adsabs/AstroCLIMB huggingface dataset:
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: Morphology, kinematics, and emission-line measurements of SDSS J1445+4926. (a) The g-, r-, and z-band composite image from DESI overlaid with the nonparametric EW[O III] map; the purple hexagon represents the MaNGA bundle size, and the purple cross marks the galaxy photometric center. (b) Gas velocity field. Black contours represent 20%, 30%, 50%, 70%, and 90% levels of EW[O III]. The black dotted ellipse in panels (a), (b) marks an off-centered region with abnormal velocities (“Region A” in the text). The cyan polygon marks a region requiring Hα broad components for emission-line modeling. (c) Stellar velocity field. The gray solid (dashed) line is the photometric major (minor) axis. (d) to (f) Hα+[N II], [S II] doublet, and [O III]λ5007 emission-line fitting results for a spaxel marked as a red cross in panel (b). Black is the observed emission-line spectrum, blue and red show the two narrow Gaussian components, and the dark-blue Gaussian in panel (d) is applied to model the broad Hα component. Green is the best-fitting model—it is a combination of all the Gaussian components. (g) Hα+[N II] fitting for the spaxel marked by the green cross in panel (b). (h) Hα+[N II] wavelength range fitted by a single Gaussian model for the spaxel marked as the blue cross in panel (b).
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: χ2 as a function of ΔBIC for different emission-line models. (a) The relation between ΔBIC12 and χ2 for the Hα+[N II] wavelength region with 6529 Å < λ < 6610 Å, where ΔBIC12 = BIC1 − BIC2 is calculated as the difference between the BIC of single (BIC1, triangles) and double (BIC2, dots) Gaussian fittings. (b) The same relation but for the double narrow Gaussian and double narrow Gaussian plus a broad Hα fitting. ΔBIC23 = BIC2 − BIC3 is measured as the difference between the BIC of emission-line models with (BIC3, crosses) and without (BIC2, dots) broad Hα components. In both panels (a) and (b), symbols are color coded by the distance from a certain spaxel to the geometric center of Region A, and the dashed line marks ΔBIC = 10. (c) The same configurations as panel (b), but the symbols are color coded by angle β (see Figure 1(b) for the definition of β).
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: Comparison of spectra inside and outside Region A. (a) The spatially resolved Hα to Hβ flux ratios, where the black dotted ellipse represents Region A and the gray solid (dashed) line is the galaxy photometric major (minor) axis. The green circle is centered on the galaxy photometric center, and its radius is set as the distance from the broad Hα flux peak (red cross) to the galaxy center. The spaxel marked with a blue cross outside Region A is located at the green circle and has similar Hα/Hβ to that of the broad Hα flux peak. (b) The Hα+[N II] spectrum for the spaxel with maximum broad Hα flux (red cross in panel (a)). The observed emission-line spectrum (black) is well modeled by two narrow Gaussian components (blue and red) plus a broad Hα component (dark blue), and the combination of these Gaussian components is the best-fitted model (green). (c) The Hα+[N II] spectrum (black) for the comparison spaxel (blue cross in panel (a)); the best-fitted single Gaussian model is shown in green for each emission line.
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: [N II]-BPT diagnostic diagram and spatially resolved BPT map. (a) The [N II]-BPT diagnostic diagram, where the dashed (Ka03; G. Kauffmann et al. 2003) and solid (Ke01; L. J. Kewley et al. 2001) lines are the demarcations for star-forming (SF, blue), composite (Comp, green) and AGNs and the dotted line (Cid10; R. Cid Fernandes et al. 2010) divides AGNs into Seyfert (red) and LINER (yellow). Overlaid square and triangle symbols represent the emission-line ratios of the primary and secondary components from the stacked spectra within Region A. (b) The spatially resolved [N II]-BPT map for the primary component with the same color code as panel (a). The black contours represent the EW[O III] with 20%, 30%, 50%, 70%, and 90% levels, and the photometric major (minor) axis is marked as a gray solid (dashed) line.
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: Distribution of g-band flux and [O III]λ5007 biconical ionized structure. The purple hexagon represents the MaNGA bundle. The 3.0 GHz VLASS radio continuum is overlaid as yellow contours, and its flux peak is marked as a yellow cross. The VLASS beam size displayed in the lower-left corner is 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩84 × 2﹩\mathop{.}\limits^{\unicode{x02033}}﹩28, and it has a position angle of 44∘ (east from north). The flux of the Hα broad component within Region A is shown as red contours, and the flux peak is marked as a red star. The overlaid color map shows EW[O III]. The white dashed line is the photometric minor axis, and the blue star marks the photometric center of this galaxy.
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: Decomposed gas kinematics. (a) Hα velocity field—the velocities within Region A are derived from the primary components, while velocities outside Region A are the centroid velocities of single Gaussian models. (b) Hα velocity field of the secondary components within Region A. (c), (d) The same configurations as panels (a), (b) but for [O III]λ5007.
Paper: A Dual Active Black Hole Candidate with Mass Ratio ~7:1 in a Disk Galaxy
Authors: Xiao Cao, Yan-Mei Chen, Yong Shi, Junfeng Wang, Zhijie Zhou, Min Bao, Qiusheng Gu, Alexei Moiseev, Luis C. Ho, Lan Wang, Guangquan Zeng
Figure caption: The effect of SNR on the detection of the broad Hα component. (a) ΔBIC23 as a function of SNR, where each black dot represents the measurement from one synthetic spectrum, and the red curve is the best-fitted power law of black dots. (b) SNR distributions for the observed emission-line spectra within Region A, including spectra modeled by double Gaussian components (the blue shaded area) and double narrow Gaussian plus a broad Hα component (the orange hatched area). The green dashed line marks SNR ~ 32.
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Optical luminosity vs. redshift for the host galaxy of FRB 20240209A (red star) and other FRB hosts in the literature (V. Ravi et al. 2019; A. C. Gordon et al. 2023; K. Lee-Waddell et al. 2023; M. Bhardwaj et al. 2024; L. Connor et al. 2024; A. L. Ibik et al. 2024a; C. J. Law et al. 2024; R. M. Shannon et al. 2024; K. Sharma et al. 2024); stars denote known repeaters while circles denote apparent nonrepeaters. The dashed line corresponds to the Gemini luminosity limit of r ≈ 25.9 mag (3σ), for which parameter space above the line is ruled out for a source coincident with the KKO localization. The range of luminosity limits on a coincident source, set by the upper limit on the redshift inferred from the DM (﹩{z}_{{\rm{\max }}}=0.19﹩), is highlighted in the blue shaded region, corresponding to ≲2.5 × 107 L⊙. This is well below the luminosity of the Small Magellanic Cloud (gray horizontal line) and below the limit of the inferred luminosity for the host of FRB 20190208A (D. M. Hewitt et al. 2024b; purple triangle). The lower bound reaches the luminosities of GCs in elliptical galaxies (yellow box; e.g., J. Strader et al. 2006). The luminosity of the GC hosting the repeating FRB 20200120E (L ≈ 1.3 × 105 L⊙) falls toward the upper side of the yellow box (F. Kirsten et al. 2022; M. Bhardwaj et al. 2021).
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Total daily exposure time (UTC and topocentric at CHIME near Penticton, Canada) at the position of FRB 20240209A (blue points) and detection times of the repeat bursts (gray vertical lines). The top panel shows the exposure times since CHIME/FRB began operations. The red line indicates a window around the time the repeater became active, and the bottom panel is zoomed in on that window. The source had a median total exposure of approximately 55 minutes per day, which includes upper and lower transits having median exposures of 13 minutes and 39 minutes, respectively. Days with lower exposure are due to system shutdowns. The exposure is slightly higher on certain days every year due to an additional fractional sidereal transit of the source on the same solar day.
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Projected physical offsets (left panel) and host-normalized offsets (right panel) of 43 FRBs that have robust host associations and offset information. Also shown are the projected physical and host-normalized offsets of GCs of the spiral galaxies Milky Way and M81, and of the elliptical galaxies NGC 821 and NGC 4278. The black dashed line shows the ∼20 kpc projected offset of FRB 20200120E, which is localized to a GC of M81. The black solid line shows the ∼40 kpc projected offset of FRB 20240209A with the gray shaded region showing the 3σ uncertainty on the offset based on the localization region. Based on its offset, FRB 20240209A is consistent with originating from a GC of its massive elliptical host galaxy.
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Gemini r-band image showing the host galaxy of FRB 20240209A (cyan crosshairs) and the 1σ (white solid) and 3σ (white dashed) localization ellipses. The source to the east of the localization ellipse is a star. The 3σ limiting magnitude is r ≳ 25.9 mag (corrected for Galactic extinction).
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: Dynamic spectra, frequency-integrated profiles, and time-integrated spectra of the 10 repeat bursts from FRB 20240209A that have baseband data saved at CHIME. The time resolution at which each burst is plotted along with the burst number (see Table 2) is indicated in the top-right corner, and the Transient Name Server (TNS) name of the burst is provided in the heading of each plot.
Paper: A Repeating Fast Radio Burst Source in the Outskirts of a Quiescent Galaxy
Authors: Vishwangi Shah, Kaitlyn Shin, Calvin Leung, Wen-fai Fong, Tarraneh Eftekhari, Mandana Amiri, Bridget C. Andersen, Shion Andrew, Mohit Bhardwaj, Charanjot Brar, Tomas Cassanelli, Shami Chatterjee, Alice Curtin, Matt Dobbs, Yuxin Dong, 雨欣 董, Fengqiu Adam Dong, Emmanuel Fonseca, B. M. Gaensler, Mark Halpern, Jason W. T. Hessels, Adaeze L. Ibik, Naman Jain, Ronniy C. Joseph, Jane Kaczmarek, Lordrick A. Kahinga, Victoria M. Kaspi, Bikash Kharel, Tom Landecker, Adam E. Lanman, Mattias Lazda, Robert Main, Lluis Mas-Ribas, Kiyoshi W. Masui, Ryan Mckinven, Juan Mena-Parra, Bradley W. Meyers, Daniele Michilli, Kenzie Nimmo, Ayush Pandhi, Swarali Shivraj Patil, Aaron B. Pearlman, Ziggy Pleunis, J. Xavier Prochaska, Masoud Rafiei-Ravandi, Mawson Sammons, Ketan R. Sand, Paul Scholz, Kendrick Smith, Ingrid Stairs
Figure caption: The purple shaded ellipses show the 1σ, 2σ, and 3σ CHIME-only baseband localization region for FRB 20240209A. The contour stripes show the CHIME–KKO VLBI localization regions for six repeat bursts, each constrained along the baseline vector. The black ellipses show the 1σ and 3σ combined VLBI localization region after accounting for correlated systematic errors.
Paper: Alpha–Proton Relative Drift: Implications for the Origins and Dynamics of the Solar Wind
Authors: Joseph H. Wang, Timothy S. Horbury, Lorenzo Matteini, Domenico Trotta
Figure caption: Magnetic field and particle time series data at PSP (left) and at Solar Orbiter (right) during a radial lineup in 2023 March. Row (a) shows magnetic field measurements (magnitude and radial component). Row (b) shows proton speed. Row (c) shows alpha drift and Alfvén speed, and row (d) shows ratio of alpha drift speed to Alfvén speed. Lines are bold during the times that fit the Alfvénic fast wind condition at PSP and are therefore included in the analysis.
Paper: Alpha–Proton Relative Drift: Implications for the Origins and Dynamics of the Solar Wind
Authors: Joseph H. Wang, Timothy S. Horbury, Lorenzo Matteini, Domenico Trotta
Figure caption: A log–log plot of radially binned means and standard deviations of the Alfvén speed and alpha drift speed in the Alfvénic fast wind. The dotted line shows a 1/R trend for the Alfvén speed, and the straight blue line marks 150 km s−1.
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: Example of fits (pink shaded regions) to the modeled NIRCam photometry (gray points with error bars) of a z = 7 simulated galaxy (full spectrum shown in gray) along a single line of sight (upper panels) and posterior SFHs (lower panels), given different assumed SFH parameterizations (see labels). The data are similarly well modeled by photometry generated using very different SFH parameterizations.
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: Left panels: offset between fitted stellar mass and true stellar mass versus offset between fitted and true Hα EW at z = 5 (upper left panel) and between fitted and true [O III] λ5007 EW at z = 8 (lower left panel). Here, we compare fits using the double power-law and bursty continuity SFH parameterizations. For both parameterizations, when stellar masses are overestimated, emission line EW is underestimated. However, offsets tend to be less severe for fits using the bursty continuity parameterization. Upper central and right-hand panels: an example of a z = 5 galaxy where the fits (purple and cyan) can diverge significantly from the underlying simulated SED (gray). Strong emission lines (Hα in F356W, F410M, and F444W and [O III] λ4959, 5007 in F277W) are not well fitted by BAGPIPES with the double power-law SFH parameterization; instead, the SED fit favors an older, more massive stellar population with stronger optical continuum and weaker emission lines. As a result, the inferred stellar mass (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=8.1{7}_{-0.12}^{+0.07}﹩) exceeds the true stellar mass (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.82﹩). This effect is less strong when the bursty continuity SFH is adopted; in this case, the stellar mass is approximately recovered: ﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.8\pm 0.3﹩. Lower central and right-hand panels: an example of a z = 8 galaxy where the fits (purple and cyan) diverge significantly from the underlying simulated SED (gray). The emission lines ([O III] λ4959, 5007 and Hβ in F444W and [O III] λ4363 in F356W, F410M, and F444W) are not well fitted by BAGPIPES, and the SED fit favors an older stellar population. Again, the inferred stellar mass (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.9\pm 0.2﹩ for both SFH parameterizations) exceeds the true stellar mass (﹩{\mathrm{log}}_{10}({M}_{\star }/{M}_{\odot })=7.42﹩).
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: SMFs at z = 10−5, constructed using intrinsic simulated stellar masses (black dashed lines), as well as using masses inferred from SED fitting, with different assumed SFHs (see colors shown in legend). The lower panels show ﹩{\mathrm{log}}_{10}{N}_{\mathrm{inferred}}-{\mathrm{log}}_{10}{N}_{\mathrm{true}}﹩. Uncertainties on the inferred functions are derived using Poisson errors. We do not include uncertainties on the simulated mass function as, although sometimes noisy, this is the “target” from the input data. The SED-inferred SMFs are a different shape than the true functions, with more low-mass galaxies at high redshift (z > 7) and fewer high-mass galaxies (M⋆ ≳ 109 M⊙, seen here at z ≤ 7, where galaxies of these masses assemble). This “tilting” effect arises due to biases in stellar mass inference: masses are typically underestimated for high-mass galaxies and overestimated for low-mass galaxies (which have high sSFRs to make it into the SPHINX20 sample). Note that we do not display the lowest-mass galaxies at each redshift, where number densities are heavily influenced by the SPHINX SFR selection. At these lowest stellar masses, the number of inferred galaxies is lower than the true number.
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: Offset between fitted stellar mass and true stellar mass ﹩({\rm{\Delta }}{M}_{\star }={\mathrm{log}}_{10}({M}_{\star ,\mathrm{fitted}}/{M}_{\odot })-{\mathrm{log}}_{10}({M}_{\star ,\mathrm{true}}/{M}_{\odot }))﹩ as a function of sSFR (upper left); “burstiness” parameter, SFR10 Myr/SFR100 Myr (upper right); Hα EW (lower left); and offset between fitted and true mass-weighted age (lower right). Each panel shows different redshifts (see colors); all are derived for fits using the bursty continuity SFH model. Stellar masses tend to be overestimated where the galaxy has a rising recent SFH (SFR10 Myr > SFR100 Myr). Galaxies with overestimated stellar masses also typically have overestimated mass-weighted stellar ages.
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: Fitted stellar mass (upper panels) and offset between fitted and true stellar mass (lower panels) versus true stellar mass for the different SFH models (labeled) and samples at different redshifts (see colored points). The shaded gray regions mark out a factor of 2 (0.3 dex) above and below the true stellar mass to guide the eye. The robustness of stellar mass recovery is a function of mass: stellar mass is overestimated at low stellar masses (M⋆ ≲ 108 M⊙) and underestimated at high stellar masses (M⋆ ≳ 109 M⊙).
Paper: High-z Stellar Masses Can Be Recovered Robustly with JWST Photometry
Authors: R. K. Cochrane, H. Katz, R. Begley, C. C. Hayward, P. N. Best
Figure caption: Stellar mass recovery for the whole sample of SPHINX galaxies with SFR > 0.3 M⊙ yr−1 at each redshift when fitted with the six SFH models. The majority of stellar masses are slightly overestimated, but masses are generally recovered to within ∼0.5 dex, regardless of SFH parameterization. Summary statistics are presented in Table 1.