adsabs/AstroCLIMB huggingface dataset:
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams of the O I λλ 7771, 7774 (7775 to the red), and 9265 lines. In all cases, some sky lines have been subtracted, which is what produces the faint vertical bands. The black streak is a cosmic ray. The contours are of the intensity of the emission of the O II λ9982 line. In this and the following figures, we plot the contours at 10%, 20%, ..., 90% of the maximum intensity. The kinematics of these O I quintuplet lines are compatible with those of the O II λ9982 line.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We present the emissivities per ion and per electron for the lines required to decompose the PV diagram of [N II] λ5755 (top left), [O III] λ4363 (top right), and [O II] λλ7319,7320 (bottom). The emissivity for charge exchange is per ion and per hydrogen atom. The legends indicate the transition wavelength in brackets. The line style indicates the physical process that excites the line: solid for radiative recombination, dashed for dielectronic recombination, dotted for collisional excitation, and dotted–dashed for charge exchange. Atomic data: see Table 1.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: The left and right columns present the PV diagrams of [N II] λ5755 and [N II] λ6583, respectively. In the top row, we present the observed PV diagrams of these lines. In the second and third rows, we present the models of the permitted emission in these lines due to recombination in the normal nebular plasma and the additional plasma component, respectively. In the bottom row, we present the difference between the observed PV diagram and the sum of the permitted emission, yielding what should be the emission due to collisional excitation only from the normal nebular plasma. The maximum of the intensity/color scale is given at the upper right of each panel (constant on the left; variable on the right). The contour lines are of the intensity of the N II λ5680 line (Figure 29/Figure 6). Clearly, the fractional contribution of recombination from both plasma components, but especially the additional plasma component, is much greater for [N II] λ5755.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These PV diagrams present the [N II] temperature. Top panel: we use the observed PV diagrams of the [N II] λλ5755,6583 lines. Middle panel: we decompose the [N II] lines using the atomic data as published (Figure 30). Bottom panel: we scale the recombination coefficients (atomic data; Table 1) by a factor of 1.2 when decomposing the [N II] lines. In all panels, the temperature scale spans the range 6000–16,000 K and the contours are of the intensity of the N II λ5680 line (Figure 29). After correcting for the recombination contribution to the [N II] lines (middle), the [N II] temperature is a much better approximation of the [O III] and [Ar III] temperatures, but may still be too high in the innermost regions. The [N II] temperature map in the bottom panel is nearly as uniform as the [O III] (Figures 14 and 36) and [Ar III] temperatures (Figure 15).
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the PV diagrams of the N II λ5680 line as observed (top), the model of the recombination in this line from the normal nebular plasma (middle), and the difference between the previous two (bottom), which is interpreted as the recombination in this line due to the additional plasma component. The contours in the three panels correspond to the contours for the N II λ5680 line (top panel). The three panels share the same intensity scale.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These panels present the decomposition of the [O II] λλ7319,7320 line profiles (top row, both columns). The middle row presents the total permitted emission in both lines using O II λ4649 (left) and O II λ9982 (right) as models. The bottom row is the difference between the observations (top) and the models (middle). All panels share a common intensity scale. The model based upon the O II λ4649 line accounts for almost all of the emission from the main shell in the [O II] λλ7319,7320 lines.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: These PV diagrams present the [O II] λ3726 and [O II] λλ7319,7320 lines (top row) and the O II λ4649 and O II λ9982 lines (bottom row). The contours on the PV diagrams in the top row are of the intensity of the PV diagrams in the bottom row. The morphology of the PV diagrams for the [O II] lines are very different. For the [O II] λ7320 line, the main shell is the brightest feature and its emission matches very closely that from O II λ9982. Also, the velocity splitting for [O II] λ3726 is greater than that for O II λ4649 whereas the velocity splitting for [O II] λ7320 is the same as for O II λ9982.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: Left: we present the temperature-sensitive O II λλ4089/4649 ratio and its uncertainty as a function of the temperature (the pink band), based upon an intensity limit at 40% of the maximum intensity and the 90% width of its distribution of pixel values. The temperature implied is rather low, ﹩\mathrm{log}{T}_{e}=3.25\mbox{--}3.7﹩ dex, unless the density is very low. Right: we present the observed value of the density-sensitive ratio O II λλ4662/4649 and its uncertainty as a function of the electron density (the pink band; same definitions). The observed O II λλ4662/4649 ratio implies high densities (104–105 cm−3) at the lowest temperatures (<2500 K) and densities of 5000–30, 000 cm−3 at higher temperatures.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: We compare the PV diagrams of the forbidden [N II] λλ5755,6583 lines (top and middle, respectively) and of their ratio. The contour lines are of the emission in the N II λ5680 line (Figure 29/Figure 6). The main shell is notably brighter, compared to the filament on its receding side, in the [N II] λ5755 line, as is the emission from the permitted N II λ5680 line. The ratio of the forbidden lines presents an excellent correspondence between the excess emission in the [N II] λ5755 line and the emission from N II λ5680.
Paper: NGC 6153: Reality is Complicated 
Authors: Michael G. Richer, Anabel Arrieta, Lorena Arias, Lesly Castañeda-Carlos, Silvia Torres-Peimbert, José Alberto López, Adolfo Galindo
Figure caption: In the left column, these panels present the lines of O II λ4089, O II λ4662, and O II λ4649. In the right column, the panels present the PV diagrams of the line ratios O II λλ4089/4649 and O II λλ4662/4649. The contours in the right panels are the intensity contours from the PV diagram of the O II λ4649 line (bottom left). The bright fringe at the top of the PV diagrams is due to imperfect subtraction of the nebular continuum. A cosmic ray contaminates the PV diagram of the O II λ4662 line.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Top: The radius that an L5 (T eff ≈ 1600 K) brown dwarf would have depending on its age over the range 0.1–10 Gyr (Baraffe et al. 2015). Bottom: The corresponding radius of the planet candidate based on the R  p /R  h  value from our MCMC modeling. The shaded region indicates the 1σ uncertainty on the planet radius.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Left: 2MASS J0835+1953's SpeX Prism spectrum (black) along with the best single spectral template fit (red). Gray boxes along the top axis denote the wavelength ranges of the J, H, and K  S  bands. The shaded region along the lower axis shows the uncertainty on 2MASS J0835+1953's spectrum as a function of wavelength. The inset shows a zoom in on a region surrounding a potential absorption feature from CH4 at 1.63 μm, which may indicate the presence of a T-dwarf companion in the spectrum. Right: The best-fitting binary template (magenta), which consists of a L5.5 primary (red) and a T0.0 secondary (blue).
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: A corner plot of the parameters in the MCMC simulation, with the 1σ range of each parameter indicated with dashed lines. Red curves show the Gaussian priors on T 0 and i. The a/R  h  posterior was calculated using the P and ρ  h  posteriors with Kepler’s third law. This plot was made with corner (Foreman-Mackey 2016).
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Follow-up light curves of 2MASS J0835+1953. The black points with error bars show the flux binned over 30 minute intervals. Each panel has the same time extent. An orange line marks the transition from 30 s to 60 s exposures in the appropriate light curves. A repeat transit event has not been observed, but these observations rule out source variability as a likely cause as the candidate event in Figure 4.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: The results of our injection and recovery simulation. Grid cells are colored by their detection rate in percent, which is also listed in the center of each cell. The occurrence rate of planets in each grid cell, as calculated in Dressing & Charbonneau (2015), is given in parentheses at the bottom of each cell (also in percent). Cells in which no planets were recovered are colored in gray. Histograms along the top and right axes show the summed detection rates along the period and radius dimensions, respectively.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Random samples from the MCMC on the night of the candidate transit. Note that the sampling was performed using all of 2MASS J0835+1953's unbinned data, and that we are only showing the night of the candidate transit for clarity. Our data is consistent with two general classes of solutions: one in which our observations are the deepest part of the transit event, and one in which we sampled the ingress of a deeper event.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: Keck/NIRC2 AO K  s -band 5σ contrast curve from our injected planet simulation (Section 4.2.2). The inset plot shows the 1″ × 1″ cutout of the combined image. No companions are observed within the contrast limits of the observations.
Paper: The Perkins INfrared Exosatellite Survey (PINES). II. Transit Candidates and Implications for Planet Occurrence around L and T Dwarfs
Authors: Patrick Tamburo, Philip S. Muirhead, Allison M. McCarthy, Murdock Hart, Johanna M. Vos, Eric Agol, Christopher Theissen, David Gracia, Daniella C. Bardalez Gagliuffi, Jacqueline Faherty
Figure caption: A Lomb–Scargle periodogram of all the unbinned data collected for 2MASS J0835+1953. A dashed orange line shows the 95% false-alarm probability threshold. No significant peaks were detected in the periodogram or in periodograms constructed using individual nights of data.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Comparison between the T eff, ﹩\mathrm{log}g﹩, and ﹩{v}_{e}\sin i﹩ values found in this work and the ones derived by Alonso-Santiago et al. (2021) for the common 11 stars. The agreement in T eff and ﹩{v}_{e}\sin i﹩ is very good; that in ﹩\mathrm{log}g﹩ is not, but this is unsurprising, as different methods for deriving spectroscopic ﹩\mathrm{log}g﹩ values for A stars are known to produce quite different values.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Example spectra for stars in our sample obtained with the SOPHIE, ESPaDOnS, and HARPS spectrographs. The wavelength range, between 4450 and 5400 Å, corresponds to the one used to derive stellar parameters. The spectra (in black) are shifted vertically for clarity; we also show the best-fit synthetic spectra (red) for each.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Gaia DR3 RVs for Stock 2 members and for our spectroscopic targets, as a function of G magnitude. Uncertainties for the members are not plotted for clarity, they have a mean value of 3 km s−1. While the RVs for our targets are consistent with the median RV for the cluster, the dispersion in the values is larger than for fainter members, as is expected for these hotter stars.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Sc vs. Ca abundances for our sample, color coded by the [Fe/H] abundance. The dotted lines indicate values of 0 dex, for reference. The size of the symbols corresponds to rotational velocity for each star; larger symbols are larger ﹩{v}_{e}\sin i﹩. The star symbols indicated the nine Am candidates listed in Table 4.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Absolute and derreddened Gaia DR3 CMD for Stock 2, with the members derived by Cantat-Gaudin et al. (2020) in blue and our spectroscopic targets indicated with orange circles. We also show a three isochrones of different ages and Solar metallicity for reference.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Mean abundances of the Am stars identified in the Pleiades, Coma Ber, and Hyades, and the mean abundances of the nine Am stars identified in this work in Stock 2.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Extinction map used to produce a dereddened CMD for Stock 2. The cluster members’ positions in Cartesian space (centered on the Sun) are indicated by the contours. Only one layer of the data cube is shown in each projection.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Abundances obtained for the full sample of stars that was analyzed. The stars are sorted based on the classification described in the text: from top to bottom, Am candidates (note the depletion in Sc, Ca, and O), uncertain cases, and normal stars.
Paper: Chemically Peculiar Stars in the Open Cluster Stock 2
Authors: Laia Casamiquela, Marwan Gebran, Marcel A. Agüeros, Hervé Bouy, Caroline Soubiran
Figure caption: Left: spatial distribution of Stock 2 members (blue), with our spectroscopic targets highlighted (orange). Right: proper-motion distribution.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Top: white-light curves (LC) composed from dividing the target by the sum of comparison stars, i.e., the raw LC. The first two columns are for the VLT/FORS2 transits, showing the exact data of Nikolov et al. (2018). The last two columns are new Magellan/IMACS observations directly from ACCESS's custom pipeline. The data points marked with an x were identified as outliers and are not included in the rest of the analysis. Middle: the detrended white LC (blue points) produced utilizing our PCA+GP routine, the corresponding best-fit transit LC (solid black line) with orbital parameters shown in Table 3, and the residuals (red points) produced by subtracting the detrended data from the model. The value of σ given on each residual panel is the standard deviation of the residuals in ppm. Bottom: the common-mode correction term, which was produced by dividing the top LC by the best-fit transit model (the black LC in the middle panel; see Appendix B.2 for detailed discussions). This term was used to correct for common systematics in the binned light curves.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Histograms used to outline the biases and precisions of both the GP (top row) and the CMC+GP (bottom row) routines. Left column: we fit each of the 500 total synthetic binned light curves using the GP and CMC+Poly routines; we then take the difference of each fitted binned depth from the true depth (R  p /R  s  = 0.1157) used to produce all synthetic data. That difference was divided by the uncertainty of the fitted depth, in order to obtain the bias from the input depth, relative to the uncertainties. The distributions of the relative differences are plotted. Middle column: this is similar to the left column, but instead is the difference of each fitted binned depth from the mean depth of all 10 bins in its corresponding transmission spectra. This provides a relative bias on obtained transit depths. In this case, “relative” means relative to the transmission spectrum’s mean depth. For both the left and middle columns, the black dashed line represents the average 16 and 84 percentiles of the histograms, the middle solid black line is the 50 percentile, and the red dotted line is 0. This corresponds to the true value of the depth; thus, when the dashed black line and dotted red line do not overlap, the routine has an inherent bias on that obtained depth. Right column: this is the standard deviation of each of the 50 transmission spectra. It shows the measured scatter of the transmission spectra, where the true scatter is 0, because the spectra were made to be flat. Here, the black dashed line is the mean width of all bins' uncertainties. Note that, although both routines produce scatter well under their respective mean uncertainty widths, because the mean uncertainty width is over six times larger for the GP routine, the CMC+Poly routine is much more precise.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: Photometric monitoring of WASP-96: The top row is TESS monitoring. There, the red dashed lines are the Juliet semi-periodic best fit. The gray dots are the original 30-minute cadence TESS observations, and the green dots are the data at 100 (∼3.34 hr) binning, with their associated error bars in blue. The right figure is from sector 29 data and the left is from sector 2, where both sectors were combined to act as one data set for the Juliet fit (the binned data were used for the fitting). The bottom row is ASAS-SN monitoring, where the blue dashed lines are the Juliet semi-periodic best fit. On the right, the green hollow circles with associated error bars correspond to the g band data. On the left, the red hollow circles with associated error bars correspond to the V band data. The V- and g-band data were used as separated data sets in the Juliet fit. For all Juliet fits (blue and red dotted lines), there is a gradient of shaded gray regions representing the 1σ, 2σ,and 3σ confidence intervals. For the TESS data, the confidence intervals are about the size of the dotted line.
Paper: ACCESS: Confirmation of a Clear Atmosphere for WASP-96b and a Comparison of Light Curve Detrending Techniques
Authors: Chima D. McGruder, Mercedes López-Morales, James Kirk, Néstor Espinoza, Benjamin V. Rackham, Munazza K. Alam, Natalie Allen, Nikolay Nikolov, Ian C. Weaver, Kevin Ortiz Ceballos, David J. Osip, Dániel Apai, Andrés Jordán, Jonathan J. Fortney
Figure caption: The transmission spectra using only the two Magellan/IMACS transits (top), only the two VLT/FORS2 transits (middle), and combining all four transits (bottom). In all three plots, the black points correspond to the final spectrum produced by taking the weighted average of all overlapping bins. When combining each spectrum, an offset is applied so that the means of each individual spectra are consistent, before the bins are averaged together. The respective centers of the Na I and K I absorptions are plotted as dotted gray and yellow lines.