adsabs/AstroCLIMB huggingface dataset:
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: BPT [O III] and [Ne V]λ3426.85Å emission line fluxes compared between GELATO and the Y16 study. For each line, we restrict to objects that have at least one component detected at the 3σ level with GELATO. We compute the total GELATO flux in each line as a sum of all detected components. For each line, the GELATO fluxes are compared to the total flux from all Y16 line components. In each panel, we show error bars corresponding to three times the median GELATO uncertainty in the bottom-right corner.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: GELATO spectroscopic fits for SDSS objIDs 1237674290218401852 (top figure) and 1237648704582844527 (bottom figure). In both instances, we show the [O III]+Hβ and [N II]+Hα complexes for the objects. The spectrum is plotted as a gray line, the components are plotted as a gray dashed line, and the overall fit is shown in red. Below each fit, the deviation (residual divided by error) is shown in gray. GELATO is able to model the additional components present in the emission lines. Specifically, GELATO can model the broad components of the Balmer lines and the blueshifted components in [O III].
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Redshift distributions of objects in the SDSS Legacy MGS and our WISE Matched S/N sample. In the left panels, we show the distribution only for redshifts 0 ≤ z < 0.3, which make up the vast majority of the samples. The distribution across all redshifts is shown in the right panels. In the top panels, we show the count histograms, while in the bottom panels, we show the density histograms. The distribution for the SDSS Legacy MGS is shown with a solid line, and the distribution for our WISE Matched S/N is shown with a dotted–dashed line.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: AB magnitude distributions of SDSS photometry in the SDSS Legacy MGS and our WISE Matched S/N sample. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram. The distributions for the SDSS Legacy MGS are shown with solid lines, and the distributions for our WISE Matched S/N sample are shown with dotted–dashed lines.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Vega magnitude distributions of the WISE photometry in our WISE Matched S/N sample. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: On the right, we plot the fraction of spectroscopic AGNs (both Type I and Type II) and composite galaxies as a function of WISE mid-IR color space. We present the new color selection as a dotted–dotted–dashed line, designed to target spectroscopic AGNs and BPT composite galaxies. On the right, we plot the distribution of where our selected objects are found in BPT space for those objects with detected emission lines. Refer to Figure 1 for a description of the BPT delineations, WISE color–color selection criteria, and error bars plotted in black. With the gray dotted–dotted–dashed line, we plot the color selection criterion from this work described in Section 5.1.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of [O III] luminosity (left) and the probability that an AGN component results in a statistically better fit as generated with an F-Test (right) for different mid-IR color selection techniques. In the top panels, we show the count histograms, while in the bottom panels, we show the density histograms. The luminosity is corrected for galactic-scale extinction using the measured Balmer decrement. The selection criteria presented in this Appendix increases the completeness at all luminosities, especially at lower luminosities, and probes galaxies with less evidence of an AGN in their SED.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of L AGN/L Tot for different mid-IR color selection criteria. On the left, the AGN luminosity is not corrected for extinction, while on the right, it is corrected for extinction. In the top panels, we show the count histograms, while in the bottom panels, we show the density histograms. The selection criterion presented in this Appendix probes objects with a lower AGN contribution to the SED.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: C and N abundance comparisons between different APOGEE data releases: DR14 to DR17 (top panels), and DR16 to DR17 (bottom labels). A representative error bar is shown in each panel. The horizontal black line represents the median change. A gray shaded region is shown in each plot to represent the scatter on the median.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: The [C/N] vs. ﹩\mathrm{log}(\mathrm{Age}[\mathrm{yr}])﹩ distribution for the final sample, composed of clusters common to the OCCAM Survey and Cantat-Gaudin sample, totaling 49 clusters. Clusters with two to four stellar members are represented by orange triangles, and those with five or more stellar members are by cyan circles.
Paper: The Open Cluster Chemical Abundances and Mapping Survey. VII. APOGEE DR17 [C/N]–Age Calibration
Authors: Taylor Spoo, Jamie Tayar, Peter M. Frinchaboy, Katia Cunha, Natalie Myers, John Donor, Steven R. Majewski, Dmitry Bizyaev, D. A. García-Hernández, Henrik Jönsson, Richard R. Lane, Kaike Pan, Penélope Longa-Peña, A. Roman-Lopes
Figure caption: The [C/N] vs. log(Age[yr]) distribution for clusters common to the OCCAM Survey and Cantat-Gaudin sample, which includes 75 clusters. Young clusters, ﹩\mathrm{log}(\mathrm{Age})\leqslant 8.5﹩, are represented with navy squares. Clusters marked with a red diamond are those with only one stellar member after cuts are applied. Clusters with two to four stellar members are represented by orange triangles, and those with five or more stellar members are represented by cyan circles.
Paper: A New Infrared Criterion for Selecting Active Galactic Nuclei to Lower Luminosities
Authors: Raphael E. Hviding, Kevin N. Hainline, Marcia Rieke, Stéphanie Juneau, Jianwei Lyu, 建伟 吕, Ragadeepika Pucha
Figure caption: Distributions of E(B − V)AGN for different mid-IR color selection criteria. In the top panel, we show the count histogram, while in the bottom panel, we show the density histogram.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Eccentricity and semimajor axis of simulated planet b’s with planet c parameters drawn according to the distributions described in Table 3. The top row shows selected timestamps from simulations Set 1, with just initial and final timestamps at t = 0 and t = 7.5 Gyr connected by gray lines on the left, and all timestamps within 20% of the system’s age (i.e., t = 5.4–7.5 Gyr) on the right. The bottom row shows the same for simulations Set 2. In all panels, the points are colored according to the simulation outcome. The upper envelope set by constant angular momentum (Equation (9)) is plotted in black for a range of a b,f within a factor of 2 of 0.01 au (shaded region), as well the upper envelope set by chaotic tides (see Wu 2018, Equation (20)). The region of the diagram that lies within 20% of the observed semimajor axis and eccentricity values reported in Brady et al. (2018) is outlined in black.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Evolution of three simulations with qualitatively different outcomes. Left: for a system with M c = 1.52 M jup, a c = 2.52 au, ec = 0.64, i bc = 112.96° initially, the inner planet becomes tidally locked after 1.2 × 106 yr. Middle: for a system with M c=1.28 M jup, a c = 1.88 au, ec = 0.51, i bc = 76.93° initially, the inner planet crosses the host star’s Roche limit after 5×106 yr. Right: for M c = 1.09 M jup, ac = 2.09 au, ec = 0.014, i bc = 121.65° initially, we reproduce our observations for a sustained, eccentric orbit for the inner planet past 6.3 × 109 yr.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Relevant dynamical timescales for Kepler-1656b in the presence of companions similar to Kepler-1656c are plotted as a function of the inner planet orbital separation, a b. The shaded blue band represents the range of eccentricity oscillation timescale t EKL for outer companions in the parameter space surrounding Kepler-1656c, with 0.1 M b  < M c < 2 M jup, P 2 = 600–4000 days (a c = 1.4 − 5 au), and e c = 0 = 0.9. For the tidal shrinking and circularization timescales, we consider a range of planet and star spin periods from 1-30 days. The upper boundary of the blue region is set by ac = 5, M c = 0.1 M  b , ec = 0, and the lower boundary is set by a c = 1.4, M c = 2 M jup, ec = 0.9.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Left: the population of known giant planets is shown in e-a space. We plot subpopulations of sub-Saturns (M = 15–60 M ⊕) in blue, Saturns (M = 60–100 M ⊕) in red, and Jupiters (M > 100 M ⊕) in tan. Kepler-1656b and Kepler-1656c are overplotted as stars and colored according to mass. Data were obtained from the NASA Exoplanet Archive (Akeson et al. 2013). Right: the same population is plotted in gray. The shaded gradient represents an increasing need for gentle companions to explain orbital configurations toward the upper envelope, and the red region represents tidally locked configurations that may indicate the presence of strong companions. In both panels, the upper envelopes set by angular momentum conservation and chaotic tides are overplotted.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Normalized distributions are plotted for various orbital outer planet parameters in Set 2 of our simulations. The models are divided into the following subsets: models in which the inner planet becomes tidally locked (left), models in which the inner planet plunges into its host star (middle), and models in which the inner planet is consistent with our observations (right). For all panels, the initial distribution of our entire set of models is shown in black. Initial and final distributions of different subsets are overplotted in red and blue, respectively.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Smoothed 2D histograms of final conditions for all models (tan) and models that are consistent with our observations (blue) from Set 2 of our simulations are shown. We see that models consistent with our observations place constraints on the mutual inclination between Kepler-1656b and Kepler-1656c, which we refer to as i bc. We also overlay Kepler-1656c based on properties found in Section 2. The diagonal panels show 1D distributions of parameters, that have been normalized to sum to 1.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: The final spin–orbit angle, or obliquity, of Kepler-1656b is shown for subsets of our simulations Set 2 for which the Kepler-1656b reproduces our observations (blue line), plunges into its host star (gray dotted line), or becomes tidally locked (red dashed line).
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Smoothed 2D initial and final companion parameter distributions for models that plunged into their host star (left) and became tidally locked (right). The diagonal panels show 1D distributions of parameters, that have been normalized to sum to 1.
Paper: Kepler-1656b’s Extreme Eccentricity: Signature of a Gentle Giant
Authors: Isabel Angelo, Smadar Naoz, Erik Petigura, Mason MacDougall, Alexander P. Stephan, Howard Isaacson, Andrew W. Howard
Figure caption: Initial and final mutual inclinations for all model timestamps consistent with observations of Kepler-1656b. The shaded region shows the initial and final inclinations predicted by the quadrupole-level approximation for inner planet eccentricities of 0.6 < e b < 0.9.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The orbital periods of the stellar companions to the M-dwarf TOIs in our sample, compared with the orbital period distributions for field M dwarfs and solar-type field stars. The orbital period of the speckle companion is marked with a solid black line. The orbital period of the AO companion is marked with a dashed black line. The orbital periods of the CPM companions are marked with dotted black lines. The median orbital period of the potential close-in companions is marked with a black dashdot line. These orbital periods were calculated assuming that the eccentricity is zero, the inclination is 90◦, and the instantaneous spatial separation is approximately the orbital semimajor axis. The yellow box demonstrates our range of resolution limits for the speckle and AO observations, assuming primary and secondary masses of our median value of 0.44 M ⊙. These limits demonstrate that we could detect stellar companions at shorter orbital periods than the speckle, AO, and CPM companions, if they existed. The dashed orange line shows a Gaussian fit to the Raghavan et al. (2010) orbital period distribution, with a peak at log P = 2.44 and a standard deviation of σ log P  = 2.3. The solid orange line shows a Gaussian fit to the Duchêne & Kraus (2013) orbital period distribution, with a peak at log P = 1.27 and a standard deviation of σ log P  = 1.3. The peak of the orbital period distribution for the multiples in our sample is at log P = 4.32 with a standard deviation of ﹩{\sigma }_{\mathrm{log}P}=1.1﹩. Therefore, the orbital period distribution of the stellar companions to the M-dwarf TOIs in our sample is shifted to longer periods compared to the distributions for solar-type field stars and field M dwarfs.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: Stellar companions detected throughout the POKEMON survey of nearby field M dwarfs (black stars) compared with the stellar companions detected throughout this survey of planet-hosting M dwarfs (white stars), overlaid on the median contrast curves from NESSI (yellow lines) and DSSI (orange lines), which were used for the POKEMON survey. The range of angular separations for these companions demonstrates that we typically detect companions at the resolution limits of our instruments. However, this was not the case for our survey of M-dwarf TOIs; the closest stellar companion revealed by our high-resolution images was at an angular separation of 0.″398.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The fraction of simulated companions detectable by the high-resolution imaging observations within 100 au for all targets in the sample. As a function of projected separation, the black line shows the median value, the orange shaded area shows the interquartile region, and the yellow shaded area shows the region between the maxima and minima. This plot shows that we are able to reliably survey the region around exoplanet hosts, even at close separations where we have found a dearth of stellar companions.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The mass ratio (left) and orbital period (right) distributions used to simulate stellar companions to the M-dwarf TOIs in our sample, from Duchêne & Kraus (2013). Values for these figures were drawn assuming a primary mass of 0.44 M ⊙, which is the median primary mass for the M-dwarf TOIs in our sample.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The temperature (left) and distance (right) distributions for the 58 M-dwarf TOIs in our sample. For a magnitude-limited sample, hotter stars are intrinsically brighter and therefore more physically distant. Since the stars in our sample are cool and faint, our spatial resolution into, and achieved inner working angle for, these systems is significantly better than it would be for solar-type stars.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The median contrast curve for each filter for each of the six speckle and AO instruments used in this survey. It should be noted that the NIRC2 contrast curves extend to roughly 4″, and that the PHARO contrast curves extend to roughly 10″. The larger apertures of Gemini North, Gemini South, PHARO, and NIRC2 allow us to probe larger delta magnitudes as compared to NESSI and DSSI, as shown by their median contrast curves.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The stellar companion revealed by Keck AO data, shown in the the J–cont filter on the left, and in the Br-γ filter on the right. The stellar companion to TOI 737 was detected at 0.″845 (247 au), at 46◦, and with deblended relative magnitudes of ΔJ = 2.64 mag and ΔK = 2.61 mag.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: The only stellar companion revealed by our speckle observations, shown in the reconstructed image on the left, and marked with a cross beneath the contrast curve on the right. The stellar companion to TOI 482 was detected at 0.″398 (57 au), at 267◦, and with a delta magnitude of 2.43 at 832 nm.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: Simulated Companions: TOI198 to TOI516.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: Simulated Companions: TOI876 to TOI1639.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: Simulated Companions: TOI633 to TOI821.
Paper: A Dearth of Close-in Stellar Companions to M-dwarf TESS Objects of Interest
Authors: Catherine A. Clark, Gerard T. van Belle, David R. Ciardi, Michael B. Lund, Steve B. Howell, Mark E. Everett, Charles A. Beichman, Jennifer G. Winters
Figure caption: Simulated Companions: TOI519 to TOI620.
Paper: Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Frederick J. Vrba, Jeffrey A. Munn, Scott E. Dahm, Justice Bruursema, Stephen J. Williams, Bryan N. Dorland, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Michael C. Cushing, Dan Caselden, Martin Kabatnik, William Pendrill, Arttu Sainio, Nikolaj Stevnbak Andersen, Christopher Tanner
Figure caption: IRTF/SpeX spectra (black) compared to spectral standards (red). The spectra are normalized between 1.27 and 1.29 μm and offset by integer values for clarity. The spectral standards are: VB 8 (M7; Burgasser et al. 2008); VB 10 (M8; Burgasser et al. 2004); LHS 2924 (M9; Burgasser & McElwain 2006); 2MASP J0345432+254023 (L0; Burgasser & McElwain 2006); SDSS J083506.16+195304.4 (L5; Chiu et al. 2006); 2MASSI J0103320+193536 (L7; Cruz et al. 2004); 2MASS J12095613−1004008 (T3; Burgasser et al. 2004); and 2MASSI J2254188+312349 (T4; Burgasser et al. 2004).