light during northern summer.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Example of an inference problem for a thermal phase curve (center left) and a reflected phase curve (center right). In both cases, a mock phase curve is generated from an l = 20 expansion of the cloudless Earth (top) with 1000 evenly spaced points over the course of one year and an extremely small photometric uncertainty of 1 ppm. The observer sits along the ecliptic and the obliquity of the Earth is set to 23.°5. Data is shown as the black points, and the maximum likelihood starry model is shown in blue. While both models fit the data equally well, the same is not true of the inferred surface maps (bottom row): only in the reflected case are the continental outlines recovered. The thermal phase curve problem is extremely ill-conditioned, but the analogous problem in reflected light is much better posed.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Same as Figure 4, but for an occultation evaluation in which the occultor intersects the terminator (case 6 in Appendix C). The reflected light algorithm is around one order of magnitude slower and comparably precise to the emitted light algorithm. It is ∼4 orders of magnitude faster and ∼10 orders of magnitude more precise than numerical integration.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Evaluation time (vertical axis) and numerical precision (point size) for a single flux evaluation in the absence of an occultor as a function of spherical harmonic degree for different methods. In purple we show results for the emitted light starry algorithm from Luger et al. (2019a; solid: no gradient; dashed: with gradient), and in blue we show results for the reflected light algorithm from this paper (solid: no gradient; dashed: with gradient). For comparison, in we also show results for discrete integration on a grid (orange) and for numerical integration using two-dimensional Gaussian quadrature (red); neither of these include gradient evaluations. The reflected light algorithm is comparable in efficiency and precision to the emitted light algorithm. It is ∼5 orders of magnitude faster and ∼10 orders of magnitude more precise than numerical integration.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Reflected light phase curve model for Kelt-9b, assuming a spherical albedo A = 0.2. The transit (phase zero) is not included. Blue is the starry model assuming a point-source illumination; purple accounts for the finite size of the star. The left panel shows the two models in parts per million of the stellar flux; the right panel shows the models normalized so their maximum value is unity. The primary effect of the extended source size is to increase the planet flux near full phase, since the stellar surface is on average slightly closer to the planet, and to change the overall curvature of the phase curve. The shape of secondary eclipse, however, is relatively insensitive to the point-source approximation (see Figure 8).
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Normalized reflected light secondary eclipse model for Kelt-9b, assuming a spherical albedo A = 0.2. Blue is the starry model assuming a point source illumination; purple accounts for the finite size of the star. The orange curves show approximate models computed using the Mandel & Agol (2002) model: a sphere of uniform intensity (solid orange) and a sphere whose intensity falls as the cosine of the viewing angle from the center of the planet disk (dashed orange). Because Kelt-9b is so close to its host star, the illumination phase changes significantly from ingress to egress, and neither approximation accurately captures the behavior of the light curve. On the other hand, the point-source approximation agrees well with the extended source solution, modulo the difference in the depth (see Figure 7).
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Normalized surface intensity on Kelt-9b viewed in a Mollweide projection assuming a point illumination source (left) and accounting for the finite extent of the star (right). The day/night terminator extends about 17° past where it is in the point-source case. The substellar intensity is higher in the extended source case, because the subplanet point on the star is closer to the planet than in the case where the star is a point source located at the center of the star.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Visible-light occultation of Io by Europa observed on 2009 December 4 by the PHEMU09 campaign (Arlot et al. 2014). The blue line is the starry model, based of an l = 15 spherical harmonic fit to the Galileo global color mosaic of Io (Becker & Geissler 2005), an l = 5 expansion of the Oren & Nayar (1994) scattering law, and orbital information from the JPL Horizons database. See text for details.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Intensity measured from a sphere at varying illumination phase under the Oren & Nayar (1994) scattering model. The top panel shows spheres rendered with different surface roughness coefficients ranging from σ = 0° (the Lambertian case) to σ = 45°. The bottom panel shows the corresponding phase curves for a sphere of unit spherical albedo illuminated by a point source, computed analytically from a degree 5 expansion of the scattering law. Dots correspond to the intensity computed numerically directly from Equation (30) in Oren & Nayar (1994).
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Scattering geometry for non-Lambertian reflection. Based on Figure 3 of Oren & Nayar (1994). The incident radiation is labeled  s  and the outgoing radiation is labeled  v . The shaded region is a small patch of surface, oriented so that the normal vector points along ﹩\hat{z}﹩. The four angles relevant to the computation of the emergent intensity are also indicated.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: The 10 principal families of cases of occultations in reflected light. In these figures, the body with the solid outline is the one whose flux we are interested in, and the body with the dashed outline is the occultor. The nightside of the occulted body is colored black (dark gray if occulted), and the dayside is colored blue (bluish-gray if occulted). Case 0 is the unocculted case (Appendix B), while cases 1–5 involve configurations in which the limb of the occultor does not intersect with the terminator at any point, so the visible flux may be computed in terms of classical starry integrals. The remaining cases require integration along the orange boundary (the curves ﹩{ \mathcal P }﹩, ﹩{ \mathcal T }﹩, and ﹩{ \mathcal Q }﹩ of Appendix C.3), which include the terminator. These involve the evaluation of incomplete elliptic integrals and are derived below. Note, finally, that there are additional subcases not shown above. For instance, cases 4, 5, 7, and 8 also encompass configurations in which the occultor does not intersect the limb of the occulted body. However, as this distinction does not affect the procedure for computing the flux in these cases (see text), we omit these subcases from the figure.
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Geometry of an occultation in reflected light, corresponding to case 6 in Figure 15. The surface integral over the occulted portion of the dayside (bluish-gray region) is computed from the line integrals of the antiderivatives of the surface intensity map along the boundary curves ﹩{ \mathcal P }﹩, ﹩{ \mathcal T }﹩, and ﹩{ \mathcal Q }﹩. See text for details .
Paper: Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons
Authors: Rodrigo Luger, Eric Agol, Fran Bartolić, Daniel Foreman-Mackey
Figure caption: Similar to Figure 12, but for 500 high signal to noise observations taken over ten days near quadrature. At the top we show the thermal and reflected phase curves and the corresponding inferred maps. At the bottom, we show the same light curves but this time including seven equatorial occultations by a (very) short period moon one-quarter the size of the planet. The presence of the occultations significantly increases the fidelity of the recovered maps near the equator (the path of the occultor). While in the thermal case there is significant overfitting at high latitudes, in the reflected case the map accurately recovers features across the entire planet.