adsabs/AstroCLIMB huggingface dataset:
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Example surface brightness profile bulge+disk fits to the QPE host galaxy eRO-QPE4. The left panel shows the 121 × 121 pixel g-band image cutout centered on the host galaxy. The middle-left panel shows our best-fit two-component (disk+bulge) Sérsic ellipse model. The middle-right panel shows the residual of our model. The right panel shows the one-dimensional surface brightness profile fit, where the observed data are represented by black circles, the bulge by the orange line, the disk by the green line, and the total model (i.e., bulge+disk) by the blue line. The residuals are shown as the red circles under the plot.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Example SED fit from prospector (B. D. Johnson et al. 2021) for the QPE host galaxy eRO-QPE4. The black circles represent the griz-band flux densities calculated from our bulge+disk decompositions, the orange squares represent the best-fitting flux densities for each of the four bands, and the red line represents the best-fit SED. From these fits, we obtain stellar masses for the host galaxies.
Paper: Quest for a Coherent Definition of Weak-line Quasars and Its Physical Implications
Authors: Xiaoqiang Cheng, Jianfeng Wu, Qiaoya Wu
Figure caption: The Eddington ratio L/LEdd distributions for our WLQ and normal quasar samples, represented by the red and blue histograms. The red and blue lines show their respective best-fit log-normal models, with the mean values depicted by the vertical dashed lines.
Paper: A Host Galaxy Morphology Link between Quasiperiodic Eruptions and Tidal Disruption Events
Authors: Olivier Gilbert, John J. Ruan, Michael Eracleous, Daryl Haggard, Jessie C. Runnoe
Figure caption: Legacy Survey griz-band image cutouts of our sample of nine QPE host galaxies. These nine QPE host galaxies include three QPE+TDE host galaxies and are listed in Table 1.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Left: the 12CO (black) and 1.4 GHz NVSS (white) contours are overplotted on the 8 μm image of the region. Circles represent the identified YSO candidates. Red circles are optically visible YSOs (group 1), green circles are embedded YSOs (group 2), and magenta circles are identified as BD candidates. The contour levels for 12CO are 25, 31, 37, 43, and 49 K km s−1, and those of NVSS emission are 0.002, 0.0025, 0.0036, and 0.0042 Jy beam−1. Right: two clumps detected from C18O (integrated intensity) data overplotted on the 5.8 μm image. The white contours contain all the YSOs detected in our study using optical, NIR, and MIR wavelengths. The red contours are the newly detected clump, in which no YSOs were detected in our study (velocity range: −9 to −7 km s−1). The contour levels for the red contours are 0.22, 0.37, 0.51, 0.65, and 0.8 K km s−1, and those of the white contours are 0.51, 1.03, 1.55, 2.08, and 2.6 K km s−1. Source A and the circular aperture of 42″ taken for analysis (green circle) are also shown. The beam size is shown in the bottom right corner (50″).
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: The V vs. (V − I) and J vs. (J − H) CMDs for the sources in the BRC 44 region obtained from the DFOT and 2MASS/TIRCAM2 data are plotted in the top and bottom panels, respectively. The inverted triangle markers represent optically visible YSOs identified using NIR and MIR data. Sources S_0, S_1, S_2, and S_3 are marked. Blue inverted triangle markers belong to group 1 (defined in Appendix A) optically visible YSOs. The brown vector indicates a reddening vector of AV = 21. Note: S_0 is not optically visible.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: 12CO contour map of the region. The velocity range is between −13 and −5 km s−1. The contour levels are 11.1, 19.7, 28.2, 36.8, 45.3, 53.9, and 62.5 K km s−1. The beam size is shown in the bottom right corner (50″).
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: RGB image of BRC 44 using Spitzer-IRAC 3.6 μm (blue), Spitzer-IRAC 5.8 μm (green), and Spitzer MIPS 24 μm (red) data. The area observed using TIRCAM2 is shown using boxes.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Proper motions of YSO candidates relative to the ionizing source HD 213023 overplotted on the Spitzer 5.8 μm image. The blue dashed line indicates the direction of the ionizing source(s) (toward the southwest). A clear indication that the YSO candidates of BRC 44 are following an opposite “rocket motion” with respect to the position of the ionizing source(s) can be seen.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Wavelength-calibrated normalized NIR spectra of the four sources. Note that lines obtained for each source are in different wavelength ranges. TANSPEC covers a larger wavelength range than shown in the figure (5500–25400 Å). We have only plotted regions where features are visible.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Sample SEDs for the NIR spectroscopic targets. The bold line indicates the best fit with the lowest χ2 value. The light lines indicate fits that have χ2 values following the ﹩{\chi }^{2}-{\chi }_{\mathrm{model}}^{2}\lt 3\times {n}_{\mathrm{data}}﹩ criteria.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Average molecular line spectra for the region. The region used for extracting the spectra is a circular aperture of 42” as discussed in Section 3.3.1
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: Completeness-corrected galaxy number densities (colored bars) and best-fit SMF (shaded curves) for the SAGAbg sample as a function of environment. The measurements are compared, where possible, with results from the literature. Completeness-uncorrected number densities n(M⋆) are shown as gray lines in each panel; number densities obtained when only the photometric incompleteness term is applied are shown as gray crosses. We fit the SAGAbg SMF with a double Schechter function; the shaded regions show the 68% and 95% CIs of the fit, while the error bars show the 68% and 95% CIs for the binned counts. Each panel shows the best-fit SMF of the full SAGAbg-SMF sample as the dotted purple curve as a visual reference for both slope and overall normalization.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: Our dwarf SHMR (blue) from abundance matching of the SAGAbg-SMF sample compared to direct observational results obtained via H I rotation curves and weak lensing. We show the relationship between stellar mass and peak halo mass; the offset between Mpeak and Mhalo(z = 0) should be small for the bulk of the sample considered. Shaded regions show the 68% and 95% CIs of our SHMR posterior. Our results are generally consistent with previous findings in the literature up to study-to-study variability in the literature at high stellar masses and are systematically lower than previous kinematic measurements at low stellar masses. The dashed line shows the extrapolation of our abundance matching results below our limiting stellar mass of M⋆ = 5 × 106M⊙.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: The SAGAbg-SMF SHMR (blue) we infer from abundance matching of the SAGAbg-SMF field sample compared to the SHMR obtained from various abundance matching (AM) and empirical modeling (EM) studies in the literature. Clockwise from top, the panels show a comparison between the SAGAbg-SMF SHMR and relations inferred from environmentally averaged samples, satellites from beyond the Local Group, and satellites of the MW and M31. Shaded regions show the 68% and 95% CIs of our SHMR posterior. Top: a comparison to empirical and semianalytic modeling of higher-mass populations. Bottom left: our field (blue) and satellite (red) SHMRs compared to studies of the MW and M31 satellite systems. Bottom right: the same as the bottom left panel, but for satellite environments beyond the MW/M31 systems. Unless otherwise noted, reported halo masses reflect peak halo mass.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: The SAGAbg-SMF sample compared to previous wide-field surveys over the joint distribution in redshift and stellar mass of dwarfs (purple 2D histogram; left), as well as the full stellar mass range (top right) and r-band magnitude (bottom right). In each panel, the purple curves correspond to SAGAbg-SMF, gray dashed and hatched curves to GAMA, and dark-gray dotted curves to the NSA analysis of SDSS spectra. In the main panel on the left, we show the mean stellar mass at the survey limiting magnitude as estimated from the mean mass-to-light relation of the SAGAbg-SMF galaxies. In both panels on the right, we show this approximate stellar mass completeness at z = 0.05 (top) and r-band magnitude limit (bottom) as colored ticks for each survey.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: The fraction of galaxies that have received a high-quality redshift in the parent SAGA photometric catalog as a function of r-band magnitude, r-band surface brightness, and (g − r) color. The size of each point corresponds to the number of galaxies that contribute to each bin in photometric parameter space. The black contours enclose between 10% and 95% of the observed photometric properties of the SAGAbg-SMF sample, with each contour evenly spaced in enclosed fraction. The black arrow in the corner of each panel shows the median difference in each space of galaxies in our sample between z = 0.005 and z = 0.05 due to observational effects alone.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: (a) (J − H) vs. (H − K) CC diagram for all the sources (gray dots) in the BRC 44 region. We have also overplotted Hα stars with plus signs (K. Ogura et al. 2002), YSOs obtained from NIR excess as red inverted triangles, and YSOs obtained from Spitzer-IRAC and MIPS photometry as black inverted triangles. (b) [3.6] – [5.8] vs. [4.5] – [8.0] CC diagram for all the Spitzer-IRAC/MIPS detected sources (gray dots) in the BRC 44 region. YSOs obtained from Spitzer-IRAC and MIPS photometry are shown as black inverted triangles.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: (a) Vector point diagram for the sources in the BRC 44 region. The proper motions of the YSO candidates are shown with blue inverted triangles. (b) Parallax vs. G-band magnitude for stars in BRC 44 using Gaia DR3. Blue circles show YSOs selected via proper motions.
Paper: Investigating the Influence of Radiative Feedback in the Bright-rimmed Cloud 44
Authors: Rishi C, Neelam Panwar, Thomas J. Haworth, Yan Sun, Saurabh Sharma, R. K. Yadav, D.K. Ojha, H.P. Singh, Jessy Jose, Ajay Kumar Singh, Jincen Jose, Shubham Yadav
Figure caption: Result of the semianalytical analysis of RDI and the photoevaporative rocket effect. The image shows the velocity, distance, mass, and radius of the cloud from left to right and then top to bottom. The dashed line is the current observed value, and the model recreates it at around 0.7 Myr.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: Quenched fraction for the combined SAGAbg-SMF and GAMA samples as a function of stellar mass (blue error bars). Left: comparison to previous observational measurements from the NSA (M. Geha et al. 2012) in green, where upper limits (open triangles) show uncertainties from binomial counting statistics alone, and the semiempirical model median (68%/ 95% CI) predictions from UM-SAGA (Y. Wang et al. 2024) in orange. Right: comparison to recent predictions from cosmological simulations. We show predictions for isolated and central galaxies (as noted in the legend) from Illustris-TNG100 (red hatches; C. M. Dickey et al. 2021), SIMBA (purple vertical hatches; C. M. Dickey et al. 2021), TNG50 (gold line and brown crosses; J. A. Benavides et al. 2025; J. Bhattacharyya et al. 2025, respectively), and FIREBox (green diamonds; R. Feldmann et al. 2023). The cosmological simulations shown here consistently predict a turnaround in isolated galaxy quenching efficiency at 108 ≲ M⋆/M⊙ ≲ 1010; however, several higher-resolution studies predict that the quenched fraction does not rise until much lower masses (see text).
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: SHMR (blue) from abundance matching of the SAGAbg-SMF sample compared to the SHMR obtained from various cosmological simulations in the literature. We show halo mass as peak halo virial mass for the SAGAbg-SMF sample; C. R. Christensen et al. (2024) and FIRE-3 (P. F. Hopkins et al. 2023) also quote SHMRs as a function of peak halo mass, while NIHAO (L. Wang et al. 2015) and EDGE (M. P. Rey et al. 2025) quote z = 0 M200 halo masses. TNG100 (C. Engler et al. 2021) instead gives the total dynamical mass associated with the halo. For our purposes (that is, for dwarf galaxies that are being compared to simulated galaxies largely in the field), these measures should be approximately comparable.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: Top: the maximum detectable redshift, ﹩{z}_{{\rm{\max }}}﹩, that our Veff measurements would correspond to in a magnitude-limited sample. Black error bars show the binned median (error bars show the 16th–84th percentile range) as a function of stellar mass. Bottom: the raw galaxy counts for each environmental subsample of the SAGAbg-SMF galaxies as a function of stellar mass. The dashed gray line shows Ngal = 10, the minimum allowed bin count. Error bars show the 68% CI derived from Poissonian counting statistics assuming a Jeffreys prior.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: The SMF of the SAGAbg sample as a function of star formation activity. From top to bottom, the panels show all star-forming galaxies, all quenched galaxies, star-forming satellites, and quenched satellites. The dotted curve in each panel shows the best-fit double Schechter function for the star-forming SAGAbg-SMF subsample.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: We model the distribution of the SAGAbg-SMF galaxies in the absolute magnitude and size space to arrive at the photometric completeness correction, fphot, as a function of stellar mass (left) and as a function of stellar mass and redshift (right). The dashed black line in both panels shows the minimum stellar mass considered in this work.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: A schematic overview of the methodology employed to measure the SAGAbg-SMF SMF, SHMR, and quenched fraction.
Paper: SAGAbg. III. Environmental Stellar Mass Functions, Self-quenching, and the Stellar-to-halo Mass Relation in the Dwarf Galaxy Regime
Authors: Erin Kado-Fong, Yao-Yuan Mao, Yasmeen Asali, Marla Geha, Risa H. Wechsler, Mithi A. C. de los Reyes, Yunchong Wang, Ethan O. Nadler, Nitya Kallivayalil, Erik J. Tollerud, Benjamin Weiner
Figure caption: The SMF of the SAGAbg sample, as in the top panel of Figure 3, but in the redshift range 0.03 < z < 0.1.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Each panel, from the upper left to the lower right, represents the atmospheric pressure of O, O2, O3, CO, CO2, H2O, CH4, SO2, and SO3 as a function of mixing ratio. The initial conditions and the produced surface mixing ratios can be seen either in Table 3 or in the files available at DOI:10.5281/zenodo.13947863. The Archean atmospheres with fUV = 1 and fUV = 10 are depicted in purple and red, while modern Earth–like atmospheres with fUV = 1 and fUV = 10 are shown in green and blue, respectively. The different surface pressures, i.e., 4.0, 2.0, 1.0, and 0.5 bars, are represented by tones gradually shifting toward lighter shades, indicating a transition from higher to lower pressure.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Upper panel: UV flux reaching the surface of the planet TOI-700 d for an Archean atmosphere, depicted in purple (fUV = 1) and red (fUV = 10), and a modern Earth–like atmosphere, depicted in green (fUV = 1) and blue (fUV = 10). The different surface pressures, namely 4.0, 2.0, 1.0, and 0.5, are represented by tones gradually shifting toward lighter shades, indicating a transition from higher to lower pressure. The solar flux reaching both Earth’s exosphere and surface is depicted by a solid black line and dashed black line, respectively, primarily for the purpose of comparison. Lower panel: a blow-up of the flux scale depicted on the upper panel.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: TOI-700 d Archean atmosphere’s transmission spectra (first and third panels) and transmittance (second and fourth panels) for the most abundant molecules. The Archean atmospheres with fUV = 1 and fUV = 10 are depicted in purple (first panel) and red (third panel), respectively. The different surface pressures, i.e., 4.0, 2.0, 1.0, and 0.5 bars, are represented by tones gradually shifting toward lighter shades, indicating a transition from higher to lower pressure. In panels (2) and (4), in addition to the most prevalent molecules, the influences of haze and Rayleigh scattering are also visible. The combined contribution is depicted by the black line.
Paper: Evaluating Habitability and Biosignature Detection on TOI-700 d: The Role of UV Environment and Atmospheric Pressure
Authors: Viktor Yuri Doná Sumida, Raissa Estrela, Adriana Valio
Figure caption: Atmospheric pressure profiles plotted against temperature for different pressures. The Archean atmospheres with fUV = 1 and fUV = 10 are depicted in purple and red, while modern Earth–like atmospheres with fUV = 1 and fUV = 10 are shown in green and blue, respectively. The Modern Earth atmosphere models of fUV = 1 and fUV = 10 can only be distinguished from one another in the case where the surface pressure (P0) equals 1 (top right), otherwise for all other pressures the curve for fUV = 10 (blue) superimposes on the fUV = 1 (green) curve.