adsabs/AstroCLIMB huggingface dataset:
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption:  Q and M statistics for our sample of disk-bearing stars in ρ Ophiuchus (top), Taurus (middle), and Upper Scorpius (bottom). Nonvariable objects are excluded. Point areas in this and subsequent plots are scaled according to variability amplitude to the one-third power (see Section 5.1). Colors in this and subsequent plots denote different types of variables, as identified by eye; see text.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Amplitudes and timescales measured for the samples of disk-bearing YSOs in ρ Oph (top), Taurus (middle), and Upper Sco (bottom). Each point is colored by its variability type; no size scaling is applied here, since amplitude is one of the axes. See text for discussion.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Examples of different light curve morphologies seen among disk-bearing stars in Taurus. As with previous clusters, we have divided the sample into eight different types of behavior (excluding eclipsing binary systems, which do not appear here). All light curves are normalized by their median flux level.
Paper: The Many-faceted Light Curves of Young Disk-bearing Stars in Taurus as Seen by K2
Authors: Ann Marie Cody, Lynne A. Hillenbrand, Luisa M. Rebull
Figure caption: Spectral type distributions for the young, low-mass stars in star-forming regions observed with K2: ρ Oph, Taurus, and Upper Sco. Although the number of cluster members with good K2 light curves varies among the regions, in each cluster, a similar stellar mass range is covered.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Kinematic substructures in Mon OB1. The top left panel shows the correlation between PMs along R.A. and positions along decl. It is evident that there are three groups of stars that are spatially and kinematically distinct. Three ellipses were used to ascertain the spatial distributions of members within them. The solid lines represent the arbitrary boundaries of each group. The other panels display the spatial distributions of members belonging to each group. Red, blue, and orange circles represent the members of the S Mon group, the Cone group, and the THF15 group, respectively. The size of circles is proportional to the brightness of individual stars.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Parallax (left) and PM (right) distributions of member candidates. The Gaia parallaxes were corrected for zero-point offsets using the recipe of Lindegren et al. (2021). We plot only stars with parallaxes larger than three times their associated errors. Dashed lines in the left panel confine the probable members to distances between 500 and 1000 pc. The right panel shows the PM distribution of member candidates between 500 and 1000 pc. Red, blue, and black circles represent the genuine members of Mon OB1, Mon R1, and the halo, respectively, while gray circles denote probable nonmembers (see the main text for detail).
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Spatial distribution of member candidates. The boundaries of Mon OB1 and Mon R1 are outlined by a red ellipse and a blue circle, respectively. A region encompassing all members is shown by a black ellipse (dashed line). The size of circles is proportional to the brightness of stars. The positions of stars are relative to the reference coordinate R.A. = 06h36m23.ˢ52, decl. = ﹩+10^\circ {04}^{{\prime} }55\buildrel{\prime\prime}\over{.} 7﹩ (J2000). The other colors of circles are the same as in the right panel of Figure 2.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Spatial distribution of members in Mon R1. Pink, green, and cyan circles represent the members of IC 447, N2245/47, and IC 446, respectively. The size of circles is proportional to the brightness of individual stars. Solid lines are used to separate stellar groups.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Distance distributions. The panels from top to bottom display the distance distributions of members in the entire survey region, Mon OB1, Mon R1, and the halo, respectively. Distances were obtained from the inverse of the Gaia parallaxes (Gaia Collaboration et al. 2021) after correction for the zero-point offsets (Lindegren et al. 2021). We used stars with parallaxes larger than five times their associated errors. The black curves shows the best-fit Gaussian distributions.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Tangential velocities and RVs of stars with respect to R.A. and decl. in Mon OB1. The vertical lines represent the errors of velocities. The colors of symbols are the same as those in Figure 5.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Color–color diagrams of YSO candidates classified with the AllWISE data (Cutri et al. 2014). Red triangles, green squares, and orange diamonds represent Class I, Class II, and YSO with a transitional disk, respectively. The color criteria for the YSO classification of Koenig & Leisawitz (2014) are shown by dashed lines.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Distributions of stars and gas in our survey region. The left and right panels display the IRIS image at 100 μm (Miville-Deschênes & Lagache 2005) and the AKARI false-color image (blue: 65 μm; green: 90 μm; red: 140 μm; Doi et al. 2015), respectively. The contours in the left panel trace the arc-like structure of the remaining cloud. In the right panel, the PM vectors of stars relative to the systemic motion of Mon OB1 are shown by solid lines. The black circles represent the halo stars. The white ellipse represents the position of the SFR G202.3+2.5. Some infrared and submillimetric sources (Beichman et al. 1988; Di Francesco et al. 2008) in the northern knot were marked by purple circles. The colors of the other symbols are the same as in Figures 5 and 7.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: CMD of stars in the survey region. The meaning of the symbols is shown in the upper right corner of the panel. The G RP magnitudes of individual stars were corrected by the distance moduli of the associated SFRs. The black and gray dashed curves show the isochrones reddened by A  V  of 0.22 and 0.62 mag, respectively, for ages of 2, 3, 5, and 10 Myr (Dotter 2016; Choi et al. 2016). The black arrow represents the reddening vector corresponding to the total extinction of A  V  = 1. mag.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Relative PMs of stars in Mon OB1. The top left panel shows the spatial distribution of its three stellar groups. Red, blue, and orange circles represent the S Mon group, the Cone group, and the THF15 group, respectively. The systemic motions of these groups relative to the median PM of Mon OB1 are shown by arrows with the same colors in the box, where the PM vectors were shifted along R.A. by ﹩35^{\prime} ﹩ to avoid confusion. We plot the PM vectors (solid lines) of individual members relative to the systemic motion of a given group in the other panels. The star symbol denotes the O-type binary S Monocerotis. The size of circles is scaled by the brightness of individual stars.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Tangential velocities and RVs of stars with respect to R.A. and decl. in Mon R1. The vertical lines represent the errors of velocities. The colors of symbols are the same as those in Figure 7.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Vectorial angle distributions of stars in the stellar groups of Mon OB1. The top panels display the vectorial angles with respect to the projected radial distances from the central positions of host groups. The distributions of vectorial angles are shown by histograms in the bottom panels. The histograms were obtained with a bin size of 45°.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Signature of rotation of the S Mon group (upper) and Cone group (lower). ΔRV denotes the difference of mean RVs between two regions separated by a projected rotational axis at a given position angle (Θ). The blue solid lines represent the best-fit sinusoidal curves. Half of the amplitude corresponds to the projected rotational velocity.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Relative PMs of stars in Mon R1. The left panel shows the spatial distribution of three stellar groups. The systemic motions of these groups relative to the median PM of Mon R1 are shown by arrows. We plot the PM vectors (solid lines) of stars relative to the systemic motion of a given group in the right panel. The size of circles is scaled by the brightness of individual stars. The colors of the symbols are the same as those in Figure 7.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Vectorial angle distributions of stars in the stellar groups of Mon R1. The top panels display the vectorial angles with respect to the projected radial distances from the centers of IC 447, N2245/47, and IC 446 (from left to right), respectively. The distributions of vectorial angles are shown by histograms in the bottom panels. The size of bins is 45°.
Paper: A Gaia View on the Star Formation in the Monoceros OB1 and R1 Associations
Authors: Beomdu Lim, Yaël Nazé, Jongsuk Hong, Sung-yong Yoon, Jinhee Lee, Narae Hwang, Byeong-Gon Park, Jeong-Eun Lee
Figure caption: Schematic sketch of star formation history in Mon OB1 and Mon R1 from > 5 Myr ago (left) to present (right). Stellar groups are labeled at the epoch when they were formed. See the text for details.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: WASP-4b transit (panel (a)) and occultation (panel (b)) timing variations predictions using the best-fit models to the timing data presented in this paper. The lines are 100 random draws from the posteriors of the orbital decay (blue) and apsidal precession (red) models. On both panels, we show the average error of the previous observations.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (1–8) from Sector 2 of WASP-4b. The best-fitting model obtained from the EXOplanet MOdeling Package (EXOMOP) is shown as a solid red line. The residuals (light curve – model) are shown below the light curve.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (9–14) from Sector 29 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Difference in mid-transit times between our analysis and Bouma et al. (2020) for the Sector 2 TESS data.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (8–16) from Sector 20 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (17–18) from Sector 2 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (1–8) from Sector 29 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (9–15) from Sector 28 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Individual TESS transit events (1–8) from Sector 28 of WASP-4b. Other comments are the same as Figure A1.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Best-fit one-planet Keplerian orbital model for WASP-4b using RadVel of only the Bouma et al. (2020) RV data. (a) The maximum-likelihood model is plotted while the orbital parameters listed in Table C2 are the median values of the posterior distributions. The thin blue line is the best-fit one-planet model. We add in quadrature the RV jitter terms listed in Table C2 with the measurement uncertainties for all RVs. (b) Residuals to the best-fit one-planet model. (c) RVs phase-folded to the ephemeris of WASP-4b. The small point colors and symbols are the same as in panel (a). Red circles are the same velocities binned in 0.08 units of orbital phase. The phase-folded model for WASP-4b is shown as the blue line.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Posterior distributions for all free parameters for the two-planet RV analysis (Model # 4) fitting for e  c . The results of this model can be found in Table 4 and Figure 4.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Posterior distributions for all free parameters for the one-planet RV analysis without (Model # 1) fitting for the linear acceleration. The results of this model can be found in Table 4 and Figure 4.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Posterior distributions for all free parameters for the one-planet RV analysis without (Model # 2) fitting for the linear acceleration. The results of this model can be found in Table 4 and Figure 4.
Paper: Characterizing the WASP-4 System with TESS and Radial Velocity Data: Constraints on the Cause of the Hot Jupiter’s Changing Orbit and Evidence of an Outer Planet
Authors: Jake D. Turner, Laura Flagg, Andrew Ridden-Harper, Ray Jayawardhana
Figure caption: Posterior distributions for all free parameters for the best-fit two-planet RV analysis (Model # 3). The results of this model can be found in Table 4 and Figure 4.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Systematic effects in the FFI data. In the left panel, we show the Sector 1 raw light curve of the central pixel of the Type Ia supernova ASASSN-18tb/SN 2018fhw. The sudden flux increases followed by a gradual decline at the beginning and middle of the light curve are caused by the scattered light from the Earth and Moon. The gap in the middle is when the data downlink occurred. The flagged points (red) indicate when the momentum dumps, periods of reduced pointing stability due to the spacecraft firing its thrusters, occurred. The high pointing jitter between 1348 and 1350 days was caused by an improper spacecraft configuration. In the right panel, we show a 40 × 40 pixel FFI cutout centered on ASASSN-18tb from Sector 1. The median value for each pixel is shown, and the color bar is calibrated to the 10%–90% range of flux values. The central pixel of ASASSN-18tb is located where the two blue lines intersect and is enclosed by a blue square.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Observation strategy of TESS (Figure 7 from Ricker et al. 2014, licensed under CC BY 4.0). The left panel shows the FOV of a single TESS sector created by its four cameras. The middle panel shows how TESS divides and observes the sky in 26 partially overlapping sectors. The right panel shows how the overlap between sectors leads to certain areas of they sky being observed for longer durations.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Diagram motivating the half-sibling regression method. The quantities in the top row (Star 1, Systematics, Star 2) are unobserved, while the quantities in the bottom row (Pixel 1, Pixel 2) are observed. The two pixels are on the same CCD and separated by at least several times the size of the PSF to ensure that no flux from one of the stars is simultaneously illuminating both pixels. Pixels 1 and 2 can be thought of as half-siblings, as they both share a common parent (Systematics). TESS Spacecraft Image Credit: NASA’s Goddard Space Flight Center.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Diagram of the train-and-test framework. In this scenario, the light curve being detrended is divided into five contiguous sections (k = 5), each indicated by a separate color. For every test section being detrended, the model coefficients are obtained by fitting to the training data, which are the rest of the light curve. As k is inversely proportional to the number of measurements in a given section, an appropriate choice for k can be made based on the timescale of the signal of interest.
Paper: The unpopular Package: A Data-driven Approach to Detrending TESS Full-frame Image Light Curves
Authors: Soichiro Hattori, Daniel Foreman-Mackey, David W. Hogg, Benjamin T. Montet, Ruth Angus, T. A. Pritchard, Jason L. Curtis, Bernhard Schölkopf
Figure caption: Normalized light curve for each pixel in the 3 × 3 aperture of ASASSN-18tb. The numbers in the top right corner of each panel indicate the pixel row and column positions.