adsabs/AstroCLIMB huggingface dataset:
Paper: A VERITAS/Breakthrough Listen Search for Optical Technosignatures
Authors: A. Acharyya, C. B. Adams, A. Archer, P. Bangale, P. Batista, W. Benbow, A. Brill, M. Capasso, M. Errando, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Fortson, A. Furniss, S. Griffin, W. Hanlon, D. Hanna, O. Hervet, C. E. Hinrichs, J. Hoang, J. Holder, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, S. Kumar, M. J. Lang, M. Lundy, G. Maier, C. E. McGrath, M. J. Millard, H. R. Miller, J. Millis, C. L. Mooney, P. Moriarty, R. Mukherjee, S. O'Brien, R. A. Ong, M. Pohl, E. Pueschel, J. Quinn, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. L. Ryan, I. Sadeh, L. Saha, M. Santander, G. H. Sembroski, R. Shang, D. Tak, A. K. Talluri, J. V. Tucci, N. Vazquez, D. A. Williams, S. L. Wong, J. Woo, D. DeBoer, H. Isaacson, I. de Pater, D. C. Price, A. Siemion
Figure caption: Upper limits on the fraction of stars with transmitting civilizations as a function of the average period between pulses, using the model from Howard et al. (2007; building on Howard et al. 2004) which assumes no candidate pulses are found. From top to bottom the five lines correspond to: all data from this paper (247 targets; upside-down triangles), the Harvard targeted search (Howard et al. 2004; 4730 targets, circles), the Harvard All-Sky nontargeted survey (Howard 2006; Mead 2013; 7320 hr, diamonds), a hypothetical nontargeted VERITAS survey using all of the data from this paper (140 hr; right-pointing triangles), and a hypothetical nontargeted survey using all data from the entire VERITAS archive (18,176 hr; left-pointing triangles). The minimum detectable pulse is ∼30 times larger for Harvard than for VERITAS.
Paper: A VERITAS/Breakthrough Listen Search for Optical Technosignatures
Authors: A. Acharyya, C. B. Adams, A. Archer, P. Bangale, P. Batista, W. Benbow, A. Brill, M. Capasso, M. Errando, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Fortson, A. Furniss, S. Griffin, W. Hanlon, D. Hanna, O. Hervet, C. E. Hinrichs, J. Hoang, J. Holder, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, S. Kumar, M. J. Lang, M. Lundy, G. Maier, C. E. McGrath, M. J. Millard, H. R. Miller, J. Millis, C. L. Mooney, P. Moriarty, R. Mukherjee, S. O'Brien, R. A. Ong, M. Pohl, E. Pueschel, J. Quinn, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. L. Ryan, I. Sadeh, L. Saha, M. Santander, G. H. Sembroski, R. Shang, D. Tak, A. K. Talluri, J. V. Tucci, N. Vazquez, D. A. Williams, S. L. Wong, J. Woo, D. DeBoer, H. Isaacson, I. de Pater, D. C. Price, A. Siemion
Figure caption: Sensitivity (minimum detectable pulse intensity) as a function of the radial distance from the center of the VERITAS telescope field of view. The three curves correspond to a pulse located at the center of a PMT (worst case), equidistant between three PMTs (best case), and at the most common location (typical case). The crosshatched region indicates the outer 75% of the camera area and the sensitivity of 75% of the possible pulse locations within this area. See the text for more details.
Paper: A VERITAS/Breakthrough Listen Search for Optical Technosignatures
Authors: A. Acharyya, C. B. Adams, A. Archer, P. Bangale, P. Batista, W. Benbow, A. Brill, M. Capasso, M. Errando, A. Falcone, Q. Feng, J. P. Finley, G. M. Foote, L. Fortson, A. Furniss, S. Griffin, W. Hanlon, D. Hanna, O. Hervet, C. E. Hinrichs, J. Hoang, J. Holder, T. B. Humensky, W. Jin, P. Kaaret, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, S. Kumar, M. J. Lang, M. Lundy, G. Maier, C. E. McGrath, M. J. Millard, H. R. Miller, J. Millis, C. L. Mooney, P. Moriarty, R. Mukherjee, S. O'Brien, R. A. Ong, M. Pohl, E. Pueschel, J. Quinn, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. L. Ryan, I. Sadeh, L. Saha, M. Santander, G. H. Sembroski, R. Shang, D. Tak, A. K. Talluri, J. V. Tucci, N. Vazquez, D. A. Williams, S. L. Wong, J. Woo, D. DeBoer, H. Isaacson, I. de Pater, D. C. Price, A. Siemion
Figure caption: Coverage across an H-R diagram for the stellar targets used in both dedicated observations and archival analysis. It is similar to the coverage found in the original Isaacson et al. (2017) catalog.
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: Top: three-color image of the heart of IC 417. Red = 4.5 μm (from Spitzer/IRAC), green = 3.6 μm (from Spitzer/IRAC), and blue = 1.3 μm (J band, from the Two Micron All Sky Survey, 2MASS). This image is a few degrees counterclockwise of north (up), and it is about 0.°5 across. Stock 8 is the cluster at the center-right, creating a “bowl” in the green nebulosity. Clusters of red objects can be seen in the “nebulous stream” in the center-left of this figure. (Image credit: NASA/JPL-Caltech, sig16-008). Bottom: IRAC-2 (4.5 μm) image from GLIMPSE360 in reverse grayscale (north is up), showing sexigesimal coordinates (green) and the footprint of the media image (yellow). See also Figure 2.
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): location of the YSO candidates on the sky, with the clusters from Table 1 and Figure 2. Red filled circle: stars identified in the literature or here via WISE as having an IR excess; blue open circle: stars identified in the literature as an O or B star; green “v”: stars identified in the literature as variable; orange open diamond: stars identified in the literature as Hα-bright; purple open stars: carbon stars from the literature; filled black dots: stars identified here as part of the NS. (b): zoom-in on the NS, with the same symbols as in the first plot, with the boundaries of the NS shown as the magenta polygon. (c): zoom-in on the NS, with magenta polygon, but this time different subclusters defined as indicated, numbered in order of increasing R.A. Black dots are just stars in the catalog; additional red circle = subcluster 1, green square = subcluster 2, cyan diamonds = subcluster 3; purple star = subcluster 4. Subcluster 3 has substantial overlap with the BPI14 literature cluster. Our YSO candidate list is biased toward stars in Stock 8 and NS because of the way we constructed the list—many of the literature YSOs are in Stock 8 because that was the focus of those studies. We defined the boundaries of the NS, so it is readily apparent in the first plot. The right plot defines possible subclusters within the NS for use later in the paper; note that some stars in the NS are not assigned to a subcluster.
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: Wide-field Infrared Survey Explorer (WISE)-2 (4.5 μm; from unWISE) reverse grayscale image of our region. This image is ∼1° on a side, centered on 5:28:00 34:30:00 (J2000). The clusters from Figure 19 in C12 are included as indicated; see the text for more information. The clusters are listed in Table 1. The yellow polygon indicating the footprint from Figure 1 is also shown for reference. The field we have focused upon is the magenta box, running from α, δ = 05:26:31.5, +34:08:50.6 (the lower-right corner of the magenta box) to 05:29:50, +34:51:05 (the upper-left corner of the magenta box). (All coordinates are J2000.)
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-2 (4.5 μm) reverse grayscale image (as in Figure 2) of our region, with the yellow polygon (coverage of press image from Figure 1) and large magenta square (our region of study) included for reference. The dark blue irregular polygon with dashed lines is the region that is NOT covered by IPHAS; note that it includes most of the NS. Green is J08 coverage; the small teal square plus the irregular teal polygon to the north is MN16; the magenta circle is the Jose et al. (2017) complex, the red polygon is Lata et al. (2019) UKIDSS coverage, extending down to decl. ∼ 34.°25, which is about the lower edge of the red Lata et al. (2019) polygon. Many studies have focused on Stock 8 (see also Figure 2); most of our work here is on the larger area, with a particular focus on the NS (see Figure 4).
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: Reverse grayscale images of J052704.46+342559.0, obtained via FinderChart, in DSS (top row), 2MASS (middle row), and WISE (bottom row); images are 30″ across. The target position is given by the crosshairs; the additional colored symbols on top of that position are positions of corresponding catalog entries (the 2MASS and WISE catalog counterparts are exactly on top of this source). The inset is an SED using all of the available data with symbols as defined in Table 2. Error bars are vertical black lines, most obvious here in WISE-4. The dashed line is the expected flux density from the photosphere assuming K s is on the photosphere. This source was identified by IPHAS as bright in Hα and by Winston et al. (2020) as having an IR excess. This is a well-behaved point source, clearly and cleanly detected in the images, with a nice, YSO-like SED showing a clear IR excess; we accept this source as a high-quality YSO candidate.
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-2 (4.5 μm) reverse grayscale image (from unWISE) of our region, zoomed in on the nebulous stream (NS). The blue clusters are the same as in Figure 2, and only include the clusters entirely or mostly within this image. The magenta polygon is empirically derived here to include the regions of nebulosity and obviously red stars in Figure 1.
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: Color–color and color–magnitude diagrams for the first six sources in Appendix D (red stars). Black numbers in each panel correspond to the source numbers here in the text. In panel (b), the numbers are on the corresponding symbols, but in panels (a), (c), and (d), they are offset to the right-hand side for clarity, but are aligned in roughly the same orientation as the symbols. Black points are the entire IC 417 catalog, and cyan points are the YSO candidates. As in earlier similar plots, green lines (where they appear) are ZAMS, blue/yellow dashed lines (where they appear) are PARSEC isochrones, and reddening vectors are computed as described in the text. The individual reddening, where possible, was estimated from the star’s placement in the JHK  s  (first panel) and applied in the optical color–magnitude diagram (last panel); the offset orange hollow star is where the star would appear if dereddened according to the assumed reddening law and JHK  s -derived magnitude.
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: Gaia absolute G vs. G  BP  − G  RP  color–magnitude diagrams, with notation the same as in Figure 21. Left: the IC 417 sample, as in Figure 11. 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. 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. The Taurus stars do a better job of clustering around the 6 Myr isochrone. The random patch of sky has no similar clustering.
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: Gaia G vs. G  BP  − G  RP  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 en masse 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. The Taurus stars do a better job of clustering around the 6 Myr isochrone.
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 griz color–color 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. 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 near the isochrones, but the reddening complicates things here, as reddening pushes things up and to the right in this plot. Stars with large blue excesses from accretion will be found below the isochrones. Some Taurus stars are found there, as are some IC 417 stars. As noted in the text, this was not as effective a way to find YSOs as we had hoped.
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: Color–color and color–magnitude diagrams for the first six sources in Appendix D (red stars). Notation is the same as in Figure 29.
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: Color–color and color–magnitude diagrams for the second six sources in Appendix D (red stars). Notation is the same as in Figure 29, except the source numbers in panel (a) are along the top rather than along the side.
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: Color–color and color–magnitude diagrams for the second six sources in Appendix D (red stars). Notation is the same as in Figure 29.
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: IPHAS riHα color–color 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 (only four stars were observed by IPHAS). 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 IPHAS ZAMS is shown in green and is from Drew et al. (2005). The IPHAS data appear quantized due to the precision with which the magnitudes are reported in Hα. Young stars that are bright in Hα will be above the ZAMS. Many more IC 417 stars are found there than stars from the random 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: Simulated JWST/NIRSpec-Prism transmission spectrum (R ∼100) of TOI-1899 b created using a 10×  solar metallicity cloud-free atmosphere assuming a equilibrium temperature of 400 K and albedo of 0 (blue) generated with ExoTransmit (Kempton et al. 2017). Error bars are calculated using PandExo (Batalha et al. 2017) assuming two observed transits of TOI-1899 b. The planetary spectrum is dominated by the absorption features of methane and water in this bandpass. We plot the same model atmosphere with the addition of an opaque cloud deck (gray absorber) at pressure levels of 1.0 mbar (green) and 0.1 mbar (purple) for comparison. As TOI-1899 b may have a similar atmosphere to Jupiter, we also consider a higher albedo of 0.5, leading to an equilibrium temperature of 320 K (300 K for ExoTransmit grid; orange). The difference in temperature does not significantly change the spectra and should not impact JWST’s ability to retrieve atmospheric abundances.
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: All transiting planets with masses measured to >5σ, plotted by planetary radius (R  p ) vs. orbital period (P) (top) and planetary radius (R  p ) vs. equilibrium temperature (T eq) (bottom). TOI-1899 b is circled in green. Points are colored by the host star T eff and scaled in size by the planet’s TSM (Kempton et al. 2018). We also highlight the transition temperatures for water vapor and ammonia, species whose presence or absence in the atmospheres of cool planets like TOI-1899 b may hint at their formation and cooling history (Fortney et al. 2020). TOI-1899 b is unique in R  p –P space in being the only M-dwarf Jupiter with P > 10 days, and in R  p –T eq space by having among the highest TSMs of Jovian-sized planets with T eq = 300–500 K, while also being the only one whose host star has T eff ≲ 4000 K. Data were retrieved from the NASA Exoplanet Archive (NASA Exoplanet Science Institute 2020) on 2023 May 15.
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 photometry of TOI-1899 b. In each panel, 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. We show transits from TESS (all available sectors, phase-folded; top left), the Perkin 17″ in SDSS ﹩{r}^{{\prime} }﹩ (top right), the Davey 24″ in SDSS ﹩{i}^{{\prime} }﹩ (bottom left), and ARCTIC in Semrock 857/30 (bottom right). Gray points are unbinned, while dark-red points have been binned to a cadence of 10 minutes. The photometry in this figure is available as Data Behind Figures.(The data used to create this figure are available.)