pith. sign in

arxiv: 1907.04473 · v1 · pith:YDXDNALGnew · submitted 2019-07-10 · 🌌 astro-ph.IM · astro-ph.GA· hep-ex

CMB-S4 Science Case, Reference Design, and Project Plan

Kevork Abazajian , Graeme Addison , Peter Adshead , Zeeshan Ahmed , Steven W. Allen , David Alonso , Marcelo Alvarez , Adam Anderson
show 217 more authors
Kam S. Arnold Carlo Baccigalupi Kathy Bailey Denis Barkats Darcy Barron Peter S. Barry James G. Bartlett Ritoban Basu Thakur Nicholas Battaglia Eric Baxter Rachel Bean Chris Bebek Amy N. Bender Bradford A. Benson Edo Berger Sanah Bhimani Colin A. Bischoff Lindsey Bleem Sebastian Bocquet Kimberly Boddy Matteo Bonato J. Richard Bond Julian Borrill Fran\c{c}ois R. Bouchet Michael L. Brown Sean Bryan Blakesley Burkhart Victor Buza Karen Byrum Erminia Calabrese Victoria Calafut Robert Caldwell John E. Carlstrom Julien Carron Thomas Cecil Anthony Challinor Clarence L. Chang Yuji Chinone Hsiao-Mei Sherry Cho Asantha Cooray Thomas M. Crawford Abigail Crites Ari Cukierman Francis-Yan Cyr-Racine Tijmen de Haan Gianfranco De Zotti Jacques Delabrouille Marcel Demarteau Mark Devlin Eleonora Di Valentino Matt Dobbs Shannon Duff Adriaan Duivenvoorden Cora Dvorkin William Edwards Joseph Eimer Josquin Errard Thomas Essinger-Hileman Giulio Fabbian Chang Feng Simone Ferraro Jeffrey P. Filippini Raphael Flauger Brenna Flaugher Aurelien A. Fraisse Andrei Frolov Nicholas Galitzki Silvia Galli Ken Ganga Martina Gerbino Murdock Gilchriese Vera Gluscevic Daniel Green Daniel Grin Evan Grohs Riccardo Gualtieri Victor Guarino Jon E. Gudmundsson Salman Habib Gunther Haller Mark Halpern Nils W. Halverson Shaul Hanany Kathleen Harrington Masaya Hasegawa Matthew Hasselfield Masashi Hazumi Katrin Heitmann Shawn Henderson Jason W. Henning J. Colin Hill Ren\'ee Hlozek Gil Holder William Holzapfel Johannes Hubmayr Kevin M. Huffenberger Michael Huffer Howard Hui Kent Irwin Bradley R. Johnson Doug Johnstone William C. Jones Kirit Karkare Nobuhiko Katayama James Kerby Sarah Kernovsky Reijo Keskitalo Theodore Kisner Lloyd Knox Arthur Kosowsky John Kovac Ely D. Kovetz Steve Kuhlmann Chao-Lin Kuo Nadine Kurita Akito Kusaka Anne Lahteenmaki Charles R. Lawrence Adrian T. Lee Antony Lewis Dale Li Eric Linder Marilena Loverde Amy Lowitz Mathew S. Madhavacheril Adam Mantz Frederick Matsuda Philip Mauskopf Jeff McMahon Matthew McQuinn P. Daniel Meerburg Jean-Baptiste Melin Joel Meyers Marius Millea Joseph Mohr Lorenzo Moncelsi Tony Mroczkowski Suvodip Mukherjee Moritz M\"unchmeyer Daisuke Nagai Johanna Nagy Toshiya Namikawa Federico Nati Tyler Natoli Mattia Negrello Laura Newburgh Michael D. Niemack Haruki Nishino Martin Nordby Valentine Novosad Paul O'Connor Georges Obied Stephen Padin Shivam Pandey Bruce Partridge Elena Pierpaoli Levon Pogosian Clement Pryke Giuseppe Puglisi Benjamin Racine Srinivasan Raghunathan Alexandra Rahlin Srini Rajagopalan Marco Raveri Mark Reichanadter Christian L. Reichardt Mathieu Remazeilles Graca Rocha Natalie A. Roe Anirban Roy John Ruhl Maria Salatino Benjamin Saliwanchik Emmanuel Schaan Alessandro Schillaci Marcel M. Schmittfull Douglas Scott Neelima Sehgal Sarah Shandera Christopher Sheehy Blake D. Sherwin Erik Shirokoff Sara M. Simon Anze Slosar Rachel Somerville David Spergel Suzanne T. Staggs Antony Stark Radek Stompor Kyle T. Story Chris Stoughton Aritoki Suzuki Osamu Tajima Grant P. Teply Keith Thompson Peter Timbie Maurizio Tomasi Jesse I. Treu Matthieu Tristram Gregory Tucker Caterina Umilt\`a Alexander van Engelen Joaquin D. Vieira Abigail G. Vieregg Mark Vogelsberger Gensheng Wang Scott Watson Martin White Nathan Whitehorn Edward J. Wollack W. L. Kimmy Wu Zhilei Xu Siavash Yasini James Yeck Ki Won Yoon Edward Young Andrea Zonca
This is my paper

Pith reviewed 2026-05-24 23:53 UTC · model grok-4.3

classification 🌌 astro-ph.IM astro-ph.GAhep-ex
keywords CMB-S4cosmic microwave backgroundground-based cosmologyscience casereference designproject planStage-4 experiment
0
0 comments X

The pith

The CMB-S4 project presents a unified science case, reference design, and project plan for a next-generation ground-based cosmic microwave background experiment.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper lays out the motivations for CMB-S4 as a Stage-4 experiment, covering measurements of primordial gravitational waves, neutrino properties, and dark energy evolution. It specifies a reference design that combines multiple telescopes and detector arrays to reach the necessary sensitivity and sky coverage. A project plan is included that addresses construction, operations, and collaboration structure. A sympathetic reader would care because the document supplies the concrete blueprint needed to move from current experiments to one that could deliver decisive cosmological data.

Core claim

The paper presents the science case, reference design, and project plan for the Stage-4 ground-based cosmic microwave background experiment CMB-S4.

What carries the argument

The CMB-S4 reference design, which specifies the telescope array, detector technology, and survey strategy required to meet the target sensitivities.

If this is right

  • The design would enable a detection or strong upper limit on the tensor-to-scalar ratio from primordial gravitational waves.
  • It would tighten constraints on the sum of neutrino masses through measurements of the CMB power spectrum and lensing.
  • CMB lensing maps would provide new information on the growth of structure and dark energy.
  • The experiment would complement optical and other surveys by supplying independent cosmological parameters.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Success would create a natural next step for combining CMB data with galaxy surveys to break degeneracies in dark energy models.
  • The reference design could serve as a template for scaling similar large-scale ground-based instruments in other wavelength bands.

Load-bearing premise

The reference design is technically and financially feasible for achieving the science goals described in the case.

What would settle it

A technical or cost review that shows the proposed detector noise levels or total project budget cannot be met within the stated timeline.

Figures

Figures reproduced from arXiv: 1907.04473 by Abigail Crites, Abigail G. Vieregg, Adam Anderson, Adam Mantz, Adriaan Duivenvoorden, Adrian T. Lee, Akito Kusaka, Alessandro Schillaci, Alexander van Engelen, Alexandra Rahlin, Amy Lowitz, Amy N. Bender, Andrea Zonca, Andrei Frolov, Anirban Roy, Anne Lahteenmaki, Anthony Challinor, Antony Lewis, Antony Stark, Anze Slosar, Ari Cukierman, Aritoki Suzuki, Arthur Kosowsky, Asantha Cooray, Aurelien A. Fraisse, Benjamin Racine, Benjamin Saliwanchik, Blake D. Sherwin, Blakesley Burkhart, Bradford A. Benson, Bradley R. Johnson, Brenna Flaugher, Bruce Partridge, Carlo Baccigalupi, Caterina Umilt\`a, Chang Feng, Chao-Lin Kuo, Charles R. Lawrence, Chris Bebek, Chris Stoughton, Christian L. Reichardt, Christopher Sheehy, Clarence L. Chang, Clement Pryke, Colin A. Bischoff, Cora Dvorkin, Daisuke Nagai, Dale Li, Daniel Green, Daniel Grin, Darcy Barron, David Alonso, David Spergel, Denis Barkats, Doug Johnstone, Douglas Scott, Edo Berger, Edward J. Wollack, Edward Young, Elena Pierpaoli, Eleonora Di Valentino, Ely D. Kovetz, Emmanuel Schaan, Eric Baxter, Eric Linder, Erik Shirokoff, Erminia Calabrese, Evan Grohs, Federico Nati, Fran\c{c}ois R. Bouchet, Francis-Yan Cyr-Racine, Frederick Matsuda, Gensheng Wang, Georges Obied, Gianfranco De Zotti, Gil Holder, Giulio Fabbian, Giuseppe Puglisi, Graca Rocha, Graeme Addison, Grant P. Teply, Gregory Tucker, Gunther Haller, Haruki Nishino, Howard Hui, Hsiao-Mei Sherry Cho, Jacques Delabrouille, James G. Bartlett, James Kerby, James Yeck, Jason W. Henning, J. Colin Hill, Jean-Baptiste Melin, Jeff McMahon, Jeffrey P. Filippini, Jesse I. Treu, Joaquin D. Vieira, Joel Meyers, Johanna Nagy, Johannes Hubmayr, John E. Carlstrom, John Kovac, John Ruhl, Jon E. Gudmundsson, Joseph Eimer, Joseph Mohr, Josquin Errard, J. Richard Bond, Julian Borrill, Julien Carron, Kam S. Arnold, Karen Byrum, Kathleen Harrington, Kathy Bailey, Katrin Heitmann, Keith Thompson, Ken Ganga, Kent Irwin, Kevin M. Huffenberger, Kevork Abazajian, Kimberly Boddy, Kirit Karkare, Ki Won Yoon, Kyle T. Story, Laura Newburgh, Levon Pogosian, Lindsey Bleem, Lloyd Knox, Lorenzo Moncelsi, Marcel Demarteau, Marcel M. Schmittfull, Marcelo Alvarez, Marco Raveri, Maria Salatino, Marilena Loverde, Marius Millea, Mark Devlin, Mark Halpern, Mark Reichanadter, Mark Vogelsberger, Martina Gerbino, Martin Nordby, Martin White, Masashi Hazumi, Masaya Hasegawa, Mathew S. Madhavacheril, Mathieu Remazeilles, Matt Dobbs, Matteo Bonato, Matthew Hasselfield, Matthew McQuinn, Matthieu Tristram, Mattia Negrello, Maurizio Tomasi, Michael D. Niemack, Michael Huffer, Michael L. Brown, Moritz M\"unchmeyer, Murdock Gilchriese, Nadine Kurita, Natalie A. Roe, Nathan Whitehorn, Neelima Sehgal, Nicholas Battaglia, Nicholas Galitzki, Nils W. Halverson, Nobuhiko Katayama, Osamu Tajima, Paul O'Connor, P. Daniel Meerburg, Peter Adshead, Peter S. Barry, Peter Timbie, Philip Mauskopf, Rachel Bean, Rachel Somerville, Radek Stompor, Raphael Flauger, Reijo Keskitalo, Ren\'ee Hlozek, Riccardo Gualtieri, Ritoban Basu Thakur, Robert Caldwell, Salman Habib, Sanah Bhimani, Sarah Kernovsky, Sarah Shandera, Sara M. Simon, Scott Watson, Sean Bryan, Sebastian Bocquet, Shannon Duff, Shaul Hanany, Shawn Henderson, Shivam Pandey, Siavash Yasini, Silvia Galli, Simone Ferraro, Srini Rajagopalan, Srinivasan Raghunathan, Stephen Padin, Steve Kuhlmann, Steven W. Allen, Suvodip Mukherjee, Suzanne T. Staggs, Theodore Kisner, Thomas Cecil, Thomas Essinger-Hileman, Thomas M. Crawford, Tijmen de Haan, Tony Mroczkowski, Toshiya Namikawa, Tyler Natoli, Valentine Novosad, Vera Gluscevic, Victor Buza, Victor Guarino, Victoria Calafut, William C. Jones, William Edwards, William Holzapfel, W. L. Kimmy Wu, Yuji Chinone, Zeeshan Ahmed, Zhilei Xu.

Figure 1
Figure 1. Figure 1: Forecast of CMB-S4 constraints in the ns–r plane for a fiducial model with r = 0.003. Also shown are the current best constraints from a combination of the BICEP2/Keck Array experiments and Planck [5]. Models that naturally explain the observed departure from scale invariance separate into two viable classes: monomial and plateau. The monomial models (V (φ) = µ 4−pφ p ) are shown for three values of p as b… view at source ↗
Figure 2
Figure 2. Figure 2: CMB-S4-enabled exploration of light relics, axions, neutrino mass, and dark matter properties. In each case, there is a window in the mass of the relevant particle where the CMB is particularly sensitive. Each such region is shown in a color (or colors) representing the observable(s) that drives the constraint. The primary CMB anisotropies at high-` (blue) is particularly sensitive to light relics, as disc… view at source ↗
Figure 3
Figure 3. Figure 3: Example lensing-deflection maps (top) and thermal SZ (Compton y-maps, bottom) recon￾structed with Planck (left) and CMB-S4 data (right). The center panels show a 25 deg2 patch of the all-sky lensing-deflection field in the WebSky simulations (top) and Compton y (bottom). The left panels show Wiener-filtered maps of the signal after adding (Gaussian) noise and residual foregrounds with levels corresponding … view at source ↗
Figure 4
Figure 4. Figure 4: CMB-S4 survey area, in Galactic coordinates, with the ecliptic plane marked as the solid line. Low-redshift structure acts to lens both the CMB and the images of intermediate-z galaxies. Detailed comparisons provides a valuable cross-check on galaxy shear measurement calibration and enables geometric tests using the longest possible lever arm. Most of the baryons in the late Universe are believed to be in … view at source ↗
Figure 5
Figure 5. Figure 5: Filled circles show 5σ limiting magnitudes for transient surveys (ASAS-SN, Zwicky Transient Facility, Large Synoptic Sky Survey, Australia SKA Pathfinder, all in black, CMB-S4 weekly flux limit in red) over a large fraction of the sky. Diagonal lines indicate constant νSν, lines separated by factors of 100: green shows a Neptune-mass planet at 500 AU; and blue lines show SEDs corresponding to a quasar or b… view at source ↗
Figure 6
Figure 6. Figure 6: Theoretical predictions for the temperature (black), E-mode (red), and tensor B-mode (blue) power spectra. Primordial B-mode spectra are shown for two representative values of the tensor-to-scalar ratio: r = 0.001 and r = 0.05. The contribution to tensor B modes from scattering during the recombination epoch peaks at ` ≈ 80 and from reionization at ` < 10. Also shown are expected values for the contributio… view at source ↗
Figure 7
Figure 7. Figure 7: Forecast of CMB-S4 constraints in the ns–r plane for a fiducial model with r = 0.003. For comparison, we also show the current best constraints from a combination of the BICEP2/Keck Array experiments, Planck [5], and BAO data. These are compared to several theoretical models. Chaotic inflation with V (φ) = µ 4−pφ p for p = 2/3, 1, 2 are shown as blue lines for 47 < N∗ < 57 (with smaller N∗ predicting lower… view at source ↗
Figure 8
Figure 8. Figure 8: Forecast of CMB-S4 constraints in the ns–r plane for a fiducial model with r = 0. Also shown are the current best constraints from a combination of the BICEP2/Keck Array experiments and Planck [5]. The Starobinsky model and Higgs inflation are shown as small and large orange filled circles. The lines show the classes of model that naturally explain the observed value of ns. The corresponding potentials all… view at source ↗
Figure 9
Figure 9. Figure 9: Reconstructed primordial power spectrum with CMB-S4 noise curve including atmospheric noise co-added with Planck noise, noise from point sources, and lensing reconstruction. We parameterize our source function δG0 in the range 0.5 < s/Mpc < 4870 with a total of 40 parameters, equispaced in logarithmic scale. Also shown are the constraints coming from the Simons Observatory baseline, for the same fraction o… view at source ↗
Figure 10
Figure 10. Figure 10: Left: Limits on the dark-matter-baryon cross-section σbDM for a Yukawa potential. Future cosmological constraints will restrict ∆Neff < 0.09 and, therefore, exclude cross-sections large enough to thermalize the (200 keV-mass) particle mediating the force [196]. This limit is compared to the direct bound on baryon-dark-matter scattering from the CMB [198] and to the constraints on dark forces from the Bull… view at source ↗
Figure 11
Figure 11. Figure 11: Left: Constraints in the Yp–Neff plane from current and future cosmological surveys, compared to the predictions of standard BBN and current astrophysical measurements of Yp [219]. Right: Inferred reach in TF for a given sensitivity to Neff . The vertical limits on TF assume we are using a vector (g = 2) to relate 2σ Neff limits to TF. We see that at CMB-S4 sensitivity, constraints have a reach two orders… view at source ↗
Figure 12
Figure 12. Figure 12: While all probes show some degeneracy between the neutrino mass and the dark-energy equation of [PITH_FULL_IMAGE:figures/full_fig_p047_12.png] view at source ↗
Figure 12
Figure 12. Figure 12: Left panel: Forecasted constraints on the neutrino mass sum for several different CMB-S4- derived cosmological probes, written here in terms of the significance of a detection of the minimum value consistent with oscillation data Mν = 58meV. Neutrino mass constraints are degenerate with the optical depth to the CMB, τ . Constraints here are shown as a function of the assumed 1 − σ errors on τ . All probes… view at source ↗
Figure 13
Figure 13. Figure 13: Left: Majorana effective neutrino mass mββ versus Mν in the scenario where NLDBD is mediated by light neutrino exchange. The area enclosed by the blue and red solid lines indicate the allowed 95% ranges from neutrino oscillation experiments [236] for normal ordering (NO) and inverted ordering (IO) assuming complete ignorance of the Majorana phases. The vertical blue and red bands show the forecasted 1σ co… view at source ↗
Figure 14
Figure 14. Figure 14: Improvement on the standard w0–wa parameters for the combination of: (i) Planck prior and expansion history measurements (DESI BAO) in black; (ii) LSST 3×2-point function measurements (including auto- and cross-correlation of galaxy number density and shear field fluctuations) in blue; and (iii) the combination of the first two items, with CMB-S4 power-spectrum measurements (temperature, polarization, and… view at source ↗
Figure 15
Figure 15. Figure 15: Constraints on the growth parameter from CMB-S4 from two independent sets of measure￾ments. Left panel: Constraints on the matter amplitude σ8 in tomographic redshift bins (indicated by the positions of points) from the combination of LSST galaxies and CMB-S4 lensing, assuming a fixed ΛCDM cosmology. Relaxing this assumption does not diminsh our ability to measure departures from the fiducial model. Right… view at source ↗
Figure 16
Figure 16. Figure 16: Black lines represent model-independent projected noise for the cosmic-birefringence rotation￾angle spectrum for CMB-S4. The noise assumes no rotation signal and is calculated in three different ways: (a) assuming no delensing and using the forecasted noise in the ILC (dot-short dash line); (b) assuming 80% delensing and with forecasted noise remaining after the foreground subtraction (solid line); and (c… view at source ↗
Figure 17
Figure 17. Figure 17: Left: Illustration of the effect of a velocity-independent spin-independent contact interaction between dark matter and baryons (with a cross-section 100 times higher than the current upper limit from Planck) on the CMB temperature power spectrum (blue), compared to the CDM case (black). Right: Upper limits on the DM-proton interaction cross-section as a function of DM mass, for spin-independent velocity￾… view at source ↗
Figure 18
Figure 18. Figure 18: Dark matter-dark radiation interaction sensitivity of Planck (adapted from Ref. [291]) and an experiment like CMB-S4; for this plot, we assumed a configuration of CMB-S4 similar to that outlined in the CDT. The x-axis corresponds to the interaction strength, while the y-axis corresponds to the abundance of dark radiation. We show two different fractions of DM interacting with the DR, as indicated on each … view at source ↗
Figure 19
Figure 19. Figure 19: Constraints on ultra-light axions (ULAs). Left: Fisher-forecasted 2σ exclusion regions for the ULA mass fraction Ωa/Ωd for the Planck alone, Planck + Simons Observatory (SO) (as discussed in Ref. [49]), and CMB-S4, where Ωd = Ωa + Ωc. Right: Residual in lensing-convergence power spectrum C κκ L for different models including ULA DM, compared with Fisher-forecasted errors for CMB-S4. constraints. In this w… view at source ↗
Figure 20
Figure 20. Figure 20: Post-component-separation noise for the Compton-y map reconstructed from the CMB-S4 LATs and Planck. The solid black curve shows the tSZ power-spectrum signal. The solid blue curve shows the ILC reconstruction noise, while the other curves show the noise levels for various foreground-deprojection options. The thin, solid magenta curve shows the ILC reconstruction noise for the Simons Observatory baseline … view at source ↗
Figure 21
Figure 21. Figure 21: CMB-S4 constraints on the cumulative electron-density (left) and thermal-energy (right) profiles will distinguish between feedback models. Top row: Stacking N = 2.5 × 105 BOSS and SDSS LRG halos of average mass M200c = 1013 M at z = 0.2. The left panel is extracted from the kSZ signal and the right panel from the tSZ signal. The lines come from density and pressure profiles around such halos measured in s… view at source ↗
Figure 22
Figure 22. Figure 22: Top: CMB-S4 constraints on the cumulative electron-density (left) and cumulative thermal￾energy (right) profiles inferred by stacking N = 1.5×103 CMB-S4 clusters of average mass M200c = 1014 M at z = 0.2. Bottom: The same inferred by stacking N = 1.1 × 103 CMB-S4 clusters of average mass M200c = 1014 M at z = 1. The panels, curves, and data points with error bars are analogous to those shown in [PITH_FUL… view at source ↗
Figure 23
Figure 23. Figure 23: Fractional constraints on the integrated pressure versus halo mass relation from a joint analysis of CMB-S4 and DESI data. 1.4.2.2 Patchy reionization The patchiness of reionization leaves its imprint on the CMB through the kSZ effect, which refers to blackbody temperature fluctuations induced by a combination of coherent bulk flows on larges scales and variations in the electron density on small scales. … view at source ↗
Figure 24
Figure 24. Figure 24: CMB-S4 constraints on the optical depth and duration of reionization in a joint analysis using the kSZ power spectrum and four-point function. detectable by CMB-S4 through the B-mode power at ` ≈ 50–500 or by explicit reconstruction of the optical depth at the map level [417]. Additionally, it is possible to correlate these patchy polarization anisotropies induced by patchy reionization with other tracers… view at source ↗
Figure 25
Figure 25. Figure 25: Cumulative number of clusters above a fixed redshift for published (solid [431, 432, 433]), and upcoming (dashed [429, 49]) CMB cluster samples. CMB-S4 will discover an order of magnitude more of the highest-redshift (z > 1.5) clusters than previous surveys. 1.4.3.2 Dusty star-forming galaxies The unique combination of resolution, depth, and area covered make CMB-S4 ideal for constructing catalogs of extr… view at source ↗
Figure 26
Figure 26. Figure 26: Left: Source density in the mm sky from SPT-SZ, SCUBA-2, and various galaxy-evolution models. With the expected 220-GHz detection threshold shown by the short-dashed line, CMB-S4 will detect over 100,000 extragalactic sources, including more than 10,000 strongly-lensed galaxies and thousands of galaxies at z > 7. Right: Expected number of DSFGs in the CMB-S4 survey. The gray line shows the measured distri… view at source ↗
Figure 27
Figure 27. Figure 27: Millimeter-wave Solar System. Red circles show predicted asteroid flux densities at 150 GHz, crosses show estimated flux densities of known dwarf planets at 90, 150, and 220 GHz, and diagonal lines show the flux density of any possible Earth-sized planet in the outer Solar System in the CMB-S4 bands. Planet 9 is estimated to be several Earth masses at a distance of several hundred AU. 1000 AU. The recent … view at source ↗
Figure 28
Figure 28. Figure 28: Each science theme has one science topic contributing to the definition of measurement requirements and instrument requirements. The choice of a combination of low-res maps and high-res maps is driven entirely by PGW. The choice of a two-tiered survey is driven by the combined requirements of the PGW and Light Relics drivers. The connections of all the drivers to the measurement properties are indicated w… view at source ↗
Figure 29
Figure 29. Figure 29: South Pole mm-wave instrumentation site as it currently exists. CMB-S4 would expand on the existing infrastructure at this site. 5 LAT 1 LAT 2 [PITH_FULL_IMAGE:figures/full_fig_p102_29.png] view at source ↗
Figure 30
Figure 30. Figure 30: CMB observatories in Chile are all at this Cerro Toco site. The white arrows indicate possible LAT locations that would not conflict with the preliminary Simons Observatory (SO) instrumentation layout. Site Number of LATs Number of SAT cryostats Number of individual SATs Chile 2 0 0 South Pole 1 6 18 [PITH_FULL_IMAGE:figures/full_fig_p102_30.png] view at source ↗
Figure 31
Figure 31. Figure 31: The CMB-S4 Large Aperture Telescope reference design is based on the design of the SO-LAT and CCAT-prime telescopes [507, 508]. The mirrors (M1 and M2) are completely enclosed in the co-moving elevation structure (left), which will improve sidelobe mitigation compared to existing telescopes. The Large Aperture Telescope receiver (LATR, right) is aligned with the telescope elevation axis. This enables two … view at source ↗
Figure 33
Figure 33. Figure 33: Left: Mirror panel views, reflecting surface (top), backside (bottom). The panel is 700 mm on a side and significantly light-weighted from a solid block of aluminum. Eight adjusters locate the panel. The five z-axis adjusters allow for some compensation of low order distortions. Middle: Three views of a preliminary carbon fiber bus structure for the primary mirror panels. The red elements are tuned CTE be… view at source ↗
Figure 34
Figure 34. Figure 34: Left: Raytrace of the CD telescope design with 19 optics tubes that are each designed to illuminate 5.5 m of the 6-m aperture telescope. Middle: Side view showing five of the 19 optics tubes. Right: Preliminary design for a 19-optics-tube cryostat developed by the Simons Observatory collaboration. Subsystem HWFE (µm rms) Primary 18 Secondary 15 Telescope alignment 21 Camera filters 10 Camera lenses 10 Cam… view at source ↗
Figure 35
Figure 35. Figure 35: Preliminary baffle and shielding studies for the Large Aperture Telescope using non-sequential ray tracing [516]. The upper left shows a baffle configuration for the Large Aperture Telescope that includes a parabolic baffle near the receiver plus large secondary and primary guard ring baffles. Current analyses suggest that the parabolic baffle (pink, left) is important, but the large guard ring baffles (g… view at source ↗
Figure 36
Figure 36. Figure 36: SO 13-tube camera design. of reflections to 3 × 10−3 , minimizing systematics effects and nearly eliminating sensitivity losses due to reflectance in silicon lenses. The LATR requires lenses with diameters up to 40 cm, while silicon is available up to 46 cm diameter. Fabrication of lenses at the production rate required for CMB-S4 is on track to be demonstrated in early 2019 for Simons Observatory. The IR… view at source ↗
Figure 37
Figure 37. Figure 37: Preliminary optics tube designs for the LAT receiver [517]. The top shows a ray trace and includes labels for all the optical elements. The bottom shows much of the internal structure of the mechanical design that will be used to support, thermally isolate, and cool the optics and detector arrays. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p121_37.png] view at source ↗
Figure 38
Figure 38. Figure 38: Thermal model of an optics tube showing all the filter elements and tube walls at each temperature stage. The light lines do not represent the actual ray trace; they merely highlight the location of the Lyot stop. 4.3.4.3 Optics tubes The optics tubes contain all optical and detector components between 4 K and 100 mK. Each tube is self contained, so it can be installed as a single unit (see [PITH_FULL_IM… view at source ↗
Figure 39
Figure 39. Figure 39: Front plate detail showing the material saved by using hexagonal windows. The gray circles are the size of the hole of equivalent minimum beam clearance at the outside surface of the front plate. Making the windows inscribed hexagons instead of the circles which circumscribe them adds a significant amount of material at the weakest point in the fplate [PITH_FULL_IMAGE:figures/full_fig_p125_39.png] view at source ↗
Figure 40
Figure 40. Figure 40: Cross-section of the front plate showing tapering of the window holes to match the beam divergence. Light is entering the cryostat from the right, and the detector arrays are on the left. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p125_40.png] view at source ↗
Figure 41
Figure 41. Figure 41: The small-telescopes instrument requirements, detailed in this subsection, are motivated by the unique measurement challenges set by measuring r to the required uncertainty using ultra-deep B-mode measurements at degree scales. while adding little technical risk. In making design choices we have distinguished between engineering issues, those that can be fully developed and demonstrated in the lab to reti… view at source ↗
Figure 42
Figure 42. Figure 42: The CMB-S4 small-telescope optics are simple cryogenic refractors of approximately half￾meter aperture, a design based on heritage from the cryogenic refractors of the BICEP series of telescopes which have proven their performance in deep r measurements through Stages 1, 2, and 3. Shown here is the BICEP3 telescope, which has been observing since 2015, as an example of an existing instrument that illustra… view at source ↗
Figure 43
Figure 43. Figure 43: The detailed optical designs for the small telescopes are based on the realized 2-lens (BICEP, left panel), and 3-lens (SO, right panel) refractors that offer large optical throughput (etendue), symmetric main beams, and excellent polarization properties. Refractors are significantly more compact compared to crossed-Dragone telescopes with the same primary aperture, and offer advantages of symmetry and si… view at source ↗
Figure 44
Figure 44. Figure 44: Left: drawing of the SO cryogenic half-wave plate section. The HWP system consists of the sapphire HWP and rotation mechanism adopting superconducting mag-lev bearing. The optical clear aperture is 50 cm in diameter. Right: a photo of the Simons Array cryogenic half-wave plate system, from which the SO system is derived. three-layer stack allows a wide-enough modulation bandwidth for the dichroic detector… view at source ↗
Figure 45
Figure 45. Figure 45: On the left, the SO cryostat, illustrating a design that uses a dilution refrigerator to cool focal plane and 1-K optics. On the right, the reference design “3-tube” cryostat. It accommodates three cryogenic optics tubes each fitting within a 70-cm diameter × 150-cm long envelope, cooled to 4 K by the three pulsetubes located around the lower perimeter of the cryostat and to 1 K and (for the focal planes)… view at source ↗
Figure 46
Figure 46. Figure 46: The CMB-S4 small-aperture telescope reference design telescope mount is based on the existing BICEP Array mount design (left). Although originally designed for four individual small-aperture telescope cryostats (each with a single pulsetube), its size is well-suited to mount the single 3-tube cryostat with three pulsetubes and dilution refrigerator (right). It allows three axis motion with infinite rotati… view at source ↗
Figure 47
Figure 47. Figure 47: Exterior view of the small-telescope mount and shielding. The 3-tube cryostat is surrounded by a co-moving absorptive forebaffle. The mount sits within a large reflective ground shield. An additional co-rotating “scoop” is used to keep the shield dimensions reasonable. A flexible environmental seal surrounds the mount structure. The mount provides a flexible environmental seal that fully encloses the comp… view at source ↗
Figure 48
Figure 48. Figure 48: Schematic diagram of a horn-coupled focal plane [529]. fluctuations in the thermal carriers of the TES weak thermal link. The CMB-S4 TES bolometers will be designed and fabricated with parameters tailored for individual passbands at each site. These parameters will be chosen to provide the detectors with sufficient dynamic range to accommodate variations in weather and to provide sufficient thermal isolat… view at source ↗
Figure 49
Figure 49. Figure 49: The figure represents a DC wafer with 32 multiplexing chips for allowing 2048-detector readout capability. The addressing lines will be routed out from top or bottom of this wafer and the bias lines will be routed out from the left/right vertices. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p143_49.png] view at source ↗
Figure 50
Figure 50. Figure 50: (Left) Photograph of an Advanced ACTPol detector array fabricated by NIST on a 150-mm diameter silicon wafer. (Right) Photograph of a POLARBEAR-2 focal plane. The diameter of the focal plane is approximately 400 mm. The focal planes for the small aperture telescopes will be constructed from from combinations of hexagonal, half-hexagon, and rhomb sub-arrays that vary with the frequency band. A hexagonal fo… view at source ↗
Figure 51
Figure 51. Figure 51: Optical microscope image of an Advanced ACTPol detector pixel highlighting several of the key components. Magnified images of the major pixel components include: (a) the planar orthomode transducer; (b) the coplanar waveguide to microstrip transmission line; (c) the band-defining in-line stub filters; (d) the 180 degree hybrid tee; and (e) one of the AlMn TESs. Fabrication plan: The detector fabrication p… view at source ↗
Figure 52
Figure 52. Figure 52: Photographs of nanofabrication facilities and devices fabricated at: (Left) ANL (Center) LBNL/ U.C. Berkeley with (Right) SLAC Fabrication quality control: One critical challenge for detector fabrication is to develop robust fabrication procedures that guard against process deviation. To address this, CMB fabrication facilities have been tracking processes throughout fabrication and ensure that the fabric… view at source ↗
Figure 53
Figure 53. Figure 53: Spline-profiled feedhorn profiles across the planned CMB-S4 frequency bands are shown on the left. The top profile is the AdvACT 27/39-GHz design, which was direct-machined into SiAl alloy. The middle profile is a Au-coated Al feedhorn with the same design as the 90/150-GHz AdvACT feedhorn. The bottom profile is an Al SO 220/280-GHz design. The figure on the right is a measurement of the beams of the AdvA… view at source ↗
Figure 54
Figure 54. Figure 54: shows the schematic of one column of a time division SQUID multiplexer. The multiplexer chips outlined in blue in this figure are located at 100 mK, whereas SQUID Array Amplifiers (SAAs) are heatsunk to ≈4 K. A detector bias/filter chip (not shown), which sits between the multiplexer and the detector, contains shunt resistors that provide the TES voltage bias and inductors to limited the bandwidth to belo… view at source ↗
Figure 55
Figure 55. Figure 55: Behind-wafer TDM packaging implemented for BICEP3. Figure reproduced from Ref. [537]. Fabrication plan Many tens of thousands of TDM SQUID channels have been fabricated and successfully deployed in astronomical instruments. The multiplexer design and fabrication are mature. TDM fabrication will be done at class 100 clean room facilities at the National Laboratories. The baseline fabrication plan utilizes … view at source ↗
Figure 56
Figure 56. Figure 56: Block diagram of one bolometer array controlled and read out by one box of warm TDM electronics. Typically all boxes attached to a given cryostat are synchronized at the 50-MHz ADC clock or at the data strobe rate, which is often ≈ 1 kHz. No technical innovation is needed to use the present electronics to control a 64 × 64 element array. Command, data and clock connections to the Observtory DAQ are via op… view at source ↗
Figure 57
Figure 57. Figure 57: Schematic of the CMB-S4 detector module stack consisting of a feedhorn array, detector array, backshort wafers, and the CRS. The CRS consists of the DI wafer with mux chips and IO wafer. optical efficiency (via a cold thermal load). Optical tests will measure the detector optical bandpass for approximately 30% of the array. This approach exploits the fact that the polarized beam is determined by the feedh… view at source ↗
Figure 58
Figure 58. Figure 58: Telescope platform detail of the observatory control system, showing high-level control of a telescope platform, warm readout, and housekeeping systems. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p156_58.png] view at source ↗
Figure 59
Figure 59. Figure 59: Overview of the observatory control system, including the alarms, data acquisition control, and monitoring, including the interface to all telescope platforms. While individual telescope subsystems within the observatory may produce large volumes of data, or may need to operate in hard real-time to meet performance requirements, there are no interactions between subsystems that require exchange or analysi… view at source ↗
Figure 60
Figure 60. Figure 60: Distribution of timing signals (IRIG timestamps, 10-MHz clock line, optional pulse-per-second) for a given observatory. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p159_60.png] view at source ↗
Figure 61
Figure 61. Figure 61: Schematic view of the data-management subsystem, spanning the range from Data Acquisition to Science Analyses, with on-project cost areas highlighted in cyan. Note that the named networking, storage and compute resources are indicative and anticipated, not yet confirmed. to perform all time-critical data reductions—primarily to generate the data products that will be sent over the network each day, includ… view at source ↗
Figure 62
Figure 62. Figure 62: Schematic view of data-transport paths from acquisition to the U.S. data centers for the Chile and South Pole sites. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p163_62.png] view at source ↗
Figure 63
Figure 63. Figure 63: Schematic view of the CMB-S4 data analysis pipeline (from figure 88 of the CMB-S4 Science Book), with boxes illustrating which elements are grouped under Data Management (Sect. 4.7) and which elements are grouped under Science Analyses (this chapter). φ reconstruction for CMB-S4 will come entirely from the combination of CMB E-mode and B-mode polarization, from the so-called EB estimator. This is partiall… view at source ↗
Figure 64
Figure 64. Figure 64: Organizational chart of the CMB-S4 col￾laboration. One recommendation of the CDT report was that the community should organize itself into a formal collaboration, and an Interim Collaboration Coordination Committee was elected to coordinated this process. The re￾sulting draft bylaws were refined at the Spring 2018 community workshop, and overwhelm￾ingly ratified on March 19th 2018, bringing the CMB-S4 col… view at source ↗
Figure 65
Figure 65. Figure 65: Organizational chart of the interim project office. The figure includes a notional distribution of project scope by funding agency (NSF = blue, DOE = green, Other = yellow). We are actively pursuing partners who could make significant scope contributions in areas aligned with their expertise. CMS. The lines of accountability for project delivery are clearly defined within the project organization. The pro… view at source ↗
Figure 66
Figure 66. Figure 66: CMB-S4 schedule and milestone summary. CMB-S4 Science Case, Reference Design, and Project Plan [PITH_FULL_IMAGE:figures/full_fig_p192_66.png] view at source ↗
Figure 67
Figure 67. Figure 67: Calculated atmospheric brightness spectra (at zenith) for the South Pole at 0.5 mm PWV and Atacama at 1.0 mm PWV (both are near median values). Atmospheric spectra are generated using Ref. [563]. The tophat bands are plotted on top of these spectra, with the height of each rectangle equal to the band-averaged brightness temperature using the South Pole spectrum. A.1.2 Cross-checks with map-based simulatio… view at source ↗
Figure 68
Figure 68. Figure 68: Forecasted lensing AL residual (grey scale plus colored contours as labeled) using the EB-only iterative delensing [562], as a function of the beam full width half maximum and noise level in Q and U. 104 105 106 10−4 10−3 10−2 10−1 σ(r) Delensed No Decorrelation No Delensing Raw Sensitivity 104 105 106 10% 100% Total Number of Detector Years (150 GHz equivalent) RMS Lensing residual Delensing/Total Effort… view at source ↗
Figure 69
Figure 69. Figure 69: Top panels: forecasted uncertainty on r as a function of effort (left) and sky fraction fsky (right). The left panel is for 3% sky fraction, whereas the right panel is for 1.8 × 106 detector years of effort, as represented by the vertical dashed lines. We included in solid black the case of full delensing, while allowing for decorrelation of the foregrounds, in solid grey the case without delensing, in do… view at source ↗
Figure 70
Figure 70. Figure 70: Optimized map-depth in each of the small-aperture channels as well as in the delensing channel, for an fsky = 3%. A.1.2.1 Map noise realizations To produce map-level simulations it is necessary to translate the BICEP/Keck noise bandpowers into a prescription for map noise. We do this by fitting the N`s to a white + ` γ model accounting for beam smoothing, etc. For the small-aperture BICEP/Keck data, we fi… view at source ↗
Figure 71
Figure 71. Figure 71: Detector-second hit patterns on the sky for small aperture telescope surveys. top: the actual BICEP3 2017 hit pattern, middle left: idealized circular pattern as used in Sect. A.1.2, middle right: simulated “Chile full” pattern, bottom left: simulated “Pole wide” pattern, and bottom right: simulated “Pole deep” pattern. Each pattern is normalized to the same sum and the color scales are equal. (The “Chile… view at source ↗
Figure 72
Figure 72. Figure 72 [PITH_FULL_IMAGE:figures/full_fig_p214_72.png] view at source ↗
Figure 73
Figure 73. Figure 73: Uncertainty on r as a function of the value of r, for 18 tubes, for “Pole deep,” “Pole wide” and “Chile full.” The upper left is a subset of [PITH_FULL_IMAGE:figures/full_fig_p215_73.png] view at source ↗
Figure 74
Figure 74. Figure 74: Uncertainty on r as a function of the value of r, for 18 optics tubes, and various splits between Pole and Chile siting. As in the previous figures, these results correspond to seven years of observation and observing efficiency in Chile equal to that at Pole. For clarity, we only show the forecast using the 28% cleanest polarized sky. Note that in the case where all the tubes are at Pole, we use the “Pol… view at source ↗
Figure 75
Figure 75. Figure 75: Impact of changes to the noise level, beam size, and sky fraction on forecasted 1σ constraints on Neff with Yp fixed by BBN consistency. Changes to fsky are taken here at fixed map depth. The forecasts shown in this figure have less detailed modeling of atmospheric effects and foreground cleaning than those shown elsewhere. The results should therefore be taken as a guide to how various experimental desig… view at source ↗
Figure 76
Figure 76. Figure 76: Impact of changes to the sky fraction at fixed effort on forecasted 1σ constraints on Neff with Yp fixed by BBN consistency. The forecasts shown in this figure have less detailed modeling of atmospheric effects and foreground cleaning than those shown elsewhere and should be taken to be accurate only at the level of about 10%. array NETs to produce effective atmosphere equivalent noise powers, in µK2 s, t… view at source ↗
Figure 77
Figure 77. Figure 77: Forecasted 1σ constraints on Neff for different choices of the minimum observing elevation as a function of the size of the galactic mask shown for the nominal scan strategy discussed in the text. A.2.4 Fisher forecasts For the forecasts, we begin with the multi-frequency model described in subsection A.2.3 and noise spectra based on the depth maps A.2.2. A harmonic space ILC algorithm [571] is used to de… view at source ↗
Figure 78
Figure 78. Figure 78: Panel 1 shows the expected number of SNR ≥ 5 clusters as a function of redshift for the deep and wide (black) and ultra-deep (gray) fields with a 6-m aperture corresponding to 1. 0 5 at 150 GHz. Panels 2, 3 show the dependence on telescope size and noise levels for the deep and wide survey. To get a sample of clusters at z& 2, given our current understanding of high-redshift clusters, an aperture size ≥ 6… view at source ↗
Figure 79
Figure 79. Figure 79: Limiting mass as a function of redshift for CMB-S4 galaxy cluster surveys. Also shown are existing catalogs of clusters selected by either SZ or X-ray, as well as the projected e-Rosita mass limit. A.3.2 Angular resolution and sensitivity In terms of angular resolution, higher resolution will always be better for more precisely constraining the astrophysics of galaxy formation; the minimum resolution is s… view at source ↗
Figure 80
Figure 80. Figure 80: Effect on limiting mass as a function of redshift by varying noise levels (left) and beam size (right). Solid lines (red, green, blue) show typical progenitor masses as a function of redshift for three different low-redshift cluster groups [PITH_FULL_IMAGE:figures/full_fig_p229_80.png] view at source ↗
Figure 81
Figure 81. Figure 81: Projections for 150-GHz transient source counts from Metzger et al. (2015) [468]. Shown are the total number of on-axis long gamma-ray bursts that are expected to be visible in the entire sky at any one time as a function of flux at 150 GHz. The width of the band schematically represents the uncertainty in this estimate. The inset shows some mm-wave follow-up observations of long gamma-ray bursts [494], s… view at source ↗
Figure 82
Figure 82. Figure 82: Cumulative fraction of time between visits for the deep and wide field, split by declination. Left panel shows the default scan strategy assumed for calculating noise curves for the reference design: right panel shows results for a scan strategy with a high cadence that results in comparable overall survey performance. The ultra-deep field is expected to revisit every location daily in the reference desig… view at source ↗
read the original abstract

We present the science case, reference design, and project plan for the Stage-4 ground-based cosmic microwave background experiment CMB-S4.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

0 major / 0 minor

Summary. The manuscript presents the science case, reference design, and project plan for the Stage-4 ground-based cosmic microwave background experiment CMB-S4.

Significance. If the outlined reference design proves feasible, the document would serve as a foundational roadmap for a major international CMB effort, enabling precision measurements that could constrain inflationary models, neutrino properties, and dark energy with unprecedented sensitivity. The comprehensive integration of science goals with technical and project planning strengthens its value to the field.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their positive review and recommendation to accept the manuscript. We appreciate the recognition that the document could serve as a foundational roadmap for the CMB-S4 effort.

Circularity Check

0 steps flagged

No significant circularity

full rationale

This is a planning white paper that presents a science case, reference design, and project plan for CMB-S4 without any derivations, equations, predictions, or empirical results. No load-bearing steps reduce to fitted inputs, self-citations, or ansatzes; the text is forward-looking and self-contained against external benchmarks with no internal reduction of claims.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a project planning document with no free parameters, axioms, or invented entities introduced; it does not contain theoretical derivations or data fits.

pith-pipeline@v0.9.0 · 6603 in / 993 out tokens · 22814 ms · 2026-05-24T23:53:20.791981+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Forward citations

Cited by 18 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score.

  1. Primordial Black Hole from Tensor-induced Density Fluctuation: First-order Phase Transitions and Domain Walls

    astro-ph.CO 2026-05 unverdicted novelty 6.0

    Tensor perturbations from first-order phase transitions and domain wall annihilation induce curvature fluctuations at second order that form primordial black holes, allowing asteroid-mass PBHs to comprise all dark mat...

  2. Graph-based Summary Statistics for Revealing the Stochastic Gravitational Wave Background in Pulsar Timing Arrays

    astro-ph.CO 2025-09 unverdicted novelty 6.0

    Graph-based summary statistics on pulsar timing residuals detect SGWB down to strain amplitude 1.2e-15 and yield 2.3 sigma evidence in NANOGrav 15-year data via clustering coefficient and edge weight measures.

  3. Constraining Inflationary Particle Production with CMB Polarization

    astro-ph.CO 2025-09 unverdicted novelty 6.0

    No evidence for primordial hotspots in Planck polarization data leads to improved bounds on inflationary particle production couplings for light particles.

  4. The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models

    astro-ph.CO 2025-03 accept novelty 6.0

    ACT DR6 CMB data shows no significant evidence for extensions beyond Lambda CDM, with neutrino effective species at 2.86 plus or minus 0.13 and sum of neutrino masses below 0.082 eV at 95 percent CL.

  5. Zee models with a non-invertible $Z_M$ symmetry

    hep-ph 2026-05 unverdicted novelty 5.0

    Zee models are classified under non-invertible Z_M symmetries; viable candidates are identified from data consistency, and a Z_7 benchmark yields numerical predictions for neutrino parameters and CLFV rates.

  6. Cosmological History of Flavour Deconstruction Models: Constraints from Monopole Production

    hep-ph 2026-05 unverdicted novelty 5.0

    Flavour deconstruction models with semi-simple gauge groups generically produce light monopoles that require low-scale reheating after inflation to satisfy cosmological and astrophysical bounds.

  7. Inflaton Accretion onto Primordial Black Holes During Reheating

    astro-ph.CO 2026-05 unverdicted novelty 5.0

    Inflaton accretion during reheating drives non-linear PBH mass growth that extends lifetimes and amplifies emitted SGWB by multiple orders of magnitude.

  8. Probing Bose-enhanced Inflaton Decay with Gravitational Waves

    hep-ph 2026-01 unverdicted novelty 5.0

    Bose enhancement from a transient condensate of inflaton decay products dramatically increases decay efficiency and amplifies stochastic gravitational wave production to potentially observable levels.

  9. Cosmological Probes of Lepton Parity Freeze-in Dark Matter: $\Delta N_{\rm eff}$ & Gravitational Waves

    hep-ph 2025-11 unverdicted novelty 5.0

    Lepton parity stabilizes a Majorana fermion as freeze-in dark matter produced via right-handed neutrino or Higgs decays, yielding detectable gravitational waves or ΔN_eff depending on scalar couplings.

  10. Probing Dark Energy Microphysics with kSZ Tomography

    astro-ph.CO 2025-11 conditional novelty 5.0

    Fisher-matrix forecasts for LSST- and CMB-S4-like surveys show kSZ tomography tightens constraints on dark energy parameters w0 and wa by 15% and 32% while assessing detectability of perturbations for different sound speeds.

  11. Chern-Simons gravitational term coupled to a spectator field

    astro-ph.CO 2025-01 unverdicted novelty 5.0

    Coupling Chern-Simons gravity to a spectator field in multi-field inflation generates distinctive parity-odd scalar-tensor bispectra with perturbativity bounds on the couplings.

  12. Single field matter bounce with dark energy era: comparison with CMB Planck 2018 data and best fit parameters

    astro-ph.CO 2026-05 conditional novelty 4.0

    A matter bounce model driven by a scalar field with exponential potential fits Planck 2018 CMB data comparably to inflationary ΛCDM, with the potential slope λ directly setting the scalar spectral index ns.

  13. Singlet-doublet dark matter induced radiative neutrino mass and TeV scale leptogenesis

    hep-ph 2026-05 unverdicted novelty 4.0

    Singlet-doublet dark matter induces radiative neutrino masses at one loop while enabling TeV-scale leptogenesis in both Majorana and Dirac realizations.

  14. Galactic foreground residue biases in cosmic-microwave-background lensing-convergence reconstruction and delensing of B-mode maps

    astro-ph.CO 2025-11 unverdicted novelty 4.0

    Galactic foreground residuals after component separation bias lensing reconstruction errors at cosmic-variance levels with Gaussian terms dominating, while non-Gaussian errors are three orders smaller; residuals becom...

  15. MUltiplexed Survey Telescope (MUST) Science White Paper I: Overview of Large-Scale Structure Cosmology in the Era of Stage-V Spectroscopic Surveys

    astro-ph.CO 2024-11 unverdicted novelty 4.0

    MUST is a planned 6.5m Stage-V spectroscopic survey telescope targeting 100M+ galaxies and quasars to z~5.5 for large-scale structure cosmology studies.

  16. A comparison between Galactic magnetic field models and polarized synchrotron emission with C-BASS at 4.76 GHz and S-PASS at 2.3 GHz

    astro-ph.GA 2026-05 unverdicted novelty 3.0

    Comparison of Galactic magnetic field models to polarized synchrotron observations shows good agreement on angles but poor match on intensity, indicating local foreground structures must be incorporated.

  17. Fundamental Physics in 2025: Status, Decisive Targets, and Path Forward

    gr-qc 2025-12 unverdicted novelty 2.0

    The review summarizes the baseline SM+GR+Lambda-CDM framework, lists major anomalies and missing pieces, surveys theoretical and experimental approaches, and outlines a staged roadmap organized by decision points.

  18. Axions as Dark Matter, Dark Energy, and Dark Radiation

    hep-ph 2025-09 unverdicted novelty 2.0

    A mini-review of axion phenomenology showing how light bosons can account for dark matter, drive cosmic acceleration, or contribute to relativistic backgrounds in the early and late Universe.

Reference graph

Works this paper leans on

294 extracted references · 294 canonical work pages · cited by 18 Pith papers · 265 internal anchors

  1. [1]

    Inflation Physics from the Cosmic Microwave Background and Large Scale Structure

    K. N. Abazajian et al., “Inflation Physics from the Cosmic Microwave Background and Large Scale Structure,” Astropart. Phys. 63 (2015) 55–65, arXiv:1309.5381 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  2. [2]

    Neutrino Physics from the Cosmic Microwave Background and Large Scale Structure

    K. N. Abazajian et al., “Neutrino Physics from the Cosmic Microwave Background and Large Scale Structure,” Astropart. Phys. 63 (2015) 66–80, arXiv:1309.5383 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  3. [3]

    CMB-S4 Science Book, First Edition

    CMB-S4 Collaboration, K. N. Abazajian et al. , “CMB-S4 Science Book, First Edition,” arXiv:1610.02743 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  4. [4]

    CMB-S4 Technology Book, First Edition

    M. H. Abitbol, Z. Ahmed, D. Barron, R. Basu Thakur, A. N. Bender, B. A. Benson, C. A. Bischoff, S. A. Bryan, J. E. Carlstrom, and C. L. Chang, “CMB-S4 Technology Book, First Edition,” arXiv e-prints (Jun, 2017) arXiv:1706.02464, arXiv:1706.02464 [astro-ph.IM]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  5. [5]

    BICEP2 / Keck Array VI: Improved Constraints On Cosmology and Foregrounds When Adding 95 GHz Data From Keck Array

    BICEP2, Keck Array Collaboration, P. A. R. Ade et al. , “Improved Constraints on Cosmology and Foregrounds from BICEP2 and Keck Array Cosmic Microwave Background Data with Inclusion of 95 GHz Band,” Phys. Rev. Lett. 116 (2016) 031302, arXiv:1510.09217 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  6. [6]

    Universality Class in Conformal Inflation

    R. Kallosh and A. Linde, “Universality Class in Conformal Inflation,” JCAP 1307 (2013) 002, arXiv:1306.5220 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  7. [7]

    A New Type of Isotropic Cosmological Models Without Singularity,

    A. A. Starobinsky, “A New Type of Isotropic Cosmological Models Without Singularity,” Phys.Lett. B91 (1980) 99–102

    work page 1980

  8. [8]

    The Standard Model Higgs boson as the inflaton

    F. L. Bezrukov and M. Shaposhnikov, “The Standard Model Higgs boson as the inflaton,” Phys. Lett. B659 (2008) 703–706, arXiv:0710.3755 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  9. [9]

    Fibre Inflation: Observable Gravity Waves from IIB String Compactifications

    M. Cicoli, C. P. Burgess, and F. Quevedo, “Fibre Inflation: Observable Gravity Waves from IIB String Compactifications,” JCAP 0903 (2009) 013, arXiv:0808.0691 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  10. [10]

    Light Sterile Neutrinos: A White Paper

    K. N. Abazajian et al., “Light Sterile Neutrinos: A White Paper,” arXiv:1204.5379 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  11. [11]

    Working Group Report: New Light Weakly Coupled Particles,

    R. Essig et al., “Working Group Report: New Light Weakly Coupled Particles,” inCommunity Summer Study 2013: Snowmass on the Mississippi (CSS2013), Minneapolis, MN, USA, July 29-August 6,

    work page 2013

  12. [12]

    Dark Sectors and New, Light, Weakly-Coupled Particles

    2013. arXiv:1311.0029 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  13. [13]

    Dark Sectors 2016 Workshop: Community Report

    J. Alexander et al. , “Dark Sectors 2016 Workshop: Community Report,” arXiv:1608.08632 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  14. [14]

    Millimeter Transient Point Sources in the SPTpol 100 Square Degree Survey

    N. Whitehorn, T. Natoli, P. A. R. Ade, J. E. Austermann, J. A. Beall, A. N. Bender, B. A. Benson, L. E. Bleem, J. E. Carlstrom, C. L. Chang, H. C. Chiang, H.-M. Cho, R. Citron, T. M. Crawford, A. T. Crites, T. de Haan, M. A. Dobbs, W. Everett, J. Gallicchio, E. M. George, A. Gilbert, N. W. Halverson, N. Harrington, J. W. Henning, G. C. Hilton, G. P. Holde...

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  15. [15]

    K. D. Alexander, E. Berger, W. Fong, P. K. G. Williams, C. Guidorzi, R. Margutti, B. D. Metzger, J. Annis, P. K. Blanchard, D. Brout, D. A. Brown, H.-Y. Chen, R. Chornock, P. S. Cowperthwaite, M. Drout, T. Eftekhari, J. Frieman, D. E. Holz, M. Nicholl, A. Rest, M. Sako, M. Soares-Santos, and V. A. Villar, “The Electromagnetic Counterpart of the Binary Neu...

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  16. [16]

    Short-Duration Gamma-Ray Bursts

    E. Berger, “Short-Duration Gamma-Ray Bursts,” Ann. Rev. Astron. Astroph. 52 (Aug., 2014) 43–105, arXiv:1311.2603 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  17. [17]

    Planck 2013 Results. XXIV. Constraints on primordial non-Gaussianity

    Planck Collaboration, Planck Collaboration XXIV, “Planck 2013 Results. XXIV. Constraints on primordial non-Gaussianity,” Astron. Astrophys. 571 (2014) A24, arXiv:1303.5084 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  18. [18]

    Planck 2015 results. XVII. Constraints on primordial non-Gaussianity

    Planck Collaboration XVII, “Planck 2015 results. XVII. Constraints on primordial non-Gaussianity,” arXiv:1502.01592 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  19. [19]

    The Dynamics of General Relativity

    R. L. Arnowitt, S. Deser, and C. W. Misner, “The Dynamics of general relativity,” Gen. Rel. Grav. 40 (2008) 1997–2027, arXiv:gr-qc/0405109 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  20. [20]

    Scale-dependent gravitational waves from a rolling axion

    R. Namba, M. Peloso, M. Shiraishi, L. Sorbo, and C. Unal, “Scale-dependent gravitational waves from a rolling axion,” JCAP 1601 no. 01, (2016) 041, arXiv:1509.07521 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  21. [21]

    Gravitational waves and large field inflation

    A. Linde, “Gravitational waves and large field inflation,” JCAP 1702 no. 02, (2017) 006, arXiv:1612.00020 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  22. [22]

    The shape of non-Gaussianities

    D. Babich, P. Creminelli, and M. Zaldarriaga, “The Shape of Non-Gaussianities,” JCAP 0408 (2004) 009, arXiv:astro-ph/0405356 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  23. [23]

    Non-Gaussianity as a Probe of the Physics of the Primordial Universe and the Astrophysics of the Low Redshift Universe

    E. Komatsu et al. , “Non-Gaussianity as a Probe of the Physics of the Primordial Universe and the Astrophysics of the Low Redshift Universe,” arXiv:0902.4759 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  24. [24]

    On CMB B-Mode Non-Gaussianity

    P. D. Meerburg, J. Meyers, A. van Engelen, and Y. Ali-Ha¨ ımoud, “CMB B -mode non-Gaussianity,” Phys. Rev. D93 no. 12, (2016) 123511, arXiv:1603.02243 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  25. [25]

    On graviton non-Gaussianities during inflation

    J. M. Maldacena and G. L. Pimentel, “On graviton non-Gaussianities during inflation,” JHEP 09 (2011) 045, arXiv:1104.2846 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  26. [26]

    Tensor Squeezed Limits and the Higuchi Bound

    L. Bordin, P. Creminelli, M. Mirbabayi, and J. Nore˜ na, “Tensor Squeezed Limits and the Higuchi Bound,” JCAP 1609 no. 09, (2016) 041, arXiv:1605.08424 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  27. [27]

    Large Tensor Non-Gaussianity from Axion-Gauge Fields Dynamics

    A. Agrawal, T. Fujita, and E. Komatsu, “Large tensor non-Gaussianity from axion-gauge field dynamics,” PRD 97 no. 10, (2018) 103526, arXiv:1707.03023 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  28. [28]

    CMB Scale Dependent Non-Gaussianity from Massive Gravity during Inflation

    G. Dom` enech, T. Hiramatsu, C. Lin, M. Sasaki, M. Shiraishi, and Y. Wang, “CMB Scale Dependent Non-Gaussianity from Massive Gravity during Inflation,” JCAP 1705 no. 05, (2017) 034, arXiv:1701.05554 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  29. [30]

    Non-Gaussianity as a Particle Detector

    H. Lee, D. Baumann, and G. L. Pimentel, “Non-Gaussianity as a Particle Detector,” JHEP 12 (2016) 040, arXiv:1607.03735 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  30. [31]

    Partially Massless Fields During Inflation

    D. Baumann, G. Goon, H. Lee, and G. L. Pimentel, “Partially Massless Fields During Inflation,” JHEP 04 (2018) 140, arXiv:1712.06624 [hep-th] . CMB-S4 Science Case, Reference Design, and Project Plan References 233

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  31. [32]

    Planck 2018 results. X. Constraints on inflation

    Planck Collaboration, Planck Collaboration X, “Planck 2018 results. X. Constraints on inflation,” arXiv:1807.06211 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  32. [33]

    First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results

    C. L. Bennett et al. , “First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Preliminary Maps and Basic Results,” Astrophys. J. Suppl. 148 (2003) 1, arXiv:astro-ph/0302207

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  33. [34]

    First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters

    D. N. Spergel et al. , “First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters,” Astrophys. J. Suppl. 148 (2003) 175, arXiv:astro-ph/0302209

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  34. [35]

    Planck 2015 results. XX. Constraints on inflation

    Planck Collaboration XX, “Planck 2015 results. XX. Constraints on inflation,” arXiv:1502.02114 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  35. [36]

    Scratches from the Past: Inflationary Archaeology through Features in the Power Spectrum of Primordial Fluctuations

    A. Slosar et al. , “Scratches from the Past: Inflationary Archaeology through Features in the Power Spectrum of Primordial Fluctuations,” arXiv:1903.09883 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 1903

  36. [37]

    Reconstructing the primordial power spectrum

    S. L. Bridle, A. M. Lewis, J. Weller, and G. Efstathiou, “Reconstructing the primordial power spectrum,” Mon. Not. Roy. Astron. Soc. 342 (July, 2003) L72–L78, arXiv:astro-ph/0302306 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  37. [38]

    Reconstruction of the primordial power spectrum from CMB data

    Z.-K. Guo, D. J. Schwarz, and Y.-Z. Zhang, “Reconstruction of the primordial power spectrum from CMB data,” Journal of Cosmology and Astro-Particle Physics 2011 (Aug., 2011) 031, arXiv:1105.5916 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  38. [39]

    The Atacama Cosmology Telescope: a measurement of the primordial power spectrum

    R. Hlozek, J. Dunkley, G. Addison, J. W. Appel, J. R. Bond, C. Sofia Carvalho, S. Das, M. J. Devlin, R. D¨ unner, T. Essinger-Hileman, J. W. Fowler, P. Gallardo, A. Hajian, M. Halpern, M. Hasselfield, M. Hilton, A. D. Hincks, J. P. Hughes, K. D. Irwin, J. Klein, A. Kosowsky, T. A. Marriage, D. Marsden, F. Menanteau, K. Moodley, M. D. Niemack, M. R. Nolta, L...

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  39. [40]

    Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets

    M. Aich, D. K. Hazra, L. Sriramkumar, and T. Souradeep, “Oscillations in the inflaton potential: Complete numerical treatment and comparison with the recent and forthcoming CMB datasets,” Phys. Rev. D 87 (Apr., 2013) 083526, arXiv:1106.2798 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  40. [41]

    Reconstruction of the primordial power spectrum of curvature perturbations using multiple data sets

    P. Hunt and S. Sarkar, “Reconstruction of the primordial power spectrum of curvature perturbations using multiple data sets,” Journal of Cosmology and Astro-Particle Physics 2014 (Jan., 2014) 025, arXiv:1308.2317 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  41. [42]

    Inflationary Freedom and Cosmological Neutrino Constraints

    R. de Putter, E. V. Linder, and A. Mishra, “Inflationary freedom and cosmological neutrino constraints,” Phys. Rev. D 89 (May, 2014) 103502, arXiv:1401.7022 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  42. [43]

    Nonlinear excitations in inflationary power spectra,

    V. Miranda, W. Hu, C. He, and H. Motohashi, “Nonlinear excitations in inflationary power spectra,” Phys. Rev. D 93 (Jan., 2016) 023504

    work page 2016

  43. [44]

    Primordial features and Planck polarization,

    D. K. Hazra, A. Shafieloo, G. F. Smoot, and A. A. Starobinsky, “Primordial features and Planck polarization,” Journal of Cosmology and Astro-Particle Physics 2016 (Sept., 2016) 009

    work page 2016

  44. [45]

    Generalized Slow Roll for Large Power Spectrum Features

    C. Dvorkin and W. Hu, “Generalized Slow Roll for Large Power Spectrum Features,” Phys. Rev. D81 (2010) 023518, arXiv:0910.2237 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  45. [46]

    CMB Constraints on Principal Components of the Inflaton Potential

    C. Dvorkin and W. Hu, “CMB Constraints on Principal Components of the Inflaton Potential,” Phys. Rev. D82 (2010) 043513, arXiv:1007.0215 [astro-ph.CO] . CMB-S4 Science Case, Reference Design, and Project Plan 234 References

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  46. [47]

    Complete WMAP Constraints on Bandlimited Inflationary Features

    C. Dvorkin and W. Hu, “Complete WMAP Constraints on Bandlimited Inflationary Features,” Phys. Rev. D84 (2011) 063515, arXiv:1106.4016 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  47. [48]

    Inflationary Features and Shifts in Cosmological Parameters from Planck 2015 Data

    G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, “Inflationary Features and Shifts in Cosmological Parameters from Planck 2015 Data,” Phys. Rev. D96 no. 8, (2017) 083526, arXiv:1706.09412 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  48. [49]

    Inflationary vs. Reionization Features from Planck 2015 Data

    G. Obied, C. Dvorkin, C. Heinrich, W. Hu, and V. Miranda, “Inflationary versus reionization features from P lanck 2015 data,” Phys. Rev. D98 no. 4, (2018) 043518, arXiv:1803.01858 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  49. [51]

    Cosmic background radiation anisotropies in universes dominated by nonbaryonic dark matter,

    J. R. Bond and G. Efstathiou, “Cosmic background radiation anisotropies in universes dominated by nonbaryonic dark matter,” Astrophys. J. 285 (1984) L45–L48

    work page 1984

  50. [52]

    Evolution of Isocurvature Perturbations. 1. Photon - Baryon Universe,

    H. Kodama and M. Sasaki, “Evolution of Isocurvature Perturbations. 1. Photon - Baryon Universe,” Int. J. Mod. Phys. A1 (1986) 265

    work page 1986

  51. [53]

    Evolution of Isocurvature Perturbations. 2. Radiation Dust Universe,

    H. Kodama and M. Sasaki, “Evolution of Isocurvature Perturbations. 2. Radiation Dust Universe,” Int. J. Mod. Phys. A2 (1987) 491

    work page 1987

  52. [54]

    Toward Understanding CMB Anisotropies and Their Implications

    W. Hu and N. Sugiyama, “Toward understanding CMB anisotropies and their implications,” Phys. Rev. D51 (1995) 2599–2630, astro-ph/9411008

    work page internal anchor Pith review Pith/arXiv arXiv 1995

  53. [55]

    Constraints on isocurvature models from the WMAP first-year data

    K. Moodley, M. Bucher, J. Dunkley, P. G. Ferreira, and C. Skordis, “Constraints on isocurvature models from the WMAP first-year data,” Phys. Rev. D70 (2004) 103520, arXiv:astro-ph/0407304 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  54. [56]

    Constraining Isocurvature Initial Conditions with WMAP 3-year data

    R. Bean, J. Dunkley, and E. Pierpaoli, “Constraining Isocurvature Initial Conditions with WMAP 3-year data,” Phys. Rev. D74 (2006) 063503, astro-ph/0606685

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  55. [57]

    Limits on isocurvature fluctuations from Boomerang and MAXIMA

    K. Enqvist, H. Kurki-Suonio, and J. Valiviita, “Limits on isocurvature fluctuations from boomerang and MAXIMA,” Phys. Rev. D62 (2000) 103003, arXiv:astro-ph/0006429 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  56. [58]

    Cosmological Parameters from the 2003 flight of BOOMERANG

    C. J. MacTavish et al., “Cosmological parameters from the 2003 flight of BOOMERANG,” Astrophys. J. 647 (2006) 799–812, arXiv:astro-ph/0507503 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  57. [59]

    Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from the WMAP data

    WMAP Collaboration, J. Dunkley et al. , “Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from the WMAP data,” Astrophys. J. Suppl. 180 (2009) 306–329, arXiv:0803.0586 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  58. [60]

    Planck 2013 results. XXII. Constraints on inflation

    Planck Collaboration, Planck Collaboration XXII, “Planck 2013 results. XXII. Constraints on inflation,” Astron. Astrophys. 571 (2014) A22, arXiv:1303.5082 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  59. [61]

    Isocurvature Baryon Perturbations and Inflation,

    S. Mollerach, “Isocurvature Baryon Perturbations and Inflation,” Phys.Rev. D42 (1990) 313–325

    work page 1990

  60. [62]

    V. F. Mukhanov, H. Feldman, and R. H. Brandenberger, “Theory of cosmological perturbations. Part

    work page

  61. [63]

    Classical perturbations. Part 2. Quantum theory of perturbations. Part 3. Extensions,” Phys.Rept. 215 (1992) 203–333

    work page 1992

  62. [64]

    Effects of Cosmological Moduli Fields on Cosmic Microwave Background

    T. Moroi and T. Takahashi, “Effects of cosmological moduli fields on cosmic microwave background,” Phys.Lett. B522 (2001) 215–221, hep-ph/0110096. CMB-S4 Science Case, Reference Design, and Project Plan References 235

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  63. [65]

    Generating the curvature perturbation without an inflaton

    D. H. Lyth and D. Wands, “Generating the curvature perturbation without an inflaton,” Phys. Lett. B524 (2002) 5–14, arXiv:hep-ph/0110002 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  64. [66]

    The primordial density perturbation in the curvaton scenario

    D. H. Lyth, C. Ungarelli, and D. Wands, “The Primordial density perturbation in the curvaton scenario,” Phys.Rev. D67 (2003) 023503, astro-ph/0208055

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  65. [67]

    The curvaton scenario in supersymmetric theories

    M. Postma, “The Curvaton scenario in supersymmetric theories,” Phys. Rev. D67 (2003) 063518, hep-ph/0212005

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  66. [68]

    MSSM curvaton in the gauge-mediated SUSY breaking

    S. Kasuya, M. Kawasaki, and F. Takahashi, “MSSM curvaton in the gauge mediated SUSY breaking,” Phys. Lett. B578 (2004) 259–268, hep-ph/0305134

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  67. [69]

    Curvaton Scenario with Affleck-Dine Baryogenesis

    M. Ikegami and T. Moroi, “Curvaton scenario with Affleck-Dine baryogenesis,” Phys. Rev. D70 (2004) 083515, hep-ph/0404253

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  68. [70]

    Sneutrino condensate as a candidate for the hot big bang cosmology

    A. Mazumdar and A. Perez-Lorenzana, “Sneutrino condensate as a candidate for the hot big bang cosmology,” Phys. Rev. D70 (2004) 083526, hep-ph/0406154

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  69. [71]

    Identifying the curvaton within MSSM

    R. Allahverdi, K. Enqvist, A. Jokinen, and A. Mazumdar, “Identifying the curvaton within MSSM,” JCAP 0610 (2006) 007, hep-ph/0603255

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  70. [72]

    Curvaton Dynamics in Brane-worlds

    E. Papantonopoulos and V. Zamarias, “Curvaton Dynamics in Brane-worlds,” JCAP 0611 (2006) 005, gr-qc/0608026

    work page internal anchor Pith review Pith/arXiv arXiv 2006

  71. [73]

    Particle physics models of inflation and curvaton scenarios

    A. Mazumdar and J. Rocher, “Particle physics models of inflation and curvaton scenarios,” Phys. Rept. 497 (2011) 85–215, arXiv:1001.0993

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  72. [74]

    The curvaton scenario in the MSSM and predictions for non-Gaussianity

    A. Mazumdar and S. Nadathur, “The curvaton scenario in the MSSM and predictions for non- Gaussianity,” Phys. Rev. Lett. 108 (2012) 111302, arXiv:1107.4078

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  73. [75]

    Observational constraints on the curvaton model of inflation

    C. Gordon and A. Lewis, “Observational constraints on the curvaton model of inflation,” Phys.Rev. D67 (2003) 123513, astro-ph/0212248

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  74. [76]

    WMAP, neutrino degeneracy and non-Gaussianity constraints on isocurvature perturbations in the curvaton model of inflation

    C. Gordon and K. A. Malik, “WMAP, neutrino degeneracy and non-Gaussianity constraints on isocurvature perturbations in the curvaton model of inflation,” Phys. Rev. D69 (2004) 063508, arXiv:astro-ph/0311102 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  75. [77]

    Future constraints on neutrino isocurvature perturbations in the curvaton scenario

    E. Di Valentino, M. Lattanzi, G. Mangano, A. Melchiorri, and P. Serpico, “Future constraints on neutrino isocurvature perturbations in the curvaton scenario,” Phys.Rev. D85 (2012) 043511, arXiv:1111.3810

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  76. [78]

    Probing a panoply of curvaton-decay scenarios using CMB data

    T. L. Smith and D. Grin, “Probing A Panoply of Curvaton-Decay Scenarios Using CMB Data,” arXiv:1511.07431 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv

  77. [79]

    Do baryons trace dark matter in the early universe?

    D. Grin, O. Dor´ e, and M. Kamionkowski, “Do baryons trace dark matter in the early universe?,” Phys. Rev. Lett. 107 (2011) 261301, arXiv:1107.1716 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  78. [80]

    Compensated Isocurvature Perturbations and the Cosmic Microwave Background

    D. Grin, O. Dor´ e, and M. Kamionkowski, “Compensated Isocurvature Perturbations and the Cosmic Microwave Background,” Phys. Rev. D84 (2011) 123003, arXiv:1107.5047 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  79. [81]

    Baryons do trace dark matter 380,000 years after the big bang: Search for compensated isocurvature perturbations with WMAP 9-year data

    D. Grin, D. Hanson, G. P. Holder, O. Dor´ e, and M. Kamionkowski, “Baryons do trace dark matter 380,000 years after the big bang: Search for compensated isocurvature perturbations with WMAP 9-year data,” Phys. Rev. D89 no. 2, (2014) 023006, arXiv:1306.4319 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  80. [82]

    Compensated isocurvature perturbations in the curvaton model

    C. He, D. Grin, and W. Hu, “Compensated isocurvature perturbations in the curvaton model,” Phys. Rev. D92 no. 6, (2015) 063018, arXiv:1505.00639 [astro-ph.CO] . CMB-S4 Science Case, Reference Design, and Project Plan 236 References

    work page internal anchor Pith review Pith/arXiv arXiv 2015

Showing first 80 references.