adsabs/AstroCLIMB huggingface dataset:
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: Individual relative transit depths compared to the relative final transmission spectrum. For each of the 10 transmission spectra, we obtain the relative transit spectrum by subtracting the average across wavelengths. We then subtract the relative final transmission spectrum from the individual relative spectra and display these transit depths for all visits in each channel. The relative transit depths are consistent across the 10 visits with the final relative spectrum. Points that are significantly away from zero (dotted lines) have larger error bars, which makes them less important in the weighted average, and thus do not bias our transmission spectrum. The uncertainty on the combined spectrum is also displayed as the gray region. In the top left panel, the broadband transit depths are shown, centered on the average across the 10 visits, highlighting the variability in the observed broadband transit depths from the different visits.
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: All 10 HST/WFC3 broadband light-curve fits of the transits of GJ 9827 d. Left: systematics-corrected and normalized broadband light curves for the 10 transits of GJ 9827 d (data points). Each visit is centered around the fitted transit time for that visit. The best-fitting transit model is also shown as the gray line. Right: residuals of the broadband light-curve fits shown on the left.
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: Observed mid-transit time (black points) for each of the 10 transits compared to a fitted linear ephemeris to all transit timings presented (except the two timings with large uncertainties; T0,BJD  = 2459185.987 ± 0.002, P = 6.20186 ± 0.00002 d). The ephemeris derived from the K2 campaign is shown (blue; Niraula et al. 2017) along with the Spitzer transit for this planet (red; Kosiarek et al. 2021). Our 10 HST/WFC3 transits suggest that there are statistically significant TTVs in the orbit of GJ 9827 d of the order of 5–10 minutes.
Paper: Water Absorption in the Transmission Spectrum of the Water World Candidate GJ 9827 d
Authors: Pierre-Alexis Roy, Björn Benneke, Caroline Piaulet, Michael A. Gully-Santiago, Ian J. M. Crossfield, Caroline V. Morley, Laura Kreidberg, Thomas Mikal-Evans, Jonathan Brande, Simon Delisle, Thomas P. Greene, Kevin K. Hardegree-Ullman, Travis Barman, Jessie L. Christiansen, Diana Dragomir, Jonathan J. Fortney, Andrew W. Howard, Molly R. Kosiarek, Joshua D. Lothringer
Figure caption: Posterior probability distributions of the free parameters used in the SCARLET free chemistry retrieval. The diagonal panels show the marginalized probability distributions of all individual parameters, whereas the off-diagonal panels show the marginalized probability distributions for each pair of parameters as colored shading. The 1σ, 2σ, and 3σ contours are shown in the 2D posteriors. Water is the only molecule detected in our retrieval analysis.
Paper: On the Sizes of Ionized Bubbles Around Galaxies During the Reionization Epoch. The Spectral Shapes of the Lyα Emission from Galaxies
Authors: Matthew J. Hayes, Claudia Scarlata
Figure caption: Left: model Lyα profiles. The far left spectrum shows the stacked profiles, where each spectrum is simply renormalized in luminosity at Δv > 0 before stacking. As an illustration, each colored line shows the stack of a subsample where all galaxies exceed the labeled O32 ratio: greater than 5 in pink to greater than 20 in black. The central spectrum shows the same as the left, but the spectra are also rescaled to the same FWHM of the red peak prior to stacking. The reference FWHM is set to 1000 km s−1 (note the different abscissa range of the two plots). Solid lines are mean stacks and dotted lines are median. The far right panel shows an example profile for GNz11 before and after IGM attenuation. We show the emergent Lyα profile as the gray line and the shape of the best-recovered Gunn–Peterson absorption in orange. The observed Lyα profile is the product of the two and is shown in black. Various characteristic velocities are labeled.
Paper: On the Sizes of Ionized Bubbles Around Galaxies During the Reionization Epoch. The Spectral Shapes of the Lyα Emission from Galaxies
Authors: Matthew J. Hayes, Claudia Scarlata
Figure caption: The Lyα observables of our sample. Δv red(Lyα) is plotted on the ordinate axis, with EW on the abscissa. Galaxy redshift is color-coded, with the color bar to the right. The shaded region shows the parameter space that can be matched using the emergent line profile of a low-z galaxy (Hayes et al. 2023) when broadened synthetically to FWHM = 500 km s−1. We assume the IGM density at z = 7, vary the velocity from 0 to 3000 km s−1, and the EW between 0 and the very high value of 800 Å.
Paper: On the Sizes of Ionized Bubbles Around Galaxies During the Reionization Epoch. The Spectral Shapes of the Lyα Emission from Galaxies
Authors: Matthew J. Hayes, Claudia Scarlata
Figure caption: Binned probability distribution functions from traces of the Monte Carlo sampler. The left shows the emergent Lyα EW, and the center shows the FWHM of the Lyα red peak. The right shows the bubble size in proper Mpc. Each posterior is color-coded by redshift, as labeled in the left plot. Hard lines show the means of the posterior distributions in each redshift bin, while faint lines show those for individual galaxies. The number of galaxies per bin is shown in the legend of the central plot.
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: (a) Multicolor light curve of SN 2023ixf (circles) with respect to time since first light (MJD 60082.833 ± 0.020) from PS1, LCO, Auburn, Thai Robotic Telescope, Nickel, and Lulin telescopes. Observed photometry is presented in the AB magnitude system and has been corrected for host galaxy and MW extinction. Light curves of CMFGEN models r1w6a (R CSM = 6 × 1014 cm, ﹩\dot{M}={10}^{-2}\,{M}_{\odot }﹩ yr−1), r1w6b (R CSM = 8 × 1014 cm, ﹩\dot{M}={10}^{-2}\,{M}_{\odot }﹩ yr−1), and r1w6c (R CSM = 1 × 1015 cm, ﹩\dot{M}={10}^{-2}\,{M}_{\odot }﹩ yr−1) are plotted as solid, dashed, and dotted lines, respectively. (b) Zoom-in of the SN 2023ixf r- and/or R-band light curve and CMFGEN models, which can reproduce the peak magnitude but are inconsistent with the early time slope. (c) CSM densities and radii for a subset of the CMFGEN model grid (e.g., Table (A2)) used to find the best fitting model for SN 2023ixf, which is plotted as a solid red line (r1w6b). Dotted black lines represent lower limits on the location of the SN shock at δ t = 6.4, 8.4, 10.6 days, for a lower limit on the SN shock velocity of ≳8500 km s−1 (Section 3.2). We expect a decrease of the optical depth to electron-scattering (i.e., τ ES) based on the plotted density profile at around ∼8 days, which is consistent with the fading of the IIn-like line profiles observed in SN 2023ixf at these phases.(The data used to create this figure are available.)
Paper: SN 2023ixf in Messier 101: Photo-ionization of Dense, Close-in Circumstellar Material in a Nearby Type II Supernova
Authors: W. V. Jacobson-Galán, L. Dessart, R. Margutti, R. Chornock, R. J. Foley, C. D. Kilpatrick, D. O. Jones, K. Taggart, C. R. Angus, S. Bhattacharjee, L. A. Braff, D. Brethauer, A. J. Burgasser, F. Cao, C. M. Carlile, K. C. Chambers, D. A. Coulter, E. Dominguez-Ruiz, C. B. Dickinson, T. de Boer, A. Gagliano, C. Gall, H. Gao, E. L. Gates, S. Gomez, M. Guolo, M. R. J. Halford, J. Hjorth, M. E. Huber, M. N. Johnson, P. R. Karpoor, T. Laskar, N LeBaron, Z. Li, Y. Lin, S. D. Loch, P. D. Lynam, E. A. Magnier, P. Maloney, D. J. Matthews, M. McDonald, H.-Y. Miao, D. Milisavljevic, Y.-C. Pan, S. Pradyumna, C. L. Ransome, J. M. Rees, A. Rest, C. Rojas-Bravo, N. R. Sandford, L. Sandoval Ascencio, S. Sanjaripour, A. Savino, H. Sears, N. Sharei, S. J. Smartt, E. R. Softich, C. A. Theissen, S. Tinyanont, H. Tohfa, V. A. Villar, Q. Wang, R. J. Wainscoat, A. L. Westerling, E. Wiston, M. A. Wozniak, S. K. Yadavalli, Y. Zenati
Figure caption: Early time spectral series of SN 2023ixf (black) with respect to CMFGEN model r1w6b (red), which is characterized by a wind mass-loss rate of ﹩\dot{M}={10}^{-2}\,{M}_{\odot }﹩ yr−1, and that extends to a CSM radius of R CSM = 8 × 1014 cm. Model spectra have been smoothed with a Gaussian kernel to match the spectral resolution of the data. Line identifications shown in blue. The disappearance of He I and N III after the δ t = +1.1 day spectrum indicates a rise in ionization and temperature in SN 2023ixf following the propagation of the shock breakout radiation.(The data used to create this figure are available.)
Paper: ALMA Reveals Hidden Morphologies in the Molecular Envelope of VY Canis Majoris
Authors: A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Comparative images of VY CMa: emission of 12CO (J = 2 → 1) at high resolution (left) and composite color HST image (right), displayed on the same scale, indicated by the 5″ bar on the top right. The approximate position of the star is given by a cross (white: ALMA; red: HST). The synthesized beam size is indicated in the lower left corner of the ALMA image. Individual features are labeled (a)–(j): (a) Arc 1, (b) Arc 2, (c) S Arc, (d) SW Clump, (e) NW Arc, (f) S Knot, (g) SE Loop, (h) E Bubble, (i) NE Extension, and (j) NE Arc (see Table 1). Some features appear in both images ((a)–(h)), but some are new ALMA detections ((i)–(j)).
Paper: The FRB 20190520B Sight Line Intersects Foreground Galaxy Clusters
Authors: Khee-Gan Lee, Ilya S. Khrykin, Sunil Simha, Metin Ata, Yuxin Huang, J. Xavier Prochaska, Nicolas Tejos, Jeff Cooke, Kentaro Nagamine, Jielai Zhang
Figure caption: Data points show the redshift and estimated halo masses of the detected groups from our FRB 20190520B spectroscopic data. Curves show the estimated mass completeness of simulated groups and clusters as a function of redshift, assuming the observational depth and completeness of our data. The dashed curve indicates the minimum mass at which groups are detectable with N rich ≥ 4 at the given redshift, while the solid curve indicates the mass at which we expect to be 100% complete.
Paper: The FRB 20190520B Sight Line Intersects Foreground Galaxy Clusters
Authors: Khee-Gan Lee, Ilya S. Khrykin, Sunil Simha, Metin Ata, Yuxin Huang, J. Xavier Prochaska, Nicolas Tejos, Jeff Cooke, Kentaro Nagamine, Jielai Zhang
Figure caption: Example of our halo mass estimation model using the group richness, built from mock groups/clusters from the Millennium simulation. The gray lines show the richness of an ensemble of mock groups selected at the redshift of our detected group at z grp = 0.1867 after incorporating the incompleteness and magnitude threshold of our data. The curve is the spline fit to this ensemble of mock groups, which is then used to estimate the halo masses as a function of the group richness.
Paper: The FRB 20190520B Sight Line Intersects Foreground Galaxy Clusters
Authors: Khee-Gan Lee, Ilya S. Khrykin, Sunil Simha, Metin Ata, Yuxin Huang, J. Xavier Prochaska, Nicolas Tejos, Jeff Cooke, Kentaro Nagamine, Jielai Zhang
Figure caption: Distribution of DMIGM for z frb = 0.241 sight lines in the Millennium simulation box, selected to intersect two M halo > 1014 M ⊙ halos. The direct influence of groups and halos has been removed according to the selection function of Figure 4. We assume f igm = 0.85 for this calculation.
Paper: ALMA Reveals Hidden Morphologies in the Molecular Envelope of VY Canis Majoris
Authors: A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: ALMA spectra of the J = 2 → 1 transition of 12CO, showing the combined profile for the entire envelope, and those extracted for individual outflows Arc 1, Arc 2, NW Arc, NE Arc, NE Extension, and E Bubble (see Section 4). The combined profile of the J = 3 → 2 transition of HCN is also shown. ESCAPADE fits are shown for select profiles (in red or gray scale).
Paper: First Constraints on Dense Molecular Gas at z = 7.5149 from the Quasar Pōniuā‘ena
Authors: Chiara Feruglio, Umberto Maio, Roberta Tripodi, Jan Martin Winters, Luca Zappacosta, Manuela Bischetti, Francesca Civano, Stefano Carniani, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Maria Vittoria Zanchettin
Figure caption: Upper panels: (left to right) the CO(6–5) emission line spectrum, the corresponding velocity-integrated CO map, and the 79.2 GHz continuum map of Pōniuā‘ena. Lower panels: the CO(7–6) emission line spectrum, the corresponding velocity-integrated map, and the 96.4 GHz continuum map relative to the phase center set at [R.A.,decl.] = [10:07:58.260, 21:15:29.20]. The velocity zero point is set to the frequency 81.207 GHz for CO(6–5) and 94.734 GHz for CO(7–6). In each panel we report the error bar showing the 1σ error bar in the 10 MHz spectral channel. Magenta lines show the fit with a single Gaussian component; FWHM is reported in Table 1. Contours are drawn starting at 2σ in steps of 1σ (σ = 0.05 Jy km s−1 for CO(6–5), 0.065 Jy km s−1 for CO(7–6), 15.5μ Jy for 79.2 GHz continuum, and 12.2μ Jy for 96.4 GHz continuum.
Paper: First Constraints on Dense Molecular Gas at z = 7.5149 from the Quasar Pōniuā‘ena
Authors: Chiara Feruglio, Umberto Maio, Roberta Tripodi, Jan Martin Winters, Luca Zappacosta, Manuela Bischetti, Francesca Civano, Stefano Carniani, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Maria Vittoria Zanchettin
Figure caption: CO SLED of Pōniuā‘ena compared with those of other QSOs at lower redshift. The CO SLED for Pōniuā‘ena is shown as red stars, for J0439+1634 at z = 6.511 as gray squares (Yang et al. 2019), for J1148+5251 at z = 6.419 as orange squares (Riechers et al. 2009a; Gallerani et al. 2014), for J0100+2802 at z = 6.327 as purple squares (Wang et al. 2019), for J2310+1855 at z = 6.003 as blue squares (Li et al. 2020), and for APM 08279+5255 at z = 3.911 as green squares (Papadopoulos et al. 2001; Weiß et al. 2007).
Paper: First Constraints on Dense Molecular Gas at z = 7.5149 from the Quasar Pōniuā‘ena
Authors: Chiara Feruglio, Umberto Maio, Roberta Tripodi, Jan Martin Winters, Luca Zappacosta, Manuela Bischetti, Francesca Civano, Stefano Carniani, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Maria Vittoria Zanchettin
Figure caption: Comoving cosmic mass density of cold molecular gas as a function of redshift. Vertical sizes indicate the uncertainties in each bin. Data are from Riechers et al. (2020a, 2020b; VLASPEC, COLDz), Decarli et al. (2020; ASPECS), Lenkić et al. (2020; PHIBSS-2), Garratt et al. (2021; UKIDSS-UDS), and Hamanowicz et al. (2023; ALMACAL-CO), and upper/lower limits from ALMACAL-abs (Klitsch et al. 2019) and Herschel PEP (Berta et al. 2013). Theoretical expectation from cold-gas simulations (dashed line) are by Maio et al. (2022).
Paper: ALMA Reveals Hidden Morphologies in the Molecular Envelope of VY Canis Majoris
Authors: A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Peak intensity (moment 8) images of J = 3 → 2 transition of HCN at 265 GHz. Left: ALMA Image at 0.″2 resolution. Right: combined ALMA and SMT image. Synthesized beam sizes are shown at lower left. Flux scale (Jy beam−1) is indicated in the figure.
Paper: First Constraints on Dense Molecular Gas at z = 7.5149 from the Quasar Pōniuā‘ena
Authors: Chiara Feruglio, Umberto Maio, Roberta Tripodi, Jan Martin Winters, Luca Zappacosta, Manuela Bischetti, Francesca Civano, Stefano Carniani, Valentina D'Odorico, Fabrizio Fiore, Simona Gallerani, Michele Ginolfi, Roberto Maiolino, Enrico Piconcelli, Rosa Valiante, Maria Vittoria Zanchettin
Figure caption: Results of the SED fitting of Pōniuā‘ena. Left panel: SED using our new NOEMA data at 3 mm (i.e., ∼80 and ∼90 GHz; green stars) and the ALMA data at ∼230 GHz taken from Yang et al. (2020; cyan diamond). The best-fitting curve with dust temperature fixed at 50 K is shown as a solid blue line. Right panels: corner plot showing the two-dimensional posterior probability distributions of M dust, β. Cyan solid lines indicate the best-fitting parameter, while the dashed lines mark the 16th and 84th percentiles for each parameter.
Paper: ALMA Reveals Hidden Morphologies in the Molecular Envelope of VY Canis Majoris
Authors: A. P. Singh, A. M. S. Richards, R. M. Humphreys, L. Decin, L. M. Ziurys
Figure caption: Peak intensity (moment 8) images of J = 2 → 1 transition of 12CO at 230 GHz. Left: ALMA Image at 0.″2 resolution. Right: combined ALMA and SMT image. Synthesized beam sizes are shown at lower left. Flux scale (Jy beam−1) is indicated on the figure.
Paper: Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?
Authors: Rui An, Vera Gluscevic, Ethan O. Nadler, Yue Zhang
Figure caption: Posterior distribution from the thermal-relic WDM fit to DES and PS1 MW satellites, presented in Nadler et al. (2021), cast into the parameter space of our self-interacting sterile-neutrino DM model (i.e., m 4, ﹩{\sin }^{2}2\theta ﹩, and λ  ϕ ). Dark (light) shaded contours represent 68% (95%) confidence intervals, respectively. Marginalized posteriors are shown in the top panel of each column. Note that σ  M , σ gal, and ﹩{\sigma }_{\mathrm{log}R}﹩ are reported in dex, ﹩{{ \mathcal M }}_{50}﹩ is reported as ﹩{\mathrm{log}}_{10}({{ \mathcal M }}_{50}/{{ \mathcal M }}_{\odot })﹩, m 4 is reported as ﹩{\mathrm{log}}_{10}({m}_{4}/\mathrm{keV})﹩, ﹩{ \mathcal A }﹩ is reported in pc, and α, ﹩{ \mathcal B }﹩, n, ﹩{\sin }^{2}2\theta ﹩, and λ  ϕ  are dimensionless. For details on the prior distributions assumed for galaxy–halo connection parameters when forward-modeling the MW satellite population, see Nadler et al. (2021).
Paper: Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?
Authors: Rui An, Vera Gluscevic, Ethan O. Nadler, Yue Zhang
Figure caption: Left panel: Combinations of neutrino self-interaction strength λ  ϕ  and mediator mass m  ϕ  that produce sterile-neutrino DM at the correct relic abundance, for a DM mass of m 4 = 40.3 keV and vacuum mixing angle of ﹩{\sin }^{2}2\theta =8.6\times {10}^{-13}﹩. Points in the three DM production regimes are labeled with A, B, and C, corresponding to the Cases described in the text. Middle panel: The corresponding DM phase-space distributions. For comparison, we also show the original DW model with no neutrino interactions as a dotted line, and the thermal-relic WDM model as a dotted–dashed line (evaluated at the 95% confidence 6.5 keV WDM mass bound from Nadler et al. (2021). Right panel: The corresponding suppression of DM clustering is illustrated as the ratio of the linear matter power spectrum in sterile-neutrino DM models to that of CDM. The vertical line indicates the half-mode scale k hm of the ruled-out WDM model.
Paper: Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?
Authors: Rui An, Vera Gluscevic, Ethan O. Nadler, Yue Zhang
Figure caption: Left panel: 95% confidence exclusion for sterile-neutrino DM from our analysis of the MW satellite galaxy population combined with particle collider bounds (colored shaded regions) is compared with X-ray annihilation bounds (light gray; Watson et al. 2012; Horiuchi et al. 2014; Bulbul et al. 2014; Boyarsky et al. 2014; Perez et al. 2017; Ng et al. 2019; Dessert et al. 2020) and the bounds from dwarf galaxy phase-space densities (dark gray; Alvey et al. 2021). Galaxy–halo connection and neutrino self-interaction parameters (m  ϕ  and λ  ϕ ) are marginalized over. The blue–green region with solid edges corresponds to the case where we only consider the limits from invisible Z-decays on λ  ϕ . The dashed, dashed–dotted or dotted lines correspond to bounds on specific mediator flavor-coupling scenarios. DW production mechanism corresponds to the solid black line. Middle and right panels: Our sterile-neutrino DM constraints divided according to the production scenario. Case A (red) is the heavy-mediator scenario ruled out by our analysis. Case B (yellow) and Case C (blue) correspond to light-mediator scenarios.
Paper: Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?
Authors: Rui An, Vera Gluscevic, Ethan O. Nadler, Yue Zhang
Figure caption: Neutrino self-interaction parameters that can populate sterile neutrinos with the entire DM relic abundance, for several combinations of m 4 and ﹩{\sin }^{2}2\theta ﹩ (gray curves). The dark green hatched region shows the constraint from invisible Z width; light green shaded regions show experimental flavor-dependent constraints (Berryman et al. 2018, 2023; Esteban et al. 2021). Diagonal black lines divide this parameter space into production regimes corresponding to Cases A, B, and C.
Paper: Can Neutrino Self-interactions Save Sterile Neutrino Dark Matter?
Authors: Rui An, Vera Gluscevic, Ethan O. Nadler, Yue Zhang
Figure caption: Sterile-neutrino ν  s  production channels, in the presence of active-neutrino self-interactions, in the cases of a heavy (left) or a light (right) scalar mediator. Oscillation of an active into a sterile neutrino is denoted with an “x.” Sterile neutrinos are populated via neutrino self-interactions and mediator decay, respectively, in these two cases.