adsabs/AstroCLIMB huggingface dataset:
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Median extracted spectra of WASP-25 (top) and WASP-124 (bottom). Each spectra is plotted in the same order in which it is printed in the legend (top to bottom). The shaded regions of the same color extending past the median lines are the 1σ range of counts extracted for that night. Each spectroscopic bin used is demarcated by dotted vertical lines, where the only gaps in the binning scheme are the strong telluric region from 7594 to 7638 Å (lightly red shaded region), the CCD gap for the first two WASP-124 observations (bottom left) at 6317–6424 Å, and the CCD gap for the other five WASP-124 observations (bottom right) at 9100–9225 Å (gray shaded region). The specific instrument and setup used for each spectrum are printed, where EFOSC2, IMACS-17.°5, and IMACS-26.°7 refer to the LRG-BEASTS (see Section 2.3), ACCESS, and MOPSS (see Section 2.1) setups, respectively. The differing throughputs between the grism used for the ACCESS and MOPSS data explain the different spectral shapes between the two WASP-124 spectra on the bottom left and the five spectra on the bottom right. Note the plotted spectrum of the NTT/EFOSC2 data (top right) was created without the sky flat, in order to visually compare with the other spectra. However, the final spectrum used for data analysis did use the sky flat as discussed in Section 2.4.
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Final detrended white light curves for each transit, utilizing the principal component analysis and Gaussian process detrending routine. The residuals obtained by the difference of the data from the best-fit model are shown below each light curve. The standard deviations of residuals are given by σ  r .
Paper: ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Benjamin V. Rackham, Erin May, Eva-Maria Ahrer, George W. King, Munazza K. Alam, Natalie H. Allen, Kevin Ortiz Ceballos, Néstor Espinoza, Tyler Gardner, Andrés Jordán, Kelly Meyer, John D. Monnier, David J. Osip, Peter J. Wheatley
Figure caption: Corner plot obtained for the PLATON best fit of WASP-25. The best fit was one with activity and no additional scatters. However, it was only slightly favored over other models. As the posteriors outline, the lack of significant features makes it difficult to strongly retrieve properties of the planetary atmosphere.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: Detection of the binary period of HD 99803A with MASCARA data. Upper left-hand panel: BLS transform of 5.4 yr of MASCARA photometric data on HD 99803A. The 26.12 days detected period and its next three higher harmonics are marked in red font. The synodic and sidereal periods of the Moon are indicated, as are some of the subharmonics of the daily observation cycle. Upper right-hand panel: zoom-in around the two lunar periods and the eclipse period. Note that the former are extremely broad, while the eclipse period is appropriately narrow. Bottom panel: folded, binned, and averaged orbital light curve about a period of 26.128 days. The eclipse is narrow (≲1% of the orbital period) and ∼4% deep, in agreement with the eclipse seen in the Sector 10 TESS data.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: Positions of the six newly discovered chemically peculiar stars, and μ Lep and β Scl in an effective temperature-surface gravity Kiel diagram. Full symbols show the positions of the stars corresponding to the observed values of ﹩\mathrm{log}g﹩ and T eff (see Table 3), while open symbols are for the best stellar model values inferred by SPInS. Colored lines are isochrones calculated for the age A SPInS inferred by SPInS. Gray-dashed lines are BaSTI-IAC evolutionary tracks of solar metallicity with masses increasing, from right- to left-hand, from 2.0 to 7.5 M ⊙, by steps of 0.5 M ⊙.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: An amplitude spectrum of the Sector 10 data for HD 99803 (HR 4423) after the eclipse was excised from the time string. There is no evidence of any pulsation out to the Nyquist frequency near 360 day−1. This plot shows on the low frequency range where there is a possibility of g-mode frequencies in a B9V star. No peaks that cannot be ascribed to instrumental variations are seen.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: An amplitude spectrum of the Sector 17 data for HD 1279 (HR 62). There is no evidence of any pulsation out to the Nyquist frequency near 360 day−1. This plot shows on the low frequency range where there is a possibility of g-mode frequencies in a B8III star. No peaks that cannot be ascribed to instrumental variations are seen.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: The light curve of HD 99803 obtained in 120 s cadence in Sector 10. The ordinate scale is Barycentric Julian Date—240 0000.0. The top panel is the full light curve; the bottom panel shows a higher time resolution view of the eclipse.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: The light curve of HD 1279 (HR 62) obtained in 120-s cadence in Sector 17. The ordinate scale is Barycentric Julian Date—240 0000.0.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: Microturbulent velocity determinations for the eight stars.
Paper: The Surface Composition of Six Newly Discovered Chemically Peculiar Stars. Comparison to the HgMn Stars mu Lep and beta Scl and the Superficially Normal B Star nu Cap
Authors: Richard Monier, E. Niemczura, D. W. Kurtz, S. Rappaport, D. M. Bowman, Simon J. Murphy, Yveline Lebreton, Remko Stuik, Morgan Deal, Thibault Merle, T. Kılıçoğlu, M. Gebran, Ewen Le Ster
Figure caption: An amplitude spectrum of the Sector 17 data for HD 123445 (HR 5294).
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The mass and radius measurements of TOI-2018 b and TOI-2018.02 (upper limits only). The solid curves are theoretical mass–radius curves from Zeng et al. (2016). The dotted and dashed lines are mass–radius curves for planets with an Earthlike core and an H/He envelope of varying mass ratios (Chen & Rogers 2016). We also show the updated mass–radius curves for water worlds when the supercritical state of water is taken into account in the equation of state (the cyan curve shows a 20%-by-mass water layer on top of an Earthlike core; Aguichine et al. 2021). We highlight other planets around low-metallicity host stars (blue symbols; [Fe/H] < −0.4). Even super-Earth (<1.5R ⊕; Rogers 2015) planets around low-metallicity stars seem to favor a lower mean density.
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The Lomb–Scargle periodograms of the TESS light curve, the WASP light curve, the HIRES S  HK  activity indicator, the measured RVs, the RV window function, and the RV residuals after subtracting the best-fit model (Figure 7). The vertical lines are, respectively, the orbital periods of TOI-2018 b (orange dashed line) and TOI-2018.02 (green dashed line), and the rotation period of the host star (red solid line). Whenever appropriate, we included horizontal dashed lines to indicate the 1% false alarm levels.
Paper: A Mini-Neptune Orbiting the Metal-poor K Dwarf BD+29 2654
Authors: Fei Dai, Kevin C. Schlaufman, Henrique Reggiani, Luke Bouma, Andrew W. Howard, Ashley Chontos, Daria Pidhorodetska, Judah Van Zandt, Joseph M. Akana Murphy, Ryan A. Rubenzahl, Alex S. Polanski, Jack Lubin, Corey Beard, Steven Giacalone, Rae Holcomb, Natalie M. Batalha, Ian Crossfield, Courtney Dressing, Benjamin Fulton, Daniel Huber, Howard Isaacson, Stephen R. Kane, Erik A. Petigura, Paul Robertson, Lauren M. Weiss, Alexander A. Belinski, Andrew W. Boyle, Christopher J. Burke, Amadeo Castro-González, David R. Ciardi, Tansu Daylan, Akihiko Fukui, Holden Gill, Natalia M. Guerrero, Coel Hellier, Steve B. Howell, Jorge Lillo-Box, Felipe Murgas, Norio Narita, Enric Pallé, David R. Rodriguez, Arjun B. Savel, Avi Shporer, Keivan G. Stassun, Stephanie Striegel, Douglas A. Caldwell, Jon M. Jenkins, George R. Ricker, Sara Seager, Roland Vanderspek, Joshua N. Winn
Figure caption: The host metallicity [Fe/H] vs. the TSM (Kempton et al. 2018) of TOI-2018 b (red) and confirmed exoplanets with a mini-Neptune size (<3R ⊕). TOI-2018 b has an estimated TSM of 103.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The contribution of different NEO sources as a function of the absolute magnitude. The ν 6 and 3:1 resonances are shown by the black and red lines, respectively. The light-green line is the contribution of weak resonances in the inner main belt. The plot shows the result for the maximum likelihood parameter set from the base model. We simply plot α  j (15) and α  j (25) for each source and connect them by a straight line (Section 5.1). The uncertainties of α  j (15) and α  j (25) are listed in Table 3.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The PDFs of a, e, i, and H from our biased base best-fit model (blue lines) are compared to the CSS NEO detections (red lines). The four panels on the left show the results for bright NEOs with 15 < H < 20, and the four panels on the right show the results for faint NEOs with 20 < H < 25. The shaded areas are 1σ (bold gray), 2σ (medium), and 3σ (light gray) envelopes. See caption of Figure 11 for the method that we used to compute these envelopes. For 20 < H < 25, the K-S test probabilities are 10−4 and 0.012 for the a and e distributions, respectively.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The probability density functions (PDFs) of a, e, i, and H from our biased base best-fit model (blue lines) and the CSS NEO detections (red lines). The shaded areas are 1σ (bold gray), 2σ (medium), and 3σ (light gray) envelopes. We used the best-fit solution (i.e., the one with the maximum likelihood) from the base model and generated 30,000 random samples with 3803 NEOs each (the sample size identical to the number of CSS’s NEOs in the model domain; 15 < H < 25). The samples were biased and binned with the standard binning (Table 2). We identified envelopes containing 68.3% (1σ), 95.5% (2σ), and 99.7% (3σ) of samples and plotted them here. The K-S test probabilities are 9.7%, 14%, 32%, and 61% for the a, e, i, and H distributions, respectively.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: Disruption models. Our base model ﹩{ \mathcal M }﹩, where the critical perihelion distance q* is assumed to be a linear function of absolute magnitude (the red line with the light-red envelope containing 68% of posteriors), is compared to Granvik et al. (2016; triangles with error bars). The surface temperature is estimated to be 820 K (average) and 930 K (subsolar) at 0.117 au (Granvik et al. 2016).
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The intrinsic (debiased) absolute magnitude distribution of NEOs from our base model (the black line is the median and the blue line is the best fit) is compared to the magnitude distribution from Harris & Chodas (2021; red line). The gray area is the 3σ envelope obtained from the posterior distribution computed by MultiNest. It contains—by definition—99.7% of our base model posteriors.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The posterior distribution of 28 NEOMOD parameters from our base MultiNest fit to CSS. The individual plots are labeled (1) to (28) following the model parameter sequence given in Table 3.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The orbital distributions of NEOs from the 3:1 source for three disruption thresholds: q* = 0.005 au (red line), q* = 0.1 au (green line), and q* = 0.2 au (blue line). By increasing the disruption distance in the model, we remove the orbits with high eccentricities, and the eccentricity distribution becomes more peaked near e = 0.5. At the same time, the inclination distribution becomes narrower.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The orbital distribution of NEOs from our biased based model (left panels) and the CSS NEO detections (right panels). The two distributions were binned with the same resolution and are shown here in the (a, e) and (a, i) projections. There are no NEOs with the aphelion inside Venus orbit in CSS (and the biased model), because the pointing strategy of CSS had negligible low solar-elongation coverage.
Paper: NEOMOD: A New Orbital Distribution Model for Near-Earth Objects
Authors: David Nesvorný, Rogerio Deienno, William F. Bottke, Robert Jedicke, Shantanu Naidu, Steven R. Chesley, Paul W. Chodas, Mikael Granvik, David Vokrouhlický, Miroslav Brož, Alessandro Morbidelli, Eric Christensen, Frank C. Shelly, Bryce T. Bolin
Figure caption: The enlarged plot on the left illustrates the degeneracy between contributions of the ν 6 resonance and weak resonances in the inner belt to bright NEOs (H = 15). The two contributions are anticorrelated and sum up to ≃30%.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Stellar flux of HIP 23309 at the stellar surface (﹩{F}_{\star }\times \tfrac{{d}_{\star }^{2}}{{r}_{\star }^{2}}﹩) in the FUV (left) and NUV (right), compared to other low-mass stars. Main-sequence comparison stars are ordered by T eff (Loyd et al. 2016). HIP 23309's stellar flux is much higher than mature stars of similar spectral type at short wavelengths due to enhanced activity because of its young age but converges with them at longer wavelengths where photospheric emission dominates. HIP 23309's flux in the FUV is similar to AU Mic’s, another extremely young M-dwarf of a similar spectral class. Overall, our spectra of HIP 23309 appear sensible in the context of other measured spectra of low-mass stars.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Comparison between HST and AstroSat-measured SEDs of HIP 23309 in the FUV (1300–1700 A). The top plot shows data in linear y-scale with error bars; the bottom plot is identical to top plot except with log y-scale and omission of error bars for easier viewing. The cyan and black data correspond to the unbinned HST and UVIT data, respectively. The blue points correspond to HST data degraded to the approximate quality of the AstroSat data, to enable a closer comparison. The green points correspond to the AstroSat data binned down by a factor of 5, to improve S/N and enable better visual comparison. We assumed Gaussian uncorrelated noise when rebinning the AstroSat data.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: UVIT FUV (left) and NUV (right) spectra of HIP 23309. Multiple NUV lines are detected; detections of FUV lines are much weaker, with only C IV being clearly detected.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Orbit-by-orbit NUV spectral (left) and band-integrated (right) flux of HIP 23309 as measured by UVIT. The band-integrated orbit-by-orbit fluxes agree with the mean flux to within 10% but are in statistically significant tension with the mean. This indicates that either our errors are underestimated, or that there is stellar variability at the ∼10% level.
Paper: UV Spectral Characterization of Low-mass Stars with AstroSat UVIT for Exoplanet Applications: The Case Study of HIP 23309
Authors: Sukrit Ranjan, Prasanta K. Nayak, J. Sebastian Pineda, Mayank Narang
Figure caption: Images of HIP 23309 in FUV-Grating1 (left) and NUV-Grating (right) are shown here. Different grating orders are marked in green.
Paper: Age Distribution of Exoplanet Host Stars: Chemical and Kinematic Age Proxies from GAIA DR3
Authors: C. Swastik, Ravinder K. Banyal, Mayank Narang, Athira Unni, Bihan Banerjee, P. Manoj, T. Sivarani
Figure caption: Comparison of δ[Fe/H] = [Fe/H]GAIA-[Fe/H]HARPS as a function of T eff. A quadratic polynomial best describes the trends of δ[Fe/H] with T eff. The blue line is the best-fit polynomial with the coefficients (p0, p1, p2) = (−3.96e–08, 2.97e–04, −4.57e–01) for the top figure, while the bottom figure shows the residuals in the approximation of the trend by the above polynomial. The green-dashed line shows the linear fit for the data.