adsabs/AstroCLIMB huggingface dataset:
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: PanSTARRS z vs. r − i color–magnitude diagrams, with notation the same as in Figure 21. Left: the IC 417 sample. Small black dots are the ensemble catalog, and larger dots are the YSO candidates, where the bluer the symbol color, the more reliable a YSO candidate it is. Center: Taurus sample of confirmed YSOs, shifted to be at 2 kpc, the distance of IC 417. Right: randomly selected adjacent patch of sky near IC 417—e.g., there are unlikely to be YSOs here. In this panel, colors correspond to point density with black/purple being the lowest number of points and orange/red being the highest. For all three plots, reddening vectors (following the reddening law from Indebetouw et al. 2008 and Mathis 1990) are as shown. The blue and yellow dashed lines are 6 Myr and 9 Myr isochrones from PARSEC models (Bressan et al. 2012), respectively. Young stars should be clustered around the isochrone corresponding to their age, but there is a fundamental degenerate uncertainty between age and distance, further complicated by reddening. The distance to Taurus is well known, but the distance to IC 417 is much less well known. The IC 417 YSO candidates hug the isochrones and are largely found between the two isochrones, as the Taurus stars are.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: (a): plot on the sky of the YSO candidates (small black dots), with the cluster circles from Figure 5 (blue circles; unlabeled here just for clarity). The OB stars are highlighted (larger blue dots); those OB stars with apparent IR excesses are larger red dots. In all plots, three OB stars are highlighted. HD 35633 is thought to be the powering source for the nebulosity around Stock 8 (MN16). BD+34°1058 is thought to be the driving source for the NS (MN16). TYC 2411-634-1 is too close to be a member of IC 417. The four carbon stars are also indicated by the yellow stars in both plots; known carbon stars have their names indicated, and the unlabeled gold point is the newly identified carbon star. (b) and (c): histograms of parallaxes and distances to the final set of YSOs in gray, with the locations of the OB and carbon stars highlighted at arbitrary y-axis positions shown as five-pointed stars (with the uncertainties from Bailer-Jones et al. 2021 indicated by horizontal lines). Red symbols represent stars with disks. The carbon stars are indicated in yellow. Certain stars are called out. One has a parallax so negative as to not appear in panel (b) (J052729.32+342502.6 = [JPO2008] IC 417 3), and that one, plus one more (J052752.39+344658.1 = IU Aur), have distances too far to appear in panel (c). The OB stars are distributed across the sky and in distance, but may preferentially appear in the clusters. They are certainly clustered at the distance of IC 417 (1–3 kpc). The carbon stars are not young and are unlikely to be members of IC 417.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: Histograms of distances from the (a) entire catalog in this region, and (b) just the NS and Stock 8. The legend is in the upper-right corners of the panels, e.g., solid black line (DR2 BJ) = DR2 Bailer-Jones et al. (2018) distances; dotted thin dark blue line (DR3 BJ) = DR3 Bailer-Jones et al. (2021) geometric distances; dotted thick turquoise line (DR3 BJpg) = DR3 Bailer-Jones et al. (2021) photogeometric distances; dashed thin green line (DR3 1/pi) = distance from inverted parallax from DR3; dashed–dotted thin orange line (DR3 gspphot) = distance from GSP-Phot from DR3 (note that the peak is up well beyond the top of the plot, at 2345); dashed–dotted thick red line (DR3 gsppphot best plx) = distance from GSP-Phot from DR3 but only for those stars where the error in parallax/parallax <0.2 (e.g., those where Andrae et al. 2023 say the distances are likely valid). The gray vertical lines going from the top to the bottom of the plot are at 1 and 3 kpc, e.g., the range of distances we accepted as members of IC 417. The short, thick gray lines at the bottom are the literature distances given for IC 417 summarized in the text. Given these bulk distributions on the left, it is clear that we are operating near the outer range of where these distances are available, let alone where they may be valid. The distributions on the right show that the distances of stars in the NS and Stock 8 are peaked at 2 kpc, which is the main reason that we took stars with a distance of 2 kpc, with a range of 1–3 kpc, as members of IC 417.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption:  JHK  s  color–color diagrams (top row), the IRAC color–magnitude diagram (second row), and the PanSTARRS color–magnitude diagram (third row), and a histogram of parallaxes (fourth row) for the entire NS (left column), and Stock 8 (right column). Colors in the top three rows correspond to YSO ranks (as in Figure 11 or Figure 18), so bluer is better. Note that the limits of the JHK  s  plot are the same as earlier in the paper, but the limits are adjusted for the other two diagrams. The yellow line in the lower-left histogram is with a broader bin size, because there are double the number of stars in Stock 8 (200) compared to the NS (92). The vertical dotted lines correspond to 1 and 3 kpc, the range of distances we took to be consistent with IC 417. The numbers at the left and right sides of the plot indicate how many outliers there are (e.g., there are three stars with parallax < − 1.5 mas and three stars with parallax >3 mas in Stock 8). The NS is likely younger than Stock 8, and they are likely at the same distance.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: Zoom-in on the NS for several properties discussed earlier for the sample as a whole—the number of points in the SED, amount of reddening (A  V ) estimated from the JHK  s  diagram, SED Class (I/flat/II/III), distance from Gaia DR3 as derived by Bailer-Jones et al. (2021; with additional annotations of the subclusters), and our final YSO confidence rank (1–5). Color scales are as indicated in each panel. Points are only plotted if there is a corresponding value—there are the fewest number of points in the fourth panel because there are fewer distances known than anything else here. Because the YSO candidates in the NS were identified by position on the sky, many objects in the NS have very few points in their SED, which results in many low-ranked SEDs. There can be a lot of reddening (as is obvious in Figure 1), which results in many sparsely populated SEDs, but also steep SEDs and few distances. NS3 has the most stars, the most A  V , and the most embedded sources.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: IRAC color–magnitude diagrams, with notation the same as in Figure 21. Left: the IC 417 sample. Small black dots are the ensemble catalog, and larger dots are the YSO candidates, where the bluer the symbol color, the more reliable a YSO candidate it is. Center: Taurus sample of confirmed YSOs, shifted to be at 2 kpc, the distance of IC 417. Right: randomly selected adjacent patch of sky near IC 417—e.g., there are unlikely to be YSOs here. In this panel, colors correspond to point density with black/purple being the lowest number of points and orange/red being the highest. For all three plots, reddening vectors (following the reddening law from Indebetouw et al. 2008 and Mathis 1990) are as shown. The green solid line is the expected color for main-sequence stars. Young stars should generally be found significantly to the right of the green line, and the Taurus sample is found there. The IC 417 YSO candidate sample is clearly more like the Taurus sample than the background stars found in the adjacent patch of sky.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption:  JHK  s  color–color diagrams (left column), the IRAC color–magnitude diagram (center column), and the PanSTARRS color–magnitude diagram (right column) for various parts of the NS: the entire NS (first row), just NS1 (second row), just NS2 (third row), just NS3 (fourth row), just NS4 (fifth row), and those NS stars not assigned to a subcluster (sixth row). Colors correspond to YSO ranks (as in Figure 11), so bluer is better. Note that the limits of the JHK  s  plot are the same as earlier in the paper, but the limits are adjusted for the other two diagrams. There are no obvious differences among the clusters, other than NS 3 being the best-populated.
Paper: Young Stellar Object Candidates in IC 417
Authors: L. M. Rebull, R. L. Anderson, G. Hall, J. D. Kirkpatrick, X. Koenig, C. E. Odden, B. Rodriguez, R. Sanchez, B. Senson, V. Urbanowski, M. Austin, K. Blood, E. Kerman, J. Long, N. Roosa
Figure caption: WISE color–color diagrams. Left: the IC 417 sample, with notation the same as in Figure 21. Small black dots are the ensemble catalog, and larger dots are the YSO candidates, where the bluer the symbol color, the more reliable a YSO candidate it is. Center: Taurus sample of confirmed YSOs. Right: randomly selected adjacent patch of sky near IC 417—e.g., there are unlikely to be YSOs here. For all three plots, reddening vectors (following the reddening law from Indebetouw et al. 2008 and Mathis 1990) are as shown. Main-sequence stars should have zero color in this plot. Young stars should be red, up and to the right in this plot, and the Taurus sample is found there. The IC 417 YSO candidate sample is clearly more like the Taurus sample than the background stars found in the adjacent patch of sky.
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: Joint-fit RVs of TOI-1899 b. The best-fit model is plotted as a black line, while the blue shaded regions denote the 1σ (darkest), 2σ, and 3σ ranges of the derived posterior solution. Top: phase-folded RVs, with HPF data from Cañas et al. (2020) in gray, new HPF data in dark red (pre-velocity break) and pink (post-velocity break), and NEID in gold. Bottom: unphased RVs and residuals as a function of time.
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 available PDCSAP photometry from TESS, with each sector separate (top) and with consecutive sectors grouped together (bottom). The x-axis is the same as previous plots for ease of comparison, but smoothing in the PDCSAP processing will suppress any signals ≳10 days.