adsabs/AstroCLIMB huggingface dataset:
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: Top: orbital semimajor axis, a, as a function of time. The colors represent different initial stellar rotation periods, and the red dashed–dotted line stands for the system’s Roche limit. Middle: change in the eccentricity, e, for each a on the top panel. Bottom: evolution of planetary radius, R p, over the timescales of tidally induced migration.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: Left: spectra of the five best-matching HPF-SpecMatch library stars, with the composite library spectrum (red) overplotted against the highest-S/N observed spectrum of the target star TOI-1899. The composite spectrum is constructed using the weights c  i  noted for each library star. Right: SED of TOI-1899 as fit by EXOFASTv2, showing the broadband photometric measurements (red; x-error bars indicate the passband width) and the derived MIST model fluxes (blue). A NextGen BT-SETTL model (Allard et al. 2012) is overlaid for reference (gray, smoothed version in black) and is not used as part of the SED fit.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: ASAS-SN, ZTF, and Gaia photometry phased to the ephemeris of TOI-1899 b, with the right panels zoomed in around the transit. The joint-fit model from Figure 2 is overplotted, including the 1σ, 2σ, and 3σ  posteriors. ASAS-SN does not have the precision to detect the transit, but we see a potential transit in ZTF and a more definitive one in Gaia.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: Top: ASAS-SN photometry fit with a celerite quasi-periodic kernel, suggesting a stellar rotation period of ﹩{29.46}_{-0.10}^{+0.07}﹩ days. Bottom left: photometry phased to the derived GP period. Dark points have been binned to better show the flux variation as a function of phase. Bottom right: histogram of posterior samples for P GP.
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: GLS periodograms of the HPF RVs, activity indicators, and window function, with the period of TOI-1899 b indicated by the vertical orange line. The FAP levels corresponding to 0.1%, 1%, and 10% are also marked.(The data used to create this figure are available.)
Paper: The Unusual M-dwarf Warm Jupiter TOI-1899 b: Refinement of Orbital and Planetary Parameters
Authors: Andrea S. J. Lin, Jessica E. Libby-Roberts, Jaime A. Alvarado-Montes, Caleb I. Cañas, Shubham Kanodia, Te Han, Leslie Hebb, Eric L. N. Jensen, Suvrath Mahadevan, Luke C. Powers, Tera N. Swaby, John Wisniewski, Corey Beard, Chad F. Bender, Cullen H. Blake, William D. Cochran, Scott A. Diddams, Robert C. Frazier, Connor Fredrick, Michael Gully-Santiago, Samuel Halverson, Sarah E. Logsdon, Michael W. McElwain, Caroline Morley, Joe P. Ninan, Jayadev Rajagopal, Lawrence W. Ramsey, Paul Robertson, Arpita Roy, Christian Schwab, Guðmundur Stefánsson, Daniel J. Stevens, Ryan C. Terrien, Jason T. Wright
Figure caption: Stellar rotation period (red, left-hand y-axis) and stellar wind braking rate (black, right-hand y-axis), as a function of time. Both quantities were analyzed for a P rot_ini,⋆ ∼ 29.5 days and a star with half of its envelope contributing to the exchange of angular momentum (i.e., ε ⋆ ζ ⋆ = 0.5).
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: CMD of stellar groups. The colors of dots represent the members of given groups corresponding to the color codes shown in Figure 7. The CMD of group C is plotted with gray dots for comparison. The red and blue curves exhibit the 5 Myr isochrones reddened by a total extinction (A  V ) of 1.86 and 3.00 mag, respectively, while the 2 Myr isochrone reddened by A  V  of 3.00 is plotted with gray curves. The CMDs of individual stellar groups are compared with that of the open cluster group C (green).
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Integrated intensity maps and PV diagrams of the entire region (left) and W5 East region (right). These radio data were obtained from the 12CO (J = 1–0) line (Heyer et al. 1998). The gray scale represents the distribution of molecular clouds. The color-coded dots show the distribution of members in the integrated intensity maps and PV diagrams. The size of dots is proportional to the brightness of members. Arrows indicate the PM vectors of the sparse group members relative to their nearest dense groups (C in W5 West and F in W5 East). The nearest dense groups containing ionizing sources in W5 West and East are groups C and F, respectively.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Identification of stellar groups in W5. A total of eight groups were identified by means of the k-means clustering algorithm. The identified clusters are shown in different colors. The size of dots is proportional to the brightness of individual stars.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Motions of stars in their host groups. The panels in the first and third rows display the spatial distributions of stars in given groups. The straight lines of different lengths represent the PM vectors of stars relative to their host groups. The Φ distributions are shown in the panels in the second and fourth rows. The colors of dots corresponds to those of stellar groups in Figure 7.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Position–velocity diagrams of stars. The colors of dots are the same as those in Figure 7. The vertical lines represent the errors of velocity measurements.
Paper: The Kinematics of the Young Stellar Population in the W5 Region of the Cassiopeia OB6 Association: Implication for the Formation Process of Stellar Associations
Authors: Beomdu Lim, Jongsuk Hong, Jinhee Lee, Hyeong-Sik Yun, Narae Hwang, Byeong-Gon Park
Figure caption: Mean PMs of stellar groups relative to the systemic motion of W5. The brownish arrows represent the relative PM vectors of individual groups. The other symbols are the same as those of Figure 7.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Residual maps for the inner two half-light radii of Lac I, with the comparison model as the best-fitting exponential (left) and Sérsic (right) models. The maps are generated by dividing the field into a 30 × 30 cell grid and calculating the estimated surface density of RGB stars at the center of each cell based on the best-fitting model. The surface density is then converted to the number of objects expected within the cell, given the cell area. The residual for a given cell is calculated by subtracting the expected number of stars within the cell from the actual number and then dividing that quantity by the square root of the actual number of stars; see Section 5.1 for more details. Residual values are color-coded according to the color bar shown on the right, which ranges from approximately +3σ to −2.5σ. The solid and dashed ellipses mark one and two half-light radii, respectively. North is up, and east is left.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: The left panel shows the residuals for the regions of Cas III inside two half-light radii, calculated from the exponential (left) and Sérsic (right) models, produced and plotted in the same way as described in the caption for Figure 10. The solid and dashed ellipses mark one and two half-light radii, respectively. The central regions of Cas III were affected by stellar crowding and so were excluded from the substructure search process (see Section 5.2.2); these areas are shown in gray. North is up, and east is left.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Residual maps for the portion of Per I inside two half-light radii, constructed using the exponential (left) and Sérsic (right) models, produced and plotted in the same way as described in the caption for Figure 10. The solid and dashed ellipses mark one and two half-light radii, respectively. North is up, and east is left.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Residual map in the region beyond two half-light radii for Cas III. The map was generated as described in Section 5.1. The main body of the galaxy, where the surface densities are above 4σ, is masked in gray. The white contours encompass 1σ, 2σ, and 3σ areas. North is up, and east is to the left.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Map of the residuals in the region of the Lac I field where the galaxy no longer dominates. The map was generated as described in Section 5.1. Overdensities above 4σ are masked in gray and considered the main body of the galaxy. The white contours encompass 1σ, 2σ, and 3σ areas. North is up, and east is to the left.
Paper: Exploring the Structures and Substructures of the Andromeda Satellite Dwarf Galaxies Cassiopeia III, Perseus I, and Lacerta I
Authors: Katherine L. Rhode, Nicholas J. Smith, Denija Crnojevic, David J. Sand, Ryan A. Lambert, Enrico Vesperini, Madison V. Smith, Steven Janowiecki, John J. Salzer, Ananthan Karunakaran, Kristine Spekkens
Figure caption: Residual map for the outer regions in the Per I field. The 1σ, 2σ, and 3σ contours are in white. The map was generated as described in Section 5.1. The areas with surface densities greater than 4σ above the background surface density are masked in gray, as they are considered part of the galaxy. North is up, and east is to the left.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: DESI-observed progress compared with a nominal simulation using the same major shutdowns. The dark time progress of the simulation is a good match for the observed dark time progress; in the simulation, 26.53% of the dark program was completed before 2022 June 15, while in the real survey, 28.97% of the survey was completed. The fraction of time elapsed is shown with a dashed line, weighting nights by the length of the night, historical weather loss, and removing nights near full moon and planned monsoon shutdowns; see Section 8 for details. These survey simulations match the progress of the bright program poorly, however, with the actual bright survey progress running ahead of the simulations by almost a factor of two. This is due to limitations of the sky brightness modeling in the simulations, as well as the use of more time in twilight and near full moon for bright observations than expected.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: DESI-delivered survey speed, compared with speeds delivered in the simulations. This is the product of factors relating to seeing, transparency, and sky brightness. The average delivered speed is 7% higher in the actual observations, but 14% higher when limiting to exposures taken in dark conditions. We note that the small difference between the average speeds here and in Figure 6 comes from the fact that here the speeds are computed from the measured seeing, transparency, and sky brightness, and in Figure 6 they are computed from the effective time delivered on each tile.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: DESI-delivered point-spread function FWHM. The blue curve shows the measurements from the GFAs during the DESI survey, while the orange curve shows data from simulations based on the MzLS. The inferred average survey speeds for both the real data and the simulated data (proportional to the square of the fraction of flux entering a fiber) are given for each case, and they agree closely.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: DESI-observed sky brightness, relative to a nominal dark sky brightness of 21.07 mag. The observed sky brightness peaks about 7% darker than this. The sky brightness models in the simulation are very simple, assigning a sky brightness of 1, 1.5, or 3.6, depending on the phase and location of the moon. The overall average survey speed, proportional to one over the sky flux, are reasonably well-matched, though the simulations are 8% slower, largely due to the slightly darker peak of the observed sky distribution versus the simulated sky distribution.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: DESI-observed transparency. The simulations show a narrower distribution of transparencies than observed, due to the simulations having deconvolved the observed distribution slightly in order to reduce the effect of measurement errors. The inferred average survey speeds are proportional to the square of the transparency, and by construction, they are identical between observations and simulations.
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: Representations of the phase-folded light curve (upper panel) and radial velocity curve (lower panel). The best-matched light curve model is shown with the red curve. Regarding radial velocities, blue and red colors are for the primary and the secondary components, respectively. Observational uncertainties are often smaller than the size of the circles in the lower panel. Phase folding is done with respect to the T 0 and P orb given in Table 3.
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: Observed APOGEE spectrum (black line) of KIC 9028474 at BJD = 2,457,264.8067 and the best-matched computed composite synthetic spectrum (red line). Three different parts of the APOGEE spectrum are shown in three panels. The blue line shows residuals from the best-matched computed composite synthetic spectrum and shifted upwards in the −y-axis for better viewing purposes. Clearly separated and unblended spectral lines of both components are marked as P and S for the primary and the secondary, respectively.
Paper: KIC 9028474: A Long-period Eclipsing Binary on a Highly Eccentric Orbit
Authors: Orkun Özdarcan
Figure caption: ETV diagram of KIC 9028474. Blue (filled) and red (open) circles denote etv of shallow and deep eclipses, respectively. We show etv of deep eclipses as the secondary axis for a better viewing purpose.