adsabs/AstroCLIMB huggingface dataset:
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Linear histogram showing the derived rotation periods for 10,470 asteroids with more than 200 detections and periods within our acceptable boundaries across TESS Cycle 1.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Log histogram showing the derived rotation periods for asteroids across TESS Cycle 1.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Light curve from this study for asteroid 10351. As no period solution was derived, the x-axis here shows the temporal extent of the observations with no folding.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Same as Figure 7 except only for objects with more than 200 photometric detections after quality control.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Comparison of the best-fit rotation periods reported by Pál et al. (2020) with the best-fit periods obtained in this work for the same objects. Note that no quality cutoff or consideration is made at this stage.
Paper: An Untargeted Survey of the Rotational Properties of Main-belt Asteroids using the Transiting Exoplanet Survey Satellite (TESS)
Authors: Andrew McNeill, Michael Gowanlock, Michael Mommert, David E. Trilling, Joe Llama, Nicholas Paddock
Figure caption: Light curve from this study for asteroid 10351 folded to the period solution of Pál et al. (2020).
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: MUSCLES Extension stars are compared with M and K dwarfs from the HAZMAT surveys. For stars from the HAZMAT surveys, open markers indicate M dwarfs from Schneider & Shkolnik (2018) while solid markers represent K dwarfs from Richey-Yowell et al. (2019). Shaded regions represent the 1σ error level of the linear fits.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Fraction of bolometric luminosity emitted in the X-ray. Wright et al. (2011) represents solar and late-type stars. Wright et al. (2018) represents fully convective M dwarfs. The black square connected by the vertical line to L 98-59 represents the X-ray luminosity during only the flaring event. The black circle representing L 98-59 shows the quiescent X-ray luminosity.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Stellar UV flux with increasing effective temperature. Note that increasing effective temperature drives the photospheric emission deeper into the UV, as discussed in Section 3.2
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Result of the HD 149026 BT-Settl scaling routine plotted with the STIS G430L spectrum. The BT-Settl stellar atmosphere model is convolved to G430L resolution and scaled by a factor of α = 0.8951.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Left: Lyα reconstruction for HD 149026 using the Youngblood et al. (2022) MCMC method. Right: Lyα reconstruction for WASP-77A using the Mg II flux estimation method.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Panchromatic stellar SEDs from 5 Å–5.5 μm. The vertical axis represents the flux density normalized by the bolometric flux, spanning approximately 10−10–10−4 Å−1. All spectra have been binned to 5 Å per pixel for visualization.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: L 98-59 X-ray and NUV light curves for F301. The EPIC light curves have been binned to 10 s to match the time resolution of the OM UVW1 data. The data have been smoothed with a Gaussian kernel for clarity. Top: OM UVW1 flare normalized to the peak of the X-ray flare. Bottom: time derivative of the X-ray flare (units of s−2) overplotted by the normalized OM UVW1 light curve (units of s−1). Note that the blue OM UVW1 curve does not match the units of the vertical axis and is only plotted here as a visual aid. The vertical black lines represent the location of the peak of each light curve.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Fraction of bolometric luminosity of UV ions vs. (a) rotation period (b) effective temperature.  = France et al. (2018) planet hosts,  = France et al. (2018) non-planet hosts, and + = this work. Histograms represent the number of stars with a bolometric luminosity ratio within the range of each bin, with blue corresponding to non-planet hosts and red to planet hosts.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Top: UV flux incident at the top of the innermost planet’s atmosphere relative to the UV flux incident at Earth. Bottom: amount of flux incident at the conservative habitable zone (average of the inner- and outermost habitable zones using Kopparapu et al. 2013 models) relative to the flux experienced at the Sun’s habitable zone of approximately 1.3 au. For both panels, red markers indicate flux over the FUV band, and black markers indicate the NUV band.
Paper: The MUSCLES Extension for Atmospheric Transmission Spectroscopy: UV and X-Ray Host-star Observations for JWST ERS & GTO Targets
Authors: Patrick R. Behr, Kevin France, Alexander Brown, Girish Duvvuri, Jacob L. Bean, Zachory Berta-Thompson, Cynthia Froning, Yamila Miguel, J. Sebastian Pineda, David J. Wilson, Allison Youngblood
Figure caption: Top: background-subtracted source light curves for F201 and F301. Bottom: background time series for each observation. Note the large background flare occurring at 20 ks in F301; this is likely due to protons within the Earth’s magnetosphere being funneled toward the detector. All data are from the EPIC pn detector with the medium filter and binned to 100 s.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: POS velocity field for the CND ionized streamers northern arm (red), eastern arm (blue), and western arc (green). Velocities are derived from Keplerian-orbit modeling with parameters in Table 4 (Zhao et al. 2009). The yellow star represents the location of Sgr A*. The background image corresponds to the HAWC+ 53 μm polarized intensity. The black lines show the area where the condition ﹩\mathrm{PI}/{\sigma }_{{p}_{I}}\geqslant 3﹩.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Top panels: steady-state flow, U 0(x, y) for two cases: stretch (left) and shear (right). Bottom panels: POS magnetic field strength, B POS, as a function of the polarization angle dispersion, σ  ϕ . The results from the modified DCF approximation for different values of U 00/σ  v —the ratio of the strength of U 0 to the velocity dispersion—are shown in color. For comparison, the classical DCF and the compressional (Skalidis & Tassis 2021) DCF are shown in dashed and dotted black lines, respectively. Values of B POS are shown for y/L = 0, x/L = 1, where L is the characteristic length of the flow in the x-direction.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Auxiliary data for DCF calculations. Left: column density map for the CND, calculated via SED fitting of Herschel data. Right: velocity dispersion map calculated from [C II] spectral emission observed with SOFIA/GREAT. In both panels, contours correspond to the HAWC+ 53 μm intensity levels, and the white star represents the location of Sgr A*.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: SOFIA/HAWC+ 53 μm observations of the CND. B-field pseudovectors (black) representing the orientation of the magnetic field are plotted on the 53 μm intensity map (Stokes I). The location of Sgr A* is depicted by the white star, and the beam size is displayed in the lower-left corner. Vectors displayed satisfy the condition p/σ  p  ≥ 3. A legend with a 5% polarization fraction is shown.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Projected and smoothed synthetic observations obtained from ideal-MHD numerical simulations performed with the AREPO code obtained from CATS. Two-dimensional maps correspond to POS coordinates and are calculated from snapshot cubes by integration along the LOS. Parameters describing the simulations are shown in Table 2. Top, left: synthetic B-field orientation on top of the column density; the line length is proportional to the polarization fraction, with a maximum value of 15%. Top, right: POS B-field. Bottom, left: velocity dispersion. Bottom, right: POS velocity. White contours in all panels correspond to levels of column density.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: POS magnetic field strength as a function of spatial scale size, L. Three values are shown: blue symbols correspond to ﹩{B}_{\mathrm{POS}}^{\mathrm{DCF}};﹩ red symbols correspond to ﹩{B}_{\mathrm{POS}}^{\mathrm{DCF},{\rm{F}}}﹩; and green symbols correspond to ﹩{B}_{\mathrm{POS}}^{\mathrm{DCF},\mathrm{SF}}﹩. In all three cases, B POS scales as a power law with L  s .
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Left: shear-flow mask for synthetic data analysis. Two criteria are used to create the mask (blue shaded region): (1) pixels where the magnetic field (red arrows) and flow direction (black arrows) differ by less than ±10o, and (2) pixels where the gradient of the flow is different from zero. Right: zoom into a region of the parallel flow and magnetic-field mask.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Distribution of POS magnetic field strength (B POS) values for the entire CND using the three DCF approximations: classical (left), large-scale flow modification (middle), and shear-flow modification (right). In all three panels, black solid vertical lines indicate the median of the distribution. Red solid vertical lines to the left and right of the median indicate the 5th and 95th percentiles, correspondingly. Dotted vertical lines indicate the spread of such values when uncertainties in B POS are considered (see the text for details).
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Average spectrum of [C II] emission from the CND. Observations were obtained with SOFIA/GREAT. The emission line was modeled as Gaussian in order to estimate its width as the turbulent velocity dispersion. Measured line widths were corrected for thermal motion widening. Figure 6 (right panel) displays the map of velocity dispersion derived from this data.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption:  B-field configuration in the CND and streamers. The B-field’s orientation is represented for each streamer by line integration contours (Cabral & Leedom 1993) inferred from the 53 μm HAWC+ data. The B-field’s strength is represented in a one-dimensional way along the main direction of the streamer. Stronger B-fields correspond to larger distances away from Sgr A* (red star), and weaker magnetic fields are inferred closer to Sgr A* where the shear flows (white arrows) are larger. The background image corresponds to the 53 μm intensity. A legend showing a velocity field of 300 km s−1 is displayed.
Paper: The Strength of the Sheared Magnetic Field in the Galactic’s Circumnuclear Disk
Authors: Jordan A. Guerra, Enrique Lopez-Rodriguez, David T. Chuss, Natalie O. Butterfield, Joan T. Schmelz
Figure caption: Results from the dispersion analysis and corresponding Markov Chain Monte Carlo (MCMC) fitting performed to the entire CND. Left: dispersion function (blue circles) as a function of ℓ 2(panel (a)) and ℓ(panel (b)). The solid red line corresponds to the best-fit model. Panel (c) displays the autocorrelated turbulent component of the dispersion function (blue circles) with its corresponding fit (red dashed line). For comparison, the autocorrelated beam is displayed with the solid gray line. Right: corner plots for the MCMC posterior distributions of parameters fitting the dispersion function.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The CSS detection probability (Equation (5)) as a function of orbital elements for four different absolute magnitude values. From top to bottom, we plot ﹩{ \mathcal P }(a,e,i,H)﹩ for H corresponding to objects with D = 3 km, 1 km, 300 m, and 50 m (H = 15.37, 17.75, 20.37, and 24.26 for the reference albedo p V = 0.14). The plots in the left column show ﹩{ \mathcal P }﹩ for the fixed orbital inclination (i = 10°) and several eccentricity values. The plots on the right show ﹩{ \mathcal P }﹩ for e = 0.6 and several inclination values. The detection probability was computed for orbits with q < 1.3 au.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The orbital distribution of main-belt asteroids (red dots) near the 3:1 resonance with Jupiter. The inner V-shaped region approximates the dynamically unstable domain where test bodies representing the 3:1 source were placed. The main-belt asteroids with orbits in the two outer strips, 2.48 < a < 2.49 au and 2.51 < a < 2.52 au for e = 0 and diagonally extending to e > 0, were used to set up the eccentricity and inclination distributions of test bodies.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The projected PDFs of model NEO orbits for different sources (projected p  j (a, e, i)): ν 6, 3:1, 5:2, 8:3, 2:1 and JFCs (from top left to bottom right). Higher values are shown by brighter colors. For reference, the red lines show orbits with q = a Earth, Q = a Earth, q = a Venus, and Q = a Venus, where Q = a(1 + e) is the aphelion distance, a Earth = 1.0 au and a Venus = 0.72 au.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The CSS detection probability (Equation (5)) as a function of orbital elements for four different absolute magnitude values. From top left to bottom right, we plot ﹩{ \mathcal P }(a,e,i,H)﹩ for H corresponding to objects with D = 3 km, 1 km, 300 m, and 50 m (H = 15.37, 17.75, 20.37, and 24.26 for the reference albedo p V = 0.14). The detection probability was averaged over all inclinations bins. The vertical strips, with ﹩{ \mathcal P }﹩ going up and down as a function of the NEO’s semimajor axis, are discussed in the main text.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The CSS’s mean rate of detection—the number of CSS FOVs in which an NEO with given orbital elements is expected to be detected—is plotted as a function of the absolute magnitude (green line). The average of ﹩{ \mathcal R }(a,e,i,H)﹩, given in Equation (4), was computed over the whole orbital domain. The original bias from Granvik et al. (2018) is shown by open circles. The gray line shows the detection rate when the trailing loss from Zavodny et al. (2008) is not accounted for.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The eccentricity (panel (a)) and inclination (panel (b)) distributions of bodies placed in the 3:1 resonance with Jupiter. The red lines are the actual distributions of main-belt asteroids near the 3:1 resonance. The black lines are the analytic approximation of these distributions described in the main text.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Predicted atmospheric composition of a hypothetical abiotic Earth-like planet orbiting HIP 23309, subject to varying estimates of its UV irradiation (Figure 7).The different colors correspond to different chemical species. The left column corresponds to chemical species emitted by the surface, while the right column corresponds to photochemically generated species. In each row, the different linestyles correspond to different SEDs. The UVIT-only SED alone is insufficient to achieve highly-precise photochemical modeling (top row), but can be used to calibrate other estimates of the stellar SED (middle row) to achieve higher precision, as done crudely here (bottom row) and with vastly more sophistication by, e.g., Peacock et al. (2019a, 2019b).
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Input UV SEDs used for modeling the atmospheric composition (Figure 8) of a hypothetical abiotic Earth-like planet orbiting HIP 23309.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Surface radiances on early Earth-like planets orbiting different M dwarfs including HIP 23309, computed as in Ranjan et al. (2017). The Rimmer et al. (2018) minimum flux criterion for HCN homologation toward ribonucleotide synthesis is shown in pink. Extremely active stars like HIP 23309 meet the Rimmer et al. (2018) criterion, illustrating the need to constrain UV emission of M dwarfs over the course of their lifetimes to understand the potential of life search on M-dwarf planets to test theories of abiogenesis (Rimmer et al. 2021a).
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Exoplanet-hosting stars for which Gaia parameters are available. The color bar represents the distance in kpc from the Sun. In addition, note the blob of the planet above the galactic plane that represents the Kepler field.