adsabs/AstroCLIMB huggingface dataset:
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Comparisons between the inner (0–1Re) and outer (0.75–1.5Re) median gradients, where the error bars represent the 1σ dispersion among all of the methods. The solid line represents the one-to-one relation. On the top and right side of each plot, a histogram of the distribution of the gradients in the diagram is provided.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Median values of the full set of gradients for each stellar property. The color code is used to indicate the different methods used to derive the radial profiles and the gradient, as introduced in Sections 3 and 4. (Med = collapsed median profiles, Int = collapsed integrated profiles, Spl = nonlinear Spline profiles, GPR = nonlinear GPR profiles, lin fit = linear fit gradients, diff fit = difference between two points from the generalized fit gradients, and diff = difference between two points from the radial profiles.) The filled and empty symbols show the inner and outer gradients, respectively, and the error bar correspond to 1σ of the distribution of each set of gradients. The vertical solid line indicates the limit between the collapsed methods to derive the radial profiles and the nonlinear ones.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: An illustration showing the interpretation of the gradients falling in each of the four quadrants of the ∇out vs. ∇in diagram, along with the cases of gradients falling in the one-to-one relation and along the zero lines. Inside each quadrant, illustrative shapes are shown of any of the radial profiles from where the gradients may come from, when located in any of the four quadrants.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Median offsets between the gradients derived without and with points below the RPSF. The color code is the same as in Figure 6.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Distribution of the inner gradients derived with the method of the difference between two radial points (see Section 4.3), for the case of the generalized fits. Color code is used to differentiate the different methods used to derive the radial profiles, as explained in Section 3.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Same as Figure 4 but for the outer gradients.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Median offsets. Color and symbol codes are the same as in Figure 6.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Pearson correlation factors. Color and symbol codes are the same as in Figure 6.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Full set of profiles for the MaNDala working sample, derived with the collapsed median method described in Section 3.1.1. Gray lines represent the profiles, while the blue squares show a binned median profile. Their associated error bars correspond to 1σ within each radial bin. We also show a fit to the binned median profile up to 1.5 Re with a blue line, while the extended transparent blue line shows its extrapolation. The details of the fit are inside the plot areas, where the coefficients correspond to those of Equation (4) and to the χ2 of the fit.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: As in the three previous figures, the black points in all panels show the spatially resolved profiles of all of the studied galaxy properties for manga-7815-6101. The green line is the probability distribution delivered by the GPR method, while the green shadow is its corresponding 95% confidence interval. The blue solid lines represent the linear fits performed to the mentioned probability distribution at the two adopted radial ranges. The red solid lines represent the generalized fit performed over the nonlinear GPR profiles.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Same as Figure 13, but for the nonlinear GPR method described in Section 3.2.2.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Spatially resolved profiles for all of the studied properties of the manga-7815-6101 galaxy, shown with black circles. On top, with green squares, are shown the collapsed median profiles, while the solid lines show the fit performed to them in the two radial ranges (0–1 Re and 0.75–1.5 Re). The red solid lines represent the generalized fit performed over the collapsed median profiles.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: As in the two previous figures, the black points in all panels show the spatially resolved profiles of all of the studied galaxy properties for manga-7815-6101. The green line is the nonlinear fit delivered by the Spline method. The blue solid lines represent the linear fits performed to the mentioned Spline fits at the two adopted radial ranges. The red solid lines represent the generalized fit performed over the nonlinear Spline profiles.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Spatially resolved profiles for all of the studied properties of the manga-7815-6101 galaxy, shown with black circles. On top, with green squares, are shown the collapsed integrated profiles, while the solid lines show the fit performed to them in the two radial ranges (0–1 Re and 0.75–1.5 Re). The red solid lines represent the generalized fit performed over the collapsed integrated profiles.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Same as Figure 13, but for the collapsed integrated method described in Section 3.1.2.
Paper: The MaNGA Dwarf Galaxy Sample (MaNDala): Stellar Profiles and Gradients Characterization
Authors: M. Cano-Díaz, A. Rodríguez-Puebla, A. C. Robleto-Orús, V. Ávila-Reese, H. M. Hernández-Toledo, J. A. Vázquez-Mata, O. Valenzuela, J. J. González, H. J. Ibarra-Medel, J. C. Clemente-González, L. Pavón-Alvarez
Figure caption: Same as Figure 13, but for the nonlinear spline method described in Section 3.2.1.
Paper: Interior and Climate Modeling of the Venus Zone Planet TOI-2285 b
Authors: Emma L. Miles, Colby Ostberg, Stephen R. Kane, Ondrea Clarkson, Cayman T. Unterborn, Tara Fetherolf, Michael J. Way, Sadie G. Welter
Figure caption: Histogram of the number of oceans of H2O as steam in a planet’s atmosphere. The distribution is bimodal, indicating two distinct populations. 29% of data points suggest TOI-2285 b is relatively dry (i.e., water poor), with <0.1% of Earth's oceans of water vapor in the atmosphere. A portion of the remaining 71% corresponds to a relatively water-rich atmosphere. For the water-rich population, the mean number of oceans is 5260 Earth oceans. The difference in variance between these populations further supports the distinction between the water-poor and water-rich populations.
Paper: Interior and Climate Modeling of the Venus Zone Planet TOI-2285 b
Authors: Emma L. Miles, Colby Ostberg, Stephen R. Kane, Ondrea Clarkson, Cayman T. Unterborn, Tara Fetherolf, Michael J. Way, Sadie G. Welter
Figure caption: A top-down view of the TOI-2285 system architecture, where the scale of the figure is shown along each axis. The CHZ is shown in light green, the OHZ extensions to the HZ are shown in dark green, and the orbit of the known planet is shown as a solid line.
Paper: Photometric Analysis of Asteroids in the Phocaea Region
Authors: Xiaoyun Xu, Xiaobing Wang, Karri Muinonen, Shenghong Gu, Antti Penttilä, Fukun Xu, Leilei Sun, Jing Huang, Pengfei Zhang, Ao Wang
Figure caption: Left: The distributions of the G-band geometric albedo ﹩{p}_{{}_{G}}﹩ and photometric slope βref for 44 asteroids. Right: The distribution of HG vs. HV for 44 asteroids. The red line represents the linear relationship HV = HG.
Paper: Photometric Analysis of Asteroids in the Phocaea Region
Authors: Xiaoyun Xu, Xiaobing Wang, Karri Muinonen, Shenghong Gu, Antti Penttilä, Fukun Xu, Leilei Sun, Jing Huang, Pengfei Zhang, Ao Wang
Figure caption: The distribution of the Phocaea family members in the (H,a) plane, our targets are marked with squares and circles for retrograde and prograde rotators, respectively. The gray line indicates the inner boundary of the V-shape of the Phocaea family, while the black dashed line represents the inner boundary of the 3:1 resonance with Jupiter.
Paper: Photometric Analysis of Asteroids in the Phocaea Region
Authors: Xiaoyun Xu, Xiaobing Wang, Karri Muinonen, Shenghong Gu, Antti Penttilä, Fukun Xu, Leilei Sun, Jing Huang, Pengfei Zhang, Ao Wang
Figure caption: Left: The distributions of pole longitudes and obliquities for 172 asteroids (41 derived from our work and 131 from previous studies). Right: The distribution of obliquities vs. spin rates for the 41 asteroids.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: Time-resolved photometric and spectroscopic observations of GALEX J071816.4+373139. Top left: phase-folded ﹩{g}^{{\prime} }﹩ light curve from the high-speed imaging photometer CHIMERA on the 5 m Hale Telescope (L. K. Harding et al. 2016). Bottom left: phase-folded ﹩{r}^{{\prime} }﹩ CHIMERA light curve. GALEX J071816.4+373139 varies by about 6% peak-to-peak with a period of 11.3 minutes. Right: phase-resolved Keck/LRIS spectra of GALEX J071816.4+373139 normalized and shifted vertically for clarity with the numbers on the right side of the plot indicating the center of each phase bin. Phase 0 corresponds to the maximum in the light curve illustrated on the left. The blue vertical line highlights hydrogen Hα while the red lines indicate absorption lines of neutral helium. At phase 0.5, Hα and the helium 5875 Å line are almost equally strong, and their Zeeman splitting implies a magnetic field with ∣B∣ ≈ 8 MG. At phase 0, only hydrogen is present and the absence of splitting indicates ∣B∣ ≲ 1 MG.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: HR diagram of massive, young white dwarfs in our sample. We plot our sample of 2195 white dwarfs as the smaller gray points. We plot as larger gray points white dwarfs that were searched for the infrared excess characteristic of unresolved giant planets by J. Farihi et al. (2008) or M. Kilic et al. (2009). We plot as black points white dwarfs in our sample with SEIP Source List photometry searched for the infrared excess characteristic of unresolved giant planets for the first time in this article. We plot as yellow curves cooling tracks for DA white dwarfs with MWD = (0.7, 0.9, 1.1, 1.29) M⊙.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: Occurrence of giant planets and brown dwarfs as function of mass. For stars with M*,i ≳ 3 M⊙, we find ﹩{\eta }_{\,\rm{GP}\,}=0.1{1}_{-0.07}^{+0.13}﹩ in the mass range 3 MJup ≲ Mp ≲ 10 MJup, and ηBD < 0.011 in the mass range 10 MJup ≲ Mp ≲ 30 MJup. The former value is in accord with the factor of 4 increase in ηGP predicted by G. M. Kennedy & S. J. Kenyon (2008) for stars with 3 M⊙ ≲ M* ≲ 4 M⊙ relative to solar-mass dwarfs.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: Left: composite spectrum of a typical young white dwarf plus young giant plant system. Right: absolute magnitude M4.5 in the Spitzer Infrared Array Camera (IRAC) 4.5 μm Channel 2 band as a function of time for both massive white dwarfs and giant planets. Planet-mass objects with clear atmospheres are therefore observable for at least a few tens of Myr after their host stars become white dwarfs.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: Histograms of infrared excess significances. Note that cores of each distribution match well with a standard Gaussian profile plotted in black. We indicate individual white dwarfs with excesses beyond 3σ in orange.
Paper: A Candidate Giant Planet Companion to the Massive, Young White Dwarf GALEX J071816.4+373139 Informs the Occurrence of Giant Planets Orbiting B Stars
Authors: Sihao Cheng, 思浩 程, Kevin C. Schlaufman, Ilaria Caiazzo
Figure caption: Dependence of giant planet occurrence on host star mass.
Paper: Mapping the Milky Way with Gaia BP/RP Spectra. III. The First Medium-resolution Follow-up Spectroscopy of Metal-poor Stars 
Authors: Xianhao Ye, David S. Aguado, Carlos Allende Prieto, Wenbo Wu, Jingkun Zhao, Jonay I. González Hernández, Rafael Rebolo, Gang Zhao, Yuqin Chen, Shuai Liu, Yaqian Wu
Figure caption: [M/H] vs. [C/Fe] derived from IDS/INT data. The error bars for both [M/H] and [C/Fe] are presented. Only stars for which [C/Fe] estimates are deemed reliable are presented. The horizontal dashed lines indicate [C/Fe] = +0.7 and [C/Fe] = –0.5. The CEMP star S7 is pointed out with arrows.
Paper: Mapping the Milky Way with Gaia BP/RP Spectra. III. The First Medium-resolution Follow-up Spectroscopy of Metal-poor Stars 
Authors: Xianhao Ye, David S. Aguado, Carlos Allende Prieto, Wenbo Wu, Jingkun Zhao, Jonay I. González Hernández, Rafael Rebolo, Gang Zhao, Yuqin Chen, Shuai Liu, Yaqian Wu
Figure caption: IDS/INT spectra and the corresponding best-fitting model spectra in FERᴙE are shown for three well-known metal-poor stars: HD 140283, G64-12, and BD+23 3130, as well as six target stars: S7, S10, S23, S27, S30, and S32. The black lines depict the normalized IDS/INT spectra. The blue and red lines show the best-fitting spectra in our model grids for the well-known metal-poor stars and six target stars. The three atmospheric parameters and [C/Fe] are also provided for each spectrum.
Paper: Mapping the Milky Way with Gaia BP/RP Spectra. III. The First Medium-resolution Follow-up Spectroscopy of Metal-poor Stars 
Authors: Xianhao Ye, David S. Aguado, Carlos Allende Prieto, Wenbo Wu, Jingkun Zhao, Jonay I. González Hernández, Rafael Rebolo, Gang Zhao, Yuqin Chen, Shuai Liu, Yaqian Wu
Figure caption: Zoom-in G-band spectral fitting for eight stars assessed to have reliable [C/Fe] estimates. For each star, the best-fitting synthetic spectrum is shown in the red line, along with synthetic spectra corresponding to carbon abundance variations of ±0.5 dex (dashed lines). The G-band spectral region and Hγ region are shaded in green and purple, respectively.
Paper: Mapping the Milky Way with Gaia BP/RP Spectra. III. The First Medium-resolution Follow-up Spectroscopy of Metal-poor Stars 
Authors: Xianhao Ye, David S. Aguado, Carlos Allende Prieto, Wenbo Wu, Jingkun Zhao, Jonay I. González Hernández, Rafael Rebolo, Gang Zhao, Yuqin Chen, Shuai Liu, Yaqian Wu
Figure caption: Comparisons between the metallicities derived from the INT data and the XP spectra. [M/H]XP from our estimation and Pristine’s estimation (PGSM) are shown in red and blue, respectively. The numbers of stars are annotated on the label. The mean error of [M/H]INT is indicated in the lower left corner. Excluding targets S4, S6, and S9, as discussed in the main text, the mean difference and scatter between [M/H]XP and [M/H]INT are 0.2 and 0.3 dex, respectively.
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: A comparison between K2-18b MIRI transmission spectra. The JexoPipe and JExoRES spectra are from M25. Eureka!’s mimic spectrum adopts the same settings described by M25. Eureka!’s optimized spectrum uses settings that minimize the white-light-curve MAD value. When adopting the same wavelength binning scheme, the spectra from both Eureka! reductions are comparable (i.e., within 1σ) to those from M25. The numerical values indicate the number of pixel rows used in a given spectroscopic channel. As discussed in Section 2.1.1, channels with red numbers have the least reliable transit depths.
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: An overview of MIRI retrieval results for different pixel shift cases (rows) using 8 pixel wide channels. The left column of each row shows a measured transit spectrum along with the median retrieved spectral model within representative 1σ and 2σ credibility envelopes. The right subpanels show the inferred 1D marginalized posterior distributions for the isothermal temperature (T), DMS, DMDS, and C2H5Cl (chloroethane). Critically, different pixel shift selections lead to different preferences for which gases best fit the spectrum and are constrained, with a trichotomy exhibited here between no abundance constraints (shifts 0, 4, and 7), constraints on DMS+DMDS (shift 5), or constraints on chloroethane (shifts 1, 2, 3, and 6).(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: Observed transit depth scatter (colored circles) compared to the mean transit depth uncertainty (black curve). We quantify the scatter by computing the median absolute difference (MAD) between adjacent channels. The colors represent different pixel shifts and correspond to those shown in Figure 2. For a low SNR spectrum, like that of K2-18b, the scatter should not significantly exceed the mean transit depth uncertainty. Furthermore, the scatter should be relatively consistent between pixel shifts. For this test, we achieve the most robust transit depths with six or eight pixel rows per channel; however, we caution against simply adopting these binning schemes for other data sets without first conducting similar tests.
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: Measured MIRI/LRS transmission spectra of K2-18b using a range of fixed channel sizes (1–8 pixel wide bins) and starting wavelengths (i.e., pixel shifts). The unbinned spectrum (panel (a)) exhibits significant scatter between adjacent channels, with a mean absolute difference of 663 ppm. For reference, the typical feature size in Figure 1 is ∼250 ppm. The scatter in the measured spectrum is seen to decrease with larger channel sizes and an even number of pixel rows (panels (b)–(h)).
Paper: K2-18b Does Not Meet the Standards of Evidence for Life
Authors: Kevin B. Stevenson, Jacob Lustig-Yaeger, E. M. May, Ravi K. Kopparapu, Thomas J. Fauchez, Jacob Haqq-Misra, Mary Anne Limbach, Edward W. Schwieterman, Kristin S. Sotzen, Shang-Min Tsai
Figure caption: NIRISS/SOSS and NIRSpec/G395H transit spectrum of K2-18b. The spectrum matches that published by M23 after applying a −50 ppm offset to their spectrum.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)