adsabs/AstroCLIMB huggingface dataset:
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Long-term time-averaged EW[He] variability as a function of age. The dashed lines show power-law fits to the data, with the shaded regions denoting the 1σ (darker gray) and 3σ (lighter gray) intervals. The plotted ages for the Hyades and Praesepe members are artificially spread to avoid overlapping points. Top panel:  The variability shown is the median absolute deviation of the EW[He] time series, scaled by 1.4826 to be statistically equivalent to the Gaussian standard deviation. Using the MAD accounts for outliers from low spectral S/N or poor spectral fitting. The error bars are generated from bootstrap sampling of the data (see text for further explanation). The variability decreases with age, plateauing above 300 Myr at 10−15 mÅ. The variability increases significantly at younger ages, but the relation is ill-defined due to only having two targets with τ ≤ 120 Myr. Bottom panel:  The plotted MAD is an estimate of the intrinsic variability in EW[He], quantifying variability that cannot be accounted for with measurement error (see text for further explanation). Only upper limits are measured for three targets, for which the 90% upper limits are denoted by the triangle marker. The variability–age relation persists, showing that the relation is intrinsic to the stars. The objects at the oldest ages are in agreement with there being intrinsic variability between 5 and 10 mÅ, with six of the eight older targets in agreement with there being no intrinsic variability, due to the magnitude of their EW[He] measurement uncertainties.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Intravisit variability of EW[He] as a function of age, to demonstrate variability within a 30 minute baseline. The plotted ages for the Hyades and Praesepe members are artificially spread for clarity. The markers show the median EW[He] difference for pairs of observations within the same visit for each object. The lines bracketed by triangles are not error bars. They show the 90th percentile range of intravisit variability measurements that would be found if we assume no intrinsic variability, only measurement error. The measured intravisit variability is in agreement with there being no intrinsic variability for eight of the ten objects, and just in slight disagreement for the other two. At these shortest timescales, the variability measurement is independent of age and can be explained solely by measurement error without any intrinsic EW[He] variability. This gives confidence that detecting even the youngest exospheres is possible with comparison observations directly surrounding transit.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: The “EW difference power spectrum” of the He-10830 triplet time series for our targets. We compute the pairwise difference in the EW[He] for each observation of a particular target as a function of the time separating the observations. We stack the “EW difference power spectra” for all targets besides V1298 Tau, as they are older and have lower long-term average variability. The small background points show all pairwise differences. We generate 10000 “EW difference power spectra” accounting for measurement uncertainty on individual EW[He], and the large foreground points show the median of these “EW difference power spectra” samples baseline-binned to reflect the typical variability at each timescale. The x-axis error bars show the timescale bin extents, and the y-axis error bars show the 16th–84th percentile error on the median “EW difference power spectrum.” The variability is smallest at the shortest timescales, increases after only a few hours, and plateaus out to separations of years.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: EW[He] as a function of stellar rotation period for our sample. The error bars are the median absolute deviation in EW[He] to show the amplitude of variability as compared to the EW[He] value (it should be noted that this is not the uncertainty on the median EW[He]). He-10830 triplet absorption shows a clear morphology with the stellar rotation period: more absorption at shorter rotation periods, leading to a plateau below P rot ∼ 20 days, before decreasing at the longest rotation period. This is indicative of the He-10830 feature’s nature as an activity-sensitive line: stars with shorter rotation periods have more intense high-energy coronal radiation and denser chromospheres, both of which help to form the stellar He-10830 feature.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Intrinsic variability of EW[He] as a function of stellar rotation period, following the calculation described in the text and also shown in Figure 8. There is no relation between the variability and rotation period, which we use as a proxy for activity level. This is unlike the case for the EW itself, which correlates with the rotation period. The two objects with high variability (V1298 Tau and K2-284) are younger than the rest of the sample.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Top Panel:  The EW[He] time series for the K2-136 intensive campaign. The data are fairly flat, and most of the variability shown is within the individual EW measurement uncertainties. Bottom panel:  The periodogram for the full intensive campaign of K2-136, which shows a peak that is significant just above the 1% false-alarm probability level. The period of the peak (P = 14 days) is close to the stellar rotation period (P = 15 days). Given the power of the peak, the periodicity found here is taken to be inconclusive.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: Periodicity analysis of the V1298 Tau intensive campaign. Top Panel:  The periodogram of the first week and a half of data from the intensive campaign, which features extreme variability. The peak of the periodogram (P = 3.02 days) is very close to the rotation period of the star (P = 2.9 days), and has power well above the 1% false-alarm probability level. Bottom panel:  The intensive campaign phased to the periodogram peak’s period, shown for the first week and a half separately from the rest of the intensive time-series data. The coherence at the start of the campaign is stark, while there is no apparent rotational modulation for the data from the remainder of the campaign.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: The EW[He] time series for the V1298 Tau intensive campaign. In the first week and a half of the campaign, there is extreme variability in the EW value, which then steadies at a slightly lower value for the remaining time-series coverage.
Paper: The Strength and Variability of the Helium 10830 Å Triplet in Young Stars, with Implications for Exosphere Detection
Authors: Daniel M. Krolikowski, Adam L. Kraus, Benjamin M. Tofflemire, Caroline V. Morley, Andrew W. Mann, Andrew Vanderburg
Figure caption: The EW[He] time series for the K2-100 intensive campaign. The data are fairly flat, and most of the variability shown is within the individual EW measurement uncertainties.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The computed values of T p,e, B p,s, ﹩{\dot{M}}_{{\rm{p}}}﹩, and L acc are shown as a function of M p and R in in the top left, top right, bottom left, and bottom right panels, respectively. All the quantities are calculated at R = R in, and two values of R in are adopted: R in = 2R p( = 3R J), and 4R p( = 6R J). When T p,e ≃ T int, T int is the fundamental parameter for B p,s, and disk truncation by planetary magnetic fields becomes possible when the accretion rate and luminosity are lower than the dashed lines. When T p,e ≃ T therm, the solutions are obtained self-consistently, and the solid lines represent the condition required for disk truncation.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The computed value of L acc as a function of M p and ﹩{\dot{M}}_{{\rm{s}}}﹩. As an example, r p = 50 au is chosen. The observability of L acc increases for high planet masses and high stellar accretion rates. The ultimate origin of L acc can be identified when the observed systems are located either in the region above the dashed line (see Equation (33)) or in the region below the solid line (see Equation (34)).
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The computed value of R in as a function of M p for a given value of ﹩{\dot{M}}_{{\rm{s}}}﹩. As examples, we show﹩{\dot{M}}_{{\rm{s}}}={10}^{-8}{M}_{\odot }﹩ yr−1 and ﹩{\dot{M}}_{{\rm{s}}}={10}^{-10}{M}_{\odot }﹩ yr−1. The prohibited regions (i.e., R in ≤ 1R p and R in > 4R p) are denoted by the gray shaded regions. High stellar accretion rates shrink R in, while it expands for massive planets. Magnetospheric accretion is viable for a wide range of parameters when T p,e ≃ T therm, as ﹩1\lt {R}_{\mathrm{in}}^{\mathrm{therm}}\leqslant 4﹩ when M p ≤ 10M J. In contrast, it only becomes possible at the later stages of disk evolution when T p,e ≃ T int.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The resulting line luminosities of accreting giant planets due to magnetospheric accretion. As in Figure 4, the planet position is set at r p = 50 au. On the left, the luminosities from an accretion shock are plotted, while on the right, those originating from an accretion flow are depicted. From top to bottom, the Hα, Paβ, and Brγ luminosities are shown. As expected, the accretion flow case leads to higher luminosities than the accretion shock case (see Table 2). Moreover, the line luminosities become weaker from the top to the bottom panels. These line luminosities (and line ratios) become a theoretical prediction of when and how accreting giant planets emit (observable) hydrogen emission lines.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The luminosities associated with accreting planets as a function of the disk inner edge. When R in > R p, most of the accretion energy is carried by the infall gas (i.e., L gas). This gas can heat up the host, accreting planets via L therm. As an example, f L = 0.8 is adopted in this plot.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The contrast and corresponding 5σ detection limit of the Hα line as a function of the distance from the host star for our observations on the left and right axes, respectively.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: The post-processed Hα image of HD 163296 taken by the Subaru/VAMPIRES. The value of KL=20 in pyklip-ADI reduction is used. In the image, north is up, and east is to the left. The central star is masked by the algorithm. No point-like sources emitting Hα are discovered.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: Comparison of the theoretical predictions with the observational results. The Hα emission from an accretion shock (orange circles) results in a higher observable flux than that from accretion flow (green squares) due to the adopted value of K Hα  (Table 3). The high extinction prevents a careful examination of whether our theoretical predictions can reproduce the observations, while they are not inconsistent with each other. The current observational sensitivity needs to be improved by at least a factor of 10 to reliably investigate the emission mechanisms of accreting giant planets.
Paper: Testing Magnetospheric Accretion as an Hα Emission Mechanism of Embedded Giant Planets: The Case Study for the Disk Exhibiting Meridional Flow Around HD 163296
Authors: Yasuhiro Hasegawa, Taichi Uyama, Jun Hashimoto, Yuhiko Aoyama, Vincent Deo, Olivier Guyon, Julien Lozi, Barnaby Norris, Motohide Tamura, Sebastien Vievard
Figure caption: Predicted line flux for Paβ and Brγ in the left and right panels, respectively, as in Figure 8. Hydrogen lines at longer wavelengths tend to be observed more readily as the effect of extinction becomes weaker. Multiband observations are crucial not only for discovering accreting giants, but also for characterizing them.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Spatial variations in the measured f disk, f acc, and ﹩{\dot{M}}_{\mathrm{acc}}﹩ in the Lagoon Nebula region (north is up, and east is to the left). In all panels, the background density map illustrates the distribution of point sources extracted from the VST/OmegaCAM images. The top panel shows local differences in proportion of disk-bearing (f disk) vs. disk-free (f evolved) sources when the field is divided into a grid of 0.°05 × 0.°05 bins. Each bin is color-coded according to the measured f disk − f evolved, following the color scheme of the side axis. The middle panel shows the same field characterization where each bin is colored according to the local difference between f acc and f disk. The bottom panel illustrates local variations in the average measured ﹩\mathrm{log}{\dot{M}}_{\mathrm{acc}}﹩. In all diagrams, O- and B-type members are identified as blue asterisks and crosses, respectively. The double arrow in the bottom right corner marks a reference distance of 3 pc at the location of the Lagoon Nebula. The two dashed red contours indicate the spatial concentrations of the youngest Lagoon Nebula YSOs identified by Prisinzano et al. (2019).
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Correlation trend between the estimated ages and ﹩{\dot{M}}_{\mathrm{acc}}﹩ values for accreting Lagoon Nebula members as a function of spectral class (colors and symbols are as labeled in the legend). Stars classified as potential accretors are encircled in black. The dashed lines mark the linear trend corresponding to the best-fit slope and intercept derived using the Theil-Sen estimator, with colors matching the corresponding spectral class.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Comparison between the statistical SpT-dependent fractions of disk-bearing and accreting stars measured for the Lagoon Nebula population, as estimated from the subset of objects with disk classifications based on Spitzer/IRAC data (left) and on the subset for which only near-IR J, H, K data were available (right). O-type stars do not appear in the diagrams because no definite estimate of f disk could be extracted for them. The arrows denote upper limits, and the equality line is dotted in gray.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: HITRAN line intensities for N2O showing orders of magnitude stronger features in the MIR versus the NIR. This comparison is not possible for CH3Br/CH3Cl, because their absolute cross sections have not been systematically measured in the 0.2–2 μm region relevant to reflected light observations of terrestrial planets (e.g., HWO).
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various levels of CH3Cl and CH3Br fluxes in the emission spectrum of an Earth-like planet around an AD Leonis–type star, after 50 days of observation with LIFE. Top: planet flux for atmospheres with and without CH3Cl and CH3Br. The gray area represents the 1σ sensitivity; the gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between an atmospheric model with and without CH3Cl and CH3Br.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various levels of CH3Cl and CH3Br fluxes in the emission spectrum of an Earth-like planet around a K6V-type star, after 50 days of observation with LIFE. Top: planet flux for atmospheres with and without CH3Cl and CH3Br. The gray area represents the 1σ sensitivity; the gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between an atmospheric model with and without CH3Cl and CH3Br. None of these cases seem to be detectable.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various levels of CH3Cl and CH3Br fluxes in the emission spectrum of an Earth-like planet around a TRAPPIST-1 type star, after 50 days of observation with LIFE. Top: planet flux for atmospheres with and without CH3Cl and CH3Br. The gray area represents the 1σ sensitivity; the gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between an atmospheric model with and without CH3Cl and CH3Br.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Detectability of various fluxes of N2O in the emission spectrum of an Earth-like planet around Proxima Centauri at its original distance, after only 1 day of observation with LIFE. Top: planet flux for atmospheres with and without N2O. The gray area represents the 1σ sensitivity; the dark gray error bars show an individual simulated observation. Bottom: Statistical significance of the detected differences between an atmospheric model with and without N2O.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Comparison—Retrieval. Histograms of the posterior distributions for N2O abundances in the three retrieval cases compared to the “ground truth” model values. While the 100 and 10 Tmol yr−1 cases are retrieved within ∼1.5σ, the 1 Tmol yr−1 case only produces an upper limit. Biases seen here can be largely attributed to a degeneracy between abundances (in particular H2O and N2O), as shown in the corner plots in Appendix Section A.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Dependence of observation time needed to detect 10 Tmol yr−1N2O in the Earth twin around Sun-like star at 5 pc example case on various mission parameters.