adsabs/AstroCLIMB huggingface dataset:
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Cooling function in warm and hot gas with n = 1 cm−3 under ionization equilibrium for metal and dust scaled abundance ﹩{Z}^{{\prime} }=1﹩ (top) and ﹩{Z}^{{\prime} }=0.01﹩ (bottom). We consider two different physical conditions for warm gas: cooling functions for nonphotoionized gas (ξ cr = 2 × 10−16, χ FUV = 1, and ζ pi = 0) are shown as solid lines, while those for photoionized gas (ξ cr = 2 × 10−16, χ FUV = 102, and ζ pi = 10−8 s−1) are shown as dashed lines. In both cases, we adopt the CIE cooling function of Gnat & Ferland (2012) for helium and metals at T > 3.5 × 104 K (see Equation (48)). The black lines show the total cooling. The cooling function contributions for hydrogen (Lyα, radiative recombination, and free–free) and other important coolants are shown separately as colored lines. The gray shaded area indicates the temperature range 2 × 104 K < T < 3.5 × 104 K, in which we make a smooth transition from self-consistent, chemistry-based cooling to the CIE cooling. The dotted lines show the total (H + He + metals) CIE cooling function of Gnat & Ferland (2012) assuming the Asplund et al. (2009) element abundance ratios. The inset in the bottom panel shows the equilibrium electron fraction (black) and neutral hydrogen fraction (red) for Z = 1.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: (Left) Cooling function in photoionized gas with n = n e = 1 cm−3 for the solar neighborhood gas metallicity and dust abundance ﹩{Z}_{{\rm{g}}}^{{\prime} }={Z}_{{\rm{d}}}^{{\prime} }=1﹩. The thick solid black line shows the total cooling function, which is the sum of cooling by collisionally excited lines of ionized metals (C, N, O, Ne, S), free–free emission (blue dashed), and hydrogen radiative recombination (blue dotted line). We assume that 80% (20%) of O, N, and Ne is singly (doubly) ionized and 50% (50%) of S is singly (doubly) ionized. Thin black solid lines show notable nebular cooling lines from metal ions that contribute to Λneb. (Right) The thick solid lines show the total cooling function at different gas densities (n = n e = 1, 102, ⋯ , 106 cm−3) for ﹩{Z}_{g}^{{\rm{{\prime} }}}=1﹩ and 0.1. Also shown in both panels are the PI heating function ﹩{{\rm{\Gamma }}}_{\mathrm{pi}}/{n}_{{\rm{e}}}=3.5\,\mathrm{eV}\times {\alpha }_{\mathrm{rr},{{\rm{H}}}^{+}}﹩ (assuming PI-recombination equilibrium; black dotted) and the total effective heating function, which is the sum of PI and grain PE heating, minus the cooling by grain-assisted recombination of H+, assuming normalized FUV radiation intensity of χ FUV = 102 (black dashed line). The equilibrium temperature of photoionized gas is where the total cooling and the total effective heating functions meet. The red dashed lines show our adopted approximation for the total cooling, using Λneb (Equation (47)), Λrr, Λff, and ﹩{{\rm{\Lambda }}}_{{{\rm{C}}}^{+}}﹩.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Equilibrium thermal pressure (top) and temperature (bottom) of unshielded gas as a function of hydrogen number density n. The gas is exposed to FUV radiation that scales with the local ISRF (χ 0, in units of the Draine 1978 value), with the primary CR ionization rate also scaled as ξ cr,0 = 2 × 10−16 s−1  χ 0. The left column shows the case of the standard total elemental abundance (﹩{Z}^{{\prime} }=1﹩) with varying χ 0 and ξ cr. The right column shows the effects varying ﹩{Z}^{{\prime} }﹩ for χ 0 = 1 and ξ cr,0 = 2.0 × 10−16 s−1. Additionally, the dashed lines in the right column show the case with ﹩{Z}_{g}^{{\rm{{\prime} }}}=0.1﹩ and ﹩{Z}_{d}^{{\rm{{\prime} }}}=0.025﹩.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Various quantities of gas in thermal/chemical equilibrium exposed to FUV radiation with χ 0 = 1 and CR ionization rate ξ cr = 2 × 10−16 s−1, considering a range of metal and dust abundance (see also the right column of Figure 5). From left to right, the first three columns show cases with ﹩{Z}_{g}^{{\rm{{\prime} }}}={Z}_{d}^{{\rm{{\prime} }}}=1﹩, 0.1, and 0.01. The fourth column shows the case with ﹩{Z}_{g}^{{\rm{{\prime} }}}=0.1﹩, ﹩{Z}_{d}^{{\rm{{\prime} }}}=0.025﹩. The top row shows the cooling (solid line) and heating (dashed line) rates per H nucleon. The total is shown in black, and contributions from individual heating and cooling terms are also shown separately. The middle row shows abundances x  s  of species that we track, relative to H. The bottom row shows temperature (solid line, left axis), grain charging parameter (dashed line, left axis), and characteristic cooling time (dashed–dotted line, right axis).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: (Left) The minimum/maximum equilibrium thermal pressure ﹩{P}^{(\min /\max )}﹩ for CNM/WNM (solid/dashed lines) as functions of the scaled FUV intensity χ 0. The CR ionization rate is set to ξ cr = 2 × 10−16 χ 0 s−1. For ﹩{P}^{(\min )}\lt P\lt {P}^{(\max )}﹩, two stable equilibrium solutions are possible so that CNM and WNM can coexist in pressure equilibrium. The color of the lines indicates the metallicity ﹩{Z}^{{\rm{{\prime} }}}={Z}_{g}^{{\rm{{\prime} }}}={Z}_{d}^{{\rm{{\prime} }}}﹩. (Middle and right) The corresponding temperature and density at ﹩{P}^{(\min )}﹩ and ﹩{P}^{(\max )}﹩. Note that ﹩T\gt {T}^{(\max )}﹩ (﹩T\lt {T}^{(\min )}﹩) on the warm (cold) branch at ﹩n\lt {n}^{(\max )}﹩ (﹩n\gt {n}^{(\min )}﹩).
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Electron-impact excitation rate for Lyα transition (1 → 2) of atomic hydrogen as a function of temperature. The black circles indicate the quantum mechanical calculations from Przybilla & Butler (2004), and the blue line is our fit to the data (see Equation (42)). The inset shows the fractional error of the fit.
Paper: Photochemistry and Heating/Cooling of the Multiphase Interstellar Medium with UV Radiative Transfer for Magnetohydrodynamic Simulations
Authors: Jeong-Gyu Kim, Munan Gong, Chang-Goo Kim, Eve C. Ostriker
Figure caption: Characteristic cooling time t cool ≡ P/(n 2Λ) multiplied by the hydrogen number density n as a function of temperature for different values of ﹩{Z}^{{\prime} }﹩. The dashed and solid lines show the cases with and without ionizing radiation, respectively (see Figure 3). As in Figure 3, the gray shaded area shows the temperature range in which we make transition to the CIE cooling.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: The linear fitting results of reddening coefficients in 21 colors. The white circles denote the median values by binning the selected target samples into 10 groups with a bin size of 0.05 in the x-axis, and the statistical errors are too small to be shown. The black lines represent weighted linear regression of the white circles. Note that we plot as equal number of stars as possible in each temperature and E(B − V) interval to clearly show that R is T eff dependent.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Reddening coefficients as a function of T eff and E(B − V) of 21 colors. The color-coded points are the median values of the gridded target sample, with colors denoting T eff bins. The error bars are overplotted. The corresponding colored curves represent the fitting results. The black dashed lines show the single-valued reddening coefficients R.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Comparison with the results in the literature. The black dots with error bars show the literature values and errors. The gray bars represent the corresponding 3σ range. The colored dots represent the calculated values of the function at different T eff.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: The comparison of the predicted (a) and corrected empirical functions (b) of reddening coefficients R(T eff, E(B − V)) for 17 colors. The symbols and lines are similar to those in Figure 5.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Mean and standard deviation of the differences between the two independent measurements of intrinsic colors (color0–color0sp ). Note the values for the (FUV − NUV) color, −0.052 and 0.306 respectively, are too large to be shown.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Examples of T eff vs. ﹩\mathrm{log}\,{\text{}}g﹩ (left panels) and T eff versus [Fe/H] (right panels) distributions of the target and control samples. From top to bottom: FUV–NUV, g PS − r PS, H − Ks, and BP − G colors, respectively. In each panel, the blue dots are the control sample stars, and the density contour represents the target sample of the given color.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Distributions of different intrinsic colors derived by the star-pair method in the stellar parameter space. The color-coded dots represent the target samples in the LAMOST DR7 catalog. The color bars represent the stellar colors of the filter combination labeled on the plots. Note that only a randomly selected 10% of the target sample is drawn.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: Same as Figure 5 but for the fitting residuals.
Paper: Empirical Temperature- and Extinction-dependent Extinction Coefficients for the GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE Passbands
Authors: Ruoyi Zhang, Haibo Yuan
Figure caption: The star numbers of control and target samples of different colors for the LAMOST DR7 (left panel) and HotPayne (right panel) catalogs. The relative fractions, with a typical value of 1%, and total numbers of the target samples are marked.
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: Effective resolution for signal-to-noise ratio >3 measurements of dust polarized intensity with Planck at 353 GHz (left) and FYST with Prime-Cam at 350 GHz (right), for the 4000 hr Wide Field Survey at different levels of spatial resolution. Translucent contours indicate the boundaries of the FYST observable region. Planck measured 3σ detections of the polarized intensity at ﹩5^{\prime} ﹩ resolution only in the inner Galactic plane. Prime-Cam will make comparable measurements over much more of the sky, and along bright sightlines will make high-fidelity measurements at higher angular resolution, as demonstrated here by the additional contour at ﹩1^{\prime} ﹩.
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: Lines accessible to EoR-Spec at different redshifts (gray shaded regions). Dashed green lines correspond to transitions of the CO rotational ladder, where lighter shading is used for lines that will likely be faint. All these CO lines are the foreground (Section 4.5) to the [C II] and [O III] lines (solid and dashed–dotted red lines; Section 4.1) targeted by the main experiment, but they will also provide line-intensity maps at intermediate redshifts (Section 4.2). Fainter fine-structure lines due to [C I], [O I], and [N II] are indicated as dotted blue lines.
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: Overview of Prime-Cam survey fields in equatorial coordinates overlaid on the Planck dust polarization map (Planck Collaboration Int. XI 2013). The planned wide-field survey field for the CMB foregrounds, galaxy-cluster evolution, and Rayleigh-scattering science cases is approximated by the white transparent band (overlapping with Advanced ACTPol and SO fields; De Bernardis et al. 2016; Stevens et al. 2018). The deep intensity mapping–reionization surveys, the galaxy evolution survey fields, the galactic polarization science targets, and the specific time-domain science fields are outlined in black, magenta, green, and blue frames respectively. See Tables 2, 3, and 6 for survey coordinates, areas, and planned integration times.
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: (Left) Scatter plot of the distributions of the best-fitting values of r, showing that the SO-SAT only results have a systematic bias at the level of δ r = 1.1 × 10−3 (green line) compared to the SO-SAT + FYST results. The orange line shows the case with no bias. (Right) Histograms of r constraints from 1500 realizations of the simulation with SO-SAT only (blue) and SO-SAT + FYST with Prime-Cam (orange), showing a significant reduction of the bias on r when combining the two data sets. Note that the simulation does not have the primordial B-mode signal, i.e., r input = 0 (vertical line).
Paper: CCAT-prime Collaboration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope
Authors: CCAT-Prime Collaboration, Manuel Aravena, Jason E. Austermann, Kaustuv Basu, Nicholas Battaglia, Benjamin Beringue, Frank Bertoldi, Frank Bigiel, J. Richard Bond, Patrick C. Breysse, Colton Broughton, Ricardo Bustos, Scott C. Chapman, Maude Charmetant, Steve K. Choi, Dongwoo T. Chung, Susan E. Clark, Nicholas F. Cothard, Abigail T. Crites, Ankur Dev, Kaela Douglas, Cody J. Duell, Rolando Dünner, Haruki Ebina, Jens Erler, Michel Fich, Laura M. Fissel, Simon Foreman, R. G. Freundt, Patricio A. Gallardo, Jiansong Gao, Pablo García, Riccardo Giovanelli, Joseph E. Golec, Christopher E. Groppi, Martha P. Haynes, Douglas Henke, Brandon Hensley, Terry Herter, Ronan Higgins, Renée Hložek, Anthony Huber, Zachary Huber, Johannes Hubmayr, Rebecca Jackson, Douglas Johnstone, Christos Karoumpis, Laura C. Keating, Eiichiro Komatsu, Yaqiong Li, Benjamin Magnelli, Brenda C. Matthews, Philip D. Mauskopf, Jeffrey J. McMahon, P. Daniel Meerburg, Joel Meyers, Vyoma Muralidhara, Norman W. Murray, Michael D. Niemack, Thomas Nikola, Yoko Okada, Roberto Puddu, Dominik A. Riechers, Erik Rosolowsky, Kayla Rossi, Kaja Rotermund, Anirban Roy, Sarah I. Sadavoy, Reinhold Schaaf, Peter Schilke, Douglas Scott, Robert Simon, Adrian K. Sinclair, Gregory R. Sivakoff, Gordon J. Stacey, Amelia M. Stutz, Juergen Stutzki, Mehrnoosh Tahani, Karun Thanjavur, Ralf A. Timmermann, Joel N. Ullom, Alexander van Engelen, Eve M. Vavagiakis, Michael R. Vissers, Jordan D. Wheeler, Simon D. M. White, Yijie Zhu, Bugao Zou
Figure caption: Distributions of the best-fitting values of the dust parameters, β d and T d, from 1500 realizations of the simulation with SO-SAT only (blue) and SO-SAT + FYST with Prime-Cam (orange). Shaded contours show the approximate 1σ and 2σ intervals, while the dots represent the simulation results outside of the 95% confidence range. This shows a significant reduction of the degeneracy when combining the two data sets.