adsabs/AstroCLIMB huggingface dataset:
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining part of OC Cepheids, which also contain the extinction, age, and distance parameters of the OCs, namely, UBC 290, NGC 6649, UBC 129, FSR 0158 (J194806.54+260526.1), IC 4725, FSR 0951, NGC 129 (DL Cas), CWNU 19, NGC 6087, Berkeley 51, Trumpler 35 (CN Sct), UBC 1273, Lynga 6, NGC 6067, FSR 0158 (GQ Vul), Berkeley 84, and UBC 130. CMDs of OC Cepheid candidates, namely, CWNU 2580, CWNU 3981, and CWNU 3305.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining part of OC Cepheid candidates, which also contain the extinction, age, and distance parameters of the OCs, namely, CWNU 3193, CWNU 3684, CWNU 3513, UBC 106, NGC 129 (V0379 Cas), Berkeley 58, CWNU 3246, UBC 409, CWNU 1903, CWNU 2490, CWNU 3310, CWNU 4287, UBC 231, Cl SX Vel, CWNU 337, and UBC 1558. CMDs of the remaining rejected OC Cepheid samples, namely, Pismis 19, Alessi 21, CWNU 4764, and CWNU 3272.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining rejected OC Cepheid samples, which also contain the extinction, age, and distance parameters of the OCs, namely, CWNU 3968, FSR 0384 (V Lac), SAI 4, FSR 0384 (X Lac), UBC 491, UBC 412, Cl V0378 Cen, Ruprecht 97, COIN-Gaia 36, Platais 1, UBC 533, Trumpler 35 (TY Sct), UBC 375, NGC 6683, CWNU 3845, CWNU 1841, UBC 190, OC 0125, Teutsch 145, and Teutsch 80.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining rejected OC Cepheid samples, which also contain the extinction, age, and distance parameters of the OCs, namely, SAI 104, CWNU 3267, IC 2395, OC 0301, CWNU 3265, Mon OB1-D, Theia 123, NGC 6193, CWNU 3603, Haffner 14, IC 2581, FSR 1500, Czernik 41, HSC 2193, SAI 149, UBC 1424, Cl ST Tau, CWNU 2959, Kronberger 84 (V733 Cyg), and UBC 1490.
Paper: Gaia DR3 Open Cluster Cepheids: A Unified Catalog with Calibrated Period–Age and Period–Wesenheit Relations
Authors: Shunhong Deng, Zhihong He, Anbing Ren, Qian Cui, Xiaoyue Zhou, Liming Peng, Chenxin Wang, Ziang Chen, Yangping Luo, Kun Wang
Figure caption: CMDs of the remaining rejected OC Cepheid samples, which also contain the extinction, age, and distance parameters of the OCs, including Ruprecht 93, FSR 0172, HSC 2961, UBC 1496, BH 222, and NGC 6453.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Lithium equivalent widths of Alpha Per cluster members (purple circle) from S. C. Balachandran et al. (2011) and F. J. Galindo-Guil et al. (2022) plotted as a function of Gaia BP − RP color. TIC 384984325 (pink star) agrees with other Alpha Per cluster members. Two other well-studied open cluster Li sequences are plotted; Tucana–Horologium (40 Myr; green square; data from A. L. Kraus et al. 2014) and the Pleiades (112 Myr, yellow diamond, data from J. Bouvier et al. 2018). Because all three clusters overlap in the parameter space of TIC 384984325 its age must lie between the two.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Relative position and velocity of TIC 384984325 (pink star) relative to cluster members identified by S. Meingast et al. (2021; purple dots). The top row shows the position (X, Y, Z) and the bottom row shows the galactic space velocity (U, V, W), both calculated from Gaia DR3 measurements. This star is in the corona of the cluster but is in good agreement with the average kinematic velocity of the cluster.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Top: unflattened TESS light curve of TOI-6109. Middle: flattened light curve with two best-fit transit models for planets b and c. The colors of these light curves correspond to each of the planets in the bottom panels. Bottom: phase-folded light curves of planet b (left) and planet c (right). These include the additional CHEOPS observations.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Individual transits for planet b. The transit model is in black and 30-minute binned points are shown in pink. The first four transits (top row) are from TESS Sector 18 while the next five are from Sector 58. The middle two transits in the third tow are from two CHEOPS visits, followed by four transits from Sector 85 with 20 s cadence observations.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Observed minus calculated transit times for TOI-6109 b (pink) and TOI-6109 c (purple) for three TESS sectors and four CHEOPS visits. The expected transit times are calculated based on fitting a linear period to the observed transit times. There is noted anticorrelation for the TTVs in the second TESS sector (second panel, bottom row). The uncertainties on transit times are smaller than the point size for most transits.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Individual transits for planet c. The transit model is in black and 30-minute binned points are shown in pink. The first two transits are from TESS Sector 18, the next four from Sector 58, and the following two transits from two CHEOPS visits, with the last row showing three transits from Sector 85.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption:  ﹩{{\rm{\Xi }}}_{\max }﹩ value for 10,000 Monte Carlo runs of Equation (2), shuffling our TTV residuals each time. Our real data have a ﹩{{\rm{\Xi }}}_{\max }﹩=51.43 (dashed line), which is 13σ larger than the median of the shuffled runs. There is extremely little chance the TTVs observed could be from photometric noise.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Period–radius diagram of injected and recovered targets. Blue points are those that were recovered by our pipeline. The pink star is TOI-6109 b and the purple star TOI-6109 c. The unconfirmed planet candidates are shown in gray.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: Posterior composition distributions for TOI-6109 b (pink) and TOI-6109 c (purple) from smint. The possible planet masses are 4–18 M⊕ for both planets. The envelope mass fractions are 7.94% for TOI-6109 b and 9.55% for TOI-6109 c.
Paper: THYME. XIII. Two Young Neptunes Orbiting a 75 Myr Star in the Alpha Persei Cluster
Authors: Anne Dattilo, Andrew M. Vanderburg, Madyson G. Barber, Andrew W. Mann, Ronan Kerr, Adam L. Kraus, Joseph R. Livesey, Cristilyn Watkins, Karen A. Collins, Juliana García-Mejía, Patrick Tamburo, Juliette Becker, Annelies Mortier, Thomas Wilson, Nicholas Scarsdale, Emily A. Gilbert, Alex S. Polanski, Steve B. Howell, Ian Crossfield, Allyson Bieryla, David R. Ciardi, Thomas Barclay, David Charbonneau, David W. Latham, Joseph M. Akana Murphy, Elisabeth Newton, Bob Massey, Richard P. Schwarz, Chris Stockdale, Francis P. Wilkin, Roberto Zambelli
Figure caption: 86 young planets (<1 Gyr) plotted via their orbital period and radius, colored by their age. The contours below are planet occurrence contours from A. Dattilo et al. (2023). The population of young planets is not a representative sample of planets compared to the older, intrinsic population of the galaxy, due to various detection biases.
Paper: Kepler-1624b Has No Significant Transit Timing Variations
Authors: Haedam Im, Morgan Saidel, Heather A. Knutson, Michael Greklek-McKeon, Shreyas Vissapragada, Karen A. Collins, Akihiko Fukui, Norio Narita, Kimberly Paragas, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Transit light curves for Kepler-1624b from multiple instruments. (a) Kepler, (b) Palomar/WIRC, (c) TESS, (d) LCOGT/SINISTRO i band, and (e) LCOGT/MuSCAT3 multiband. For Kepler, the light curves of individual transits are phased up using the individual best-fit transit times. For TESS, we phase individual transits using transit times from the best-fit one-planet model. For (a), the gray points show unbinned phased data, where each point corresponds to a 30 minute integration. For (b), unbinned photometry is shown as gray circles, and 10 minute binned photometry is shown as black circles. For (c), we use 10 minute bins for the black points and 2 minute bins for the gray points. For (d), we show the unbinned data as gray points. For (a)–(d), the best-fit transit light curves are overplotted in red, with the 1σ confidence range overplotted as light red shading. For (e), transits in g, r, i, and zs bands are plotted with different colors with an arbitrary vertical offset, and the gray points represent the observed data, while the colored lines show the best-fit transit model for each band with a 1σ confidence range overplotted with the corresponding color of shading. For some of the panels, the 1σ confidence shading is not visually noticeable due to very tight confidence ranges.
Paper: Kepler-1624b Has No Significant Transit Timing Variations
Authors: Haedam Im, Morgan Saidel, Heather A. Knutson, Michael Greklek-McKeon, Shreyas Vissapragada, Karen A. Collins, Akihiko Fukui, Norio Narita, Kimberly Paragas, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Transit timing variations with dynamical models. The 100 random posterior draws from the two-planet model (blue) and one-planet model (red) are plotted. The top-left panel displays the original Kepler TTVs from T. Holczer et al. (2016), showing a clear sinusoidal pattern. The bottom-left panel presents our reanalysis of the Kepler data. The top-right panel displays all observed transit timings from Kepler, Palomar, and LCOGT. The time intervals where TESS transits occur are shaded in gray. The Kepler points are plotted with black circles. The Palomar point is plotted with a triangle, and the two LCOGT points are plotted with stars. The bottom-right panel presents a zoomed-in view of the Kepler data from the top-right panel.
Paper: Kepler-1624b Has No Significant Transit Timing Variations
Authors: Haedam Im, Morgan Saidel, Heather A. Knutson, Michael Greklek-McKeon, Shreyas Vissapragada, Karen A. Collins, Akihiko Fukui, Norio Narita, Kimberly Paragas, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Orbital period vs. planet radius for all planet pairs with period ratios within 2% of a first-order resonance. The colors of the points indicate the effective temperature of the host star, and each planet pair is connected by a solid black line. The location of Kepler-1624b in this space is marked by a star. This plot was generated using data from the NASA Exoplanet Archive (R. L. Akeson et al. 2013).
Paper: Kepler-1624b Has No Significant Transit Timing Variations
Authors: Haedam Im, Morgan Saidel, Heather A. Knutson, Michael Greklek-McKeon, Shreyas Vissapragada, Karen A. Collins, Akihiko Fukui, Norio Narita, Kimberly Paragas, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Kepler light curve before detrending (left) and after detrending (right). The red line shows the Gaussian kernel convolution trend described in Section 2.2. Blue points indicate masked data (±0.8 transit durations around each transit midtime).
Paper: Kepler-1624b Has No Significant Transit Timing Variations
Authors: Haedam Im, Morgan Saidel, Heather A. Knutson, Michael Greklek-McKeon, Shreyas Vissapragada, Karen A. Collins, Akihiko Fukui, Norio Narita, Kimberly Paragas, Richard P. Schwarz, Avi Shporer, Gregor Srdoc
Figure caption: Comparison to published TTVs. Our TTVs are plotted with black circles. TTVs reported by T. Holczer et al. (2016), P. Gajdoš et al. (2019), and L. Kaye & S. Aigrain (2025) are plotted in red, blue, and yellow circles, respectively. The Δ values in the legend represent the average difference between each study’s TTVs and ours, normalized by the measurement uncertainties of our TTVs.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Left: the transmission fraction (e−τ) of H I, He I, and He II gas in the ISM as a function of wavelength from 50 to 1230 Å for a range of H I column densities typical for the LISM. Only bound–free (continuum) opacity is shown. N(He I)/N(H I) = 0.08 and N(He II)/N(He I) = 1.5 (upper limit) were assumed (J. Dupuis et al. 1995). The ionization edges of He II (229 Å), He I (504 Å), and H I (912 Å) are marked with vertical lines. At λ > 912 Å, transmission is unity. Colored vertical ticks mark the wavelengths of the ground-state series of H I (red), He I (green), and He II (blue), along with He I autoionization lines (magenta), where additional opacity is expected, but not shown. Right: a close-up of the transmission curve of H I and D I at Lyα (1215.67 and 1215.34 Å, respectively) as a function of wavelength and velocity for the same range of N(H I) values as the left panel. N(D I)/N(H I) = 1.56 × 10−5, bHI = 10.8 km s−1, and high spectral resolution (R > 100,000) were assumed.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Map in Galactic coordinates of sight lines within 25 pc with N(H I) values known to precision better than 0.3 dex. Stars within 4 pc are shown as open black circles, and stars between 4 and 25 pc are shown as filled circles. Stars beyond 4 pc with (﹩\bar{n}﹩(H I) + ﹩{\sigma }_{\bar{n}(\mathrm{HI})}﹩) > 0.1 cm−3 are shown as filled red circles, otherwise filled black circles. The circle sizes are scaled linearly with the ﹩\bar{n}﹩(H I) value of each sight line. The approximate position of the LIC and G cloud interaction axis is shown as a green ×.
Paper: Toward a 2D H I Map of the Local Interstellar Medium
Authors: Allison Youngblood, Kevin France, Tommi Koskinen, James Paul Mason, Seth Redfield, Brian E. Wood, Vincent Bourrier, Leonardo dos Santos, Christopher Johns-Krull, George W. King, Jeffrey L. Linsky, Sarah Peacock
Figure caption: Left: the H I column densities for each target in our sample as a function of distance. The targets are color-coded by sky quadrant (see legend), where eastern targets have l > 180° and northern targets have b > 0°. The gray dashed contours show constant, average line-of-sight H I volume densities, ﹩\bar{n}﹩(H I), from upper left to lower right: 1.0, 0.1, 0.01, and 0.001 cm−3. Horizontal shaded lines show the average N(H I) values for different distance shells (1–10 pc, 10–50 pc, 50–100 pc), broken up by sky quadrant. Right: median line-of-sight average volume densities are shown as a function of distance in logarithmic distance bins. Error bars show the inner 68% spread of values centered around the median. Colored points show the median values for stars in the different sky quadrants.
Paper: The Interpolation Constraint in the RV Analysis of M Dwarfs Using Empirical Templates
Authors: Dhvani Doshi, Nicolas B. Cowan, Étienne Artigau, René Doyon, André M. Silva, Khaled Al Moulla, Yashar Hezaveh
Figure caption: Top: each color represents a separate noiseless synthetic SPIRou observation along with its corresponding upsampled (spline interpolated) spectrum. For clarity, only three observations are shown. Middle: the upsampled spectra are BERV-registered to reduce the line shift to a fraction of their width. The template shown as the dashed black line is the median of 10 BERV-registered spectra. Bottom: discrepancies between the template and instrumentally broadened intrinsic spectrum, demonstrating that the template contains altered stellar features. We further plot the residuals between a BERV-shifted observation and the template interpolated to the same wavelength grid.
Paper: The Interpolation Constraint in the RV Analysis of M Dwarfs Using Empirical Templates
Authors: Dhvani Doshi, Nicolas B. Cowan, Étienne Artigau, René Doyon, André M. Silva, Khaled Al Moulla, Yashar Hezaveh
Figure caption: Top: an intrinsic stellar spectrum which is Doppler shifted and then convolved. Middle: the convolved spectrum is down-sampled to SPIRou’s resolution, but no photon noise is added, thus representing a noiseless observation. Here, each black point represents a SPIRou pixel. This synthetic observation is then upsampled using spline interpolation as a precursor to constructing the template. Bottom: discrepancies between the upsampled and convolved spectrum, indicating that the template will contain altered stellar features.
Paper: The Interpolation Constraint in the RV Analysis of M Dwarfs Using Empirical Templates
Authors: Dhvani Doshi, Nicolas B. Cowan, Étienne Artigau, René Doyon, André M. Silva, Khaled Al Moulla, Yashar Hezaveh
Figure caption: This flowchart describes the steps taken in the numerical simulation to create synthetic RV observations and the template that will then be used for RV estimation.
Paper: Characterizing the Time Variability of 2M1207 A + b with JWST NIRSpec/PRISM
Authors: Arthur D. Adams, Yifan Zhou, Gabriel-Dominique Marleau, Daniel Apai, Beth A. Biller, Aarynn L. Carter, Johanna M. Vos, Niall Whiteford, Stephan Birkmann, Theodora Karalidi, Xianyu Tan, Jason Wang, Yuhiko Aoyama, Brendan P. Bowler, Mickaël Bonnefoy, Jun Hashimoto
Figure caption: Wavelength-binned images of the 2M1207 system (also known as TWA 27). The top and bottom rows show NIRSpec IFU PRISM/CLEAR (0.6–5.3 μm, R ∼ 30–300) images before and after the PSF subtraction, respectively. The field of view of the IFU is 3″ × 3″. All images are plotted on the same logarithmic intensity to color scale. We choose to bin the images according to approximations of common band boundaries: Hα, J, H, K, and the total range of NIRSpec NRS when used with the G395M/H dispersers. This highlights, for example, the very red color (J–K = 2.72 mag; K. L. Luhman et al. 2023) of 2M1207 b as a planetary-mass companion compared with field objects of a similar late L spectral type.