adsabs/AstroCLIMB huggingface dataset:
Paper: Gap Opening and Inner Disk Structure in the Strongly Accreting Transition Disk of DM Tau
Authors: Logan Francis, Nienke van der Marel, Doug Johnstone, Eiji Akiyama, Simon Bruderer, Ruobing Dong, Jun Hashimoto, Hauyu Baobab Liu, Takayuki Muto, Yi Yang
Figure caption: Same as Figure 21, but for the comparison of different values of h  c  within 30 au, as described in Section 5.2.4. First row: gas temperature; second row: CO gas abundance; third row: comparison of the gas temperature at the τ = 1 surface for the 12CO, 13CO, and C18O lines.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Left panels: Stellar mass–age relations for the MaNDala galaxies (symbols) and the whole MaNGa sample (isodensity contours). The ages are defined within the FoV of each galaxy, while for M *, we used the NSA catalog. The upper and middle panels show the mass- and luminosity-weighted ages, respectively, while the lower panels show the logarithms of their ratios. The colors and symbols are as in Figure 12. The isocontours enclose 99%, 96%, 84%, and 37% of the data (no correction for volume completeness was applied). Their right inset panels show the distributions of logAgemw, logAgelw, and ﹩\mathrm{log}({\mathrm{Age}}_{\mathrm{mw}}/{\mathrm{Age}}_{\mathrm{lw}})﹩ for the MaNDala galaxies. The black dashed lines indicate the respective medians, while the blue and red dashed lines correspond to medians of the LTG and ETG subsamples, respectively. Right panels: Same as left panels, but for the mass- and light-weighted stellar metallicities. The isocontours in this case enclose 97%, 61%, 45%, 33%, 23%, 13%, and 5% of the data (no correction for volume completeness was applied). In the middle panel, we have added determinations from several previous studies, as indicated in the inset box (see text).
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: The g-band absolute magnitude vs. g-band effective radius of the MaNDala sample, separated into LTG and ETG dwarfs (blue and red stars, respectively). The large blue and red circles with error bars are the respective running median and 16–84th percentiles. For the purpose of comparison, other samples of DGs are plotted (see the sources in the inset). The magenta dashed line marks the M  g  = −18.5 mag limit imposed to select this sample, using the NSA Catalog photometric data.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Set of histograms that characterize the full MaNDala sample (left column), the early-type galaxies (middle columns), and the late-types (right column). From the uppermost to the bottom, the panels show the distributions of the following properties: Sérsic index, effective radius, apparent magnitude, absolute magnitude, central surface brightness, color measured at the center, and color gradients measured between 0.1 and 1 R  e . The color code is the same used to present the surface brightness and color profiles in Figure 3. The magenta dashed line in the absolute magnitude panel marks the M  g  = −18.5 mag limit imposed to select this sample, used with the NSA Catalog photometric data.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Kormendy’s diagrams for the MaNDala sample in the g band, compared with the Poulain et al. (2021) dwarf galaxy sample. In the upper panels, our galaxies are color-coded to represent the two morphology groups present in the sample: red for early-types and blue for late-types, while the red and blue circles represent their means, and the error bars indicate their respective 1σ. In the bottom panel, the color code represents the environment: dark yellow for dwarfs with D  host  ≤ 1.0 Mpc and purple for those with D  host  > 1.0 Mpc. In the left-side panels, magenta dashed lines mark the M  g  = −18.5 mag limit imposed to select this sample, using the NSA Catalog photometric data.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: The BPT-N II diagram for the MaNDala galaxies reported in this paper. The line intensities are integrated within the FoV of each galaxy. The blue, green, and red colors refer to our classifications of Star-forming (SFg), Transitioning (T), and Passive (P) galaxies, respectively, while closed circles and open triangles are for the LTG and ETG dwarfs, respectively. The lines indicate different criteria to identify the level of SF and AGN activity: the red line indicates the Kewley criteria (Kewley et al. 2001), and the black line indicates the Kauffmann criterion (Kauffmann et al. 2003).
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Location of the MaNDala galaxies in the mass–size relation (in red and blue stars for ETGs and LTGs, respectively; their averages are shown by the red and blue circles, while the error bar shows 1σ of their distribution). For comparison, the contours underneath trace the location of all the NSA DGs that fulfill the same selection criteria as our sample (from the innermost to the outermost, they represent: 0.5σ, 1σ, 1.5σ, and 2σ of this data set). The solid lines are the fits reported for this relation by Nedkova et al. (2021) for quiescent and star-forming galaxies in red and blue, respectively. The dashed lines are also fits reported by Lange et al. (2015) for early- and late-type galaxies, respectively. Diamonds in red and blue show a comparison of higher-mass galaxies with derivations for the R  e  given by Meert et al. (2013, 2016) and for the M * by Rodríguez-Puebla et al. (2020b).
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Color and color gradients in the top and bottom panels, respectively. Both panels are color-coded according to morphology types, red for early-types and blue for late-types. Symbols correspond to environment, where diamonds represent galaxies with D  host  ≤ 1.0 Mpc and crosses galaxies with D  host  >1.0 Mpc. Green points in the bottom panels represent the mean 〈μ  e 〉 g  and ∇(g − r) values for all galaxies below and above 22 mag arcsec−2 in 〈μ  e 〉 g , and error bars represent their standard deviation.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Cumulative (upper panel) and differential (lower panel) distributions of the look-back times at which 50%, 80%, and 90% of the stellar masses of the MaNDala galaxies were formed. T  x , with x = 50%, 80%, and 90%, represents the age at which the given fraction of stars formed, and ﹩{T}_{{z}_{\mathrm{obs}}}﹩ is the look-back time at the observation redshift of a given galaxy for the assumed cosmology in this paper. The dashed line in the upper panel marks the 0.5 value for the cumulative distribution.
Paper: SDSS-IV MaNGA: The MaNGA Dwarf Galaxy Sample Presentation
Authors: M. Cano-Díaz, H. M. Hernández-Toledo, A. Rodríguez-Puebla, H. J. Ibarra-Medel, V. Ávila-Reese, O. Valenzuela, A. E. Medellin-Hurtado, J. A. Vázquez-Mata, A. Weijmans, J. J. González, E. Aquino-Ortiz, L. A. Martínez-Vázquez, Richard R. Lane
Figure caption: Relationship between the Agemw/Agelw and Z ⋆,mw/Z ⋆,lw ratios shown in the lower panels of Figure 13 for the MaNDAla (symbols) and whole MaNGA (isodensity contours) samples. Symbols and colors are as in Figure 13. The isocontours enclose 99%, 96%, 84%, and 37% of the data.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Published detections and non-detections/upper-limits of helium absorption in the literature, separated into gas giants (black circles), sub-Neptunes (blue hexagons) and super-Earths/Earths (green squares). These are plotted in terms of the XUV flux received against amplitude of excess helium absorption observed, in units of the planets’ atmospheric scale heights. The red circles show our new results for WASP-52b and WASP-177b, including the upper limit after correcting for the planet’s grazing transit configuration. We reiterate that WASP-52 and WASP-177 do not have measured XUV fluxes, but instead we use appropriate spectra from the MUSCLES survey (France et al. 2016) and assume these are accurate to within a factor of three (see the text for details). We note that HAT-P-18b is shown with a lower opacity due to its detection with photometry (Paragas et al. 2021) which could be underestimating the full amplitude of this planet’s absorption. The references for these planets are given in Table 3.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Frame clipping for WASP-52b. The transit light curves are shown for order 70 (blue) and order 71 (orange), calculated in a 0.43 Å wide bin centered on the redder two lines of the helium triplet. These light curves are given in terms of the excess transit absorption. The green line shows a fit to the combined data. The shaded green region indicates ±3 median absolute deviations from the model. Any frame falling outside this region was removed (and is shown at a lower opacity). The plot symbols show how we defined the various stages of the transit, with the first-to-fourth contact points labeled. We note that frame 11 for order 71 fell off the bottom of this figure. This figure also demonstrates the repeatibility of our signal in the two separate orders.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Sample of exoplanets that have been the focus of helium studies, along with the boundaries of the Neptune Desert as defined by Mazeh et al. (2016; dashed gray lines). Each data point’s color is related to the effective temperature of its host star. Those exoplanets with detections of helium are shown within squares and those with upper limits/non-detections are shown with crosses. The sizes of the uncertainties are smaller than the plot symbols. WASP-52b and WASP-177b (this work) are shown in red. See Table 3 for references.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Same as Figure 13, but with H fraction as a free parameter. Note that the mass-loss rate is represented in logarithmic scale.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Posterior distributions of the atmospheric escape rate, outflow temperature, and bulk velocity of the outflow for WASP-52b. These results are based on 1D, isothermal Parker wind models fitted to the observed transmission spectrum.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Sample of 100 1D, isothermal planetary wind models (red) with H fraction as a free parameter fitted to the observed transmission spectrum of WASP-52b (black symbols).
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Same as Figure 16, but for WASP-177b and with the H fraction fixed to 0.90.
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Same as Figure 13, but for WASP-177b
Paper: Keck/NIRSPEC Studies of He I in the Atmospheres of Two Inflated Hot Gas Giants Orbiting K Dwarfs: WASP-52b and WASP-177b
Authors: James Kirk, Leonardo A. Dos Santos, Mercedes López-Morales, Munazza K. Alam, Antonija Oklopčić, Morgan MacLeod, Li Zeng, George Zhou
Figure caption: Frame clipping for WASP-177b. See Figure 20 for details.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Distribution of the 39 observed stars in the q-u plane. The dotted line crossing at q = u = 0 denotes the dustless solar neighborhood, and the gray solid line represents the Galactic parallel. The black dashed box is the 1σ boundary of all the stars observed with mean polarization 2.22% ± 1.16% and angle 84° ± 16°. 1σ box corresponding to mean degree of polarization (0.93% ± 0.29%, 2.80% ± 1.04%) and polarization angles (82° ± 11°, 77° ± 5°) of group 2 (region 2) and group 3 (region 3) of Figure 2 are shown as boxes of blue and red dotted lines, respectively.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Polarization angle vs. degree of polarization in Sloan i band of 39 stars toward the Czernik 3 cluster. The dashed lines are drawn to separate three groups in the observed sample—group 1 (green), group 2 (blue), and group 3(red).
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Polarization efficiency toward the Czernik 3 cluster. Two gray lines: dashed and dashed–dotted represent the empirical upper limit and the average value for the diffuse ISM, respectively, in Sloan i band using λ max = 0.55 μm and K = 1.15. See the text for further details of the shaded regions.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: WISE W4 integrated intensity map of the 3′ region around Czernik 3 with 10 contour levels between 113.02 and 113.508 DN at intervals of 0.054 DN. Polarization measurements are denoted by white lines. The cyan and blue circles centered at the star location represent the member and nonmember stars, respectively. The green dashed lines correspond to the Galactic coordinate grid passing through the center of the cluster.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Top row: VPDs for cluster Czernik 3. Bottom row: G vs. (G BP − G RP) CMDs. Bottom left panel: the entire sample. Bottom middle panel: stars within the circle of 0.5 mas yr−1 radius. Bottom right panel: probable background/foreground field stars in the direction of the Czernik 3 cluster.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Variation of degree of polarization, polarization angle, and WISE flux counts of stars toward Czernik 3, with angular distance from center of cluster. Member stars and YSO candidates are denoted with red circles and blue squares, respectively.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Observed polarization as a function of total PM of stars observed toward the Czernik 3 cluster. Two stars (#23 and #28) are excluded from this plot having PM > 10 mas yr−1.
Paper: Optical Linear Polarization Study toward Czernik 3 Open Cluster at Different Spatial Scales
Authors: Namita Uppal, Shashikiran Ganesh, D. Bisht
Figure caption: Polarization measurement of 39 stars toward the Czernik 3 open cluster superimposed on a 3′ × 3′ g-band image of Pan-STARRS. Details are described in Section 3.1.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: White dwarf cooling tracks from Bédard et al. 2020 for thick (q H ≡ M H/M * = 10−4) and thin (q H = 10−10) H layers (left and right panels, respectively). The cooling tracks cover white dwarf masses in the range 0.2−1.3 M ⊙ in steps of 0.05 M ⊙. The limits of region in the (log g, T eff) plane where wdwarfdate relies on cooling tracks are shown with blue dashed lines. We also included isochrones between 0.3 Myr−3 Gyr in gray for comparison and show where the density of isochrones increases.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Comparison of the initial-to-final mass relations included in wdwarfdate: Cummings et al. (2018) MIST-based (solid blue line) and PARSEC-based (dashed-dotted light blue line), Marigo et al. 2020 (dotted orange line), Salaris et al. 2009 (solid thin red line), and Williams et al. 2009 (dashed green line). We include the data from Cummings et al. (2018) as gray points with uncertainties for comparison. As a gray line we show the short extension we included in wdwarfdate of the IFMR from Cummings et al. (2018) and Marigo et al. (2020) at the low-mass end.
Paper: wdwarfdate: A Python Package to Derive Bayesian Ages of White Dwarfs
Authors: Rocio Kiman, Siyi Xu, 偲艺 许, Jacqueline K. Faherty, Jonathan Gagné, Ruth Angus, Timothy D. Brandt, Sarah L. Casewell, Kelle L. Cruz
Figure caption: Steps required to estimate a white dwarf total age from an effective temperature and surface gravity (T eff and log g). In this diagram, m f and m i are the final mass (mass of the white dwarf) and initial mass (mass of the progenitor star), and t cool, t ms, and t tot are the cooling age of the white dwarf, the main-sequence age of the progenitor star and the total age of the object, respectively. σ x indicates the uncertainty of each parameter x.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of 55 Cancri. This star hosts at least four giant planets, 55 Cancri b, c, f, and d. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. The expected H3 + line positions are shown separately for each planet. 55 Cancri d and f are not plotted as they are not considered good candidates for H3 + detection. The upper limits for H3 + emission for 55 Cancri b from the Q(1,0) and Q(3,0) lines are 7.4 × 1018 W and 8.4 × 1018 W, respectively. The corresponding upper limits for 55 Cancri c are 1.6 × 1018 W and 1.4 × 1018 W.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of υ Andromedae. This star hosts at least three giant planets, υ Andromedae b, c, and d. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. The expected H3 + line positions are shown separately for each planet. υ Andromedae d is not plotted as it is not considered a good candidate for H3 + detection. The upper limits for H3 + emission for υ Andromedae b from the Q(1,0) and Q(3,0) lines are 2.9 × 1018 W and 8.7 × 1018 W, respectively. The corresponding upper limits for υ Andromedae c are 2.5 × 1018 W and 1.0 × 1019 W.
Paper: Limits on the Auroral Generation of H3 + in Brown Dwarf and Extrasolar Giant Planet Atmospheres with the Keck Near Infrared Echelle Spectrograph
Authors: Aidan Gibbs, Michael P. Fitzgerald
Figure caption: Spectrum of HD 217107. This star hosts two giant planets, HD 217107 b and c. The orbit of HD 217107c is still poorly constrained and is not expected to have observable H3 +, so possible line positions are not shown. Each panel is zoomed into the expected position of one or more H3 + emission lines. The top portion of each panel shows the continuum normalized science and telluric model produced by molecfit together, while the bottom portion shows only the science spectrum after the telluric model has been divided out. The inclination of HD 217107 b is not known, so the line positions show a range from the minimum to maximum possible planetary RVs. The upper limits for H3 + emission for HD 217107 b from the Q(1,0) and Q(3,0) lines are 2.9 × 1018 W and 8.7 × 1018 W, respectively.