adsabs/AstroCLIMB huggingface dataset:
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Best-fitting results for B/C and B/O ratios and C, O fluxes. In each panel, the dashed line is for the LIS spectrum, and the solid one is for the TOA spectrum with ϕ = 600 MV.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Best-fitting results for proton and helium fluxes. In each panel, the dashed line is for the LIS spectrum, and the solid one is for the TOA spectrum with ϕ = 600 MV.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Deuteron fluxes when adding a primary component (dotted line) with D/H = 1.6 × 10−3 to the secondary contribution (long dashed line) calculated for nuclei with Z ≤ 8.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Model-predicted flux ratios of D/4He (left) and 3He/4He (right) compared with the AMS-02 measurements (M. Aguilar et al. 2024). In the left panel, we also show the result when adjusting slightly the production cross section of D for Z ≥ 6 nuclei (dashed line).
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Deuteron (left) and helium-3 (right) fluxes for fragmentation of nuclei up to oxygen compared with the measurements (O. Adriani et al. 2016; M. Aguilar et al. 2024).
Paper: On the Origin of a Broad Quasiperiodic Fast-propagating Wave Train: Unwinding Jet as the Driver
Authors: Xinping Zhou, Zehao Tang, Zhining Qu, Ke Yu, Chengrui Zhou, Yuqi Xiang, Ahmed Ahmed Ibrahim, Yuandeng Shen
Figure caption: Panels (a1)–(a3) are the time–distance stack plots obtained from the AIA 171 and 193 Å running-difference images along the slices Sa and Sb shown in Figure 3(d). The white arrows in panel (a2) point to the positions where the intensity profile is used to analyze the periodicity of the wave trains. Panel (b1) displays the GOES 1–8 Å X-ray flux and normalized AIA 94, 131 and 335 Å light flux curves within the eruption source region marked with the black box in Figure 1(i). Panel (b2) is the derivative curve of the GOES 1–8 Å flux. Panels (c1) and (c2), respectively, show the wavelet spectrum of the flare and broad QFP wave train, and their corresponding periods are listed in the figures. The main periods and their errors are determined by the peak and FWHM of the corresponding global wavelet power spectra. The dark blue curves in the wavelet spectrum outline the 95% significance level, while the crosshatched areas in the wavelet spectrum indicate the cone of influence region due to the edge effect of the data. Panels (d1)–(d3) are three snapshots to show the evolution of the narrow QFP wave train, where the red arrow in each panel is located at a specific position.
Paper: On the Origin of a Broad Quasiperiodic Fast-propagating Wave Train: Unwinding Jet as the Driver
Authors: Xinping Zhou, Zehao Tang, Zhining Qu, Ke Yu, Chengrui Zhou, Yuqi Xiang, Ahmed Ahmed Ibrahim, Yuandeng Shen
Figure caption: Panel (a1) shows the coordinate system ﹩x^{\prime} \unicode{8210}y^{\prime} ﹩ relative to the arcsec coordinate system x–y. The colored “+” symbols in the inset of panel (a1) represent the variations of the location coordinates of the MBFs relative to the ﹩x^{\prime} \unicode{8210}y^{\prime} ﹩ coordinate system. Panels (a2) and (a3) show the evolution of MBFs in the ﹩x^{\prime} ﹩- and ﹩y^{\prime} ﹩-directions, respectively. The fitted parameters are listed on the corresponding panels. Panels (b1)–(d) are the time–distance stack plots reconstructed along the slices S1–S5 in Figure 1, using the AIA 131 (b1)–(b4) and 304 Å (c1)–(d) raw images. The ridges’ slope represents the moving material’s speeds, and their speeds obtained by linear fitting are listed in each panel. Errors in parameters such as speed and period, etc., are estimated by making the fit 10 times.
Paper: Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae
Authors: Ore Gottlieb, Brian D. Metzger
Figure caption: Required engine peak luminosity, L eng, and duration at this luminosity, t eng (e.g., magnetar spin-down luminosity and timescale, respectively), to explain the observed peak luminosities, L pk, and rise times, t pk, of a large sample of Type I SLSN light curves (S. Gomez et al. 2024), for two different assumptions about the ejecta mass, M ej = 10 M ⊙ (black stars) and 3 M ⊙ (blue squares), bracketing the typical range inferred for Type I SLSNe (M. Nicholl et al. 2017). For comparison, we show the approximate range of timescales and luminosities of the early premaximum bumps observed in the light curves of Type I SLSNe (shaded blue ellipse; see, e.g., M. Nicholl & S. J. Smartt 2016). A multiday-lasting jet from the same central engine responsible for powering the bulk of the SLSNe is thus capable of powering the early bumps, assuming that the jet luminosity, L  j , is a fraction ∼1%–10% of L eng. The assumed jet properties for the numerical simulation presented in this Letter are illustrated with an orange square, while bidirectional arrows indicate the degeneracy in engine properties ﹩{L}_{\mathrm{eng}}\propto {t}_{\mathrm{eng}}^{-1}﹩ that result in the same hydrodynamic evolution for fixed ejecta properties. Details: for each event, we estimate the ejecta kinetic energy, ﹩{E}_{\mathrm{KE}}={M}_{\mathrm{ej}}\,{v}_{\mathrm{ej}}^{2}/2﹩, by equating the observed SN rise timescale to the diffusion timescale for a centrally concentrated energy source, ﹩{t}_{\mathrm{diff}}\simeq 0.4{(\kappa {M}_{\mathrm{ej}}/\,{v}_{\mathrm{ej}}c)}^{1/2}﹩ (D. K. Khatami & D. N. Kasen 2019). Assuming that the explosion energy E KE comes exclusively from the engine, i.e., E eng = L eng t eng = E KE, we estimate the required engine timescale assuming that the engine luminosity decays similarly to magnetic dipole spin-down ﹩{L}_{\mathrm{pk}}={({E}_{\mathrm{eng}}/{t}_{\mathrm{eng}})(1+{t}_{\mathrm{pk}}/{t}_{\mathrm{eng}})}^{-2}﹩, for t eng < t pk. If the engine contributes only a fraction of the explosion energy E KE, then a greater engine duration is needed to explain the observed luminosities, and points will shift toward the lower right part of the diagram as indicated by the arrow.
Paper: Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae
Authors: Ore Gottlieb, Brian D. Metzger
Figure caption: 2D ﹩\hat{x}-\hat{z}﹩ plane cuts at various times of the azimuthally averaged logarithmic comoving thermal energy density, e = 3p maps. The white and black contours represent the photosphere and trapping radius, respectively.
Paper: Late Jets, Early Sparks: Illuminating the Premaximum Bumps in Superluminous Supernovae
Authors: Ore Gottlieb, Brian D. Metzger
Figure caption: 3D rendering of the logarithmic comoving mass density at the end of the jet activity, t = t eng, when the ejecta front is at r ej ≈ 8.5 × 1014 km. As the jet escapes from the high-density expanding spherical ejecta (yellow), it generates a stratified structure of the lower-density cocoon (red). The interaction of the jet and the cocoon with the expanding ejecta close to the breakout radius generates bright NUV/optical emission over a ∼week timescale.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Posterior distributions for important atmospheric volatile species (top; blue) and the stellar heterogeneity component (bottom; orange) for the POSEIDON retrieval (top rows) using a CLR agnostic prior on the background gas and for the SCARLET retrieval (bottom rows) where H2/He is the filler (background) gas. Different colors correspond to different retrievals where spots or faculae are included or excluded (see legend). Our constraints on the HMMW atmospheric volatile species are broadly unaffected by our treatment of stellar contamination, and the retrieval only provides a lower limit on the H2O abundance. For the SCARLET retrieval, the distributions on T spot and T fac are derived from the posterior distributions on ΔT spot, ΔT fac, and T phot,star. The POSEIDON prior on the spot temperature extends all the way to 2300 K, while SCARLET assumes that spots are at most 800 K colder than the photosphere.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Top panels: white light curves showing the full baseline and the transit model. The 1σ flux range during times of quiescence is highlighted. We opt to use the transit depth from visit 1 during visit 2 due to degeneracy between the depth and the flare decay tail of F3. Bottom left panels: from top to bottom, white light transit light curve, TESS-band time series, and T eff time series for the flare-only continuum spectra are shown for visit 1 (left) and visit 2 (right). Times during flares are highlighted, where flares are defined as events where the TESS-band flux increases with two or more points exceeding the local noise by 3σ in the binned light curve. The 16.5 s cadence data are shown in gray, while binned time series are shown in blue and black for the TESS and T eff time series, respectively. A fitted linear trend in the out-of-transit light curve has been removed from the white light curve to better show flare events. The transit model shown in the top panel has been subtracted from the TESS time series. Gaps in the T eff time series are due to low S/N or nondetections outside of the flare peak. .
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Result from the stctm fit (spots only) to the NIRISS/SOSS + HST/WFC3 spectrum of GJ 9827 d. The combined JWST+HST spectrum is binned to R = 50 for visual purposes (black points). The 1σ, 2σ, and 3σ constraints on the retrieved stellar-contamination-only spectra are shown (semitransparent regions) as well as the median (coral line) and best-fit spectrum (black line). Stellar contamination without a planetary atmosphere signal cannot reproduce the water features observed in the transmission spectrum of GJ 9827 d (see Figure 3 for an atmosphere+stellar contamination fit).
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Transmission spectra of K2-18 b (N. Madhusudhan et al. 2023), TOI-270 d (B. Benneke et al. 2024a), and GJ 9827 d in units of scale heights for a H2/He-dominated atmosphere, offset. For clarity, the spectra of TOI-270 d and GJ 9827 d are binned to a resolving power of 50 (gray points). The best-fit models from the retrievals run on the spectra of GJ 9827 d and TOI-270 d are shown on top of the observations (colored lines), and for K2-18 b, we show a representative SCARLET model for the retrieved abundances quoted in N. Madhusudhan et al. (2023). The background color and line colors encode the variation in equilibrium temperature between the three sub-Neptunes, but they also have different sizes and densities (see annotated temperatures for a Bond albedo of 0.3, masses, and radii).
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Comparison of the spectrum of GJ 9827 d over both JWST/NIRISS/SOSS transit epochs and with the HST/WFC3 observations. Top panel: transmission of GJ 9827 d as observed during the first (blue) and second (orange) visit, with the spectrum of visit 1 shifted down by about 40 ppm to match the median value of the visit 2 spectrum. The combined spectrum from both visits is shown in black. Bottom panel: combined JWST/NIRISS/SOSS transmission spectrum (gray) along with binned version (black) and the spectrum as observed from 10 HST/WFC3 transits (P.-A. Roy et al. 2023), shifted up by 10 ppm.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Comparison of the fitted transit time variations for visits 1 and 2 with NIRISS/SOSS (black points) to the previous measurements from Kepler (blue), HST (purple), and Spitzer (pink). We show the TTVs as a function of epoch after fitting a new ephemeris to all the transit times combined. The inset zooms in on the two NIRISS/SOSS transits presented in this work. The JWST transits nearly double the baseline, occurring over 1000 days after the last HST transit, improving the precision of the orbital period measurement by a factor of 5.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Time-averaged spectra of all integrations during the flare peak times of the F1–F4 candidates. Each spectrum is obtained by subtracting the out-of-flare stellar spectrum to create a flare-only spectrum. The flare-only spectrum is binned in wavelength and fit with a single-temperature blackbody model to obtain the hottest T eff reached during each event.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Comparison between the spectra that were extracted at high (1 pixel in blue and 2 pixels in orange) resolution and the R = 100 (black) spectrum for visit 1 (top panel) and visit 2 (bottom panel) using the supreme-SPOON version of the data reduction. The three versions of the transmission spectrum for each visit are consistent to well within their quoted uncertainties in each spectral bin.
Paper: JWST/NIRISS Reveals the Water-rich “Steam World” Atmosphere of GJ 9827 d
Authors: Caroline Piaulet-Ghorayeb, Björn Benneke, Michael Radica, Eshan Raul, Louis-Philippe Coulombe, Eva-Maria Ahrer, Daria Kubyshkina, Ward S. Howard, Joshua Krissansen-Totton, Ryan J. MacDonald, Pierre-Alexis Roy, Amy Louca, Duncan Christie, Marylou Fournier-Tondreau, Romain Allart, Yamila Miguel, Hilke E. Schlichting, Luis Welbanks, Charles Cadieux, Caroline Dorn, Thomas M. Evans-Soma, Jonathan J. Fortney, Raymond Pierrehumbert, David Lafrenière, Lorena Acuña, Thaddeus Komacek, Hamish Innes, Thomas G. Beatty, Ryan Cloutier, René Doyon, Anna Gagnebin, Cyril Gapp, Heather A. Knutson
Figure caption: Comparison between the spectra obtained from the supreme-SPOON (blue) and NAMELESS (orange) data reductions. The top panel shows the R = 100 spectrum for visit 1, and the bottom panel shows the same thing for visit 2. The spectra agree to better than 1σ in almost all spectral bins.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Expected fluxes of D (left) and 3He (right) from the fragmentation of all nuclei compared with the measurements by PAMELA (O. Adriani et al. 2016) and AMS-02 (M. Aguilar et al. 2024). The dashed line is the LIS spectrum, the solid line corresponds to the modulated spectrum on top of the atmosphere (TOA) for ϕ = 600 MV, and the shaded bands show the uncertainty ranges of the model predictions. The bottom subpanels show the data-to-model ratios together with the uncertainty bands of the predictions.
Paper: The AMS-02 Cosmic-Ray Deuteron Flux is Consistent with a Secondary Origin
Authors: Qiang Yuan, Yi-Zhong Fan
Figure caption: Deuteron fluxes when adjusting slightly (see Figure A4 in Appendix C) the production cross section of deuterons from B. Coste et al. (2012).
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: Top: predictions for the number of detectable progenitors in the virial volume of the MW at different z, as a function of the magnification factor. From the 50 merger histories provided by the NEFERTITI model, we calculate the mean number of detections (solid lines) and the standard deviation (shaded areas). Bottom: comparison between the number of systems detected in the Firefly Sparkle (dark green) and the number of progenitors predicted to be detectable in the same conditions (i.e., z, volume, lensing). The white area highlights the lensing range of the central region of the Firefly Sparkle.
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: SFR (top panel) and Z gas (bottom panel) as a function of M ⋆ for all the MW progenitors predicted by the NEFERTITI model at z = 8.3. Assuming the detection limits of CANUCS (C. J. Willott et al. 2022), the gray points represent the nondetectable systems, while the colored ones are detectable with different magnification factors (i.e., orange for μ = 30, yellow for μ = 24, light green for μ = 18, and dark green for μ = 12). The best-fitting progenitors to the Firefly Sparkle are highlighted with star markers. On top and the sides, we show the probability distribution functions (PDF) of the properties of all the progenitors and of the detectable ones, again color-coded for μ.
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: Left: average synthetic SEDs for the MW major branch simulated by the NEFERTITI model, color-coded for redshift. For each mean SED, we show the corresponding photometries in the JWST NIRCam filters. The shaded area represents the standard deviation due to the different merger tree realizations. Right: average star formation (top panel) and metal-enrichment histories (bottom panel) of the MW major branch, with the same color coding. On the bottom-right, we report the mean M ⋆ at the redshifts shown on the left.
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: Star formation (gold) and metal-enrichment (blue) histories of the progenitors that best fit the emission of each system of the Firefly Sparkle, in order of increasing estimated M ⋆. The synthetic SED is shown in the top-right inset (red), together with the L. Mowla et al. (2024) observations (black). The gray areas are not included in the fit. The histories of the minor branches (dotted lines) that have merged with the most massive progenitor (solid lines) to form the final one at z = 8.3 are also shown.
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: SFR (top panel) and Z gas (bottom panel) as a function of M ⋆ for all the MW progenitors predicted by the NEFERTITI model at z = 8.3, colored by density of points. The best-fitting progenitors to the Firefly Sparkle are highlighted with star markers. On top and the sides, we show the probability distribution functions (PDF) of the properties of all the progenitors (beige) and the detectable ones (red), assuming μ = 24 and the detection limits of CANUCS (C. J. Willott et al. 2022).
Paper: Linking High-z and Low-z: Are We Observing the Progenitors of the Milky Way with JWST?
Authors: Elka Rusta, Stefania Salvadori, Viola Gelli, Ioanna Koutsouridou, Alessandro Marconi
Figure caption: Physical properties of all the MW major branches simulated by NEFERTITI: halo mass (top left), stellar mass (bottom left), star formation rate (top right), and gas metallicity (bottom right), colored by halo mass at z = 6. The black error bars represent the mean value and the relative standard deviation at z = 14, 12, 10, 9, 8, 7, and 6.