adsabs/AstroCLIMB huggingface dataset:
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Kinetic and excitation temperature maps for H-MM1 are shown in the left and right panels, respectively. The contours and markers are the same as in Figure 1. These maps only include pixels where the uncertainty is smaller than 1 K.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Integrated intensity maps of the NH3 (1,1) and (2,2) main line components are shown in the left and right panels, respectively. The contours are for NH3 (1,1) in both panels. The contour levels start from 1.5 K km s−1, and the spacing is 0.75 K km s−1. The beam size and the scale bar are shown in the lower left and lower right corners, respectively.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: NH3 column density map. The central part of the map (where H2 peaks) shows a nearly constant NH3 column density, while the peak is located in the northern part of the core. The contours and markers are the same as in Figure 1.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Centroid velocity and velocity dispersion maps derived from NH3 are shown in the left and right panels, respectively. The velocity fields show an elongated redshifted feature connecting the southeast edge and the central region of the core. The contours and the markers are as in Figure 1.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: Dust-derived total H2 column density map of the H-MM1 region. The map shows a peak close to the center of the image. The resolution and scale bar are shown in the lower left and lower right corners, respectively. The contours show the NH3 (1,1) integrated intensity, as in Figure 1.
Paper: An Interferometric View of H-MM1. I. Direct Observation of NH3 Depletion
Authors: Jaime E. Pineda, Jorma Harju, Paola Caselli, Olli Sipilä, Mika Juvela, Charlotte Vastel, Erik Rosolowsky, Andreas Burkert, Rachel K. Friesen, Yancy Shirley, María José Maureira, Spandan Choudhury, Dominique M. Segura-Cox, Rolf Güsten, Anna Punanova, Luca Bizzocchi, Alyssa A. Goodman
Figure caption: The KDEs of the kinetic temperature as a function of NH3 and H2 column density are shown in the left and right panels, respectively. The black horizontal segments show the mean values within the column density bins. The gas temperature drops from ≈12 K down to ≈11 K toward the highest column densities in the core.
Paper: HEALPix Alchemy: Fast All-Sky Geometry and Image Arithmetic in a Relational Database for Multimessenger Astronomy Brokers
Authors: Leo P. Singer, B. Parazin, Michael W. Coughlin, Joshua S. Bloom, Arien Crellin-Quick, Daniel A. Goldstein, Stéfan van der Walt
Figure caption: The 47 deg2 footprint of the ZTF camera as a HEALPix MOC, refined to a maximum level of l = 10. The left panel shows the footprint as a collection of filled polygons: each of the small filled squares is one CCD quadrant, each 2 × 2 cluster of quadrants comprise a CCD, and the 4 × 4 grid of CCDs comprise the entire focal plane. The middle panel shows the outlines of the multi-resolution HEALPix tiles that comprise the MOC. The inset panel at right shows a small portion of the MOC, with each pixel labeled with its resolution level l and its nested pixel index i.
Paper: HEALPix Alchemy: Fast All-Sky Geometry and Image Arithmetic in a Relational Database for Multimessenger Astronomy Brokers
Authors: Leo P. Singer, B. Parazin, Michael W. Coughlin, Joshua S. Bloom, Arien Crellin-Quick, Daniel A. Goldstein, Stéfan van der Walt
Figure caption: An example of the multi-resolution HEALPix sampling scheme that is used in GW localizations. The top panel shows the localization of LIGO/Virgo event GW200115_042309 (Abbott et al. 2021; GraceDB ID S200115j) as a heat map image; darker, deeper colors represent higher probability density. The bottom panel shows the boundaries of the multi-resolution HEALPix tiles on which the sky map was sampled.
Paper: HEALPix Alchemy: Fast All-Sky Geometry and Image Arithmetic in a Relational Database for Multimessenger Astronomy Brokers
Authors: Leo P. Singer, B. Parazin, Michael W. Coughlin, Joshua S. Bloom, Arien Crellin-Quick, Daniel A. Goldstein, Stéfan van der Walt
Figure caption: Illustration of the nested nature of HEALPix. Level 0 divides the unit sphere into 12 equal-area tiles. In each subsequent level, every tile is divided equally into four new tiles.
Paper: HEALPix Alchemy: Fast All-Sky Geometry and Image Arithmetic in a Relational Database for Multimessenger Astronomy Brokers
Authors: Leo P. Singer, B. Parazin, Michael W. Coughlin, Joshua S. Bloom, Arien Crellin-Quick, Daniel A. Goldstein, Stéfan van der Walt
Figure caption: The first three levels of the HEALPix RING and NESTED indexing schemes. In each panel, the horizontal axis is R.A., and the vertical axis is the sine of the decl. After Górski et al. (2005).
Paper: HEALPix Alchemy: Fast All-Sky Geometry and Image Arithmetic in a Relational Database for Multimessenger Astronomy Brokers
Authors: Leo P. Singer, B. Parazin, Michael W. Coughlin, Joshua S. Bloom, Arien Crellin-Quick, Daniel A. Goldstein, Stéfan van der Walt
Figure caption: Run time on AWS as a function of the number of fields of three representative queries in HEALPix Alchemy.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The MEGNO maps of WASP-35 with the perturber initially on a coplanar + circular orbit (a), on a coplanar+slightly eccentric orbit (e = 0.2) (b), and on an inclined+slightly eccentric orbit (e = 0.2) (c). The dark dots represent the upper mass limit of the rms of the WASP-35b TTVs, while the yellow curves are from the constraints of the rms of the WASP-35 RV residuals after removing the components of WASP-35b. The regular orbital configurations denoted with green are distinguished from the chaotic ones labeled with red in the MEGNO map.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The MEGNO maps of HAT-P-30 with the perturber initially on a coplanar + circular orbit (a), a coplanar+slightly eccentric orbit (e = 0.2) (b), and on an inclined+slightly eccentric orbit (e = 0.2) (c). The dark dots represent the upper mass limit of the rms of the HAT-P-30b TTVs, while the yellow curves are from the constraints of the rms of the HAT-P-30 RV residuals after removing the components of HAT-P-30b. The regular orbital configurations denoted with green are distinguished from the chaotic ones labeled with red in the MEGNO map.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: Transit timing variations after subtracting the constant-period model of HAT-P-30. The green and blue dots are the new transit times from TESS and YO-1 m, the dark yellow dots are refined transit times from the data of Johnson et al. (2011), the violet dot is from the data of Maciejewski et al. (2016), the purple dots are from Wang et al. (2021), the olive dots are from Saha et al. (2021), the cyan dot is from Edwards et al. (2021), and the orange dots denote those from ETD. The black curve shows the expected orbital decay model, and the red curve shows the apsidal precession model.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: Transit timing variations after subtracting the constant-period model of WASP-35. The green and blue dots are the new transit times from TESS and YO-1 m, the olive dots are from Enoch et al. (2011), and the orange dots denote the data points from ETD. The black curve shows the expected orbital decay model, and the red curve shows the apsidal precession model.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The RV data of HAT-P-30 with the linear trend best-fitting model and the residuals (right panel). The green dots are the RV data from Enoch et al. (2011), and the blue dots are from Johnson et al. (2011).
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The final transit light curves of HAT-P-30 with the best-fitting transit models and the residuals.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The final transit light curves of WASP-35 with the best-fitting transit models and the residuals.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distribution of ﹩{\tilde{{ \mathcal H }}}_{o}-{\tilde{{ \mathcal H }}}_{a}﹩ of ﹩{{\mathscr{U}}}_{h}﹩, where definitions of the colored regions are identical to those in Figure 4.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of ﹩{\tilde{{ \mathcal H }}}_{o}﹩ and i  m  of Monte Carlo simulations for (a) well-determined objects and (b) objects with poor orbit determinations.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of η and κ with different i  m  and ﹩{\tilde{{ \mathcal H }}}_{o}-{\tilde{{ \mathcal H }}}_{a}﹩.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: (a) Time evolution of orbital elements of 2019 VL5, and (b) 2019 VL5's orbit in the Sun–EMB dimensionless rotating frame.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Frequency distribution histograms of U of the 221 potential ECOs, where the red dashed line denotes the 50th percentile.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distribution of objects with possible Mars or Venus close encounters.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of different sets of well-determined objects in the multiplanet model.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of the newly identified ECOs.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: The measured portions of the spectral energy distributions for planets HR 8799 c, d, and e (black markers, data sources described in the text). Barman/Brock Phoenix models with temperature and surface gravity fixed at the values predicted by hot-start evolutionary models (T eff = 1075 K, ﹩\mathrm{log}(g)=4.1﹩) are fit to the data by varying two cloud parameters. Blue points are for a fit letting the radius float between 1.25 and 1.45 R Jup. Teal points show a fit where radius is fixed to 1.29 R Jup. Thick clouds with small grains are preferred for each planet, suggesting that such conditions are necessary to bring atmospheric models and evolutionary models into agreement. We also show the T eff = 1100 K, ﹩\mathrm{log}(g)=4﹩, Phoenix model presented by Konopacky et al. (2013) and Greenbaum et al. (2018; gray markers). This model is also consistent with the evolutionary model predictions. It was drawn from the same Barman/Brock family of models presented here but includes a supersolar C/O ratio.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Left: luminosity vs. age. The gray curves represent the predictions of the Baraffe et al. (2003) evolutionary models. Blue horizontal lines indicate the luminosity constraints for the HR 8799 planets. The green curve corresponds to the right axis and shows the probability distribution function for system age, giving equal weight to the contracting and expanding scenarios from Baines et al. (2012). Right: luminosity vs. mass. Gray curves are from the evolutionary model. Blue horizontal lines indicate the luminosity constraints. The orange and green curves correspond to the right axis and indicate probability distribution functions derived from stability arguments (orange) and from the astrometric influence of planet e (green).
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Spectra recovered with negative planet injection for HR 8799 c, d, and e, showing apparent flux. We compare our LMIRCam/ALES spectra to the 3.3 μm magnitudes from Skemer et al. (2012), the narrowband magnitudes from Skemer et al. (2014), the broad L′-band and 4.05 μm magnitudes from Currie et al. (2014), and the M-band magnitudes from Galicher et al. (2011). The light gray and dark gray vertical swaths correspond to the vAPP absorption band, with an absolute transmission of 40% and 25% respectively, as shown in Figure 11.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Transmission measurements of the vAPP in the 2.8–4.2 μm range using a grism to disperse the vAPP and non-coronagraphic PSF.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Predictions of temperature, surface gravity, and radius from four hot-start evolutionary models, given the age, mass, and luminosity constraints for HR 8799 c, d, and e. Predictions are narrowly peaked and are relatively model-independent.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: The measured portions of the spectral energy distributions for planets HR 8799 c, d, and e (black markers, data sources described in the text). Colored markers indicate best-fit model spectra from three model families. Blue points are from the Barman/Brock Phoenix models. Teal points show DRIFT–Phoenix models, and orange points are blackbodies.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: LMIRCam/ALES image of HR 8799 c, d, and e using the dgvAPP360 coronagraph. The final image is the combination of the individual wavelength slices between 3.55 and 4.15 μm. North is up, east is left.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Contrast as a function of separation using LMIRCam/ALES with the dgvAPP360. The background limit is quickly reached outside the inner working angle of the coronagraph.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Gaia HR diagram depicting stars within 100 pc (using the “ABC” cut described by Lindegren et al. 2018), represented as a two-dimensional histogram (top, bottom left) and a scatter plot (gray points, bottom right). Overlaid are LHS 1678 (green star) and other TESS M dwarf exoplanet systems (blue circles). LHS 1678 is the only TESS exoplanet system so far that is associated with the observed gap in the lower main sequence. In the top panel, the gap is labeled with a blue arrow and is visually seen as the darker-colored, diagonal band, seemingly “cutting into” the main sequence from the left-hand side. The two bottom panels focus on the region around the gap and show LHS 1678's association with that feature. The next closest system, GJ 357 (labeled “D”), lies just above the gap at BP − RP ≈ 2.4. TOI-122 (“H”) and LHS 1972 (“J”) are also close to or in a less visually obvious region of the gap at BP − RP ≈ 2.6 BP − RP ≈ 2.7. Left to right: TOI-1749, TOI-1235, TOI-1728, TOI-1899, TOI-532, LP 714-47, LP 961-53, L 168-9, AU Mic, TOI-1266, LHS 1815, TOI-1231, LHS 1678, GJ 1252 (labeled “A” in the bottom-right panel), TOI-270 (“B”), TOI-1201, TOI-700 (“C”), GJ 357 (“D”), TOI-1685, TOI-1634, L 98-59 (“E”), LHS 1478, TOI-674 (“F”), HATS-71 (“G”), LTT 1445A, TOI-122 (“H”), LTT 3780 (“I”), LHS 1972 (“J”), GJ 486 (“K”), TOI-237, TOI-2406, TOI-540, LHS 3844, LP 791-18 (see references in Appendix B).
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Residual astrometric motion of LHS 1678 when parallax and proper motion are accounted for and removed from 16 yr of monitoring. The remaining motion of the star indicates a binary system with an orbital period on the order of decades. The allowed periods and amplitude of the perturbation suggest a low-mass star or brown dwarf companion. The red line traces an orbital fit to the photocenter’s motion. The four points marked with an “x” were taken in a slightly different V filter, and as such were not included in the orbital fit.