adsabs/AstroCLIMB huggingface dataset:
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Overview of hypotheses discussed throughout this paper for complex rotators (and scallop shells). All hypotheses are contrasted against observational constraints.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Comparison of TESS 2 and 30 minute light curves on the example of TIC 201789285, showing that the complex rotators’ sharp-peaked features are blurred in long-cadence data. TESS’ 2 minutes and upcoming 20 s observing cadences are hence ideal for detecting more of these targets.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: All available TESS light curves of young M dwarfs with complex photometric variability, spanning multiple Sectors of TESS observations. Each light curve shows the data of one TESS orbit (14 days of observations) phase-folded onto the rotational period of each star, with, e.g., “S1 i” denoting the first orbit of Sector 1 and “S13 ii” denoting the second orbit of Sector 13. Flares have been removed prior to phase-folding and plotting. All complex rotators’ features show remarkable stability and longevity over many weeks to a year (at least). See also Figure 8 for a closer view of TIC 17730996.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: All SED fits for the 10 complex rotators. The results are used to determine the stars’ apparent effective temperatures and radii. The near-UV and blue optical excesses for some targets are consistent with chromospheric activity, another indicator of strong magnetic activity for these stars. Notably, no infrared excesses are seen.
Paper: Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle
Authors: Maximilian N. Günther, David A. Berardo, Elsa Ducrot, Catriona A. Murray, Keivan G. Stassun, Katalin Olah, L. G. Bouma, Saul Rappaport, Joshua N. Winn, Adina D. Feinstein, Elisabeth C. Matthews, Daniel Sebastian, Benjamin V. Rackham, Bálint Seli, Amaury H. M. J. Triaud, Edward Gillen, Alan M. Levine, Brice-Olivier Demory, Michaël Gillon, Didier Queloz, George R. Ricker, Roland K. Vanderspek, Sara Seager, David W. Latham, Jon M. Jenkins, C. E. Brasseur, Knicole D. Colón, Tansu Daylan, Laetitia Delrez, Michael Fausnaugh, Lionel J. Garcia, Rahul Jayaraman, Emmanuel Jehin, Martti H. Kristiansen, J. M. Diederik Kruijssen, Peter Pihlmann Pedersen, Francisco J. Pozuelos, Joseph E. Rodriguez, Bill Wohler, and Zhuchang Zhan
Figure caption: Toy models of a complex rotator derived from three different hypotheses, aiming to replicate the morphology of TIC 201789285.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: FUV image of a WLM star-forming region (region 1 in this paper, as in Figures 3–6) overlaid with the PDR indicated by the [C II] λ158 μm contours (red) of 2.5 × 10−19 and 4.6 × 10−19 W m−2 pix−1, for pixels of 3.″13 per side from Cigan et al. (2016) and six CO core contours (green) from Rubio et al. (2015).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: V-band image of WLM showing the ALMA field of view (FOV) from Rubio et al. (2015; smaller magenta squares) and Rubio et al. (2022, in preparation; larger magenta rectangle). The orientation of the image is such that north is up and east is to the left. Colorbar values can be converted from counts in one pixel (DN/pixel) to Johnson magnitudes with the equation: ﹩{V}_{\mathrm{Johnson}}\,=0.0157{(B-V)}_{\mathrm{Johnson}}-2.5\mathrm{log}{V}_{\mathrm{counts}}+29.41﹩.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: FUV image of WLM showing the ALMA FOV of region 1 from Rubio et al. (2015; smaller magenta square) and of the Rubio et al. (2022, in preparation) survey (larger magenta rectangle), the regions and annuli defined here (blue circles for regions with CO cores and red dashed circles for the regions without CO cores), and the CO cores (tiny green circles). Colorbar values can be converted from counts to calibrated AB magnitudes with the equation: FUVAB = −2.5log10(FUVcounts) + 18.82.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: As in Figure 3, but for stellar-mass surface density. The color bar values are in units of M⊙ pc−2.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: As in Figure 3, but for H I, with a beam size of 7.″6 × 5.″1. The color bar values can be multiplied by 0.231 to convert from J bm−1 m s−1 to M⊙ pc−2 (see Section 2.2).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: As in Figure 3, but for pressure with a beam size of 7.″6 × 5.″1. The pressure is dominated by the gas, as is evident from a comparison with Figure 5. The color bar values are in units of g s−2 cm−1.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left: histogram of ages of the environment where CO cores formed (blue) and the environment surrounding the star-forming regions without any CO cores (red). Right: histogram of ages of the star-forming regions with CO cores (blue) and the star-forming regions without any CO cores (red). Ages were computed using the Chabrier IMF.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: FUV image of star-forming regions (blue solid or red dashed circles), star-forming knots (red circles), and CO cores (green circles) for which we compared the average of the ages of the individual knots to the calculated age of the entire region. We find that the individual knot ages are the same as or similar to the age of the region comprising the knots.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: The age of the inner region plotted against the average distance of the CO cores in that region to its nearest FUV knot in parsecs. Age error bars that appear one sided are the result of the upper or lower color uncertainties finding the same age in the model. Regions 18 and 22 are marked with an (×) as the age was determined from UBV alone.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Comparison of (a) inferred ages, log(age), and (b) color excesses, E(B − V), of the inner regions, computed using either background-subtracted fluxes (method 1; horizontal axes) or background-subtracted colors (method 2; vertical axes). Age error bars that appear one sided are the result of the upper or lower color uncertainties finding the same age in the model. The gray line represents where both methods return the same age or E(B − V). Regions 18 and 22 are marked with an (×) as the age from the background flux subtraction was determined from UBV alone. The regions without CO (regions 23, 24, 25, and 26) are marked with a red star (⋆).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Histograms of the properties of the inner regions where CO cores currently sit (blue) and the inner regions without any CO cores (red). Left: average stellar-mass surface density. Center: average H I surface density. Right: difference between the average ΣH I ,SF and the corresponding azimuthally averaged radial profile ΣH I ,rad at the region (ΣH I,SF − ΣH I ,rad).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: H I surface density of each inner region vs. the total mass of CO cores of that region, where the H I uncertainties are smaller than the size of the plot markers. We find that a higher H I surface density is found in regions with a higher total CO core mass (regions 1, 2, 9, and 15), while a high H I surface density does not necessarily correspond to a higher total CO core mass (regions 3, 4, 17, 19, 21, and 22).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left: stellar-mass surface density of each inner region plotted against the total mass of CO cores of that region. The regions without CO cores (region 23, 24, 25, and 26) are marked with a red star (⋆) and have a total MCO,vir of zero, but have been placed at a total MCO,vir of 1.2 × 102M⊙ to show their corresponding Σ*. Right: percentage of original total molecular cloud mass that is dark H2 gas in each inner region plotted against the total mass of CO cores in that region. We do not show the ﹩{M}_{\mathrm{Dark}\,{{\rm{H}}}_{2}}﹩/MMC against the total MCO,vir of regions without detected CO as they all have a total MCO,vir of zero and thus a dark H2 mass percentage of 100%. Region 9 is displayed with an arrow marker to indicate that the actual dark H2 mass ratio value is 0% but has been shifted up to better show the distribution of the dark H2 mass ratios of the other regions. The correct dark H2 mass percentages are listed in Table 2. Regions 18 and 22 are marked with an (×) as their stellar-mass surface density and dark H2 were determined from UBV alone.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left: stellar-mass surface density of each inner region plotted against the median individual CO core surface density of that region. Regions 18 and 22 are marked with an (×) as the stellar-mass surface density was determined from UBV alone. Right: H I surface density of each inner region plotted against the median individual CO core surface density of that region, where the H I uncertainties are smaller than the size of the plot markers. The x-axis error bars are not uncertainties but instead represent the range of CO core surface densities for that region, with some being smaller than the size of the marker, especially if the region only has one CO core. The regions without CO cores (region 23, 24, 25, and 26) are marked with a red star (⋆) and have a CO core surface density of zero.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left: stellar-mass surface density of each inner region plotted against the age of that region. Center: ratio (%) of dark H2 mass to original total molecular cloud mass of each inner region plotted against the age of that region. Region 9 is displayed with an arrow marker to indicate that the actual dark H2 mass ratio value is 0% but has been shifted up to better show the distribution of the dark H2 mass ratios of the other regions. Right: H I surface density of each inner region plotted against the age of that region, where the H I uncertainties are smaller than the size of the plot markers. Age error bars that appear one sided are the result of the upper or lower color uncertainties finding the same age in the model. Regions 18 and 22 are marked with an (×) as the age and stellar mass were determined from UBV alone. The regions without CO (region 23, 24, 25, and 26) are marked with a red star (⋆) and are assumed to have a dark H2 mass percentage of 100%. Neither the stellar-mass surface densities nor dark H2 mass percentages take into account the current structure of the molecular cloud, which would break up and dissociate with time.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left: stellar-mass surface density of each inner region plotted against the ratio of dark H2 mass to total molecular cloud mass of that region. Right: H I surface density of each inner region plotted against the ratio of dark H2 mass to total molecular cloud mass of that region, where the H I uncertainties are smaller than the size of the plot markers. Region 9 is displayed with a left-pointing arrow marker to indicate that the actual dark H2 mass ratio value is 0% but has been shifted right to better show the distribution of the other dark H2 mass ratios. Regions 18 and 22 are marked with an (×) as the stellar-mass surface density and dark H2 were determined from UBV alone. The regions without CO (region 23, 24, 25, and 26) are marked with a red star (⋆) and are assumed to have a dark H2 mass percentage of 100%. Neither the original molecular cloud mass nor the Σ*,SF account for the dispersal of the molecular cloud over time, which may affect any correlation seen between the two quantities. The correct stellar-mass surface densities and dark H2 mass percentages are listed in Table 2.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Histogram of average stellar-mass surface density (left), pressure (center), and H I surface density (right) of annuli representing the environment where CO cores formed (blue) and the annuli of the star-forming regions without any CO cores (red).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Stellar-mass surface density (left), pressure (center), and H I surface density (right) of each annulus plotted against the log of the total CO core mass of that region. H I uncertainties are smaller than the size of the plot markers. The regions without CO cores (regions 23, 24, 25, and 26) are marked with a red star (⋆) and have a total MCO,vir of zero, but have been placed at an MCO,vir of 1.2 × 102M⊙ to show their corresponding Σ*,env, pressure, and ΣH I ,env.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Stellar-mass surface density (left), pressure (center), and H I surface density (right) of each annulus plotted against the median individual CO core surface density of that region. H I uncertainties are smaller than the size of the plot markers. The x-axis error bars are not uncertainties but instead represent the range of CO core surface densities for that region, with some being smaller than the size of the marker. The regions without CO cores (regions 23, 24, 25, and 26) are marked with a red star (⋆) and have a CO core surface density of zero.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Left column: stellar-mass surface density (top), pressure (center), and H I surface density (bottom) of each annulus plotted against the age of that annulus. Right column: stellar-mass surface density (top), pressure (center), and H I surface density (bottom) of each annulus plotted against the age of the corresponding inner region. The age of the inner regions spans a much larger range than the age of the annuli; however, most star-forming regions are less than 100 Myr while the ages of the environment are mostly older than 100 Myr. The H I uncertainties are smaller than the size of the plot markers. Age error bars that appear one sided are the result of the upper or lower color uncertainties finding the same age in the model. Regions 18 and 22 are marked with an (×) as the age and stellar mass were determined from UBV alone. The regions without CO (regions 23, 24, 25, and 26) are marked with a red star (⋆).
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Stellar-mass surface density (left), pressure (center), and H I surface density of each annulus plotted against the dark H2 mass to original total molecular cloud mass ratio of that region. H I uncertainties are smaller than the size of the plot markers. Region 9 is displayed with a left-pointing arrow marker to indicate that the actual dark H2 mass ratio is 0% but has been shifted right to better show the distribution of the other dark H2 mass ratios. The total molecular cloud mass is the original mass of the cloud and does not take into account the dissociation of the cloud over time. Regions 18 and 22 are marked with an (×) as the dark H2 was determined from the stellar mass that was derived from UBV alone. The regions without CO (regions 23, 24, 25, and 26) are marked with a red star (⋆) and assumed to have a dark H2 mass percentage of 100%.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Spitzer 8 μm image of WLM showing the regions defined here (larger blue and red dashed circles) and the CO cores (tiny green circles). Colorbar values are in units of MJy sr−1.
Paper: The Environments of CO Cores and Star Formation in the Dwarf Irregular Galaxy WLM
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Phil Cigan, Rolf A. Jansen, Rogier A. Windhorst, Leslie K. Hunt, and Monica Rubio
Figure caption: Ratio of young stellar mass to observed CO virial mass in the inner region (M*/MCO,vir) against the age of the inner region. The gray dashed line at M*/MCO,vir = 2% shows where M*/MCO,vir is equal to the star formation efficiency of 2%.
Paper: Hierarchical Bayesian Atmospheric Retrieval Modeling for Population Studies of Exoplanet Atmospheres: A Case Study on the Habitable Zone
Authors: Jacob Lustig-Yaeger, Kristin S. Sotzen, Kevin B. Stevenson, Rodrigo Luger, Erin M. May, L. C. Mayorga, Kathleen Mandt, and Noam R. Izenberg
Figure caption: Transmission spectrum models (left) for a sample of 20 hypothetical rocky exoplanets generated following the trend in CO2 with stellar irradiation predicated on the assumption of a functioning carbonate–silicate weathering feedback mechanism (right). Planets near the outer edge of the HZ at lower stellar irradiation are predicted to possess atmospheres with higher CO2 abundances than those near the inner edge of the HZ, and such variations in CO2 manifest in observable features in the transmission spectrum.