adsabs/AstroCLIMB huggingface dataset:
Paper: A Candidate for the Least-massive Black Hole in the First 1.1 Billion Years of the Universe
Authors: Masafusa Onoue, Kohei Inayoshi, Xuheng Ding, Wenxiu Li, Zhengrong Li, Juan Molina, Akio K. Inoue, Linhua Jiang, Luis C. Ho
Figure caption: The z = 5 AGN candidate presented in this Letter, CEERS-AGN-z5-1. Top: the snapshot images of seven NIRCam filters employed in CEERS. The image size of each panel is 1.″5 × 1.″5. There is a companion source to the upper left from the central source. Bottom: the optical-to-NIR SED of CEERS-AGN-z5-1. The NIRCam flux densities based on model magnitudes are presented in red. CEERS-AGN-z5-1 has an entry in the CANDELS catalog of Stefanon et al. (2017). Here we show optical CFHT/MegaCam (u *, ﹩g^{\prime} ﹩, ﹩r^{\prime} ﹩, ﹩i^{\prime} ﹩, and ﹩z^{\prime} ﹩), HST/ACS (F606W and F814W) + WCS3 (F105W, F125W, F140W, and F160W), and Spitzer/IRAC (3.6 μm and 4.5 μm) in black. Three sigma upper-limit flux densities are shown for those with signal-to-noise ratios less than 3. Horizontal and vertical error bars correspond to the filter bandwidths and photometric errors, respectively. The gray dashed line shows our best-fit power-law continuum model, where the continuum slope index is α  λ  = −1.32 ± 0.30.
Paper: A Candidate for the Least-massive Black Hole in the First 1.1 Billion Years of the Universe
Authors: Masafusa Onoue, Kohei Inayoshi, Xuheng Ding, Wenxiu Li, Zhengrong Li, Juan Molina, Akio K. Inoue, Linhua Jiang, Luis C. Ho
Figure caption: The z ∼ 5 UV luminosity function of AGNs. Our constraint from CEERS-AGN-z5-1 is shown in red. The quasar luminosity function data obtained from different surveys are shown: the rest-UV-selected quasars combining Subaru HSC and SDSS (Niida et al. 2020, cross) and CFHTLS (McGreer et al. 2018, dot) in blue. The abundance of AGNs at M 1450 = −19.5 mag is significantly higher than the extrapolation of the rest-UV-selected quasar LF (dashed line), while within the Poisson error from one object. Our data point is consistent with the AGN luminosity function from the X-ray-detected AGN candidates in the CANDELS field (Giallongo et al. 2019), which are shown in cyan. Shown in gray are the UV luminosity function of galaxies from Bouwens et al. (2021; circle) and Harikane et al. (2022a; square).
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Sensitivity of ocean pH to ﹩{P}_{{\mathrm{CO}}_{2}}﹩ at T = 288 K for pure (a) Ca, (b) Mg, and (c) Fe systems. Upper and lower bounds of ocean pH are represented by the blue shaded region. Pink shaded regions are forbidden.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Model parameters, ﹩{n}_{{{\rm{D}}}_{\mathrm{tot}}}﹩, where D = Ca, Mg or Fe, ﹩{n}_{{\mathrm{SiO}}_{2,\mathrm{tot}}}﹩, ﹩{P}_{{\mathrm{CO}}_{2}}﹩, P atm, P oc, and T. See Section 2 and Table 1 for a full list of output quantities and description.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Numerical, analytical, and semi-analytical solutions of the upper and lower limits of ocean pH in the Ca system.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Carbonate compensation depth (CCD) as a function of ﹩{P}_{{\mathrm{CO}}_{2}}﹩ and T (P atm = 1 bar) for (a) Ca, (b) Mg, and (c) Fe systems. Gray contours represent the weathering-dependent cation number density as a function of ﹩{P}_{{\mathrm{CO}}_{2}}﹩ and T (Equation (13)). Gray disk denotes modern Earth ﹩{P}_{{\mathrm{CO}}_{2}}﹩ and T.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Partitioning of (a) Ca, (b) Mg, and (c) Fe in aqueous, carbonate, and silicate phases as a function of ﹩{P}_{{\mathrm{CO}}_{2}}﹩ at T = 310 K (P atm = P oc = 1 bar) in pure Ca, Mg, and Fe systems, respectively.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: The sensitivity of ocean pH to (a) P and (b) T in the Ca system.
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Top left: the IR SED of SN 2021afdx at a phase of 197–200 rest-frame days (circles), compared to models of dust emission (solid lines). The dashed line shows the hot blackbody component without extinction and the dotted–dashed line shows the warm graphite dust component. The dotted line shows a blackbody with the same temperature and radius as the dust. The blackbody plus dust model describes our observations well. Top right: same as left, but excluding F444W from the fit (open circle). This filter may be contaminated by carbon monoxide emission. Excluding it gives a slightly better fit to the remaining data points, so we adopt this as our preferred model. Bottom left: same as above, but excluding all filters redward of F444W (open circles), i.e., all the mid-IR observations. This wavelength coverage is analogous to previous SN observations with the Spitzer Warm Mission. The dust SED is very poorly constrained and is not consistent with our mid-IR observations, leading to incorrect inferences about the dust properties. Bottom right: same as others, but using the observed spectrum of SN 2017eaw (Rho et al. 2018), extrapolated as λ −4 (dashed line), to model the near-IR filters. The resulting dust parameters are nearly identical to the blackbody fit (top left) but with a slightly higher intrinsic scatter.
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Top: ground-based optical light curve of SN 2021afdx from ATLAS and Las Cumbres Observatory, corrected for Milky Way extinction. Arrows indicate 3σ nondetections. Phases are given with respect to the last prediscovery nondetection. Center: pseudobolometric (U to I) light curve of SN 2021afdx compared to the pseudobolometric light curves of the Type IIb SN 1993J and the Type II SN 2021yja, approximately aligned to their peak phase. Open markers indicate epochs with detections in only two filters, which may not yield reliable luminosity or temperature measurements. The gradual rise and decline of SN 2021afdx, rather than a rapid rise to a plateau, suggests a Type IIb classification. Bottom: the photospheric temperature (red; left axis) and radius (blue; right axis) of SN 2021afdx derived from the data above. The dotted line shows that the ejecta radius inferred from the measured Hα velocity is consistent with the photospheric radius around peak.(The data used to create this figure are available.)
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Spectral series of SN 2021afdx compared to spectra of the Type IIb SN 2016gkg and the Type II SN 2021yja, all from FLOYDS. Phases are given to the right of each spectrum in rest-frame days. The latest spectrum is binned by a factor of 2 for clarity. We attribute the narrow emission lines (marked with gray dotted lines) to the underlying star-forming region in the Cartwheel Galaxy. The strongest telluric feature is marked with the ⊕ symbol. The remaining features can be explained by P Cygni profiles of hydrogen, helium, and Ca II. The broad, deep, asymmetric hydrogen absorption feature, the high helium-to-hydrogen line ratio, and relatively red continuum suggest a Type IIb classification for SN 2021afdx, although we never observe the hydrogen feature fully disappear.(The data used to create this figure are available.)
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: 10″ × 10″ cutouts of JWST images of the Cartwheel Galaxy centered on SN 2021afdx in 10 filters. The images are in their native resolution but have been resampled to have north up and east to the left. White circles mark the aperture used for photometry. White squares mark the region used for background subtraction. The filter name and SN brightness (in AB magnitudes) are reported in the lower left corner of each panel.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Same as Figure 4 but with no silica ﹩{n}_{{\mathrm{SiO}}_{2,\mathrm{tot}}}﹩ = 0.
Paper: Diverse Carbonates in Exoplanet Oceans Promote the Carbon Cycle
Authors: Kaustubh Hakim, Meng Tian, Dan J. Bower, Kevin Heng
Figure caption: Same as Figure 3 but with no silica ﹩{n}_{{\mathrm{SiO}}_{2,\mathrm{tot}}}﹩ = 0.
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Composite image of the Cartwheel Galaxy taken with JWST’s NIRCam and MIRI instruments, with 7.″6 × 7.″6 insets of SN 2021afdx. Credit: NASA, ESA, CSA, STScI, Webb ERO Production Team.
Paper: JWST Imaging of the Cartwheel Galaxy Reveals Dust Associated with SN 2021afdx
Authors: Griffin Hosseinzadeh, David J. Sand, Jacob E. Jencson, Jennifer E. Andrews, Irene Shivaei, K. Azalee Bostroem, Stefano Valenti, Tamás Szalai, Jamison Burke, D. Andrew Howell, Curtis McCully, Megan Newsome, Estefania Padilla Gonzalez, Craig Pellegrino, Giacomo Terreran
Figure caption: Dust masses in SNe II observed by Spitzer (circles) from Szalai et al. (2019). Lines connect multiple measurements for individual SNe, and downward-pointing arrows indicate upper limits on dust masses when reference images for subtraction were not available. The dust mass of SN 2021afdx measured here (black star) is consistent with most of their distribution. Notably, our measurement is higher than the dust masses in any of the previously observed SNe IIb, although the sample size is small.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Specific entropy s (top row), H (bottom row, solid lines), and He (bottom row, dashed lines) TAMS profiles for nonrotating single stars (red), accretors (orange), and “engineered” models of the same total mass as the post-RLOF mass of the accretors. The overlapping gray bands emphasize the CEB region, X c(1H) + 0.01 < X(1H) < X surf(1H) − 0.01, with X  c  and X surf the central and surface value of the hydrogen mass fraction. The CEB size of the engineered models increases from blue to yellow.⏬ ✎
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: H-R diagram of the binary systems. The thin dashed lines show the evolution of the donors until RLOF detachment, the solid lines show the accretors from ZAMS, through RLOF (marked by a yellow outline), until core carbon depletion. Dots with black outlines mark the accretor’s TAMS (not shown for donor). The thin dotted lines mark constant radii of R = 100, 200, 300, 500, 1000 R ⊙; all models have Z = 0.0019, an initial orbital period of 100 days, and initial masses of 38 and 30 M ⊙ (green), 20 and 17 M ⊙ (orange), 18 and 15 M ⊙ (blue).⏬ ✎
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Ratios of the binding energy profiles (including internal energy, α th = 1) of the accretor stars divided the binding energy profile of stars of the same total mass post-RLOF. The orange solid line at 1 shows the ratio of the accretor to itself as a check on the models interpolation; red solid lines show the ratio of the accretor to a nonrotating single star, while the other colors show the ratio to “engineered” stars (see Figure 2, increasing CEB size from blue to yellow; see also Appendix A.1). Each panel shows the ratios at the first time the models reach the radius indicated on the right and by the vertical dotted gray lines. The vertical gray bands mark the radial extent of the CEB in the accretors only, which may differ in the other stars. For the binding energy profiles in the numerator and denominator of the fractions plotted here see Figure 9.⏬ ✎
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Binding energy profile at fixed photospheric radius R (right y-axis) as a function of radial coordinate r. We only show profiles with α th = 1, which is accounting for the internal energy content of the star. Orange, red, and other colors show, respectively, the accretor models, single stars of same post-RLOF total mass, and engineered models with varying CEB steepness (increasing CEB size from blue to yellow; see Figure 2). Titles indicates the pre-RLOF and approximate post-RLOF accretor masses. The vertical colored lines mark the outer edge of the helium cores of the accretor and single star, which is the outermost location where Y > 0.1 and X < 0.01 (solid lines), or X < 0.1 (dashed), or X < 0.2 (dotted–dashed). The dotted gray lines mark the total radius R of these models.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: The structure of the CEB at the end of the main sequence impacts the envelope binding energy profile throughout the remaining evolution. Dashed lines show the gravitational contribution only; while solid lines include the contribution of the internal energy. The red lines show a 30 M ⊙, nonrotating, Z = 0.0019 model compared to “engineered” models of the same mass (see Figure 5, increasing CEB size from blue to yellow), but artificially imposed profile at TAMS (other colors; see text). The top (bottom) axis indicates mass coordinate (radius). We compare the models when they first reach 500 R ⊙.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Evolution as a function of the photospheric radius R of the binding energy (including the thermal energy, α th = 1) of the accretors and single stars of the same (post-RLOF) total mass. The solid and dotted lines show the accretors and single stars, respectively, and they are thin when previously the models reached larger radii. The bottom panels show the ratio of the binding energies, which is always smaller than 1 the first time a certain radius R is reached (thick lines), indicating that the accretors might have envelopes easier to unbind in at the start of a CE event. Excursions above 1 of the ratio occur only during phases of radius decrease (thin lines), which could not initiate a CE. See Figure 4 for the radial binding energy profile at given outer radii R.⏬ ✎
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Profile of the binding energy parameter λ CE as a function of mass coordinate for accretors (orange), single stars (red), and our engineered stars (other colors) at selected total radii. The vertical lines mark the outer edge of the helium cores of the accretor and single star, which is the outermost location where Y > 0.1 and X < 0.01 (solid lines), or X < 0.1 (dashed), or X < 0.2 (dotted–dashed). The CEB size of engineered models increases from blue to yellow.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Same as Figure 6 but comparing single stars differing by their initial rotation rate.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Specific entropy (top row), H (bottom row, solid lines), and He (bottom row, dashed lines) profiles for nonrotating single stars (red), accretors (orange), and “engineered” models of the same total mass as the ZAMS mass of the accretors. The overlapping gray bands emphasize the CEB region, increasing in size from blue to yellow in the engineered models.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: TAMS entropy profile of a single 30 M ⊙ star (red) and engineered models where we artificially modify the CEB region (gray shaded area partially overlapping for multiple models, increasing CEB size from blue to yellow). The CEB for a single 30 M ⊙ star has a mass thickness of 5.81 M ⊙ at TAMS, while the engineered models span the range ∼3–9.4 M ⊙.
Paper: Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events
Authors: M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger
Figure caption: Ratio of binding energy of a nonrotating 18 M ⊙ model (left) or of our 15 → 18 M ⊙ accretor (right) divided by the binding energy of the rotating models of Figure 7. The binding energy includes the internal energy (α th = 1); the gray bands highlight the CEB region of the models in the numerator. Lighter colors indicate ratios to an initially faster-rotating single star; see also legend in Figure 7.
Paper: Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Authors: P. Santini, A. Fontana, M. Castellano, N. Leethochawalit, M. Trenti, T. Treu, D. Belfiori, S. Birrer, A. Bonchi, E. Merlin, C. Mason, T. Morishita, M. Nonino, D. Paris, G. Polenta, P. Rosati, L. Yang, K. Boyett, M. Bradac, A. Calabrò, A. Dressler, K. Glazebrook, D. Marchesini, S. Mascia, T. Nanayakkara, L. Pentericci, G. Roberts-Borsani, C. Scarlata, B. Vulcani, Xin Wang
Figure caption: Relative uncertainty on the stellar mass as a function of stellar mass (upper panel) and redshift (lower panel). Large gray symbols show GLASS observations, with stars and circles indicating the color-selected candidates and the additional ones included via photo-z criteria, respectively. Smaller blue, purple, and orange symbols show the results for CANDELS GOODS-S, CANDELS COSMOS, and the parallel Hubble Frontier Field A2744, respectively, analyzed in the same way as GLASS. For the comparison samples, we restrict to galaxies with z > 6.9 and ﹩7.2\lt \mathrm{log}M/{M}_{\odot }\lt 9.3﹩. For all four data sets, curves show the median values in bins of stellar mass and redshift, plotted at the median x-value. The binning, whose step is 0.75 in both stellar mass and redshift, is the same for the various data sets. The shaded region represents the area between the 16th and 84th percentiles of the distributions.
Paper: Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Authors: P. Santini, A. Fontana, M. Castellano, N. Leethochawalit, M. Trenti, T. Treu, D. Belfiori, S. Birrer, A. Bonchi, E. Merlin, C. Mason, T. Morishita, M. Nonino, D. Paris, G. Polenta, P. Rosati, L. Yang, K. Boyett, M. Bradac, A. Calabrò, A. Dressler, K. Glazebrook, D. Marchesini, S. Mascia, T. Nanayakkara, L. Pentericci, G. Roberts-Borsani, C. Scarlata, B. Vulcani, Xin Wang
Figure caption: Spectral energy distribution and best-fit template of four of our candidates (we note that Lyα is not accounted for in the fit). Upper limits are shown at a 2σ confidence level. The two top panels show z ∼ 7.5–8 galaxies, exhibiting large (top) and low (central top) D4000 and M/L. The two bottom panels show the two most robust z > 10 galaxies identified by Castellano et al. (2022).
Paper: Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Authors: P. Santini, A. Fontana, M. Castellano, N. Leethochawalit, M. Trenti, T. Treu, D. Belfiori, S. Birrer, A. Bonchi, E. Merlin, C. Mason, T. Morishita, M. Nonino, D. Paris, G. Polenta, P. Rosati, L. Yang, K. Boyett, M. Bradac, A. Calabrò, A. Dressler, K. Glazebrook, D. Marchesini, S. Mascia, T. Nanayakkara, L. Pentericci, G. Roberts-Borsani, C. Scarlata, B. Vulcani, Xin Wang
Figure caption: Stellar mass as a function of observed absolute magnitude at 1500 Å, color-coded by redshift. Open stars and circles show the candidates selected by means of colors and the additional ones added via photometric redshifts, respectively. Gray solid curves and light blue dashed ones enclose 10%, 30%, 50%, 70%, and 90% probability densities of the total and of the z < 9 sample, respectively. Colored thick solid curves show mass–luminosity relations from the literature (Duncan et al. 2014; Song et al. 2016; Bhatawdekar et al. 2019; Kikuchihara et al. 2020; Stefanon et al. 2021) at z ∼ 8, scaled to the same IMF and color-coded according to the legend, in the relevant range of luminosities.
Paper: Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Authors: P. Santini, A. Fontana, M. Castellano, N. Leethochawalit, M. Trenti, T. Treu, D. Belfiori, S. Birrer, A. Bonchi, E. Merlin, C. Mason, T. Morishita, M. Nonino, D. Paris, G. Polenta, P. Rosati, L. Yang, K. Boyett, M. Bradac, A. Calabrò, A. Dressler, K. Glazebrook, D. Marchesini, S. Mascia, T. Nanayakkara, L. Pentericci, G. Roberts-Borsani, C. Scarlata, B. Vulcani, Xin Wang
Figure caption: Mass-to-light ratio at 1500 Å as a function of redshift, color-coded by D4000. Open stars and circles show the color and the additional photo-z-selected candidates, respectively. The mass-to-light ratio is in units of the M/Lof a 100 Myr old galaxy, with solar metallicity, no dust, and constant SFH (see text). Small gray dots are the predictions from the Santa Cruz semianalytic model (Somerville et al. 2021), with the dark gray curve showing the median predicted M/L in bins of redshift.